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then sys_lib_search_path_spec="/usr/lib/hpux32 /usr/local/lib/hpux32 /usr/local/lib" else sys_lib_search_path_spec="/usr/lib/hpux64 /usr/local/lib/hpux64" fi sys_lib_dlsearch_path_spec=$sys_lib_search_path_spec ;; hppa*64*) shrext_cmds='.sl' hardcode_into_libs=yes dynamic_linker="$host_os dld.sl" shlibpath_var=LD_LIBRARY_PATH # How should we handle SHLIB_PATH shlibpath_overrides_runpath=yes # Unless +noenvvar is specified. library_names_spec='${libname}${release}${shared_ext}$versuffix ${libname}${release}${shared_ext}$major $libname${shared_ext}' soname_spec='${libname}${release}${shared_ext}$major' sys_lib_search_path_spec="/usr/lib/pa20_64 /usr/ccs/lib/pa20_64" sys_lib_dlsearch_path_spec=$sys_lib_search_path_spec ;; *) shrext_cmds='.sl' dynamic_linker="$host_os dld.sl" shlibpath_var=SHLIB_PATH shlibpath_overrides_runpath=no # +s is required to enable SHLIB_PATH library_names_spec='${libname}${release}${shared_ext}$versuffix ${libname}${release}${shared_ext}$major $libname${shared_ext}' soname_spec='${libname}${release}${shared_ext}$major' ;; esac # HP-UX runs *really* slowly unless shared libraries are mode 555, ... postinstall_cmds='chmod 555 $lib' # or fails outright, so override atomically: install_override_mode=555 ;; interix[[3-9]]*) version_type=linux # correct to gnu/linux during the next big refactor need_lib_prefix=no need_version=no library_names_spec='${libname}${release}${shared_ext}$versuffix ${libname}${release}${shared_ext}$major ${libname}${shared_ext}' soname_spec='${libname}${release}${shared_ext}$major' dynamic_linker='Interix 3.x ld.so.1 (PE, like ELF)' shlibpath_var=LD_LIBRARY_PATH shlibpath_overrides_runpath=no hardcode_into_libs=yes ;; irix5* | irix6* | nonstopux*) case $host_os in nonstopux*) version_type=nonstopux ;; *) if test "$lt_cv_prog_gnu_ld" = yes; then version_type=linux # correct to gnu/linux during the next big refactor else version_type=irix fi ;; esac need_lib_prefix=no need_version=no soname_spec='${libname}${release}${shared_ext}$major' library_names_spec='${libname}${release}${shared_ext}$versuffix ${libname}${release}${shared_ext}$major ${libname}${release}${shared_ext} $libname${shared_ext}' case $host_os in irix5* | nonstopux*) libsuff= shlibsuff= ;; *) case $LD in # libtool.m4 will add one of these switches to LD *-32|*"-32 "|*-melf32bsmip|*"-melf32bsmip ") libsuff= shlibsuff= libmagic=32-bit;; *-n32|*"-n32 "|*-melf32bmipn32|*"-melf32bmipn32 ") libsuff=32 shlibsuff=N32 libmagic=N32;; *-64|*"-64 "|*-melf64bmip|*"-melf64bmip ") libsuff=64 shlibsuff=64 libmagic=64-bit;; *) libsuff= shlibsuff= libmagic=never-match;; esac ;; esac shlibpath_var=LD_LIBRARY${shlibsuff}_PATH shlibpath_overrides_runpath=no sys_lib_search_path_spec="/usr/lib${libsuff} /lib${libsuff} /usr/local/lib${libsuff}" sys_lib_dlsearch_path_spec="/usr/lib${libsuff} /lib${libsuff}" hardcode_into_libs=yes ;; # No shared lib support for Linux oldld, aout, or coff. linux*oldld* | linux*aout* | linux*coff*) dynamic_linker=no ;; # This must be glibc/ELF. linux* | k*bsd*-gnu | kopensolaris*-gnu) version_type=linux # correct to gnu/linux during the next big refactor need_lib_prefix=no need_version=no library_names_spec='${libname}${release}${shared_ext}$versuffix ${libname}${release}${shared_ext}$major $libname${shared_ext}' soname_spec='${libname}${release}${shared_ext}$major' finish_cmds='PATH="\$PATH:/sbin" ldconfig -n $libdir' shlibpath_var=LD_LIBRARY_PATH shlibpath_overrides_runpath=no # Some binutils ld are patched to set DT_RUNPATH AC_CACHE_VAL([lt_cv_shlibpath_overrides_runpath], [lt_cv_shlibpath_overrides_runpath=no save_LDFLAGS=$LDFLAGS save_libdir=$libdir eval "libdir=/foo; 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See mingw*. lt_cv_deplibs_check_method='file_magic file format pe-arm-.*little(.*architecture: arm)?' lt_cv_file_magic_cmd='$OBJDUMP -f' ;; darwin* | rhapsody*) lt_cv_deplibs_check_method=pass_all ;; freebsd* | dragonfly*) if echo __ELF__ | $CC -E - | $GREP __ELF__ > /dev/null; then case $host_cpu in i*86 ) # Not sure whether the presence of OpenBSD here was a mistake. # Let's accept both of them until this is cleared up. lt_cv_deplibs_check_method='file_magic (FreeBSD|OpenBSD|DragonFly)/i[[3-9]]86 (compact )?demand paged shared library' lt_cv_file_magic_cmd=/usr/bin/file lt_cv_file_magic_test_file=`echo /usr/lib/libc.so.*` ;; esac else lt_cv_deplibs_check_method=pass_all fi ;; gnu*) lt_cv_deplibs_check_method=pass_all ;; haiku*) lt_cv_deplibs_check_method=pass_all ;; hpux10.20* | hpux11*) lt_cv_file_magic_cmd=/usr/bin/file case $host_cpu in ia64*) lt_cv_deplibs_check_method='file_magic (s[[0-9]][[0-9]][[0-9]]|ELF-[[0-9]][[0-9]]) shared object file - IA64' lt_cv_file_magic_test_file=/usr/lib/hpux32/libc.so ;; hppa*64*) [lt_cv_deplibs_check_method='file_magic (s[0-9][0-9][0-9]|ELF[ -][0-9][0-9])(-bit)?( [LM]SB)? shared object( file)?[, -]* PA-RISC [0-9]\.[0-9]'] lt_cv_file_magic_test_file=/usr/lib/pa20_64/libc.sl ;; *) lt_cv_deplibs_check_method='file_magic (s[[0-9]][[0-9]][[0-9]]|PA-RISC[[0-9]]\.[[0-9]]) shared library' lt_cv_file_magic_test_file=/usr/lib/libc.sl ;; esac ;; interix[[3-9]]*) # PIC code is broken on Interix 3.x, that's why |\.a not |_pic\.a here lt_cv_deplibs_check_method='match_pattern /lib[[^/]]+(\.so|\.a)$' ;; irix5* | irix6* | nonstopux*) case $LD in *-32|*"-32 ") libmagic=32-bit;; *-n32|*"-n32 ") libmagic=N32;; *-64|*"-64 ") libmagic=64-bit;; *) libmagic=never-match;; esac lt_cv_deplibs_check_method=pass_all ;; # This must be glibc/ELF. linux* | k*bsd*-gnu | kopensolaris*-gnu) lt_cv_deplibs_check_method=pass_all ;; netbsd*) if echo __ELF__ | $CC -E - | $GREP __ELF__ > /dev/null; then lt_cv_deplibs_check_method='match_pattern /lib[[^/]]+(\.so\.[[0-9]]+\.[[0-9]]+|_pic\.a)$' else lt_cv_deplibs_check_method='match_pattern /lib[[^/]]+(\.so|_pic\.a)$' fi ;; newos6*) lt_cv_deplibs_check_method='file_magic ELF [[0-9]][[0-9]]*-bit [[ML]]SB (executable|dynamic lib)' lt_cv_file_magic_cmd=/usr/bin/file lt_cv_file_magic_test_file=/usr/lib/libnls.so ;; *nto* | *qnx*) lt_cv_deplibs_check_method=pass_all ;; openbsd*) if test -z "`echo __ELF__ | $CC -E - | $GREP __ELF__`" || test "$host_os-$host_cpu" = "openbsd2.8-powerpc"; then lt_cv_deplibs_check_method='match_pattern /lib[[^/]]+(\.so\.[[0-9]]+\.[[0-9]]+|\.so|_pic\.a)$' else lt_cv_deplibs_check_method='match_pattern /lib[[^/]]+(\.so\.[[0-9]]+\.[[0-9]]+|_pic\.a)$' fi ;; osf3* | osf4* | osf5*) lt_cv_deplibs_check_method=pass_all ;; rdos*) lt_cv_deplibs_check_method=pass_all ;; solaris*) lt_cv_deplibs_check_method=pass_all ;; sysv5* | sco3.2v5* | sco5v6* | unixware* | OpenUNIX* | sysv4*uw2*) lt_cv_deplibs_check_method=pass_all ;; sysv4 | sysv4.3*) case $host_vendor in motorola) lt_cv_deplibs_check_method='file_magic ELF [[0-9]][[0-9]]*-bit [[ML]]SB (shared object|dynamic lib) M[[0-9]][[0-9]]* Version [[0-9]]' lt_cv_file_magic_test_file=`echo /usr/lib/libc.so*` ;; ncr) lt_cv_deplibs_check_method=pass_all ;; sequent) lt_cv_file_magic_cmd='/bin/file' lt_cv_deplibs_check_method='file_magic ELF [[0-9]][[0-9]]*-bit [[LM]]SB (shared object|dynamic lib )' ;; sni) lt_cv_file_magic_cmd='/bin/file' lt_cv_deplibs_check_method="file_magic ELF [[0-9]][[0-9]]*-bit [[LM]]SB dynamic lib" lt_cv_file_magic_test_file=/lib/libc.so ;; siemens) lt_cv_deplibs_check_method=pass_all ;; pc) lt_cv_deplibs_check_method=pass_all ;; esac ;; tpf*) lt_cv_deplibs_check_method=pass_all ;; esac ]) file_magic_glob= want_nocaseglob=no if test "$build" = "$host"; then case $host_os in mingw* | pw32*) if ( shopt | grep nocaseglob ) >/dev/null 2>&1; then want_nocaseglob=yes else file_magic_glob=`echo aAbBcCdDeEfFgGhHiIjJkKlLmMnNoOpPqQrRsStTuUvVwWxXyYzZ | $SED -e "s/\(..\)/s\/[[\1]]\/[[\1]]\/g;/g"` fi ;; esac fi file_magic_cmd=$lt_cv_file_magic_cmd deplibs_check_method=$lt_cv_deplibs_check_method test -z "$deplibs_check_method" && deplibs_check_method=unknown _LT_DECL([], [deplibs_check_method], [1], [Method to check whether dependent libraries are shared objects]) _LT_DECL([], [file_magic_cmd], [1], [Command to use when deplibs_check_method = "file_magic"]) _LT_DECL([], [file_magic_glob], [1], [How to find potential files when deplibs_check_method = "file_magic"]) _LT_DECL([], [want_nocaseglob], [1], [Find potential files using nocaseglob when deplibs_check_method = "file_magic"]) ])# _LT_CHECK_MAGIC_METHOD # LT_PATH_NM # ---------- # find the pathname to a BSD- or MS-compatible name lister AC_DEFUN([LT_PATH_NM], [AC_REQUIRE([AC_PROG_CC])dnl AC_CACHE_CHECK([for BSD- or MS-compatible name lister (nm)], lt_cv_path_NM, [if test -n "$NM"; then # Let the user override the test. lt_cv_path_NM="$NM" else lt_nm_to_check="${ac_tool_prefix}nm" if test -n "$ac_tool_prefix" && test "$build" = "$host"; then lt_nm_to_check="$lt_nm_to_check nm" fi for lt_tmp_nm in $lt_nm_to_check; do lt_save_ifs="$IFS"; IFS=$PATH_SEPARATOR for ac_dir in $PATH /usr/ccs/bin/elf /usr/ccs/bin /usr/ucb /bin; do IFS="$lt_save_ifs" test -z "$ac_dir" && ac_dir=. tmp_nm="$ac_dir/$lt_tmp_nm" if test -f "$tmp_nm" || test -f "$tmp_nm$ac_exeext" ; then # Check to see if the nm accepts a BSD-compat flag. # Adding the `sed 1q' prevents false positives on HP-UX, which says: # nm: unknown option "B" ignored # Tru64's nm complains that /dev/null is an invalid object file case `"$tmp_nm" -B /dev/null 2>&1 | sed '1q'` in */dev/null* | *'Invalid file or object type'*) lt_cv_path_NM="$tmp_nm -B" break ;; *) case `"$tmp_nm" -p /dev/null 2>&1 | sed '1q'` in */dev/null*) lt_cv_path_NM="$tmp_nm -p" break ;; *) lt_cv_path_NM=${lt_cv_path_NM="$tmp_nm"} # keep the first match, but continue # so that we can try to find one that supports BSD flags ;; esac ;; esac fi done IFS="$lt_save_ifs" done : ${lt_cv_path_NM=no} fi]) if test "$lt_cv_path_NM" != "no"; then NM="$lt_cv_path_NM" else # Didn't find any BSD compatible name lister, look for dumpbin. if test -n "$DUMPBIN"; then : # Let the user override the test. else AC_CHECK_TOOLS(DUMPBIN, [dumpbin "link -dump"], :) case `$DUMPBIN -symbols /dev/null 2>&1 | sed '1q'` in *COFF*) DUMPBIN="$DUMPBIN -symbols" ;; *) DUMPBIN=: ;; esac fi AC_SUBST([DUMPBIN]) if test "$DUMPBIN" != ":"; then NM="$DUMPBIN" fi fi test -z "$NM" && NM=nm AC_SUBST([NM]) _LT_DECL([], [NM], [1], [A BSD- or MS-compatible name lister])dnl AC_CACHE_CHECK([the name lister ($NM) interface], [lt_cv_nm_interface], [lt_cv_nm_interface="BSD nm" echo "int some_variable = 0;" > conftest.$ac_ext (eval echo "\"\$as_me:$LINENO: $ac_compile\"" >&AS_MESSAGE_LOG_FD) (eval "$ac_compile" 2>conftest.err) cat conftest.err >&AS_MESSAGE_LOG_FD (eval echo "\"\$as_me:$LINENO: $NM \\\"conftest.$ac_objext\\\"\"" >&AS_MESSAGE_LOG_FD) (eval "$NM \"conftest.$ac_objext\"" 2>conftest.err > conftest.out) cat conftest.err >&AS_MESSAGE_LOG_FD (eval echo "\"\$as_me:$LINENO: output\"" >&AS_MESSAGE_LOG_FD) cat conftest.out >&AS_MESSAGE_LOG_FD if $GREP 'External.*some_variable' conftest.out > /dev/null; then lt_cv_nm_interface="MS dumpbin" fi rm -f conftest*]) ])# LT_PATH_NM # Old names: AU_ALIAS([AM_PROG_NM], [LT_PATH_NM]) AU_ALIAS([AC_PROG_NM], [LT_PATH_NM]) dnl aclocal-1.4 backwards compatibility: dnl AC_DEFUN([AM_PROG_NM], []) dnl AC_DEFUN([AC_PROG_NM], []) # _LT_CHECK_SHAREDLIB_FROM_LINKLIB # -------------------------------- # how to determine the name of the shared library # associated with a specific link library. # -- PORTME fill in with the dynamic library characteristics m4_defun([_LT_CHECK_SHAREDLIB_FROM_LINKLIB], [m4_require([_LT_DECL_EGREP]) m4_require([_LT_DECL_OBJDUMP]) m4_require([_LT_DECL_DLLTOOL]) AC_CACHE_CHECK([how to associate runtime and link libraries], lt_cv_sharedlib_from_linklib_cmd, [lt_cv_sharedlib_from_linklib_cmd='unknown' case $host_os in cygwin* | mingw* | pw32* | cegcc*) # two different shell functions defined in ltmain.sh # decide which to use based on capabilities of $DLLTOOL case `$DLLTOOL --help 2>&1` in *--identify-strict*) lt_cv_sharedlib_from_linklib_cmd=func_cygming_dll_for_implib ;; *) lt_cv_sharedlib_from_linklib_cmd=func_cygming_dll_for_implib_fallback ;; esac ;; *) # fallback: assume linklib IS sharedlib lt_cv_sharedlib_from_linklib_cmd="$ECHO" ;; esac ]) sharedlib_from_linklib_cmd=$lt_cv_sharedlib_from_linklib_cmd test -z "$sharedlib_from_linklib_cmd" && sharedlib_from_linklib_cmd=$ECHO _LT_DECL([], [sharedlib_from_linklib_cmd], [1], [Command to associate shared and link libraries]) ])# _LT_CHECK_SHAREDLIB_FROM_LINKLIB # _LT_PATH_MANIFEST_TOOL # ---------------------- # locate the manifest tool m4_defun([_LT_PATH_MANIFEST_TOOL], [AC_CHECK_TOOL(MANIFEST_TOOL, mt, :) test -z "$MANIFEST_TOOL" && MANIFEST_TOOL=mt AC_CACHE_CHECK([if $MANIFEST_TOOL is a manifest tool], [lt_cv_path_mainfest_tool], [lt_cv_path_mainfest_tool=no echo "$as_me:$LINENO: $MANIFEST_TOOL '-?'" >&AS_MESSAGE_LOG_FD $MANIFEST_TOOL '-?' 2>conftest.err > conftest.out cat conftest.err >&AS_MESSAGE_LOG_FD if $GREP 'Manifest Tool' conftest.out > /dev/null; then lt_cv_path_mainfest_tool=yes fi rm -f conftest*]) if test "x$lt_cv_path_mainfest_tool" != xyes; then MANIFEST_TOOL=: fi _LT_DECL([], [MANIFEST_TOOL], [1], [Manifest tool])dnl ])# _LT_PATH_MANIFEST_TOOL # LT_LIB_M # -------- # check for math library AC_DEFUN([LT_LIB_M], [AC_REQUIRE([AC_CANONICAL_HOST])dnl LIBM= case $host in *-*-beos* | *-*-cegcc* | *-*-cygwin* | *-*-haiku* | *-*-pw32* | *-*-darwin*) # These system don't have libm, or don't need it ;; *-ncr-sysv4.3*) AC_CHECK_LIB(mw, _mwvalidcheckl, LIBM="-lmw") AC_CHECK_LIB(m, cos, LIBM="$LIBM -lm") ;; *) AC_CHECK_LIB(m, cos, LIBM="-lm") ;; esac AC_SUBST([LIBM]) ])# LT_LIB_M # Old name: AU_ALIAS([AC_CHECK_LIBM], [LT_LIB_M]) dnl aclocal-1.4 backwards compatibility: dnl AC_DEFUN([AC_CHECK_LIBM], []) # _LT_COMPILER_NO_RTTI([TAGNAME]) # ------------------------------- m4_defun([_LT_COMPILER_NO_RTTI], [m4_require([_LT_TAG_COMPILER])dnl _LT_TAGVAR(lt_prog_compiler_no_builtin_flag, $1)= if test "$GCC" = yes; then case $cc_basename in nvcc*) _LT_TAGVAR(lt_prog_compiler_no_builtin_flag, $1)=' -Xcompiler -fno-builtin' ;; *) _LT_TAGVAR(lt_prog_compiler_no_builtin_flag, $1)=' -fno-builtin' ;; esac _LT_COMPILER_OPTION([if $compiler supports -fno-rtti -fno-exceptions], lt_cv_prog_compiler_rtti_exceptions, [-fno-rtti -fno-exceptions], [], [_LT_TAGVAR(lt_prog_compiler_no_builtin_flag, $1)="$_LT_TAGVAR(lt_prog_compiler_no_builtin_flag, $1) -fno-rtti -fno-exceptions"]) fi _LT_TAGDECL([no_builtin_flag], [lt_prog_compiler_no_builtin_flag], [1], [Compiler flag to turn off builtin functions]) ])# _LT_COMPILER_NO_RTTI # _LT_CMD_GLOBAL_SYMBOLS # ---------------------- m4_defun([_LT_CMD_GLOBAL_SYMBOLS], [AC_REQUIRE([AC_CANONICAL_HOST])dnl AC_REQUIRE([AC_PROG_CC])dnl AC_REQUIRE([AC_PROG_AWK])dnl AC_REQUIRE([LT_PATH_NM])dnl AC_REQUIRE([LT_PATH_LD])dnl m4_require([_LT_DECL_SED])dnl m4_require([_LT_DECL_EGREP])dnl m4_require([_LT_TAG_COMPILER])dnl # Check for command to grab the raw symbol name followed by C symbol from nm. AC_MSG_CHECKING([command to parse $NM output from $compiler object]) AC_CACHE_VAL([lt_cv_sys_global_symbol_pipe], [ # These are sane defaults that work on at least a few old systems. # [They come from Ultrix. What could be older than Ultrix?!! ;)] # Character class describing NM global symbol codes. symcode='[[BCDEGRST]]' # Regexp to match symbols that can be accessed directly from C. sympat='\([[_A-Za-z]][[_A-Za-z0-9]]*\)' # Define system-specific variables. case $host_os in aix*) symcode='[[BCDT]]' ;; cygwin* | mingw* | pw32* | cegcc*) symcode='[[ABCDGISTW]]' ;; hpux*) if test "$host_cpu" = ia64; then symcode='[[ABCDEGRST]]' fi ;; irix* | nonstopux*) symcode='[[BCDEGRST]]' ;; osf*) symcode='[[BCDEGQRST]]' ;; solaris*) symcode='[[BDRT]]' ;; sco3.2v5*) symcode='[[DT]]' ;; sysv4.2uw2*) symcode='[[DT]]' ;; sysv5* | sco5v6* | unixware* | OpenUNIX*) symcode='[[ABDT]]' ;; sysv4) symcode='[[DFNSTU]]' ;; esac # If we're using GNU nm, then use its standard symbol codes. case `$NM -V 2>&1` in *GNU* | *'with BFD'*) symcode='[[ABCDGIRSTW]]' ;; esac # Transform an extracted symbol line into a proper C declaration. # Some systems (esp. on ia64) link data and code symbols differently, # so use this general approach. lt_cv_sys_global_symbol_to_cdecl="sed -n -e 's/^T .* \(.*\)$/extern int \1();/p' -e 's/^$symcode* .* \(.*\)$/extern char \1;/p'" # Transform an extracted symbol line into symbol name and symbol address lt_cv_sys_global_symbol_to_c_name_address="sed -n -e 's/^: \([[^ ]]*\)[[ ]]*$/ {\\\"\1\\\", (void *) 0},/p' -e 's/^$symcode* \([[^ ]]*\) \([[^ ]]*\)$/ {\"\2\", (void *) \&\2},/p'" lt_cv_sys_global_symbol_to_c_name_address_lib_prefix="sed -n -e 's/^: \([[^ ]]*\)[[ ]]*$/ {\\\"\1\\\", (void *) 0},/p' -e 's/^$symcode* \([[^ ]]*\) \(lib[[^ ]]*\)$/ {\"\2\", (void *) \&\2},/p' -e 's/^$symcode* \([[^ ]]*\) \([[^ ]]*\)$/ {\"lib\2\", (void *) \&\2},/p'" # Handle CRLF in mingw tool chain opt_cr= case $build_os in mingw*) opt_cr=`$ECHO 'x\{0,1\}' | tr x '\015'` # option cr in regexp ;; esac # Try without a prefix underscore, then with it. for ac_symprfx in "" "_"; do # Transform symcode, sympat, and symprfx into a raw symbol and a C symbol. symxfrm="\\1 $ac_symprfx\\2 \\2" # Write the raw and C identifiers. if test "$lt_cv_nm_interface" = "MS dumpbin"; then # Fake it for dumpbin and say T for any non-static function # and D for any global variable. # Also find C++ and __fastcall symbols from MSVC++, # which start with @ or ?. lt_cv_sys_global_symbol_pipe="$AWK ['"\ " {last_section=section; section=\$ 3};"\ " /^COFF SYMBOL TABLE/{for(i in hide) delete hide[i]};"\ " /Section length .*#relocs.*(pick any)/{hide[last_section]=1};"\ " \$ 0!~/External *\|/{next};"\ " / 0+ UNDEF /{next}; / UNDEF \([^|]\)*()/{next};"\ " {if(hide[section]) next};"\ " {f=0}; \$ 0~/\(\).*\|/{f=1}; {printf f ? \"T \" : \"D \"};"\ " {split(\$ 0, a, /\||\r/); split(a[2], s)};"\ " s[1]~/^[@?]/{print s[1], s[1]; next};"\ " s[1]~prfx {split(s[1],t,\"@\"); print t[1], substr(t[1],length(prfx))}"\ " ' prfx=^$ac_symprfx]" else lt_cv_sys_global_symbol_pipe="sed -n -e 's/^.*[[ ]]\($symcode$symcode*\)[[ ]][[ ]]*$ac_symprfx$sympat$opt_cr$/$symxfrm/p'" fi lt_cv_sys_global_symbol_pipe="$lt_cv_sys_global_symbol_pipe | sed '/ __gnu_lto/d'" # Check to see that the pipe works correctly. pipe_works=no rm -f conftest* cat > conftest.$ac_ext <<_LT_EOF #ifdef __cplusplus extern "C" { #endif char nm_test_var; void nm_test_func(void); void nm_test_func(void){} #ifdef __cplusplus } #endif int main(){nm_test_var='a';nm_test_func();return(0);} _LT_EOF if AC_TRY_EVAL(ac_compile); then # Now try to grab the symbols. nlist=conftest.nm if AC_TRY_EVAL(NM conftest.$ac_objext \| "$lt_cv_sys_global_symbol_pipe" \> $nlist) && test -s "$nlist"; then # Try sorting and uniquifying the output. if sort "$nlist" | uniq > "$nlist"T; then mv -f "$nlist"T "$nlist" else rm -f "$nlist"T fi # Make sure that we snagged all the symbols we need. if $GREP ' nm_test_var$' "$nlist" >/dev/null; then if $GREP ' nm_test_func$' "$nlist" >/dev/null; then cat <<_LT_EOF > conftest.$ac_ext /* Keep this code in sync between libtool.m4, ltmain, lt_system.h, and tests. */ #if defined(_WIN32) || defined(__CYGWIN__) || defined(_WIN32_WCE) /* DATA imports from DLLs on WIN32 con't be const, because runtime relocations are performed -- see ld's documentation on pseudo-relocs. */ # define LT@&t@_DLSYM_CONST #elif defined(__osf__) /* This system does not cope well with relocations in const data. */ # define LT@&t@_DLSYM_CONST #else # define LT@&t@_DLSYM_CONST const #endif #ifdef __cplusplus extern "C" { #endif _LT_EOF # Now generate the symbol file. eval "$lt_cv_sys_global_symbol_to_cdecl"' < "$nlist" | $GREP -v main >> conftest.$ac_ext' cat <<_LT_EOF >> conftest.$ac_ext /* The mapping between symbol names and symbols. */ LT@&t@_DLSYM_CONST struct { const char *name; void *address; } lt__PROGRAM__LTX_preloaded_symbols[[]] = { { "@PROGRAM@", (void *) 0 }, _LT_EOF $SED "s/^$symcode$symcode* \(.*\) \(.*\)$/ {\"\2\", (void *) \&\2},/" < "$nlist" | $GREP -v main >> conftest.$ac_ext cat <<\_LT_EOF >> conftest.$ac_ext {0, (void *) 0} }; /* This works around a problem in FreeBSD linker */ #ifdef FREEBSD_WORKAROUND static const void *lt_preloaded_setup() { return lt__PROGRAM__LTX_preloaded_symbols; } #endif #ifdef __cplusplus } #endif _LT_EOF # Now try linking the two files. mv conftest.$ac_objext conftstm.$ac_objext lt_globsym_save_LIBS=$LIBS lt_globsym_save_CFLAGS=$CFLAGS LIBS="conftstm.$ac_objext" CFLAGS="$CFLAGS$_LT_TAGVAR(lt_prog_compiler_no_builtin_flag, $1)" if AC_TRY_EVAL(ac_link) && test -s conftest${ac_exeext}; then pipe_works=yes fi LIBS=$lt_globsym_save_LIBS CFLAGS=$lt_globsym_save_CFLAGS else echo "cannot find nm_test_func in $nlist" >&AS_MESSAGE_LOG_FD fi else echo "cannot find nm_test_var in $nlist" >&AS_MESSAGE_LOG_FD fi else echo "cannot run $lt_cv_sys_global_symbol_pipe" >&AS_MESSAGE_LOG_FD fi else echo "$progname: failed program was:" >&AS_MESSAGE_LOG_FD cat conftest.$ac_ext >&5 fi rm -rf conftest* conftst* # Do not use the global_symbol_pipe unless it works. if test "$pipe_works" = yes; then break else lt_cv_sys_global_symbol_pipe= fi done ]) if test -z "$lt_cv_sys_global_symbol_pipe"; then lt_cv_sys_global_symbol_to_cdecl= fi if test -z "$lt_cv_sys_global_symbol_pipe$lt_cv_sys_global_symbol_to_cdecl"; then AC_MSG_RESULT(failed) else AC_MSG_RESULT(ok) fi # Response file support. if test "$lt_cv_nm_interface" = "MS dumpbin"; then nm_file_list_spec='@' elif $NM --help 2>/dev/null | grep '[[@]]FILE' >/dev/null; then nm_file_list_spec='@' fi _LT_DECL([global_symbol_pipe], [lt_cv_sys_global_symbol_pipe], [1], [Take the output of nm and produce a listing of raw symbols and C names]) _LT_DECL([global_symbol_to_cdecl], [lt_cv_sys_global_symbol_to_cdecl], [1], [Transform the output of nm in a proper C declaration]) _LT_DECL([global_symbol_to_c_name_address], [lt_cv_sys_global_symbol_to_c_name_address], [1], [Transform the output of nm in a C name address pair]) _LT_DECL([global_symbol_to_c_name_address_lib_prefix], [lt_cv_sys_global_symbol_to_c_name_address_lib_prefix], [1], [Transform the output of nm in a C name address pair when lib prefix is needed]) _LT_DECL([], [nm_file_list_spec], [1], [Specify filename containing input files for $NM]) ]) # _LT_CMD_GLOBAL_SYMBOLS # _LT_COMPILER_PIC([TAGNAME]) # --------------------------- m4_defun([_LT_COMPILER_PIC], [m4_require([_LT_TAG_COMPILER])dnl _LT_TAGVAR(lt_prog_compiler_wl, $1)= _LT_TAGVAR(lt_prog_compiler_pic, $1)= _LT_TAGVAR(lt_prog_compiler_static, $1)= m4_if([$1], [CXX], [ # C++ specific cases for pic, static, wl, etc. if test "$GXX" = yes; then _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' _LT_TAGVAR(lt_prog_compiler_static, $1)='-static' case $host_os in aix*) # All AIX code is PIC. if test "$host_cpu" = ia64; then # AIX 5 now supports IA64 processor _LT_TAGVAR(lt_prog_compiler_static, $1)='-Bstatic' fi ;; amigaos*) case $host_cpu in powerpc) # see comment about AmigaOS4 .so support _LT_TAGVAR(lt_prog_compiler_pic, $1)='-fPIC' ;; m68k) # FIXME: we need at least 68020 code to build shared libraries, but # adding the `-m68020' flag to GCC prevents building anything better, # like `-m68040'. _LT_TAGVAR(lt_prog_compiler_pic, $1)='-m68020 -resident32 -malways-restore-a4' ;; esac ;; beos* | irix5* | irix6* | nonstopux* | osf3* | osf4* | osf5*) # PIC is the default for these OSes. ;; mingw* | cygwin* | os2* | pw32* | cegcc*) # This hack is so that the source file can tell whether it is being # built for inclusion in a dll (and should export symbols for example). # Although the cygwin gcc ignores -fPIC, still need this for old-style # (--disable-auto-import) libraries m4_if([$1], [GCJ], [], [_LT_TAGVAR(lt_prog_compiler_pic, $1)='-DDLL_EXPORT']) ;; darwin* | rhapsody*) # PIC is the default on this platform # Common symbols not allowed in MH_DYLIB files _LT_TAGVAR(lt_prog_compiler_pic, $1)='-fno-common' ;; *djgpp*) # DJGPP does not support shared libraries at all _LT_TAGVAR(lt_prog_compiler_pic, $1)= ;; haiku*) # PIC is the default for Haiku. # The "-static" flag exists, but is broken. _LT_TAGVAR(lt_prog_compiler_static, $1)= ;; interix[[3-9]]*) # Interix 3.x gcc -fpic/-fPIC options generate broken code. # Instead, we relocate shared libraries at runtime. ;; sysv4*MP*) if test -d /usr/nec; then _LT_TAGVAR(lt_prog_compiler_pic, $1)=-Kconform_pic fi ;; hpux*) # PIC is the default for 64-bit PA HP-UX, but not for 32-bit # PA HP-UX. On IA64 HP-UX, PIC is the default but the pic flag # sets the default TLS model and affects inlining. case $host_cpu in hppa*64*) ;; *) _LT_TAGVAR(lt_prog_compiler_pic, $1)='-fPIC' ;; esac ;; *qnx* | *nto*) # QNX uses GNU C++, but need to define -shared option too, otherwise # it will coredump. _LT_TAGVAR(lt_prog_compiler_pic, $1)='-fPIC -shared' ;; *) _LT_TAGVAR(lt_prog_compiler_pic, $1)='-fPIC' ;; esac else case $host_os in aix[[4-9]]*) # All AIX code is PIC. if test "$host_cpu" = ia64; then # AIX 5 now supports IA64 processor _LT_TAGVAR(lt_prog_compiler_static, $1)='-Bstatic' else _LT_TAGVAR(lt_prog_compiler_static, $1)='-bnso -bI:/lib/syscalls.exp' fi ;; chorus*) case $cc_basename in cxch68*) # Green Hills C++ Compiler # _LT_TAGVAR(lt_prog_compiler_static, $1)="--no_auto_instantiation -u __main -u __premain -u _abort -r $COOL_DIR/lib/libOrb.a $MVME_DIR/lib/CC/libC.a $MVME_DIR/lib/classix/libcx.s.a" ;; esac ;; mingw* | cygwin* | os2* | pw32* | cegcc*) # This hack is so that the source file can tell whether it is being # built for inclusion in a dll (and should export symbols for example). m4_if([$1], [GCJ], [], [_LT_TAGVAR(lt_prog_compiler_pic, $1)='-DDLL_EXPORT']) ;; dgux*) case $cc_basename in ec++*) _LT_TAGVAR(lt_prog_compiler_pic, $1)='-KPIC' ;; ghcx*) # Green Hills C++ Compiler _LT_TAGVAR(lt_prog_compiler_pic, $1)='-pic' ;; *) ;; esac ;; freebsd* | dragonfly*) # FreeBSD uses GNU C++ ;; hpux9* | hpux10* | hpux11*) case $cc_basename in CC*) _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' _LT_TAGVAR(lt_prog_compiler_static, $1)='${wl}-a ${wl}archive' if test "$host_cpu" != ia64; then _LT_TAGVAR(lt_prog_compiler_pic, $1)='+Z' fi ;; aCC*) _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' _LT_TAGVAR(lt_prog_compiler_static, $1)='${wl}-a ${wl}archive' case $host_cpu in hppa*64*|ia64*) # +Z the default ;; *) _LT_TAGVAR(lt_prog_compiler_pic, $1)='+Z' ;; esac ;; *) ;; esac ;; interix*) # This is c89, which is MS Visual C++ (no shared libs) # Anyone wants to do a port? ;; irix5* | irix6* | nonstopux*) case $cc_basename in CC*) _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' _LT_TAGVAR(lt_prog_compiler_static, $1)='-non_shared' # CC pic flag -KPIC is the default. ;; *) ;; esac ;; linux* | k*bsd*-gnu | kopensolaris*-gnu) case $cc_basename in KCC*) # KAI C++ Compiler _LT_TAGVAR(lt_prog_compiler_wl, $1)='--backend -Wl,' _LT_TAGVAR(lt_prog_compiler_pic, $1)='-fPIC' ;; ecpc* ) # old Intel C++ for x86_64 which still supported -KPIC. _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' _LT_TAGVAR(lt_prog_compiler_pic, $1)='-KPIC' _LT_TAGVAR(lt_prog_compiler_static, $1)='-static' ;; icpc* ) # Intel C++, used to be incompatible with GCC. # ICC 10 doesn't accept -KPIC any more. _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' _LT_TAGVAR(lt_prog_compiler_pic, $1)='-fPIC' _LT_TAGVAR(lt_prog_compiler_static, $1)='-static' ;; pgCC* | pgcpp*) # Portland Group C++ compiler _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' _LT_TAGVAR(lt_prog_compiler_pic, $1)='-fpic' _LT_TAGVAR(lt_prog_compiler_static, $1)='-Bstatic' ;; cxx*) # Compaq C++ # Make sure the PIC flag is empty. It appears that all Alpha # Linux and Compaq Tru64 Unix objects are PIC. _LT_TAGVAR(lt_prog_compiler_pic, $1)= _LT_TAGVAR(lt_prog_compiler_static, $1)='-non_shared' ;; xlc* | xlC* | bgxl[[cC]]* | mpixl[[cC]]*) # IBM XL 8.0, 9.0 on PPC and BlueGene _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' _LT_TAGVAR(lt_prog_compiler_pic, $1)='-qpic' _LT_TAGVAR(lt_prog_compiler_static, $1)='-qstaticlink' ;; *) case `$CC -V 2>&1 | sed 5q` in *Sun\ C*) # Sun C++ 5.9 _LT_TAGVAR(lt_prog_compiler_pic, $1)='-KPIC' _LT_TAGVAR(lt_prog_compiler_static, $1)='-Bstatic' _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Qoption ld ' ;; esac ;; esac ;; lynxos*) ;; m88k*) ;; mvs*) case $cc_basename in cxx*) _LT_TAGVAR(lt_prog_compiler_pic, $1)='-W c,exportall' ;; *) ;; esac ;; netbsd*) ;; *qnx* | *nto*) # QNX uses GNU C++, but need to define -shared option too, otherwise # it will coredump. _LT_TAGVAR(lt_prog_compiler_pic, $1)='-fPIC -shared' ;; osf3* | osf4* | osf5*) case $cc_basename in KCC*) _LT_TAGVAR(lt_prog_compiler_wl, $1)='--backend -Wl,' ;; RCC*) # Rational C++ 2.4.1 _LT_TAGVAR(lt_prog_compiler_pic, $1)='-pic' ;; cxx*) # Digital/Compaq C++ _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' # Make sure the PIC flag is empty. It appears that all Alpha # Linux and Compaq Tru64 Unix objects are PIC. _LT_TAGVAR(lt_prog_compiler_pic, $1)= _LT_TAGVAR(lt_prog_compiler_static, $1)='-non_shared' ;; *) ;; esac ;; psos*) ;; solaris*) case $cc_basename in CC* | sunCC*) # Sun C++ 4.2, 5.x and Centerline C++ _LT_TAGVAR(lt_prog_compiler_pic, $1)='-KPIC' _LT_TAGVAR(lt_prog_compiler_static, $1)='-Bstatic' _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Qoption ld ' ;; gcx*) # Green Hills C++ Compiler _LT_TAGVAR(lt_prog_compiler_pic, $1)='-PIC' ;; *) ;; esac ;; sunos4*) case $cc_basename in CC*) # Sun C++ 4.x _LT_TAGVAR(lt_prog_compiler_pic, $1)='-pic' _LT_TAGVAR(lt_prog_compiler_static, $1)='-Bstatic' ;; lcc*) # Lucid _LT_TAGVAR(lt_prog_compiler_pic, $1)='-pic' ;; *) ;; esac ;; sysv5* | unixware* | sco3.2v5* | sco5v6* | OpenUNIX*) case $cc_basename in CC*) _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' _LT_TAGVAR(lt_prog_compiler_pic, $1)='-KPIC' _LT_TAGVAR(lt_prog_compiler_static, $1)='-Bstatic' ;; esac ;; tandem*) case $cc_basename in NCC*) # NonStop-UX NCC 3.20 _LT_TAGVAR(lt_prog_compiler_pic, $1)='-KPIC' ;; *) ;; esac ;; vxworks*) ;; *) _LT_TAGVAR(lt_prog_compiler_can_build_shared, $1)=no ;; esac fi ], [ if test "$GCC" = yes; then _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' _LT_TAGVAR(lt_prog_compiler_static, $1)='-static' case $host_os in aix*) # All AIX code is PIC. if test "$host_cpu" = ia64; then # AIX 5 now supports IA64 processor _LT_TAGVAR(lt_prog_compiler_static, $1)='-Bstatic' fi ;; amigaos*) case $host_cpu in powerpc) # see comment about AmigaOS4 .so support _LT_TAGVAR(lt_prog_compiler_pic, $1)='-fPIC' ;; m68k) # FIXME: we need at least 68020 code to build shared libraries, but # adding the `-m68020' flag to GCC prevents building anything better, # like `-m68040'. _LT_TAGVAR(lt_prog_compiler_pic, $1)='-m68020 -resident32 -malways-restore-a4' ;; esac ;; beos* | irix5* | irix6* | nonstopux* | osf3* | osf4* | osf5*) # PIC is the default for these OSes. ;; mingw* | cygwin* | pw32* | os2* | cegcc*) # This hack is so that the source file can tell whether it is being # built for inclusion in a dll (and should export symbols for example). # Although the cygwin gcc ignores -fPIC, still need this for old-style # (--disable-auto-import) libraries m4_if([$1], [GCJ], [], [_LT_TAGVAR(lt_prog_compiler_pic, $1)='-DDLL_EXPORT']) ;; darwin* | rhapsody*) # PIC is the default on this platform # Common symbols not allowed in MH_DYLIB files _LT_TAGVAR(lt_prog_compiler_pic, $1)='-fno-common' ;; haiku*) # PIC is the default for Haiku. # The "-static" flag exists, but is broken. _LT_TAGVAR(lt_prog_compiler_static, $1)= ;; hpux*) # PIC is the default for 64-bit PA HP-UX, but not for 32-bit # PA HP-UX. On IA64 HP-UX, PIC is the default but the pic flag # sets the default TLS model and affects inlining. case $host_cpu in hppa*64*) # +Z the default ;; *) _LT_TAGVAR(lt_prog_compiler_pic, $1)='-fPIC' ;; esac ;; interix[[3-9]]*) # Interix 3.x gcc -fpic/-fPIC options generate broken code. # Instead, we relocate shared libraries at runtime. ;; msdosdjgpp*) # Just because we use GCC doesn't mean we suddenly get shared libraries # on systems that don't support them. _LT_TAGVAR(lt_prog_compiler_can_build_shared, $1)=no enable_shared=no ;; *nto* | *qnx*) # QNX uses GNU C++, but need to define -shared option too, otherwise # it will coredump. _LT_TAGVAR(lt_prog_compiler_pic, $1)='-fPIC -shared' ;; sysv4*MP*) if test -d /usr/nec; then _LT_TAGVAR(lt_prog_compiler_pic, $1)=-Kconform_pic fi ;; *) _LT_TAGVAR(lt_prog_compiler_pic, $1)='-fPIC' ;; esac case $cc_basename in nvcc*) # Cuda Compiler Driver 2.2 _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Xlinker ' if test -n "$_LT_TAGVAR(lt_prog_compiler_pic, $1)"; then _LT_TAGVAR(lt_prog_compiler_pic, $1)="-Xcompiler $_LT_TAGVAR(lt_prog_compiler_pic, $1)" fi ;; esac else # PORTME Check for flag to pass linker flags through the system compiler. case $host_os in aix*) _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' if test "$host_cpu" = ia64; then # AIX 5 now supports IA64 processor _LT_TAGVAR(lt_prog_compiler_static, $1)='-Bstatic' else _LT_TAGVAR(lt_prog_compiler_static, $1)='-bnso -bI:/lib/syscalls.exp' fi ;; mingw* | cygwin* | pw32* | os2* | cegcc*) # This hack is so that the source file can tell whether it is being # built for inclusion in a dll (and should export symbols for example). m4_if([$1], [GCJ], [], [_LT_TAGVAR(lt_prog_compiler_pic, $1)='-DDLL_EXPORT']) ;; hpux9* | hpux10* | hpux11*) _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' # PIC is the default for IA64 HP-UX and 64-bit HP-UX, but # not for PA HP-UX. case $host_cpu in hppa*64*|ia64*) # +Z the default ;; *) _LT_TAGVAR(lt_prog_compiler_pic, $1)='+Z' ;; esac # Is there a better lt_prog_compiler_static that works with the bundled CC? _LT_TAGVAR(lt_prog_compiler_static, $1)='${wl}-a ${wl}archive' ;; irix5* | irix6* | nonstopux*) _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' # PIC (with -KPIC) is the default. _LT_TAGVAR(lt_prog_compiler_static, $1)='-non_shared' ;; linux* | k*bsd*-gnu | kopensolaris*-gnu) case $cc_basename in # old Intel for x86_64 which still supported -KPIC. ecc*) _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' _LT_TAGVAR(lt_prog_compiler_pic, $1)='-KPIC' _LT_TAGVAR(lt_prog_compiler_static, $1)='-static' ;; # icc used to be incompatible with GCC. # ICC 10 doesn't accept -KPIC any more. icc* | ifort*) _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' _LT_TAGVAR(lt_prog_compiler_pic, $1)='-fPIC' _LT_TAGVAR(lt_prog_compiler_static, $1)='-static' ;; # Lahey Fortran 8.1. lf95*) _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' _LT_TAGVAR(lt_prog_compiler_pic, $1)='--shared' _LT_TAGVAR(lt_prog_compiler_static, $1)='--static' ;; nagfor*) # NAG Fortran compiler _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,-Wl,,' _LT_TAGVAR(lt_prog_compiler_pic, $1)='-PIC' _LT_TAGVAR(lt_prog_compiler_static, $1)='-Bstatic' ;; pgcc* | pgf77* | pgf90* | pgf95* | pgfortran*) # Portland Group compilers (*not* the Pentium gcc compiler, # which looks to be a dead project) _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' _LT_TAGVAR(lt_prog_compiler_pic, $1)='-fpic' _LT_TAGVAR(lt_prog_compiler_static, $1)='-Bstatic' ;; ccc*) _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' # All Alpha code is PIC. _LT_TAGVAR(lt_prog_compiler_static, $1)='-non_shared' ;; xl* | bgxl* | bgf* | mpixl*) # IBM XL C 8.0/Fortran 10.1, 11.1 on PPC and BlueGene _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' _LT_TAGVAR(lt_prog_compiler_pic, $1)='-qpic' _LT_TAGVAR(lt_prog_compiler_static, $1)='-qstaticlink' ;; *) case `$CC -V 2>&1 | sed 5q` in *Sun\ Ceres\ Fortran* | *Sun*Fortran*\ [[1-7]].* | *Sun*Fortran*\ 8.[[0-3]]*) # Sun Fortran 8.3 passes all unrecognized flags to the linker _LT_TAGVAR(lt_prog_compiler_pic, $1)='-KPIC' _LT_TAGVAR(lt_prog_compiler_static, $1)='-Bstatic' _LT_TAGVAR(lt_prog_compiler_wl, $1)='' ;; *Sun\ F* | *Sun*Fortran*) _LT_TAGVAR(lt_prog_compiler_pic, $1)='-KPIC' _LT_TAGVAR(lt_prog_compiler_static, $1)='-Bstatic' _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Qoption ld ' ;; *Sun\ C*) # Sun C 5.9 _LT_TAGVAR(lt_prog_compiler_pic, $1)='-KPIC' _LT_TAGVAR(lt_prog_compiler_static, $1)='-Bstatic' _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' ;; *Intel*\ [[CF]]*Compiler*) _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' _LT_TAGVAR(lt_prog_compiler_pic, $1)='-fPIC' _LT_TAGVAR(lt_prog_compiler_static, $1)='-static' ;; *Portland\ Group*) _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' _LT_TAGVAR(lt_prog_compiler_pic, $1)='-fpic' _LT_TAGVAR(lt_prog_compiler_static, $1)='-Bstatic' ;; esac ;; esac ;; newsos6) _LT_TAGVAR(lt_prog_compiler_pic, $1)='-KPIC' _LT_TAGVAR(lt_prog_compiler_static, $1)='-Bstatic' ;; *nto* | *qnx*) # QNX uses GNU C++, but need to define -shared option too, otherwise # it will coredump. _LT_TAGVAR(lt_prog_compiler_pic, $1)='-fPIC -shared' ;; osf3* | osf4* | osf5*) _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' # All OSF/1 code is PIC. _LT_TAGVAR(lt_prog_compiler_static, $1)='-non_shared' ;; rdos*) _LT_TAGVAR(lt_prog_compiler_static, $1)='-non_shared' ;; solaris*) _LT_TAGVAR(lt_prog_compiler_pic, $1)='-KPIC' _LT_TAGVAR(lt_prog_compiler_static, $1)='-Bstatic' case $cc_basename in f77* | f90* | f95* | sunf77* | sunf90* | sunf95*) _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Qoption ld ';; *) _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,';; esac ;; sunos4*) _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Qoption ld ' _LT_TAGVAR(lt_prog_compiler_pic, $1)='-PIC' _LT_TAGVAR(lt_prog_compiler_static, $1)='-Bstatic' ;; sysv4 | sysv4.2uw2* | sysv4.3*) _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' _LT_TAGVAR(lt_prog_compiler_pic, $1)='-KPIC' _LT_TAGVAR(lt_prog_compiler_static, $1)='-Bstatic' ;; sysv4*MP*) if test -d /usr/nec ;then _LT_TAGVAR(lt_prog_compiler_pic, $1)='-Kconform_pic' _LT_TAGVAR(lt_prog_compiler_static, $1)='-Bstatic' fi ;; sysv5* | unixware* | sco3.2v5* | sco5v6* | OpenUNIX*) _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' _LT_TAGVAR(lt_prog_compiler_pic, $1)='-KPIC' _LT_TAGVAR(lt_prog_compiler_static, $1)='-Bstatic' ;; unicos*) _LT_TAGVAR(lt_prog_compiler_wl, $1)='-Wl,' _LT_TAGVAR(lt_prog_compiler_can_build_shared, $1)=no ;; uts4*) _LT_TAGVAR(lt_prog_compiler_pic, $1)='-pic' _LT_TAGVAR(lt_prog_compiler_static, $1)='-Bstatic' ;; *) _LT_TAGVAR(lt_prog_compiler_can_build_shared, $1)=no ;; esac fi ]) case $host_os in # For platforms which do not support PIC, -DPIC is meaningless: *djgpp*) _LT_TAGVAR(lt_prog_compiler_pic, $1)= ;; *) _LT_TAGVAR(lt_prog_compiler_pic, $1)="$_LT_TAGVAR(lt_prog_compiler_pic, $1)@&t@m4_if([$1],[],[ -DPIC],[m4_if([$1],[CXX],[ -DPIC],[])])" ;; esac AC_CACHE_CHECK([for $compiler option to produce PIC], [_LT_TAGVAR(lt_cv_prog_compiler_pic, $1)], [_LT_TAGVAR(lt_cv_prog_compiler_pic, $1)=$_LT_TAGVAR(lt_prog_compiler_pic, $1)]) _LT_TAGVAR(lt_prog_compiler_pic, $1)=$_LT_TAGVAR(lt_cv_prog_compiler_pic, $1) # # Check to make sure the PIC flag actually works. # if test -n "$_LT_TAGVAR(lt_prog_compiler_pic, $1)"; then _LT_COMPILER_OPTION([if $compiler PIC flag $_LT_TAGVAR(lt_prog_compiler_pic, $1) works], [_LT_TAGVAR(lt_cv_prog_compiler_pic_works, $1)], [$_LT_TAGVAR(lt_prog_compiler_pic, $1)@&t@m4_if([$1],[],[ -DPIC],[m4_if([$1],[CXX],[ -DPIC],[])])], [], [case $_LT_TAGVAR(lt_prog_compiler_pic, $1) in "" | " "*) ;; *) _LT_TAGVAR(lt_prog_compiler_pic, $1)=" $_LT_TAGVAR(lt_prog_compiler_pic, $1)" ;; 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osf4* | osf5*) # as osf3* with the addition of -msym flag if test "$GCC" = yes; then _LT_TAGVAR(allow_undefined_flag, $1)=' ${wl}-expect_unresolved ${wl}\*' _LT_TAGVAR(archive_cmds, $1)='$CC -shared${allow_undefined_flag} $pic_flag $libobjs $deplibs $compiler_flags ${wl}-msym ${wl}-soname ${wl}$soname `test -n "$verstring" && func_echo_all "${wl}-set_version ${wl}$verstring"` ${wl}-update_registry ${wl}${output_objdir}/so_locations -o $lib' _LT_TAGVAR(hardcode_libdir_flag_spec, $1)='${wl}-rpath ${wl}$libdir' else _LT_TAGVAR(allow_undefined_flag, $1)=' -expect_unresolved \*' _LT_TAGVAR(archive_cmds, $1)='$CC -shared${allow_undefined_flag} $libobjs $deplibs $compiler_flags -msym -soname $soname `test -n "$verstring" && func_echo_all "-set_version $verstring"` -update_registry ${output_objdir}/so_locations -o $lib' _LT_TAGVAR(archive_expsym_cmds, $1)='for i in `cat $export_symbols`; do printf "%s %s\\n" -exported_symbol "\$i" >> $lib.exp; done; printf "%s\\n" "-hidden">> $lib.exp~ $CC -shared${allow_undefined_flag} ${wl}-input ${wl}$lib.exp $compiler_flags $libobjs $deplibs -soname $soname `test -n "$verstring" && $ECHO "-set_version $verstring"` -update_registry ${output_objdir}/so_locations -o $lib~$RM $lib.exp' # Both c and cxx compiler support -rpath directly _LT_TAGVAR(hardcode_libdir_flag_spec, $1)='-rpath $libdir' fi _LT_TAGVAR(archive_cmds_need_lc, $1)='no' _LT_TAGVAR(hardcode_libdir_separator, $1)=: ;; solaris*) _LT_TAGVAR(no_undefined_flag, $1)=' -z defs' if test "$GCC" = yes; then wlarc='${wl}' _LT_TAGVAR(archive_cmds, $1)='$CC -shared $pic_flag ${wl}-z ${wl}text ${wl}-h ${wl}$soname -o $lib $libobjs $deplibs $compiler_flags' _LT_TAGVAR(archive_expsym_cmds, $1)='echo "{ global:" > $lib.exp~cat $export_symbols | $SED -e "s/\(.*\)/\1;/" >> $lib.exp~echo "local: *; };" >> $lib.exp~ $CC -shared $pic_flag ${wl}-z ${wl}text ${wl}-M ${wl}$lib.exp ${wl}-h ${wl}$soname -o $lib $libobjs $deplibs $compiler_flags~$RM $lib.exp' else case `$CC -V 2>&1` in *"Compilers 5.0"*) wlarc='' _LT_TAGVAR(archive_cmds, $1)='$LD -G${allow_undefined_flag} -h $soname -o $lib $libobjs $deplibs $linker_flags' _LT_TAGVAR(archive_expsym_cmds, $1)='echo "{ global:" > $lib.exp~cat $export_symbols | $SED -e "s/\(.*\)/\1;/" >> $lib.exp~echo "local: *; };" >> $lib.exp~ $LD -G${allow_undefined_flag} -M $lib.exp -h $soname -o $lib $libobjs $deplibs $linker_flags~$RM $lib.exp' ;; *) wlarc='${wl}' _LT_TAGVAR(archive_cmds, $1)='$CC -G${allow_undefined_flag} -h $soname -o $lib $libobjs $deplibs $compiler_flags' _LT_TAGVAR(archive_expsym_cmds, $1)='echo "{ global:" > $lib.exp~cat $export_symbols | $SED -e "s/\(.*\)/\1;/" >> $lib.exp~echo "local: *; };" >> $lib.exp~ $CC -G${allow_undefined_flag} -M $lib.exp -h $soname -o $lib $libobjs $deplibs $compiler_flags~$RM $lib.exp' ;; esac fi _LT_TAGVAR(hardcode_libdir_flag_spec, $1)='-R$libdir' _LT_TAGVAR(hardcode_shlibpath_var, $1)=no case $host_os in solaris2.[[0-5]] | solaris2.[[0-5]].*) ;; *) # The compiler driver will combine and reorder linker options, # but understands `-z linker_flag'. GCC discards it without `$wl', # but is careful enough not to reorder. # Supported since Solaris 2.6 (maybe 2.5.1?) if test "$GCC" = yes; then _LT_TAGVAR(whole_archive_flag_spec, $1)='${wl}-z ${wl}allextract$convenience ${wl}-z ${wl}defaultextract' else _LT_TAGVAR(whole_archive_flag_spec, $1)='-z allextract$convenience -z defaultextract' fi ;; esac _LT_TAGVAR(link_all_deplibs, $1)=yes ;; sunos4*) if test "x$host_vendor" = xsequent; then # Use $CC to link under sequent, because it throws in some extra .o # files that make .init and .fini sections work. _LT_TAGVAR(archive_cmds, $1)='$CC -G ${wl}-h $soname -o $lib $libobjs $deplibs $compiler_flags' else _LT_TAGVAR(archive_cmds, $1)='$LD -assert pure-text -Bstatic -o $lib $libobjs $deplibs $linker_flags' fi _LT_TAGVAR(hardcode_libdir_flag_spec, $1)='-L$libdir' _LT_TAGVAR(hardcode_direct, $1)=yes _LT_TAGVAR(hardcode_minus_L, $1)=yes _LT_TAGVAR(hardcode_shlibpath_var, $1)=no ;; sysv4) case $host_vendor in sni) _LT_TAGVAR(archive_cmds, $1)='$LD -G -h $soname -o $lib $libobjs $deplibs $linker_flags' _LT_TAGVAR(hardcode_direct, $1)=yes # is this really true??? ;; siemens) ## LD is ld it makes a PLAMLIB ## CC just makes a GrossModule. _LT_TAGVAR(archive_cmds, $1)='$LD -G -o $lib $libobjs $deplibs $linker_flags' _LT_TAGVAR(reload_cmds, $1)='$CC -r -o $output$reload_objs' _LT_TAGVAR(hardcode_direct, $1)=no ;; motorola) _LT_TAGVAR(archive_cmds, $1)='$LD -G -h $soname -o $lib $libobjs $deplibs $linker_flags' _LT_TAGVAR(hardcode_direct, $1)=no #Motorola manual says yes, but my tests say they lie ;; esac runpath_var='LD_RUN_PATH' _LT_TAGVAR(hardcode_shlibpath_var, $1)=no ;; sysv4.3*) _LT_TAGVAR(archive_cmds, $1)='$LD -G -h $soname -o $lib $libobjs $deplibs $linker_flags' _LT_TAGVAR(hardcode_shlibpath_var, $1)=no _LT_TAGVAR(export_dynamic_flag_spec, $1)='-Bexport' ;; sysv4*MP*) if test -d /usr/nec; then _LT_TAGVAR(archive_cmds, $1)='$LD -G -h $soname -o $lib $libobjs $deplibs $linker_flags' _LT_TAGVAR(hardcode_shlibpath_var, $1)=no runpath_var=LD_RUN_PATH hardcode_runpath_var=yes _LT_TAGVAR(ld_shlibs, $1)=yes fi ;; sysv4*uw2* | sysv5OpenUNIX* | sysv5UnixWare7.[[01]].[[10]]* | unixware7* | sco3.2v5.0.[[024]]*) _LT_TAGVAR(no_undefined_flag, $1)='${wl}-z,text' _LT_TAGVAR(archive_cmds_need_lc, $1)=no _LT_TAGVAR(hardcode_shlibpath_var, $1)=no runpath_var='LD_RUN_PATH' if test "$GCC" = yes; then _LT_TAGVAR(archive_cmds, $1)='$CC -shared ${wl}-h,$soname -o $lib $libobjs $deplibs $compiler_flags' _LT_TAGVAR(archive_expsym_cmds, $1)='$CC -shared ${wl}-Bexport:$export_symbols ${wl}-h,$soname -o $lib $libobjs $deplibs $compiler_flags' else _LT_TAGVAR(archive_cmds, $1)='$CC -G ${wl}-h,$soname -o $lib $libobjs $deplibs $compiler_flags' _LT_TAGVAR(archive_expsym_cmds, $1)='$CC -G ${wl}-Bexport:$export_symbols ${wl}-h,$soname -o $lib $libobjs $deplibs $compiler_flags' fi ;; sysv5* | sco3.2v5* | sco5v6*) # Note: We can NOT use -z defs as we might desire, because we do not # link with -lc, and that would cause any symbols used from libc to # always be unresolved, which means just about no library would # ever link correctly. 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(KAI) C++ Compiler # KCC will only create a shared library if the output file # ends with ".so" (or ".sl" for HP-UX), so rename the library # to its proper name (with version) after linking. _LT_TAGVAR(archive_cmds, $1)='tempext=`echo $shared_ext | $SED -e '\''s/\([[^()0-9A-Za-z{}]]\)/\\\\\1/g'\''`; templib=`echo $lib | $SED -e "s/\${tempext}\..*/.so/"`; $CC $predep_objects $libobjs $deplibs $postdep_objects $compiler_flags --soname $soname -o \$templib; mv \$templib $lib' _LT_TAGVAR(archive_expsym_cmds, $1)='tempext=`echo $shared_ext | $SED -e '\''s/\([[^()0-9A-Za-z{}]]\)/\\\\\1/g'\''`; templib=`echo $lib | $SED -e "s/\${tempext}\..*/.so/"`; $CC $predep_objects $libobjs $deplibs $postdep_objects $compiler_flags --soname $soname -o \$templib ${wl}-retain-symbols-file,$export_symbols; mv \$templib $lib' # Commands to make compiler produce verbose output that lists # what "hidden" libraries, object files and flags are used when # linking a shared library. # # There doesn't appear to be a way to prevent this compiler from # explicitly linking system object files so we need to strip them # from the output so that they don't get included in the library # dependencies. output_verbose_link_cmd='templist=`$CC $CFLAGS -v conftest.$objext -o libconftest$shared_ext 2>&1 | $GREP "ld"`; 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These are needed # for certain cross-compile configurations and native mingw. m4_defun([_LT_PATH_CONVERSION_FUNCTIONS], [AC_REQUIRE([AC_CANONICAL_HOST])dnl AC_REQUIRE([AC_CANONICAL_BUILD])dnl AC_MSG_CHECKING([how to convert $build file names to $host format]) AC_CACHE_VAL(lt_cv_to_host_file_cmd, [case $host in *-*-mingw* ) case $build in *-*-mingw* ) # actually msys lt_cv_to_host_file_cmd=func_convert_file_msys_to_w32 ;; *-*-cygwin* ) lt_cv_to_host_file_cmd=func_convert_file_cygwin_to_w32 ;; * ) # otherwise, assume *nix lt_cv_to_host_file_cmd=func_convert_file_nix_to_w32 ;; esac ;; *-*-cygwin* ) case $build in *-*-mingw* ) # actually msys lt_cv_to_host_file_cmd=func_convert_file_msys_to_cygwin ;; *-*-cygwin* ) lt_cv_to_host_file_cmd=func_convert_file_noop ;; * ) # otherwise, assume *nix lt_cv_to_host_file_cmd=func_convert_file_nix_to_cygwin ;; esac ;; * ) # unhandled hosts (and "normal" native builds) lt_cv_to_host_file_cmd=func_convert_file_noop ;; esac ]) to_host_file_cmd=$lt_cv_to_host_file_cmd AC_MSG_RESULT([$lt_cv_to_host_file_cmd]) _LT_DECL([to_host_file_cmd], [lt_cv_to_host_file_cmd], [0], [convert $build file names to $host format])dnl AC_MSG_CHECKING([how to convert $build file names to toolchain format]) AC_CACHE_VAL(lt_cv_to_tool_file_cmd, [#assume ordinary cross tools, or native build. lt_cv_to_tool_file_cmd=func_convert_file_noop case $host in *-*-mingw* ) case $build in *-*-mingw* ) # actually msys lt_cv_to_tool_file_cmd=func_convert_file_msys_to_w32 ;; esac ;; esac ]) to_tool_file_cmd=$lt_cv_to_tool_file_cmd AC_MSG_RESULT([$lt_cv_to_tool_file_cmd]) _LT_DECL([to_tool_file_cmd], [lt_cv_to_tool_file_cmd], [0], [convert $build files to toolchain format])dnl ])# _LT_PATH_CONVERSION_FUNCTIONS # Helper functions for option handling. -*- Autoconf -*- # # Copyright (C) 2004, 2005, 2007, 2008, 2009 Free Software Foundation, # Inc. # Written by Gary V. Vaughan, 2004 # # This file is free software; the Free Software Foundation gives # unlimited permission to copy and/or distribute it, with or without # modifications, as long as this notice is preserved. # serial 7 ltoptions.m4 # This is to help aclocal find these macros, as it can't see m4_define. AC_DEFUN([LTOPTIONS_VERSION], [m4_if([1])]) # _LT_MANGLE_OPTION(MACRO-NAME, OPTION-NAME) # ------------------------------------------ m4_define([_LT_MANGLE_OPTION], [[_LT_OPTION_]m4_bpatsubst($1__$2, [[^a-zA-Z0-9_]], [_])]) # _LT_SET_OPTION(MACRO-NAME, OPTION-NAME) # --------------------------------------- # Set option OPTION-NAME for macro MACRO-NAME, and if there is a # matching handler defined, dispatch to it. Other OPTION-NAMEs are # saved as a flag. m4_define([_LT_SET_OPTION], [m4_define(_LT_MANGLE_OPTION([$1], [$2]))dnl m4_ifdef(_LT_MANGLE_DEFUN([$1], [$2]), _LT_MANGLE_DEFUN([$1], [$2]), [m4_warning([Unknown $1 option `$2'])])[]dnl ]) # _LT_IF_OPTION(MACRO-NAME, OPTION-NAME, IF-SET, [IF-NOT-SET]) # ------------------------------------------------------------ # Execute IF-SET if OPTION is set, IF-NOT-SET otherwise. m4_define([_LT_IF_OPTION], [m4_ifdef(_LT_MANGLE_OPTION([$1], [$2]), [$3], [$4])]) # _LT_UNLESS_OPTIONS(MACRO-NAME, OPTION-LIST, IF-NOT-SET) # ------------------------------------------------------- # Execute IF-NOT-SET unless all options in OPTION-LIST for MACRO-NAME # are set. m4_define([_LT_UNLESS_OPTIONS], [m4_foreach([_LT_Option], m4_split(m4_normalize([$2])), [m4_ifdef(_LT_MANGLE_OPTION([$1], _LT_Option), [m4_define([$0_found])])])[]dnl m4_ifdef([$0_found], [m4_undefine([$0_found])], [$3 ])[]dnl ]) # _LT_SET_OPTIONS(MACRO-NAME, OPTION-LIST) # ---------------------------------------- # OPTION-LIST is a space-separated list of Libtool options associated # with MACRO-NAME. If any OPTION has a matching handler declared with # LT_OPTION_DEFINE, dispatch to that macro; otherwise complain about # the unknown option and exit. m4_defun([_LT_SET_OPTIONS], [# Set options m4_foreach([_LT_Option], m4_split(m4_normalize([$2])), [_LT_SET_OPTION([$1], _LT_Option)]) m4_if([$1],[LT_INIT],[ dnl dnl Simply set some default values (i.e off) if boolean options were not dnl specified: _LT_UNLESS_OPTIONS([LT_INIT], [dlopen], [enable_dlopen=no ]) _LT_UNLESS_OPTIONS([LT_INIT], [win32-dll], [enable_win32_dll=no ]) dnl dnl If no reference was made to various pairs of opposing options, then dnl we run the default mode handler for the pair. For example, if neither dnl `shared' nor `disable-shared' was passed, we enable building of shared dnl archives by default: _LT_UNLESS_OPTIONS([LT_INIT], [shared disable-shared], [_LT_ENABLE_SHARED]) _LT_UNLESS_OPTIONS([LT_INIT], [static disable-static], [_LT_ENABLE_STATIC]) _LT_UNLESS_OPTIONS([LT_INIT], [pic-only no-pic], [_LT_WITH_PIC]) _LT_UNLESS_OPTIONS([LT_INIT], [fast-install disable-fast-install], [_LT_ENABLE_FAST_INSTALL]) ]) ])# _LT_SET_OPTIONS # _LT_MANGLE_DEFUN(MACRO-NAME, OPTION-NAME) # ----------------------------------------- m4_define([_LT_MANGLE_DEFUN], [[_LT_OPTION_DEFUN_]m4_bpatsubst(m4_toupper([$1__$2]), [[^A-Z0-9_]], [_])]) # LT_OPTION_DEFINE(MACRO-NAME, OPTION-NAME, CODE) # ----------------------------------------------- m4_define([LT_OPTION_DEFINE], [m4_define(_LT_MANGLE_DEFUN([$1], [$2]), [$3])[]dnl ])# LT_OPTION_DEFINE # dlopen # ------ LT_OPTION_DEFINE([LT_INIT], [dlopen], [enable_dlopen=yes ]) AU_DEFUN([AC_LIBTOOL_DLOPEN], [_LT_SET_OPTION([LT_INIT], [dlopen]) AC_DIAGNOSE([obsolete], [$0: Remove this warning and the call to _LT_SET_OPTION when you put the `dlopen' option into LT_INIT's first parameter.]) ]) dnl aclocal-1.4 backwards compatibility: dnl AC_DEFUN([AC_LIBTOOL_DLOPEN], []) # win32-dll # --------- # Declare package support for building win32 dll's. LT_OPTION_DEFINE([LT_INIT], [win32-dll], [enable_win32_dll=yes case $host in *-*-cygwin* | *-*-mingw* | *-*-pw32* | *-*-cegcc*) AC_CHECK_TOOL(AS, as, false) AC_CHECK_TOOL(DLLTOOL, dlltool, false) AC_CHECK_TOOL(OBJDUMP, objdump, false) ;; esac test -z "$AS" && AS=as _LT_DECL([], [AS], [1], [Assembler program])dnl test -z "$DLLTOOL" && DLLTOOL=dlltool _LT_DECL([], [DLLTOOL], [1], [DLL creation program])dnl test -z "$OBJDUMP" && OBJDUMP=objdump _LT_DECL([], [OBJDUMP], [1], [Object dumper program])dnl ])# win32-dll AU_DEFUN([AC_LIBTOOL_WIN32_DLL], [AC_REQUIRE([AC_CANONICAL_HOST])dnl _LT_SET_OPTION([LT_INIT], [win32-dll]) AC_DIAGNOSE([obsolete], [$0: Remove this warning and the call to _LT_SET_OPTION when you put the `win32-dll' option into LT_INIT's first parameter.]) ]) dnl aclocal-1.4 backwards compatibility: dnl AC_DEFUN([AC_LIBTOOL_WIN32_DLL], []) # _LT_ENABLE_SHARED([DEFAULT]) # ---------------------------- # implement the --enable-shared flag, and supports the `shared' and # `disable-shared' LT_INIT options. # DEFAULT is either `yes' or `no'. If omitted, it defaults to `yes'. m4_define([_LT_ENABLE_SHARED], [m4_define([_LT_ENABLE_SHARED_DEFAULT], [m4_if($1, no, no, yes)])dnl AC_ARG_ENABLE([shared], [AS_HELP_STRING([--enable-shared@<:@=PKGS@:>@], [build shared libraries @<:@default=]_LT_ENABLE_SHARED_DEFAULT[@:>@])], [p=${PACKAGE-default} case $enableval in yes) enable_shared=yes ;; no) enable_shared=no ;; *) enable_shared=no # Look at the argument we got. We use all the common list separators. lt_save_ifs="$IFS"; IFS="${IFS}$PATH_SEPARATOR," for pkg in $enableval; do IFS="$lt_save_ifs" if test "X$pkg" = "X$p"; then enable_shared=yes fi done IFS="$lt_save_ifs" ;; esac], [enable_shared=]_LT_ENABLE_SHARED_DEFAULT) _LT_DECL([build_libtool_libs], [enable_shared], [0], [Whether or not to build shared libraries]) ])# _LT_ENABLE_SHARED LT_OPTION_DEFINE([LT_INIT], [shared], [_LT_ENABLE_SHARED([yes])]) LT_OPTION_DEFINE([LT_INIT], [disable-shared], [_LT_ENABLE_SHARED([no])]) # Old names: AC_DEFUN([AC_ENABLE_SHARED], [_LT_SET_OPTION([LT_INIT], m4_if([$1], [no], [disable-])[shared]) ]) AC_DEFUN([AC_DISABLE_SHARED], [_LT_SET_OPTION([LT_INIT], [disable-shared]) ]) AU_DEFUN([AM_ENABLE_SHARED], [AC_ENABLE_SHARED($@)]) AU_DEFUN([AM_DISABLE_SHARED], [AC_DISABLE_SHARED($@)]) dnl aclocal-1.4 backwards compatibility: dnl AC_DEFUN([AM_ENABLE_SHARED], []) dnl AC_DEFUN([AM_DISABLE_SHARED], []) # _LT_ENABLE_STATIC([DEFAULT]) # ---------------------------- # implement the --enable-static flag, and support the `static' and # `disable-static' LT_INIT options. # DEFAULT is either `yes' or `no'. If omitted, it defaults to `yes'. m4_define([_LT_ENABLE_STATIC], [m4_define([_LT_ENABLE_STATIC_DEFAULT], [m4_if($1, no, no, yes)])dnl AC_ARG_ENABLE([static], [AS_HELP_STRING([--enable-static@<:@=PKGS@:>@], [build static libraries @<:@default=]_LT_ENABLE_STATIC_DEFAULT[@:>@])], [p=${PACKAGE-default} case $enableval in yes) enable_static=yes ;; no) enable_static=no ;; *) enable_static=no # Look at the argument we got. We use all the common list separators. lt_save_ifs="$IFS"; IFS="${IFS}$PATH_SEPARATOR," for pkg in $enableval; do IFS="$lt_save_ifs" if test "X$pkg" = "X$p"; then enable_static=yes fi done IFS="$lt_save_ifs" ;; esac], [enable_static=]_LT_ENABLE_STATIC_DEFAULT) _LT_DECL([build_old_libs], [enable_static], [0], [Whether or not to build static libraries]) ])# _LT_ENABLE_STATIC LT_OPTION_DEFINE([LT_INIT], [static], [_LT_ENABLE_STATIC([yes])]) LT_OPTION_DEFINE([LT_INIT], [disable-static], [_LT_ENABLE_STATIC([no])]) # Old names: AC_DEFUN([AC_ENABLE_STATIC], [_LT_SET_OPTION([LT_INIT], m4_if([$1], [no], [disable-])[static]) ]) AC_DEFUN([AC_DISABLE_STATIC], [_LT_SET_OPTION([LT_INIT], [disable-static]) ]) AU_DEFUN([AM_ENABLE_STATIC], [AC_ENABLE_STATIC($@)]) AU_DEFUN([AM_DISABLE_STATIC], [AC_DISABLE_STATIC($@)]) dnl aclocal-1.4 backwards compatibility: dnl AC_DEFUN([AM_ENABLE_STATIC], []) dnl AC_DEFUN([AM_DISABLE_STATIC], []) # _LT_ENABLE_FAST_INSTALL([DEFAULT]) # ---------------------------------- # implement the --enable-fast-install flag, and support the `fast-install' # and `disable-fast-install' LT_INIT options. # DEFAULT is either `yes' or `no'. If omitted, it defaults to `yes'. m4_define([_LT_ENABLE_FAST_INSTALL], [m4_define([_LT_ENABLE_FAST_INSTALL_DEFAULT], [m4_if($1, no, no, yes)])dnl AC_ARG_ENABLE([fast-install], [AS_HELP_STRING([--enable-fast-install@<:@=PKGS@:>@], [optimize for fast installation @<:@default=]_LT_ENABLE_FAST_INSTALL_DEFAULT[@:>@])], [p=${PACKAGE-default} case $enableval in yes) enable_fast_install=yes ;; no) enable_fast_install=no ;; *) enable_fast_install=no # Look at the argument we got. We use all the common list separators. lt_save_ifs="$IFS"; IFS="${IFS}$PATH_SEPARATOR," for pkg in $enableval; do IFS="$lt_save_ifs" if test "X$pkg" = "X$p"; then enable_fast_install=yes fi done IFS="$lt_save_ifs" ;; esac], [enable_fast_install=]_LT_ENABLE_FAST_INSTALL_DEFAULT) _LT_DECL([fast_install], [enable_fast_install], [0], [Whether or not to optimize for fast installation])dnl ])# _LT_ENABLE_FAST_INSTALL LT_OPTION_DEFINE([LT_INIT], [fast-install], [_LT_ENABLE_FAST_INSTALL([yes])]) LT_OPTION_DEFINE([LT_INIT], [disable-fast-install], [_LT_ENABLE_FAST_INSTALL([no])]) # Old names: AU_DEFUN([AC_ENABLE_FAST_INSTALL], [_LT_SET_OPTION([LT_INIT], m4_if([$1], [no], [disable-])[fast-install]) AC_DIAGNOSE([obsolete], [$0: Remove this warning and the call to _LT_SET_OPTION when you put the `fast-install' option into LT_INIT's first parameter.]) ]) AU_DEFUN([AC_DISABLE_FAST_INSTALL], [_LT_SET_OPTION([LT_INIT], [disable-fast-install]) AC_DIAGNOSE([obsolete], [$0: Remove this warning and the call to _LT_SET_OPTION when you put the `disable-fast-install' option into LT_INIT's first parameter.]) ]) dnl aclocal-1.4 backwards compatibility: dnl AC_DEFUN([AC_ENABLE_FAST_INSTALL], []) dnl AC_DEFUN([AM_DISABLE_FAST_INSTALL], []) # _LT_WITH_PIC([MODE]) # -------------------- # implement the --with-pic flag, and support the `pic-only' and `no-pic' # LT_INIT options. # MODE is either `yes' or `no'. If omitted, it defaults to `both'. m4_define([_LT_WITH_PIC], [AC_ARG_WITH([pic], [AS_HELP_STRING([--with-pic@<:@=PKGS@:>@], [try to use only PIC/non-PIC objects @<:@default=use both@:>@])], [lt_p=${PACKAGE-default} case $withval in yes|no) pic_mode=$withval ;; *) pic_mode=default # Look at the argument we got. We use all the common list separators. lt_save_ifs="$IFS"; IFS="${IFS}$PATH_SEPARATOR," for lt_pkg in $withval; do IFS="$lt_save_ifs" if test "X$lt_pkg" = "X$lt_p"; then pic_mode=yes fi done IFS="$lt_save_ifs" ;; esac], [pic_mode=default]) test -z "$pic_mode" && pic_mode=m4_default([$1], [default]) _LT_DECL([], [pic_mode], [0], [What type of objects to build])dnl ])# _LT_WITH_PIC LT_OPTION_DEFINE([LT_INIT], [pic-only], [_LT_WITH_PIC([yes])]) LT_OPTION_DEFINE([LT_INIT], [no-pic], [_LT_WITH_PIC([no])]) # Old name: AU_DEFUN([AC_LIBTOOL_PICMODE], [_LT_SET_OPTION([LT_INIT], [pic-only]) AC_DIAGNOSE([obsolete], [$0: Remove this warning and the call to _LT_SET_OPTION when you put the `pic-only' option into LT_INIT's first parameter.]) ]) dnl aclocal-1.4 backwards compatibility: dnl AC_DEFUN([AC_LIBTOOL_PICMODE], []) m4_define([_LTDL_MODE], []) LT_OPTION_DEFINE([LTDL_INIT], [nonrecursive], [m4_define([_LTDL_MODE], [nonrecursive])]) LT_OPTION_DEFINE([LTDL_INIT], [recursive], [m4_define([_LTDL_MODE], [recursive])]) LT_OPTION_DEFINE([LTDL_INIT], [subproject], [m4_define([_LTDL_MODE], [subproject])]) m4_define([_LTDL_TYPE], []) LT_OPTION_DEFINE([LTDL_INIT], [installable], [m4_define([_LTDL_TYPE], [installable])]) LT_OPTION_DEFINE([LTDL_INIT], [convenience], [m4_define([_LTDL_TYPE], [convenience])]) # ltsugar.m4 -- libtool m4 base layer. -*-Autoconf-*- # # Copyright (C) 2004, 2005, 2007, 2008 Free Software Foundation, Inc. # Written by Gary V. Vaughan, 2004 # # This file is free software; the Free Software Foundation gives # unlimited permission to copy and/or distribute it, with or without # modifications, as long as this notice is preserved. # serial 6 ltsugar.m4 # This is to help aclocal find these macros, as it can't see m4_define. AC_DEFUN([LTSUGAR_VERSION], [m4_if([0.1])]) # lt_join(SEP, ARG1, [ARG2...]) # ----------------------------- # Produce ARG1SEPARG2...SEPARGn, omitting [] arguments and their # associated separator. # Needed until we can rely on m4_join from Autoconf 2.62, since all earlier # versions in m4sugar had bugs. m4_define([lt_join], [m4_if([$#], [1], [], [$#], [2], [[$2]], [m4_if([$2], [], [], [[$2]_])$0([$1], m4_shift(m4_shift($@)))])]) m4_define([_lt_join], [m4_if([$#$2], [2], [], [m4_if([$2], [], [], [[$1$2]])$0([$1], m4_shift(m4_shift($@)))])]) # lt_car(LIST) # lt_cdr(LIST) # ------------ # Manipulate m4 lists. # These macros are necessary as long as will still need to support # Autoconf-2.59 which quotes differently. m4_define([lt_car], [[$1]]) m4_define([lt_cdr], [m4_if([$#], 0, [m4_fatal([$0: cannot be called without arguments])], [$#], 1, [], [m4_dquote(m4_shift($@))])]) m4_define([lt_unquote], $1) # lt_append(MACRO-NAME, STRING, [SEPARATOR]) # ------------------------------------------ # Redefine MACRO-NAME to hold its former content plus `SEPARATOR'`STRING'. # Note that neither SEPARATOR nor STRING are expanded; they are appended # to MACRO-NAME as is (leaving the expansion for when MACRO-NAME is invoked). # No SEPARATOR is output if MACRO-NAME was previously undefined (different # than defined and empty). # # This macro is needed until we can rely on Autoconf 2.62, since earlier # versions of m4sugar mistakenly expanded SEPARATOR but not STRING. m4_define([lt_append], [m4_define([$1], m4_ifdef([$1], [m4_defn([$1])[$3]])[$2])]) # lt_combine(SEP, PREFIX-LIST, INFIX, SUFFIX1, [SUFFIX2...]) # ---------------------------------------------------------- # Produce a SEP delimited list of all paired combinations of elements of # PREFIX-LIST with SUFFIX1 through SUFFIXn. Each element of the list # has the form PREFIXmINFIXSUFFIXn. # Needed until we can rely on m4_combine added in Autoconf 2.62. m4_define([lt_combine], [m4_if(m4_eval([$# > 3]), [1], [m4_pushdef([_Lt_sep], [m4_define([_Lt_sep], m4_defn([lt_car]))])]]dnl [[m4_foreach([_Lt_prefix], [$2], [m4_foreach([_Lt_suffix], ]m4_dquote(m4_dquote(m4_shift(m4_shift(m4_shift($@)))))[, [_Lt_sep([$1])[]m4_defn([_Lt_prefix])[$3]m4_defn([_Lt_suffix])])])])]) # lt_if_append_uniq(MACRO-NAME, VARNAME, [SEPARATOR], [UNIQ], [NOT-UNIQ]) # ----------------------------------------------------------------------- # Iff MACRO-NAME does not yet contain VARNAME, then append it (delimited # by SEPARATOR if supplied) and expand UNIQ, else NOT-UNIQ. m4_define([lt_if_append_uniq], [m4_ifdef([$1], [m4_if(m4_index([$3]m4_defn([$1])[$3], [$3$2$3]), [-1], [lt_append([$1], [$2], [$3])$4], [$5])], [lt_append([$1], [$2], [$3])$4])]) # lt_dict_add(DICT, KEY, VALUE) # ----------------------------- m4_define([lt_dict_add], [m4_define([$1($2)], [$3])]) # lt_dict_add_subkey(DICT, KEY, SUBKEY, VALUE) # -------------------------------------------- m4_define([lt_dict_add_subkey], [m4_define([$1($2:$3)], [$4])]) # lt_dict_fetch(DICT, KEY, [SUBKEY]) # ---------------------------------- m4_define([lt_dict_fetch], [m4_ifval([$3], m4_ifdef([$1($2:$3)], [m4_defn([$1($2:$3)])]), m4_ifdef([$1($2)], [m4_defn([$1($2)])]))]) # lt_if_dict_fetch(DICT, KEY, [SUBKEY], VALUE, IF-TRUE, [IF-FALSE]) # ----------------------------------------------------------------- m4_define([lt_if_dict_fetch], [m4_if(lt_dict_fetch([$1], [$2], [$3]), [$4], [$5], [$6])]) # lt_dict_filter(DICT, [SUBKEY], VALUE, [SEPARATOR], KEY, [...]) # -------------------------------------------------------------- m4_define([lt_dict_filter], [m4_if([$5], [], [], [lt_join(m4_quote(m4_default([$4], [[, ]])), lt_unquote(m4_split(m4_normalize(m4_foreach(_Lt_key, lt_car([m4_shiftn(4, $@)]), [lt_if_dict_fetch([$1], _Lt_key, [$2], [$3], [_Lt_key ])])))))])[]dnl ]) # ltversion.m4 -- version numbers -*- Autoconf -*- # # Copyright (C) 2004 Free Software Foundation, Inc. # Written by Scott James Remnant, 2004 # # This file is free software; the Free Software Foundation gives # unlimited permission to copy and/or distribute it, with or without # modifications, as long as this notice is preserved. # @configure_input@ # serial 3337 ltversion.m4 # This file is part of GNU Libtool m4_define([LT_PACKAGE_VERSION], [2.4.2]) m4_define([LT_PACKAGE_REVISION], [1.3337]) AC_DEFUN([LTVERSION_VERSION], [macro_version='2.4.2' macro_revision='1.3337' _LT_DECL(, macro_version, 0, [Which release of libtool.m4 was used?]) _LT_DECL(, macro_revision, 0) ]) # lt~obsolete.m4 -- aclocal satisfying obsolete definitions. -*-Autoconf-*- # # Copyright (C) 2004, 2005, 2007, 2009 Free Software Foundation, Inc. # Written by Scott James Remnant, 2004. # # This file is free software; the Free Software Foundation gives # unlimited permission to copy and/or distribute it, with or without # modifications, as long as this notice is preserved. # serial 5 lt~obsolete.m4 # These exist entirely to fool aclocal when bootstrapping libtool. # # In the past libtool.m4 has provided macros via AC_DEFUN (or AU_DEFUN) # which have later been changed to m4_define as they aren't part of the # exported API, or moved to Autoconf or Automake where they belong. # # The trouble is, aclocal is a bit thick. It'll see the old AC_DEFUN # in /usr/share/aclocal/libtool.m4 and remember it, then when it sees us # using a macro with the same name in our local m4/libtool.m4 it'll # pull the old libtool.m4 in (it doesn't see our shiny new m4_define # and doesn't know about Autoconf macros at all.) # # So we provide this file, which has a silly filename so it's always # included after everything else. This provides aclocal with the # AC_DEFUNs it wants, but when m4 processes it, it doesn't do anything # because those macros already exist, or will be overwritten later. # We use AC_DEFUN over AU_DEFUN for compatibility with aclocal-1.6. # # Anytime we withdraw an AC_DEFUN or AU_DEFUN, remember to add it here. # Yes, that means every name once taken will need to remain here until # we give up compatibility with versions before 1.7, at which point # we need to keep only those names which we still refer to. # This is to help aclocal find these macros, as it can't see m4_define. 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Multiple calls are # equivalent to a single call with all the marker files in the list. # Automake checks that the files listed here are not in the list of # distributed files, and issues a warning if they are. AC_DEFUN([STAR_PREDIST_SOURCES], [m4_ifval([$1], [], [AC_FATAL([$0: called with no stamp file])])dnl _star_tmp='$1' for marker in $_star_tmp do if test -f $marker; then _star_predist_marker_present=: AC_MSG_NOTICE([found predist marker file $marker]) else _star_predist_marker_present=false fi case $_star_predist_status in unknown) if $_star_predist_marker_present; then # we do want to build sourceset files _star_predist_status=predist PREDIST= AC_MSG_NOTICE([in pre-distribution state]) else _star_predist_status=postdist PREDIST='#' AC_MSG_NOTICE([in post-distribution state]) fi ;; predist) if $_star_predist_marker_present; then : OK else AC_MSG_WARN([Building predist, but marker file $marker is not present]) fi ;; postdist) if $_star_predist_marker_present; then AC_MSG_WARN([In postdistribution state, but predist marker file $marker is present]) fi ;; *) AC_MSG_ERROR([impossible predist status $_star_predist_status]) ;; esac done ])# STAR_PREDIST_SOURCES # STAR_CNF_COMPATIBLE_SYMBOLS # --------------------------- # # Work out what is required to have the Fortran compiler produce # library symbols which are compatible with those expected by the CNF # package. If you are building a library in which C code refers to # Fortran libraries, then you should call this macro, which possibly # adjusts the AM_FCFLAGS variable. That is, if you include cnf.h, you # should have this macro in the configure.ac. # # This macro deals with the following issue. The cnf.h header # includes a macro F77_EXTERNAL_NAME which mangles a C name into the # corresponding name the Fortran compiler would generate; this # generally means no more than appending a single underscore. As the # autoconf documentation for AC_FC_WRAPPERS points out, this is less # general than it could be, as some Fortrans fold symbols to # uppercase, and some (in particular g77) add two underscores to # symbols which already contain one (thus mangling 'ab' to 'ab_', but # 'a_b' to 'a_b__'). This behaviour would break the F77_EXTERNAL_NAME # macro, which is used throughout the Starlink code in both cases, # unless we compiled all the Starlink Fortran libraries in a mode which # suppressed this second underscore. Working out how to do that -- # if it's necessary at all -- is what this macro does. # # The more restricted interface of F77_EXTERNAL_NAME is, by the way, # the reason why we cannot simply copy the FC_FUNC definition to the # cnf.h file as F77_EXTERNAL_NAME: the latter macro is used for # symbols both with and without an underscore. # # If we ever have to migrate the Starlink software to a Fortran which # does more complicated name mangling, we'll almost certainly have to # perform more serious surgery on cnf.h, using the results of # AC_FC_WRAPPERS, along with similar surgery on the code which invokes # it. # # This macro is designed to work with CNF, however it does _not_ # require the cnf.h headers to be installed, because it should remain # callable at configuration time before _anything_ has been installed. # In the test code below, we therefore emulate the definition of # F77_EXTERNAL_NAME in cnf.h, which appends a single underscore. # to the end of C symbols. # AC_DEFUN([STAR_CNF_COMPATIBLE_SYMBOLS], [$_star_docs_only && AC_MSG_ERROR([STAR[]_CNF_COMPATIBLE_SYMBOLS in docs-only dir]) AC_CACHE_CHECK([how to make Fortran and C play nicely], [star_cv_cnf_compatible_symbols], [dnl AC_REQUIRE([AC_PROG_FC])dnl dnl AC_REQUIRE([AC_PROG_CC])dnl AC_LANG_PUSH([C]) AC_LANG_CONFTEST([AC_LANG_SOURCE([ void funcone_() { return; } void func_two_() { return; } ])]) if (eval $ac_compile) 2>&5 then mv conftest.$ac_objext c-conftest.$ac_objext else AC_MSG_ERROR([cannot compile a C program!]) fi AC_LANG_POP(C) AC_LANG_PUSH([Fortran]) AC_LANG_CONFTEST([AC_LANG_SOURCE([ PROGRAM conftest CALL funcone CALL func_two END ])]) star_cv_cnf_compatible_symbols=cantlink # The only Fortran we (need to) handle at present is # g77, which has a -fno-second-underscore option for # simplifying the mangling here. Other Fortrans we've # used do only the single-underscore mangling. for opt in "" "-fno-second-underscore" do if $FC $FCFLAGS $opt -o conftest conftest.f c-conftest.$ac_objext 2>&5 then star_cv_cnf_compatible_symbols=$opt break fi done AC_LANG_POP([Fortran]) rm -f conftest* c-conftest* ]) if test "$star_cv_cnf_compatible_symbols" = cantlink then AC_MSG_ERROR([cannot work out how]) else STAR_FCFLAGS="$STAR_FCFLAGS $star_cv_cnf_compatible_symbols" STAR_FFLAGS="$STAR_FFLAGS $star_cv_cnf_compatible_symbols" fi ])# STAR_CNF_COMPATIBLE_SYMBOLS # STAR_CNF_F2C_COMPATIBLE # ----------------------- # # Work out if the compiler is using 'f2c' compatible calling conventions. # # The `f2c' calling conventions, used by GNU Fortran compilers, require # functions that return type REAL to actually return the C type 'double' # (there is also special handling of COMPLEX returns, but that's not supported # by CNF). When operating in 'non-f2c' mode such functions return the expected # C type 'float'. # # The effect of this macro is subsitute the variable REAL_FUNCTION_TYPE # to either float or double as required. # # This function is not infallable and will usually return float for GNU # compilers, as the calling convention seems to not matter on 32-bit platforms # for the test in use. A stronger test would be to attempt calling a intrinsic # function, which is supposed to fail. Non-GNU compilers should always # return float. However, this test is used as it is all that is required. # AC_DEFUN([STAR_CNF_F2C_COMPATIBLE], [$_star_docs_only && AC_MSG_ERROR([STAR[]_CNF_F2C_SYMBOLS in docs-only dir]) AC_CACHE_CHECK([if $FC is in strict f2c compatible mode], [star_cv_cnf_f2c_compatible], [AC_REQUIRE([AC_PROG_FC])dnl if test "$ac_cv_fc_compiler_gnu" = yes; then AC_REQUIRE([AC_PROG_CC])dnl AC_LANG_PUSH([C]) AC_LANG_CONFTEST([AC_LANG_SOURCE([ float fred_() { return 1.0f; } ])]) if (eval $ac_compile) 2>&5 then mv conftest.$ac_objext c-conftest.$ac_objext else AC_MSG_ERROR([cannot compile a C function!]) fi AC_LANG_POP(C) AC_LANG_PUSH([Fortran]) AC_LANG_CONFTEST([AC_LANG_SOURCE([ PROGRAM F2CTEST REAL FRED REAL R R = FRED() IF ( R .NE. 0.0 ) THEN WRITE(*,*) 'no' ELSE WRITE(*,*) 'yes' ENDIF END ])]) star_cv_cnf_f2c_compatible=yes $FC $FCFLAGS $opt -o conftest conftest.f c-conftest.$ac_objext 2>&5 if test -r conftest then star_cv_cnf_f2c_compatible=`eval ./conftest | sed 's/\ //g'` > /dev/null else AC_MSG_ERROR([failed to link program]) fi AC_LANG_POP([Fortran]) rm -f conftest* c-conftest* else # Not a GNU compiler. star_cv_cnf_f2c_compatible=no fi ]) if test "$star_cv_cnf_f2c_compatible" = "yes" then AC_SUBST(REAL_FUNCTION_TYPE, double) else AC_SUBST(REAL_FUNCTION_TYPE, float) fi ])# STAR_CNF_F2C_COMPATIBLE # STAR_CNF_BLANK_COMMON # --------------------- # Define the global symbol used to access the Fortran blank common block. # Usually under UNIX this is _BLNK__, but gfortran uses __BLNK__, so we # need to check for that. Gfortran is just detected by being a GNU compiler # and having "Fortran (GCC) 4.x[x].x[x]" as part of its --version output. # # The effect of this macro is to substitute BLANK_COMMON_SYMBOL with # the expected value. # AC_DEFUN([STAR_CNF_BLANK_COMMON], [AC_CACHE_CHECK([symbol used for blank common in Fortran], [star_cv_blank_common_symbol], [AC_REQUIRE([AC_PROG_FC]) star_cv_blank_common_symbol=_BLNK__ if test "$ac_cv_fc_compiler_gnu" = yes; then if "$FC" --version 2>&1 < /dev/null | grep 'GNU Fortran.*[[4-9]]\.[[0-9]][[0-9]]*\.[[0-9]][[0-9]]*' > /dev/null; then star_cv_blank_common_symbol=__BLNK__ fi fi]) AC_SUBST([BLANK_COMMON_SYMBOL], $star_cv_blank_common_symbol ) ])# STAR_CNF_BLANK_COMMON # STAR_PRM_COMPATIBLE_SYMBOLS # --------------------------- # # See if any special flags are required to support PRM and the use of the # PRM_PAR constants. If a typeless BOZ descriptor is available (usually 'X) # then this macro will have no effect, however, if there's no typeless BOZ # support any special Fortran compiler flags that are required when using # PRM_PAR will be defined as part of the STAR_FCFLAGS and STAR_FFLAGS # variables. # # In fact this macro is only currently used for the gfortran and Solaris f95 # compilers. Gfortran has no typeless BOZ support, so requires that the # -fno-range-check flag is set so that assigments to integers can silently # overflow (BOZ constants are replaced with their plain integer and floating # point equivalents). The Solaris f95 compiler doesn't allow assignments to # LOGICAL parameters, so we need to use the -f77 flag. # # In general this macro should be used by all packages that include PRM_PAR, # all monoliths are assumed to use this by default. # AC_DEFUN([STAR_PRM_COMPATIBLE_SYMBOLS], [$_star_docs_only && AC_MSG_ERROR([STAR[]_PRM_COMPATIBLE_SYMBOLS in docs-only dir]) AC_CACHE_CHECK([how to make compiler accept PRM constants], [star_cv_prm_compatible_symbols], [star_cv_prm_compatible_symbols="nocheck" AC_MSG_NOTICE([ ]) AC_FC_HAVE_TYPELESS_BOZ 2>&5 if test $ac_cv_fc_have_typeless_boz = no; then AC_FC_HAVE_OLD_TYPELESS_BOZ 2>&5 if test $ac_cv_fc_have_old_typeless_boz = no; then # Test if -f77 works. Note need to clear the cached variables # for these tests. unset ac_cv_fc_have_typeless_boz unset ac_cv_fc_have_old_typeless_boz old_FCFLAGS="$FCFLAGS" FCFLAGS="-f77 $FCFLAGS" AC_FC_HAVE_TYPELESS_BOZ 2>&5 if test $ac_cv_fc_have_typeless_boz = no; then AC_FC_HAVE_OLD_TYPELESS_BOZ 2>&5 if test $ac_cv_fc_have_old_typeless_boz = no; then star_cv_prm_compatible_symbols="nocheck" else star_cv_prm_compatible_symbols="-f77" fi else star_cv_prm_compatible_symbols="-f77" fi FCFLAGS="$old_FCFLAGS" if test "$star_cv_prm_compatible_symbols" = "nocheck"; then # Test if "-fno-range-check" works. AC_REQUIRE([AC_PROG_FC])dnl AC_LANG_PUSH([Fortran]) AC_LANG_CONFTEST([AC_LANG_SOURCE([ PROGRAM conftest INTEGER*2 VAL__BADUW PARAMETER ( VAL__BADUW = 65535 ) BYTE VAL__BADUB PARAMETER ( VAL__BADUB = 255 ) END ])]) if $FC -c $FCFLAGS -fno-range-check -o conftest conftest.f 2>&5 then star_cv_prm_compatible_symbols="-fno-range-check" fi AC_LANG_POP([Fortran]) rm -f conftest.f fi else star_cv_prm_compatible_symbols="" fi else star_cv_prm_compatible_symbols="" fi]) if test "$star_cv_prm_compatible_symbols" = "nocheck"; then AC_MSG_ERROR([cannot work out how]) else STAR_FCFLAGS="$STAR_FCFLAGS $star_cv_prm_compatible_symbols" STAR_FFLAGS="$STAR_FFLAGS $star_cv_prm_compatible_symbols" fi ])# STAR_PRM_COMPATIBLE_SYMBOLS # STAR_CNF_TRAIL_TYPE # ------------------- # # Work out what type to use for the trailing lengths of character strings # passed from Fortran to C. See the "TRAIL" descriptions in SUN/209. # # For most compilers the maximum length of a string is limited to a 32bit # unsigned int, but for others, this can be a 64bit unsigned long. Currently # the only compilers with 64bit strings are 64bit Intel fortran and # Solaris studio12 with -m64. # # The test is only performed for 64bit compilers, all others are assumed # to use 32bit lengths. Various attempts to trap this issue permanently # using a test program have failed (especially for the Intel compiler), so the # actual test is to check for a known 64 bit compiler first and then try a # program that has had some success. Note no GNU compilers seem to have this # problem so they are never tested. # # The side-effect of this macro is to substitute TRAIL_TYPE with # the derived value and define TRAIL_TYPE. See "f77.h" in CNF. # AC_DEFUN([STAR_CNF_TRAIL_TYPE], [AC_CHECK_SIZEOF(void*)dnl AC_FC_HAVE_PERCENTLOC dnl AC_CACHE_CHECK([type used for Fortran string lengths], [star_cv_cnf_trail_type], [if test "$ac_cv_sizeof_voidp" = 8 -a "$ac_cv_fc_compiler_gnu" = no; then if "$FC" -V 2>&1 < /dev/null | grep 'Intel.*64' > /dev/null; then star_cv_cnf_trail_type=long elif "$FC" -V 2>&1 < /dev/null | grep 'Sun.*Fortran' > /dev/null; then star_cv_cnf_trail_type=long else AC_REQUIRE([AC_PROG_FC])dnl AC_LANG_PUSH([Fortran]) if test "$ac_cv_fc_have_percentloc" = yes; then FORTRAN_GETLOC='%loc' else FORTRAN_GETLOC='loc' fi AC_LANG_CONFTEST([AC_LANG_SOURCE([ program conftest C checks passing 4 byte character string lengths on 64bit compiler. integer*8 ip1, ip2 integer*4 l1, l2 integer dummy1, dummy2 real dummy3, dummy4 double precision dummy5, dummy6 character str1*(1024) character str2*(2048) ip1 = $FORTRAN_GETLOC (str1) ip2 = $FORTRAN_GETLOC (str2) l1 = 1024 l2 = 2048 call report( dummy1, dummy2, %val(ip1), dummy3, dummy4, : %val(ip2), dummy5, dummy6, : %val(l1), %val(l2) ) end subroutine report( dummy1, dummy2, str1, dummy3, dummy4, : str2, dummy5, dummy6 ) integer dummy1, dummy2 real dummy3, dummy4 double precision dummy5, dummy6 character*(*) str1 character*(*) str2 if ( [len(str1)] .eq. 1024 .and. [len(str2)] .eq. 2048 ) then print *, 'int' else print *, 'long' endif end ])]) star_cv_cnf_trail_type=int $FC $FCFLAGS $opt -o conftest conftest.f 2>&5 if test -r conftest then star_cv_cnf_trail_type=`eval ./conftest | sed 's/\ //g'` > /dev/null else AC_MSG_ERROR([failed to link program]) fi rm -f conftest* AC_LANG_POP([Fortran]) fi else dnl sizeof(void *) != 8 or GNU so no problems. star_cv_cnf_trail_type=int fi ]) AC_SUBST([TRAIL_TYPE], $star_cv_cnf_trail_type ) AC_DEFINE_UNQUOTED([TRAIL_TYPE], $star_cv_cnf_trail_type, [Type of Fortran CNF TRAIL argument] ) ])# STAR_CNF_TRAIL_TYPE # STAR_PATH_TCLTK([minversion=0], [options='']) # --------------------------------------------- # # Finds a tclsh and wish, and the associated libraries. Sets output variable # TCL_CFLAGS to the C compiler flags necessary to compile with Tcl, TCL_LIBS # to the required library flags, and TCLSH to the full path of the tclsh # executable, TCL_PREFIX to the installation root and TCL_LD_SEARCH_FLAGS # to the default search path for loading the shareable library; if Tk is # requested, it similarly sets TK_CFLAGS, TK_LIBS and WISH. Define the # cpp variable TCL_MISSING to 1 if Tcl is not available. Similar to # macro AC_PATH_XTRA. # # If argument MINVERSION is present, it specifies the minimum Tcl/Tk # version number required. # # The macro searches first in the path, and # then in a selection of platform-specific standard locations. The # configure option --with-tcl allows you to provide a path to a tclsh # binary, which is put at the head of the list of locations to search. # Option --without-tcl suppresses the search, and results in no # variables being substituted. # # If the argument OPTIONS is present, it is a space-separated list of # the words 'tk' or 'itcl'. If one or both of these is present, then # the macro will find a Tcl location which also has Tk or itcl # installed (note that the itcl test doesn't do anything at present). AC_DEFUN([STAR_PATH_TCLTK], [_star_use_tcl=: AC_ARG_WITH([tcl], AS_HELP_STRING([--with-tcl], [give path to tclsh (dir which contains binary)]), [if test "X$withval" = Xno; then _star_use_tcl=false elif test "X$withval" = Xyes; then _star_use_tcl=: else _star_use_tcl=: _star_try_tcldir=$withval fi]) if $_star_use_tcl; then _star_searchfor=Tcl if expr "x m4_ifval([$2], [$2], []) " : 'x.* tk ' >/dev/null; then search_tk=: _star_searchfor="$_star_searchfor/Tk" else search_tk=false fi if expr "x m4_ifval([$2], [$2], []) " : 'x.* itcl ' >/dev/null; then search_itcl=: _star_searchfor="$_star_searchfor/itcl" echo "Searching for itcl does nothing so far!" else search_itcl=false fi AC_MSG_CHECKING([where to find $_star_searchfor m4_ifval([$1], [$1+], [(any version)])]) AC_CACHE_VAL([star_cv_settcldir], [star_cv_settcldir=unknown reqversint=`echo m4_ifval([$1], [$1], 0.0)-0-0 | [sed 's/\([0-9]*\)[^0-9]*\([0-9]*\)[^0-9]*\([0-9]*\).*/10000 \1* 100 \2*+ \3+p/']|dc` tclsources=`echo $PATH | sed "s/$PATH_SEPARATOR/ /g"` stdsources=' dnl Search in /usr and /usr/local at least /usr/bin /usr/local/bin dnl /opt/local and /sw are the default installation locations for OpenDarwin dnl and Fink on OSX /opt/local/bin /sw/bin' for d in $_star_try_tcldir $STARCONF_DEFAULT_STARLINK/bin $tclsources $stdsources do locok=: if test -d $d; then tcldir=`cd $d/..; pwd` test -f $d/tclsh -a -f $tcldir/include/tcl.h || locok=false else locok=false fi if $locok && $search_tk; then test -f $d/wish -a -f $tcldir/include/tk.h || locok=false fi if $locok && $search_itcl; then test -f $tcldir/lib/libitcl.aXXX || locok=false fi if $locok; then if test ! -f $tcldir/lib/tclConfig.sh; then echo "$tcldir/lib/tclConfig.sh unexpectedly missing" break fi if $search_tk && test ! -f $tcldir/lib/tkConfig.sh; then echo "$tcldir/lib/tkConfig.sh unexpectedly missing" break fi rm -f conftest.results # Run in a subshell, to isolate settings in tclConfig.sh # Send output to conftest.results, and return # 0 if all is ok ( . $tcldir/lib/tclConfig.sh if $search_tk; then . $tcldir/lib/tkConfig.sh fi tclversint=`[echo $TCL_VERSION$TCL_PATCH_LEVEL-0-0 | sed 's/\([0-9]*\)[^0-9]*\([0-9]*\)[^0-9]*\([0-9]*\).*/10000 \1* 100 \2*+ \3+p/'|dc]` if test $tclversint -gt $reqversint; then # New enough version. # Dereference the tclsh and wish links -- the "->" _is_ standard, # mandated by POSIX. lslink=`ls -l $tcldir/bin/tclsh` tclsh_loc=`expr "x$lslink" : "x.*-> *\(.*\)"` if test -n "$tclsh_loc" -a -x "$tclsh_loc"; then : OK elif test -x "$tcldir/bin/tclsh"; then # Odd: either .../bin/tclsh isn't a link, or it doesn't point to an # executable. But .../bin/tclsh is OK, so use that. tclsh_loc="$tcldir/bin/tclsh" else # This really shouldn't happen, since we checked above that # $d/tclsh was executable. Still, it clearly has happened, # so don't go mad. echo "Warning: found Tcl libraries, but not tclsh!" >&2 tclsh_loc= fi res="_star_tcldir=$tcldir;" # Make the TCL version number available. res="$res TCL_VERSION=\"$TCL_VERSION\";" # Export the TCL_PREFIX value. res="$res TCL_PREFIX=\"$TCL_PREFIX\";" # Export the TCL_LD_SEARCH_FLAGS value (need LIB_RUNTIME_DIR # which is part of the symbol). res="$res LIB_RUNTIME_DIR=\"$TCL_PREFIX/lib\";" res="$res TCL_LD_SEARCH_FLAGS=\"$TCL_LD_SEARCH_FLAGS\";" # These envs include $TCL_DBGX -- expand this out. eval "I=\"$TCL_INCLUDE_SPEC\"; L=\"$TCL_LIB_SPEC\"" res="$res TCL_CFLAGS=\"$I\"; TCL_LIBS=\"$L\"; TCLSH=\"$tclsh_loc\";" if $search_tk; then # Same for wish lslink=`ls -l $tcldir/bin/wish` wish_loc=`expr "x$lslink" : "x.*-> *\(.*\)"` if test -n "$wish_loc" -a -x "$wish_loc"; then : OK elif test -x "$tcldir/bin/wish"; then wish_loc="$tcldir/bin/wish" else echo "Warning: found Tk libraries, but not wish!" >&2 wish_loc= fi # These envs potentially include $TK_DBGX -- expand this out. eval "I=\"$TK_XINCLUDES\"; L=\"$TK_LIB_SPEC\"" res="$res TK_CFLAGS=\"$I\"; TK_LIBS=\"$L\"; WISH=\"$wish_loc\";" fi # similarly for $search_itcl echo $res >conftest.results status=0 else msg="$tcldir: found Tcl-$TCL_VERSION$TCL_PATCH_LEVEL" if $search_tk; then msg="$msg, Tk-$TK_VERSION$TK_PATCH_LEVEL" fi echo "$msg: older than required" >&2 status=1 fi exit $status ) teststat=$? if test $teststat = 0; then star_cv_settcldir=`cat conftest.results` fi if test "$star_cv_settcldir" != unknown; then break fi fi # $locok done]) if test "$star_cv_settcldir" = unknown; then AC_MSG_RESULT(unknown) else eval $star_cv_settcldir AC_MSG_RESULT($_star_tcldir) fi else # $_star_use_tcl AC_MSG_WARN(Compiling without Tcl/Tk) fi # $_star_use_tcl if $_star_use_tcl && test "$star_cv_settcldir" != unknown; then : else AC_DEFINE(TCL_MISSING, 1, [Define to 1 if no Tcl/Tk libraries can be found]) fi AC_SUBST(TCL_VERSION) AC_SUBST(TCL_PREFIX) AC_SUBST(TCL_LD_SEARCH_FLAGS) AC_SUBST(TCL_CFLAGS) AC_SUBST(TCL_LIBS) AC_SUBST(TCLSH) AC_SUBST(TK_CFLAGS) AC_SUBST(TK_LIBS) AC_SUBST(WISH) # add itcl variables here ])# STAR_PATH_TCLTK # STAR_LATEX_DOCUMENTATION(documentcode, [targets]) # ------------------------------------------------- # Generate the standard makefile targets to handle LaTeX documentation # source. The parameter documentcode should be something like # `sun123' -- it should not include any .tex extension. # # The second, optional, argument gives an explicit list of the targets # which are build. If this is _not_ specified, then a standard list # is used (.tex, .ps and .tar_htx) and corresponding rules added to # the generated makefile. If it is specified, it must be non-null, # and its value is a list of files which are to be added to the # distribution, and no extra Makefile rules are added. Thus if users need # anything complicated done, they should use this second argument and # provide rules for satisfying the given targets. # # In the latter case, the .tex -> htx_tar rule is still emitted, so # you can use it, but it requires the substitution variable # @STAR[]2HTML@, and so if you _do_ use it, you will have to make that # available, either through [STAR_CHECK_PROGS(star2html)] or otherwise. AC_DEFUN([STAR_LATEX_DOCUMENTATION], [m4_ifval([$1], [], [AC_FATAL([$0: called with no documentcode])])dnl m4_if(m4_bregexp([$1], [^ *\([a-z][a-z]*[0-9]*/? *\)*$]), [0], [], [AC_FATAL([$0: bad doccode in $1 -- must be eg sun123 or sun123/])]) STAR_DOCUMENTATION="$STAR_DOCUMENTATION m4_bpatsubst([$1],[/])" m4_ifval([$2], [dnl non-empty second argument -- just add to variable m4_if(m4_bregexp([$1], [/]), -1, [], [AC_FATAL([$0: do not mix non-null second argument and .../ syntax])]) if $_star_build_docs; then STAR@&t@_LATEX_DOCUMENTATION="$2" fi ], [dnl second arg empty -- use defaults if $_star_build_docs; then AC_FOREACH([DocCode], [$1], [m4_if(m4_bregexp(DocCode,[/]), -1, [STAR@&t@_LATEX_DOCUMENTATION="$STAR@&t@_LATEX_DOCUMENTATION DocCode.tex DocCode.pdf DocCode.htx_tar" ], [m4_define([_T], m4_bpatsubst(DocCode,[/]))dnl STAR_LATEX_DOCUMENTATION_[]_STAR_UPCASE(_T)="_T.tex _T.pdf _T.htx_tar" AC_SUBST(STAR_LATEX_DOCUMENTATION_[]_STAR_UPCASE(_T))])]) fi STAR_DECLARE_DEPENDENCIES([sourceset], [star2html]) STAR_CHECK_PROGS([star2html]) ]) if $_star_build_docs; then : ${LATEX2DVI='$$LATEX "\\batchmode\\input $$[]1" && $$LATEX "\\batchmode\\input $$[]1"'} AC_SUBST(LATEX2DVI) else AC_MSG_WARN([not installing docs $1]) fi AC_SUBST([STAR@&t@_LATEX_DOCUMENTATION])dnl ])# STAR_LATEX_DOCUMENTATION # STAR_XML_DOCUMENTATION(documentcode, [targets]) # ----------------------------------------------- # Generate the standard makefile targets to handle XML documentation # source. The parameter documentcode should be something like # `sun123' -- it should not include any .xml extension. For each of the # documentcodes which does not end with a slash, append # .{texml_tar,htx_tar,ps} to STAR_XML_DOCUMENTATION; # for each which does end with a slash, define instead the # variable STAR_XML_DOCUMENTATION_. In either case, # append the documentcode to STAR_DOCUMENTATION # # The second, optional, argument gives an explicit list of the targets # which are build. If this is _not_ specified, then a standard list # is used (.texml_tar, .ps and .htx_tar) and corresponding rules added to # the generated makefile. If it is specified, it must be non-null, # and its value is a list of files which are to be added to the # distribution, and no extra Makefile rules are added. Thus if users need # anything complicated done, they should use this second argument and # provide rules for satisfying the given targets. # # In the latter case, the .tex -> htx_tar rule is still emitted, so # you can use it, but it requires the substitution variables JADE, SGMLNORM, # and SGMLKIT_HOME. This is rather inconvenient, and it is fortunate that # you almost certainly won't need to use this. AC_DEFUN([STAR_XML_DOCUMENTATION], [m4_ifval([$1], [], [AC_FATAL([$0: called with no documentcode])])dnl m4_if(m4_bregexp([$1], [^ *\([a-z][a-z]*[0-9]*/? *\)*$]), [0], [], [AC_FATAL([$0: bad doccode in $1 -- must be eg sun123 or sun123/])]) STAR_DOCUMENTATION="$STAR_DOCUMENTATION m4_bpatsubst([$1],[/])" m4_ifval([$2], [dnl non-empty second argument -- just add to variable m4_if(m4_bregexp([$1], [/]), -1, [], [AC_FATAL([$0: do not mix non-null second argument and .../ syntax])]) if $_star_build_docs; then STAR@&t@_XML_DOCUMENTATION="$2" fi ], [dnl second arg empty -- use defaults if $_star_build_docs; then do_the_build= # blank if we're to go ahead, string expl. otherwise AC_PATH_PROGS(JADE, [openjade jade], NOJADE) AC_PATH_PROGS(SGMLNORM, [osgmlnorm sgmlnorm], NOSGMLNORM) STAR_CHECK_PROGS([sgml2docs]) if test "$JADE" = NOJADE -o "$SGMLNORM" = NOSGMLNORM -o "$SGML2DOCS" = "sgml2docs"; then if $_star_docs_only; then # Building documentation is all we're supposed to do, # and we can't, so suppress further building. do_the_build=\ "This docs-only component requires Jade, sgmlnorm and sgml2docs. All I could find were: $JADE for Jade, $SGMLNORM for sgmlnorm and $SGML2DOCS for sgml2docs (requires full path). Your system may have a way to install Jade and sgmlnorm as a package, sgml2docs is part of the SGMLKIT package." else AC_MSG_WARN([can't find (open)jade + (o)sgmlnorm + sgml2docs -- skipping XML documentation $1]) fi else # Test Jade version AC_MSG_CHECKING([version of $JADE (need 1.3.2 or better)]) $JADE -v conftest.version 2>&1 JADEVERS=[`sed -n '/:I:.*[Jj]ade.*version/{ s/.*:I:// s/[^0-9][^0-9]*/ /gp }' conftest.version`] # The following converts space-separated integers to a single # one. It's perhaps a leeettle funkier than necessary... VERSINT=[`echo "[Ss[z0conftest-d1/d/f (cd conftest-d1/d; $LN_S f l; $LN_S x broken) if test ! -h conftest-d1/d/l; then # We don't have links! So plain cp -R will do star_cv_cp_r="$CP -R" else star_cv_cp_r= for try in "$CP -R --no-dereference -p -f" "$CP -R -P -p -f" "$CP -R -P -p" "$CP -R -p" "${PAX-false} -r -w -p p" do rm -Rf conftest-d2/* if (cd conftest-d1; $try . ../conftest-d2 2>/dev/null); then if test -h conftest-d2/d/l -a -h conftest-d2/d/broken; then star_cv_cp_r="$try" break fi fi done fi rm -Rf conftest*]) if test -z "$star_cv_cp_r"; then AC_MSG_ERROR([unable to find working cp or pax]) fi AC_SUBST(CP_RECURSIVE, $star_cv_cp_r)dnl ])# STAR_SPECIAL_INSTALL_COMMAND # STAR_MONOLITHS # -------------- # Declare that we will be creating monoliths. This does whatever # configuration is necessary to handle these. # # Note that the declarations done in the Makefile.am, declaring the # name of the monolith and the names and source files of the tasks, # are slightly redundant inasmuch as some of that information could be # implied. However, this is required to be explicit for clarity and # consistency, and so accomodate the (currently unexploited) # possibility that the tasks and .ifl files longer have the # one-task-per-file relationship they have now. AC_DEFUN([STAR_MONOLITHS], [$_star_docs_only && AC_MSG_ERROR([STAR[]_MONOLITHS in docs-only directory]) dnl Installation in monoliths.am uses $(LN_S) AC_REQUIRE([AC_PROG_LN_S])dnl # To build monoliths, we need both compifl to build the .ifc # files (in the parsecon component), and alink # to link the monoliths (in dtask). Both are now part of # the pcs component. STAR_DECLARE_DEPENDENCIES(build, [pcs]) # So try to find alink and compifl. STAR_CHECK_PROGS([compifl alink]) # When we're building monoliths, we will almost certainly be # using Fortran, and so we might as well include this, # partly in case the user forgets, but also because this is # reasonably part of the default setup required for monoliths. STAR_CNF_COMPATIBLE_SYMBOLS STAR_PRM_COMPATIBLE_SYMBOLS ])# STAR_MONOLITHS # STAR_HELP_FILES(helpfiles) # -------------------------- # Declare a list of files to be installed into the Starlink help # directory. This can be used both internally and in user # configure.ac files. AC_DEFUN([STAR_HELP_FILES], [_STAR_EXTRADIR_COMMON([help], [$1])]) # STAR_ETC_FILES(etcfiles) # ------------------------ # Declare a list of files to be installed into the Starlink etc # directory. This can be used both internally and in user # configure.ac files. AC_DEFUN([STAR_ETC_FILES], [_STAR_EXTRADIR_COMMON([etc], [$1])]) # STAR_DOCS_FILES(docfiles) # ------------------------- # Declare a list of files to be installed into the Starlink # documentation directory. This can be used both internally and in # user configure.ac files. AC_DEFUN([STAR_DOCS_FILES], [_STAR_EXTRADIR_COMMON([docs], [$1])]) # STAR_EXAMPLES_FILES(examplesfiles) # ---------------------------------- # Declare a list of files to be installed into the Starlink # examples directory. This can be used both internally and in # user configure.ac files. AC_DEFUN([STAR_EXAMPLES_FILES], [_STAR_EXTRADIR_COMMON([examples], [$1])]) # STAR_DECLARE_DEPENDENCIES(type, deplist, option='') # --------------------------------------------------- # # Declare dependencies of this component. The TYPE is one of # `sourceset', `build', `link', `use', `test' or `configure', and the # DEPLIST is a space separated list of component names, which this # component depends on in the given way. # # -- Sourceset dependencies are those components which must be # installed in order to build the complete set of sources, either for # building or for distribution. This includes documentation, so it # would include star2html as well as messgen. # # -- Build dependencies are those which are required in order to build # this component. This typically means include files, but if part of # the component is an executable file (such as compifl within the # parsecon component), then that's a build dependence also (but see # the discussion of `option', below). You may not have two components # which have a build dependency on each other, since that would mean # that each would have to be built before the other, which is # impossible. # # -- Link dependencies are those required to link against the # libraries in a component. That means all the libraries that this # component's libraries use. These are not necessarily build # dependencies, since if you are building a library, any called # libraries don't have to be present in order to build this library; # you can have two components which have mutual link dependencies. If # you are building an application, however, then all its link # dependencies will actually be build dependencies and should be # declared as such. In other words, the distinction between build and # link dependencies is important only for library components. # # -- Use dependencies are those which are required in order for the # component to be used by something else, after it has been built and # installed. For example a library which called another application # as part of its functionality would have only a use dependency on the # component which contained that application. If no use dependencies # are declared, we take the use dependencies to be the same as the # link dependencies. # # -- Test dependencies are those which are required in order to run # any regression tests which come with the component. It's generally # a good idea to avoid making this a larger set than the use # dependencies, but sometimes this is unavoidable. If no test # dependencies are declared, we take the test dependencies to be the # same as the use dependencies. # # -- Configure dependencies are those which must be satisfied before # this component can be successfully configured. In this case, we # also check that the corresponding manifest files have been installed # in current_MANIFESTS, and if not exit with a message, and the suggestion # that the user runs 'make configure-deps'. # # The point of this is that different dependencies are required at # different times. The set of dependencies in the master makefile is # composed of all the `sourceset' and `build' dependencies, but not # `link' or `use' dependencies, and since the core Starlink libraries # are closely interdependent, the set of `build' dependencies needs to # be kept as small as possible in order to avoid circularities (that # is, A depending on B, which depends, possibly indirectly, on A). # # All these relationships are transitive: if A has a build dependency # on B, and B has one on C, then A has a build dependency on C. You # can augment this by using the final `option' argument: if, in # component A's declaration element you say # STAR_DECLARE_DEPENDENCIES(build, B, link), then you declare that A # has a build-time dependency on B, but that (presumably because you # are building an application within a component which is mostly # libraries) you need to link against B, so component A has a # dependency on all of B's _link_ dependencies, not just its build # dependencies. This is (I believe) the only case where this `option' # attribute is useful, though it is legal for each of the dependency types. # # You need only declare direct dependencies. If package A depends on # package B, which depends in turn on package C, then package A need # not declare a dependency on C. # # The macro may be called more than once. The results of this macro # are expressed in the file component.xml in the component directory. AC_DEFUN([STAR_DECLARE_DEPENDENCIES], [m4_ifval([$1], [], [AC_FATAL([$0: no type given])])dnl m4_if(m4_bregexp([$1], [^\(sourceset\|build\|link\|use\|test\|configure\)$]), [0], [], [AC_FATAL([$0: unrecognised dependency type: $1])])dnl m4_ifval([$2], [], [AC_FATAL([$0: no deplist given])])dnl for _star_tmp in $2 do STAR_DEPENDENCIES_CHILDREN="$STAR_DEPENDENCIES_CHILDREN<[$1]m4_ifval([$3], [ option='$3'], [])>$_star_tmp" done m4_if([$1], [configure], [# check that configure-deps ran... for _star_tmp in $2 do echo "$as_me:$LINENO: checking for configure-deps/$_star_tmp" >&5 echo $ECHO_N "checking for configure-deps/$_star_tmp... $ECHO_C" >&6 if test -f $current_MANIFESTS/$_star_tmp; then echo "$as_me:$LINENO: result: ok" >&5 echo "${ECHO_T}ok" >&6 else echo "$as_me:$LINENO: result: not found!" >&5 echo "${ECHO_T}not found" >&6 echo "*** This package has a configure dependency on $_star_tmp" >&6 echo " but that component doesn't appear to be installed." >&6 echo " (I can't find $current_MANIFESTS/$_star_tmp:" >&6 echo " have you forgotten to run 'make configure-deps'?)" >&6 echo " Giving up!" >&6 exit 1 fi done ])dnl ])# STAR_DECLARE_DEPENDENCIES # STAR_PLATFORM_SOURCES(target-file-list, platform-list) # ------------------------------------------------------ # # Generate the given target-file for each of the files in the list # TARGET-FILE-LIST, by selecting the appropriate element of the # PLATFORM-LIST based on the value of [AC_CANONICAL_BUILD]. Both # lists are space-separated lists. # # For each of the platforms,

, in platform-list, there should be a # file `

'. There should always be a file # `default', and if none of the platform-list strings # matches, this is the file which is used. If the `default' file is # listed in the `platform-list', then it is matched in the normal run # of things; if it is not listed, it still matches, but a warning is # issued. # # If you wish no match _not_ to be an error -- perhaps because there # is a platform-dependent file which is redundant on unlisted platforms # -- then end the platform-list with `NONE'. In this case, if no file # matches, then no link is made, with no error or warning. # # This macro uses the results of ./config.guess to determine the # current platform. That returns a triple consisting of # cpu-vendor-os, such as `i686-pc-linux-gnu' (OS=linux-gnu), # `sparc-sun-solaris2.9', or `alphaev6-dec-osf5.1' # # The extensions

in platform-list should all have the form # `cpu_vendor[_os]', where each of the components `cpu', `vendor' and # `os' may be blank. If not blank, they are matched as a prefix of # the corresponding part of the config.guess value. Thus # `_sun_solaris' would match `sparc-sun-solaris2.9' but not # `sparc-sun-sunos', and `_sun' would match both. For a # file foo.c, this would result in `ln -s foo.c_sun foo.c' # # Calls AC_LIBSOURCE for each of the implied platform-specific files. # AC_DEFUN([STAR_PLATFORM_SOURCES], [ $_star_docs_only && AC_MSG_ERROR([STAR_[]PLATFORM_SOURCES in docs-only dir]) AC_REQUIRE([AC_CANONICAL_BUILD])dnl m4_ifval([$1], [], [AC_FATAL([$0: no target-file-list given])])dnl m4_ifval([$2], [], [AC_FATAL([$0: no platform-list given])])dnl AC_FOREACH([TargetFile], [$1], [AC_FOREACH([Ext], [$2], [m4_if(Ext, [NONE], , [AC_LIBSOURCE(TargetFile[]Ext)])])])dnl AC_MSG_CHECKING([platform-specific source for file(s) $1]) _star_tmp= for platform in $2 do if test $platform = NONE; then # Special case -- no file required _star_tmp=NONE break; fi if test $platform = default; then _star_tmp=default break; fi if expr $build : `echo $platform | sed 's/_/.*-/g'` >/dev/null; then _star_tmp=$platform break; fi done if test -z "$_star_tmp"; then # Use default, but it wasn't listed in the platform-list # (though it should have been) AC_MSG_WARN([build platform $build does not match any of ($2): using `default']) _star_tmp=default fi if test $_star_tmp = NONE; then AC_MSG_RESULT([none required]) else AC_MSG_RESULT([using $_star_tmp]) for _t in $1 do if test -f $srcdir/$_t$_star_tmp; then (cd $srcdir; rm -f $_t; cp -p $_t$_star_tmp $_t) else AC_MSG_WARN([platform $_star_tmp matched, but no file $_t$_star_tmp found]) fi done fi ])# STAR_PLATFORM_SOURCES # STAR_INITIALISE_FORTRAN_RTL # --------------------------- # # Define a macro which can be used in a C main program to initialise the # Fortran RTL, including, for example, doing whatever work is required so that # the Fortran getarg() function works. This defines the macro # STAR_INITIALISE_FORTRAN(argc,argv). The implementation necessarily uses # functions which are specific to the Fortran implementation, and the body of # this macro is basically a switch to determine the compiler and thus the # appropriate compiler-specific magic. If no implementation is available, # then the macro should expand to nothing. # # Note that the Starlink functions wrapping getarg() are robust against # getarg() failing because this information is not available. This function # is nonetheless necessary because some platforms have link problems otherwise # (specifically OSX, on which the most readily available compiler is g77, # cannot link properly if the getarg() function is referenced by a library, # but there is a C main function, so that the Fortran main function's call of # f_setarg is omitted). Thus it is generally harmless to leave this function # unimplemented on those platforms which do not have these link problems, and # it is harmless that the test below is extremely compiler specific (though we # would probably have to add implementations for any other compilers used on # OSX). It's also generally harmless not to call the defined function, or # invoke this macro, if your application doesn't have the link problems which # makeit necessary, though of course calling it will make getarg() work where # it otherwise wouldn't, which may be an advantage. # # All was well until g95 and gfortran, these are "gnu" compilers, but use # different semantics. In the case of g95 the calling the startup code is not # optional (docs say that heap initialisation relies on the startup call). # # The test for g95 relies on the output from `g95 --version' containing the # string "G95". Gfortran requires "GNU Fortran (GCC) 4+.x[x].x[x]". Note that # this whole area probably needs rethinking as g95 also has a g95_runtime_stop() # function, that should be called. # # At gfortran 4.6 the call sequence stopped allowing a NULL argv, so a dummy # version had to be added. The argv[0] value is always de-referenced in an # an attempt to get the program name. # # Intel Fortran needs the for_rtl_init_ function, there is also a # for_rtl_finish_ to run during closedown. The intel compiler signature # is to have "IFORT" in the --version string. # # Under Solaris and the studio compilers the argc and argv values are no # longer automatically shared, so we test for "Sun Fortran" and have a # code section that copies the given argc and argv directly to the global # variable __xargc and __xargv, this may need fixing from time to time. # Doesn't seem to be a function for doing this job. # AC_DEFUN([STAR_INITIALISE_FORTRAN_RTL], [AC_CACHE_CHECK([how to initialise the Fortran RTL], [star_cv_initialise_fortran], [AC_REQUIRE([AC_PROG_FC]) if test "$ac_cv_fc_compiler_gnu" = yes; then if "$FC" --version 2>&1 < /dev/null | grep 'G95' > /dev/null; then star_cv_initialise_fortran=g95-start elif "$FC" --version 2>&1 < /dev/null | grep 'GNU Fortran.*[[4-9]]\.[[0-9]][[0-9]]*\.[[0-9]][[0-9]]*' > /dev/null; then star_cv_initialise_fortran=gfortran-setarg else star_cv_initialise_fortran=g77-setarg fi else if "$FC" --version 2>&1 < /dev/null | grep 'IFORT' > /dev/null; then star_cv_initialise_fortran=ifort-setarg elif "$FC" -V 2>&1 < /dev/null | grep 'Sun Fortran' > /dev/null; then star_cv_initialise_fortran=sunstudio-setarg else star_cv_initialise_fortran= fi fi]) AH_TEMPLATE([STAR_INITIALISE_FORTRAN], [Define to a function call which will initialise the Fortran RTL]) case "$star_cv_initialise_fortran" in g77-setarg) AC_DEFINE([STAR_INITIALISE_FORTRAN(argc,argv)], [{extern void f_setarg(int,char**); f_setarg(argc, argv);}]) ;; g95-start) AC_DEFINE([STAR_INITIALISE_FORTRAN(argc,argv)], [{extern void g95_runtime_start(int,char**); g95_runtime_start(argc, argv);}]) ;; gfortran-setarg) AC_DEFINE([STAR_INITIALISE_FORTRAN(argc,argv)], [{extern void _gfortran_set_args(int,char**); if (argv == NULL) {static char *sc_dummy[[]]={NULL};_gfortran_set_args(0,sc_dummy);} else {_gfortran_set_args(argc,argv);}}]) ;; ifort-setarg) AC_DEFINE([STAR_INITIALISE_FORTRAN(argc,argv)], [{extern void for_rtl_init_(int*,char**); for_rtl_init_(&argc, argv);}]) ;; sunstudio-setarg) AC_DEFINE([STAR_INITIALISE_FORTRAN(argc,argv)], [{extern int __xargc; extern char **__xargv;__xargc = argc;__xargv = argv;}]) ;; *) AC_DEFINE([STAR_INITIALISE_FORTRAN(argc,argv)],[]) ;; esac dnl AC_DEFINE_UNQUOTED([STAR_INITIALISE_FORTRAN(argc,argv)], dnl $star_cv_initialise_fortran) ])# STAR_INITIALISE_FORTRAN # STAR_SUPPRESS_BUILD_IF(test, message) # ------------------------------------- # Call once at the end of the configure script. # # If the given shell test evaluates to true, then suppress the build, # without having ./configure fail. The test is any command which # returns true if the build should be suppressed, and may be shell # commands `true' or `false', or might be a more complicated test, # such as `test -n "$SOMEENV"'. # # The macro communicates with the generated Makefile.in by creating a file # STAR_SUPPRESS_BUILD if the test evaluates to true. The file contains # the text of the explanation. AC_DEFUN([STAR_SUPPRESS_BUILD_IF], [m4_ifval([$1], [], [AC_FATAL([$0: needs two arguments])])dnl m4_ifval([$2], [], [AC_FATAL([$0: needs two arguments])])dnl rm -f STAR_SUPPRESS_BUILD if [$1]; then AC_MSG_WARN([Build inhibited: $2]) echo "$2" >STAR_SUPPRESS_BUILD ALL_TARGET=all-am-suppress else ALL_TARGET=all-am-normal fi AC_SUBST(ALL_TARGET) ])# STAR_SUPPRESS_BUILD_IF # starconf internal macros # _STAR_UPCASE(string) # -------------------- # Expands to STRING with all letters translated to uppercase. 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This library is a collection of code designed to aid in replacing the SLA library with code from SOFA. Where possible the API is similar to the C SLA API except for the use of a "pal" prefix.

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We still # use `HOST_CC' if defined, but it is deprecated. # Portable tmp directory creation inspired by the Autoconf team. set_cc_for_build=' trap "exitcode=\$?; (rm -f \$tmpfiles 2>/dev/null; rmdir \$tmp 2>/dev/null) && exit \$exitcode" 0 ; trap "rm -f \$tmpfiles 2>/dev/null; rmdir \$tmp 2>/dev/null; exit 1" 1 2 13 15 ; : ${TMPDIR=/tmp} ; { tmp=`(umask 077 && mktemp -d "$TMPDIR/cgXXXXXX") 2>/dev/null` && test -n "$tmp" && test -d "$tmp" ; } || { test -n "$RANDOM" && tmp=$TMPDIR/cg$$-$RANDOM && (umask 077 && mkdir $tmp) ; } || { tmp=$TMPDIR/cg-$$ && (umask 077 && mkdir $tmp) && echo "Warning: creating insecure temp directory" >&2 ; } || { echo "$me: cannot create a temporary directory in $TMPDIR" >&2 ; exit 1 ; } ; dummy=$tmp/dummy ; tmpfiles="$dummy.c $dummy.o $dummy.rel $dummy" ; case $CC_FOR_BUILD,$HOST_CC,$CC in ,,) echo "int x;" > $dummy.c ; for c in cc gcc c89 c99 ; do if ($c -c -o $dummy.o $dummy.c) >/dev/null 2>&1 ; then CC_FOR_BUILD="$c"; break ; fi ; done ; if test x"$CC_FOR_BUILD" = x ; then CC_FOR_BUILD=no_compiler_found ; fi ;; ,,*) CC_FOR_BUILD=$CC ;; ,*,*) CC_FOR_BUILD=$HOST_CC ;; esac ; set_cc_for_build= ;' # This is needed to find uname on a Pyramid OSx when run in the BSD universe. # (ghazi@noc.rutgers.edu 1994-08-24) if (test -f /.attbin/uname) >/dev/null 2>&1 ; then PATH=$PATH:/.attbin ; export PATH fi UNAME_MACHINE=`(uname -m) 2>/dev/null` || UNAME_MACHINE=unknown UNAME_RELEASE=`(uname -r) 2>/dev/null` || UNAME_RELEASE=unknown UNAME_SYSTEM=`(uname -s) 2>/dev/null` || UNAME_SYSTEM=unknown UNAME_VERSION=`(uname -v) 2>/dev/null` || UNAME_VERSION=unknown case "${UNAME_SYSTEM}" in Linux|GNU|GNU/*) # If the system lacks a compiler, then just pick glibc. # We could probably try harder. LIBC=gnu eval $set_cc_for_build cat <<-EOF > $dummy.c #include #if defined(__UCLIBC__) LIBC=uclibc #elif defined(__dietlibc__) LIBC=dietlibc #else LIBC=gnu #endif EOF eval `$CC_FOR_BUILD -E $dummy.c 2>/dev/null | grep '^LIBC'` ;; esac # Note: order is significant - the case branches are not exclusive. case "${UNAME_MACHINE}:${UNAME_SYSTEM}:${UNAME_RELEASE}:${UNAME_VERSION}" in *:NetBSD:*:*) # NetBSD (nbsd) targets should (where applicable) match one or # more of the tuples: *-*-netbsdelf*, *-*-netbsdaout*, # *-*-netbsdecoff* and *-*-netbsd*. For targets that recently # switched to ELF, *-*-netbsd* would select the old # object file format. This provides both forward # compatibility and a consistent mechanism for selecting the # object file format. # # Note: NetBSD doesn't particularly care about the vendor # portion of the name. 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Ake) contributed MIS and NILE. if test "`(/bin/universe) 2>/dev/null`" = att ; then echo pyramid-pyramid-sysv3 else echo pyramid-pyramid-bsd fi exit ;; NILE*:*:*:dcosx) echo pyramid-pyramid-svr4 exit ;; DRS?6000:unix:4.0:6*) echo sparc-icl-nx6 exit ;; DRS?6000:UNIX_SV:4.2*:7* | DRS?6000:isis:4.2*:7*) case `/usr/bin/uname -p` in sparc) echo sparc-icl-nx7; exit ;; esac ;; s390x:SunOS:*:*) echo ${UNAME_MACHINE}-ibm-solaris2`echo ${UNAME_RELEASE}|sed -e 's/[^.]*//'` exit ;; sun4H:SunOS:5.*:*) echo sparc-hal-solaris2`echo ${UNAME_RELEASE}|sed -e 's/[^.]*//'` exit ;; sun4*:SunOS:5.*:* | tadpole*:SunOS:5.*:*) echo sparc-sun-solaris2`echo ${UNAME_RELEASE}|sed -e 's/[^.]*//'` exit ;; i86pc:AuroraUX:5.*:* | i86xen:AuroraUX:5.*:*) echo i386-pc-auroraux${UNAME_RELEASE} exit ;; i86pc:SunOS:5.*:* | i86xen:SunOS:5.*:*) eval $set_cc_for_build SUN_ARCH="i386" # If there is a compiler, see if it is configured for 64-bit objects. # Note that the Sun cc does not turn __LP64__ into 1 like gcc does. # This test works for both compilers. if [ "$CC_FOR_BUILD" != 'no_compiler_found' ]; then if (echo '#ifdef __amd64'; echo IS_64BIT_ARCH; echo '#endif') | \ (CCOPTS= $CC_FOR_BUILD -E - 2>/dev/null) | \ grep IS_64BIT_ARCH >/dev/null then SUN_ARCH="x86_64" fi fi echo ${SUN_ARCH}-pc-solaris2`echo ${UNAME_RELEASE}|sed -e 's/[^.]*//'` exit ;; sun4*:SunOS:6*:*) # According to config.sub, this is the proper way to canonicalize # SunOS6. 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The system name ranges from "MiNT" over "FreeMiNT" # to the lowercase version "mint" (or "freemint"). Finally # the system name "TOS" denotes a system which is actually not # MiNT. But MiNT is downward compatible to TOS, so this should # be no problem. atarist[e]:*MiNT:*:* | atarist[e]:*mint:*:* | atarist[e]:*TOS:*:*) echo m68k-atari-mint${UNAME_RELEASE} exit ;; atari*:*MiNT:*:* | atari*:*mint:*:* | atarist[e]:*TOS:*:*) echo m68k-atari-mint${UNAME_RELEASE} exit ;; *falcon*:*MiNT:*:* | *falcon*:*mint:*:* | *falcon*:*TOS:*:*) echo m68k-atari-mint${UNAME_RELEASE} exit ;; milan*:*MiNT:*:* | milan*:*mint:*:* | *milan*:*TOS:*:*) echo m68k-milan-mint${UNAME_RELEASE} exit ;; hades*:*MiNT:*:* | hades*:*mint:*:* | *hades*:*TOS:*:*) echo m68k-hades-mint${UNAME_RELEASE} exit ;; *:*MiNT:*:* | *:*mint:*:* | *:*TOS:*:*) echo m68k-unknown-mint${UNAME_RELEASE} exit ;; m68k:machten:*:*) echo m68k-apple-machten${UNAME_RELEASE} exit ;; powerpc:machten:*:*) echo powerpc-apple-machten${UNAME_RELEASE} exit ;; RISC*:Mach:*:*) echo mips-dec-mach_bsd4.3 exit ;; RISC*:ULTRIX:*:*) echo mips-dec-ultrix${UNAME_RELEASE} exit ;; VAX*:ULTRIX*:*:*) echo vax-dec-ultrix${UNAME_RELEASE} exit ;; 2020:CLIX:*:* | 2430:CLIX:*:*) echo clipper-intergraph-clix${UNAME_RELEASE} exit ;; mips:*:*:UMIPS | mips:*:*:RISCos) eval $set_cc_for_build sed 's/^ //' << EOF >$dummy.c #ifdef __cplusplus #include /* for printf() prototype */ int main (int argc, char *argv[]) { #else int main (argc, argv) int argc; char *argv[]; { #endif #if defined (host_mips) && defined (MIPSEB) #if defined (SYSTYPE_SYSV) printf ("mips-mips-riscos%ssysv\n", argv[1]); exit (0); #endif #if defined (SYSTYPE_SVR4) printf ("mips-mips-riscos%ssvr4\n", argv[1]); exit (0); #endif #if defined (SYSTYPE_BSD43) || defined(SYSTYPE_BSD) printf ("mips-mips-riscos%sbsd\n", argv[1]); exit (0); #endif #endif exit (-1); } EOF $CC_FOR_BUILD -o $dummy $dummy.c && dummyarg=`echo "${UNAME_RELEASE}" | sed -n 's/\([0-9]*\).*/\1/p'` && SYSTEM_NAME=`$dummy $dummyarg` && { echo "$SYSTEM_NAME"; exit; } echo mips-mips-riscos${UNAME_RELEASE} exit ;; Motorola:PowerMAX_OS:*:*) echo powerpc-motorola-powermax exit ;; Motorola:*:4.3:PL8-*) echo powerpc-harris-powermax exit ;; Night_Hawk:*:*:PowerMAX_OS | Synergy:PowerMAX_OS:*:*) echo powerpc-harris-powermax exit ;; Night_Hawk:Power_UNIX:*:*) echo powerpc-harris-powerunix exit ;; m88k:CX/UX:7*:*) echo m88k-harris-cxux7 exit ;; m88k:*:4*:R4*) echo m88k-motorola-sysv4 exit ;; m88k:*:3*:R3*) echo m88k-motorola-sysv3 exit ;; AViiON:dgux:*:*) # DG/UX returns AViiON for all architectures UNAME_PROCESSOR=`/usr/bin/uname -p` if [ $UNAME_PROCESSOR = mc88100 ] || [ $UNAME_PROCESSOR = mc88110 ] then if [ ${TARGET_BINARY_INTERFACE}x = m88kdguxelfx ] || \ [ ${TARGET_BINARY_INTERFACE}x = x ] then echo m88k-dg-dgux${UNAME_RELEASE} else echo m88k-dg-dguxbcs${UNAME_RELEASE} fi else echo i586-dg-dgux${UNAME_RELEASE} fi exit ;; M88*:DolphinOS:*:*) # DolphinOS (SVR3) echo m88k-dolphin-sysv3 exit ;; M88*:*:R3*:*) # Delta 88k system running SVR3 echo m88k-motorola-sysv3 exit ;; XD88*:*:*:*) # Tektronix XD88 system running UTekV (SVR3) echo m88k-tektronix-sysv3 exit ;; Tek43[0-9][0-9]:UTek:*:*) # Tektronix 4300 system running UTek (BSD) echo m68k-tektronix-bsd exit ;; *:IRIX*:*:*) echo mips-sgi-irix`echo ${UNAME_RELEASE}|sed -e 's/-/_/g'` exit ;; ????????:AIX?:[12].1:2) # AIX 2.2.1 or AIX 2.1.1 is RT/PC AIX. echo romp-ibm-aix # uname -m gives an 8 hex-code CPU id exit ;; # Note that: echo "'`uname -s`'" gives 'AIX ' i*86:AIX:*:*) echo i386-ibm-aix exit ;; ia64:AIX:*:*) if [ -x /usr/bin/oslevel ] ; then IBM_REV=`/usr/bin/oslevel` else IBM_REV=${UNAME_VERSION}.${UNAME_RELEASE} fi echo ${UNAME_MACHINE}-ibm-aix${IBM_REV} exit ;; *:AIX:2:3) if grep bos325 /usr/include/stdio.h >/dev/null 2>&1; then eval $set_cc_for_build sed 's/^ //' << EOF >$dummy.c #include main() { if (!__power_pc()) exit(1); puts("powerpc-ibm-aix3.2.5"); exit(0); } EOF if $CC_FOR_BUILD -o $dummy $dummy.c && SYSTEM_NAME=`$dummy` then echo "$SYSTEM_NAME" else echo rs6000-ibm-aix3.2.5 fi elif grep bos324 /usr/include/stdio.h >/dev/null 2>&1; then echo rs6000-ibm-aix3.2.4 else echo rs6000-ibm-aix3.2 fi exit ;; *:AIX:*:[4567]) IBM_CPU_ID=`/usr/sbin/lsdev -C -c processor -S available | sed 1q | awk '{ print $1 }'` if /usr/sbin/lsattr -El ${IBM_CPU_ID} | grep ' POWER' >/dev/null 2>&1; then IBM_ARCH=rs6000 else IBM_ARCH=powerpc fi if [ -x /usr/bin/oslevel ] ; then IBM_REV=`/usr/bin/oslevel` else IBM_REV=${UNAME_VERSION}.${UNAME_RELEASE} fi echo ${IBM_ARCH}-ibm-aix${IBM_REV} exit ;; *:AIX:*:*) echo rs6000-ibm-aix exit ;; ibmrt:4.4BSD:*|romp-ibm:BSD:*) echo romp-ibm-bsd4.4 exit ;; ibmrt:*BSD:*|romp-ibm:BSD:*) # covers RT/PC BSD and echo romp-ibm-bsd${UNAME_RELEASE} # 4.3 with uname added to exit ;; # report: romp-ibm BSD 4.3 *:BOSX:*:*) echo rs6000-bull-bosx exit ;; DPX/2?00:B.O.S.:*:*) echo m68k-bull-sysv3 exit ;; 9000/[34]??:4.3bsd:1.*:*) echo m68k-hp-bsd exit ;; hp300:4.4BSD:*:* | 9000/[34]??:4.3bsd:2.*:*) echo m68k-hp-bsd4.4 exit ;; 9000/[34678]??:HP-UX:*:*) HPUX_REV=`echo ${UNAME_RELEASE}|sed -e 's/[^.]*.[0B]*//'` case "${UNAME_MACHINE}" in 9000/31? ) HP_ARCH=m68000 ;; 9000/[34]?? ) HP_ARCH=m68k ;; 9000/[678][0-9][0-9]) if [ -x /usr/bin/getconf ]; then sc_cpu_version=`/usr/bin/getconf SC_CPU_VERSION 2>/dev/null` sc_kernel_bits=`/usr/bin/getconf SC_KERNEL_BITS 2>/dev/null` case "${sc_cpu_version}" in 523) HP_ARCH="hppa1.0" ;; # CPU_PA_RISC1_0 528) HP_ARCH="hppa1.1" ;; # CPU_PA_RISC1_1 532) # CPU_PA_RISC2_0 case "${sc_kernel_bits}" in 32) HP_ARCH="hppa2.0n" ;; 64) HP_ARCH="hppa2.0w" ;; '') HP_ARCH="hppa2.0" ;; # HP-UX 10.20 esac ;; esac fi if [ "${HP_ARCH}" = "" ]; then eval $set_cc_for_build sed 's/^ //' << EOF >$dummy.c #define _HPUX_SOURCE #include #include int main () { #if defined(_SC_KERNEL_BITS) long bits = sysconf(_SC_KERNEL_BITS); #endif long cpu = sysconf (_SC_CPU_VERSION); switch (cpu) { case CPU_PA_RISC1_0: puts ("hppa1.0"); break; case CPU_PA_RISC1_1: puts ("hppa1.1"); break; case CPU_PA_RISC2_0: #if defined(_SC_KERNEL_BITS) switch (bits) { case 64: puts ("hppa2.0w"); break; case 32: puts ("hppa2.0n"); break; default: puts ("hppa2.0"); break; } break; #else /* !defined(_SC_KERNEL_BITS) */ puts ("hppa2.0"); break; #endif default: puts ("hppa1.0"); break; } exit (0); } EOF (CCOPTS= $CC_FOR_BUILD -o $dummy $dummy.c 2>/dev/null) && HP_ARCH=`$dummy` test -z "$HP_ARCH" && HP_ARCH=hppa fi ;; esac if [ ${HP_ARCH} = "hppa2.0w" ] then eval $set_cc_for_build # hppa2.0w-hp-hpux* has a 64-bit kernel and a compiler generating # 32-bit code. hppa64-hp-hpux* has the same kernel and a compiler # generating 64-bit code. GNU and HP use different nomenclature: # # $ CC_FOR_BUILD=cc ./config.guess # => hppa2.0w-hp-hpux11.23 # $ CC_FOR_BUILD="cc +DA2.0w" ./config.guess # => hppa64-hp-hpux11.23 if echo __LP64__ | (CCOPTS= $CC_FOR_BUILD -E - 2>/dev/null) | grep -q __LP64__ then HP_ARCH="hppa2.0w" else HP_ARCH="hppa64" fi fi echo ${HP_ARCH}-hp-hpux${HPUX_REV} exit ;; ia64:HP-UX:*:*) HPUX_REV=`echo ${UNAME_RELEASE}|sed -e 's/[^.]*.[0B]*//'` echo ia64-hp-hpux${HPUX_REV} exit ;; 3050*:HI-UX:*:*) eval $set_cc_for_build sed 's/^ //' << EOF >$dummy.c #include int main () { long cpu = sysconf (_SC_CPU_VERSION); /* The order matters, because CPU_IS_HP_MC68K erroneously returns true for CPU_PA_RISC1_0. CPU_IS_PA_RISC returns correct results, however. */ if (CPU_IS_PA_RISC (cpu)) { switch (cpu) { case CPU_PA_RISC1_0: puts ("hppa1.0-hitachi-hiuxwe2"); break; case CPU_PA_RISC1_1: puts ("hppa1.1-hitachi-hiuxwe2"); break; case CPU_PA_RISC2_0: puts ("hppa2.0-hitachi-hiuxwe2"); break; default: puts ("hppa-hitachi-hiuxwe2"); break; } } else if (CPU_IS_HP_MC68K (cpu)) puts ("m68k-hitachi-hiuxwe2"); else puts ("unknown-hitachi-hiuxwe2"); exit (0); } EOF $CC_FOR_BUILD -o $dummy $dummy.c && SYSTEM_NAME=`$dummy` && { echo "$SYSTEM_NAME"; exit; } echo unknown-hitachi-hiuxwe2 exit ;; 9000/7??:4.3bsd:*:* | 9000/8?[79]:4.3bsd:*:* ) echo hppa1.1-hp-bsd exit ;; 9000/8??:4.3bsd:*:*) echo hppa1.0-hp-bsd exit ;; *9??*:MPE/iX:*:* | *3000*:MPE/iX:*:*) echo hppa1.0-hp-mpeix exit ;; hp7??:OSF1:*:* | hp8?[79]:OSF1:*:* ) echo hppa1.1-hp-osf exit ;; hp8??:OSF1:*:*) echo hppa1.0-hp-osf exit ;; i*86:OSF1:*:*) if [ -x /usr/sbin/sysversion ] ; then echo ${UNAME_MACHINE}-unknown-osf1mk else echo ${UNAME_MACHINE}-unknown-osf1 fi exit ;; parisc*:Lites*:*:*) echo hppa1.1-hp-lites exit ;; C1*:ConvexOS:*:* | convex:ConvexOS:C1*:*) echo c1-convex-bsd exit ;; C2*:ConvexOS:*:* | convex:ConvexOS:C2*:*) if getsysinfo -f scalar_acc then echo c32-convex-bsd else echo c2-convex-bsd fi exit ;; C34*:ConvexOS:*:* | convex:ConvexOS:C34*:*) echo c34-convex-bsd exit ;; C38*:ConvexOS:*:* | convex:ConvexOS:C38*:*) echo c38-convex-bsd exit ;; C4*:ConvexOS:*:* | convex:ConvexOS:C4*:*) echo c4-convex-bsd exit ;; CRAY*Y-MP:*:*:*) echo ymp-cray-unicos${UNAME_RELEASE} | sed -e 's/\.[^.]*$/.X/' exit ;; CRAY*[A-Z]90:*:*:*) echo ${UNAME_MACHINE}-cray-unicos${UNAME_RELEASE} \ | sed -e 's/CRAY.*\([A-Z]90\)/\1/' \ -e y/ABCDEFGHIJKLMNOPQRSTUVWXYZ/abcdefghijklmnopqrstuvwxyz/ \ -e 's/\.[^.]*$/.X/' exit ;; CRAY*TS:*:*:*) echo t90-cray-unicos${UNAME_RELEASE} | sed -e 's/\.[^.]*$/.X/' exit ;; CRAY*T3E:*:*:*) echo alphaev5-cray-unicosmk${UNAME_RELEASE} | sed -e 's/\.[^.]*$/.X/' exit ;; CRAY*SV1:*:*:*) echo sv1-cray-unicos${UNAME_RELEASE} | sed -e 's/\.[^.]*$/.X/' exit ;; *:UNICOS/mp:*:*) echo craynv-cray-unicosmp${UNAME_RELEASE} | sed -e 's/\.[^.]*$/.X/' exit ;; F30[01]:UNIX_System_V:*:* | F700:UNIX_System_V:*:*) FUJITSU_PROC=`uname -m | tr 'ABCDEFGHIJKLMNOPQRSTUVWXYZ' 'abcdefghijklmnopqrstuvwxyz'` FUJITSU_SYS=`uname -p | tr 'ABCDEFGHIJKLMNOPQRSTUVWXYZ' 'abcdefghijklmnopqrstuvwxyz' | sed -e 's/\///'` FUJITSU_REL=`echo ${UNAME_RELEASE} | sed -e 's/ /_/'` echo "${FUJITSU_PROC}-fujitsu-${FUJITSU_SYS}${FUJITSU_REL}" exit ;; 5000:UNIX_System_V:4.*:*) FUJITSU_SYS=`uname -p | tr 'ABCDEFGHIJKLMNOPQRSTUVWXYZ' 'abcdefghijklmnopqrstuvwxyz' | sed -e 's/\///'` FUJITSU_REL=`echo ${UNAME_RELEASE} | tr 'ABCDEFGHIJKLMNOPQRSTUVWXYZ' 'abcdefghijklmnopqrstuvwxyz' | sed -e 's/ /_/'` echo "sparc-fujitsu-${FUJITSU_SYS}${FUJITSU_REL}" exit ;; i*86:BSD/386:*:* | i*86:BSD/OS:*:* | *:Ascend\ Embedded/OS:*:*) echo ${UNAME_MACHINE}-pc-bsdi${UNAME_RELEASE} exit ;; sparc*:BSD/OS:*:*) echo sparc-unknown-bsdi${UNAME_RELEASE} exit ;; *:BSD/OS:*:*) echo ${UNAME_MACHINE}-unknown-bsdi${UNAME_RELEASE} exit ;; *:FreeBSD:*:*) UNAME_PROCESSOR=`/usr/bin/uname -p` case ${UNAME_PROCESSOR} in amd64) echo x86_64-unknown-freebsd`echo ${UNAME_RELEASE}|sed -e 's/[-(].*//'` ;; *) echo ${UNAME_PROCESSOR}-unknown-freebsd`echo ${UNAME_RELEASE}|sed -e 's/[-(].*//'` ;; esac exit ;; i*:CYGWIN*:*) echo ${UNAME_MACHINE}-pc-cygwin exit ;; *:MINGW64*:*) echo ${UNAME_MACHINE}-pc-mingw64 exit ;; *:MINGW*:*) echo ${UNAME_MACHINE}-pc-mingw32 exit ;; i*:MSYS*:*) echo ${UNAME_MACHINE}-pc-msys exit ;; i*:windows32*:*) # uname -m includes "-pc" on this system. echo ${UNAME_MACHINE}-mingw32 exit ;; i*:PW*:*) echo ${UNAME_MACHINE}-pc-pw32 exit ;; *:Interix*:*) case ${UNAME_MACHINE} in x86) echo i586-pc-interix${UNAME_RELEASE} exit ;; authenticamd | genuineintel | EM64T) echo x86_64-unknown-interix${UNAME_RELEASE} exit ;; IA64) echo ia64-unknown-interix${UNAME_RELEASE} exit ;; esac ;; [345]86:Windows_95:* | [345]86:Windows_98:* | [345]86:Windows_NT:*) echo i${UNAME_MACHINE}-pc-mks exit ;; 8664:Windows_NT:*) echo x86_64-pc-mks exit ;; i*:Windows_NT*:* | Pentium*:Windows_NT*:*) # How do we know it's Interix rather than the generic POSIX subsystem? # It also conflicts with pre-2.0 versions of AT&T UWIN. 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EV56) UNAME_MACHINE=alphaev56 ;; PCA56) UNAME_MACHINE=alphapca56 ;; PCA57) UNAME_MACHINE=alphapca56 ;; EV6) UNAME_MACHINE=alphaev6 ;; EV67) UNAME_MACHINE=alphaev67 ;; EV68*) UNAME_MACHINE=alphaev68 ;; esac objdump --private-headers /bin/sh | grep -q ld.so.1 if test "$?" = 0 ; then LIBC="gnulibc1" ; fi echo ${UNAME_MACHINE}-unknown-linux-${LIBC} exit ;; arc:Linux:*:* | arceb:Linux:*:*) echo ${UNAME_MACHINE}-unknown-linux-${LIBC} exit ;; arm*:Linux:*:*) eval $set_cc_for_build if echo __ARM_EABI__ | $CC_FOR_BUILD -E - 2>/dev/null \ | grep -q __ARM_EABI__ then echo ${UNAME_MACHINE}-unknown-linux-${LIBC} else if echo __ARM_PCS_VFP | $CC_FOR_BUILD -E - 2>/dev/null \ | grep -q __ARM_PCS_VFP then echo ${UNAME_MACHINE}-unknown-linux-${LIBC}eabi else echo ${UNAME_MACHINE}-unknown-linux-${LIBC}eabihf fi fi exit ;; avr32*:Linux:*:*) echo ${UNAME_MACHINE}-unknown-linux-${LIBC} exit ;; cris:Linux:*:*) echo ${UNAME_MACHINE}-axis-linux-${LIBC} exit ;; crisv32:Linux:*:*) echo ${UNAME_MACHINE}-axis-linux-${LIBC} exit ;; frv:Linux:*:*) echo ${UNAME_MACHINE}-unknown-linux-${LIBC} exit ;; hexagon:Linux:*:*) echo ${UNAME_MACHINE}-unknown-linux-${LIBC} exit ;; i*86:Linux:*:*) echo ${UNAME_MACHINE}-pc-linux-${LIBC} exit ;; ia64:Linux:*:*) echo ${UNAME_MACHINE}-unknown-linux-${LIBC} exit ;; m32r*:Linux:*:*) echo ${UNAME_MACHINE}-unknown-linux-${LIBC} exit ;; m68*:Linux:*:*) echo ${UNAME_MACHINE}-unknown-linux-${LIBC} exit ;; mips:Linux:*:* | mips64:Linux:*:*) eval $set_cc_for_build sed 's/^ //' << EOF >$dummy.c #undef CPU #undef ${UNAME_MACHINE} #undef ${UNAME_MACHINE}el #if defined(__MIPSEL__) || defined(__MIPSEL) || defined(_MIPSEL) || defined(MIPSEL) CPU=${UNAME_MACHINE}el #else #if defined(__MIPSEB__) || defined(__MIPSEB) || defined(_MIPSEB) || defined(MIPSEB) CPU=${UNAME_MACHINE} #else CPU= #endif #endif EOF eval `$CC_FOR_BUILD -E $dummy.c 2>/dev/null | grep '^CPU'` test x"${CPU}" != x && { echo "${CPU}-unknown-linux-${LIBC}"; exit; } ;; or1k:Linux:*:*) echo ${UNAME_MACHINE}-unknown-linux-${LIBC} exit ;; or32:Linux:*:*) echo ${UNAME_MACHINE}-unknown-linux-${LIBC} exit ;; padre:Linux:*:*) echo sparc-unknown-linux-${LIBC} exit ;; parisc64:Linux:*:* | hppa64:Linux:*:*) echo hppa64-unknown-linux-${LIBC} exit ;; parisc:Linux:*:* | hppa:Linux:*:*) # Look for CPU level case `grep '^cpu[^a-z]*:' /proc/cpuinfo 2>/dev/null | cut -d' ' -f2` in PA7*) echo hppa1.1-unknown-linux-${LIBC} ;; PA8*) echo hppa2.0-unknown-linux-${LIBC} ;; *) echo hppa-unknown-linux-${LIBC} ;; esac exit ;; ppc64:Linux:*:*) echo powerpc64-unknown-linux-${LIBC} exit ;; ppc:Linux:*:*) echo powerpc-unknown-linux-${LIBC} exit ;; ppc64le:Linux:*:*) echo powerpc64le-unknown-linux-${LIBC} exit ;; ppcle:Linux:*:*) echo powerpcle-unknown-linux-${LIBC} exit ;; s390:Linux:*:* | s390x:Linux:*:*) echo ${UNAME_MACHINE}-ibm-linux-${LIBC} exit ;; sh64*:Linux:*:*) echo ${UNAME_MACHINE}-unknown-linux-${LIBC} exit ;; sh*:Linux:*:*) echo ${UNAME_MACHINE}-unknown-linux-${LIBC} exit ;; sparc:Linux:*:* | sparc64:Linux:*:*) echo ${UNAME_MACHINE}-unknown-linux-${LIBC} exit ;; tile*:Linux:*:*) echo ${UNAME_MACHINE}-unknown-linux-${LIBC} exit ;; vax:Linux:*:*) echo ${UNAME_MACHINE}-dec-linux-${LIBC} exit ;; x86_64:Linux:*:*) echo ${UNAME_MACHINE}-unknown-linux-${LIBC} exit ;; xtensa*:Linux:*:*) echo ${UNAME_MACHINE}-unknown-linux-${LIBC} exit ;; i*86:DYNIX/ptx:4*:*) # ptx 4.0 does uname -s correctly, with DYNIX/ptx in there. # earlier versions are messed up and put the nodename in both # sysname and nodename. echo i386-sequent-sysv4 exit ;; i*86:UNIX_SV:4.2MP:2.*) # Unixware is an offshoot of SVR4, but it has its own version # number series starting with 2... # I am not positive that other SVR4 systems won't match this, # I just have to hope. -- rms. # Use sysv4.2uw... so that sysv4* matches it. echo ${UNAME_MACHINE}-pc-sysv4.2uw${UNAME_VERSION} exit ;; i*86:OS/2:*:*) # If we were able to find `uname', then EMX Unix compatibility # is probably installed. echo ${UNAME_MACHINE}-pc-os2-emx exit ;; i*86:XTS-300:*:STOP) echo ${UNAME_MACHINE}-unknown-stop exit ;; i*86:atheos:*:*) echo ${UNAME_MACHINE}-unknown-atheos exit ;; i*86:syllable:*:*) echo ${UNAME_MACHINE}-pc-syllable exit ;; i*86:LynxOS:2.*:* | i*86:LynxOS:3.[01]*:* | i*86:LynxOS:4.[02]*:*) echo i386-unknown-lynxos${UNAME_RELEASE} exit ;; i*86:*DOS:*:*) echo ${UNAME_MACHINE}-pc-msdosdjgpp exit ;; i*86:*:4.*:* | i*86:SYSTEM_V:4.*:*) UNAME_REL=`echo ${UNAME_RELEASE} | sed 's/\/MP$//'` if grep Novell /usr/include/link.h >/dev/null 2>/dev/null; then echo ${UNAME_MACHINE}-univel-sysv${UNAME_REL} else echo ${UNAME_MACHINE}-pc-sysv${UNAME_REL} fi exit ;; i*86:*:5:[678]*) # UnixWare 7.x, OpenUNIX and OpenServer 6. case `/bin/uname -X | grep "^Machine"` in *486*) UNAME_MACHINE=i486 ;; *Pentium) UNAME_MACHINE=i586 ;; *Pent*|*Celeron) UNAME_MACHINE=i686 ;; esac echo ${UNAME_MACHINE}-unknown-sysv${UNAME_RELEASE}${UNAME_SYSTEM}${UNAME_VERSION} exit ;; i*86:*:3.2:*) if test -f /usr/options/cb.name; then UNAME_REL=`sed -n 's/.*Version //p' /dev/null >/dev/null ; then UNAME_REL=`(/bin/uname -X|grep Release|sed -e 's/.*= //')` (/bin/uname -X|grep i80486 >/dev/null) && UNAME_MACHINE=i486 (/bin/uname -X|grep '^Machine.*Pentium' >/dev/null) \ && UNAME_MACHINE=i586 (/bin/uname -X|grep '^Machine.*Pent *II' >/dev/null) \ && UNAME_MACHINE=i686 (/bin/uname -X|grep '^Machine.*Pentium Pro' >/dev/null) \ && UNAME_MACHINE=i686 echo ${UNAME_MACHINE}-pc-sco$UNAME_REL else echo ${UNAME_MACHINE}-pc-sysv32 fi exit ;; pc:*:*:*) # Left here for compatibility: # uname -m prints for DJGPP always 'pc', but it prints nothing about # the processor, so we play safe by assuming i586. # Note: whatever this is, it MUST be the same as what config.sub # prints for the "djgpp" host, or else GDB configury will decide that # this is a cross-build. echo i586-pc-msdosdjgpp exit ;; Intel:Mach:3*:*) echo i386-pc-mach3 exit ;; paragon:*:*:*) echo i860-intel-osf1 exit ;; i860:*:4.*:*) # i860-SVR4 if grep Stardent /usr/include/sys/uadmin.h >/dev/null 2>&1 ; then echo i860-stardent-sysv${UNAME_RELEASE} # Stardent Vistra i860-SVR4 else # Add other i860-SVR4 vendors below as they are discovered. echo i860-unknown-sysv${UNAME_RELEASE} # Unknown i860-SVR4 fi exit ;; mini*:CTIX:SYS*5:*) # "miniframe" echo m68010-convergent-sysv exit ;; mc68k:UNIX:SYSTEM5:3.51m) echo m68k-convergent-sysv exit ;; M680?0:D-NIX:5.3:*) echo m68k-diab-dnix exit ;; M68*:*:R3V[5678]*:*) test -r /sysV68 && { echo 'm68k-motorola-sysv'; exit; } ;; 3[345]??:*:4.0:3.0 | 3[34]??A:*:4.0:3.0 | 3[34]??,*:*:4.0:3.0 | 3[34]??/*:*:4.0:3.0 | 4400:*:4.0:3.0 | 4850:*:4.0:3.0 | SKA40:*:4.0:3.0 | SDS2:*:4.0:3.0 | SHG2:*:4.0:3.0 | S7501*:*:4.0:3.0) OS_REL='' test -r /etc/.relid \ && OS_REL=.`sed -n 's/[^ ]* [^ ]* \([0-9][0-9]\).*/\1/p' < /etc/.relid` /bin/uname -p 2>/dev/null | grep 86 >/dev/null \ && { echo i486-ncr-sysv4.3${OS_REL}; exit; } /bin/uname -p 2>/dev/null | /bin/grep entium >/dev/null \ && { echo i586-ncr-sysv4.3${OS_REL}; exit; } ;; 3[34]??:*:4.0:* | 3[34]??,*:*:4.0:*) /bin/uname -p 2>/dev/null | grep 86 >/dev/null \ && { echo i486-ncr-sysv4; exit; } ;; NCR*:*:4.2:* | MPRAS*:*:4.2:*) OS_REL='.3' test -r /etc/.relid \ && OS_REL=.`sed -n 's/[^ ]* [^ ]* \([0-9][0-9]\).*/\1/p' < /etc/.relid` /bin/uname -p 2>/dev/null | grep 86 >/dev/null \ && { echo i486-ncr-sysv4.3${OS_REL}; exit; } /bin/uname -p 2>/dev/null | /bin/grep entium >/dev/null \ && { echo i586-ncr-sysv4.3${OS_REL}; exit; } /bin/uname -p 2>/dev/null | /bin/grep pteron >/dev/null \ && { echo i586-ncr-sysv4.3${OS_REL}; exit; } ;; m68*:LynxOS:2.*:* | m68*:LynxOS:3.0*:*) echo m68k-unknown-lynxos${UNAME_RELEASE} exit ;; mc68030:UNIX_System_V:4.*:*) echo m68k-atari-sysv4 exit ;; TSUNAMI:LynxOS:2.*:*) echo sparc-unknown-lynxos${UNAME_RELEASE} exit ;; rs6000:LynxOS:2.*:*) echo rs6000-unknown-lynxos${UNAME_RELEASE} exit ;; PowerPC:LynxOS:2.*:* | PowerPC:LynxOS:3.[01]*:* | PowerPC:LynxOS:4.[02]*:*) echo powerpc-unknown-lynxos${UNAME_RELEASE} exit ;; SM[BE]S:UNIX_SV:*:*) echo mips-dde-sysv${UNAME_RELEASE} exit ;; RM*:ReliantUNIX-*:*:*) echo mips-sni-sysv4 exit ;; RM*:SINIX-*:*:*) echo mips-sni-sysv4 exit ;; *:SINIX-*:*:*) if uname -p 2>/dev/null >/dev/null ; then UNAME_MACHINE=`(uname -p) 2>/dev/null` echo ${UNAME_MACHINE}-sni-sysv4 else echo ns32k-sni-sysv fi exit ;; PENTIUM:*:4.0*:*) # Unisys `ClearPath HMP IX 4000' SVR4/MP effort # says echo i586-unisys-sysv4 exit ;; *:UNIX_System_V:4*:FTX*) # From Gerald Hewes . # How about differentiating between stratus architectures? -djm echo hppa1.1-stratus-sysv4 exit ;; *:*:*:FTX*) # From seanf@swdc.stratus.com. echo i860-stratus-sysv4 exit ;; i*86:VOS:*:*) # From Paul.Green@stratus.com. echo ${UNAME_MACHINE}-stratus-vos exit ;; *:VOS:*:*) # From Paul.Green@stratus.com. echo hppa1.1-stratus-vos exit ;; mc68*:A/UX:*:*) echo m68k-apple-aux${UNAME_RELEASE} exit ;; news*:NEWS-OS:6*:*) echo mips-sony-newsos6 exit ;; R[34]000:*System_V*:*:* | R4000:UNIX_SYSV:*:* | R*000:UNIX_SV:*:*) if [ -d /usr/nec ]; then echo mips-nec-sysv${UNAME_RELEASE} else echo mips-unknown-sysv${UNAME_RELEASE} fi exit ;; BeBox:BeOS:*:*) # BeOS running on hardware made by Be, PPC only. echo powerpc-be-beos exit ;; BeMac:BeOS:*:*) # BeOS running on Mac or Mac clone, PPC only. echo powerpc-apple-beos exit ;; BePC:BeOS:*:*) # BeOS running on Intel PC compatible. echo i586-pc-beos exit ;; BePC:Haiku:*:*) # Haiku running on Intel PC compatible. echo i586-pc-haiku exit ;; x86_64:Haiku:*:*) echo x86_64-unknown-haiku exit ;; SX-4:SUPER-UX:*:*) echo sx4-nec-superux${UNAME_RELEASE} exit ;; SX-5:SUPER-UX:*:*) echo sx5-nec-superux${UNAME_RELEASE} exit ;; SX-6:SUPER-UX:*:*) echo sx6-nec-superux${UNAME_RELEASE} exit ;; SX-7:SUPER-UX:*:*) echo sx7-nec-superux${UNAME_RELEASE} exit ;; SX-8:SUPER-UX:*:*) echo sx8-nec-superux${UNAME_RELEASE} exit ;; SX-8R:SUPER-UX:*:*) echo sx8r-nec-superux${UNAME_RELEASE} exit ;; Power*:Rhapsody:*:*) echo powerpc-apple-rhapsody${UNAME_RELEASE} exit ;; *:Rhapsody:*:*) echo ${UNAME_MACHINE}-apple-rhapsody${UNAME_RELEASE} exit ;; *:Darwin:*:*) UNAME_PROCESSOR=`uname -p` || UNAME_PROCESSOR=unknown eval $set_cc_for_build if test "$UNAME_PROCESSOR" = unknown ; then UNAME_PROCESSOR=powerpc fi if test `echo "$UNAME_RELEASE" | sed -e 's/\..*//'` -le 10 ; then if [ "$CC_FOR_BUILD" != 'no_compiler_found' ]; then if (echo '#ifdef __LP64__'; echo IS_64BIT_ARCH; echo '#endif') | \ (CCOPTS= $CC_FOR_BUILD -E - 2>/dev/null) | \ grep IS_64BIT_ARCH >/dev/null then case $UNAME_PROCESSOR in i386) UNAME_PROCESSOR=x86_64 ;; powerpc) UNAME_PROCESSOR=powerpc64 ;; esac fi fi elif test "$UNAME_PROCESSOR" = i386 ; then # Avoid executing cc on OS X 10.9, as it ships with a stub # that puts up a graphical alert prompting to install # developer tools. Any system running Mac OS X 10.7 or # later (Darwin 11 and later) is required to have a 64-bit # processor. This is not true of the ARM version of Darwin # that Apple uses in portable devices. UNAME_PROCESSOR=x86_64 fi echo ${UNAME_PROCESSOR}-apple-darwin${UNAME_RELEASE} exit ;; *:procnto*:*:* | *:QNX:[0123456789]*:*) UNAME_PROCESSOR=`uname -p` if test "$UNAME_PROCESSOR" = "x86"; then UNAME_PROCESSOR=i386 UNAME_MACHINE=pc fi echo ${UNAME_PROCESSOR}-${UNAME_MACHINE}-nto-qnx${UNAME_RELEASE} exit ;; *:QNX:*:4*) echo i386-pc-qnx exit ;; NEO-?:NONSTOP_KERNEL:*:*) echo neo-tandem-nsk${UNAME_RELEASE} exit ;; NSE-*:NONSTOP_KERNEL:*:*) echo nse-tandem-nsk${UNAME_RELEASE} exit ;; NSR-?:NONSTOP_KERNEL:*:*) echo nsr-tandem-nsk${UNAME_RELEASE} exit ;; *:NonStop-UX:*:*) echo mips-compaq-nonstopux exit ;; BS2000:POSIX*:*:*) echo bs2000-siemens-sysv exit ;; DS/*:UNIX_System_V:*:*) echo ${UNAME_MACHINE}-${UNAME_SYSTEM}-${UNAME_RELEASE} exit ;; *:Plan9:*:*) # "uname -m" is not consistent, so use $cputype instead. 386 # is converted to i386 for consistency with other x86 # operating systems. if test "$cputype" = "386"; then UNAME_MACHINE=i386 else UNAME_MACHINE="$cputype" fi echo ${UNAME_MACHINE}-unknown-plan9 exit ;; *:TOPS-10:*:*) echo pdp10-unknown-tops10 exit ;; *:TENEX:*:*) echo pdp10-unknown-tenex exit ;; KS10:TOPS-20:*:* | KL10:TOPS-20:*:* | TYPE4:TOPS-20:*:*) echo pdp10-dec-tops20 exit ;; XKL-1:TOPS-20:*:* | TYPE5:TOPS-20:*:*) echo pdp10-xkl-tops20 exit ;; *:TOPS-20:*:*) echo pdp10-unknown-tops20 exit ;; *:ITS:*:*) echo pdp10-unknown-its exit ;; SEI:*:*:SEIUX) echo mips-sei-seiux${UNAME_RELEASE} exit ;; *:DragonFly:*:*) echo ${UNAME_MACHINE}-unknown-dragonfly`echo ${UNAME_RELEASE}|sed -e 's/[-(].*//'` exit ;; *:*VMS:*:*) UNAME_MACHINE=`(uname -p) 2>/dev/null` case "${UNAME_MACHINE}" in A*) echo alpha-dec-vms ; exit ;; I*) echo ia64-dec-vms ; exit ;; V*) echo vax-dec-vms ; exit ;; esac ;; *:XENIX:*:SysV) echo i386-pc-xenix exit ;; i*86:skyos:*:*) echo ${UNAME_MACHINE}-pc-skyos`echo ${UNAME_RELEASE}` | sed -e 's/ .*$//' exit ;; i*86:rdos:*:*) echo ${UNAME_MACHINE}-pc-rdos exit ;; i*86:AROS:*:*) echo ${UNAME_MACHINE}-pc-aros exit ;; x86_64:VMkernel:*:*) echo ${UNAME_MACHINE}-unknown-esx exit ;; esac eval $set_cc_for_build cat >$dummy.c < # include #endif main () { #if defined (sony) #if defined (MIPSEB) /* BFD wants "bsd" instead of "newsos". Perhaps BFD should be changed, I don't know.... */ printf ("mips-sony-bsd\n"); exit (0); #else #include printf ("m68k-sony-newsos%s\n", #ifdef NEWSOS4 "4" #else "" #endif ); exit (0); #endif #endif #if defined (__arm) && defined (__acorn) && defined (__unix) printf ("arm-acorn-riscix\n"); exit (0); #endif #if defined (hp300) && !defined (hpux) printf ("m68k-hp-bsd\n"); exit (0); #endif #if defined (NeXT) #if !defined (__ARCHITECTURE__) #define __ARCHITECTURE__ "m68k" #endif int version; version=`(hostinfo | sed -n 's/.*NeXT Mach \([0-9]*\).*/\1/p') 2>/dev/null`; if (version < 4) printf ("%s-next-nextstep%d\n", __ARCHITECTURE__, version); else printf ("%s-next-openstep%d\n", __ARCHITECTURE__, version); exit (0); #endif #if defined (MULTIMAX) || defined (n16) #if defined (UMAXV) printf ("ns32k-encore-sysv\n"); exit (0); #else #if defined (CMU) printf ("ns32k-encore-mach\n"); exit (0); #else printf ("ns32k-encore-bsd\n"); exit (0); #endif #endif #endif #if defined (__386BSD__) printf ("i386-pc-bsd\n"); exit (0); #endif #if defined (sequent) #if defined (i386) printf ("i386-sequent-dynix\n"); exit (0); #endif #if defined (ns32000) printf ("ns32k-sequent-dynix\n"); exit (0); #endif #endif #if defined (_SEQUENT_) struct utsname un; uname(&un); if (strncmp(un.version, "V2", 2) == 0) { printf ("i386-sequent-ptx2\n"); exit (0); } if (strncmp(un.version, "V1", 2) == 0) { /* XXX is V1 correct? */ printf ("i386-sequent-ptx1\n"); exit (0); } printf ("i386-sequent-ptx\n"); exit (0); #endif #if defined (vax) # if !defined (ultrix) # include # if defined (BSD) # if BSD == 43 printf ("vax-dec-bsd4.3\n"); exit (0); # else # if BSD == 199006 printf ("vax-dec-bsd4.3reno\n"); exit (0); # else printf ("vax-dec-bsd\n"); exit (0); # endif # endif # else printf ("vax-dec-bsd\n"); exit (0); # endif # else printf ("vax-dec-ultrix\n"); exit (0); # endif #endif #if defined (alliant) && defined (i860) printf ("i860-alliant-bsd\n"); exit (0); #endif exit (1); } EOF $CC_FOR_BUILD -o $dummy $dummy.c 2>/dev/null && SYSTEM_NAME=`$dummy` && { echo "$SYSTEM_NAME"; exit; } # Apollos put the system type in the environment. test -d /usr/apollo && { echo ${ISP}-apollo-${SYSTYPE}; exit; } # Convex versions that predate uname can use getsysinfo(1) if [ -x /usr/convex/getsysinfo ] then case `getsysinfo -f cpu_type` in c1*) echo c1-convex-bsd exit ;; c2*) if getsysinfo -f scalar_acc then echo c32-convex-bsd else echo c2-convex-bsd fi exit ;; c34*) echo c34-convex-bsd exit ;; c38*) echo c38-convex-bsd exit ;; c4*) echo c4-convex-bsd exit ;; esac fi cat >&2 < in order to provide the needed information to handle your system. config.guess timestamp = $timestamp uname -m = `(uname -m) 2>/dev/null || echo unknown` uname -r = `(uname -r) 2>/dev/null || echo unknown` uname -s = `(uname -s) 2>/dev/null || echo unknown` uname -v = `(uname -v) 2>/dev/null || echo unknown` /usr/bin/uname -p = `(/usr/bin/uname -p) 2>/dev/null` /bin/uname -X = `(/bin/uname -X) 2>/dev/null` hostinfo = `(hostinfo) 2>/dev/null` /bin/universe = `(/bin/universe) 2>/dev/null` /usr/bin/arch -k = `(/usr/bin/arch -k) 2>/dev/null` /bin/arch = `(/bin/arch) 2>/dev/null` /usr/bin/oslevel = `(/usr/bin/oslevel) 2>/dev/null` /usr/convex/getsysinfo = `(/usr/convex/getsysinfo) 2>/dev/null` UNAME_MACHINE = ${UNAME_MACHINE} UNAME_RELEASE = ${UNAME_RELEASE} UNAME_SYSTEM = ${UNAME_SYSTEM} UNAME_VERSION = ${UNAME_VERSION} EOF exit 1 # Local variables: # eval: (add-hook 'write-file-hooks 'time-stamp) # time-stamp-start: "timestamp='" # time-stamp-format: "%:y-%02m-%02d" # time-stamp-end: "'" # End: pal-0.5.0/config.h.in000644 000765 000024 00000004005 12366007540 014423 0ustar00timjstaff000000 000000 /* config.h.in. Generated from configure.ac by autoheader. */ /* Define to 1 if you have the `copysign' function. */ #undef HAVE_COPYSIGN /* Define to 1 if you have the header file. */ #undef HAVE_DLFCN_H /* Define to 1 if you have the header file. */ #undef HAVE_INTTYPES_H /* Define to 1 if you have the `isblank' function. */ #undef HAVE_ISBLANK /* Define to 1 if you have the `m' library (-lm). */ #undef HAVE_LIBM /* Define to 1 if you have the header file. */ #undef HAVE_MEMORY_H /* "Build with SOFA library" */ #undef HAVE_SOFA_H /* Define to 1 if you have the header file. */ #undef HAVE_STAR_UTIL_H /* Define to 1 if you have the header file. */ #undef HAVE_STDINT_H /* Define to 1 if you have the header file. */ #undef HAVE_STDLIB_H /* Define to 1 if you have the header file. */ #undef HAVE_STRINGS_H /* Define to 1 if you have the header file. */ #undef HAVE_STRING_H /* Define to 1 if you have the `strlcpy' function. */ #undef HAVE_STRLCPY /* Define to 1 if you have the header file. */ #undef HAVE_SYS_STAT_H /* Define to 1 if you have the header file. */ #undef HAVE_SYS_TYPES_H /* Define to 1 if you have the header file. */ #undef HAVE_UNISTD_H /* Define to the sub-directory in which libtool stores uninstalled libraries. */ #undef LT_OBJDIR /* Name of package */ #undef PACKAGE /* Define to the address where bug reports for this package should be sent. */ #undef PACKAGE_BUGREPORT /* Define to the full name of this package. */ #undef PACKAGE_NAME /* Define to the full name and version of this package. */ #undef PACKAGE_STRING /* Define to the one symbol short name of this package. */ #undef PACKAGE_TARNAME /* Define to the home page for this package. */ #undef PACKAGE_URL /* Define to the version of this package. */ #undef PACKAGE_VERSION /* Define to 1 if you have the ANSI C header files. */ #undef STDC_HEADERS /* Version number of package */ #undef VERSION pal-0.5.0/config.sub000755 000765 000024 00000105412 12363621607 014372 0ustar00timjstaff000000 000000 #! /bin/sh # Configuration validation subroutine script. # Copyright 1992-2013 Free Software Foundation, Inc. timestamp='2013-10-01' # This file is free software; you can redistribute it and/or modify it # under the terms of the GNU General Public License as published by # the Free Software Foundation; either version 3 of the License, or # (at your option) any later version. # # This program is distributed in the hope that it will be useful, but # WITHOUT ANY WARRANTY; without even the implied warranty of # MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the GNU # General Public License for more details. # # You should have received a copy of the GNU General Public License # along with this program; if not, see . # # As a special exception to the GNU General Public License, if you # distribute this file as part of a program that contains a # configuration script generated by Autoconf, you may include it under # the same distribution terms that you use for the rest of that # program. This Exception is an additional permission under section 7 # of the GNU General Public License, version 3 ("GPLv3"). # Please send patches with a ChangeLog entry to config-patches@gnu.org. # # Configuration subroutine to validate and canonicalize a configuration type. # Supply the specified configuration type as an argument. # If it is invalid, we print an error message on stderr and exit with code 1. # Otherwise, we print the canonical config type on stdout and succeed. # You can get the latest version of this script from: # http://git.savannah.gnu.org/gitweb/?p=config.git;a=blob_plain;f=config.sub;hb=HEAD # This file is supposed to be the same for all GNU packages # and recognize all the CPU types, system types and aliases # that are meaningful with *any* GNU software. # Each package is responsible for reporting which valid configurations # it does not support. The user should be able to distinguish # a failure to support a valid configuration from a meaningless # configuration. # The goal of this file is to map all the various variations of a given # machine specification into a single specification in the form: # CPU_TYPE-MANUFACTURER-OPERATING_SYSTEM # or in some cases, the newer four-part form: # CPU_TYPE-MANUFACTURER-KERNEL-OPERATING_SYSTEM # It is wrong to echo any other type of specification. me=`echo "$0" | sed -e 's,.*/,,'` usage="\ Usage: $0 [OPTION] CPU-MFR-OPSYS $0 [OPTION] ALIAS Canonicalize a configuration name. Operation modes: -h, --help print this help, then exit -t, --time-stamp print date of last modification, then exit -v, --version print version number, then exit Report bugs and patches to ." version="\ GNU config.sub ($timestamp) Copyright 1992-2013 Free Software Foundation, Inc. This is free software; see the source for copying conditions. There is NO warranty; not even for MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE." help=" Try \`$me --help' for more information." # Parse command line while test $# -gt 0 ; do case $1 in --time-stamp | --time* | -t ) echo "$timestamp" ; exit ;; --version | -v ) echo "$version" ; exit ;; --help | --h* | -h ) echo "$usage"; exit ;; -- ) # Stop option processing shift; break ;; - ) # Use stdin as input. break ;; -* ) echo "$me: invalid option $1$help" exit 1 ;; *local*) # First pass through any local machine types. echo $1 exit ;; * ) break ;; esac done case $# in 0) echo "$me: missing argument$help" >&2 exit 1;; 1) ;; *) echo "$me: too many arguments$help" >&2 exit 1;; esac # Separate what the user gave into CPU-COMPANY and OS or KERNEL-OS (if any). # Here we must recognize all the valid KERNEL-OS combinations. maybe_os=`echo $1 | sed 's/^\(.*\)-\([^-]*-[^-]*\)$/\2/'` case $maybe_os in nto-qnx* | linux-gnu* | linux-android* | linux-dietlibc | linux-newlib* | \ linux-musl* | linux-uclibc* | uclinux-uclibc* | uclinux-gnu* | kfreebsd*-gnu* | \ knetbsd*-gnu* | netbsd*-gnu* | \ kopensolaris*-gnu* | \ storm-chaos* | os2-emx* | rtmk-nova*) os=-$maybe_os basic_machine=`echo $1 | sed 's/^\(.*\)-\([^-]*-[^-]*\)$/\1/'` ;; android-linux) os=-linux-android basic_machine=`echo $1 | sed 's/^\(.*\)-\([^-]*-[^-]*\)$/\1/'`-unknown ;; *) basic_machine=`echo $1 | sed 's/-[^-]*$//'` if [ $basic_machine != $1 ] then os=`echo $1 | sed 's/.*-/-/'` else os=; fi ;; esac ### Let's recognize common machines as not being operating systems so ### that things like config.sub decstation-3100 work. We also ### recognize some manufacturers as not being operating systems, so we ### can provide default operating systems below. case $os in -sun*os*) # Prevent following clause from handling this invalid input. ;; -dec* | -mips* | -sequent* | -encore* | -pc532* | -sgi* | -sony* | \ -att* | -7300* | -3300* | -delta* | -motorola* | -sun[234]* | \ -unicom* | -ibm* | -next | -hp | -isi* | -apollo | -altos* | \ -convergent* | -ncr* | -news | -32* | -3600* | -3100* | -hitachi* |\ -c[123]* | -convex* | -sun | -crds | -omron* | -dg | -ultra | -tti* | \ -harris | -dolphin | -highlevel | -gould | -cbm | -ns | -masscomp | \ -apple | -axis | -knuth | -cray | -microblaze*) os= basic_machine=$1 ;; -bluegene*) os=-cnk ;; -sim | -cisco | -oki | -wec | -winbond) os= basic_machine=$1 ;; -scout) ;; -wrs) os=-vxworks basic_machine=$1 ;; -chorusos*) os=-chorusos basic_machine=$1 ;; -chorusrdb) os=-chorusrdb basic_machine=$1 ;; -hiux*) os=-hiuxwe2 ;; -sco6) os=-sco5v6 basic_machine=`echo $1 | sed -e 's/86-.*/86-pc/'` ;; -sco5) os=-sco3.2v5 basic_machine=`echo $1 | sed -e 's/86-.*/86-pc/'` ;; -sco4) os=-sco3.2v4 basic_machine=`echo $1 | sed -e 's/86-.*/86-pc/'` ;; -sco3.2.[4-9]*) os=`echo $os | sed -e 's/sco3.2./sco3.2v/'` basic_machine=`echo $1 | sed -e 's/86-.*/86-pc/'` ;; -sco3.2v[4-9]*) # Don't forget version if it is 3.2v4 or newer. basic_machine=`echo $1 | sed -e 's/86-.*/86-pc/'` ;; -sco5v6*) # Don't forget version if it is 3.2v4 or newer. basic_machine=`echo $1 | sed -e 's/86-.*/86-pc/'` ;; -sco*) os=-sco3.2v2 basic_machine=`echo $1 | sed -e 's/86-.*/86-pc/'` ;; -udk*) basic_machine=`echo $1 | sed -e 's/86-.*/86-pc/'` ;; -isc) os=-isc2.2 basic_machine=`echo $1 | sed -e 's/86-.*/86-pc/'` ;; -clix*) basic_machine=clipper-intergraph ;; -isc*) basic_machine=`echo $1 | sed -e 's/86-.*/86-pc/'` ;; -lynx*178) os=-lynxos178 ;; -lynx*5) os=-lynxos5 ;; -lynx*) os=-lynxos ;; -ptx*) basic_machine=`echo $1 | sed -e 's/86-.*/86-sequent/'` ;; -windowsnt*) os=`echo $os | sed -e 's/windowsnt/winnt/'` ;; -psos*) os=-psos ;; -mint | -mint[0-9]*) basic_machine=m68k-atari os=-mint ;; esac # Decode aliases for certain CPU-COMPANY combinations. case $basic_machine in # Recognize the basic CPU types without company name. # Some are omitted here because they have special meanings below. 1750a | 580 \ | a29k \ | aarch64 | aarch64_be \ | alpha | alphaev[4-8] | alphaev56 | alphaev6[78] | alphapca5[67] \ | alpha64 | alpha64ev[4-8] | alpha64ev56 | alpha64ev6[78] | alpha64pca5[67] \ | am33_2.0 \ | arc | arceb \ | arm | arm[bl]e | arme[lb] | armv[2-8] | armv[3-8][lb] | armv7[arm] \ | avr | avr32 \ | be32 | be64 \ | bfin \ | c4x | c8051 | clipper \ | d10v | d30v | dlx | dsp16xx \ | epiphany \ | fido | fr30 | frv \ | h8300 | h8500 | hppa | hppa1.[01] | hppa2.0 | hppa2.0[nw] | hppa64 \ | hexagon \ | i370 | i860 | i960 | ia64 \ | ip2k | iq2000 \ | k1om \ | le32 | le64 \ | lm32 \ | m32c | m32r | m32rle | m68000 | m68k | m88k \ | maxq | mb | microblaze | microblazeel | mcore | mep | metag \ | mips | mipsbe | mipseb | mipsel | mipsle \ | mips16 \ | mips64 | mips64el \ | mips64octeon | mips64octeonel \ | mips64orion | mips64orionel \ | mips64r5900 | mips64r5900el \ | mips64vr | mips64vrel \ | mips64vr4100 | mips64vr4100el \ | mips64vr4300 | mips64vr4300el \ | mips64vr5000 | mips64vr5000el \ | mips64vr5900 | mips64vr5900el \ | mipsisa32 | mipsisa32el \ | mipsisa32r2 | mipsisa32r2el \ | mipsisa64 | mipsisa64el \ | mipsisa64r2 | mipsisa64r2el \ | mipsisa64sb1 | mipsisa64sb1el \ | mipsisa64sr71k | mipsisa64sr71kel \ | mipsr5900 | mipsr5900el \ | mipstx39 | mipstx39el \ | mn10200 | mn10300 \ | moxie \ | mt \ | msp430 \ | nds32 | nds32le | nds32be \ | nios | nios2 | nios2eb | nios2el \ | ns16k | ns32k \ | open8 \ | or1k | or32 \ | pdp10 | pdp11 | pj | pjl \ | powerpc | powerpc64 | powerpc64le | powerpcle \ | pyramid \ | rl78 | rx \ | score \ | sh | sh[1234] | sh[24]a | sh[24]aeb | sh[23]e | sh[34]eb | sheb | shbe | shle | sh[1234]le | sh3ele \ | sh64 | sh64le \ | sparc | sparc64 | sparc64b | sparc64v | sparc86x | sparclet | sparclite \ | sparcv8 | sparcv9 | sparcv9b | sparcv9v \ | spu \ | tahoe | tic4x | tic54x | tic55x | tic6x | tic80 | tron \ | ubicom32 \ | v850 | v850e | v850e1 | v850e2 | v850es | v850e2v3 \ | we32k \ | x86 | xc16x | xstormy16 | xtensa \ | z8k | z80) basic_machine=$basic_machine-unknown ;; c54x) basic_machine=tic54x-unknown ;; c55x) basic_machine=tic55x-unknown ;; c6x) basic_machine=tic6x-unknown ;; m6811 | m68hc11 | m6812 | m68hc12 | m68hcs12x | nvptx | picochip) basic_machine=$basic_machine-unknown os=-none ;; m88110 | m680[12346]0 | m683?2 | m68360 | m5200 | v70 | w65 | z8k) ;; ms1) basic_machine=mt-unknown ;; strongarm | thumb | xscale) basic_machine=arm-unknown ;; xgate) basic_machine=$basic_machine-unknown os=-none ;; xscaleeb) basic_machine=armeb-unknown ;; xscaleel) basic_machine=armel-unknown ;; # We use `pc' rather than `unknown' # because (1) that's what they normally are, and # (2) the word "unknown" tends to confuse beginning users. i*86 | x86_64) basic_machine=$basic_machine-pc ;; # Object if more than one company name word. *-*-*) echo Invalid configuration \`$1\': machine \`$basic_machine\' not recognized 1>&2 exit 1 ;; # Recognize the basic CPU types with company name. 580-* \ | a29k-* \ | aarch64-* | aarch64_be-* \ | alpha-* | alphaev[4-8]-* | alphaev56-* | alphaev6[78]-* \ | alpha64-* | alpha64ev[4-8]-* | alpha64ev56-* | alpha64ev6[78]-* \ | alphapca5[67]-* | alpha64pca5[67]-* | arc-* | arceb-* \ | arm-* | armbe-* | armle-* | armeb-* | armv*-* \ | avr-* | avr32-* \ | be32-* | be64-* \ | bfin-* | bs2000-* \ | c[123]* | c30-* | [cjt]90-* | c4x-* \ | c8051-* | clipper-* | craynv-* | cydra-* \ | d10v-* | d30v-* | dlx-* \ | elxsi-* \ | f30[01]-* | f700-* | fido-* | fr30-* | frv-* | fx80-* \ | h8300-* | h8500-* \ | hppa-* | hppa1.[01]-* | hppa2.0-* | hppa2.0[nw]-* | hppa64-* \ | hexagon-* \ | i*86-* | i860-* | i960-* | ia64-* \ | ip2k-* | iq2000-* \ | k1om-* \ | le32-* | le64-* \ | lm32-* \ | m32c-* | m32r-* | m32rle-* \ | m68000-* | m680[012346]0-* | m68360-* | m683?2-* | m68k-* \ | m88110-* | m88k-* | maxq-* | mcore-* | metag-* \ | microblaze-* | microblazeel-* \ | mips-* | mipsbe-* | mipseb-* | mipsel-* | mipsle-* \ | mips16-* \ | mips64-* | mips64el-* \ | mips64octeon-* | mips64octeonel-* \ | mips64orion-* | mips64orionel-* \ | mips64r5900-* | mips64r5900el-* \ | mips64vr-* | mips64vrel-* \ | mips64vr4100-* | mips64vr4100el-* \ | mips64vr4300-* | mips64vr4300el-* \ | mips64vr5000-* | mips64vr5000el-* \ | mips64vr5900-* | mips64vr5900el-* \ | mipsisa32-* | mipsisa32el-* \ | mipsisa32r2-* | mipsisa32r2el-* \ | mipsisa64-* | mipsisa64el-* \ | mipsisa64r2-* | mipsisa64r2el-* \ | mipsisa64sb1-* | mipsisa64sb1el-* \ | mipsisa64sr71k-* | mipsisa64sr71kel-* \ | mipsr5900-* | mipsr5900el-* \ | mipstx39-* | mipstx39el-* \ | mmix-* \ | mt-* \ | msp430-* \ | nds32-* | nds32le-* | nds32be-* \ | nios-* | nios2-* | nios2eb-* | nios2el-* \ | none-* | np1-* | ns16k-* | ns32k-* \ | open8-* \ | orion-* \ | pdp10-* | pdp11-* | pj-* | pjl-* | pn-* | power-* \ | powerpc-* | powerpc64-* | powerpc64le-* | powerpcle-* \ | pyramid-* \ | rl78-* | romp-* | rs6000-* | rx-* \ | sh-* | sh[1234]-* | sh[24]a-* | sh[24]aeb-* | sh[23]e-* | sh[34]eb-* | sheb-* | shbe-* \ | shle-* | sh[1234]le-* | sh3ele-* | sh64-* | sh64le-* \ | sparc-* | sparc64-* | sparc64b-* | sparc64v-* | sparc86x-* | sparclet-* \ | sparclite-* \ | sparcv8-* | sparcv9-* | sparcv9b-* | sparcv9v-* | sv1-* | sx?-* \ | tahoe-* \ | tic30-* | tic4x-* | tic54x-* | tic55x-* | tic6x-* | tic80-* \ | tile*-* \ | tron-* \ | ubicom32-* \ | v850-* | v850e-* | v850e1-* | v850es-* | v850e2-* | v850e2v3-* \ | vax-* \ | we32k-* \ | x86-* | x86_64-* | xc16x-* | xps100-* \ | xstormy16-* | xtensa*-* \ | ymp-* \ | z8k-* | z80-*) ;; # Recognize the basic CPU types without company name, with glob match. xtensa*) basic_machine=$basic_machine-unknown ;; # Recognize the various machine names and aliases which stand # for a CPU type and a company and sometimes even an OS. 386bsd) basic_machine=i386-unknown os=-bsd ;; 3b1 | 7300 | 7300-att | att-7300 | pc7300 | safari | unixpc) basic_machine=m68000-att ;; 3b*) basic_machine=we32k-att ;; a29khif) basic_machine=a29k-amd os=-udi ;; abacus) basic_machine=abacus-unknown ;; adobe68k) basic_machine=m68010-adobe os=-scout ;; alliant | fx80) basic_machine=fx80-alliant ;; altos | altos3068) basic_machine=m68k-altos ;; am29k) basic_machine=a29k-none os=-bsd ;; amd64) basic_machine=x86_64-pc ;; amd64-*) basic_machine=x86_64-`echo $basic_machine | sed 's/^[^-]*-//'` ;; amdahl) basic_machine=580-amdahl os=-sysv ;; amiga | amiga-*) basic_machine=m68k-unknown ;; amigaos | amigados) basic_machine=m68k-unknown os=-amigaos ;; amigaunix | amix) basic_machine=m68k-unknown os=-sysv4 ;; apollo68) basic_machine=m68k-apollo os=-sysv ;; apollo68bsd) basic_machine=m68k-apollo os=-bsd ;; aros) basic_machine=i386-pc os=-aros ;; aux) basic_machine=m68k-apple os=-aux ;; balance) basic_machine=ns32k-sequent os=-dynix ;; blackfin) basic_machine=bfin-unknown os=-linux ;; blackfin-*) basic_machine=bfin-`echo $basic_machine | sed 's/^[^-]*-//'` os=-linux ;; bluegene*) basic_machine=powerpc-ibm os=-cnk ;; c54x-*) basic_machine=tic54x-`echo $basic_machine | sed 's/^[^-]*-//'` ;; c55x-*) basic_machine=tic55x-`echo $basic_machine | sed 's/^[^-]*-//'` ;; c6x-*) basic_machine=tic6x-`echo $basic_machine | sed 's/^[^-]*-//'` ;; c90) basic_machine=c90-cray os=-unicos ;; cegcc) basic_machine=arm-unknown os=-cegcc ;; convex-c1) basic_machine=c1-convex os=-bsd ;; convex-c2) basic_machine=c2-convex os=-bsd ;; convex-c32) basic_machine=c32-convex os=-bsd ;; convex-c34) basic_machine=c34-convex os=-bsd ;; convex-c38) basic_machine=c38-convex os=-bsd ;; cray | j90) basic_machine=j90-cray os=-unicos ;; craynv) basic_machine=craynv-cray os=-unicosmp ;; cr16 | cr16-*) basic_machine=cr16-unknown os=-elf ;; crds | unos) basic_machine=m68k-crds ;; crisv32 | crisv32-* | etraxfs*) basic_machine=crisv32-axis ;; cris | cris-* | etrax*) basic_machine=cris-axis ;; crx) basic_machine=crx-unknown os=-elf ;; da30 | da30-*) basic_machine=m68k-da30 ;; decstation | decstation-3100 | pmax | pmax-* | pmin | dec3100 | decstatn) basic_machine=mips-dec ;; decsystem10* | dec10*) basic_machine=pdp10-dec os=-tops10 ;; decsystem20* | dec20*) basic_machine=pdp10-dec os=-tops20 ;; delta | 3300 | motorola-3300 | motorola-delta \ | 3300-motorola | delta-motorola) basic_machine=m68k-motorola ;; delta88) basic_machine=m88k-motorola os=-sysv3 ;; dicos) basic_machine=i686-pc os=-dicos ;; djgpp) basic_machine=i586-pc os=-msdosdjgpp ;; dpx20 | dpx20-*) basic_machine=rs6000-bull os=-bosx ;; dpx2* | dpx2*-bull) basic_machine=m68k-bull os=-sysv3 ;; ebmon29k) basic_machine=a29k-amd os=-ebmon ;; elxsi) basic_machine=elxsi-elxsi os=-bsd ;; encore | umax | mmax) basic_machine=ns32k-encore ;; es1800 | OSE68k | ose68k | ose | OSE) basic_machine=m68k-ericsson os=-ose ;; fx2800) basic_machine=i860-alliant ;; genix) basic_machine=ns32k-ns ;; gmicro) basic_machine=tron-gmicro os=-sysv ;; go32) basic_machine=i386-pc os=-go32 ;; h3050r* | hiux*) basic_machine=hppa1.1-hitachi os=-hiuxwe2 ;; h8300hms) basic_machine=h8300-hitachi os=-hms ;; h8300xray) basic_machine=h8300-hitachi os=-xray ;; h8500hms) basic_machine=h8500-hitachi os=-hms ;; harris) basic_machine=m88k-harris os=-sysv3 ;; hp300-*) basic_machine=m68k-hp ;; hp300bsd) basic_machine=m68k-hp os=-bsd ;; hp300hpux) basic_machine=m68k-hp os=-hpux ;; hp3k9[0-9][0-9] | hp9[0-9][0-9]) basic_machine=hppa1.0-hp ;; hp9k2[0-9][0-9] | hp9k31[0-9]) basic_machine=m68000-hp ;; hp9k3[2-9][0-9]) basic_machine=m68k-hp ;; hp9k6[0-9][0-9] | hp6[0-9][0-9]) basic_machine=hppa1.0-hp ;; hp9k7[0-79][0-9] | hp7[0-79][0-9]) basic_machine=hppa1.1-hp ;; hp9k78[0-9] | hp78[0-9]) # FIXME: really hppa2.0-hp basic_machine=hppa1.1-hp ;; hp9k8[67]1 | hp8[67]1 | hp9k80[24] | hp80[24] | hp9k8[78]9 | hp8[78]9 | hp9k893 | hp893) # FIXME: really hppa2.0-hp basic_machine=hppa1.1-hp ;; hp9k8[0-9][13679] | hp8[0-9][13679]) basic_machine=hppa1.1-hp ;; hp9k8[0-9][0-9] | hp8[0-9][0-9]) basic_machine=hppa1.0-hp ;; hppa-next) os=-nextstep3 ;; hppaosf) basic_machine=hppa1.1-hp os=-osf ;; hppro) basic_machine=hppa1.1-hp os=-proelf ;; i370-ibm* | ibm*) basic_machine=i370-ibm ;; i*86v32) basic_machine=`echo $1 | sed -e 's/86.*/86-pc/'` os=-sysv32 ;; i*86v4*) basic_machine=`echo $1 | sed -e 's/86.*/86-pc/'` os=-sysv4 ;; i*86v) basic_machine=`echo $1 | sed -e 's/86.*/86-pc/'` os=-sysv ;; i*86sol2) basic_machine=`echo $1 | sed -e 's/86.*/86-pc/'` os=-solaris2 ;; i386mach) basic_machine=i386-mach os=-mach ;; i386-vsta | vsta) basic_machine=i386-unknown os=-vsta ;; iris | iris4d) basic_machine=mips-sgi case $os in -irix*) ;; *) os=-irix4 ;; esac ;; isi68 | isi) basic_machine=m68k-isi os=-sysv ;; m68knommu) basic_machine=m68k-unknown os=-linux ;; m68knommu-*) basic_machine=m68k-`echo $basic_machine | sed 's/^[^-]*-//'` os=-linux ;; m88k-omron*) basic_machine=m88k-omron ;; magnum | m3230) basic_machine=mips-mips os=-sysv ;; merlin) basic_machine=ns32k-utek os=-sysv ;; microblaze*) basic_machine=microblaze-xilinx ;; mingw64) basic_machine=x86_64-pc os=-mingw64 ;; mingw32) basic_machine=i686-pc os=-mingw32 ;; mingw32ce) basic_machine=arm-unknown os=-mingw32ce ;; miniframe) basic_machine=m68000-convergent ;; *mint | -mint[0-9]* | *MiNT | *MiNT[0-9]*) basic_machine=m68k-atari os=-mint ;; mips3*-*) basic_machine=`echo $basic_machine | sed -e 's/mips3/mips64/'` ;; mips3*) basic_machine=`echo $basic_machine | sed -e 's/mips3/mips64/'`-unknown ;; monitor) basic_machine=m68k-rom68k os=-coff ;; morphos) basic_machine=powerpc-unknown os=-morphos ;; msdos) basic_machine=i386-pc os=-msdos ;; ms1-*) basic_machine=`echo $basic_machine | sed -e 's/ms1-/mt-/'` ;; msys) basic_machine=i686-pc os=-msys ;; mvs) basic_machine=i370-ibm os=-mvs ;; nacl) basic_machine=le32-unknown os=-nacl ;; ncr3000) basic_machine=i486-ncr os=-sysv4 ;; netbsd386) basic_machine=i386-unknown os=-netbsd ;; netwinder) basic_machine=armv4l-rebel os=-linux ;; news | news700 | news800 | news900) basic_machine=m68k-sony os=-newsos ;; news1000) basic_machine=m68030-sony os=-newsos ;; news-3600 | risc-news) basic_machine=mips-sony os=-newsos ;; necv70) basic_machine=v70-nec os=-sysv ;; next | m*-next ) basic_machine=m68k-next case $os in -nextstep* ) ;; -ns2*) os=-nextstep2 ;; *) os=-nextstep3 ;; esac ;; nh3000) basic_machine=m68k-harris os=-cxux ;; nh[45]000) basic_machine=m88k-harris os=-cxux ;; nindy960) basic_machine=i960-intel os=-nindy ;; mon960) basic_machine=i960-intel os=-mon960 ;; nonstopux) basic_machine=mips-compaq os=-nonstopux ;; np1) basic_machine=np1-gould ;; neo-tandem) basic_machine=neo-tandem ;; nse-tandem) basic_machine=nse-tandem ;; nsr-tandem) basic_machine=nsr-tandem ;; op50n-* | op60c-*) basic_machine=hppa1.1-oki os=-proelf ;; openrisc | openrisc-*) basic_machine=or32-unknown ;; os400) basic_machine=powerpc-ibm os=-os400 ;; OSE68000 | ose68000) basic_machine=m68000-ericsson os=-ose ;; os68k) basic_machine=m68k-none os=-os68k ;; pa-hitachi) basic_machine=hppa1.1-hitachi os=-hiuxwe2 ;; paragon) basic_machine=i860-intel os=-osf ;; parisc) basic_machine=hppa-unknown os=-linux ;; parisc-*) basic_machine=hppa-`echo $basic_machine | sed 's/^[^-]*-//'` os=-linux ;; pbd) basic_machine=sparc-tti ;; pbb) basic_machine=m68k-tti ;; pc532 | pc532-*) basic_machine=ns32k-pc532 ;; pc98) basic_machine=i386-pc ;; pc98-*) basic_machine=i386-`echo $basic_machine | sed 's/^[^-]*-//'` ;; pentium | p5 | k5 | k6 | nexgen | viac3) basic_machine=i586-pc ;; pentiumpro | p6 | 6x86 | athlon | athlon_*) basic_machine=i686-pc ;; pentiumii | pentium2 | pentiumiii | pentium3) basic_machine=i686-pc ;; pentium4) basic_machine=i786-pc ;; pentium-* | p5-* | k5-* | k6-* | nexgen-* | viac3-*) basic_machine=i586-`echo $basic_machine | sed 's/^[^-]*-//'` ;; pentiumpro-* | p6-* | 6x86-* | athlon-*) basic_machine=i686-`echo $basic_machine | sed 's/^[^-]*-//'` ;; pentiumii-* | pentium2-* | pentiumiii-* | pentium3-*) basic_machine=i686-`echo $basic_machine | sed 's/^[^-]*-//'` ;; pentium4-*) basic_machine=i786-`echo $basic_machine | sed 's/^[^-]*-//'` ;; pn) basic_machine=pn-gould ;; power) basic_machine=power-ibm ;; ppc | ppcbe) basic_machine=powerpc-unknown ;; ppc-* | ppcbe-*) basic_machine=powerpc-`echo $basic_machine | sed 's/^[^-]*-//'` ;; ppcle | powerpclittle | ppc-le | powerpc-little) basic_machine=powerpcle-unknown ;; ppcle-* | powerpclittle-*) basic_machine=powerpcle-`echo $basic_machine | sed 's/^[^-]*-//'` ;; ppc64) basic_machine=powerpc64-unknown ;; ppc64-*) basic_machine=powerpc64-`echo $basic_machine | sed 's/^[^-]*-//'` ;; ppc64le | powerpc64little | ppc64-le | powerpc64-little) basic_machine=powerpc64le-unknown ;; ppc64le-* | powerpc64little-*) basic_machine=powerpc64le-`echo $basic_machine | sed 's/^[^-]*-//'` ;; ps2) basic_machine=i386-ibm ;; pw32) basic_machine=i586-unknown os=-pw32 ;; rdos | rdos64) basic_machine=x86_64-pc os=-rdos ;; rdos32) basic_machine=i386-pc os=-rdos ;; rom68k) basic_machine=m68k-rom68k os=-coff ;; rm[46]00) basic_machine=mips-siemens ;; rtpc | rtpc-*) basic_machine=romp-ibm ;; s390 | s390-*) basic_machine=s390-ibm ;; s390x | s390x-*) basic_machine=s390x-ibm ;; sa29200) basic_machine=a29k-amd os=-udi ;; sb1) basic_machine=mipsisa64sb1-unknown ;; sb1el) basic_machine=mipsisa64sb1el-unknown ;; sde) basic_machine=mipsisa32-sde os=-elf ;; sei) basic_machine=mips-sei os=-seiux ;; sequent) basic_machine=i386-sequent ;; sh) basic_machine=sh-hitachi os=-hms ;; sh5el) basic_machine=sh5le-unknown ;; sh64) basic_machine=sh64-unknown ;; sparclite-wrs | simso-wrs) basic_machine=sparclite-wrs os=-vxworks ;; sps7) basic_machine=m68k-bull os=-sysv2 ;; spur) basic_machine=spur-unknown ;; st2000) basic_machine=m68k-tandem ;; stratus) basic_machine=i860-stratus os=-sysv4 ;; strongarm-* | thumb-*) basic_machine=arm-`echo $basic_machine | sed 's/^[^-]*-//'` ;; sun2) basic_machine=m68000-sun ;; sun2os3) basic_machine=m68000-sun os=-sunos3 ;; sun2os4) basic_machine=m68000-sun os=-sunos4 ;; sun3os3) basic_machine=m68k-sun os=-sunos3 ;; sun3os4) basic_machine=m68k-sun os=-sunos4 ;; sun4os3) basic_machine=sparc-sun os=-sunos3 ;; sun4os4) basic_machine=sparc-sun os=-sunos4 ;; sun4sol2) basic_machine=sparc-sun os=-solaris2 ;; sun3 | sun3-*) basic_machine=m68k-sun ;; sun4) basic_machine=sparc-sun ;; sun386 | sun386i | roadrunner) basic_machine=i386-sun ;; sv1) basic_machine=sv1-cray os=-unicos ;; symmetry) basic_machine=i386-sequent os=-dynix ;; t3e) basic_machine=alphaev5-cray os=-unicos ;; t90) basic_machine=t90-cray os=-unicos ;; tile*) basic_machine=$basic_machine-unknown os=-linux-gnu ;; tx39) basic_machine=mipstx39-unknown ;; tx39el) basic_machine=mipstx39el-unknown ;; toad1) basic_machine=pdp10-xkl os=-tops20 ;; tower | tower-32) basic_machine=m68k-ncr ;; tpf) basic_machine=s390x-ibm os=-tpf ;; udi29k) basic_machine=a29k-amd os=-udi ;; ultra3) basic_machine=a29k-nyu os=-sym1 ;; v810 | necv810) basic_machine=v810-nec os=-none ;; vaxv) basic_machine=vax-dec os=-sysv ;; vms) basic_machine=vax-dec os=-vms ;; vpp*|vx|vx-*) basic_machine=f301-fujitsu ;; vxworks960) basic_machine=i960-wrs os=-vxworks ;; vxworks68) basic_machine=m68k-wrs os=-vxworks ;; vxworks29k) basic_machine=a29k-wrs os=-vxworks ;; w65*) basic_machine=w65-wdc os=-none ;; w89k-*) basic_machine=hppa1.1-winbond os=-proelf ;; xbox) basic_machine=i686-pc os=-mingw32 ;; xps | xps100) basic_machine=xps100-honeywell ;; xscale-* | xscalee[bl]-*) basic_machine=`echo $basic_machine | sed 's/^xscale/arm/'` ;; ymp) basic_machine=ymp-cray os=-unicos ;; z8k-*-coff) basic_machine=z8k-unknown os=-sim ;; z80-*-coff) basic_machine=z80-unknown os=-sim ;; none) basic_machine=none-none os=-none ;; # Here we handle the default manufacturer of certain CPU types. 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Likely further. if test -x /sbin/sysctl; then lt_cv_sys_max_cmd_len=`/sbin/sysctl -n kern.argmax` elif test -x /usr/sbin/sysctl; then lt_cv_sys_max_cmd_len=`/usr/sbin/sysctl -n kern.argmax` else lt_cv_sys_max_cmd_len=65536 # usable default for all BSDs fi # And add a safety zone lt_cv_sys_max_cmd_len=`expr $lt_cv_sys_max_cmd_len \/ 4` lt_cv_sys_max_cmd_len=`expr $lt_cv_sys_max_cmd_len \* 3` ;; interix*) # We know the value 262144 and hardcode it with a safety zone (like BSD) lt_cv_sys_max_cmd_len=196608 ;; os2*) # The test takes a long time on OS/2. lt_cv_sys_max_cmd_len=8192 ;; osf*) # Dr. Hans Ekkehard Plesser reports seeing a kernel panic running configure # due to this test when exec_disable_arg_limit is 1 on Tru64. It is not # nice to cause kernel panics so lets avoid the loop below. # First set a reasonable default. lt_cv_sys_max_cmd_len=16384 # if test -x /sbin/sysconfig; then case `/sbin/sysconfig -q proc exec_disable_arg_limit` in *1*) lt_cv_sys_max_cmd_len=-1 ;; esac fi ;; sco3.2v5*) lt_cv_sys_max_cmd_len=102400 ;; sysv5* | sco5v6* | sysv4.2uw2*) kargmax=`grep ARG_MAX /etc/conf/cf.d/stune 2>/dev/null` if test -n "$kargmax"; then lt_cv_sys_max_cmd_len=`echo $kargmax | sed 's/.*[ ]//'` else lt_cv_sys_max_cmd_len=32768 fi ;; *) lt_cv_sys_max_cmd_len=`(getconf ARG_MAX) 2> /dev/null` if test -n "$lt_cv_sys_max_cmd_len"; then lt_cv_sys_max_cmd_len=`expr $lt_cv_sys_max_cmd_len \/ 4` lt_cv_sys_max_cmd_len=`expr $lt_cv_sys_max_cmd_len \* 3` else # Make teststring a little bigger before we do anything with it. # a 1K string should be a reasonable start. for i in 1 2 3 4 5 6 7 8 ; do teststring=$teststring$teststring done SHELL=${SHELL-${CONFIG_SHELL-/bin/sh}} # If test is not a shell built-in, we'll probably end up computing a # maximum length that is only half of the actual maximum length, but # we can't tell. while { test "X"`env echo "$teststring$teststring" 2>/dev/null` \ = "X$teststring$teststring"; } >/dev/null 2>&1 && test $i != 17 # 1/2 MB should be enough do i=`expr $i + 1` teststring=$teststring$teststring done # Only check the string length outside the loop. lt_cv_sys_max_cmd_len=`expr "X$teststring" : ".*" 2>&1` teststring= # Add a significant safety factor because C++ compilers can tack on # massive amounts of additional arguments before passing them to the # linker. It appears as though 1/2 is a usable value. lt_cv_sys_max_cmd_len=`expr $lt_cv_sys_max_cmd_len \/ 2` fi ;; esac fi if test -n $lt_cv_sys_max_cmd_len ; then { $as_echo "$as_me:${as_lineno-$LINENO}: result: $lt_cv_sys_max_cmd_len" >&5 $as_echo "$lt_cv_sys_max_cmd_len" >&6; } else { $as_echo "$as_me:${as_lineno-$LINENO}: result: none" >&5 $as_echo "none" >&6; } fi max_cmd_len=$lt_cv_sys_max_cmd_len : ${CP="cp -f"} : ${MV="mv -f"} : ${RM="rm -f"} { $as_echo "$as_me:${as_lineno-$LINENO}: checking whether the shell understands some XSI constructs" >&5 $as_echo_n "checking whether the shell understands some XSI constructs... " >&6; } # Try some XSI features xsi_shell=no ( _lt_dummy="a/b/c" test "${_lt_dummy##*/},${_lt_dummy%/*},${_lt_dummy#??}"${_lt_dummy%"$_lt_dummy"}, \ = c,a/b,b/c, \ && eval 'test $(( 1 + 1 )) -eq 2 \ && test "${#_lt_dummy}" -eq 5' ) >/dev/null 2>&1 \ && xsi_shell=yes { $as_echo "$as_me:${as_lineno-$LINENO}: result: $xsi_shell" >&5 $as_echo "$xsi_shell" >&6; } { $as_echo "$as_me:${as_lineno-$LINENO}: checking whether the shell understands \"+=\"" >&5 $as_echo_n "checking whether the shell understands \"+=\"... " >&6; } lt_shell_append=no ( foo=bar; set foo baz; eval "$1+=\$2" && test "$foo" = barbaz ) \ >/dev/null 2>&1 \ && lt_shell_append=yes { $as_echo "$as_me:${as_lineno-$LINENO}: result: $lt_shell_append" >&5 $as_echo "$lt_shell_append" >&6; } if ( (MAIL=60; unset MAIL) || exit) >/dev/null 2>&1; then lt_unset=unset else lt_unset=false fi # test EBCDIC or ASCII case `echo X|tr X '\101'` in A) # ASCII based system # \n is not interpreted correctly by Solaris 8 /usr/ucb/tr lt_SP2NL='tr \040 \012' lt_NL2SP='tr \015\012 \040\040' ;; *) # EBCDIC based system lt_SP2NL='tr \100 \n' lt_NL2SP='tr \r\n \100\100' ;; esac { $as_echo "$as_me:${as_lineno-$LINENO}: checking how to convert $build file names to $host format" >&5 $as_echo_n "checking how to convert $build file names to $host format... " >&6; } if ${lt_cv_to_host_file_cmd+:} false; then : $as_echo_n "(cached) " >&6 else case $host in *-*-mingw* ) case $build in *-*-mingw* ) # actually msys lt_cv_to_host_file_cmd=func_convert_file_msys_to_w32 ;; *-*-cygwin* ) lt_cv_to_host_file_cmd=func_convert_file_cygwin_to_w32 ;; * ) # otherwise, assume *nix lt_cv_to_host_file_cmd=func_convert_file_nix_to_w32 ;; esac ;; *-*-cygwin* ) case $build in *-*-mingw* ) # actually msys lt_cv_to_host_file_cmd=func_convert_file_msys_to_cygwin ;; *-*-cygwin* ) lt_cv_to_host_file_cmd=func_convert_file_noop ;; * ) # otherwise, assume *nix lt_cv_to_host_file_cmd=func_convert_file_nix_to_cygwin ;; esac ;; * ) # unhandled hosts (and "normal" native builds) lt_cv_to_host_file_cmd=func_convert_file_noop ;; esac fi to_host_file_cmd=$lt_cv_to_host_file_cmd { $as_echo "$as_me:${as_lineno-$LINENO}: result: $lt_cv_to_host_file_cmd" >&5 $as_echo "$lt_cv_to_host_file_cmd" >&6; } { $as_echo "$as_me:${as_lineno-$LINENO}: checking how to convert $build file names to toolchain format" >&5 $as_echo_n "checking how to convert $build file names to toolchain format... " >&6; } if ${lt_cv_to_tool_file_cmd+:} false; then : $as_echo_n "(cached) " >&6 else #assume ordinary cross tools, or native build. lt_cv_to_tool_file_cmd=func_convert_file_noop case $host in *-*-mingw* ) case $build in *-*-mingw* ) # actually msys lt_cv_to_tool_file_cmd=func_convert_file_msys_to_w32 ;; esac ;; esac fi to_tool_file_cmd=$lt_cv_to_tool_file_cmd { $as_echo "$as_me:${as_lineno-$LINENO}: result: $lt_cv_to_tool_file_cmd" >&5 $as_echo "$lt_cv_to_tool_file_cmd" >&6; } { $as_echo "$as_me:${as_lineno-$LINENO}: checking for $LD option to reload object files" >&5 $as_echo_n "checking for $LD option to reload object files... " >&6; } if ${lt_cv_ld_reload_flag+:} false; then : $as_echo_n "(cached) " >&6 else lt_cv_ld_reload_flag='-r' fi { $as_echo "$as_me:${as_lineno-$LINENO}: result: $lt_cv_ld_reload_flag" >&5 $as_echo "$lt_cv_ld_reload_flag" >&6; } reload_flag=$lt_cv_ld_reload_flag case $reload_flag in "" | " "*) ;; *) reload_flag=" $reload_flag" ;; esac reload_cmds='$LD$reload_flag -o $output$reload_objs' case $host_os in cygwin* | mingw* | pw32* | cegcc*) if test "$GCC" != yes; then reload_cmds=false fi ;; darwin*) if test "$GCC" = yes; then reload_cmds='$LTCC $LTCFLAGS -nostdlib ${wl}-r -o $output$reload_objs' else reload_cmds='$LD$reload_flag -o $output$reload_objs' fi ;; esac if test -n "$ac_tool_prefix"; then # Extract the first word of "${ac_tool_prefix}objdump", so it can be a program name with args. set dummy ${ac_tool_prefix}objdump; ac_word=$2 { $as_echo "$as_me:${as_lineno-$LINENO}: checking for $ac_word" >&5 $as_echo_n "checking for $ac_word... " >&6; } if ${ac_cv_prog_OBJDUMP+:} false; then : $as_echo_n "(cached) " >&6 else if test -n "$OBJDUMP"; then ac_cv_prog_OBJDUMP="$OBJDUMP" # Let the user override the test. else as_save_IFS=$IFS; IFS=$PATH_SEPARATOR for as_dir in $PATH do IFS=$as_save_IFS test -z "$as_dir" && as_dir=. for ac_exec_ext in '' $ac_executable_extensions; do if as_fn_executable_p "$as_dir/$ac_word$ac_exec_ext"; then ac_cv_prog_OBJDUMP="${ac_tool_prefix}objdump" $as_echo "$as_me:${as_lineno-$LINENO}: found $as_dir/$ac_word$ac_exec_ext" >&5 break 2 fi done done IFS=$as_save_IFS fi fi OBJDUMP=$ac_cv_prog_OBJDUMP if test -n "$OBJDUMP"; then { $as_echo "$as_me:${as_lineno-$LINENO}: result: $OBJDUMP" >&5 $as_echo "$OBJDUMP" >&6; } else { $as_echo "$as_me:${as_lineno-$LINENO}: result: no" >&5 $as_echo "no" >&6; } fi fi if test -z "$ac_cv_prog_OBJDUMP"; then ac_ct_OBJDUMP=$OBJDUMP # Extract the first word of "objdump", so it can be a program name with args. set dummy objdump; ac_word=$2 { $as_echo "$as_me:${as_lineno-$LINENO}: checking for $ac_word" >&5 $as_echo_n "checking for $ac_word... " >&6; } if ${ac_cv_prog_ac_ct_OBJDUMP+:} false; then : $as_echo_n "(cached) " >&6 else if test -n "$ac_ct_OBJDUMP"; then ac_cv_prog_ac_ct_OBJDUMP="$ac_ct_OBJDUMP" # Let the user override the test. else as_save_IFS=$IFS; IFS=$PATH_SEPARATOR for as_dir in $PATH do IFS=$as_save_IFS test -z "$as_dir" && as_dir=. for ac_exec_ext in '' $ac_executable_extensions; do if as_fn_executable_p "$as_dir/$ac_word$ac_exec_ext"; then ac_cv_prog_ac_ct_OBJDUMP="objdump" $as_echo "$as_me:${as_lineno-$LINENO}: found $as_dir/$ac_word$ac_exec_ext" >&5 break 2 fi done done IFS=$as_save_IFS fi fi ac_ct_OBJDUMP=$ac_cv_prog_ac_ct_OBJDUMP if test -n "$ac_ct_OBJDUMP"; then { $as_echo "$as_me:${as_lineno-$LINENO}: result: $ac_ct_OBJDUMP" >&5 $as_echo "$ac_ct_OBJDUMP" >&6; } else { $as_echo "$as_me:${as_lineno-$LINENO}: result: no" >&5 $as_echo "no" >&6; } fi if test "x$ac_ct_OBJDUMP" = x; then OBJDUMP="false" else case $cross_compiling:$ac_tool_warned in yes:) { $as_echo "$as_me:${as_lineno-$LINENO}: WARNING: using cross tools not prefixed with host triplet" >&5 $as_echo "$as_me: WARNING: using cross tools not prefixed with host triplet" >&2;} ac_tool_warned=yes ;; esac OBJDUMP=$ac_ct_OBJDUMP fi else OBJDUMP="$ac_cv_prog_OBJDUMP" fi test -z "$OBJDUMP" && OBJDUMP=objdump { $as_echo "$as_me:${as_lineno-$LINENO}: checking how to recognize dependent libraries" >&5 $as_echo_n "checking how to recognize dependent libraries... " >&6; } if ${lt_cv_deplibs_check_method+:} false; then : $as_echo_n "(cached) " >&6 else lt_cv_file_magic_cmd='$MAGIC_CMD' lt_cv_file_magic_test_file= lt_cv_deplibs_check_method='unknown' # Need to set the preceding variable on all platforms that support # interlibrary dependencies. # 'none' -- dependencies not supported. # `unknown' -- same as none, but documents that we really don't know. # 'pass_all' -- all dependencies passed with no checks. # 'test_compile' -- check by making test program. # 'file_magic [[regex]]' -- check by looking for files in library path # which responds to the $file_magic_cmd with a given extended regex. # If you have `file' or equivalent on your system and you're not sure # whether `pass_all' will *always* work, you probably want this one. case $host_os in aix[4-9]*) lt_cv_deplibs_check_method=pass_all ;; beos*) lt_cv_deplibs_check_method=pass_all ;; bsdi[45]*) lt_cv_deplibs_check_method='file_magic ELF [0-9][0-9]*-bit [ML]SB (shared object|dynamic lib)' lt_cv_file_magic_cmd='/usr/bin/file -L' lt_cv_file_magic_test_file=/shlib/libc.so ;; cygwin*) # func_win32_libid is a shell function defined in ltmain.sh lt_cv_deplibs_check_method='file_magic ^x86 archive import|^x86 DLL' lt_cv_file_magic_cmd='func_win32_libid' ;; mingw* | pw32*) # Base MSYS/MinGW do not provide the 'file' command needed by # func_win32_libid shell function, so use a weaker test based on 'objdump', # unless we find 'file', for example because we are cross-compiling. # func_win32_libid assumes BSD nm, so disallow it if using MS dumpbin. if ( test "$lt_cv_nm_interface" = "BSD nm" && file / ) >/dev/null 2>&1; then lt_cv_deplibs_check_method='file_magic ^x86 archive import|^x86 DLL' lt_cv_file_magic_cmd='func_win32_libid' else # Keep this pattern in sync with the one in func_win32_libid. lt_cv_deplibs_check_method='file_magic file format (pei*-i386(.*architecture: i386)?|pe-arm-wince|pe-x86-64)' lt_cv_file_magic_cmd='$OBJDUMP -f' fi ;; cegcc*) # use the weaker test based on 'objdump'. See mingw*. lt_cv_deplibs_check_method='file_magic file format pe-arm-.*little(.*architecture: arm)?' lt_cv_file_magic_cmd='$OBJDUMP -f' ;; darwin* | rhapsody*) lt_cv_deplibs_check_method=pass_all ;; freebsd* | dragonfly*) if echo __ELF__ | $CC -E - | $GREP __ELF__ > /dev/null; then case $host_cpu in i*86 ) # Not sure whether the presence of OpenBSD here was a mistake. # Let's accept both of them until this is cleared up. lt_cv_deplibs_check_method='file_magic (FreeBSD|OpenBSD|DragonFly)/i[3-9]86 (compact )?demand paged shared library' lt_cv_file_magic_cmd=/usr/bin/file lt_cv_file_magic_test_file=`echo /usr/lib/libc.so.*` ;; esac else lt_cv_deplibs_check_method=pass_all fi ;; gnu*) lt_cv_deplibs_check_method=pass_all ;; haiku*) lt_cv_deplibs_check_method=pass_all ;; hpux10.20* | hpux11*) lt_cv_file_magic_cmd=/usr/bin/file case $host_cpu in ia64*) lt_cv_deplibs_check_method='file_magic (s[0-9][0-9][0-9]|ELF-[0-9][0-9]) shared object file - IA64' lt_cv_file_magic_test_file=/usr/lib/hpux32/libc.so ;; hppa*64*) lt_cv_deplibs_check_method='file_magic (s[0-9][0-9][0-9]|ELF[ -][0-9][0-9])(-bit)?( [LM]SB)? shared object( file)?[, -]* PA-RISC [0-9]\.[0-9]' lt_cv_file_magic_test_file=/usr/lib/pa20_64/libc.sl ;; *) lt_cv_deplibs_check_method='file_magic (s[0-9][0-9][0-9]|PA-RISC[0-9]\.[0-9]) shared library' lt_cv_file_magic_test_file=/usr/lib/libc.sl ;; esac ;; interix[3-9]*) # PIC code is broken on Interix 3.x, that's why |\.a not |_pic\.a here lt_cv_deplibs_check_method='match_pattern /lib[^/]+(\.so|\.a)$' ;; irix5* | irix6* | nonstopux*) case $LD in *-32|*"-32 ") libmagic=32-bit;; *-n32|*"-n32 ") libmagic=N32;; *-64|*"-64 ") libmagic=64-bit;; *) libmagic=never-match;; esac lt_cv_deplibs_check_method=pass_all ;; # This must be glibc/ELF. linux* | k*bsd*-gnu | kopensolaris*-gnu) lt_cv_deplibs_check_method=pass_all ;; netbsd*) if echo __ELF__ | $CC -E - | $GREP __ELF__ > /dev/null; then lt_cv_deplibs_check_method='match_pattern /lib[^/]+(\.so\.[0-9]+\.[0-9]+|_pic\.a)$' else lt_cv_deplibs_check_method='match_pattern /lib[^/]+(\.so|_pic\.a)$' fi ;; newos6*) lt_cv_deplibs_check_method='file_magic ELF [0-9][0-9]*-bit [ML]SB (executable|dynamic lib)' lt_cv_file_magic_cmd=/usr/bin/file lt_cv_file_magic_test_file=/usr/lib/libnls.so ;; *nto* | *qnx*) lt_cv_deplibs_check_method=pass_all ;; openbsd*) if test -z "`echo __ELF__ | $CC -E - | $GREP __ELF__`" || test "$host_os-$host_cpu" = "openbsd2.8-powerpc"; then lt_cv_deplibs_check_method='match_pattern /lib[^/]+(\.so\.[0-9]+\.[0-9]+|\.so|_pic\.a)$' else lt_cv_deplibs_check_method='match_pattern /lib[^/]+(\.so\.[0-9]+\.[0-9]+|_pic\.a)$' fi ;; osf3* | osf4* | osf5*) lt_cv_deplibs_check_method=pass_all ;; rdos*) lt_cv_deplibs_check_method=pass_all ;; solaris*) lt_cv_deplibs_check_method=pass_all ;; sysv5* | sco3.2v5* | sco5v6* | unixware* | OpenUNIX* | sysv4*uw2*) lt_cv_deplibs_check_method=pass_all ;; sysv4 | sysv4.3*) case $host_vendor in motorola) lt_cv_deplibs_check_method='file_magic ELF [0-9][0-9]*-bit [ML]SB (shared object|dynamic lib) M[0-9][0-9]* Version [0-9]' lt_cv_file_magic_test_file=`echo /usr/lib/libc.so*` ;; ncr) lt_cv_deplibs_check_method=pass_all ;; sequent) lt_cv_file_magic_cmd='/bin/file' lt_cv_deplibs_check_method='file_magic ELF [0-9][0-9]*-bit [LM]SB (shared object|dynamic lib )' ;; sni) lt_cv_file_magic_cmd='/bin/file' lt_cv_deplibs_check_method="file_magic ELF [0-9][0-9]*-bit [LM]SB dynamic lib" lt_cv_file_magic_test_file=/lib/libc.so ;; siemens) lt_cv_deplibs_check_method=pass_all ;; pc) lt_cv_deplibs_check_method=pass_all ;; esac ;; tpf*) lt_cv_deplibs_check_method=pass_all ;; esac fi { $as_echo "$as_me:${as_lineno-$LINENO}: result: $lt_cv_deplibs_check_method" >&5 $as_echo "$lt_cv_deplibs_check_method" >&6; } file_magic_glob= want_nocaseglob=no if test "$build" = "$host"; then case $host_os in mingw* | pw32*) if ( shopt | grep nocaseglob ) >/dev/null 2>&1; then want_nocaseglob=yes else file_magic_glob=`echo aAbBcCdDeEfFgGhHiIjJkKlLmMnNoOpPqQrRsStTuUvVwWxXyYzZ | $SED -e "s/\(..\)/s\/[\1]\/[\1]\/g;/g"` fi ;; esac fi file_magic_cmd=$lt_cv_file_magic_cmd deplibs_check_method=$lt_cv_deplibs_check_method test -z "$deplibs_check_method" && deplibs_check_method=unknown if test -n "$ac_tool_prefix"; then # Extract the first word of "${ac_tool_prefix}dlltool", so it can be a program name with args. set dummy ${ac_tool_prefix}dlltool; ac_word=$2 { $as_echo "$as_me:${as_lineno-$LINENO}: checking for $ac_word" >&5 $as_echo_n "checking for $ac_word... " >&6; } if ${ac_cv_prog_DLLTOOL+:} false; then : $as_echo_n "(cached) " >&6 else if test -n "$DLLTOOL"; then ac_cv_prog_DLLTOOL="$DLLTOOL" # Let the user override the test. else as_save_IFS=$IFS; IFS=$PATH_SEPARATOR for as_dir in $PATH do IFS=$as_save_IFS test -z "$as_dir" && as_dir=. for ac_exec_ext in '' $ac_executable_extensions; do if as_fn_executable_p "$as_dir/$ac_word$ac_exec_ext"; then ac_cv_prog_DLLTOOL="${ac_tool_prefix}dlltool" $as_echo "$as_me:${as_lineno-$LINENO}: found $as_dir/$ac_word$ac_exec_ext" >&5 break 2 fi done done IFS=$as_save_IFS fi fi DLLTOOL=$ac_cv_prog_DLLTOOL if test -n "$DLLTOOL"; then { $as_echo "$as_me:${as_lineno-$LINENO}: result: $DLLTOOL" >&5 $as_echo "$DLLTOOL" >&6; } else { $as_echo "$as_me:${as_lineno-$LINENO}: result: no" >&5 $as_echo "no" >&6; } fi fi if test -z "$ac_cv_prog_DLLTOOL"; then ac_ct_DLLTOOL=$DLLTOOL # Extract the first word of "dlltool", so it can be a program name with args. set dummy dlltool; ac_word=$2 { $as_echo "$as_me:${as_lineno-$LINENO}: checking for $ac_word" >&5 $as_echo_n "checking for $ac_word... " >&6; } if ${ac_cv_prog_ac_ct_DLLTOOL+:} false; then : $as_echo_n "(cached) " >&6 else if test -n "$ac_ct_DLLTOOL"; then ac_cv_prog_ac_ct_DLLTOOL="$ac_ct_DLLTOOL" # Let the user override the test. else as_save_IFS=$IFS; IFS=$PATH_SEPARATOR for as_dir in $PATH do IFS=$as_save_IFS test -z "$as_dir" && as_dir=. for ac_exec_ext in '' $ac_executable_extensions; do if as_fn_executable_p "$as_dir/$ac_word$ac_exec_ext"; then ac_cv_prog_ac_ct_DLLTOOL="dlltool" $as_echo "$as_me:${as_lineno-$LINENO}: found $as_dir/$ac_word$ac_exec_ext" >&5 break 2 fi done done IFS=$as_save_IFS fi fi ac_ct_DLLTOOL=$ac_cv_prog_ac_ct_DLLTOOL if test -n "$ac_ct_DLLTOOL"; then { $as_echo "$as_me:${as_lineno-$LINENO}: result: $ac_ct_DLLTOOL" >&5 $as_echo "$ac_ct_DLLTOOL" >&6; } else { $as_echo "$as_me:${as_lineno-$LINENO}: result: no" >&5 $as_echo "no" >&6; } fi if test "x$ac_ct_DLLTOOL" = x; then DLLTOOL="false" else case $cross_compiling:$ac_tool_warned in yes:) { $as_echo "$as_me:${as_lineno-$LINENO}: WARNING: using cross tools not prefixed with host triplet" >&5 $as_echo "$as_me: WARNING: using cross tools not prefixed with host triplet" >&2;} ac_tool_warned=yes ;; esac DLLTOOL=$ac_ct_DLLTOOL fi else DLLTOOL="$ac_cv_prog_DLLTOOL" fi test -z "$DLLTOOL" && DLLTOOL=dlltool { $as_echo "$as_me:${as_lineno-$LINENO}: checking how to associate runtime and link libraries" >&5 $as_echo_n "checking how to associate runtime and link libraries... " >&6; } if ${lt_cv_sharedlib_from_linklib_cmd+:} false; then : $as_echo_n "(cached) " >&6 else lt_cv_sharedlib_from_linklib_cmd='unknown' case $host_os in cygwin* | mingw* | pw32* | cegcc*) # two different shell functions defined in ltmain.sh # decide which to use based on capabilities of $DLLTOOL case `$DLLTOOL --help 2>&1` in *--identify-strict*) lt_cv_sharedlib_from_linklib_cmd=func_cygming_dll_for_implib ;; *) lt_cv_sharedlib_from_linklib_cmd=func_cygming_dll_for_implib_fallback ;; esac ;; *) # fallback: assume linklib IS sharedlib lt_cv_sharedlib_from_linklib_cmd="$ECHO" ;; esac fi { $as_echo "$as_me:${as_lineno-$LINENO}: result: $lt_cv_sharedlib_from_linklib_cmd" >&5 $as_echo "$lt_cv_sharedlib_from_linklib_cmd" >&6; } sharedlib_from_linklib_cmd=$lt_cv_sharedlib_from_linklib_cmd test -z "$sharedlib_from_linklib_cmd" && sharedlib_from_linklib_cmd=$ECHO if test -n "$ac_tool_prefix"; then for ac_prog in ar do # Extract the first word of "$ac_tool_prefix$ac_prog", so it can be a program name with args. set dummy $ac_tool_prefix$ac_prog; ac_word=$2 { $as_echo "$as_me:${as_lineno-$LINENO}: checking for $ac_word" >&5 $as_echo_n "checking for $ac_word... " >&6; } if ${ac_cv_prog_AR+:} false; then : $as_echo_n "(cached) " >&6 else if test -n "$AR"; then ac_cv_prog_AR="$AR" # Let the user override the test. else as_save_IFS=$IFS; IFS=$PATH_SEPARATOR for as_dir in $PATH do IFS=$as_save_IFS test -z "$as_dir" && as_dir=. for ac_exec_ext in '' $ac_executable_extensions; do if as_fn_executable_p "$as_dir/$ac_word$ac_exec_ext"; then ac_cv_prog_AR="$ac_tool_prefix$ac_prog" $as_echo "$as_me:${as_lineno-$LINENO}: found $as_dir/$ac_word$ac_exec_ext" >&5 break 2 fi done done IFS=$as_save_IFS fi fi AR=$ac_cv_prog_AR if test -n "$AR"; then { $as_echo "$as_me:${as_lineno-$LINENO}: result: $AR" >&5 $as_echo "$AR" >&6; } else { $as_echo "$as_me:${as_lineno-$LINENO}: result: no" >&5 $as_echo "no" >&6; } fi test -n "$AR" && break done fi if test -z "$AR"; then ac_ct_AR=$AR for ac_prog in ar do # Extract the first word of "$ac_prog", so it can be a program name with args. set dummy $ac_prog; ac_word=$2 { $as_echo "$as_me:${as_lineno-$LINENO}: checking for $ac_word" >&5 $as_echo_n "checking for $ac_word... " >&6; } if ${ac_cv_prog_ac_ct_AR+:} false; then : $as_echo_n "(cached) " >&6 else if test -n "$ac_ct_AR"; then ac_cv_prog_ac_ct_AR="$ac_ct_AR" # Let the user override the test. else as_save_IFS=$IFS; IFS=$PATH_SEPARATOR for as_dir in $PATH do IFS=$as_save_IFS test -z "$as_dir" && as_dir=. for ac_exec_ext in '' $ac_executable_extensions; do if as_fn_executable_p "$as_dir/$ac_word$ac_exec_ext"; then ac_cv_prog_ac_ct_AR="$ac_prog" $as_echo "$as_me:${as_lineno-$LINENO}: found $as_dir/$ac_word$ac_exec_ext" >&5 break 2 fi done done IFS=$as_save_IFS fi fi ac_ct_AR=$ac_cv_prog_ac_ct_AR if test -n "$ac_ct_AR"; then { $as_echo "$as_me:${as_lineno-$LINENO}: result: $ac_ct_AR" >&5 $as_echo "$ac_ct_AR" >&6; } else { $as_echo "$as_me:${as_lineno-$LINENO}: result: no" >&5 $as_echo "no" >&6; } fi test -n "$ac_ct_AR" && break done if test "x$ac_ct_AR" = x; then AR="false" else case $cross_compiling:$ac_tool_warned in yes:) { $as_echo "$as_me:${as_lineno-$LINENO}: WARNING: using cross tools not prefixed with host triplet" >&5 $as_echo "$as_me: WARNING: using cross tools not prefixed with host triplet" >&2;} ac_tool_warned=yes ;; esac AR=$ac_ct_AR fi fi : ${AR=ar} : ${AR_FLAGS=cru} { $as_echo "$as_me:${as_lineno-$LINENO}: checking for archiver @FILE support" >&5 $as_echo_n "checking for archiver @FILE support... " >&6; } if ${lt_cv_ar_at_file+:} false; then : $as_echo_n "(cached) " >&6 else lt_cv_ar_at_file=no cat confdefs.h - <<_ACEOF >conftest.$ac_ext /* end confdefs.h. */ int main () { ; return 0; } _ACEOF if ac_fn_c_try_compile "$LINENO"; then : echo conftest.$ac_objext > conftest.lst lt_ar_try='$AR $AR_FLAGS libconftest.a @conftest.lst >&5' { { eval echo "\"\$as_me\":${as_lineno-$LINENO}: \"$lt_ar_try\""; } >&5 (eval $lt_ar_try) 2>&5 ac_status=$? $as_echo "$as_me:${as_lineno-$LINENO}: \$? = $ac_status" >&5 test $ac_status = 0; } if test "$ac_status" -eq 0; then # Ensure the archiver fails upon bogus file names. rm -f conftest.$ac_objext libconftest.a { { eval echo "\"\$as_me\":${as_lineno-$LINENO}: \"$lt_ar_try\""; } >&5 (eval $lt_ar_try) 2>&5 ac_status=$? $as_echo "$as_me:${as_lineno-$LINENO}: \$? = $ac_status" >&5 test $ac_status = 0; } if test "$ac_status" -ne 0; then lt_cv_ar_at_file=@ fi fi rm -f conftest.* libconftest.a fi rm -f core conftest.err conftest.$ac_objext conftest.$ac_ext fi { $as_echo "$as_me:${as_lineno-$LINENO}: result: $lt_cv_ar_at_file" >&5 $as_echo "$lt_cv_ar_at_file" >&6; } if test "x$lt_cv_ar_at_file" = xno; then archiver_list_spec= else archiver_list_spec=$lt_cv_ar_at_file fi if test -n "$ac_tool_prefix"; then # Extract the first word of "${ac_tool_prefix}strip", so it can be a program name with args. set dummy ${ac_tool_prefix}strip; ac_word=$2 { $as_echo "$as_me:${as_lineno-$LINENO}: checking for $ac_word" >&5 $as_echo_n "checking for $ac_word... " >&6; } if ${ac_cv_prog_STRIP+:} false; then : $as_echo_n "(cached) " >&6 else if test -n "$STRIP"; then ac_cv_prog_STRIP="$STRIP" # Let the user override the test. else as_save_IFS=$IFS; IFS=$PATH_SEPARATOR for as_dir in $PATH do IFS=$as_save_IFS test -z "$as_dir" && as_dir=. for ac_exec_ext in '' $ac_executable_extensions; do if as_fn_executable_p "$as_dir/$ac_word$ac_exec_ext"; then ac_cv_prog_STRIP="${ac_tool_prefix}strip" $as_echo "$as_me:${as_lineno-$LINENO}: found $as_dir/$ac_word$ac_exec_ext" >&5 break 2 fi done done IFS=$as_save_IFS fi fi STRIP=$ac_cv_prog_STRIP if test -n "$STRIP"; then { $as_echo "$as_me:${as_lineno-$LINENO}: result: $STRIP" >&5 $as_echo "$STRIP" >&6; } else { $as_echo "$as_me:${as_lineno-$LINENO}: result: no" >&5 $as_echo "no" >&6; } fi fi if test -z "$ac_cv_prog_STRIP"; then ac_ct_STRIP=$STRIP # Extract the first word of "strip", so it can be a program name with args. set dummy strip; ac_word=$2 { $as_echo "$as_me:${as_lineno-$LINENO}: checking for $ac_word" >&5 $as_echo_n "checking for $ac_word... " >&6; } if ${ac_cv_prog_ac_ct_STRIP+:} false; then : $as_echo_n "(cached) " >&6 else if test -n "$ac_ct_STRIP"; then ac_cv_prog_ac_ct_STRIP="$ac_ct_STRIP" # Let the user override the test. else as_save_IFS=$IFS; IFS=$PATH_SEPARATOR for as_dir in $PATH do IFS=$as_save_IFS test -z "$as_dir" && as_dir=. for ac_exec_ext in '' $ac_executable_extensions; do if as_fn_executable_p "$as_dir/$ac_word$ac_exec_ext"; then ac_cv_prog_ac_ct_STRIP="strip" $as_echo "$as_me:${as_lineno-$LINENO}: found $as_dir/$ac_word$ac_exec_ext" >&5 break 2 fi done done IFS=$as_save_IFS fi fi ac_ct_STRIP=$ac_cv_prog_ac_ct_STRIP if test -n "$ac_ct_STRIP"; then { $as_echo "$as_me:${as_lineno-$LINENO}: result: $ac_ct_STRIP" >&5 $as_echo "$ac_ct_STRIP" >&6; } else { $as_echo "$as_me:${as_lineno-$LINENO}: result: no" >&5 $as_echo "no" >&6; } fi if test "x$ac_ct_STRIP" = x; then STRIP=":" else case $cross_compiling:$ac_tool_warned in yes:) { $as_echo "$as_me:${as_lineno-$LINENO}: WARNING: using cross tools not prefixed with host triplet" >&5 $as_echo "$as_me: WARNING: using cross tools not prefixed with host triplet" >&2;} ac_tool_warned=yes ;; esac STRIP=$ac_ct_STRIP fi else STRIP="$ac_cv_prog_STRIP" fi test -z "$STRIP" && STRIP=: if test -n "$ac_tool_prefix"; then # Extract the first word of "${ac_tool_prefix}ranlib", so it can be a program name with args. set dummy ${ac_tool_prefix}ranlib; ac_word=$2 { $as_echo "$as_me:${as_lineno-$LINENO}: checking for $ac_word" >&5 $as_echo_n "checking for $ac_word... " >&6; } if ${ac_cv_prog_RANLIB+:} false; then : $as_echo_n "(cached) " >&6 else if test -n "$RANLIB"; then ac_cv_prog_RANLIB="$RANLIB" # Let the user override the test. else as_save_IFS=$IFS; IFS=$PATH_SEPARATOR for as_dir in $PATH do IFS=$as_save_IFS test -z "$as_dir" && as_dir=. for ac_exec_ext in '' $ac_executable_extensions; do if as_fn_executable_p "$as_dir/$ac_word$ac_exec_ext"; then ac_cv_prog_RANLIB="${ac_tool_prefix}ranlib" $as_echo "$as_me:${as_lineno-$LINENO}: found $as_dir/$ac_word$ac_exec_ext" >&5 break 2 fi done done IFS=$as_save_IFS fi fi RANLIB=$ac_cv_prog_RANLIB if test -n "$RANLIB"; then { $as_echo "$as_me:${as_lineno-$LINENO}: result: $RANLIB" >&5 $as_echo "$RANLIB" >&6; } else { $as_echo "$as_me:${as_lineno-$LINENO}: result: no" >&5 $as_echo "no" >&6; } fi fi if test -z "$ac_cv_prog_RANLIB"; then ac_ct_RANLIB=$RANLIB # Extract the first word of "ranlib", so it can be a program name with args. set dummy ranlib; ac_word=$2 { $as_echo "$as_me:${as_lineno-$LINENO}: checking for $ac_word" >&5 $as_echo_n "checking for $ac_word... " >&6; } if ${ac_cv_prog_ac_ct_RANLIB+:} false; then : $as_echo_n "(cached) " >&6 else if test -n "$ac_ct_RANLIB"; then ac_cv_prog_ac_ct_RANLIB="$ac_ct_RANLIB" # Let the user override the test. else as_save_IFS=$IFS; IFS=$PATH_SEPARATOR for as_dir in $PATH do IFS=$as_save_IFS test -z "$as_dir" && as_dir=. for ac_exec_ext in '' $ac_executable_extensions; do if as_fn_executable_p "$as_dir/$ac_word$ac_exec_ext"; then ac_cv_prog_ac_ct_RANLIB="ranlib" $as_echo "$as_me:${as_lineno-$LINENO}: found $as_dir/$ac_word$ac_exec_ext" >&5 break 2 fi done done IFS=$as_save_IFS fi fi ac_ct_RANLIB=$ac_cv_prog_ac_ct_RANLIB if test -n "$ac_ct_RANLIB"; then { $as_echo "$as_me:${as_lineno-$LINENO}: result: $ac_ct_RANLIB" >&5 $as_echo "$ac_ct_RANLIB" >&6; } else { $as_echo "$as_me:${as_lineno-$LINENO}: result: no" >&5 $as_echo "no" >&6; } fi if test "x$ac_ct_RANLIB" = x; then RANLIB=":" else case $cross_compiling:$ac_tool_warned in yes:) { $as_echo "$as_me:${as_lineno-$LINENO}: WARNING: using cross tools not prefixed with host triplet" >&5 $as_echo "$as_me: WARNING: using cross tools not prefixed with host triplet" >&2;} ac_tool_warned=yes ;; esac RANLIB=$ac_ct_RANLIB fi else RANLIB="$ac_cv_prog_RANLIB" fi test -z "$RANLIB" && RANLIB=: # Determine commands to create old-style static archives. old_archive_cmds='$AR $AR_FLAGS $oldlib$oldobjs' old_postinstall_cmds='chmod 644 $oldlib' old_postuninstall_cmds= if test -n "$RANLIB"; then case $host_os in openbsd*) old_postinstall_cmds="$old_postinstall_cmds~\$RANLIB -t \$tool_oldlib" ;; *) old_postinstall_cmds="$old_postinstall_cmds~\$RANLIB \$tool_oldlib" ;; esac old_archive_cmds="$old_archive_cmds~\$RANLIB \$tool_oldlib" fi case $host_os in darwin*) lock_old_archive_extraction=yes ;; *) lock_old_archive_extraction=no ;; esac # If no C compiler was specified, use CC. LTCC=${LTCC-"$CC"} # If no C compiler flags were specified, use CFLAGS. LTCFLAGS=${LTCFLAGS-"$CFLAGS"} # Allow CC to be a program name with arguments. compiler=$CC # Check for command to grab the raw symbol name followed by C symbol from nm. { $as_echo "$as_me:${as_lineno-$LINENO}: checking command to parse $NM output from $compiler object" >&5 $as_echo_n "checking command to parse $NM output from $compiler object... " >&6; } if ${lt_cv_sys_global_symbol_pipe+:} false; then : $as_echo_n "(cached) " >&6 else # These are sane defaults that work on at least a few old systems. # [They come from Ultrix. What could be older than Ultrix?!! ;)] # Character class describing NM global symbol codes. symcode='[BCDEGRST]' # Regexp to match symbols that can be accessed directly from C. sympat='\([_A-Za-z][_A-Za-z0-9]*\)' # Define system-specific variables. case $host_os in aix*) symcode='[BCDT]' ;; cygwin* | mingw* | pw32* | cegcc*) symcode='[ABCDGISTW]' ;; hpux*) if test "$host_cpu" = ia64; then symcode='[ABCDEGRST]' fi ;; irix* | nonstopux*) symcode='[BCDEGRST]' ;; osf*) symcode='[BCDEGQRST]' ;; solaris*) symcode='[BDRT]' ;; sco3.2v5*) symcode='[DT]' ;; sysv4.2uw2*) symcode='[DT]' ;; sysv5* | sco5v6* | unixware* | OpenUNIX*) symcode='[ABDT]' ;; sysv4) symcode='[DFNSTU]' ;; esac # If we're using GNU nm, then use its standard symbol codes. case `$NM -V 2>&1` in *GNU* | *'with BFD'*) symcode='[ABCDGIRSTW]' ;; esac # Transform an extracted symbol line into a proper C declaration. # Some systems (esp. on ia64) link data and code symbols differently, # so use this general approach. lt_cv_sys_global_symbol_to_cdecl="sed -n -e 's/^T .* \(.*\)$/extern int \1();/p' -e 's/^$symcode* .* \(.*\)$/extern char \1;/p'" # Transform an extracted symbol line into symbol name and symbol address lt_cv_sys_global_symbol_to_c_name_address="sed -n -e 's/^: \([^ ]*\)[ ]*$/ {\\\"\1\\\", (void *) 0},/p' -e 's/^$symcode* \([^ ]*\) \([^ ]*\)$/ {\"\2\", (void *) \&\2},/p'" lt_cv_sys_global_symbol_to_c_name_address_lib_prefix="sed -n -e 's/^: \([^ ]*\)[ ]*$/ {\\\"\1\\\", (void *) 0},/p' -e 's/^$symcode* \([^ ]*\) \(lib[^ ]*\)$/ {\"\2\", (void *) \&\2},/p' -e 's/^$symcode* \([^ ]*\) \([^ ]*\)$/ {\"lib\2\", (void *) \&\2},/p'" # Handle CRLF in mingw tool chain opt_cr= case $build_os in mingw*) opt_cr=`$ECHO 'x\{0,1\}' | tr x '\015'` # option cr in regexp ;; esac # Try without a prefix underscore, then with it. for ac_symprfx in "" "_"; do # Transform symcode, sympat, and symprfx into a raw symbol and a C symbol. symxfrm="\\1 $ac_symprfx\\2 \\2" # Write the raw and C identifiers. if test "$lt_cv_nm_interface" = "MS dumpbin"; then # Fake it for dumpbin and say T for any non-static function # and D for any global variable. # Also find C++ and __fastcall symbols from MSVC++, # which start with @ or ?. lt_cv_sys_global_symbol_pipe="$AWK '"\ " {last_section=section; section=\$ 3};"\ " /^COFF SYMBOL TABLE/{for(i in hide) delete hide[i]};"\ " /Section length .*#relocs.*(pick any)/{hide[last_section]=1};"\ " \$ 0!~/External *\|/{next};"\ " / 0+ UNDEF /{next}; / UNDEF \([^|]\)*()/{next};"\ " {if(hide[section]) next};"\ " {f=0}; \$ 0~/\(\).*\|/{f=1}; {printf f ? \"T \" : \"D \"};"\ " {split(\$ 0, a, /\||\r/); split(a[2], s)};"\ " s[1]~/^[@?]/{print s[1], s[1]; next};"\ " s[1]~prfx {split(s[1],t,\"@\"); print t[1], substr(t[1],length(prfx))}"\ " ' prfx=^$ac_symprfx" else lt_cv_sys_global_symbol_pipe="sed -n -e 's/^.*[ ]\($symcode$symcode*\)[ ][ ]*$ac_symprfx$sympat$opt_cr$/$symxfrm/p'" fi lt_cv_sys_global_symbol_pipe="$lt_cv_sys_global_symbol_pipe | sed '/ __gnu_lto/d'" # Check to see that the pipe works correctly. pipe_works=no rm -f conftest* cat > conftest.$ac_ext <<_LT_EOF #ifdef __cplusplus extern "C" { #endif char nm_test_var; void nm_test_func(void); void nm_test_func(void){} #ifdef __cplusplus } #endif int main(){nm_test_var='a';nm_test_func();return(0);} _LT_EOF if { { eval echo "\"\$as_me\":${as_lineno-$LINENO}: \"$ac_compile\""; } >&5 (eval $ac_compile) 2>&5 ac_status=$? $as_echo "$as_me:${as_lineno-$LINENO}: \$? = $ac_status" >&5 test $ac_status = 0; }; then # Now try to grab the symbols. nlist=conftest.nm if { { eval echo "\"\$as_me\":${as_lineno-$LINENO}: \"$NM conftest.$ac_objext \| "$lt_cv_sys_global_symbol_pipe" \> $nlist\""; } >&5 (eval $NM conftest.$ac_objext \| "$lt_cv_sys_global_symbol_pipe" \> $nlist) 2>&5 ac_status=$? $as_echo "$as_me:${as_lineno-$LINENO}: \$? = $ac_status" >&5 test $ac_status = 0; } && test -s "$nlist"; then # Try sorting and uniquifying the output. if sort "$nlist" | uniq > "$nlist"T; then mv -f "$nlist"T "$nlist" else rm -f "$nlist"T fi # Make sure that we snagged all the symbols we need. if $GREP ' nm_test_var$' "$nlist" >/dev/null; then if $GREP ' nm_test_func$' "$nlist" >/dev/null; then cat <<_LT_EOF > conftest.$ac_ext /* Keep this code in sync between libtool.m4, ltmain, lt_system.h, and tests. */ #if defined(_WIN32) || defined(__CYGWIN__) || defined(_WIN32_WCE) /* DATA imports from DLLs on WIN32 con't be const, because runtime relocations are performed -- see ld's documentation on pseudo-relocs. */ # define LT_DLSYM_CONST #elif defined(__osf__) /* This system does not cope well with relocations in const data. */ # define LT_DLSYM_CONST #else # define LT_DLSYM_CONST const #endif #ifdef __cplusplus extern "C" { #endif _LT_EOF # Now generate the symbol file. eval "$lt_cv_sys_global_symbol_to_cdecl"' < "$nlist" | $GREP -v main >> conftest.$ac_ext' cat <<_LT_EOF >> conftest.$ac_ext /* The mapping between symbol names and symbols. */ LT_DLSYM_CONST struct { const char *name; void *address; } lt__PROGRAM__LTX_preloaded_symbols[] = { { "@PROGRAM@", (void *) 0 }, _LT_EOF $SED "s/^$symcode$symcode* \(.*\) \(.*\)$/ {\"\2\", (void *) \&\2},/" < "$nlist" | $GREP -v main >> conftest.$ac_ext cat <<\_LT_EOF >> conftest.$ac_ext {0, (void *) 0} }; /* This works around a problem in FreeBSD linker */ #ifdef FREEBSD_WORKAROUND static const void *lt_preloaded_setup() { return lt__PROGRAM__LTX_preloaded_symbols; } #endif #ifdef __cplusplus } #endif _LT_EOF # Now try linking the two files. mv conftest.$ac_objext conftstm.$ac_objext lt_globsym_save_LIBS=$LIBS lt_globsym_save_CFLAGS=$CFLAGS LIBS="conftstm.$ac_objext" CFLAGS="$CFLAGS$lt_prog_compiler_no_builtin_flag" if { { eval echo "\"\$as_me\":${as_lineno-$LINENO}: \"$ac_link\""; } >&5 (eval $ac_link) 2>&5 ac_status=$? $as_echo "$as_me:${as_lineno-$LINENO}: \$? = $ac_status" >&5 test $ac_status = 0; } && test -s conftest${ac_exeext}; then pipe_works=yes fi LIBS=$lt_globsym_save_LIBS CFLAGS=$lt_globsym_save_CFLAGS else echo "cannot find nm_test_func in $nlist" >&5 fi else echo "cannot find nm_test_var in $nlist" >&5 fi else echo "cannot run $lt_cv_sys_global_symbol_pipe" >&5 fi else echo "$progname: failed program was:" >&5 cat conftest.$ac_ext >&5 fi rm -rf conftest* conftst* # Do not use the global_symbol_pipe unless it works. if test "$pipe_works" = yes; then break else lt_cv_sys_global_symbol_pipe= fi done fi if test -z "$lt_cv_sys_global_symbol_pipe"; then lt_cv_sys_global_symbol_to_cdecl= fi if test -z "$lt_cv_sys_global_symbol_pipe$lt_cv_sys_global_symbol_to_cdecl"; then { $as_echo "$as_me:${as_lineno-$LINENO}: result: failed" >&5 $as_echo "failed" >&6; } else { $as_echo "$as_me:${as_lineno-$LINENO}: result: ok" >&5 $as_echo "ok" >&6; } fi # Response file support. if test "$lt_cv_nm_interface" = "MS dumpbin"; then nm_file_list_spec='@' elif $NM --help 2>/dev/null | grep '[@]FILE' >/dev/null; then nm_file_list_spec='@' fi { $as_echo "$as_me:${as_lineno-$LINENO}: checking for sysroot" >&5 $as_echo_n "checking for sysroot... " >&6; } # Check whether --with-sysroot was given. if test "${with_sysroot+set}" = set; then : withval=$with_sysroot; else with_sysroot=no fi lt_sysroot= case ${with_sysroot} in #( yes) if test "$GCC" = yes; then lt_sysroot=`$CC --print-sysroot 2>/dev/null` fi ;; #( /*) lt_sysroot=`echo "$with_sysroot" | sed -e "$sed_quote_subst"` ;; #( no|'') ;; #( *) { $as_echo "$as_me:${as_lineno-$LINENO}: result: ${with_sysroot}" >&5 $as_echo "${with_sysroot}" >&6; } as_fn_error $? "The sysroot must be an absolute path." "$LINENO" 5 ;; esac { $as_echo "$as_me:${as_lineno-$LINENO}: result: ${lt_sysroot:-no}" >&5 $as_echo "${lt_sysroot:-no}" >&6; } # Check whether --enable-libtool-lock was given. if test "${enable_libtool_lock+set}" = set; then : enableval=$enable_libtool_lock; fi test "x$enable_libtool_lock" != xno && enable_libtool_lock=yes # Some flags need to be propagated to the compiler or linker for good # libtool support. case $host in ia64-*-hpux*) # Find out which ABI we are using. echo 'int i;' > conftest.$ac_ext if { { eval echo "\"\$as_me\":${as_lineno-$LINENO}: \"$ac_compile\""; } >&5 (eval $ac_compile) 2>&5 ac_status=$? $as_echo "$as_me:${as_lineno-$LINENO}: \$? = $ac_status" >&5 test $ac_status = 0; }; then case `/usr/bin/file conftest.$ac_objext` in *ELF-32*) HPUX_IA64_MODE="32" ;; *ELF-64*) HPUX_IA64_MODE="64" ;; esac fi rm -rf conftest* ;; *-*-irix6*) # Find out which ABI we are using. echo '#line '$LINENO' "configure"' > conftest.$ac_ext if { { eval echo "\"\$as_me\":${as_lineno-$LINENO}: \"$ac_compile\""; } >&5 (eval $ac_compile) 2>&5 ac_status=$? $as_echo "$as_me:${as_lineno-$LINENO}: \$? = $ac_status" >&5 test $ac_status = 0; }; then if test "$lt_cv_prog_gnu_ld" = yes; then case `/usr/bin/file conftest.$ac_objext` in *32-bit*) LD="${LD-ld} -melf32bsmip" ;; *N32*) LD="${LD-ld} -melf32bmipn32" ;; *64-bit*) LD="${LD-ld} -melf64bmip" ;; esac else case `/usr/bin/file conftest.$ac_objext` in *32-bit*) LD="${LD-ld} -32" ;; *N32*) LD="${LD-ld} -n32" ;; *64-bit*) LD="${LD-ld} -64" ;; esac fi fi rm -rf conftest* ;; x86_64-*kfreebsd*-gnu|x86_64-*linux*|ppc*-*linux*|powerpc*-*linux*| \ s390*-*linux*|s390*-*tpf*|sparc*-*linux*) # Find out which ABI we are using. echo 'int i;' > conftest.$ac_ext if { { eval echo "\"\$as_me\":${as_lineno-$LINENO}: \"$ac_compile\""; } >&5 (eval $ac_compile) 2>&5 ac_status=$? $as_echo "$as_me:${as_lineno-$LINENO}: \$? = $ac_status" >&5 test $ac_status = 0; }; then case `/usr/bin/file conftest.o` in *32-bit*) case $host in x86_64-*kfreebsd*-gnu) LD="${LD-ld} -m elf_i386_fbsd" ;; x86_64-*linux*) LD="${LD-ld} -m elf_i386" ;; ppc64-*linux*|powerpc64-*linux*) LD="${LD-ld} -m elf32ppclinux" ;; s390x-*linux*) LD="${LD-ld} -m elf_s390" ;; sparc64-*linux*) LD="${LD-ld} -m elf32_sparc" ;; esac ;; *64-bit*) case $host in x86_64-*kfreebsd*-gnu) LD="${LD-ld} -m elf_x86_64_fbsd" ;; x86_64-*linux*) LD="${LD-ld} -m elf_x86_64" ;; ppc*-*linux*|powerpc*-*linux*) LD="${LD-ld} -m elf64ppc" ;; s390*-*linux*|s390*-*tpf*) LD="${LD-ld} -m elf64_s390" ;; sparc*-*linux*) LD="${LD-ld} -m elf64_sparc" ;; esac ;; esac fi rm -rf conftest* ;; *-*-sco3.2v5*) # On SCO OpenServer 5, we need -belf to get full-featured binaries. SAVE_CFLAGS="$CFLAGS" CFLAGS="$CFLAGS -belf" { $as_echo "$as_me:${as_lineno-$LINENO}: checking whether the C compiler needs -belf" >&5 $as_echo_n "checking whether the C compiler needs -belf... " >&6; } if ${lt_cv_cc_needs_belf+:} false; then : $as_echo_n "(cached) " >&6 else ac_ext=c ac_cpp='$CPP $CPPFLAGS' ac_compile='$CC -c $CFLAGS $CPPFLAGS conftest.$ac_ext >&5' ac_link='$CC -o conftest$ac_exeext $CFLAGS $CPPFLAGS $LDFLAGS conftest.$ac_ext $LIBS >&5' ac_compiler_gnu=$ac_cv_c_compiler_gnu cat confdefs.h - <<_ACEOF >conftest.$ac_ext /* end confdefs.h. */ int main () { ; return 0; } _ACEOF if ac_fn_c_try_link "$LINENO"; then : lt_cv_cc_needs_belf=yes else lt_cv_cc_needs_belf=no fi rm -f core conftest.err conftest.$ac_objext \ conftest$ac_exeext conftest.$ac_ext ac_ext=c ac_cpp='$CPP $CPPFLAGS' ac_compile='$CC -c $CFLAGS $CPPFLAGS conftest.$ac_ext >&5' ac_link='$CC -o conftest$ac_exeext $CFLAGS $CPPFLAGS $LDFLAGS conftest.$ac_ext $LIBS >&5' ac_compiler_gnu=$ac_cv_c_compiler_gnu fi { $as_echo "$as_me:${as_lineno-$LINENO}: result: $lt_cv_cc_needs_belf" >&5 $as_echo "$lt_cv_cc_needs_belf" >&6; } if test x"$lt_cv_cc_needs_belf" != x"yes"; then # this is probably gcc 2.8.0, egcs 1.0 or newer; no need for -belf CFLAGS="$SAVE_CFLAGS" fi ;; *-*solaris*) # Find out which ABI we are using. echo 'int i;' > conftest.$ac_ext if { { eval echo "\"\$as_me\":${as_lineno-$LINENO}: \"$ac_compile\""; } >&5 (eval $ac_compile) 2>&5 ac_status=$? $as_echo "$as_me:${as_lineno-$LINENO}: \$? = $ac_status" >&5 test $ac_status = 0; }; then case `/usr/bin/file conftest.o` in *64-bit*) case $lt_cv_prog_gnu_ld in yes*) case $host in i?86-*-solaris*) LD="${LD-ld} -m elf_x86_64" ;; sparc*-*-solaris*) LD="${LD-ld} -m elf64_sparc" ;; esac # GNU ld 2.21 introduced _sol2 emulations. Use them if available. if ${LD-ld} -V | grep _sol2 >/dev/null 2>&1; then LD="${LD-ld}_sol2" fi ;; *) if ${LD-ld} -64 -r -o conftest2.o conftest.o >/dev/null 2>&1; then LD="${LD-ld} -64" fi ;; esac ;; esac fi rm -rf conftest* ;; esac need_locks="$enable_libtool_lock" if test -n "$ac_tool_prefix"; then # Extract the first word of "${ac_tool_prefix}mt", so it can be a program name with args. set dummy ${ac_tool_prefix}mt; ac_word=$2 { $as_echo "$as_me:${as_lineno-$LINENO}: checking for $ac_word" >&5 $as_echo_n "checking for $ac_word... " >&6; } if ${ac_cv_prog_MANIFEST_TOOL+:} false; then : $as_echo_n "(cached) " >&6 else if test -n "$MANIFEST_TOOL"; then ac_cv_prog_MANIFEST_TOOL="$MANIFEST_TOOL" # Let the user override the test. else as_save_IFS=$IFS; IFS=$PATH_SEPARATOR for as_dir in $PATH do IFS=$as_save_IFS test -z "$as_dir" && as_dir=. for ac_exec_ext in '' $ac_executable_extensions; do if as_fn_executable_p "$as_dir/$ac_word$ac_exec_ext"; then ac_cv_prog_MANIFEST_TOOL="${ac_tool_prefix}mt" $as_echo "$as_me:${as_lineno-$LINENO}: found $as_dir/$ac_word$ac_exec_ext" >&5 break 2 fi done done IFS=$as_save_IFS fi fi MANIFEST_TOOL=$ac_cv_prog_MANIFEST_TOOL if test -n "$MANIFEST_TOOL"; then { $as_echo "$as_me:${as_lineno-$LINENO}: result: $MANIFEST_TOOL" >&5 $as_echo "$MANIFEST_TOOL" >&6; } else { $as_echo "$as_me:${as_lineno-$LINENO}: result: no" >&5 $as_echo "no" >&6; } fi fi if test -z "$ac_cv_prog_MANIFEST_TOOL"; then ac_ct_MANIFEST_TOOL=$MANIFEST_TOOL # Extract the first word of "mt", so it can be a program name with args. set dummy mt; ac_word=$2 { $as_echo "$as_me:${as_lineno-$LINENO}: checking for $ac_word" >&5 $as_echo_n "checking for $ac_word... " >&6; } if ${ac_cv_prog_ac_ct_MANIFEST_TOOL+:} false; then : $as_echo_n "(cached) " >&6 else if test -n "$ac_ct_MANIFEST_TOOL"; then ac_cv_prog_ac_ct_MANIFEST_TOOL="$ac_ct_MANIFEST_TOOL" # Let the user override the test. else as_save_IFS=$IFS; IFS=$PATH_SEPARATOR for as_dir in $PATH do IFS=$as_save_IFS test -z "$as_dir" && as_dir=. for ac_exec_ext in '' $ac_executable_extensions; do if as_fn_executable_p "$as_dir/$ac_word$ac_exec_ext"; then ac_cv_prog_ac_ct_MANIFEST_TOOL="mt" $as_echo "$as_me:${as_lineno-$LINENO}: found $as_dir/$ac_word$ac_exec_ext" >&5 break 2 fi done done IFS=$as_save_IFS fi fi ac_ct_MANIFEST_TOOL=$ac_cv_prog_ac_ct_MANIFEST_TOOL if test -n "$ac_ct_MANIFEST_TOOL"; then { $as_echo "$as_me:${as_lineno-$LINENO}: result: $ac_ct_MANIFEST_TOOL" >&5 $as_echo "$ac_ct_MANIFEST_TOOL" >&6; } else { $as_echo "$as_me:${as_lineno-$LINENO}: result: no" >&5 $as_echo "no" >&6; } fi if test "x$ac_ct_MANIFEST_TOOL" = x; then MANIFEST_TOOL=":" else case $cross_compiling:$ac_tool_warned in yes:) { $as_echo "$as_me:${as_lineno-$LINENO}: WARNING: using cross tools not prefixed with host triplet" >&5 $as_echo "$as_me: WARNING: using cross tools not prefixed with host triplet" >&2;} ac_tool_warned=yes ;; esac MANIFEST_TOOL=$ac_ct_MANIFEST_TOOL fi else MANIFEST_TOOL="$ac_cv_prog_MANIFEST_TOOL" fi test -z "$MANIFEST_TOOL" && MANIFEST_TOOL=mt { $as_echo "$as_me:${as_lineno-$LINENO}: checking if $MANIFEST_TOOL is a manifest tool" >&5 $as_echo_n "checking if $MANIFEST_TOOL is a manifest tool... " >&6; } if ${lt_cv_path_mainfest_tool+:} false; then : $as_echo_n "(cached) " >&6 else lt_cv_path_mainfest_tool=no echo "$as_me:$LINENO: $MANIFEST_TOOL '-?'" >&5 $MANIFEST_TOOL '-?' 2>conftest.err > conftest.out cat conftest.err >&5 if $GREP 'Manifest Tool' conftest.out > /dev/null; then lt_cv_path_mainfest_tool=yes fi rm -f conftest* fi { $as_echo "$as_me:${as_lineno-$LINENO}: result: $lt_cv_path_mainfest_tool" >&5 $as_echo "$lt_cv_path_mainfest_tool" >&6; } if test "x$lt_cv_path_mainfest_tool" != xyes; then MANIFEST_TOOL=: fi case $host_os in rhapsody* | darwin*) if test -n "$ac_tool_prefix"; then # Extract the first word of "${ac_tool_prefix}dsymutil", so it can be a program name with args. set dummy ${ac_tool_prefix}dsymutil; ac_word=$2 { $as_echo "$as_me:${as_lineno-$LINENO}: checking for $ac_word" >&5 $as_echo_n "checking for $ac_word... " >&6; } if ${ac_cv_prog_DSYMUTIL+:} false; then : $as_echo_n "(cached) " >&6 else if test -n "$DSYMUTIL"; then ac_cv_prog_DSYMUTIL="$DSYMUTIL" # Let the user override the test. else as_save_IFS=$IFS; IFS=$PATH_SEPARATOR for as_dir in $PATH do IFS=$as_save_IFS test -z "$as_dir" && as_dir=. for ac_exec_ext in '' $ac_executable_extensions; do if as_fn_executable_p "$as_dir/$ac_word$ac_exec_ext"; then ac_cv_prog_DSYMUTIL="${ac_tool_prefix}dsymutil" $as_echo "$as_me:${as_lineno-$LINENO}: found $as_dir/$ac_word$ac_exec_ext" >&5 break 2 fi done done IFS=$as_save_IFS fi fi DSYMUTIL=$ac_cv_prog_DSYMUTIL if test -n "$DSYMUTIL"; then { $as_echo "$as_me:${as_lineno-$LINENO}: result: $DSYMUTIL" >&5 $as_echo "$DSYMUTIL" >&6; } else { $as_echo "$as_me:${as_lineno-$LINENO}: result: no" >&5 $as_echo "no" >&6; } fi fi if test -z "$ac_cv_prog_DSYMUTIL"; then ac_ct_DSYMUTIL=$DSYMUTIL # Extract the first word of "dsymutil", so it can be a program name with args. set dummy dsymutil; ac_word=$2 { $as_echo "$as_me:${as_lineno-$LINENO}: checking for $ac_word" >&5 $as_echo_n "checking for $ac_word... " >&6; } if ${ac_cv_prog_ac_ct_DSYMUTIL+:} false; then : $as_echo_n "(cached) " >&6 else if test -n "$ac_ct_DSYMUTIL"; then ac_cv_prog_ac_ct_DSYMUTIL="$ac_ct_DSYMUTIL" # Let the user override the test. else as_save_IFS=$IFS; IFS=$PATH_SEPARATOR for as_dir in $PATH do IFS=$as_save_IFS test -z "$as_dir" && as_dir=. for ac_exec_ext in '' $ac_executable_extensions; do if as_fn_executable_p "$as_dir/$ac_word$ac_exec_ext"; then ac_cv_prog_ac_ct_DSYMUTIL="dsymutil" $as_echo "$as_me:${as_lineno-$LINENO}: found $as_dir/$ac_word$ac_exec_ext" >&5 break 2 fi done done IFS=$as_save_IFS fi fi ac_ct_DSYMUTIL=$ac_cv_prog_ac_ct_DSYMUTIL if test -n "$ac_ct_DSYMUTIL"; then { $as_echo "$as_me:${as_lineno-$LINENO}: result: $ac_ct_DSYMUTIL" >&5 $as_echo "$ac_ct_DSYMUTIL" >&6; } else { $as_echo "$as_me:${as_lineno-$LINENO}: result: no" >&5 $as_echo "no" >&6; } fi if test "x$ac_ct_DSYMUTIL" = x; then DSYMUTIL=":" else case $cross_compiling:$ac_tool_warned in yes:) { $as_echo "$as_me:${as_lineno-$LINENO}: WARNING: using cross tools not prefixed with host triplet" >&5 $as_echo "$as_me: WARNING: using cross tools not prefixed with host triplet" >&2;} ac_tool_warned=yes ;; esac DSYMUTIL=$ac_ct_DSYMUTIL fi else DSYMUTIL="$ac_cv_prog_DSYMUTIL" fi if test -n "$ac_tool_prefix"; then # Extract the first word of "${ac_tool_prefix}nmedit", so it can be a program name with args. set dummy ${ac_tool_prefix}nmedit; ac_word=$2 { $as_echo "$as_me:${as_lineno-$LINENO}: checking for $ac_word" >&5 $as_echo_n "checking for $ac_word... " >&6; } if ${ac_cv_prog_NMEDIT+:} false; then : $as_echo_n "(cached) " >&6 else if test -n "$NMEDIT"; then ac_cv_prog_NMEDIT="$NMEDIT" # Let the user override the test. else as_save_IFS=$IFS; IFS=$PATH_SEPARATOR for as_dir in $PATH do IFS=$as_save_IFS test -z "$as_dir" && as_dir=. for ac_exec_ext in '' $ac_executable_extensions; do if as_fn_executable_p "$as_dir/$ac_word$ac_exec_ext"; then ac_cv_prog_NMEDIT="${ac_tool_prefix}nmedit" $as_echo "$as_me:${as_lineno-$LINENO}: found $as_dir/$ac_word$ac_exec_ext" >&5 break 2 fi done done IFS=$as_save_IFS fi fi NMEDIT=$ac_cv_prog_NMEDIT if test -n "$NMEDIT"; then { $as_echo "$as_me:${as_lineno-$LINENO}: result: $NMEDIT" >&5 $as_echo "$NMEDIT" >&6; } else { $as_echo "$as_me:${as_lineno-$LINENO}: result: no" >&5 $as_echo "no" >&6; } fi fi if test -z "$ac_cv_prog_NMEDIT"; then ac_ct_NMEDIT=$NMEDIT # Extract the first word of "nmedit", so it can be a program name with args. set dummy nmedit; ac_word=$2 { $as_echo "$as_me:${as_lineno-$LINENO}: checking for $ac_word" >&5 $as_echo_n "checking for $ac_word... " >&6; } if ${ac_cv_prog_ac_ct_NMEDIT+:} false; then : $as_echo_n "(cached) " >&6 else if test -n "$ac_ct_NMEDIT"; then ac_cv_prog_ac_ct_NMEDIT="$ac_ct_NMEDIT" # Let the user override the test. else as_save_IFS=$IFS; IFS=$PATH_SEPARATOR for as_dir in $PATH do IFS=$as_save_IFS test -z "$as_dir" && as_dir=. for ac_exec_ext in '' $ac_executable_extensions; do if as_fn_executable_p "$as_dir/$ac_word$ac_exec_ext"; then ac_cv_prog_ac_ct_NMEDIT="nmedit" $as_echo "$as_me:${as_lineno-$LINENO}: found $as_dir/$ac_word$ac_exec_ext" >&5 break 2 fi done done IFS=$as_save_IFS fi fi ac_ct_NMEDIT=$ac_cv_prog_ac_ct_NMEDIT if test -n "$ac_ct_NMEDIT"; then { $as_echo "$as_me:${as_lineno-$LINENO}: result: $ac_ct_NMEDIT" >&5 $as_echo "$ac_ct_NMEDIT" >&6; } else { $as_echo "$as_me:${as_lineno-$LINENO}: result: no" >&5 $as_echo "no" >&6; } fi if test "x$ac_ct_NMEDIT" = x; then NMEDIT=":" else case $cross_compiling:$ac_tool_warned in yes:) { $as_echo "$as_me:${as_lineno-$LINENO}: WARNING: using cross tools not prefixed with host triplet" >&5 $as_echo "$as_me: WARNING: using cross tools not prefixed with host triplet" >&2;} ac_tool_warned=yes ;; esac NMEDIT=$ac_ct_NMEDIT fi else NMEDIT="$ac_cv_prog_NMEDIT" fi if test -n "$ac_tool_prefix"; then # Extract the first word of "${ac_tool_prefix}lipo", so it can be a program name with args. set dummy ${ac_tool_prefix}lipo; ac_word=$2 { $as_echo "$as_me:${as_lineno-$LINENO}: checking for $ac_word" >&5 $as_echo_n "checking for $ac_word... " >&6; } if ${ac_cv_prog_LIPO+:} false; then : $as_echo_n "(cached) " >&6 else if test -n "$LIPO"; then ac_cv_prog_LIPO="$LIPO" # Let the user override the test. else as_save_IFS=$IFS; IFS=$PATH_SEPARATOR for as_dir in $PATH do IFS=$as_save_IFS test -z "$as_dir" && as_dir=. for ac_exec_ext in '' $ac_executable_extensions; do if as_fn_executable_p "$as_dir/$ac_word$ac_exec_ext"; then ac_cv_prog_LIPO="${ac_tool_prefix}lipo" $as_echo "$as_me:${as_lineno-$LINENO}: found $as_dir/$ac_word$ac_exec_ext" >&5 break 2 fi done done IFS=$as_save_IFS fi fi LIPO=$ac_cv_prog_LIPO if test -n "$LIPO"; then { $as_echo "$as_me:${as_lineno-$LINENO}: result: $LIPO" >&5 $as_echo "$LIPO" >&6; } else { $as_echo "$as_me:${as_lineno-$LINENO}: result: no" >&5 $as_echo "no" >&6; } fi fi if test -z "$ac_cv_prog_LIPO"; then ac_ct_LIPO=$LIPO # Extract the first word of "lipo", so it can be a program name with args. set dummy lipo; ac_word=$2 { $as_echo "$as_me:${as_lineno-$LINENO}: checking for $ac_word" >&5 $as_echo_n "checking for $ac_word... " >&6; } if ${ac_cv_prog_ac_ct_LIPO+:} false; then : $as_echo_n "(cached) " >&6 else if test -n "$ac_ct_LIPO"; then ac_cv_prog_ac_ct_LIPO="$ac_ct_LIPO" # Let the user override the test. else as_save_IFS=$IFS; IFS=$PATH_SEPARATOR for as_dir in $PATH do IFS=$as_save_IFS test -z "$as_dir" && as_dir=. for ac_exec_ext in '' $ac_executable_extensions; do if as_fn_executable_p "$as_dir/$ac_word$ac_exec_ext"; then ac_cv_prog_ac_ct_LIPO="lipo" $as_echo "$as_me:${as_lineno-$LINENO}: found $as_dir/$ac_word$ac_exec_ext" >&5 break 2 fi done done IFS=$as_save_IFS fi fi ac_ct_LIPO=$ac_cv_prog_ac_ct_LIPO if test -n "$ac_ct_LIPO"; then { $as_echo "$as_me:${as_lineno-$LINENO}: result: $ac_ct_LIPO" >&5 $as_echo "$ac_ct_LIPO" >&6; } else { $as_echo "$as_me:${as_lineno-$LINENO}: result: no" >&5 $as_echo "no" >&6; } fi if test "x$ac_ct_LIPO" = x; then LIPO=":" else case $cross_compiling:$ac_tool_warned in yes:) { $as_echo "$as_me:${as_lineno-$LINENO}: WARNING: using cross tools not prefixed with host triplet" >&5 $as_echo "$as_me: WARNING: using cross tools not prefixed with host triplet" >&2;} ac_tool_warned=yes ;; esac LIPO=$ac_ct_LIPO fi else LIPO="$ac_cv_prog_LIPO" fi if test -n "$ac_tool_prefix"; then # Extract the first word of "${ac_tool_prefix}otool", so it can be a program name with args. set dummy ${ac_tool_prefix}otool; ac_word=$2 { $as_echo "$as_me:${as_lineno-$LINENO}: checking for $ac_word" >&5 $as_echo_n "checking for $ac_word... " >&6; } if ${ac_cv_prog_OTOOL+:} false; then : $as_echo_n "(cached) " >&6 else if test -n "$OTOOL"; then ac_cv_prog_OTOOL="$OTOOL" # Let the user override the test. else as_save_IFS=$IFS; IFS=$PATH_SEPARATOR for as_dir in $PATH do IFS=$as_save_IFS test -z "$as_dir" && as_dir=. for ac_exec_ext in '' $ac_executable_extensions; do if as_fn_executable_p "$as_dir/$ac_word$ac_exec_ext"; then ac_cv_prog_OTOOL="${ac_tool_prefix}otool" $as_echo "$as_me:${as_lineno-$LINENO}: found $as_dir/$ac_word$ac_exec_ext" >&5 break 2 fi done done IFS=$as_save_IFS fi fi OTOOL=$ac_cv_prog_OTOOL if test -n "$OTOOL"; then { $as_echo "$as_me:${as_lineno-$LINENO}: result: $OTOOL" >&5 $as_echo "$OTOOL" >&6; } else { $as_echo "$as_me:${as_lineno-$LINENO}: result: no" >&5 $as_echo "no" >&6; } fi fi if test -z "$ac_cv_prog_OTOOL"; then ac_ct_OTOOL=$OTOOL # Extract the first word of "otool", so it can be a program name with args. set dummy otool; ac_word=$2 { $as_echo "$as_me:${as_lineno-$LINENO}: checking for $ac_word" >&5 $as_echo_n "checking for $ac_word... " >&6; } if ${ac_cv_prog_ac_ct_OTOOL+:} false; then : $as_echo_n "(cached) " >&6 else if test -n "$ac_ct_OTOOL"; then ac_cv_prog_ac_ct_OTOOL="$ac_ct_OTOOL" # Let the user override the test. else as_save_IFS=$IFS; IFS=$PATH_SEPARATOR for as_dir in $PATH do IFS=$as_save_IFS test -z "$as_dir" && as_dir=. for ac_exec_ext in '' $ac_executable_extensions; do if as_fn_executable_p "$as_dir/$ac_word$ac_exec_ext"; then ac_cv_prog_ac_ct_OTOOL="otool" $as_echo "$as_me:${as_lineno-$LINENO}: found $as_dir/$ac_word$ac_exec_ext" >&5 break 2 fi done done IFS=$as_save_IFS fi fi ac_ct_OTOOL=$ac_cv_prog_ac_ct_OTOOL if test -n "$ac_ct_OTOOL"; then { $as_echo "$as_me:${as_lineno-$LINENO}: result: $ac_ct_OTOOL" >&5 $as_echo "$ac_ct_OTOOL" >&6; } else { $as_echo "$as_me:${as_lineno-$LINENO}: result: no" >&5 $as_echo "no" >&6; } fi if test "x$ac_ct_OTOOL" = x; then OTOOL=":" else case $cross_compiling:$ac_tool_warned in yes:) { $as_echo "$as_me:${as_lineno-$LINENO}: WARNING: using cross tools not prefixed with host triplet" >&5 $as_echo "$as_me: WARNING: using cross tools not prefixed with host triplet" >&2;} ac_tool_warned=yes ;; esac OTOOL=$ac_ct_OTOOL fi else OTOOL="$ac_cv_prog_OTOOL" fi if test -n "$ac_tool_prefix"; then # Extract the first word of "${ac_tool_prefix}otool64", so it can be a program name with args. set dummy ${ac_tool_prefix}otool64; ac_word=$2 { $as_echo "$as_me:${as_lineno-$LINENO}: checking for $ac_word" >&5 $as_echo_n "checking for $ac_word... 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" >&6; } if ${lt_cv_apple_cc_single_mod+:} false; then : $as_echo_n "(cached) " >&6 else lt_cv_apple_cc_single_mod=no if test -z "${LT_MULTI_MODULE}"; then # By default we will add the -single_module flag. You can override # by either setting the environment variable LT_MULTI_MODULE # non-empty at configure time, or by adding -multi_module to the # link flags. rm -rf libconftest.dylib* echo "int foo(void){return 1;}" > conftest.c echo "$LTCC $LTCFLAGS $LDFLAGS -o libconftest.dylib \ -dynamiclib -Wl,-single_module conftest.c" >&5 $LTCC $LTCFLAGS $LDFLAGS -o libconftest.dylib \ -dynamiclib -Wl,-single_module conftest.c 2>conftest.err _lt_result=$? # If there is a non-empty error log, and "single_module" # appears in it, assume the flag caused a linker warning if test -s conftest.err && $GREP single_module conftest.err; then cat conftest.err >&5 # Otherwise, if the output was created with a 0 exit code from # the compiler, it worked. elif test -f libconftest.dylib && test $_lt_result -eq 0; then lt_cv_apple_cc_single_mod=yes else cat conftest.err >&5 fi rm -rf libconftest.dylib* rm -f conftest.* fi fi { $as_echo "$as_me:${as_lineno-$LINENO}: result: $lt_cv_apple_cc_single_mod" >&5 $as_echo "$lt_cv_apple_cc_single_mod" >&6; } { $as_echo "$as_me:${as_lineno-$LINENO}: checking for -exported_symbols_list linker flag" >&5 $as_echo_n "checking for -exported_symbols_list linker flag... " >&6; } if ${lt_cv_ld_exported_symbols_list+:} false; then : $as_echo_n "(cached) " >&6 else lt_cv_ld_exported_symbols_list=no save_LDFLAGS=$LDFLAGS echo "_main" > conftest.sym LDFLAGS="$LDFLAGS -Wl,-exported_symbols_list,conftest.sym" cat confdefs.h - <<_ACEOF >conftest.$ac_ext /* end confdefs.h. */ int main () { ; return 0; } _ACEOF if ac_fn_c_try_link "$LINENO"; then : lt_cv_ld_exported_symbols_list=yes else lt_cv_ld_exported_symbols_list=no fi rm -f core conftest.err conftest.$ac_objext \ conftest$ac_exeext conftest.$ac_ext LDFLAGS="$save_LDFLAGS" fi { $as_echo "$as_me:${as_lineno-$LINENO}: result: $lt_cv_ld_exported_symbols_list" >&5 $as_echo "$lt_cv_ld_exported_symbols_list" >&6; } { $as_echo "$as_me:${as_lineno-$LINENO}: checking for -force_load linker flag" >&5 $as_echo_n "checking for -force_load linker flag... " >&6; } if ${lt_cv_ld_force_load+:} false; then : $as_echo_n "(cached) " >&6 else lt_cv_ld_force_load=no cat > conftest.c << _LT_EOF int forced_loaded() { return 2;} _LT_EOF echo "$LTCC $LTCFLAGS -c -o conftest.o conftest.c" >&5 $LTCC $LTCFLAGS -c -o conftest.o conftest.c 2>&5 echo "$AR cru libconftest.a conftest.o" >&5 $AR cru libconftest.a conftest.o 2>&5 echo "$RANLIB libconftest.a" >&5 $RANLIB libconftest.a 2>&5 cat > conftest.c << _LT_EOF int main() { return 0;} _LT_EOF echo "$LTCC $LTCFLAGS $LDFLAGS -o conftest conftest.c -Wl,-force_load,./libconftest.a" >&5 $LTCC $LTCFLAGS $LDFLAGS -o conftest conftest.c -Wl,-force_load,./libconftest.a 2>conftest.err _lt_result=$? if test -s conftest.err && $GREP force_load conftest.err; then cat conftest.err >&5 elif test -f conftest && test $_lt_result -eq 0 && $GREP forced_load conftest >/dev/null 2>&1 ; then lt_cv_ld_force_load=yes else cat conftest.err >&5 fi rm -f conftest.err libconftest.a conftest conftest.c rm -rf conftest.dSYM fi { $as_echo "$as_me:${as_lineno-$LINENO}: result: $lt_cv_ld_force_load" >&5 $as_echo "$lt_cv_ld_force_load" >&6; } case $host_os in rhapsody* | darwin1.[012]) _lt_dar_allow_undefined='${wl}-undefined ${wl}suppress' ;; darwin1.*) _lt_dar_allow_undefined='${wl}-flat_namespace ${wl}-undefined ${wl}suppress' ;; darwin*) # darwin 5.x on # if running on 10.5 or later, the deployment target defaults # to the OS version, if on x86, and 10.4, the deployment # target defaults to 10.4. 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Now check whether nonexistent headers # can be detected and how. cat confdefs.h - <<_ACEOF >conftest.$ac_ext /* end confdefs.h. */ #include _ACEOF if ac_fn_c_try_cpp "$LINENO"; then : # Broken: success on invalid input. continue else # Passes both tests. ac_preproc_ok=: break fi rm -f conftest.err conftest.i conftest.$ac_ext done # Because of `break', _AC_PREPROC_IFELSE's cleaning code was skipped. rm -f conftest.i conftest.err conftest.$ac_ext if $ac_preproc_ok; then : break fi done ac_cv_prog_CPP=$CPP fi CPP=$ac_cv_prog_CPP else ac_cv_prog_CPP=$CPP fi { $as_echo "$as_me:${as_lineno-$LINENO}: result: $CPP" >&5 $as_echo "$CPP" >&6; } ac_preproc_ok=false for ac_c_preproc_warn_flag in '' yes do # Use a header file that comes with gcc, so configuring glibc # with a fresh cross-compiler works. # Prefer to if __STDC__ is defined, since # exists even on freestanding compilers. # On the NeXT, cc -E runs the code through the compiler's parser, # not just through cpp. "Syntax error" is here to catch this case. cat confdefs.h - <<_ACEOF >conftest.$ac_ext /* end confdefs.h. */ #ifdef __STDC__ # include #else # include #endif Syntax error _ACEOF if ac_fn_c_try_cpp "$LINENO"; then : else # Broken: fails on valid input. continue fi rm -f conftest.err conftest.i conftest.$ac_ext # OK, works on sane cases. 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*) archive_cmds='$CC -shared $pic_flag -o $lib $libobjs $deplibs $compiler_flags' hardcode_libdir_flag_spec='${wl}-rpath,$libdir' ;; esac fi else ld_shlibs=no fi ;; os2*) hardcode_libdir_flag_spec='-L$libdir' hardcode_minus_L=yes allow_undefined_flag=unsupported archive_cmds='$ECHO "LIBRARY $libname INITINSTANCE" > $output_objdir/$libname.def~$ECHO "DESCRIPTION \"$libname\"" >> $output_objdir/$libname.def~echo DATA >> $output_objdir/$libname.def~echo " SINGLE NONSHARED" >> $output_objdir/$libname.def~echo EXPORTS >> $output_objdir/$libname.def~emxexp $libobjs >> $output_objdir/$libname.def~$CC -Zdll -Zcrtdll -o $lib $libobjs $deplibs $compiler_flags $output_objdir/$libname.def' old_archive_from_new_cmds='emximp -o $output_objdir/$libname.a $output_objdir/$libname.def' ;; osf3*) if test "$GCC" = yes; then allow_undefined_flag=' ${wl}-expect_unresolved ${wl}\*' archive_cmds='$CC -shared${allow_undefined_flag} $libobjs $deplibs $compiler_flags ${wl}-soname ${wl}$soname `test -n "$verstring" && func_echo_all "${wl}-set_version ${wl}$verstring"` ${wl}-update_registry ${wl}${output_objdir}/so_locations -o $lib' else allow_undefined_flag=' -expect_unresolved \*' archive_cmds='$CC -shared${allow_undefined_flag} $libobjs $deplibs $compiler_flags -soname $soname `test -n "$verstring" && func_echo_all "-set_version $verstring"` -update_registry ${output_objdir}/so_locations -o $lib' fi archive_cmds_need_lc='no' hardcode_libdir_flag_spec='${wl}-rpath ${wl}$libdir' hardcode_libdir_separator=: ;; 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solaris*) no_undefined_flag=' -z defs' if test "$GCC" = yes; then wlarc='${wl}' archive_cmds='$CC -shared $pic_flag ${wl}-z ${wl}text ${wl}-h ${wl}$soname -o $lib $libobjs $deplibs $compiler_flags' archive_expsym_cmds='echo "{ global:" > $lib.exp~cat $export_symbols | $SED -e "s/\(.*\)/\1;/" >> $lib.exp~echo "local: *; };" >> $lib.exp~ $CC -shared $pic_flag ${wl}-z ${wl}text ${wl}-M ${wl}$lib.exp ${wl}-h ${wl}$soname -o $lib $libobjs $deplibs $compiler_flags~$RM $lib.exp' else case `$CC -V 2>&1` in *"Compilers 5.0"*) wlarc='' archive_cmds='$LD -G${allow_undefined_flag} -h $soname -o $lib $libobjs $deplibs $linker_flags' archive_expsym_cmds='echo "{ global:" > $lib.exp~cat $export_symbols | $SED -e "s/\(.*\)/\1;/" >> $lib.exp~echo "local: *; };" >> $lib.exp~ $LD -G${allow_undefined_flag} -M $lib.exp -h $soname -o $lib $libobjs $deplibs $linker_flags~$RM $lib.exp' ;; *) wlarc='${wl}' archive_cmds='$CC -G${allow_undefined_flag} -h $soname -o $lib $libobjs $deplibs $compiler_flags' archive_expsym_cmds='echo "{ global:" > $lib.exp~cat $export_symbols | $SED -e "s/\(.*\)/\1;/" >> $lib.exp~echo "local: *; };" >> $lib.exp~ $CC -G${allow_undefined_flag} -M $lib.exp -h $soname -o $lib $libobjs $deplibs $compiler_flags~$RM $lib.exp' ;; esac fi hardcode_libdir_flag_spec='-R$libdir' hardcode_shlibpath_var=no case $host_os in solaris2.[0-5] | solaris2.[0-5].*) ;; *) # The compiler driver will combine and reorder linker options, # but understands `-z linker_flag'. GCC discards it without `$wl', # but is careful enough not to reorder. # Supported since Solaris 2.6 (maybe 2.5.1?) if test "$GCC" = yes; then whole_archive_flag_spec='${wl}-z ${wl}allextract$convenience ${wl}-z ${wl}defaultextract' else whole_archive_flag_spec='-z allextract$convenience -z defaultextract' fi ;; esac link_all_deplibs=yes ;; sunos4*) if test "x$host_vendor" = xsequent; then # Use $CC to link under sequent, because it throws in some extra .o # files that make .init and .fini sections work. archive_cmds='$CC -G ${wl}-h $soname -o $lib $libobjs $deplibs $compiler_flags' else archive_cmds='$LD -assert pure-text -Bstatic -o $lib $libobjs $deplibs $linker_flags' fi hardcode_libdir_flag_spec='-L$libdir' hardcode_direct=yes hardcode_minus_L=yes hardcode_shlibpath_var=no ;; sysv4) case $host_vendor in sni) archive_cmds='$LD -G -h $soname -o $lib $libobjs $deplibs $linker_flags' hardcode_direct=yes # is this really true??? ;; siemens) ## LD is ld it makes a PLAMLIB ## CC just makes a GrossModule. archive_cmds='$LD -G -o $lib $libobjs $deplibs $linker_flags' reload_cmds='$CC -r -o $output$reload_objs' hardcode_direct=no ;; motorola) archive_cmds='$LD -G -h $soname -o $lib $libobjs $deplibs $linker_flags' hardcode_direct=no #Motorola manual says yes, but my tests say they lie ;; esac runpath_var='LD_RUN_PATH' hardcode_shlibpath_var=no ;; sysv4.3*) archive_cmds='$LD -G -h $soname -o $lib $libobjs $deplibs $linker_flags' hardcode_shlibpath_var=no export_dynamic_flag_spec='-Bexport' ;; sysv4*MP*) if test -d /usr/nec; then archive_cmds='$LD -G -h $soname -o $lib $libobjs $deplibs $linker_flags' hardcode_shlibpath_var=no runpath_var=LD_RUN_PATH hardcode_runpath_var=yes ld_shlibs=yes fi ;; sysv4*uw2* | sysv5OpenUNIX* | sysv5UnixWare7.[01].[10]* | unixware7* | sco3.2v5.0.[024]*) no_undefined_flag='${wl}-z,text' archive_cmds_need_lc=no hardcode_shlibpath_var=no runpath_var='LD_RUN_PATH' if test "$GCC" = yes; then archive_cmds='$CC -shared ${wl}-h,$soname -o $lib $libobjs $deplibs $compiler_flags' archive_expsym_cmds='$CC -shared ${wl}-Bexport:$export_symbols ${wl}-h,$soname -o $lib $libobjs $deplibs $compiler_flags' else archive_cmds='$CC -G ${wl}-h,$soname -o $lib $libobjs $deplibs $compiler_flags' archive_expsym_cmds='$CC -G ${wl}-Bexport:$export_symbols ${wl}-h,$soname -o $lib $libobjs $deplibs $compiler_flags' fi ;; sysv5* | sco3.2v5* | sco5v6*) # Note: We can NOT use -z defs as we might desire, because we do not # link with -lc, and that would cause any symbols used from libc to # always be unresolved, which means just about no library would # ever link correctly. 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The import file would start with # the line `#! .'. This would cause the generated library to # depend on `.', always an invalid library. This was fixed in # development snapshots of GCC prior to 3.0. case $host_os in aix4 | aix4.[01] | aix4.[01].*) if { echo '#if __GNUC__ > 2 || (__GNUC__ == 2 && __GNUC_MINOR__ >= 97)' echo ' yes ' echo '#endif'; } | ${CC} -E - | $GREP yes > /dev/null; then : else can_build_shared=no fi ;; esac # AIX (on Power*) has no versioning support, so currently we can not hardcode correct # soname into executable. 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do libname=`func_echo_all "$lib" | $SED '\''s%^.*/\([^/]*\)\.ixlibrary$%\1%'\''`; test $RM /sys/libs/${libname}_ixlibrary.a; $show "cd /sys/libs && $LN_S $lib ${libname}_ixlibrary.a"; cd /sys/libs && $LN_S $lib ${libname}_ixlibrary.a || exit 1; done' ;; esac ;; beos*) library_names_spec='${libname}${shared_ext}' dynamic_linker="$host_os ld.so" shlibpath_var=LIBRARY_PATH ;; bsdi[45]*) version_type=linux # correct to gnu/linux during the next big refactor need_version=no library_names_spec='${libname}${release}${shared_ext}$versuffix ${libname}${release}${shared_ext}$major $libname${shared_ext}' soname_spec='${libname}${release}${shared_ext}$major' finish_cmds='PATH="\$PATH:/sbin" ldconfig $libdir' shlibpath_var=LD_LIBRARY_PATH sys_lib_search_path_spec="/shlib /usr/lib /usr/X11/lib /usr/contrib/lib /lib /usr/local/lib" sys_lib_dlsearch_path_spec="/shlib /usr/lib /usr/local/lib" # the default ld.so.conf also contains /usr/contrib/lib and # /usr/X11R6/lib (/usr/X11 is a link to /usr/X11R6), but let us allow # libtool to hard-code these into programs ;; 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then sys_lib_search_path_spec="/usr/lib/hpux32 /usr/local/lib/hpux32 /usr/local/lib" else sys_lib_search_path_spec="/usr/lib/hpux64 /usr/local/lib/hpux64" fi sys_lib_dlsearch_path_spec=$sys_lib_search_path_spec ;; hppa*64*) shrext_cmds='.sl' hardcode_into_libs=yes dynamic_linker="$host_os dld.sl" shlibpath_var=LD_LIBRARY_PATH # How should we handle SHLIB_PATH shlibpath_overrides_runpath=yes # Unless +noenvvar is specified. library_names_spec='${libname}${release}${shared_ext}$versuffix ${libname}${release}${shared_ext}$major $libname${shared_ext}' soname_spec='${libname}${release}${shared_ext}$major' sys_lib_search_path_spec="/usr/lib/pa20_64 /usr/ccs/lib/pa20_64" sys_lib_dlsearch_path_spec=$sys_lib_search_path_spec ;; *) shrext_cmds='.sl' dynamic_linker="$host_os dld.sl" shlibpath_var=SHLIB_PATH shlibpath_overrides_runpath=no # +s is required to enable SHLIB_PATH library_names_spec='${libname}${release}${shared_ext}$versuffix ${libname}${release}${shared_ext}$major $libname${shared_ext}' soname_spec='${libname}${release}${shared_ext}$major' ;; esac # HP-UX runs *really* slowly unless shared libraries are mode 555, ... postinstall_cmds='chmod 555 $lib' # or fails outright, so override atomically: install_override_mode=555 ;; interix[3-9]*) version_type=linux # correct to gnu/linux during the next big refactor need_lib_prefix=no need_version=no library_names_spec='${libname}${release}${shared_ext}$versuffix ${libname}${release}${shared_ext}$major ${libname}${shared_ext}' soname_spec='${libname}${release}${shared_ext}$major' dynamic_linker='Interix 3.x ld.so.1 (PE, like ELF)' shlibpath_var=LD_LIBRARY_PATH shlibpath_overrides_runpath=no hardcode_into_libs=yes ;; irix5* | irix6* | nonstopux*) case $host_os in nonstopux*) version_type=nonstopux ;; *) if test "$lt_cv_prog_gnu_ld" = yes; then version_type=linux # correct to gnu/linux during the next big refactor else version_type=irix fi ;; esac need_lib_prefix=no need_version=no soname_spec='${libname}${release}${shared_ext}$major' library_names_spec='${libname}${release}${shared_ext}$versuffix ${libname}${release}${shared_ext}$major ${libname}${release}${shared_ext} $libname${shared_ext}' case $host_os in irix5* | nonstopux*) libsuff= shlibsuff= ;; *) case $LD in # libtool.m4 will add one of these switches to LD *-32|*"-32 "|*-melf32bsmip|*"-melf32bsmip ") libsuff= shlibsuff= libmagic=32-bit;; *-n32|*"-n32 "|*-melf32bmipn32|*"-melf32bmipn32 ") libsuff=32 shlibsuff=N32 libmagic=N32;; *-64|*"-64 "|*-melf64bmip|*"-melf64bmip ") libsuff=64 shlibsuff=64 libmagic=64-bit;; *) libsuff= shlibsuff= libmagic=never-match;; esac ;; esac shlibpath_var=LD_LIBRARY${shlibsuff}_PATH shlibpath_overrides_runpath=no sys_lib_search_path_spec="/usr/lib${libsuff} /lib${libsuff} /usr/local/lib${libsuff}" sys_lib_dlsearch_path_spec="/usr/lib${libsuff} /lib${libsuff}" hardcode_into_libs=yes ;; # No shared lib support for Linux oldld, aout, or coff. linux*oldld* | linux*aout* | linux*coff*) dynamic_linker=no ;; # This must be glibc/ELF. linux* | k*bsd*-gnu | kopensolaris*-gnu) version_type=linux # correct to gnu/linux during the next big refactor need_lib_prefix=no need_version=no library_names_spec='${libname}${release}${shared_ext}$versuffix ${libname}${release}${shared_ext}$major $libname${shared_ext}' soname_spec='${libname}${release}${shared_ext}$major' finish_cmds='PATH="\$PATH:/sbin" ldconfig -n $libdir' shlibpath_var=LD_LIBRARY_PATH shlibpath_overrides_runpath=no # Some binutils ld are patched to set DT_RUNPATH if ${lt_cv_shlibpath_overrides_runpath+:} false; then : $as_echo_n "(cached) " >&6 else lt_cv_shlibpath_overrides_runpath=no save_LDFLAGS=$LDFLAGS save_libdir=$libdir eval "libdir=/foo; wl=\"$lt_prog_compiler_wl\"; \ LDFLAGS=\"\$LDFLAGS $hardcode_libdir_flag_spec\"" cat confdefs.h - <<_ACEOF >conftest.$ac_ext /* end confdefs.h. */ int main () { ; return 0; } _ACEOF if ac_fn_c_try_link "$LINENO"; then : if ($OBJDUMP -p conftest$ac_exeext) 2>/dev/null | grep "RUNPATH.*$libdir" >/dev/null; then : lt_cv_shlibpath_overrides_runpath=yes fi fi rm -f core conftest.err conftest.$ac_objext \ conftest$ac_exeext conftest.$ac_ext LDFLAGS=$save_LDFLAGS libdir=$save_libdir fi shlibpath_overrides_runpath=$lt_cv_shlibpath_overrides_runpath # This implies no fast_install, which is unacceptable. # Some rework will be needed to allow for fast_install # before this can be enabled. hardcode_into_libs=yes # Append ld.so.conf contents to the search path if test -f /etc/ld.so.conf; then lt_ld_extra=`awk '/^include / { system(sprintf("cd /etc; cat %s 2>/dev/null", \$2)); 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esac else shlibpath_overrides_runpath=yes fi ;; os2*) libname_spec='$name' shrext_cmds=".dll" need_lib_prefix=no library_names_spec='$libname${shared_ext} $libname.a' dynamic_linker='OS/2 ld.exe' shlibpath_var=LIBPATH ;; osf3* | osf4* | osf5*) version_type=osf need_lib_prefix=no need_version=no soname_spec='${libname}${release}${shared_ext}$major' library_names_spec='${libname}${release}${shared_ext}$versuffix ${libname}${release}${shared_ext}$major $libname${shared_ext}' shlibpath_var=LD_LIBRARY_PATH sys_lib_search_path_spec="/usr/shlib /usr/ccs/lib /usr/lib/cmplrs/cc /usr/lib /usr/local/lib /var/shlib" sys_lib_dlsearch_path_spec="$sys_lib_search_path_spec" ;; rdos*) dynamic_linker=no ;; solaris*) version_type=linux # correct to gnu/linux during the next big refactor need_lib_prefix=no need_version=no library_names_spec='${libname}${release}${shared_ext}$versuffix ${libname}${release}${shared_ext}$major $libname${shared_ext}' soname_spec='${libname}${release}${shared_ext}$major' shlibpath_var=LD_LIBRARY_PATH shlibpath_overrides_runpath=yes hardcode_into_libs=yes # ldd complains unless libraries are executable postinstall_cmds='chmod +x $lib' ;; 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sysv5* | sco3.2v5* | sco5v6* | unixware* | OpenUNIX* | sysv4*uw2*) version_type=freebsd-elf need_lib_prefix=no need_version=no library_names_spec='${libname}${release}${shared_ext}$versuffix ${libname}${release}${shared_ext} $libname${shared_ext}' soname_spec='${libname}${release}${shared_ext}$major' shlibpath_var=LD_LIBRARY_PATH shlibpath_overrides_runpath=yes hardcode_into_libs=yes if test "$with_gnu_ld" = yes; then sys_lib_search_path_spec='/usr/local/lib /usr/gnu/lib /usr/ccs/lib /usr/lib /lib' else sys_lib_search_path_spec='/usr/ccs/lib /usr/lib' case $host_os in sco3.2v5*) sys_lib_search_path_spec="$sys_lib_search_path_spec /lib" ;; esac fi sys_lib_dlsearch_path_spec='/usr/lib' ;; tpf*) # TPF is a cross-target only. Preferred cross-host = GNU/Linux. version_type=linux # correct to gnu/linux during the next big refactor need_lib_prefix=no need_version=no library_names_spec='${libname}${release}${shared_ext}$versuffix ${libname}${release}${shared_ext}$major $libname${shared_ext}' shlibpath_var=LD_LIBRARY_PATH shlibpath_overrides_runpath=no hardcode_into_libs=yes ;; uts4*) version_type=linux # correct to gnu/linux during the next big refactor library_names_spec='${libname}${release}${shared_ext}$versuffix ${libname}${release}${shared_ext}$major $libname${shared_ext}' soname_spec='${libname}${release}${shared_ext}$major' shlibpath_var=LD_LIBRARY_PATH ;; *) dynamic_linker=no ;; esac { $as_echo "$as_me:${as_lineno-$LINENO}: result: $dynamic_linker" >&5 $as_echo "$dynamic_linker" >&6; } test "$dynamic_linker" = no && can_build_shared=no variables_saved_for_relink="PATH $shlibpath_var $runpath_var" if test "$GCC" = yes; then variables_saved_for_relink="$variables_saved_for_relink GCC_EXEC_PREFIX COMPILER_PATH LIBRARY_PATH" fi if test "${lt_cv_sys_lib_search_path_spec+set}" = set; then sys_lib_search_path_spec="$lt_cv_sys_lib_search_path_spec" fi if test "${lt_cv_sys_lib_dlsearch_path_spec+set}" = set; then sys_lib_dlsearch_path_spec="$lt_cv_sys_lib_dlsearch_path_spec" fi { $as_echo "$as_me:${as_lineno-$LINENO}: checking how to hardcode library paths into programs" >&5 $as_echo_n "checking how to hardcode library paths into programs... " >&6; } hardcode_action= if test -n "$hardcode_libdir_flag_spec" || test -n "$runpath_var" || test "X$hardcode_automatic" = "Xyes" ; then # We can hardcode non-existent directories. if test "$hardcode_direct" != no && # If the only mechanism to avoid hardcoding is shlibpath_var, we # have to relink, otherwise we might link with an installed library # when we should be linking with a yet-to-be-installed one ## test "$_LT_TAGVAR(hardcode_shlibpath_var, )" != no && test "$hardcode_minus_L" != no; then # Linking always hardcodes the temporary library directory. hardcode_action=relink else # We can link without hardcoding, and we can hardcode nonexisting dirs. hardcode_action=immediate fi else # We cannot hardcode anything, or else we can only hardcode existing # directories. hardcode_action=unsupported fi { $as_echo "$as_me:${as_lineno-$LINENO}: result: $hardcode_action" >&5 $as_echo "$hardcode_action" >&6; } if test "$hardcode_action" = relink || test "$inherit_rpath" = yes; then # Fast installation is not supported enable_fast_install=no elif test "$shlibpath_overrides_runpath" = yes || test "$enable_shared" = no; then # Fast installation is not necessary enable_fast_install=needless fi if test "x$enable_dlopen" != xyes; then enable_dlopen=unknown enable_dlopen_self=unknown enable_dlopen_self_static=unknown else lt_cv_dlopen=no lt_cv_dlopen_libs= case $host_os in beos*) lt_cv_dlopen="load_add_on" lt_cv_dlopen_libs= lt_cv_dlopen_self=yes ;; mingw* | pw32* | cegcc*) lt_cv_dlopen="LoadLibrary" lt_cv_dlopen_libs= ;; cygwin*) lt_cv_dlopen="dlopen" lt_cv_dlopen_libs= ;; darwin*) # if libdl is installed we need to link against it { $as_echo "$as_me:${as_lineno-$LINENO}: checking for dlopen in -ldl" >&5 $as_echo_n "checking for dlopen in -ldl... " >&6; } if ${ac_cv_lib_dl_dlopen+:} false; then : $as_echo_n "(cached) " >&6 else ac_check_lib_save_LIBS=$LIBS LIBS="-ldl $LIBS" cat confdefs.h - <<_ACEOF >conftest.$ac_ext /* end confdefs.h. */ /* Override any GCC internal prototype to avoid an error. Use char because int might match the return type of a GCC builtin and then its argument prototype would still apply. */ #ifdef __cplusplus extern "C" #endif char dlopen (); int main () { return dlopen (); ; return 0; } _ACEOF if ac_fn_c_try_link "$LINENO"; then : ac_cv_lib_dl_dlopen=yes else ac_cv_lib_dl_dlopen=no fi rm -f core conftest.err conftest.$ac_objext \ conftest$ac_exeext conftest.$ac_ext LIBS=$ac_check_lib_save_LIBS fi { $as_echo "$as_me:${as_lineno-$LINENO}: result: $ac_cv_lib_dl_dlopen" >&5 $as_echo "$ac_cv_lib_dl_dlopen" >&6; } if test "x$ac_cv_lib_dl_dlopen" = xyes; then : lt_cv_dlopen="dlopen" lt_cv_dlopen_libs="-ldl" else lt_cv_dlopen="dyld" lt_cv_dlopen_libs= lt_cv_dlopen_self=yes fi ;; *) ac_fn_c_check_func "$LINENO" "shl_load" "ac_cv_func_shl_load" if test "x$ac_cv_func_shl_load" = xyes; then : lt_cv_dlopen="shl_load" else { $as_echo "$as_me:${as_lineno-$LINENO}: checking for shl_load in -ldld" >&5 $as_echo_n "checking for shl_load in -ldld... " >&6; } if ${ac_cv_lib_dld_shl_load+:} false; then : $as_echo_n "(cached) " >&6 else ac_check_lib_save_LIBS=$LIBS LIBS="-ldld $LIBS" cat confdefs.h - <<_ACEOF >conftest.$ac_ext /* end confdefs.h. */ /* Override any GCC internal prototype to avoid an error. Use char because int might match the return type of a GCC builtin and then its argument prototype would still apply. */ #ifdef __cplusplus extern "C" #endif char shl_load (); int main () { return shl_load (); ; return 0; } _ACEOF if ac_fn_c_try_link "$LINENO"; then : ac_cv_lib_dld_shl_load=yes else ac_cv_lib_dld_shl_load=no fi rm -f core conftest.err conftest.$ac_objext \ conftest$ac_exeext conftest.$ac_ext LIBS=$ac_check_lib_save_LIBS fi { $as_echo "$as_me:${as_lineno-$LINENO}: result: $ac_cv_lib_dld_shl_load" >&5 $as_echo "$ac_cv_lib_dld_shl_load" >&6; } if test "x$ac_cv_lib_dld_shl_load" = xyes; then : lt_cv_dlopen="shl_load" lt_cv_dlopen_libs="-ldld" else ac_fn_c_check_func "$LINENO" "dlopen" "ac_cv_func_dlopen" if test "x$ac_cv_func_dlopen" = xyes; then : lt_cv_dlopen="dlopen" else { $as_echo "$as_me:${as_lineno-$LINENO}: checking for dlopen in -ldl" >&5 $as_echo_n "checking for dlopen in -ldl... " >&6; } if ${ac_cv_lib_dl_dlopen+:} false; then : $as_echo_n "(cached) " >&6 else ac_check_lib_save_LIBS=$LIBS LIBS="-ldl $LIBS" cat confdefs.h - <<_ACEOF >conftest.$ac_ext /* end confdefs.h. */ /* Override any GCC internal prototype to avoid an error. Use char because int might match the return type of a GCC builtin and then its argument prototype would still apply. */ #ifdef __cplusplus extern "C" #endif char dlopen (); int main () { return dlopen (); ; return 0; } _ACEOF if ac_fn_c_try_link "$LINENO"; then : ac_cv_lib_dl_dlopen=yes else ac_cv_lib_dl_dlopen=no fi rm -f core conftest.err conftest.$ac_objext \ conftest$ac_exeext conftest.$ac_ext LIBS=$ac_check_lib_save_LIBS fi { $as_echo "$as_me:${as_lineno-$LINENO}: result: $ac_cv_lib_dl_dlopen" >&5 $as_echo "$ac_cv_lib_dl_dlopen" >&6; } if test "x$ac_cv_lib_dl_dlopen" = xyes; then : lt_cv_dlopen="dlopen" lt_cv_dlopen_libs="-ldl" else { $as_echo "$as_me:${as_lineno-$LINENO}: checking for dlopen in -lsvld" >&5 $as_echo_n "checking for dlopen in -lsvld... " >&6; } if ${ac_cv_lib_svld_dlopen+:} false; then : $as_echo_n "(cached) " >&6 else ac_check_lib_save_LIBS=$LIBS LIBS="-lsvld $LIBS" cat confdefs.h - <<_ACEOF >conftest.$ac_ext /* end confdefs.h. */ /* Override any GCC internal prototype to avoid an error. Use char because int might match the return type of a GCC builtin and then its argument prototype would still apply. */ #ifdef __cplusplus extern "C" #endif char dlopen (); int main () { return dlopen (); ; return 0; } _ACEOF if ac_fn_c_try_link "$LINENO"; then : ac_cv_lib_svld_dlopen=yes else ac_cv_lib_svld_dlopen=no fi rm -f core conftest.err conftest.$ac_objext \ conftest$ac_exeext conftest.$ac_ext LIBS=$ac_check_lib_save_LIBS fi { $as_echo "$as_me:${as_lineno-$LINENO}: result: $ac_cv_lib_svld_dlopen" >&5 $as_echo "$ac_cv_lib_svld_dlopen" >&6; } if test "x$ac_cv_lib_svld_dlopen" = xyes; then : lt_cv_dlopen="dlopen" lt_cv_dlopen_libs="-lsvld" else { $as_echo "$as_me:${as_lineno-$LINENO}: checking for dld_link in -ldld" >&5 $as_echo_n "checking for dld_link in -ldld... " >&6; } if ${ac_cv_lib_dld_dld_link+:} false; then : $as_echo_n "(cached) " >&6 else ac_check_lib_save_LIBS=$LIBS LIBS="-ldld $LIBS" cat confdefs.h - <<_ACEOF >conftest.$ac_ext /* end confdefs.h. */ /* Override any GCC internal prototype to avoid an error. Use char because int might match the return type of a GCC builtin and then its argument prototype would still apply. */ #ifdef __cplusplus extern "C" #endif char dld_link (); int main () { return dld_link (); ; return 0; } _ACEOF if ac_fn_c_try_link "$LINENO"; then : ac_cv_lib_dld_dld_link=yes else ac_cv_lib_dld_dld_link=no fi rm -f core conftest.err conftest.$ac_objext \ conftest$ac_exeext conftest.$ac_ext LIBS=$ac_check_lib_save_LIBS fi { $as_echo "$as_me:${as_lineno-$LINENO}: result: $ac_cv_lib_dld_dld_link" >&5 $as_echo "$ac_cv_lib_dld_dld_link" >&6; } if test "x$ac_cv_lib_dld_dld_link" = xyes; then : lt_cv_dlopen="dld_link" lt_cv_dlopen_libs="-ldld" fi fi fi fi fi fi ;; esac if test "x$lt_cv_dlopen" != xno; then enable_dlopen=yes else enable_dlopen=no fi case $lt_cv_dlopen in dlopen) save_CPPFLAGS="$CPPFLAGS" test "x$ac_cv_header_dlfcn_h" = xyes && CPPFLAGS="$CPPFLAGS -DHAVE_DLFCN_H" save_LDFLAGS="$LDFLAGS" wl=$lt_prog_compiler_wl eval LDFLAGS=\"\$LDFLAGS $export_dynamic_flag_spec\" save_LIBS="$LIBS" LIBS="$lt_cv_dlopen_libs $LIBS" { $as_echo "$as_me:${as_lineno-$LINENO}: checking whether a program can dlopen itself" >&5 $as_echo_n "checking whether a program can dlopen itself... " >&6; } if ${lt_cv_dlopen_self+:} false; then : $as_echo_n "(cached) " >&6 else if test "$cross_compiling" = yes; then : lt_cv_dlopen_self=cross else lt_dlunknown=0; lt_dlno_uscore=1; lt_dlneed_uscore=2 lt_status=$lt_dlunknown cat > conftest.$ac_ext <<_LT_EOF #line $LINENO "configure" #include "confdefs.h" #if HAVE_DLFCN_H #include #endif #include #ifdef RTLD_GLOBAL # define LT_DLGLOBAL RTLD_GLOBAL #else # ifdef DL_GLOBAL # define LT_DLGLOBAL DL_GLOBAL # else # define LT_DLGLOBAL 0 # endif #endif /* We may have to define LT_DLLAZY_OR_NOW in the command line if we find out it does not work in some platform. */ #ifndef LT_DLLAZY_OR_NOW # ifdef RTLD_LAZY # define LT_DLLAZY_OR_NOW RTLD_LAZY # else # ifdef DL_LAZY # define LT_DLLAZY_OR_NOW DL_LAZY # else # ifdef RTLD_NOW # define LT_DLLAZY_OR_NOW RTLD_NOW # else # ifdef DL_NOW # define LT_DLLAZY_OR_NOW DL_NOW # else # define LT_DLLAZY_OR_NOW 0 # endif # endif # endif # endif #endif /* When -fvisbility=hidden is used, assume the code has been annotated correspondingly for the symbols needed. */ #if defined(__GNUC__) && (((__GNUC__ == 3) && (__GNUC_MINOR__ >= 3)) || (__GNUC__ > 3)) int fnord () __attribute__((visibility("default"))); #endif int fnord () { return 42; } int main () { void *self = dlopen (0, LT_DLGLOBAL|LT_DLLAZY_OR_NOW); int status = $lt_dlunknown; if (self) { if (dlsym (self,"fnord")) status = $lt_dlno_uscore; else { if (dlsym( self,"_fnord")) status = $lt_dlneed_uscore; else puts (dlerror ()); } /* dlclose (self); */ } else puts (dlerror ()); return status; } _LT_EOF if { { eval echo "\"\$as_me\":${as_lineno-$LINENO}: \"$ac_link\""; } >&5 (eval $ac_link) 2>&5 ac_status=$? $as_echo "$as_me:${as_lineno-$LINENO}: \$? = $ac_status" >&5 test $ac_status = 0; } && test -s conftest${ac_exeext} 2>/dev/null; then (./conftest; exit; ) >&5 2>/dev/null lt_status=$? case x$lt_status in x$lt_dlno_uscore) lt_cv_dlopen_self=yes ;; x$lt_dlneed_uscore) lt_cv_dlopen_self=yes ;; x$lt_dlunknown|x*) lt_cv_dlopen_self=no ;; esac else : # compilation failed lt_cv_dlopen_self=no fi fi rm -fr conftest* fi { $as_echo "$as_me:${as_lineno-$LINENO}: result: $lt_cv_dlopen_self" >&5 $as_echo "$lt_cv_dlopen_self" >&6; } if test "x$lt_cv_dlopen_self" = xyes; then wl=$lt_prog_compiler_wl eval LDFLAGS=\"\$LDFLAGS $lt_prog_compiler_static\" { $as_echo "$as_me:${as_lineno-$LINENO}: checking whether a statically linked program can dlopen itself" >&5 $as_echo_n "checking whether a statically linked program can dlopen itself... " >&6; } if ${lt_cv_dlopen_self_static+:} false; then : $as_echo_n "(cached) " >&6 else if test "$cross_compiling" = yes; then : lt_cv_dlopen_self_static=cross else lt_dlunknown=0; lt_dlno_uscore=1; lt_dlneed_uscore=2 lt_status=$lt_dlunknown cat > conftest.$ac_ext <<_LT_EOF #line $LINENO "configure" #include "confdefs.h" #if HAVE_DLFCN_H #include #endif #include #ifdef RTLD_GLOBAL # define LT_DLGLOBAL RTLD_GLOBAL #else # ifdef DL_GLOBAL # define LT_DLGLOBAL DL_GLOBAL # else # define LT_DLGLOBAL 0 # endif #endif /* We may have to define LT_DLLAZY_OR_NOW in the command line if we find out it does not work in some platform. */ #ifndef LT_DLLAZY_OR_NOW # ifdef RTLD_LAZY # define LT_DLLAZY_OR_NOW RTLD_LAZY # else # ifdef DL_LAZY # define LT_DLLAZY_OR_NOW DL_LAZY # else # ifdef RTLD_NOW # define LT_DLLAZY_OR_NOW RTLD_NOW # else # ifdef DL_NOW # define LT_DLLAZY_OR_NOW DL_NOW # else # define LT_DLLAZY_OR_NOW 0 # endif # endif # endif # endif #endif /* When -fvisbility=hidden is used, assume the code has been annotated correspondingly for the symbols needed. */ #if defined(__GNUC__) && (((__GNUC__ == 3) && (__GNUC_MINOR__ >= 3)) || (__GNUC__ > 3)) int fnord () __attribute__((visibility("default"))); #endif int fnord () { return 42; } int main () { void *self = dlopen (0, LT_DLGLOBAL|LT_DLLAZY_OR_NOW); int status = $lt_dlunknown; if (self) { if (dlsym (self,"fnord")) status = $lt_dlno_uscore; else { if (dlsym( self,"_fnord")) status = $lt_dlneed_uscore; else puts (dlerror ()); } /* dlclose (self); */ } else puts (dlerror ()); return status; } _LT_EOF if { { eval echo "\"\$as_me\":${as_lineno-$LINENO}: \"$ac_link\""; } >&5 (eval $ac_link) 2>&5 ac_status=$? $as_echo "$as_me:${as_lineno-$LINENO}: \$? = $ac_status" >&5 test $ac_status = 0; } && test -s conftest${ac_exeext} 2>/dev/null; then (./conftest; exit; ) >&5 2>/dev/null lt_status=$? case x$lt_status in x$lt_dlno_uscore) lt_cv_dlopen_self_static=yes ;; x$lt_dlneed_uscore) lt_cv_dlopen_self_static=yes ;; x$lt_dlunknown|x*) lt_cv_dlopen_self_static=no ;; esac else : # compilation failed lt_cv_dlopen_self_static=no fi fi rm -fr conftest* fi { $as_echo "$as_me:${as_lineno-$LINENO}: result: $lt_cv_dlopen_self_static" >&5 $as_echo "$lt_cv_dlopen_self_static" >&6; } fi CPPFLAGS="$save_CPPFLAGS" LDFLAGS="$save_LDFLAGS" LIBS="$save_LIBS" ;; esac case $lt_cv_dlopen_self in yes|no) enable_dlopen_self=$lt_cv_dlopen_self ;; *) enable_dlopen_self=unknown ;; esac case $lt_cv_dlopen_self_static in yes|no) enable_dlopen_self_static=$lt_cv_dlopen_self_static ;; *) enable_dlopen_self_static=unknown ;; esac fi striplib= old_striplib= { $as_echo "$as_me:${as_lineno-$LINENO}: checking whether stripping libraries is possible" >&5 $as_echo_n "checking whether stripping libraries is possible... " >&6; } if test -n "$STRIP" && $STRIP -V 2>&1 | $GREP "GNU strip" >/dev/null; then test -z "$old_striplib" && old_striplib="$STRIP --strip-debug" test -z "$striplib" && striplib="$STRIP --strip-unneeded" { $as_echo "$as_me:${as_lineno-$LINENO}: result: yes" >&5 $as_echo "yes" >&6; } else # FIXME - insert some real tests, host_os isn't really good enough case $host_os in darwin*) if test -n "$STRIP" ; then striplib="$STRIP -x" old_striplib="$STRIP -S" { $as_echo "$as_me:${as_lineno-$LINENO}: result: yes" >&5 $as_echo "yes" >&6; } else { $as_echo "$as_me:${as_lineno-$LINENO}: result: no" >&5 $as_echo "no" >&6; } fi ;; *) { $as_echo "$as_me:${as_lineno-$LINENO}: result: no" >&5 $as_echo "no" >&6; } ;; esac fi # Report which library types will actually be built { $as_echo "$as_me:${as_lineno-$LINENO}: checking if libtool supports shared libraries" >&5 $as_echo_n "checking if libtool supports shared libraries... " >&6; } { $as_echo "$as_me:${as_lineno-$LINENO}: result: $can_build_shared" >&5 $as_echo "$can_build_shared" >&6; } { $as_echo "$as_me:${as_lineno-$LINENO}: checking whether to build shared libraries" >&5 $as_echo_n "checking whether to build shared libraries... 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" >&6; } if ${ac_cv_search_strlcpy+:} false; then : $as_echo_n "(cached) " >&6 else ac_func_search_save_LIBS=$LIBS cat confdefs.h - <<_ACEOF >conftest.$ac_ext /* end confdefs.h. */ /* Override any GCC internal prototype to avoid an error. Use char because int might match the return type of a GCC builtin and then its argument prototype would still apply. */ #ifdef __cplusplus extern "C" #endif char strlcpy (); int main () { return strlcpy (); ; return 0; } _ACEOF for ac_lib in '' bsd; do if test -z "$ac_lib"; then ac_res="none required" else ac_res=-l$ac_lib LIBS="-l$ac_lib $ac_func_search_save_LIBS" fi if ac_fn_c_try_link "$LINENO"; then : ac_cv_search_strlcpy=$ac_res fi rm -f core conftest.err conftest.$ac_objext \ conftest$ac_exeext if ${ac_cv_search_strlcpy+:} false; then : break fi done if ${ac_cv_search_strlcpy+:} false; then : else ac_cv_search_strlcpy=no fi rm conftest.$ac_ext LIBS=$ac_func_search_save_LIBS fi { $as_echo "$as_me:${as_lineno-$LINENO}: result: $ac_cv_search_strlcpy" >&5 $as_echo "$ac_cv_search_strlcpy" >&6; } ac_res=$ac_cv_search_strlcpy if test "$ac_res" != no; then : test "$ac_res" = "none required" || LIBS="$ac_res $LIBS" fi for ac_func in strlcpy do : ac_fn_c_check_func "$LINENO" "strlcpy" "ac_cv_func_strlcpy" if test "x$ac_cv_func_strlcpy" = xyes; then : cat >>confdefs.h <<_ACEOF #define HAVE_STRLCPY 1 _ACEOF fi done # Need the math library { $as_echo "$as_me:${as_lineno-$LINENO}: checking for sin in -lm" >&5 $as_echo_n "checking for sin in -lm... 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When coming back to configure, we # need to make the FD available again. if test "$no_create" != yes; then ac_cs_success=: ac_config_status_args= test "$silent" = yes && ac_config_status_args="$ac_config_status_args --quiet" exec 5>/dev/null $SHELL $CONFIG_STATUS $ac_config_status_args || ac_cs_success=false exec 5>>config.log # Use ||, not &&, to avoid exiting from the if with $? = 1, which # would make configure fail if this is the last instruction. $ac_cs_success || as_fn_exit 1 fi if test -n "$ac_unrecognized_opts" && test "$enable_option_checking" != no; then { $as_echo "$as_me:${as_lineno-$LINENO}: WARNING: unrecognized options: $ac_unrecognized_opts" >&5 $as_echo "$as_me: WARNING: unrecognized options: $ac_unrecognized_opts" >&2;} fi pal-0.5.0/configure.ac000644 000765 000024 00000006537 12366007525 014705 0ustar00timjstaff000000 000000 dnl Process this file with autoconf to produce a configure script AC_REVISION($Revision: 27534 $) dnl Initialisation: package name and version number AC_INIT([pal],[0.5.0],[starlink@jiscmail.ac.uk]) dnl Require autoconf-2.50 at least AC_PREREQ([2.69]) dnl Require Starlink automake AM_INIT_AUTOMAKE(1.8.2-starlink) dnl Sanity-check: name a file in the source directory -- if this dnl isn't found then configure will complain AC_CONFIG_SRCDIR([pal.h]) dnl Include defaults for Starlink configurations STAR_DEFAULTS dnl Find required versions of the programs we need for configuration AC_PROG_CC LT_INIT # If --with-pic=no is set we should honour that. AM_CONDITIONAL(NOPIC, test x$pic_mode = xno) dnl copysign and isblank are a c99 feature AC_CHECK_FUNCS(copysign) AC_CHECK_FUNCS(isblank) dnl Use strlcpy if it is available AC_SEARCH_LIBS([strlcpy], [bsd]) AC_CHECK_FUNCS([strlcpy]) # Need the math library AC_CHECK_LIB([m],[sin]) dnl We can not simply test for Starlink starutil because dnl when configure runs in a Starlink build starutil will not dnl have been built yet. If --without-starlink has been used dnl $STARLINK will be unset so we test that. dnl If we do not have Starlink we can do the test anyhow just in case if test -n "$STARLINK" then AC_SUBST( STARUTIL_LIBADD, "${libdir}/libstarutil.la" ) AC_SUBST( ERFA_LIBADD, "${libdir}/liberfa.la" ) AC_SUBST( ERFA_LDFLAGS, "" ) AC_DEFINE( [HAVE_STAR_UTIL_H], [1], [Define to 1 if you have the header file]) else dnl AC_CHECK_HEADERS does not search $includedir save_CPPFLAGS="$CPPFLAGS" eval CPPFLAGS=\"$CPPFLAGS -I${includdir}\" eval CPPFLAGS=\"$CPPFLAGS\" AC_CHECK_HEADERS( star/util.h ) CPPFLAGS="$save_CPPFLAGS" dnl for some reason AC_CHECK_LIB does not look in the --prefix hierarchy so dnl $libdir is not searched. dnl and we use eval twice to convert $libdir -> $exec_prefix/lib -> $prefix/lib save_LDFLAGS="$LDFLAGS" eval LDFLAGS=\"$LDFLAGS -L${libdir}\" eval LDFLAGS=\"$LDFLAGS\" AC_CHECK_LIB([starutil],[star_strlcpy], [AC_SUBST(STARUTIL_LIBADD, "-lstarutil")], [AC_SUBST(STARUTIL_LIBADD, "")]) AC_CHECK_LIB([erfa],[eraCal2jd], [AC_SUBST(ERFA_LIBADD, "-lerfa")], [ AC_CHECK_LIB([sofa_c],[iauCal2jd], [AC_SUBST(ERFA_LIBADD, "-lsofa_c") AC_DEFINE([HAVE_SOFA_H],[1],"Build with SOFA library")], [AC_MSG_ERROR(Neither ERFA nor SOFA library located. Can not continue)]) ]) LDFLAGS="$save_LDFLAGS" dnl Ensure that we use the $prefix values AC_SUBST( ERFA_LDFLAGS, "-L${libdir}" ) AC_SUBST( ERFA_CPPFLAGS, "-I${includedir}" ) dnl Disable document building regardless of --without-stardocs _star_build_docs=: fi dnl Declare the build and use dependencies for this package STAR_DECLARE_DEPENDENCIES(build, [sofa starutil]) STAR_DECLARE_DEPENDENCIES(link, [sofa starutil]) dnl List the sun/ssn/... numbers which document this package and dnl which are present as .tex files in this directory. STAR_LATEX_DOCUMENTATION(sun267) dnl If you wish to configure extra files, you can add them to this dnl declaration. AC_CONFIG_FILES(Makefile component.xml) AC_CONFIG_HEADERS( config.h ) dnl This is the bit that does the actual work AC_OUTPUT pal-0.5.0/COPYING000644 000765 000024 00000104513 12360544345 013443 0ustar00timjstaff000000 000000 GNU GENERAL PUBLIC LICENSE Version 3, 29 June 2007 Copyright (C) 2007 Free Software Foundation, Inc. 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But first, please read . pal-0.5.0/COPYING.LESSER000644 000765 000024 00000016743 12360544345 014446 0ustar00timjstaff000000 000000 GNU LESSER GENERAL PUBLIC LICENSE Version 3, 29 June 2007 Copyright (C) 2007 Free Software Foundation, Inc. Everyone is permitted to copy and distribute verbatim copies of this license document, but changing it is not allowed. This version of the GNU Lesser General Public License incorporates the terms and conditions of version 3 of the GNU General Public License, supplemented by the additional permissions listed below. 0. Additional Definitions. As used herein, "this License" refers to version 3 of the GNU Lesser General Public License, and the "GNU GPL" refers to version 3 of the GNU General Public License. "The Library" refers to a covered work governed by this License, other than an Application or a Combined Work as defined below. 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If the Library as you received it specifies that a proxy can decide whether future versions of the GNU Lesser General Public License shall apply, that proxy's public statement of acceptance of any version is permanent authorization for you to choose that version for the Library. pal-0.5.0/depcomp000755 000765 000024 00000056016 12363621607 013771 0ustar00timjstaff000000 000000 #! /bin/sh # depcomp - compile a program generating dependencies as side-effects scriptversion=2013-05-30.07; # UTC # Copyright (C) 1999-2013 Free Software Foundation, Inc. # This program is free software; you can redistribute it and/or modify # it under the terms of the GNU General Public License as published by # the Free Software Foundation; either version 2, or (at your option) # any later version. # This program is distributed in the hope that it will be useful, # but WITHOUT ANY WARRANTY; without even the implied warranty of # MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the # GNU General Public License for more details. # You should have received a copy of the GNU General Public License # along with this program. If not, see . # As a special exception to the GNU General Public License, if you # distribute this file as part of a program that contains a # configuration script generated by Autoconf, you may include it under # the same distribution terms that you use for the rest of that program. # Originally written by Alexandre Oliva . case $1 in '') echo "$0: No command. Try '$0 --help' for more information." 1>&2 exit 1; ;; -h | --h*) cat <<\EOF Usage: depcomp [--help] [--version] PROGRAM [ARGS] Run PROGRAMS ARGS to compile a file, generating dependencies as side-effects. Environment variables: depmode Dependency tracking mode. source Source file read by 'PROGRAMS ARGS'. object Object file output by 'PROGRAMS ARGS'. DEPDIR directory where to store dependencies. depfile Dependency file to output. tmpdepfile Temporary file to use when outputting dependencies. libtool Whether libtool is used (yes/no). Report bugs to . EOF exit $? ;; -v | --v*) echo "depcomp $scriptversion" exit $? ;; esac # Get the directory component of the given path, and save it in the # global variables '$dir'. Note that this directory component will # be either empty or ending with a '/' character. This is deliberate. set_dir_from () { case $1 in */*) dir=`echo "$1" | sed -e 's|/[^/]*$|/|'`;; *) dir=;; esac } # Get the suffix-stripped basename of the given path, and save it the # global variable '$base'. set_base_from () { base=`echo "$1" | sed -e 's|^.*/||' -e 's/\.[^.]*$//'` } # If no dependency file was actually created by the compiler invocation, # we still have to create a dummy depfile, to avoid errors with the # Makefile "include basename.Plo" scheme. make_dummy_depfile () { echo "#dummy" > "$depfile" } # Factor out some common post-processing of the generated depfile. # Requires the auxiliary global variable '$tmpdepfile' to be set. aix_post_process_depfile () { # If the compiler actually managed to produce a dependency file, # post-process it. if test -f "$tmpdepfile"; then # Each line is of the form 'foo.o: dependency.h'. # Do two passes, one to just change these to # $object: dependency.h # and one to simply output # dependency.h: # which is needed to avoid the deleted-header problem. { sed -e "s,^.*\.[$lower]*:,$object:," < "$tmpdepfile" sed -e "s,^.*\.[$lower]*:[$tab ]*,," -e 's,$,:,' < "$tmpdepfile" } > "$depfile" rm -f "$tmpdepfile" else make_dummy_depfile fi } # A tabulation character. tab=' ' # A newline character. nl=' ' # Character ranges might be problematic outside the C locale. # These definitions help. upper=ABCDEFGHIJKLMNOPQRSTUVWXYZ lower=abcdefghijklmnopqrstuvwxyz digits=0123456789 alpha=${upper}${lower} if test -z "$depmode" || test -z "$source" || test -z "$object"; then echo "depcomp: Variables source, object and depmode must be set" 1>&2 exit 1 fi # Dependencies for sub/bar.o or sub/bar.obj go into sub/.deps/bar.Po. depfile=${depfile-`echo "$object" | sed 's|[^\\/]*$|'${DEPDIR-.deps}'/&|;s|\.\([^.]*\)$|.P\1|;s|Pobj$|Po|'`} tmpdepfile=${tmpdepfile-`echo "$depfile" | sed 's/\.\([^.]*\)$/.T\1/'`} rm -f "$tmpdepfile" # Avoid interferences from the environment. gccflag= dashmflag= # Some modes work just like other modes, but use different flags. We # parameterize here, but still list the modes in the big case below, # to make depend.m4 easier to write. Note that we *cannot* use a case # here, because this file can only contain one case statement. if test "$depmode" = hp; then # HP compiler uses -M and no extra arg. gccflag=-M depmode=gcc fi if test "$depmode" = dashXmstdout; then # This is just like dashmstdout with a different argument. dashmflag=-xM depmode=dashmstdout fi cygpath_u="cygpath -u -f -" if test "$depmode" = msvcmsys; then # This is just like msvisualcpp but w/o cygpath translation. # Just convert the backslash-escaped backslashes to single forward # slashes to satisfy depend.m4 cygpath_u='sed s,\\\\,/,g' depmode=msvisualcpp fi if test "$depmode" = msvc7msys; then # This is just like msvc7 but w/o cygpath translation. # Just convert the backslash-escaped backslashes to single forward # slashes to satisfy depend.m4 cygpath_u='sed s,\\\\,/,g' depmode=msvc7 fi if test "$depmode" = xlc; then # IBM C/C++ Compilers xlc/xlC can output gcc-like dependency information. gccflag=-qmakedep=gcc,-MF depmode=gcc fi case "$depmode" in gcc3) ## gcc 3 implements dependency tracking that does exactly what ## we want. Yay! Note: for some reason libtool 1.4 doesn't like ## it if -MD -MP comes after the -MF stuff. Hmm. ## Unfortunately, FreeBSD c89 acceptance of flags depends upon ## the command line argument order; so add the flags where they ## appear in depend2.am. Note that the slowdown incurred here ## affects only configure: in makefiles, %FASTDEP% shortcuts this. for arg do case $arg in -c) set fnord "$@" -MT "$object" -MD -MP -MF "$tmpdepfile" "$arg" ;; *) set fnord "$@" "$arg" ;; esac shift # fnord shift # $arg done "$@" stat=$? if test $stat -ne 0; then rm -f "$tmpdepfile" exit $stat fi mv "$tmpdepfile" "$depfile" ;; gcc) ## Note that this doesn't just cater to obsosete pre-3.x GCC compilers. ## but also to in-use compilers like IMB xlc/xlC and the HP C compiler. ## (see the conditional assignment to $gccflag above). ## There are various ways to get dependency output from gcc. Here's ## why we pick this rather obscure method: ## - Don't want to use -MD because we'd like the dependencies to end ## up in a subdir. Having to rename by hand is ugly. ## (We might end up doing this anyway to support other compilers.) ## - The DEPENDENCIES_OUTPUT environment variable makes gcc act like ## -MM, not -M (despite what the docs say). Also, it might not be ## supported by the other compilers which use the 'gcc' depmode. ## - Using -M directly means running the compiler twice (even worse ## than renaming). if test -z "$gccflag"; then gccflag=-MD, fi "$@" -Wp,"$gccflag$tmpdepfile" stat=$? if test $stat -ne 0; then rm -f "$tmpdepfile" exit $stat fi rm -f "$depfile" echo "$object : \\" > "$depfile" # The second -e expression handles DOS-style file names with drive # letters. sed -e 's/^[^:]*: / /' \ -e 's/^['$alpha']:\/[^:]*: / /' < "$tmpdepfile" >> "$depfile" ## This next piece of magic avoids the "deleted header file" problem. ## The problem is that when a header file which appears in a .P file ## is deleted, the dependency causes make to die (because there is ## typically no way to rebuild the header). We avoid this by adding ## dummy dependencies for each header file. Too bad gcc doesn't do ## this for us directly. ## Some versions of gcc put a space before the ':'. On the theory ## that the space means something, we add a space to the output as ## well. hp depmode also adds that space, but also prefixes the VPATH ## to the object. Take care to not repeat it in the output. ## Some versions of the HPUX 10.20 sed can't process this invocation ## correctly. Breaking it into two sed invocations is a workaround. tr ' ' "$nl" < "$tmpdepfile" \ | sed -e 's/^\\$//' -e '/^$/d' -e "s|.*$object$||" -e '/:$/d' \ | sed -e 's/$/ :/' >> "$depfile" rm -f "$tmpdepfile" ;; hp) # This case exists only to let depend.m4 do its work. It works by # looking at the text of this script. This case will never be run, # since it is checked for above. exit 1 ;; sgi) if test "$libtool" = yes; then "$@" "-Wp,-MDupdate,$tmpdepfile" else "$@" -MDupdate "$tmpdepfile" fi stat=$? if test $stat -ne 0; then rm -f "$tmpdepfile" exit $stat fi rm -f "$depfile" if test -f "$tmpdepfile"; then # yes, the sourcefile depend on other files echo "$object : \\" > "$depfile" # Clip off the initial element (the dependent). Don't try to be # clever and replace this with sed code, as IRIX sed won't handle # lines with more than a fixed number of characters (4096 in # IRIX 6.2 sed, 8192 in IRIX 6.5). We also remove comment lines; # the IRIX cc adds comments like '#:fec' to the end of the # dependency line. tr ' ' "$nl" < "$tmpdepfile" \ | sed -e 's/^.*\.o://' -e 's/#.*$//' -e '/^$/ d' \ | tr "$nl" ' ' >> "$depfile" echo >> "$depfile" # The second pass generates a dummy entry for each header file. tr ' ' "$nl" < "$tmpdepfile" \ | sed -e 's/^.*\.o://' -e 's/#.*$//' -e '/^$/ d' -e 's/$/:/' \ >> "$depfile" else make_dummy_depfile fi rm -f "$tmpdepfile" ;; xlc) # This case exists only to let depend.m4 do its work. It works by # looking at the text of this script. This case will never be run, # since it is checked for above. exit 1 ;; aix) # The C for AIX Compiler uses -M and outputs the dependencies # in a .u file. In older versions, this file always lives in the # current directory. Also, the AIX compiler puts '$object:' at the # start of each line; $object doesn't have directory information. # Version 6 uses the directory in both cases. set_dir_from "$object" set_base_from "$object" if test "$libtool" = yes; then tmpdepfile1=$dir$base.u tmpdepfile2=$base.u tmpdepfile3=$dir.libs/$base.u "$@" -Wc,-M else tmpdepfile1=$dir$base.u tmpdepfile2=$dir$base.u tmpdepfile3=$dir$base.u "$@" -M fi stat=$? if test $stat -ne 0; then rm -f "$tmpdepfile1" "$tmpdepfile2" "$tmpdepfile3" exit $stat fi for tmpdepfile in "$tmpdepfile1" "$tmpdepfile2" "$tmpdepfile3" do test -f "$tmpdepfile" && break done aix_post_process_depfile ;; tcc) # tcc (Tiny C Compiler) understand '-MD -MF file' since version 0.9.26 # FIXME: That version still under development at the moment of writing. # Make that this statement remains true also for stable, released # versions. # It will wrap lines (doesn't matter whether long or short) with a # trailing '\', as in: # # foo.o : \ # foo.c \ # foo.h \ # # It will put a trailing '\' even on the last line, and will use leading # spaces rather than leading tabs (at least since its commit 0394caf7 # "Emit spaces for -MD"). "$@" -MD -MF "$tmpdepfile" stat=$? if test $stat -ne 0; then rm -f "$tmpdepfile" exit $stat fi rm -f "$depfile" # Each non-empty line is of the form 'foo.o : \' or ' dep.h \'. # We have to change lines of the first kind to '$object: \'. sed -e "s|.*:|$object :|" < "$tmpdepfile" > "$depfile" # And for each line of the second kind, we have to emit a 'dep.h:' # dummy dependency, to avoid the deleted-header problem. sed -n -e 's|^ *\(.*\) *\\$|\1:|p' < "$tmpdepfile" >> "$depfile" rm -f "$tmpdepfile" ;; ## The order of this option in the case statement is important, since the ## shell code in configure will try each of these formats in the order ## listed in this file. A plain '-MD' option would be understood by many ## compilers, so we must ensure this comes after the gcc and icc options. pgcc) # Portland's C compiler understands '-MD'. # Will always output deps to 'file.d' where file is the root name of the # source file under compilation, even if file resides in a subdirectory. # The object file name does not affect the name of the '.d' file. # pgcc 10.2 will output # foo.o: sub/foo.c sub/foo.h # and will wrap long lines using '\' : # foo.o: sub/foo.c ... \ # sub/foo.h ... \ # ... set_dir_from "$object" # Use the source, not the object, to determine the base name, since # that's sadly what pgcc will do too. set_base_from "$source" tmpdepfile=$base.d # For projects that build the same source file twice into different object # files, the pgcc approach of using the *source* file root name can cause # problems in parallel builds. Use a locking strategy to avoid stomping on # the same $tmpdepfile. lockdir=$base.d-lock trap " echo '$0: caught signal, cleaning up...' >&2 rmdir '$lockdir' exit 1 " 1 2 13 15 numtries=100 i=$numtries while test $i -gt 0; do # mkdir is a portable test-and-set. if mkdir "$lockdir" 2>/dev/null; then # This process acquired the lock. "$@" -MD stat=$? # Release the lock. rmdir "$lockdir" break else # If the lock is being held by a different process, wait # until the winning process is done or we timeout. while test -d "$lockdir" && test $i -gt 0; do sleep 1 i=`expr $i - 1` done fi i=`expr $i - 1` done trap - 1 2 13 15 if test $i -le 0; then echo "$0: failed to acquire lock after $numtries attempts" >&2 echo "$0: check lockdir '$lockdir'" >&2 exit 1 fi if test $stat -ne 0; then rm -f "$tmpdepfile" exit $stat fi rm -f "$depfile" # Each line is of the form `foo.o: dependent.h', # or `foo.o: dep1.h dep2.h \', or ` dep3.h dep4.h \'. # Do two passes, one to just change these to # `$object: dependent.h' and one to simply `dependent.h:'. sed "s,^[^:]*:,$object :," < "$tmpdepfile" > "$depfile" # Some versions of the HPUX 10.20 sed can't process this invocation # correctly. Breaking it into two sed invocations is a workaround. sed 's,^[^:]*: \(.*\)$,\1,;s/^\\$//;/^$/d;/:$/d' < "$tmpdepfile" \ | sed -e 's/$/ :/' >> "$depfile" rm -f "$tmpdepfile" ;; hp2) # The "hp" stanza above does not work with aCC (C++) and HP's ia64 # compilers, which have integrated preprocessors. The correct option # to use with these is +Maked; it writes dependencies to a file named # 'foo.d', which lands next to the object file, wherever that # happens to be. # Much of this is similar to the tru64 case; see comments there. set_dir_from "$object" set_base_from "$object" if test "$libtool" = yes; then tmpdepfile1=$dir$base.d tmpdepfile2=$dir.libs/$base.d "$@" -Wc,+Maked else tmpdepfile1=$dir$base.d tmpdepfile2=$dir$base.d "$@" +Maked fi stat=$? if test $stat -ne 0; then rm -f "$tmpdepfile1" "$tmpdepfile2" exit $stat fi for tmpdepfile in "$tmpdepfile1" "$tmpdepfile2" do test -f "$tmpdepfile" && break done if test -f "$tmpdepfile"; then sed -e "s,^.*\.[$lower]*:,$object:," "$tmpdepfile" > "$depfile" # Add 'dependent.h:' lines. sed -ne '2,${ s/^ *// s/ \\*$// s/$/:/ p }' "$tmpdepfile" >> "$depfile" else make_dummy_depfile fi rm -f "$tmpdepfile" "$tmpdepfile2" ;; tru64) # The Tru64 compiler uses -MD to generate dependencies as a side # effect. 'cc -MD -o foo.o ...' puts the dependencies into 'foo.o.d'. # At least on Alpha/Redhat 6.1, Compaq CCC V6.2-504 seems to put # dependencies in 'foo.d' instead, so we check for that too. # Subdirectories are respected. set_dir_from "$object" set_base_from "$object" if test "$libtool" = yes; then # Libtool generates 2 separate objects for the 2 libraries. These # two compilations output dependencies in $dir.libs/$base.o.d and # in $dir$base.o.d. We have to check for both files, because # one of the two compilations can be disabled. We should prefer # $dir$base.o.d over $dir.libs/$base.o.d because the latter is # automatically cleaned when .libs/ is deleted, while ignoring # the former would cause a distcleancheck panic. tmpdepfile1=$dir$base.o.d # libtool 1.5 tmpdepfile2=$dir.libs/$base.o.d # Likewise. tmpdepfile3=$dir.libs/$base.d # Compaq CCC V6.2-504 "$@" -Wc,-MD else tmpdepfile1=$dir$base.d tmpdepfile2=$dir$base.d tmpdepfile3=$dir$base.d "$@" -MD fi stat=$? if test $stat -ne 0; then rm -f "$tmpdepfile1" "$tmpdepfile2" "$tmpdepfile3" exit $stat fi for tmpdepfile in "$tmpdepfile1" "$tmpdepfile2" "$tmpdepfile3" do test -f "$tmpdepfile" && break done # Same post-processing that is required for AIX mode. aix_post_process_depfile ;; msvc7) if test "$libtool" = yes; then showIncludes=-Wc,-showIncludes else showIncludes=-showIncludes fi "$@" $showIncludes > "$tmpdepfile" stat=$? grep -v '^Note: including file: ' "$tmpdepfile" if test $stat -ne 0; then rm -f "$tmpdepfile" exit $stat fi rm -f "$depfile" echo "$object : \\" > "$depfile" # The first sed program below extracts the file names and escapes # backslashes for cygpath. The second sed program outputs the file # name when reading, but also accumulates all include files in the # hold buffer in order to output them again at the end. This only # works with sed implementations that can handle large buffers. sed < "$tmpdepfile" -n ' /^Note: including file: *\(.*\)/ { s//\1/ s/\\/\\\\/g p }' | $cygpath_u | sort -u | sed -n ' s/ /\\ /g s/\(.*\)/'"$tab"'\1 \\/p s/.\(.*\) \\/\1:/ H $ { s/.*/'"$tab"'/ G p }' >> "$depfile" echo >> "$depfile" # make sure the fragment doesn't end with a backslash rm -f "$tmpdepfile" ;; msvc7msys) # This case exists only to let depend.m4 do its work. It works by # looking at the text of this script. This case will never be run, # since it is checked for above. exit 1 ;; #nosideeffect) # This comment above is used by automake to tell side-effect # dependency tracking mechanisms from slower ones. dashmstdout) # Important note: in order to support this mode, a compiler *must* # always write the preprocessed file to stdout, regardless of -o. "$@" || exit $? # Remove the call to Libtool. if test "$libtool" = yes; then while test "X$1" != 'X--mode=compile'; do shift done shift fi # Remove '-o $object'. IFS=" " for arg do case $arg in -o) shift ;; $object) shift ;; *) set fnord "$@" "$arg" shift # fnord shift # $arg ;; esac done test -z "$dashmflag" && dashmflag=-M # Require at least two characters before searching for ':' # in the target name. This is to cope with DOS-style filenames: # a dependency such as 'c:/foo/bar' could be seen as target 'c' otherwise. "$@" $dashmflag | sed "s|^[$tab ]*[^:$tab ][^:][^:]*:[$tab ]*|$object: |" > "$tmpdepfile" rm -f "$depfile" cat < "$tmpdepfile" > "$depfile" # Some versions of the HPUX 10.20 sed can't process this sed invocation # correctly. Breaking it into two sed invocations is a workaround. tr ' ' "$nl" < "$tmpdepfile" \ | sed -e 's/^\\$//' -e '/^$/d' -e '/:$/d' \ | sed -e 's/$/ :/' >> "$depfile" rm -f "$tmpdepfile" ;; dashXmstdout) # This case only exists to satisfy depend.m4. It is never actually # run, as this mode is specially recognized in the preamble. exit 1 ;; makedepend) "$@" || exit $? # Remove any Libtool call if test "$libtool" = yes; then while test "X$1" != 'X--mode=compile'; do shift done shift fi # X makedepend shift cleared=no eat=no for arg do case $cleared in no) set ""; shift cleared=yes ;; esac if test $eat = yes; then eat=no continue fi case "$arg" in -D*|-I*) set fnord "$@" "$arg"; shift ;; # Strip any option that makedepend may not understand. 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"$@" || exit $? # Remove the call to Libtool. if test "$libtool" = yes; then while test "X$1" != 'X--mode=compile'; do shift done shift fi # Remove '-o $object'. IFS=" " for arg do case $arg in -o) shift ;; $object) shift ;; *) set fnord "$@" "$arg" shift # fnord shift # $arg ;; esac done "$@" -E \ | sed -n -e '/^# [0-9][0-9]* "\([^"]*\)".*/ s:: \1 \\:p' \ -e '/^#line [0-9][0-9]* "\([^"]*\)".*/ s:: \1 \\:p' \ | sed '$ s: \\$::' > "$tmpdepfile" rm -f "$depfile" echo "$object : \\" > "$depfile" cat < "$tmpdepfile" >> "$depfile" sed < "$tmpdepfile" '/^$/d;s/^ //;s/ \\$//;s/$/ :/' >> "$depfile" rm -f "$tmpdepfile" ;; msvisualcpp) # Important note: in order to support this mode, a compiler *must* # always write the preprocessed file to stdout. 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There is NO # warranty; not even for MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. # GNU Libtool is free software; you can redistribute it and/or modify # it under the terms of the GNU General Public License as published by # the Free Software Foundation; either version 2 of the License, or # (at your option) any later version. # # As a special exception to the GNU General Public License, # if you distribute this file as part of a program or library that # is built using GNU Libtool, you may include this file under the # same distribution terms that you use for the rest of that program. # # GNU Libtool is distributed in the hope that it will be useful, but # WITHOUT ANY WARRANTY; without even the implied warranty of # MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the GNU # General Public License for more details. # # You should have received a copy of the GNU General Public License # along with GNU Libtool; see the file COPYING. 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If nonempty, add APPEND to the result, # otherwise set result to NONDIR_REPLACEMENT. func_dirname () { func_dirname_result=`$ECHO "${1}" | $SED "$dirname"` if test "X$func_dirname_result" = "X${1}"; then func_dirname_result="${3}" else func_dirname_result="$func_dirname_result${2}" fi } # func_dirname may be replaced by extended shell implementation # func_basename file func_basename () { func_basename_result=`$ECHO "${1}" | $SED "$basename"` } # func_basename may be replaced by extended shell implementation # func_dirname_and_basename file append nondir_replacement # perform func_basename and func_dirname in a single function # call: # dirname: Compute the dirname of FILE. If nonempty, # add APPEND to the result, otherwise set result # to NONDIR_REPLACEMENT. # value returned in "$func_dirname_result" # basename: Compute filename of FILE. # value retuned in "$func_basename_result" # Implementation must be kept synchronized with func_dirname # and func_basename. 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We also want # the path to end with a slash for ease of parsing, so make sure # there is one (and only one) here. func_normal_abspath_tpath=`$ECHO "$func_normal_abspath_tpath" | $SED \ -e "$removedotparts" -e "$collapseslashes" -e "$finalslash"` while :; do # Processed it all yet? if test "$func_normal_abspath_tpath" = / ; then # If we ascended to the root using ".." the result may be empty now. if test -z "$func_normal_abspath_result" ; then func_normal_abspath_result=/ fi break fi func_normal_abspath_tcomponent=`$ECHO "$func_normal_abspath_tpath" | $SED \ -e "$pathcar"` func_normal_abspath_tpath=`$ECHO "$func_normal_abspath_tpath" | $SED \ -e "$pathcdr"` # Figure out what to do with it case $func_normal_abspath_tcomponent in "") # Trailing empty path component, ignore it. ;; ..) # Parent dir; strip last assembled component from result. func_dirname "$func_normal_abspath_result" func_normal_abspath_result=$func_dirname_result ;; *) # Actual path component, append it. func_normal_abspath_result=$func_normal_abspath_result/$func_normal_abspath_tcomponent ;; esac done # Restore leading double-slash if one was found on entry. func_normal_abspath_result=$func_normal_abspath_altnamespace$func_normal_abspath_result } # func_relative_path SRCDIR DSTDIR # generates a relative path from SRCDIR to DSTDIR, with a trailing # slash if non-empty, suitable for immediately appending a filename # without needing to append a separator. # value returned in "$func_relative_path_result" func_relative_path () { func_relative_path_result= func_normal_abspath "$1" func_relative_path_tlibdir=$func_normal_abspath_result func_normal_abspath "$2" func_relative_path_tbindir=$func_normal_abspath_result # Ascend the tree starting from libdir while :; do # check if we have found a prefix of bindir case $func_relative_path_tbindir in $func_relative_path_tlibdir) # found an exact match func_relative_path_tcancelled= break ;; $func_relative_path_tlibdir*) # found a matching prefix func_stripname "$func_relative_path_tlibdir" '' "$func_relative_path_tbindir" func_relative_path_tcancelled=$func_stripname_result if test -z "$func_relative_path_result"; then func_relative_path_result=. fi break ;; *) func_dirname $func_relative_path_tlibdir func_relative_path_tlibdir=${func_dirname_result} if test "x$func_relative_path_tlibdir" = x ; then # Have to descend all the way to the root! func_relative_path_result=../$func_relative_path_result func_relative_path_tcancelled=$func_relative_path_tbindir break fi func_relative_path_result=../$func_relative_path_result ;; esac done # Now calculate path; take care to avoid doubling-up slashes. func_stripname '' '/' "$func_relative_path_result" func_relative_path_result=$func_stripname_result func_stripname '/' '/' "$func_relative_path_tcancelled" if test "x$func_stripname_result" != x ; then func_relative_path_result=${func_relative_path_result}/${func_stripname_result} fi # Normalisation. If bindir is libdir, return empty string, # else relative path ending with a slash; either way, target # file name can be directly appended. if test ! -z "$func_relative_path_result"; then func_stripname './' '' "$func_relative_path_result/" func_relative_path_result=$func_stripname_result fi } # The name of this program: func_dirname_and_basename "$progpath" progname=$func_basename_result # Make sure we have an absolute path for reexecution: case $progpath in [\\/]*|[A-Za-z]:\\*) ;; *[\\/]*) progdir=$func_dirname_result progdir=`cd "$progdir" && pwd` progpath="$progdir/$progname" ;; *) save_IFS="$IFS" IFS=${PATH_SEPARATOR-:} for progdir in $PATH; do IFS="$save_IFS" test -x "$progdir/$progname" && break done IFS="$save_IFS" test -n "$progdir" || progdir=`pwd` progpath="$progdir/$progname" ;; esac # Sed substitution that helps us do robust quoting. It backslashifies # metacharacters that are still active within double-quoted strings. Xsed="${SED}"' -e 1s/^X//' sed_quote_subst='s/\([`"$\\]\)/\\\1/g' # Same as above, but do not quote variable references. double_quote_subst='s/\(["`\\]\)/\\\1/g' # Sed substitution that turns a string into a regex matching for the # string literally. sed_make_literal_regex='s,[].[^$\\*\/],\\&,g' # Sed substitution that converts a w32 file name or path # which contains forward slashes, into one that contains # (escaped) backslashes. A very naive implementation. lt_sed_naive_backslashify='s|\\\\*|\\|g;s|/|\\|g;s|\\|\\\\|g' # Re-`\' parameter expansions in output of double_quote_subst that were # `\'-ed in input to the same. If an odd number of `\' preceded a '$' # in input to double_quote_subst, that '$' was protected from expansion. # Since each input `\' is now two `\'s, look for any number of runs of # four `\'s followed by two `\'s and then a '$'. `\' that '$'. bs='\\' bs2='\\\\' bs4='\\\\\\\\' dollar='\$' sed_double_backslash="\ s/$bs4/&\\ /g s/^$bs2$dollar/$bs&/ s/\\([^$bs]\\)$bs2$dollar/\\1$bs2$bs$dollar/g s/\n//g" # Standard options: opt_dry_run=false opt_help=false opt_quiet=false opt_verbose=false opt_warning=: # func_echo arg... # Echo program name prefixed message, along with the current mode # name if it has been set yet. func_echo () { $ECHO "$progname: ${opt_mode+$opt_mode: }$*" } # func_verbose arg... # Echo program name prefixed message in verbose mode only. func_verbose () { $opt_verbose && func_echo ${1+"$@"} # A bug in bash halts the script if the last line of a function # fails when set -e is in force, so we need another command to # work around that: : } # func_echo_all arg... # Invoke $ECHO with all args, space-separated. func_echo_all () { $ECHO "$*" } # func_error arg... # Echo program name prefixed message to standard error. func_error () { $ECHO "$progname: ${opt_mode+$opt_mode: }"${1+"$@"} 1>&2 } # func_warning arg... # Echo program name prefixed warning message to standard error. func_warning () { $opt_warning && $ECHO "$progname: ${opt_mode+$opt_mode: }warning: "${1+"$@"} 1>&2 # bash bug again: : } # func_fatal_error arg... # Echo program name prefixed message to standard error, and exit. func_fatal_error () { func_error ${1+"$@"} exit $EXIT_FAILURE } # func_fatal_help arg... # Echo program name prefixed message to standard error, followed by # a help hint, and exit. func_fatal_help () { func_error ${1+"$@"} func_fatal_error "$help" } help="Try \`$progname --help' for more information." ## default # func_grep expression filename # Check whether EXPRESSION matches any line of FILENAME, without output. func_grep () { $GREP "$1" "$2" >/dev/null 2>&1 } # func_mkdir_p directory-path # Make sure the entire path to DIRECTORY-PATH is available. func_mkdir_p () { my_directory_path="$1" my_dir_list= if test -n "$my_directory_path" && test "$opt_dry_run" != ":"; then # Protect directory names starting with `-' case $my_directory_path in -*) my_directory_path="./$my_directory_path" ;; esac # While some portion of DIR does not yet exist... while test ! -d "$my_directory_path"; do # ...make a list in topmost first order. Use a colon delimited # list incase some portion of path contains whitespace. my_dir_list="$my_directory_path:$my_dir_list" # If the last portion added has no slash in it, the list is done case $my_directory_path in */*) ;; *) break ;; esac # ...otherwise throw away the child directory and loop my_directory_path=`$ECHO "$my_directory_path" | $SED -e "$dirname"` done my_dir_list=`$ECHO "$my_dir_list" | $SED 's,:*$,,'` save_mkdir_p_IFS="$IFS"; IFS=':' for my_dir in $my_dir_list; do IFS="$save_mkdir_p_IFS" # mkdir can fail with a `File exist' error if two processes # try to create one of the directories concurrently. Don't # stop in that case! $MKDIR "$my_dir" 2>/dev/null || : done IFS="$save_mkdir_p_IFS" # Bail out if we (or some other process) failed to create a directory. test -d "$my_directory_path" || \ func_fatal_error "Failed to create \`$1'" fi } # func_mktempdir [string] # Make a temporary directory that won't clash with other running # libtool processes, and avoids race conditions if possible. If # given, STRING is the basename for that directory. func_mktempdir () { my_template="${TMPDIR-/tmp}/${1-$progname}" if test "$opt_dry_run" = ":"; then # Return a directory name, but don't create it in dry-run mode my_tmpdir="${my_template}-$$" else # If mktemp works, use that first and foremost my_tmpdir=`mktemp -d "${my_template}-XXXXXXXX" 2>/dev/null` if test ! -d "$my_tmpdir"; then # Failing that, at least try and use $RANDOM to avoid a race my_tmpdir="${my_template}-${RANDOM-0}$$" save_mktempdir_umask=`umask` umask 0077 $MKDIR "$my_tmpdir" umask $save_mktempdir_umask fi # If we're not in dry-run mode, bomb out on failure test -d "$my_tmpdir" || \ func_fatal_error "cannot create temporary directory \`$my_tmpdir'" fi $ECHO "$my_tmpdir" } # func_quote_for_eval arg # Aesthetically quote ARG to be evaled later. # This function returns two values: FUNC_QUOTE_FOR_EVAL_RESULT # is double-quoted, suitable for a subsequent eval, whereas # FUNC_QUOTE_FOR_EVAL_UNQUOTED_RESULT has merely all characters # which are still active within double quotes backslashified. func_quote_for_eval () { case $1 in *[\\\`\"\$]*) func_quote_for_eval_unquoted_result=`$ECHO "$1" | $SED "$sed_quote_subst"` ;; *) func_quote_for_eval_unquoted_result="$1" ;; esac case $func_quote_for_eval_unquoted_result in # Double-quote args containing shell metacharacters to delay # word splitting, command substitution and and variable # expansion for a subsequent eval. # Many Bourne shells cannot handle close brackets correctly # in scan sets, so we specify it separately. *[\[\~\#\^\&\*\(\)\{\}\|\;\<\>\?\'\ \ ]*|*]*|"") func_quote_for_eval_result="\"$func_quote_for_eval_unquoted_result\"" ;; *) func_quote_for_eval_result="$func_quote_for_eval_unquoted_result" esac } # func_quote_for_expand arg # Aesthetically quote ARG to be evaled later; same as above, # but do not quote variable references. func_quote_for_expand () { case $1 in *[\\\`\"]*) my_arg=`$ECHO "$1" | $SED \ -e "$double_quote_subst" -e "$sed_double_backslash"` ;; *) my_arg="$1" ;; esac case $my_arg in # Double-quote args containing shell metacharacters to delay # word splitting and command substitution for a subsequent eval. # Many Bourne shells cannot handle close brackets correctly # in scan sets, so we specify it separately. *[\[\~\#\^\&\*\(\)\{\}\|\;\<\>\?\'\ \ ]*|*]*|"") my_arg="\"$my_arg\"" ;; esac func_quote_for_expand_result="$my_arg" } # func_show_eval cmd [fail_exp] # Unless opt_silent is true, then output CMD. Then, if opt_dryrun is # not true, evaluate CMD. If the evaluation of CMD fails, and FAIL_EXP # is given, then evaluate it. func_show_eval () { my_cmd="$1" my_fail_exp="${2-:}" ${opt_silent-false} || { func_quote_for_expand "$my_cmd" eval "func_echo $func_quote_for_expand_result" } if ${opt_dry_run-false}; then :; else eval "$my_cmd" my_status=$? if test "$my_status" -eq 0; then :; else eval "(exit $my_status); $my_fail_exp" fi fi } # func_show_eval_locale cmd [fail_exp] # Unless opt_silent is true, then output CMD. Then, if opt_dryrun is # not true, evaluate CMD. If the evaluation of CMD fails, and FAIL_EXP # is given, then evaluate it. Use the saved locale for evaluation. func_show_eval_locale () { my_cmd="$1" my_fail_exp="${2-:}" ${opt_silent-false} || { func_quote_for_expand "$my_cmd" eval "func_echo $func_quote_for_expand_result" } if ${opt_dry_run-false}; then :; else eval "$lt_user_locale $my_cmd" my_status=$? eval "$lt_safe_locale" if test "$my_status" -eq 0; then :; else eval "(exit $my_status); $my_fail_exp" fi fi } # func_tr_sh # Turn $1 into a string suitable for a shell variable name. # Result is stored in $func_tr_sh_result. All characters # not in the set a-zA-Z0-9_ are replaced with '_'. Further, # if $1 begins with a digit, a '_' is prepended as well. func_tr_sh () { case $1 in [0-9]* | *[!a-zA-Z0-9_]*) func_tr_sh_result=`$ECHO "$1" | $SED 's/^\([0-9]\)/_\1/; s/[^a-zA-Z0-9_]/_/g'` ;; * ) func_tr_sh_result=$1 ;; esac } # func_version # Echo version message to standard output and exit. func_version () { $opt_debug $SED -n '/(C)/!b go :more /\./!{ N s/\n# / / b more } :go /^# '$PROGRAM' (GNU /,/# warranty; / { s/^# // s/^# *$// s/\((C)\)[ 0-9,-]*\( [1-9][0-9]*\)/\1\2/ p }' < "$progpath" exit $? } # func_usage # Echo short help message to standard output and exit. func_usage () { $opt_debug $SED -n '/^# Usage:/,/^# *.*--help/ { s/^# // s/^# *$// s/\$progname/'$progname'/ p }' < "$progpath" echo $ECHO "run \`$progname --help | more' for full usage" exit $? } # func_help [NOEXIT] # Echo long help message to standard output and exit, # unless 'noexit' is passed as argument. func_help () { $opt_debug $SED -n '/^# Usage:/,/# Report bugs to/ { :print s/^# // s/^# *$// s*\$progname*'$progname'* s*\$host*'"$host"'* s*\$SHELL*'"$SHELL"'* s*\$LTCC*'"$LTCC"'* s*\$LTCFLAGS*'"$LTCFLAGS"'* s*\$LD*'"$LD"'* s/\$with_gnu_ld/'"$with_gnu_ld"'/ s/\$automake_version/'"`(${AUTOMAKE-automake} --version) 2>/dev/null |$SED 1q`"'/ s/\$autoconf_version/'"`(${AUTOCONF-autoconf} --version) 2>/dev/null |$SED 1q`"'/ p d } /^# .* home page:/b print /^# General help using/b print ' < "$progpath" ret=$? if test -z "$1"; then exit $ret fi } # func_missing_arg argname # Echo program name prefixed message to standard error and set global # exit_cmd. func_missing_arg () { $opt_debug func_error "missing argument for $1." exit_cmd=exit } # func_split_short_opt shortopt # Set func_split_short_opt_name and func_split_short_opt_arg shell # variables after splitting SHORTOPT after the 2nd character. func_split_short_opt () { my_sed_short_opt='1s/^\(..\).*$/\1/;q' my_sed_short_rest='1s/^..\(.*\)$/\1/;q' func_split_short_opt_name=`$ECHO "$1" | $SED "$my_sed_short_opt"` func_split_short_opt_arg=`$ECHO "$1" | $SED "$my_sed_short_rest"` } # func_split_short_opt may be replaced by extended shell implementation # func_split_long_opt longopt # Set func_split_long_opt_name and func_split_long_opt_arg shell # variables after splitting LONGOPT at the `=' sign. func_split_long_opt () { my_sed_long_opt='1s/^\(--[^=]*\)=.*/\1/;q' my_sed_long_arg='1s/^--[^=]*=//' func_split_long_opt_name=`$ECHO "$1" | $SED "$my_sed_long_opt"` func_split_long_opt_arg=`$ECHO "$1" | $SED "$my_sed_long_arg"` } # func_split_long_opt may be replaced by extended shell implementation exit_cmd=: magic="%%%MAGIC variable%%%" magic_exe="%%%MAGIC EXE variable%%%" # Global variables. nonopt= preserve_args= lo2o="s/\\.lo\$/.${objext}/" o2lo="s/\\.${objext}\$/.lo/" extracted_archives= extracted_serial=0 # If this variable is set in any of the actions, the command in it # will be execed at the end. This prevents here-documents from being # left over by shells. exec_cmd= # func_append var value # Append VALUE to the end of shell variable VAR. func_append () { eval "${1}=\$${1}\${2}" } # func_append may be replaced by extended shell implementation # func_append_quoted var value # Quote VALUE and append to the end of shell variable VAR, separated # by a space. func_append_quoted () { func_quote_for_eval "${2}" eval "${1}=\$${1}\\ \$func_quote_for_eval_result" } # func_append_quoted may be replaced by extended shell implementation # func_arith arithmetic-term... func_arith () { func_arith_result=`expr "${@}"` } # func_arith may be replaced by extended shell implementation # func_len string # STRING may not start with a hyphen. func_len () { func_len_result=`expr "${1}" : ".*" 2>/dev/null || echo $max_cmd_len` } # func_len may be replaced by extended shell implementation # func_lo2o object func_lo2o () { func_lo2o_result=`$ECHO "${1}" | $SED "$lo2o"` } # func_lo2o may be replaced by extended shell implementation # func_xform libobj-or-source func_xform () { func_xform_result=`$ECHO "${1}" | $SED 's/\.[^.]*$/.lo/'` } # func_xform may be replaced by extended shell implementation # func_fatal_configuration arg... # Echo program name prefixed message to standard error, followed by # a configuration failure hint, and exit. func_fatal_configuration () { func_error ${1+"$@"} func_error "See the $PACKAGE documentation for more information." func_fatal_error "Fatal configuration error." } # func_config # Display the configuration for all the tags in this script. func_config () { re_begincf='^# ### BEGIN LIBTOOL' re_endcf='^# ### END LIBTOOL' # Default configuration. $SED "1,/$re_begincf CONFIG/d;/$re_endcf CONFIG/,\$d" < "$progpath" # Now print the configurations for the tags. for tagname in $taglist; do $SED -n "/$re_begincf TAG CONFIG: $tagname\$/,/$re_endcf TAG CONFIG: $tagname\$/p" < "$progpath" done exit $? } # func_features # Display the features supported by this script. func_features () { echo "host: $host" if test "$build_libtool_libs" = yes; then echo "enable shared libraries" else echo "disable shared libraries" fi if test "$build_old_libs" = yes; then echo "enable static libraries" else echo "disable static libraries" fi exit $? } # func_enable_tag tagname # Verify that TAGNAME is valid, and either flag an error and exit, or # enable the TAGNAME tag. We also add TAGNAME to the global $taglist # variable here. func_enable_tag () { # Global variable: tagname="$1" re_begincf="^# ### BEGIN LIBTOOL TAG CONFIG: $tagname\$" re_endcf="^# ### END LIBTOOL TAG CONFIG: $tagname\$" sed_extractcf="/$re_begincf/,/$re_endcf/p" # Validate tagname. case $tagname in *[!-_A-Za-z0-9,/]*) func_fatal_error "invalid tag name: $tagname" ;; esac # Don't test for the "default" C tag, as we know it's # there but not specially marked. case $tagname in CC) ;; *) if $GREP "$re_begincf" "$progpath" >/dev/null 2>&1; then taglist="$taglist $tagname" # Evaluate the configuration. Be careful to quote the path # and the sed script, to avoid splitting on whitespace, but # also don't use non-portable quotes within backquotes within # quotes we have to do it in 2 steps: extractedcf=`$SED -n -e "$sed_extractcf" < "$progpath"` eval "$extractedcf" else func_error "ignoring unknown tag $tagname" fi ;; esac } # func_check_version_match # Ensure that we are using m4 macros, and libtool script from the same # release of libtool. func_check_version_match () { if test "$package_revision" != "$macro_revision"; then if test "$VERSION" != "$macro_version"; then if test -z "$macro_version"; then cat >&2 <<_LT_EOF $progname: Version mismatch error. This is $PACKAGE $VERSION, but the $progname: definition of this LT_INIT comes from an older release. $progname: You should recreate aclocal.m4 with macros from $PACKAGE $VERSION $progname: and run autoconf again. _LT_EOF else cat >&2 <<_LT_EOF $progname: Version mismatch error. This is $PACKAGE $VERSION, but the $progname: definition of this LT_INIT comes from $PACKAGE $macro_version. $progname: You should recreate aclocal.m4 with macros from $PACKAGE $VERSION $progname: and run autoconf again. _LT_EOF fi else cat >&2 <<_LT_EOF $progname: Version mismatch error. This is $PACKAGE $VERSION, revision $package_revision, $progname: but the definition of this LT_INIT comes from revision $macro_revision. $progname: You should recreate aclocal.m4 with macros from revision $package_revision $progname: of $PACKAGE $VERSION and run autoconf again. _LT_EOF fi exit $EXIT_MISMATCH fi } # Shorthand for --mode=foo, only valid as the first argument case $1 in clean|clea|cle|cl) shift; set dummy --mode clean ${1+"$@"}; shift ;; compile|compil|compi|comp|com|co|c) shift; set dummy --mode compile ${1+"$@"}; shift ;; execute|execut|execu|exec|exe|ex|e) shift; set dummy --mode execute ${1+"$@"}; shift ;; finish|finis|fini|fin|fi|f) shift; set dummy --mode finish ${1+"$@"}; shift ;; install|instal|insta|inst|ins|in|i) shift; set dummy --mode install ${1+"$@"}; shift ;; link|lin|li|l) shift; set dummy --mode link ${1+"$@"}; shift ;; uninstall|uninstal|uninsta|uninst|unins|unin|uni|un|u) shift; set dummy --mode uninstall ${1+"$@"}; shift ;; esac # Option defaults: opt_debug=: opt_dry_run=false opt_config=false opt_preserve_dup_deps=false opt_features=false opt_finish=false opt_help=false opt_help_all=false opt_silent=: opt_warning=: opt_verbose=: opt_silent=false opt_verbose=false # Parse options once, thoroughly. This comes as soon as possible in the # script to make things like `--version' happen as quickly as we can. { # this just eases exit handling while test $# -gt 0; do opt="$1" shift case $opt in --debug|-x) opt_debug='set -x' func_echo "enabling shell trace mode" $opt_debug ;; --dry-run|--dryrun|-n) opt_dry_run=: ;; --config) opt_config=: func_config ;; --dlopen|-dlopen) optarg="$1" opt_dlopen="${opt_dlopen+$opt_dlopen }$optarg" shift ;; --preserve-dup-deps) opt_preserve_dup_deps=: ;; --features) opt_features=: func_features ;; --finish) opt_finish=: set dummy --mode finish ${1+"$@"}; shift ;; --help) opt_help=: ;; --help-all) opt_help_all=: opt_help=': help-all' ;; --mode) test $# = 0 && func_missing_arg $opt && break optarg="$1" opt_mode="$optarg" case $optarg in # Valid mode arguments: clean|compile|execute|finish|install|link|relink|uninstall) ;; # Catch anything else as an error *) func_error "invalid argument for $opt" exit_cmd=exit break ;; esac shift ;; --no-silent|--no-quiet) opt_silent=false func_append preserve_args " $opt" ;; --no-warning|--no-warn) opt_warning=false func_append preserve_args " $opt" ;; --no-verbose) opt_verbose=false func_append preserve_args " $opt" ;; --silent|--quiet) opt_silent=: func_append preserve_args " $opt" opt_verbose=false ;; --verbose|-v) opt_verbose=: func_append preserve_args " $opt" opt_silent=false ;; --tag) test $# = 0 && func_missing_arg $opt && break optarg="$1" opt_tag="$optarg" func_append preserve_args " $opt $optarg" func_enable_tag "$optarg" shift ;; -\?|-h) func_usage ;; --help) func_help ;; --version) func_version ;; # Separate optargs to long options: --*=*) func_split_long_opt "$opt" set dummy "$func_split_long_opt_name" "$func_split_long_opt_arg" ${1+"$@"} shift ;; # Separate non-argument short options: -\?*|-h*|-n*|-v*) func_split_short_opt "$opt" set dummy "$func_split_short_opt_name" "-$func_split_short_opt_arg" ${1+"$@"} shift ;; --) break ;; -*) func_fatal_help "unrecognized option \`$opt'" ;; *) set dummy "$opt" ${1+"$@"}; shift; break ;; esac done # Validate options: # save first non-option argument if test "$#" -gt 0; then nonopt="$opt" shift fi # preserve --debug test "$opt_debug" = : || func_append preserve_args " --debug" case $host in *cygwin* | *mingw* | *pw32* | *cegcc*) # don't eliminate duplications in $postdeps and $predeps opt_duplicate_compiler_generated_deps=: ;; *) opt_duplicate_compiler_generated_deps=$opt_preserve_dup_deps ;; esac $opt_help || { # Sanity checks first: func_check_version_match if test "$build_libtool_libs" != yes && test "$build_old_libs" != yes; then func_fatal_configuration "not configured to build any kind of library" fi # Darwin sucks eval std_shrext=\"$shrext_cmds\" # Only execute mode is allowed to have -dlopen flags. if test -n "$opt_dlopen" && test "$opt_mode" != execute; then func_error "unrecognized option \`-dlopen'" $ECHO "$help" 1>&2 exit $EXIT_FAILURE fi # Change the help message to a mode-specific one. generic_help="$help" help="Try \`$progname --help --mode=$opt_mode' for more information." } # Bail if the options were screwed $exit_cmd $EXIT_FAILURE } ## ----------- ## ## Main. ## ## ----------- ## # func_lalib_p file # True iff FILE is a libtool `.la' library or `.lo' object file. # This function is only a basic sanity check; it will hardly flush out # determined imposters. func_lalib_p () { test -f "$1" && $SED -e 4q "$1" 2>/dev/null \ | $GREP "^# Generated by .*$PACKAGE" > /dev/null 2>&1 } # func_lalib_unsafe_p file # True iff FILE is a libtool `.la' library or `.lo' object file. # This function implements the same check as func_lalib_p without # resorting to external programs. To this end, it redirects stdin and # closes it afterwards, without saving the original file descriptor. # As a safety measure, use it only where a negative result would be # fatal anyway. Works if `file' does not exist. func_lalib_unsafe_p () { lalib_p=no if test -f "$1" && test -r "$1" && exec 5<&0 <"$1"; then for lalib_p_l in 1 2 3 4 do read lalib_p_line case "$lalib_p_line" in \#\ Generated\ by\ *$PACKAGE* ) lalib_p=yes; break;; esac done exec 0<&5 5<&- fi test "$lalib_p" = yes } # func_ltwrapper_script_p file # True iff FILE is a libtool wrapper script # This function is only a basic sanity check; it will hardly flush out # determined imposters. func_ltwrapper_script_p () { func_lalib_p "$1" } # func_ltwrapper_executable_p file # True iff FILE is a libtool wrapper executable # This function is only a basic sanity check; it will hardly flush out # determined imposters. func_ltwrapper_executable_p () { func_ltwrapper_exec_suffix= case $1 in *.exe) ;; *) func_ltwrapper_exec_suffix=.exe ;; esac $GREP "$magic_exe" "$1$func_ltwrapper_exec_suffix" >/dev/null 2>&1 } # func_ltwrapper_scriptname file # Assumes file is an ltwrapper_executable # uses $file to determine the appropriate filename for a # temporary ltwrapper_script. func_ltwrapper_scriptname () { func_dirname_and_basename "$1" "" "." func_stripname '' '.exe' "$func_basename_result" func_ltwrapper_scriptname_result="$func_dirname_result/$objdir/${func_stripname_result}_ltshwrapper" } # func_ltwrapper_p file # True iff FILE is a libtool wrapper script or wrapper executable # This function is only a basic sanity check; it will hardly flush out # determined imposters. func_ltwrapper_p () { func_ltwrapper_script_p "$1" || func_ltwrapper_executable_p "$1" } # func_execute_cmds commands fail_cmd # Execute tilde-delimited COMMANDS. # If FAIL_CMD is given, eval that upon failure. # FAIL_CMD may read-access the current command in variable CMD! func_execute_cmds () { $opt_debug save_ifs=$IFS; IFS='~' for cmd in $1; do IFS=$save_ifs eval cmd=\"$cmd\" func_show_eval "$cmd" "${2-:}" done IFS=$save_ifs } # func_source file # Source FILE, adding directory component if necessary. # Note that it is not necessary on cygwin/mingw to append a dot to # FILE even if both FILE and FILE.exe exist: automatic-append-.exe # behavior happens only for exec(3), not for open(2)! Also, sourcing # `FILE.' does not work on cygwin managed mounts. func_source () { $opt_debug case $1 in */* | *\\*) . "$1" ;; *) . "./$1" ;; esac } # func_resolve_sysroot PATH # Replace a leading = in PATH with a sysroot. Store the result into # func_resolve_sysroot_result func_resolve_sysroot () { func_resolve_sysroot_result=$1 case $func_resolve_sysroot_result in =*) func_stripname '=' '' "$func_resolve_sysroot_result" func_resolve_sysroot_result=$lt_sysroot$func_stripname_result ;; esac } # func_replace_sysroot PATH # If PATH begins with the sysroot, replace it with = and # store the result into func_replace_sysroot_result. func_replace_sysroot () { case "$lt_sysroot:$1" in ?*:"$lt_sysroot"*) func_stripname "$lt_sysroot" '' "$1" func_replace_sysroot_result="=$func_stripname_result" ;; *) # Including no sysroot. func_replace_sysroot_result=$1 ;; esac } # func_infer_tag arg # Infer tagged configuration to use if any are available and # if one wasn't chosen via the "--tag" command line option. # Only attempt this if the compiler in the base compile # command doesn't match the default compiler. # arg is usually of the form 'gcc ...' func_infer_tag () { $opt_debug if test -n "$available_tags" && test -z "$tagname"; then CC_quoted= for arg in $CC; do func_append_quoted CC_quoted "$arg" done CC_expanded=`func_echo_all $CC` CC_quoted_expanded=`func_echo_all $CC_quoted` case $@ in # Blanks in the command may have been stripped by the calling shell, # but not from the CC environment variable when configure was run. " $CC "* | "$CC "* | " $CC_expanded "* | "$CC_expanded "* | \ " $CC_quoted"* | "$CC_quoted "* | " $CC_quoted_expanded "* | "$CC_quoted_expanded "*) ;; # Blanks at the start of $base_compile will cause this to fail # if we don't check for them as well. *) for z in $available_tags; do if $GREP "^# ### BEGIN LIBTOOL TAG CONFIG: $z$" < "$progpath" > /dev/null; then # Evaluate the configuration. eval "`${SED} -n -e '/^# ### BEGIN LIBTOOL TAG CONFIG: '$z'$/,/^# ### END LIBTOOL TAG CONFIG: '$z'$/p' < $progpath`" CC_quoted= for arg in $CC; do # Double-quote args containing other shell metacharacters. func_append_quoted CC_quoted "$arg" done CC_expanded=`func_echo_all $CC` CC_quoted_expanded=`func_echo_all $CC_quoted` case "$@ " in " $CC "* | "$CC "* | " $CC_expanded "* | "$CC_expanded "* | \ " $CC_quoted"* | "$CC_quoted "* | " $CC_quoted_expanded "* | "$CC_quoted_expanded "*) # The compiler in the base compile command matches # the one in the tagged configuration. # Assume this is the tagged configuration we want. tagname=$z break ;; esac fi done # If $tagname still isn't set, then no tagged configuration # was found and let the user know that the "--tag" command # line option must be used. if test -z "$tagname"; then func_echo "unable to infer tagged configuration" func_fatal_error "specify a tag with \`--tag'" # else # func_verbose "using $tagname tagged configuration" fi ;; esac fi } # func_write_libtool_object output_name pic_name nonpic_name # Create a libtool object file (analogous to a ".la" file), # but don't create it if we're doing a dry run. func_write_libtool_object () { write_libobj=${1} if test "$build_libtool_libs" = yes; then write_lobj=\'${2}\' else write_lobj=none fi if test "$build_old_libs" = yes; then write_oldobj=\'${3}\' else write_oldobj=none fi $opt_dry_run || { cat >${write_libobj}T </dev/null` if test "$?" -eq 0 && test -n "${func_convert_core_file_wine_to_w32_tmp}"; then func_convert_core_file_wine_to_w32_result=`$ECHO "$func_convert_core_file_wine_to_w32_tmp" | $SED -e "$lt_sed_naive_backslashify"` else func_convert_core_file_wine_to_w32_result= fi fi } # end: func_convert_core_file_wine_to_w32 # func_convert_core_path_wine_to_w32 ARG # Helper function used by path conversion functions when $build is *nix, and # $host is mingw, cygwin, or some other w32 environment. Relies on a correctly # configured wine environment available, with the winepath program in $build's # $PATH. Assumes ARG has no leading or trailing path separator characters. # # ARG is path to be converted from $build format to win32. # Result is available in $func_convert_core_path_wine_to_w32_result. # Unconvertible file (directory) names in ARG are skipped; if no directory names # are convertible, then the result may be empty. func_convert_core_path_wine_to_w32 () { $opt_debug # unfortunately, winepath doesn't convert paths, only file names func_convert_core_path_wine_to_w32_result="" if test -n "$1"; then oldIFS=$IFS IFS=: for func_convert_core_path_wine_to_w32_f in $1; do IFS=$oldIFS func_convert_core_file_wine_to_w32 "$func_convert_core_path_wine_to_w32_f" if test -n "$func_convert_core_file_wine_to_w32_result" ; then if test -z "$func_convert_core_path_wine_to_w32_result"; then func_convert_core_path_wine_to_w32_result="$func_convert_core_file_wine_to_w32_result" else func_append func_convert_core_path_wine_to_w32_result ";$func_convert_core_file_wine_to_w32_result" fi fi done IFS=$oldIFS fi } # end: func_convert_core_path_wine_to_w32 # func_cygpath ARGS... # Wrapper around calling the cygpath program via LT_CYGPATH. This is used when # when (1) $build is *nix and Cygwin is hosted via a wine environment; or (2) # $build is MSYS and $host is Cygwin, or (3) $build is Cygwin. In case (1) or # (2), returns the Cygwin file name or path in func_cygpath_result (input # file name or path is assumed to be in w32 format, as previously converted # from $build's *nix or MSYS format). In case (3), returns the w32 file name # or path in func_cygpath_result (input file name or path is assumed to be in # Cygwin format). Returns an empty string on error. # # ARGS are passed to cygpath, with the last one being the file name or path to # be converted. # # Specify the absolute *nix (or w32) name to cygpath in the LT_CYGPATH # environment variable; do not put it in $PATH. func_cygpath () { $opt_debug if test -n "$LT_CYGPATH" && test -f "$LT_CYGPATH"; then func_cygpath_result=`$LT_CYGPATH "$@" 2>/dev/null` if test "$?" -ne 0; then # on failure, ensure result is empty func_cygpath_result= fi else func_cygpath_result= func_error "LT_CYGPATH is empty or specifies non-existent file: \`$LT_CYGPATH'" fi } #end: func_cygpath # func_convert_core_msys_to_w32 ARG # Convert file name or path ARG from MSYS format to w32 format. Return # result in func_convert_core_msys_to_w32_result. func_convert_core_msys_to_w32 () { $opt_debug # awkward: cmd appends spaces to result func_convert_core_msys_to_w32_result=`( cmd //c echo "$1" ) 2>/dev/null | $SED -e 's/[ ]*$//' -e "$lt_sed_naive_backslashify"` } #end: func_convert_core_msys_to_w32 # func_convert_file_check ARG1 ARG2 # Verify that ARG1 (a file name in $build format) was converted to $host # format in ARG2. Otherwise, emit an error message, but continue (resetting # func_to_host_file_result to ARG1). func_convert_file_check () { $opt_debug if test -z "$2" && test -n "$1" ; then func_error "Could not determine host file name corresponding to" func_error " \`$1'" func_error "Continuing, but uninstalled executables may not work." # Fallback: func_to_host_file_result="$1" fi } # end func_convert_file_check # func_convert_path_check FROM_PATHSEP TO_PATHSEP FROM_PATH TO_PATH # Verify that FROM_PATH (a path in $build format) was converted to $host # format in TO_PATH. Otherwise, emit an error message, but continue, resetting # func_to_host_file_result to a simplistic fallback value (see below). func_convert_path_check () { $opt_debug if test -z "$4" && test -n "$3"; then func_error "Could not determine the host path corresponding to" func_error " \`$3'" func_error "Continuing, but uninstalled executables may not work." # Fallback. This is a deliberately simplistic "conversion" and # should not be "improved". See libtool.info. if test "x$1" != "x$2"; then lt_replace_pathsep_chars="s|$1|$2|g" func_to_host_path_result=`echo "$3" | $SED -e "$lt_replace_pathsep_chars"` else func_to_host_path_result="$3" fi fi } # end func_convert_path_check # func_convert_path_front_back_pathsep FRONTPAT BACKPAT REPL ORIG # Modifies func_to_host_path_result by prepending REPL if ORIG matches FRONTPAT # and appending REPL if ORIG matches BACKPAT. func_convert_path_front_back_pathsep () { $opt_debug case $4 in $1 ) func_to_host_path_result="$3$func_to_host_path_result" ;; esac case $4 in $2 ) func_append func_to_host_path_result "$3" ;; esac } # end func_convert_path_front_back_pathsep ################################################## # $build to $host FILE NAME CONVERSION FUNCTIONS # ################################################## # invoked via `$to_host_file_cmd ARG' # # In each case, ARG is the path to be converted from $build to $host format. # Result will be available in $func_to_host_file_result. # func_to_host_file ARG # Converts the file name ARG from $build format to $host format. Return result # in func_to_host_file_result. func_to_host_file () { $opt_debug $to_host_file_cmd "$1" } # end func_to_host_file # func_to_tool_file ARG LAZY # converts the file name ARG from $build format to toolchain format. Return # result in func_to_tool_file_result. If the conversion in use is listed # in (the comma separated) LAZY, no conversion takes place. func_to_tool_file () { $opt_debug case ,$2, in *,"$to_tool_file_cmd",*) func_to_tool_file_result=$1 ;; *) $to_tool_file_cmd "$1" func_to_tool_file_result=$func_to_host_file_result ;; esac } # end func_to_tool_file # func_convert_file_noop ARG # Copy ARG to func_to_host_file_result. func_convert_file_noop () { func_to_host_file_result="$1" } # end func_convert_file_noop # func_convert_file_msys_to_w32 ARG # Convert file name ARG from (mingw) MSYS to (mingw) w32 format; automatic # conversion to w32 is not available inside the cwrapper. Returns result in # func_to_host_file_result. func_convert_file_msys_to_w32 () { $opt_debug func_to_host_file_result="$1" if test -n "$1"; then func_convert_core_msys_to_w32 "$1" func_to_host_file_result="$func_convert_core_msys_to_w32_result" fi func_convert_file_check "$1" "$func_to_host_file_result" } # end func_convert_file_msys_to_w32 # func_convert_file_cygwin_to_w32 ARG # Convert file name ARG from Cygwin to w32 format. Returns result in # func_to_host_file_result. func_convert_file_cygwin_to_w32 () { $opt_debug func_to_host_file_result="$1" if test -n "$1"; then # because $build is cygwin, we call "the" cygpath in $PATH; no need to use # LT_CYGPATH in this case. func_to_host_file_result=`cygpath -m "$1"` fi func_convert_file_check "$1" "$func_to_host_file_result" } # end func_convert_file_cygwin_to_w32 # func_convert_file_nix_to_w32 ARG # Convert file name ARG from *nix to w32 format. Requires a wine environment # and a working winepath. Returns result in func_to_host_file_result. func_convert_file_nix_to_w32 () { $opt_debug func_to_host_file_result="$1" if test -n "$1"; then func_convert_core_file_wine_to_w32 "$1" func_to_host_file_result="$func_convert_core_file_wine_to_w32_result" fi func_convert_file_check "$1" "$func_to_host_file_result" } # end func_convert_file_nix_to_w32 # func_convert_file_msys_to_cygwin ARG # Convert file name ARG from MSYS to Cygwin format. Requires LT_CYGPATH set. # Returns result in func_to_host_file_result. func_convert_file_msys_to_cygwin () { $opt_debug func_to_host_file_result="$1" if test -n "$1"; then func_convert_core_msys_to_w32 "$1" func_cygpath -u "$func_convert_core_msys_to_w32_result" func_to_host_file_result="$func_cygpath_result" fi func_convert_file_check "$1" "$func_to_host_file_result" } # end func_convert_file_msys_to_cygwin # func_convert_file_nix_to_cygwin ARG # Convert file name ARG from *nix to Cygwin format. Requires Cygwin installed # in a wine environment, working winepath, and LT_CYGPATH set. Returns result # in func_to_host_file_result. func_convert_file_nix_to_cygwin () { $opt_debug func_to_host_file_result="$1" if test -n "$1"; then # convert from *nix to w32, then use cygpath to convert from w32 to cygwin. func_convert_core_file_wine_to_w32 "$1" func_cygpath -u "$func_convert_core_file_wine_to_w32_result" func_to_host_file_result="$func_cygpath_result" fi func_convert_file_check "$1" "$func_to_host_file_result" } # end func_convert_file_nix_to_cygwin ############################################# # $build to $host PATH CONVERSION FUNCTIONS # ############################################# # invoked via `$to_host_path_cmd ARG' # # In each case, ARG is the path to be converted from $build to $host format. # The result will be available in $func_to_host_path_result. # # Path separators are also converted from $build format to $host format. If # ARG begins or ends with a path separator character, it is preserved (but # converted to $host format) on output. # # All path conversion functions are named using the following convention: # file name conversion function : func_convert_file_X_to_Y () # path conversion function : func_convert_path_X_to_Y () # where, for any given $build/$host combination the 'X_to_Y' value is the # same. If conversion functions are added for new $build/$host combinations, # the two new functions must follow this pattern, or func_init_to_host_path_cmd # will break. # func_init_to_host_path_cmd # Ensures that function "pointer" variable $to_host_path_cmd is set to the # appropriate value, based on the value of $to_host_file_cmd. to_host_path_cmd= func_init_to_host_path_cmd () { $opt_debug if test -z "$to_host_path_cmd"; then func_stripname 'func_convert_file_' '' "$to_host_file_cmd" to_host_path_cmd="func_convert_path_${func_stripname_result}" fi } # func_to_host_path ARG # Converts the path ARG from $build format to $host format. Return result # in func_to_host_path_result. func_to_host_path () { $opt_debug func_init_to_host_path_cmd $to_host_path_cmd "$1" } # end func_to_host_path # func_convert_path_noop ARG # Copy ARG to func_to_host_path_result. func_convert_path_noop () { func_to_host_path_result="$1" } # end func_convert_path_noop # func_convert_path_msys_to_w32 ARG # Convert path ARG from (mingw) MSYS to (mingw) w32 format; automatic # conversion to w32 is not available inside the cwrapper. Returns result in # func_to_host_path_result. func_convert_path_msys_to_w32 () { $opt_debug func_to_host_path_result="$1" if test -n "$1"; then # Remove leading and trailing path separator characters from ARG. MSYS # behavior is inconsistent here; cygpath turns them into '.;' and ';.'; # and winepath ignores them completely. func_stripname : : "$1" func_to_host_path_tmp1=$func_stripname_result func_convert_core_msys_to_w32 "$func_to_host_path_tmp1" func_to_host_path_result="$func_convert_core_msys_to_w32_result" func_convert_path_check : ";" \ "$func_to_host_path_tmp1" "$func_to_host_path_result" func_convert_path_front_back_pathsep ":*" "*:" ";" "$1" fi } # end func_convert_path_msys_to_w32 # func_convert_path_cygwin_to_w32 ARG # Convert path ARG from Cygwin to w32 format. Returns result in # func_to_host_file_result. func_convert_path_cygwin_to_w32 () { $opt_debug func_to_host_path_result="$1" if test -n "$1"; then # See func_convert_path_msys_to_w32: func_stripname : : "$1" func_to_host_path_tmp1=$func_stripname_result func_to_host_path_result=`cygpath -m -p "$func_to_host_path_tmp1"` func_convert_path_check : ";" \ "$func_to_host_path_tmp1" "$func_to_host_path_result" func_convert_path_front_back_pathsep ":*" "*:" ";" "$1" fi } # end func_convert_path_cygwin_to_w32 # func_convert_path_nix_to_w32 ARG # Convert path ARG from *nix to w32 format. Requires a wine environment and # a working winepath. Returns result in func_to_host_file_result. func_convert_path_nix_to_w32 () { $opt_debug func_to_host_path_result="$1" if test -n "$1"; then # See func_convert_path_msys_to_w32: func_stripname : : "$1" func_to_host_path_tmp1=$func_stripname_result func_convert_core_path_wine_to_w32 "$func_to_host_path_tmp1" func_to_host_path_result="$func_convert_core_path_wine_to_w32_result" func_convert_path_check : ";" \ "$func_to_host_path_tmp1" "$func_to_host_path_result" func_convert_path_front_back_pathsep ":*" "*:" ";" "$1" fi } # end func_convert_path_nix_to_w32 # func_convert_path_msys_to_cygwin ARG # Convert path ARG from MSYS to Cygwin format. Requires LT_CYGPATH set. # Returns result in func_to_host_file_result. func_convert_path_msys_to_cygwin () { $opt_debug func_to_host_path_result="$1" if test -n "$1"; then # See func_convert_path_msys_to_w32: func_stripname : : "$1" func_to_host_path_tmp1=$func_stripname_result func_convert_core_msys_to_w32 "$func_to_host_path_tmp1" func_cygpath -u -p "$func_convert_core_msys_to_w32_result" func_to_host_path_result="$func_cygpath_result" func_convert_path_check : : \ "$func_to_host_path_tmp1" "$func_to_host_path_result" func_convert_path_front_back_pathsep ":*" "*:" : "$1" fi } # end func_convert_path_msys_to_cygwin # func_convert_path_nix_to_cygwin ARG # Convert path ARG from *nix to Cygwin format. Requires Cygwin installed in a # a wine environment, working winepath, and LT_CYGPATH set. Returns result in # func_to_host_file_result. func_convert_path_nix_to_cygwin () { $opt_debug func_to_host_path_result="$1" if test -n "$1"; then # Remove leading and trailing path separator characters from # ARG. msys behavior is inconsistent here, cygpath turns them # into '.;' and ';.', and winepath ignores them completely. func_stripname : : "$1" func_to_host_path_tmp1=$func_stripname_result func_convert_core_path_wine_to_w32 "$func_to_host_path_tmp1" func_cygpath -u -p "$func_convert_core_path_wine_to_w32_result" func_to_host_path_result="$func_cygpath_result" func_convert_path_check : : \ "$func_to_host_path_tmp1" "$func_to_host_path_result" func_convert_path_front_back_pathsep ":*" "*:" : "$1" fi } # end func_convert_path_nix_to_cygwin # func_mode_compile arg... func_mode_compile () { $opt_debug # Get the compilation command and the source file. base_compile= srcfile="$nonopt" # always keep a non-empty value in "srcfile" suppress_opt=yes suppress_output= arg_mode=normal libobj= later= pie_flag= for arg do case $arg_mode in arg ) # do not "continue". Instead, add this to base_compile lastarg="$arg" arg_mode=normal ;; target ) libobj="$arg" arg_mode=normal continue ;; normal ) # Accept any command-line options. case $arg in -o) test -n "$libobj" && \ func_fatal_error "you cannot specify \`-o' more than once" arg_mode=target continue ;; -pie | -fpie | -fPIE) func_append pie_flag " $arg" continue ;; -shared | -static | -prefer-pic | -prefer-non-pic) func_append later " $arg" continue ;; -no-suppress) suppress_opt=no continue ;; -Xcompiler) arg_mode=arg # the next one goes into the "base_compile" arg list continue # The current "srcfile" will either be retained or ;; # replaced later. I would guess that would be a bug. -Wc,*) func_stripname '-Wc,' '' "$arg" args=$func_stripname_result lastarg= save_ifs="$IFS"; IFS=',' for arg in $args; do IFS="$save_ifs" func_append_quoted lastarg "$arg" done IFS="$save_ifs" func_stripname ' ' '' "$lastarg" lastarg=$func_stripname_result # Add the arguments to base_compile. func_append base_compile " $lastarg" continue ;; *) # Accept the current argument as the source file. # The previous "srcfile" becomes the current argument. # lastarg="$srcfile" srcfile="$arg" ;; esac # case $arg ;; esac # case $arg_mode # Aesthetically quote the previous argument. func_append_quoted base_compile "$lastarg" done # for arg case $arg_mode in arg) func_fatal_error "you must specify an argument for -Xcompile" ;; target) func_fatal_error "you must specify a target with \`-o'" ;; *) # Get the name of the library object. test -z "$libobj" && { func_basename "$srcfile" libobj="$func_basename_result" } ;; esac # Recognize several different file suffixes. # If the user specifies -o file.o, it is replaced with file.lo case $libobj in *.[cCFSifmso] | \ *.ada | *.adb | *.ads | *.asm | \ *.c++ | *.cc | *.ii | *.class | *.cpp | *.cxx | \ *.[fF][09]? | *.for | *.java | *.go | *.obj | *.sx | *.cu | *.cup) func_xform "$libobj" libobj=$func_xform_result ;; esac case $libobj in *.lo) func_lo2o "$libobj"; obj=$func_lo2o_result ;; *) func_fatal_error "cannot determine name of library object from \`$libobj'" ;; esac func_infer_tag $base_compile for arg in $later; do case $arg in -shared) test "$build_libtool_libs" != yes && \ func_fatal_configuration "can not build a shared library" build_old_libs=no continue ;; -static) build_libtool_libs=no build_old_libs=yes continue ;; -prefer-pic) pic_mode=yes continue ;; -prefer-non-pic) pic_mode=no continue ;; esac done func_quote_for_eval "$libobj" test "X$libobj" != "X$func_quote_for_eval_result" \ && $ECHO "X$libobj" | $GREP '[]~#^*{};<>?"'"'"' &()|`$[]' \ && func_warning "libobj name \`$libobj' may not contain shell special characters." func_dirname_and_basename "$obj" "/" "" objname="$func_basename_result" xdir="$func_dirname_result" lobj=${xdir}$objdir/$objname test -z "$base_compile" && \ func_fatal_help "you must specify a compilation command" # Delete any leftover library objects. if test "$build_old_libs" = yes; then removelist="$obj $lobj $libobj ${libobj}T" else removelist="$lobj $libobj ${libobj}T" fi # On Cygwin there's no "real" PIC flag so we must build both object types case $host_os in cygwin* | mingw* | pw32* | os2* | cegcc*) pic_mode=default ;; esac if test "$pic_mode" = no && test "$deplibs_check_method" != pass_all; then # non-PIC code in shared libraries is not supported pic_mode=default fi # Calculate the filename of the output object if compiler does # not support -o with -c if test "$compiler_c_o" = no; then output_obj=`$ECHO "$srcfile" | $SED 's%^.*/%%; s%\.[^.]*$%%'`.${objext} lockfile="$output_obj.lock" else output_obj= need_locks=no lockfile= fi # Lock this critical section if it is needed # We use this script file to make the link, it avoids creating a new file if test "$need_locks" = yes; then until $opt_dry_run || ln "$progpath" "$lockfile" 2>/dev/null; do func_echo "Waiting for $lockfile to be removed" sleep 2 done elif test "$need_locks" = warn; then if test -f "$lockfile"; then $ECHO "\ *** ERROR, $lockfile exists and contains: `cat $lockfile 2>/dev/null` This indicates that another process is trying to use the same temporary object file, and libtool could not work around it because your compiler does not support \`-c' and \`-o' together. If you repeat this compilation, it may succeed, by chance, but you had better avoid parallel builds (make -j) in this platform, or get a better compiler." $opt_dry_run || $RM $removelist exit $EXIT_FAILURE fi func_append removelist " $output_obj" $ECHO "$srcfile" > "$lockfile" fi $opt_dry_run || $RM $removelist func_append removelist " $lockfile" trap '$opt_dry_run || $RM $removelist; exit $EXIT_FAILURE' 1 2 15 func_to_tool_file "$srcfile" func_convert_file_msys_to_w32 srcfile=$func_to_tool_file_result func_quote_for_eval "$srcfile" qsrcfile=$func_quote_for_eval_result # Only build a PIC object if we are building libtool libraries. if test "$build_libtool_libs" = yes; then # Without this assignment, base_compile gets emptied. fbsd_hideous_sh_bug=$base_compile if test "$pic_mode" != no; then command="$base_compile $qsrcfile $pic_flag" else # Don't build PIC code command="$base_compile $qsrcfile" fi func_mkdir_p "$xdir$objdir" if test -z "$output_obj"; then # Place PIC objects in $objdir func_append command " -o $lobj" fi func_show_eval_locale "$command" \ 'test -n "$output_obj" && $RM $removelist; exit $EXIT_FAILURE' if test "$need_locks" = warn && test "X`cat $lockfile 2>/dev/null`" != "X$srcfile"; then $ECHO "\ *** ERROR, $lockfile contains: `cat $lockfile 2>/dev/null` but it should contain: $srcfile This indicates that another process is trying to use the same temporary object file, and libtool could not work around it because your compiler does not support \`-c' and \`-o' together. If you repeat this compilation, it may succeed, by chance, but you had better avoid parallel builds (make -j) in this platform, or get a better compiler." $opt_dry_run || $RM $removelist exit $EXIT_FAILURE fi # Just move the object if needed, then go on to compile the next one if test -n "$output_obj" && test "X$output_obj" != "X$lobj"; then func_show_eval '$MV "$output_obj" "$lobj"' \ 'error=$?; $opt_dry_run || $RM $removelist; exit $error' fi # Allow error messages only from the first compilation. if test "$suppress_opt" = yes; then suppress_output=' >/dev/null 2>&1' fi fi # Only build a position-dependent object if we build old libraries. if test "$build_old_libs" = yes; then if test "$pic_mode" != yes; then # Don't build PIC code command="$base_compile $qsrcfile$pie_flag" else command="$base_compile $qsrcfile $pic_flag" fi if test "$compiler_c_o" = yes; then func_append command " -o $obj" fi # Suppress compiler output if we already did a PIC compilation. func_append command "$suppress_output" func_show_eval_locale "$command" \ '$opt_dry_run || $RM $removelist; exit $EXIT_FAILURE' if test "$need_locks" = warn && test "X`cat $lockfile 2>/dev/null`" != "X$srcfile"; then $ECHO "\ *** ERROR, $lockfile contains: `cat $lockfile 2>/dev/null` but it should contain: $srcfile This indicates that another process is trying to use the same temporary object file, and libtool could not work around it because your compiler does not support \`-c' and \`-o' together. If you repeat this compilation, it may succeed, by chance, but you had better avoid parallel builds (make -j) in this platform, or get a better compiler." $opt_dry_run || $RM $removelist exit $EXIT_FAILURE fi # Just move the object if needed if test -n "$output_obj" && test "X$output_obj" != "X$obj"; then func_show_eval '$MV "$output_obj" "$obj"' \ 'error=$?; $opt_dry_run || $RM $removelist; exit $error' fi fi $opt_dry_run || { func_write_libtool_object "$libobj" "$objdir/$objname" "$objname" # Unlock the critical section if it was locked if test "$need_locks" != no; then removelist=$lockfile $RM "$lockfile" fi } exit $EXIT_SUCCESS } $opt_help || { test "$opt_mode" = compile && func_mode_compile ${1+"$@"} } func_mode_help () { # We need to display help for each of the modes. case $opt_mode in "") # Generic help is extracted from the usage comments # at the start of this file. func_help ;; clean) $ECHO \ "Usage: $progname [OPTION]... --mode=clean RM [RM-OPTION]... FILE... Remove files from the build directory. RM is the name of the program to use to delete files associated with each FILE (typically \`/bin/rm'). RM-OPTIONS are options (such as \`-f') to be passed to RM. If FILE is a libtool library, object or program, all the files associated with it are deleted. Otherwise, only FILE itself is deleted using RM." ;; compile) $ECHO \ "Usage: $progname [OPTION]... --mode=compile COMPILE-COMMAND... SOURCEFILE Compile a source file into a libtool library object. This mode accepts the following additional options: -o OUTPUT-FILE set the output file name to OUTPUT-FILE -no-suppress do not suppress compiler output for multiple passes -prefer-pic try to build PIC objects only -prefer-non-pic try to build non-PIC objects only -shared do not build a \`.o' file suitable for static linking -static only build a \`.o' file suitable for static linking -Wc,FLAG pass FLAG directly to the compiler COMPILE-COMMAND is a command to be used in creating a \`standard' object file from the given SOURCEFILE. The output file name is determined by removing the directory component from SOURCEFILE, then substituting the C source code suffix \`.c' with the library object suffix, \`.lo'." ;; execute) $ECHO \ "Usage: $progname [OPTION]... --mode=execute COMMAND [ARGS]... Automatically set library path, then run a program. This mode accepts the following additional options: -dlopen FILE add the directory containing FILE to the library path This mode sets the library path environment variable according to \`-dlopen' flags. If any of the ARGS are libtool executable wrappers, then they are translated into their corresponding uninstalled binary, and any of their required library directories are added to the library path. Then, COMMAND is executed, with ARGS as arguments." ;; finish) $ECHO \ "Usage: $progname [OPTION]... --mode=finish [LIBDIR]... Complete the installation of libtool libraries. Each LIBDIR is a directory that contains libtool libraries. The commands that this mode executes may require superuser privileges. Use the \`--dry-run' option if you just want to see what would be executed." ;; install) $ECHO \ "Usage: $progname [OPTION]... --mode=install INSTALL-COMMAND... Install executables or libraries. INSTALL-COMMAND is the installation command. The first component should be either the \`install' or \`cp' program. The following components of INSTALL-COMMAND are treated specially: -inst-prefix-dir PREFIX-DIR Use PREFIX-DIR as a staging area for installation The rest of the components are interpreted as arguments to that command (only BSD-compatible install options are recognized)." ;; link) $ECHO \ "Usage: $progname [OPTION]... --mode=link LINK-COMMAND... Link object files or libraries together to form another library, or to create an executable program. LINK-COMMAND is a command using the C compiler that you would use to create a program from several object files. The following components of LINK-COMMAND are treated specially: -all-static do not do any dynamic linking at all -avoid-version do not add a version suffix if possible -bindir BINDIR specify path to binaries directory (for systems where libraries must be found in the PATH setting at runtime) -dlopen FILE \`-dlpreopen' FILE if it cannot be dlopened at runtime -dlpreopen FILE link in FILE and add its symbols to lt_preloaded_symbols -export-dynamic allow symbols from OUTPUT-FILE to be resolved with dlsym(3) -export-symbols SYMFILE try to export only the symbols listed in SYMFILE -export-symbols-regex REGEX try to export only the symbols matching REGEX -LLIBDIR search LIBDIR for required installed libraries -lNAME OUTPUT-FILE requires the installed library libNAME -module build a library that can dlopened -no-fast-install disable the fast-install mode -no-install link a not-installable executable -no-undefined declare that a library does not refer to external symbols -o OUTPUT-FILE create OUTPUT-FILE from the specified objects -objectlist FILE Use a list of object files found in FILE to specify objects -precious-files-regex REGEX don't remove output files matching REGEX -release RELEASE specify package release information -rpath LIBDIR the created library will eventually be installed in LIBDIR -R[ ]LIBDIR add LIBDIR to the runtime path of programs and libraries -shared only do dynamic linking of libtool libraries -shrext SUFFIX override the standard shared library file extension -static do not do any dynamic linking of uninstalled libtool libraries -static-libtool-libs do not do any dynamic linking of libtool libraries -version-info CURRENT[:REVISION[:AGE]] specify library version info [each variable defaults to 0] -weak LIBNAME declare that the target provides the LIBNAME interface -Wc,FLAG -Xcompiler FLAG pass linker-specific FLAG directly to the compiler -Wl,FLAG -Xlinker FLAG pass linker-specific FLAG directly to the linker -XCClinker FLAG pass link-specific FLAG to the compiler driver (CC) All other options (arguments beginning with \`-') are ignored. Every other argument is treated as a filename. Files ending in \`.la' are treated as uninstalled libtool libraries, other files are standard or library object files. If the OUTPUT-FILE ends in \`.la', then a libtool library is created, only library objects (\`.lo' files) may be specified, and \`-rpath' is required, except when creating a convenience library. If OUTPUT-FILE ends in \`.a' or \`.lib', then a standard library is created using \`ar' and \`ranlib', or on Windows using \`lib'. If OUTPUT-FILE ends in \`.lo' or \`.${objext}', then a reloadable object file is created, otherwise an executable program is created." ;; uninstall) $ECHO \ "Usage: $progname [OPTION]... --mode=uninstall RM [RM-OPTION]... FILE... Remove libraries from an installation directory. RM is the name of the program to use to delete files associated with each FILE (typically \`/bin/rm'). RM-OPTIONS are options (such as \`-f') to be passed to RM. If FILE is a libtool library, all the files associated with it are deleted. Otherwise, only FILE itself is deleted using RM." ;; *) func_fatal_help "invalid operation mode \`$opt_mode'" ;; esac echo $ECHO "Try \`$progname --help' for more information about other modes." } # Now that we've collected a possible --mode arg, show help if necessary if $opt_help; then if test "$opt_help" = :; then func_mode_help else { func_help noexit for opt_mode in compile link execute install finish uninstall clean; do func_mode_help done } | sed -n '1p; 2,$s/^Usage:/ or: /p' { func_help noexit for opt_mode in compile link execute install finish uninstall clean; do echo func_mode_help done } | sed '1d /^When reporting/,/^Report/{ H d } $x /information about other modes/d /more detailed .*MODE/d s/^Usage:.*--mode=\([^ ]*\) .*/Description of \1 mode:/' fi exit $? fi # func_mode_execute arg... func_mode_execute () { $opt_debug # The first argument is the command name. cmd="$nonopt" test -z "$cmd" && \ func_fatal_help "you must specify a COMMAND" # Handle -dlopen flags immediately. for file in $opt_dlopen; do test -f "$file" \ || func_fatal_help "\`$file' is not a file" dir= case $file in *.la) func_resolve_sysroot "$file" file=$func_resolve_sysroot_result # Check to see that this really is a libtool archive. func_lalib_unsafe_p "$file" \ || func_fatal_help "\`$lib' is not a valid libtool archive" # Read the libtool library. dlname= library_names= func_source "$file" # Skip this library if it cannot be dlopened. if test -z "$dlname"; then # Warn if it was a shared library. test -n "$library_names" && \ func_warning "\`$file' was not linked with \`-export-dynamic'" continue fi func_dirname "$file" "" "." dir="$func_dirname_result" if test -f "$dir/$objdir/$dlname"; then func_append dir "/$objdir" else if test ! -f "$dir/$dlname"; then func_fatal_error "cannot find \`$dlname' in \`$dir' or \`$dir/$objdir'" fi fi ;; *.lo) # Just add the directory containing the .lo file. func_dirname "$file" "" "." dir="$func_dirname_result" ;; *) func_warning "\`-dlopen' is ignored for non-libtool libraries and objects" continue ;; esac # Get the absolute pathname. absdir=`cd "$dir" && pwd` test -n "$absdir" && dir="$absdir" # Now add the directory to shlibpath_var. if eval "test -z \"\$$shlibpath_var\""; then eval "$shlibpath_var=\"\$dir\"" else eval "$shlibpath_var=\"\$dir:\$$shlibpath_var\"" fi done # This variable tells wrapper scripts just to set shlibpath_var # rather than running their programs. libtool_execute_magic="$magic" # Check if any of the arguments is a wrapper script. args= for file do case $file in -* | *.la | *.lo ) ;; *) # Do a test to see if this is really a libtool program. if func_ltwrapper_script_p "$file"; then func_source "$file" # Transform arg to wrapped name. file="$progdir/$program" elif func_ltwrapper_executable_p "$file"; then func_ltwrapper_scriptname "$file" func_source "$func_ltwrapper_scriptname_result" # Transform arg to wrapped name. file="$progdir/$program" fi ;; esac # Quote arguments (to preserve shell metacharacters). func_append_quoted args "$file" done if test "X$opt_dry_run" = Xfalse; then if test -n "$shlibpath_var"; then # Export the shlibpath_var. eval "export $shlibpath_var" fi # Restore saved environment variables for lt_var in LANG LANGUAGE LC_ALL LC_CTYPE LC_COLLATE LC_MESSAGES do eval "if test \"\${save_$lt_var+set}\" = set; then $lt_var=\$save_$lt_var; export $lt_var else $lt_unset $lt_var fi" done # Now prepare to actually exec the command. exec_cmd="\$cmd$args" else # Display what would be done. if test -n "$shlibpath_var"; then eval "\$ECHO \"\$shlibpath_var=\$$shlibpath_var\"" echo "export $shlibpath_var" fi $ECHO "$cmd$args" exit $EXIT_SUCCESS fi } test "$opt_mode" = execute && func_mode_execute ${1+"$@"} # func_mode_finish arg... func_mode_finish () { $opt_debug libs= libdirs= admincmds= for opt in "$nonopt" ${1+"$@"} do if test -d "$opt"; then func_append libdirs " $opt" elif test -f "$opt"; then if func_lalib_unsafe_p "$opt"; then func_append libs " $opt" else func_warning "\`$opt' is not a valid libtool archive" fi else func_fatal_error "invalid argument \`$opt'" fi done if test -n "$libs"; then if test -n "$lt_sysroot"; then sysroot_regex=`$ECHO "$lt_sysroot" | $SED "$sed_make_literal_regex"` sysroot_cmd="s/\([ ']\)$sysroot_regex/\1/g;" else sysroot_cmd= fi # Remove sysroot references if $opt_dry_run; then for lib in $libs; do echo "removing references to $lt_sysroot and \`=' prefixes from $lib" done else tmpdir=`func_mktempdir` for lib in $libs; do sed -e "${sysroot_cmd} s/\([ ']-[LR]\)=/\1/g; s/\([ ']\)=/\1/g" $lib \ > $tmpdir/tmp-la mv -f $tmpdir/tmp-la $lib done ${RM}r "$tmpdir" fi fi if test -n "$finish_cmds$finish_eval" && test -n "$libdirs"; then for libdir in $libdirs; do if test -n "$finish_cmds"; then # Do each command in the finish commands. func_execute_cmds "$finish_cmds" 'admincmds="$admincmds '"$cmd"'"' fi if test -n "$finish_eval"; then # Do the single finish_eval. eval cmds=\"$finish_eval\" $opt_dry_run || eval "$cmds" || func_append admincmds " $cmds" fi done fi # Exit here if they wanted silent mode. $opt_silent && exit $EXIT_SUCCESS if test -n "$finish_cmds$finish_eval" && test -n "$libdirs"; then echo "----------------------------------------------------------------------" echo "Libraries have been installed in:" for libdir in $libdirs; do $ECHO " $libdir" done echo echo "If you ever happen to want to link against installed libraries" echo "in a given directory, LIBDIR, you must either use libtool, and" echo "specify the full pathname of the library, or use the \`-LLIBDIR'" echo "flag during linking and do at least one of the following:" if test -n "$shlibpath_var"; then echo " - add LIBDIR to the \`$shlibpath_var' environment variable" echo " during execution" fi if test -n "$runpath_var"; then echo " - add LIBDIR to the \`$runpath_var' environment variable" echo " during linking" fi if test -n "$hardcode_libdir_flag_spec"; then libdir=LIBDIR eval flag=\"$hardcode_libdir_flag_spec\" $ECHO " - use the \`$flag' linker flag" fi if test -n "$admincmds"; then $ECHO " - have your system administrator run these commands:$admincmds" fi if test -f /etc/ld.so.conf; then echo " - have your system administrator add LIBDIR to \`/etc/ld.so.conf'" fi echo echo "See any operating system documentation about shared libraries for" case $host in solaris2.[6789]|solaris2.1[0-9]) echo "more information, such as the ld(1), crle(1) and ld.so(8) manual" echo "pages." ;; *) echo "more information, such as the ld(1) and ld.so(8) manual pages." ;; esac echo "----------------------------------------------------------------------" fi exit $EXIT_SUCCESS } test "$opt_mode" = finish && func_mode_finish ${1+"$@"} # func_mode_install arg... func_mode_install () { $opt_debug # There may be an optional sh(1) argument at the beginning of # install_prog (especially on Windows NT). if test "$nonopt" = "$SHELL" || test "$nonopt" = /bin/sh || # Allow the use of GNU shtool's install command. case $nonopt in *shtool*) :;; *) false;; esac; then # Aesthetically quote it. func_quote_for_eval "$nonopt" install_prog="$func_quote_for_eval_result " arg=$1 shift else install_prog= arg=$nonopt fi # The real first argument should be the name of the installation program. # Aesthetically quote it. func_quote_for_eval "$arg" func_append install_prog "$func_quote_for_eval_result" install_shared_prog=$install_prog case " $install_prog " in *[\\\ /]cp\ *) install_cp=: ;; *) install_cp=false ;; esac # We need to accept at least all the BSD install flags. dest= files= opts= prev= install_type= isdir=no stripme= no_mode=: for arg do arg2= if test -n "$dest"; then func_append files " $dest" dest=$arg continue fi case $arg in -d) isdir=yes ;; -f) if $install_cp; then :; else prev=$arg fi ;; -g | -m | -o) prev=$arg ;; -s) stripme=" -s" continue ;; -*) ;; *) # If the previous option needed an argument, then skip it. if test -n "$prev"; then if test "x$prev" = x-m && test -n "$install_override_mode"; then arg2=$install_override_mode no_mode=false fi prev= else dest=$arg continue fi ;; esac # Aesthetically quote the argument. func_quote_for_eval "$arg" func_append install_prog " $func_quote_for_eval_result" if test -n "$arg2"; then func_quote_for_eval "$arg2" fi func_append install_shared_prog " $func_quote_for_eval_result" done test -z "$install_prog" && \ func_fatal_help "you must specify an install program" test -n "$prev" && \ func_fatal_help "the \`$prev' option requires an argument" if test -n "$install_override_mode" && $no_mode; then if $install_cp; then :; else func_quote_for_eval "$install_override_mode" func_append install_shared_prog " -m $func_quote_for_eval_result" fi fi if test -z "$files"; then if test -z "$dest"; then func_fatal_help "no file or destination specified" else func_fatal_help "you must specify a destination" fi fi # Strip any trailing slash from the destination. func_stripname '' '/' "$dest" dest=$func_stripname_result # Check to see that the destination is a directory. test -d "$dest" && isdir=yes if test "$isdir" = yes; then destdir="$dest" destname= else func_dirname_and_basename "$dest" "" "." destdir="$func_dirname_result" destname="$func_basename_result" # Not a directory, so check to see that there is only one file specified. set dummy $files; shift test "$#" -gt 1 && \ func_fatal_help "\`$dest' is not a directory" fi case $destdir in [\\/]* | [A-Za-z]:[\\/]*) ;; *) for file in $files; do case $file in *.lo) ;; *) func_fatal_help "\`$destdir' must be an absolute directory name" ;; esac done ;; esac # This variable tells wrapper scripts just to set variables rather # than running their programs. libtool_install_magic="$magic" staticlibs= future_libdirs= current_libdirs= for file in $files; do # Do each installation. case $file in *.$libext) # Do the static libraries later. func_append staticlibs " $file" ;; *.la) func_resolve_sysroot "$file" file=$func_resolve_sysroot_result # Check to see that this really is a libtool archive. func_lalib_unsafe_p "$file" \ || func_fatal_help "\`$file' is not a valid libtool archive" library_names= old_library= relink_command= func_source "$file" # Add the libdir to current_libdirs if it is the destination. if test "X$destdir" = "X$libdir"; then case "$current_libdirs " in *" $libdir "*) ;; *) func_append current_libdirs " $libdir" ;; esac else # Note the libdir as a future libdir. case "$future_libdirs " in *" $libdir "*) ;; *) func_append future_libdirs " $libdir" ;; esac fi func_dirname "$file" "/" "" dir="$func_dirname_result" func_append dir "$objdir" if test -n "$relink_command"; then # Determine the prefix the user has applied to our future dir. inst_prefix_dir=`$ECHO "$destdir" | $SED -e "s%$libdir\$%%"` # Don't allow the user to place us outside of our expected # location b/c this prevents finding dependent libraries that # are installed to the same prefix. # At present, this check doesn't affect windows .dll's that # are installed into $libdir/../bin (currently, that works fine) # but it's something to keep an eye on. test "$inst_prefix_dir" = "$destdir" && \ func_fatal_error "error: cannot install \`$file' to a directory not ending in $libdir" if test -n "$inst_prefix_dir"; then # Stick the inst_prefix_dir data into the link command. relink_command=`$ECHO "$relink_command" | $SED "s%@inst_prefix_dir@%-inst-prefix-dir $inst_prefix_dir%"` else relink_command=`$ECHO "$relink_command" | $SED "s%@inst_prefix_dir@%%"` fi func_warning "relinking \`$file'" func_show_eval "$relink_command" \ 'func_fatal_error "error: relink \`$file'\'' with the above command before installing it"' fi # See the names of the shared library. set dummy $library_names; shift if test -n "$1"; then realname="$1" shift srcname="$realname" test -n "$relink_command" && srcname="$realname"T # Install the shared library and build the symlinks. func_show_eval "$install_shared_prog $dir/$srcname $destdir/$realname" \ 'exit $?' tstripme="$stripme" case $host_os in cygwin* | mingw* | pw32* | cegcc*) case $realname in *.dll.a) tstripme="" ;; esac ;; esac if test -n "$tstripme" && test -n "$striplib"; then func_show_eval "$striplib $destdir/$realname" 'exit $?' fi if test "$#" -gt 0; then # Delete the old symlinks, and create new ones. # Try `ln -sf' first, because the `ln' binary might depend on # the symlink we replace! Solaris /bin/ln does not understand -f, # so we also need to try rm && ln -s. for linkname do test "$linkname" != "$realname" \ && func_show_eval "(cd $destdir && { $LN_S -f $realname $linkname || { $RM $linkname && $LN_S $realname $linkname; }; })" done fi # Do each command in the postinstall commands. lib="$destdir/$realname" func_execute_cmds "$postinstall_cmds" 'exit $?' fi # Install the pseudo-library for information purposes. func_basename "$file" name="$func_basename_result" instname="$dir/$name"i func_show_eval "$install_prog $instname $destdir/$name" 'exit $?' # Maybe install the static library, too. test -n "$old_library" && func_append staticlibs " $dir/$old_library" ;; *.lo) # Install (i.e. copy) a libtool object. # Figure out destination file name, if it wasn't already specified. if test -n "$destname"; then destfile="$destdir/$destname" else func_basename "$file" destfile="$func_basename_result" destfile="$destdir/$destfile" fi # Deduce the name of the destination old-style object file. case $destfile in *.lo) func_lo2o "$destfile" staticdest=$func_lo2o_result ;; *.$objext) staticdest="$destfile" destfile= ;; *) func_fatal_help "cannot copy a libtool object to \`$destfile'" ;; esac # Install the libtool object if requested. test -n "$destfile" && \ func_show_eval "$install_prog $file $destfile" 'exit $?' # Install the old object if enabled. if test "$build_old_libs" = yes; then # Deduce the name of the old-style object file. func_lo2o "$file" staticobj=$func_lo2o_result func_show_eval "$install_prog \$staticobj \$staticdest" 'exit $?' fi exit $EXIT_SUCCESS ;; *) # Figure out destination file name, if it wasn't already specified. if test -n "$destname"; then destfile="$destdir/$destname" else func_basename "$file" destfile="$func_basename_result" destfile="$destdir/$destfile" fi # If the file is missing, and there is a .exe on the end, strip it # because it is most likely a libtool script we actually want to # install stripped_ext="" case $file in *.exe) if test ! -f "$file"; then func_stripname '' '.exe' "$file" file=$func_stripname_result stripped_ext=".exe" fi ;; esac # Do a test to see if this is really a libtool program. case $host in *cygwin* | *mingw*) if func_ltwrapper_executable_p "$file"; then func_ltwrapper_scriptname "$file" wrapper=$func_ltwrapper_scriptname_result else func_stripname '' '.exe' "$file" wrapper=$func_stripname_result fi ;; *) wrapper=$file ;; esac if func_ltwrapper_script_p "$wrapper"; then notinst_deplibs= relink_command= func_source "$wrapper" # Check the variables that should have been set. test -z "$generated_by_libtool_version" && \ func_fatal_error "invalid libtool wrapper script \`$wrapper'" finalize=yes for lib in $notinst_deplibs; do # Check to see that each library is installed. libdir= if test -f "$lib"; then func_source "$lib" fi libfile="$libdir/"`$ECHO "$lib" | $SED 's%^.*/%%g'` ### testsuite: skip nested quoting test if test -n "$libdir" && test ! -f "$libfile"; then func_warning "\`$lib' has not been installed in \`$libdir'" finalize=no fi done relink_command= func_source "$wrapper" outputname= if test "$fast_install" = no && test -n "$relink_command"; then $opt_dry_run || { if test "$finalize" = yes; then tmpdir=`func_mktempdir` func_basename "$file$stripped_ext" file="$func_basename_result" outputname="$tmpdir/$file" # Replace the output file specification. relink_command=`$ECHO "$relink_command" | $SED 's%@OUTPUT@%'"$outputname"'%g'` $opt_silent || { func_quote_for_expand "$relink_command" eval "func_echo $func_quote_for_expand_result" } if eval "$relink_command"; then : else func_error "error: relink \`$file' with the above command before installing it" $opt_dry_run || ${RM}r "$tmpdir" continue fi file="$outputname" else func_warning "cannot relink \`$file'" fi } else # Install the binary that we compiled earlier. file=`$ECHO "$file$stripped_ext" | $SED "s%\([^/]*\)$%$objdir/\1%"` fi fi # remove .exe since cygwin /usr/bin/install will append another # one anyway case $install_prog,$host in */usr/bin/install*,*cygwin*) case $file:$destfile in *.exe:*.exe) # this is ok ;; *.exe:*) destfile=$destfile.exe ;; *:*.exe) func_stripname '' '.exe' "$destfile" destfile=$func_stripname_result ;; esac ;; esac func_show_eval "$install_prog\$stripme \$file \$destfile" 'exit $?' $opt_dry_run || if test -n "$outputname"; then ${RM}r "$tmpdir" fi ;; esac done for file in $staticlibs; do func_basename "$file" name="$func_basename_result" # Set up the ranlib parameters. oldlib="$destdir/$name" func_to_tool_file "$oldlib" func_convert_file_msys_to_w32 tool_oldlib=$func_to_tool_file_result func_show_eval "$install_prog \$file \$oldlib" 'exit $?' if test -n "$stripme" && test -n "$old_striplib"; then func_show_eval "$old_striplib $tool_oldlib" 'exit $?' fi # Do each command in the postinstall commands. func_execute_cmds "$old_postinstall_cmds" 'exit $?' done test -n "$future_libdirs" && \ func_warning "remember to run \`$progname --finish$future_libdirs'" if test -n "$current_libdirs"; then # Maybe just do a dry run. $opt_dry_run && current_libdirs=" -n$current_libdirs" exec_cmd='$SHELL $progpath $preserve_args --finish$current_libdirs' else exit $EXIT_SUCCESS fi } test "$opt_mode" = install && func_mode_install ${1+"$@"} # func_generate_dlsyms outputname originator pic_p # Extract symbols from dlprefiles and create ${outputname}S.o with # a dlpreopen symbol table. func_generate_dlsyms () { $opt_debug my_outputname="$1" my_originator="$2" my_pic_p="${3-no}" my_prefix=`$ECHO "$my_originator" | sed 's%[^a-zA-Z0-9]%_%g'` my_dlsyms= if test -n "$dlfiles$dlprefiles" || test "$dlself" != no; then if test -n "$NM" && test -n "$global_symbol_pipe"; then my_dlsyms="${my_outputname}S.c" else func_error "not configured to extract global symbols from dlpreopened files" fi fi if test -n "$my_dlsyms"; then case $my_dlsyms in "") ;; *.c) # Discover the nlist of each of the dlfiles. nlist="$output_objdir/${my_outputname}.nm" func_show_eval "$RM $nlist ${nlist}S ${nlist}T" # Parse the name list into a source file. func_verbose "creating $output_objdir/$my_dlsyms" $opt_dry_run || $ECHO > "$output_objdir/$my_dlsyms" "\ /* $my_dlsyms - symbol resolution table for \`$my_outputname' dlsym emulation. */ /* Generated by $PROGRAM (GNU $PACKAGE$TIMESTAMP) $VERSION */ #ifdef __cplusplus extern \"C\" { #endif #if defined(__GNUC__) && (((__GNUC__ == 4) && (__GNUC_MINOR__ >= 4)) || (__GNUC__ > 4)) #pragma GCC diagnostic ignored \"-Wstrict-prototypes\" #endif /* Keep this code in sync between libtool.m4, ltmain, lt_system.h, and tests. */ #if defined(_WIN32) || defined(__CYGWIN__) || defined(_WIN32_WCE) /* DATA imports from DLLs on WIN32 con't be const, because runtime relocations are performed -- see ld's documentation on pseudo-relocs. */ # define LT_DLSYM_CONST #elif defined(__osf__) /* This system does not cope well with relocations in const data. */ # define LT_DLSYM_CONST #else # define LT_DLSYM_CONST const #endif /* External symbol declarations for the compiler. */\ " if test "$dlself" = yes; then func_verbose "generating symbol list for \`$output'" $opt_dry_run || echo ': @PROGRAM@ ' > "$nlist" # Add our own program objects to the symbol list. progfiles=`$ECHO "$objs$old_deplibs" | $SP2NL | $SED "$lo2o" | $NL2SP` for progfile in $progfiles; do func_to_tool_file "$progfile" func_convert_file_msys_to_w32 func_verbose "extracting global C symbols from \`$func_to_tool_file_result'" $opt_dry_run || eval "$NM $func_to_tool_file_result | $global_symbol_pipe >> '$nlist'" done if test -n "$exclude_expsyms"; then $opt_dry_run || { eval '$EGREP -v " ($exclude_expsyms)$" "$nlist" > "$nlist"T' eval '$MV "$nlist"T "$nlist"' } fi if test -n "$export_symbols_regex"; then $opt_dry_run || { eval '$EGREP -e "$export_symbols_regex" "$nlist" > "$nlist"T' eval '$MV "$nlist"T "$nlist"' } fi # Prepare the list of exported symbols if test -z "$export_symbols"; then export_symbols="$output_objdir/$outputname.exp" $opt_dry_run || { $RM $export_symbols eval "${SED} -n -e '/^: @PROGRAM@ $/d' -e 's/^.* \(.*\)$/\1/p' "'< "$nlist" > "$export_symbols"' case $host in *cygwin* | *mingw* | *cegcc* ) eval "echo EXPORTS "'> "$output_objdir/$outputname.def"' eval 'cat "$export_symbols" >> "$output_objdir/$outputname.def"' ;; esac } else $opt_dry_run || { eval "${SED} -e 's/\([].[*^$]\)/\\\\\1/g' -e 's/^/ /' -e 's/$/$/'"' < "$export_symbols" > "$output_objdir/$outputname.exp"' eval '$GREP -f "$output_objdir/$outputname.exp" < "$nlist" > "$nlist"T' eval '$MV "$nlist"T "$nlist"' case $host in *cygwin* | *mingw* | *cegcc* ) eval "echo EXPORTS "'> "$output_objdir/$outputname.def"' eval 'cat "$nlist" >> "$output_objdir/$outputname.def"' ;; esac } fi fi for dlprefile in $dlprefiles; do func_verbose "extracting global C symbols from \`$dlprefile'" func_basename "$dlprefile" name="$func_basename_result" case $host in *cygwin* | *mingw* | *cegcc* ) # if an import library, we need to obtain dlname if func_win32_import_lib_p "$dlprefile"; then func_tr_sh "$dlprefile" eval "curr_lafile=\$libfile_$func_tr_sh_result" dlprefile_dlbasename="" if test -n "$curr_lafile" && func_lalib_p "$curr_lafile"; then # Use subshell, to avoid clobbering current variable values dlprefile_dlname=`source "$curr_lafile" && echo "$dlname"` if test -n "$dlprefile_dlname" ; then func_basename "$dlprefile_dlname" dlprefile_dlbasename="$func_basename_result" else # no lafile. user explicitly requested -dlpreopen . $sharedlib_from_linklib_cmd "$dlprefile" dlprefile_dlbasename=$sharedlib_from_linklib_result fi fi $opt_dry_run || { if test -n "$dlprefile_dlbasename" ; then eval '$ECHO ": $dlprefile_dlbasename" >> "$nlist"' else func_warning "Could not compute DLL name from $name" eval '$ECHO ": $name " >> "$nlist"' fi func_to_tool_file "$dlprefile" func_convert_file_msys_to_w32 eval "$NM \"$func_to_tool_file_result\" 2>/dev/null | $global_symbol_pipe | $SED -e '/I __imp/d' -e 's/I __nm_/D /;s/_nm__//' >> '$nlist'" } else # not an import lib $opt_dry_run || { eval '$ECHO ": $name " >> "$nlist"' func_to_tool_file "$dlprefile" func_convert_file_msys_to_w32 eval "$NM \"$func_to_tool_file_result\" 2>/dev/null | $global_symbol_pipe >> '$nlist'" } fi ;; *) $opt_dry_run || { eval '$ECHO ": $name " >> "$nlist"' func_to_tool_file "$dlprefile" func_convert_file_msys_to_w32 eval "$NM \"$func_to_tool_file_result\" 2>/dev/null | $global_symbol_pipe >> '$nlist'" } ;; esac done $opt_dry_run || { # Make sure we have at least an empty file. test -f "$nlist" || : > "$nlist" if test -n "$exclude_expsyms"; then $EGREP -v " ($exclude_expsyms)$" "$nlist" > "$nlist"T $MV "$nlist"T "$nlist" fi # Try sorting and uniquifying the output. if $GREP -v "^: " < "$nlist" | if sort -k 3 /dev/null 2>&1; then sort -k 3 else sort +2 fi | uniq > "$nlist"S; then : else $GREP -v "^: " < "$nlist" > "$nlist"S fi if test -f "$nlist"S; then eval "$global_symbol_to_cdecl"' < "$nlist"S >> "$output_objdir/$my_dlsyms"' else echo '/* NONE */' >> "$output_objdir/$my_dlsyms" fi echo >> "$output_objdir/$my_dlsyms" "\ /* The mapping between symbol names and symbols. */ typedef struct { const char *name; void *address; } lt_dlsymlist; extern LT_DLSYM_CONST lt_dlsymlist lt_${my_prefix}_LTX_preloaded_symbols[]; LT_DLSYM_CONST lt_dlsymlist lt_${my_prefix}_LTX_preloaded_symbols[] = {\ { \"$my_originator\", (void *) 0 }," case $need_lib_prefix in no) eval "$global_symbol_to_c_name_address" < "$nlist" >> "$output_objdir/$my_dlsyms" ;; *) eval "$global_symbol_to_c_name_address_lib_prefix" < "$nlist" >> "$output_objdir/$my_dlsyms" ;; esac echo >> "$output_objdir/$my_dlsyms" "\ {0, (void *) 0} }; /* This works around a problem in FreeBSD linker */ #ifdef FREEBSD_WORKAROUND static const void *lt_preloaded_setup() { return lt_${my_prefix}_LTX_preloaded_symbols; } #endif #ifdef __cplusplus } #endif\ " } # !$opt_dry_run pic_flag_for_symtable= case "$compile_command " in *" -static "*) ;; *) case $host in # compiling the symbol table file with pic_flag works around # a FreeBSD bug that causes programs to crash when -lm is # linked before any other PIC object. But we must not use # pic_flag when linking with -static. The problem exists in # FreeBSD 2.2.6 and is fixed in FreeBSD 3.1. *-*-freebsd2.*|*-*-freebsd3.0*|*-*-freebsdelf3.0*) pic_flag_for_symtable=" $pic_flag -DFREEBSD_WORKAROUND" ;; *-*-hpux*) pic_flag_for_symtable=" $pic_flag" ;; *) if test "X$my_pic_p" != Xno; then pic_flag_for_symtable=" $pic_flag" fi ;; esac ;; esac symtab_cflags= for arg in $LTCFLAGS; do case $arg in -pie | -fpie | -fPIE) ;; *) func_append symtab_cflags " $arg" ;; esac done # Now compile the dynamic symbol file. func_show_eval '(cd $output_objdir && $LTCC$symtab_cflags -c$no_builtin_flag$pic_flag_for_symtable "$my_dlsyms")' 'exit $?' # Clean up the generated files. func_show_eval '$RM "$output_objdir/$my_dlsyms" "$nlist" "${nlist}S" "${nlist}T"' # Transform the symbol file into the correct name. symfileobj="$output_objdir/${my_outputname}S.$objext" case $host in *cygwin* | *mingw* | *cegcc* ) if test -f "$output_objdir/$my_outputname.def"; then compile_command=`$ECHO "$compile_command" | $SED "s%@SYMFILE@%$output_objdir/$my_outputname.def $symfileobj%"` finalize_command=`$ECHO "$finalize_command" | $SED "s%@SYMFILE@%$output_objdir/$my_outputname.def $symfileobj%"` else compile_command=`$ECHO "$compile_command" | $SED "s%@SYMFILE@%$symfileobj%"` finalize_command=`$ECHO "$finalize_command" | $SED "s%@SYMFILE@%$symfileobj%"` fi ;; *) compile_command=`$ECHO "$compile_command" | $SED "s%@SYMFILE@%$symfileobj%"` finalize_command=`$ECHO "$finalize_command" | $SED "s%@SYMFILE@%$symfileobj%"` ;; esac ;; *) func_fatal_error "unknown suffix for \`$my_dlsyms'" ;; esac else # We keep going just in case the user didn't refer to # lt_preloaded_symbols. The linker will fail if global_symbol_pipe # really was required. # Nullify the symbol file. compile_command=`$ECHO "$compile_command" | $SED "s% @SYMFILE@%%"` finalize_command=`$ECHO "$finalize_command" | $SED "s% @SYMFILE@%%"` fi } # func_win32_libid arg # return the library type of file 'arg' # # Need a lot of goo to handle *both* DLLs and import libs # Has to be a shell function in order to 'eat' the argument # that is supplied when $file_magic_command is called. # Despite the name, also deal with 64 bit binaries. func_win32_libid () { $opt_debug win32_libid_type="unknown" win32_fileres=`file -L $1 2>/dev/null` case $win32_fileres in *ar\ archive\ import\ library*) # definitely import win32_libid_type="x86 archive import" ;; *ar\ archive*) # could be an import, or static # Keep the egrep pattern in sync with the one in _LT_CHECK_MAGIC_METHOD. if eval $OBJDUMP -f $1 | $SED -e '10q' 2>/dev/null | $EGREP 'file format (pei*-i386(.*architecture: i386)?|pe-arm-wince|pe-x86-64)' >/dev/null; then func_to_tool_file "$1" func_convert_file_msys_to_w32 win32_nmres=`eval $NM -f posix -A \"$func_to_tool_file_result\" | $SED -n -e ' 1,100{ / I /{ s,.*,import, p q } }'` case $win32_nmres in import*) win32_libid_type="x86 archive import";; *) win32_libid_type="x86 archive static";; esac fi ;; *DLL*) win32_libid_type="x86 DLL" ;; *executable*) # but shell scripts are "executable" too... case $win32_fileres in *MS\ Windows\ PE\ Intel*) win32_libid_type="x86 DLL" ;; esac ;; esac $ECHO "$win32_libid_type" } # func_cygming_dll_for_implib ARG # # Platform-specific function to extract the # name of the DLL associated with the specified # import library ARG. # Invoked by eval'ing the libtool variable # $sharedlib_from_linklib_cmd # Result is available in the variable # $sharedlib_from_linklib_result func_cygming_dll_for_implib () { $opt_debug sharedlib_from_linklib_result=`$DLLTOOL --identify-strict --identify "$1"` } # func_cygming_dll_for_implib_fallback_core SECTION_NAME LIBNAMEs # # The is the core of a fallback implementation of a # platform-specific function to extract the name of the # DLL associated with the specified import library LIBNAME. # # SECTION_NAME is either .idata$6 or .idata$7, depending # on the platform and compiler that created the implib. # # Echos the name of the DLL associated with the # specified import library. func_cygming_dll_for_implib_fallback_core () { $opt_debug match_literal=`$ECHO "$1" | $SED "$sed_make_literal_regex"` $OBJDUMP -s --section "$1" "$2" 2>/dev/null | $SED '/^Contents of section '"$match_literal"':/{ # Place marker at beginning of archive member dllname section s/.*/====MARK====/ p d } # These lines can sometimes be longer than 43 characters, but # are always uninteresting /:[ ]*file format pe[i]\{,1\}-/d /^In archive [^:]*:/d # Ensure marker is printed /^====MARK====/p # Remove all lines with less than 43 characters /^.\{43\}/!d # From remaining lines, remove first 43 characters s/^.\{43\}//' | $SED -n ' # Join marker and all lines until next marker into a single line /^====MARK====/ b para H $ b para b :para x s/\n//g # Remove the marker s/^====MARK====// # Remove trailing dots and whitespace s/[\. \t]*$// # Print /./p' | # we now have a list, one entry per line, of the stringified # contents of the appropriate section of all members of the # archive which possess that section. Heuristic: eliminate # all those which have a first or second character that is # a '.' (that is, objdump's representation of an unprintable # character.) This should work for all archives with less than # 0x302f exports -- but will fail for DLLs whose name actually # begins with a literal '.' or a single character followed by # a '.'. # # Of those that remain, print the first one. $SED -e '/^\./d;/^.\./d;q' } # func_cygming_gnu_implib_p ARG # This predicate returns with zero status (TRUE) if # ARG is a GNU/binutils-style import library. Returns # with nonzero status (FALSE) otherwise. func_cygming_gnu_implib_p () { $opt_debug func_to_tool_file "$1" func_convert_file_msys_to_w32 func_cygming_gnu_implib_tmp=`$NM "$func_to_tool_file_result" | eval "$global_symbol_pipe" | $EGREP ' (_head_[A-Za-z0-9_]+_[ad]l*|[A-Za-z0-9_]+_[ad]l*_iname)$'` test -n "$func_cygming_gnu_implib_tmp" } # func_cygming_ms_implib_p ARG # This predicate returns with zero status (TRUE) if # ARG is an MS-style import library. Returns # with nonzero status (FALSE) otherwise. func_cygming_ms_implib_p () { $opt_debug func_to_tool_file "$1" func_convert_file_msys_to_w32 func_cygming_ms_implib_tmp=`$NM "$func_to_tool_file_result" | eval "$global_symbol_pipe" | $GREP '_NULL_IMPORT_DESCRIPTOR'` test -n "$func_cygming_ms_implib_tmp" } # func_cygming_dll_for_implib_fallback ARG # Platform-specific function to extract the # name of the DLL associated with the specified # import library ARG. # # This fallback implementation is for use when $DLLTOOL # does not support the --identify-strict option. # Invoked by eval'ing the libtool variable # $sharedlib_from_linklib_cmd # Result is available in the variable # $sharedlib_from_linklib_result func_cygming_dll_for_implib_fallback () { $opt_debug if func_cygming_gnu_implib_p "$1" ; then # binutils import library sharedlib_from_linklib_result=`func_cygming_dll_for_implib_fallback_core '.idata$7' "$1"` elif func_cygming_ms_implib_p "$1" ; then # ms-generated import library sharedlib_from_linklib_result=`func_cygming_dll_for_implib_fallback_core '.idata$6' "$1"` else # unknown sharedlib_from_linklib_result="" fi } # func_extract_an_archive dir oldlib func_extract_an_archive () { $opt_debug f_ex_an_ar_dir="$1"; shift f_ex_an_ar_oldlib="$1" if test "$lock_old_archive_extraction" = yes; then lockfile=$f_ex_an_ar_oldlib.lock until $opt_dry_run || ln "$progpath" "$lockfile" 2>/dev/null; do func_echo "Waiting for $lockfile to be removed" sleep 2 done fi func_show_eval "(cd \$f_ex_an_ar_dir && $AR x \"\$f_ex_an_ar_oldlib\")" \ 'stat=$?; rm -f "$lockfile"; exit $stat' if test "$lock_old_archive_extraction" = yes; then $opt_dry_run || rm -f "$lockfile" fi if ($AR t "$f_ex_an_ar_oldlib" | sort | sort -uc >/dev/null 2>&1); then : else func_fatal_error "object name conflicts in archive: $f_ex_an_ar_dir/$f_ex_an_ar_oldlib" fi } # func_extract_archives gentop oldlib ... func_extract_archives () { $opt_debug my_gentop="$1"; shift my_oldlibs=${1+"$@"} my_oldobjs="" my_xlib="" my_xabs="" my_xdir="" for my_xlib in $my_oldlibs; do # Extract the objects. case $my_xlib in [\\/]* | [A-Za-z]:[\\/]*) my_xabs="$my_xlib" ;; *) my_xabs=`pwd`"/$my_xlib" ;; esac func_basename "$my_xlib" my_xlib="$func_basename_result" my_xlib_u=$my_xlib while :; do case " $extracted_archives " in *" $my_xlib_u "*) func_arith $extracted_serial + 1 extracted_serial=$func_arith_result my_xlib_u=lt$extracted_serial-$my_xlib ;; *) break ;; esac done extracted_archives="$extracted_archives $my_xlib_u" my_xdir="$my_gentop/$my_xlib_u" func_mkdir_p "$my_xdir" case $host in *-darwin*) func_verbose "Extracting $my_xabs" # Do not bother doing anything if just a dry run $opt_dry_run || { darwin_orig_dir=`pwd` cd $my_xdir || exit $? darwin_archive=$my_xabs darwin_curdir=`pwd` darwin_base_archive=`basename "$darwin_archive"` darwin_arches=`$LIPO -info "$darwin_archive" 2>/dev/null | $GREP Architectures 2>/dev/null || true` if test -n "$darwin_arches"; then darwin_arches=`$ECHO "$darwin_arches" | $SED -e 's/.*are://'` darwin_arch= func_verbose "$darwin_base_archive has multiple architectures $darwin_arches" for darwin_arch in $darwin_arches ; do func_mkdir_p "unfat-$$/${darwin_base_archive}-${darwin_arch}" $LIPO -thin $darwin_arch -output "unfat-$$/${darwin_base_archive}-${darwin_arch}/${darwin_base_archive}" "${darwin_archive}" cd "unfat-$$/${darwin_base_archive}-${darwin_arch}" func_extract_an_archive "`pwd`" "${darwin_base_archive}" cd "$darwin_curdir" $RM "unfat-$$/${darwin_base_archive}-${darwin_arch}/${darwin_base_archive}" done # $darwin_arches ## Okay now we've a bunch of thin objects, gotta fatten them up :) darwin_filelist=`find unfat-$$ -type f -name \*.o -print -o -name \*.lo -print | $SED -e "$basename" | sort -u` darwin_file= darwin_files= for darwin_file in $darwin_filelist; do darwin_files=`find unfat-$$ -name $darwin_file -print | sort | $NL2SP` $LIPO -create -output "$darwin_file" $darwin_files done # $darwin_filelist $RM -rf unfat-$$ cd "$darwin_orig_dir" else cd $darwin_orig_dir func_extract_an_archive "$my_xdir" "$my_xabs" fi # $darwin_arches } # !$opt_dry_run ;; *) func_extract_an_archive "$my_xdir" "$my_xabs" ;; esac my_oldobjs="$my_oldobjs "`find $my_xdir -name \*.$objext -print -o -name \*.lo -print | sort | $NL2SP` done func_extract_archives_result="$my_oldobjs" } # func_emit_wrapper [arg=no] # # Emit a libtool wrapper script on stdout. # Don't directly open a file because we may want to # incorporate the script contents within a cygwin/mingw # wrapper executable. Must ONLY be called from within # func_mode_link because it depends on a number of variables # set therein. # # ARG is the value that the WRAPPER_SCRIPT_BELONGS_IN_OBJDIR # variable will take. If 'yes', then the emitted script # will assume that the directory in which it is stored is # the $objdir directory. This is a cygwin/mingw-specific # behavior. func_emit_wrapper () { func_emit_wrapper_arg1=${1-no} $ECHO "\ #! $SHELL # $output - temporary wrapper script for $objdir/$outputname # Generated by $PROGRAM (GNU $PACKAGE$TIMESTAMP) $VERSION # # The $output program cannot be directly executed until all the libtool # libraries that it depends on are installed. # # This wrapper script should never be moved out of the build directory. # If it is, it will not operate correctly. # Sed substitution that helps us do robust quoting. It backslashifies # metacharacters that are still active within double-quoted strings. sed_quote_subst='$sed_quote_subst' # Be Bourne compatible if test -n \"\${ZSH_VERSION+set}\" && (emulate sh) >/dev/null 2>&1; then emulate sh NULLCMD=: # Zsh 3.x and 4.x performs word splitting on \${1+\"\$@\"}, which # is contrary to our usage. Disable this feature. alias -g '\${1+\"\$@\"}'='\"\$@\"' setopt NO_GLOB_SUBST else case \`(set -o) 2>/dev/null\` in *posix*) set -o posix;; esac fi BIN_SH=xpg4; export BIN_SH # for Tru64 DUALCASE=1; export DUALCASE # for MKS sh # The HP-UX ksh and POSIX shell print the target directory to stdout # if CDPATH is set. (unset CDPATH) >/dev/null 2>&1 && unset CDPATH relink_command=\"$relink_command\" # This environment variable determines our operation mode. if test \"\$libtool_install_magic\" = \"$magic\"; then # install mode needs the following variables: generated_by_libtool_version='$macro_version' notinst_deplibs='$notinst_deplibs' else # When we are sourced in execute mode, \$file and \$ECHO are already set. if test \"\$libtool_execute_magic\" != \"$magic\"; then file=\"\$0\"" qECHO=`$ECHO "$ECHO" | $SED "$sed_quote_subst"` $ECHO "\ # A function that is used when there is no print builtin or printf. func_fallback_echo () { eval 'cat <<_LTECHO_EOF \$1 _LTECHO_EOF' } ECHO=\"$qECHO\" fi # Very basic option parsing. These options are (a) specific to # the libtool wrapper, (b) are identical between the wrapper # /script/ and the wrapper /executable/ which is used only on # windows platforms, and (c) all begin with the string "--lt-" # (application programs are unlikely to have options which match # this pattern). # # There are only two supported options: --lt-debug and # --lt-dump-script. There is, deliberately, no --lt-help. # # The first argument to this parsing function should be the # script's $0 value, followed by "$@". lt_option_debug= func_parse_lt_options () { lt_script_arg0=\$0 shift for lt_opt do case \"\$lt_opt\" in --lt-debug) lt_option_debug=1 ;; --lt-dump-script) lt_dump_D=\`\$ECHO \"X\$lt_script_arg0\" | $SED -e 's/^X//' -e 's%/[^/]*$%%'\` test \"X\$lt_dump_D\" = \"X\$lt_script_arg0\" && lt_dump_D=. lt_dump_F=\`\$ECHO \"X\$lt_script_arg0\" | $SED -e 's/^X//' -e 's%^.*/%%'\` cat \"\$lt_dump_D/\$lt_dump_F\" exit 0 ;; --lt-*) \$ECHO \"Unrecognized --lt- option: '\$lt_opt'\" 1>&2 exit 1 ;; esac done # Print the debug banner immediately: if test -n \"\$lt_option_debug\"; then echo \"${outputname}:${output}:\${LINENO}: libtool wrapper (GNU $PACKAGE$TIMESTAMP) $VERSION\" 1>&2 fi } # Used when --lt-debug. Prints its arguments to stdout # (redirection is the responsibility of the caller) func_lt_dump_args () { lt_dump_args_N=1; for lt_arg do \$ECHO \"${outputname}:${output}:\${LINENO}: newargv[\$lt_dump_args_N]: \$lt_arg\" lt_dump_args_N=\`expr \$lt_dump_args_N + 1\` done } # Core function for launching the target application func_exec_program_core () { " case $host in # Backslashes separate directories on plain windows *-*-mingw | *-*-os2* | *-cegcc*) $ECHO "\ if test -n \"\$lt_option_debug\"; then \$ECHO \"${outputname}:${output}:\${LINENO}: newargv[0]: \$progdir\\\\\$program\" 1>&2 func_lt_dump_args \${1+\"\$@\"} 1>&2 fi exec \"\$progdir\\\\\$program\" \${1+\"\$@\"} " ;; *) $ECHO "\ if test -n \"\$lt_option_debug\"; then \$ECHO \"${outputname}:${output}:\${LINENO}: newargv[0]: \$progdir/\$program\" 1>&2 func_lt_dump_args \${1+\"\$@\"} 1>&2 fi exec \"\$progdir/\$program\" \${1+\"\$@\"} " ;; esac $ECHO "\ \$ECHO \"\$0: cannot exec \$program \$*\" 1>&2 exit 1 } # A function to encapsulate launching the target application # Strips options in the --lt-* namespace from \$@ and # launches target application with the remaining arguments. func_exec_program () { case \" \$* \" in *\\ --lt-*) for lt_wr_arg do case \$lt_wr_arg in --lt-*) ;; *) set x \"\$@\" \"\$lt_wr_arg\"; shift;; esac shift done ;; esac func_exec_program_core \${1+\"\$@\"} } # Parse options func_parse_lt_options \"\$0\" \${1+\"\$@\"} # Find the directory that this script lives in. thisdir=\`\$ECHO \"\$file\" | $SED 's%/[^/]*$%%'\` test \"x\$thisdir\" = \"x\$file\" && thisdir=. # Follow symbolic links until we get to the real thisdir. file=\`ls -ld \"\$file\" | $SED -n 's/.*-> //p'\` while test -n \"\$file\"; do destdir=\`\$ECHO \"\$file\" | $SED 's%/[^/]*\$%%'\` # If there was a directory component, then change thisdir. if test \"x\$destdir\" != \"x\$file\"; then case \"\$destdir\" in [\\\\/]* | [A-Za-z]:[\\\\/]*) thisdir=\"\$destdir\" ;; *) thisdir=\"\$thisdir/\$destdir\" ;; esac fi file=\`\$ECHO \"\$file\" | $SED 's%^.*/%%'\` file=\`ls -ld \"\$thisdir/\$file\" | $SED -n 's/.*-> //p'\` done # Usually 'no', except on cygwin/mingw when embedded into # the cwrapper. WRAPPER_SCRIPT_BELONGS_IN_OBJDIR=$func_emit_wrapper_arg1 if test \"\$WRAPPER_SCRIPT_BELONGS_IN_OBJDIR\" = \"yes\"; then # special case for '.' if test \"\$thisdir\" = \".\"; then thisdir=\`pwd\` fi # remove .libs from thisdir case \"\$thisdir\" in *[\\\\/]$objdir ) thisdir=\`\$ECHO \"\$thisdir\" | $SED 's%[\\\\/][^\\\\/]*$%%'\` ;; $objdir ) thisdir=. ;; esac fi # Try to get the absolute directory name. absdir=\`cd \"\$thisdir\" && pwd\` test -n \"\$absdir\" && thisdir=\"\$absdir\" " if test "$fast_install" = yes; then $ECHO "\ program=lt-'$outputname'$exeext progdir=\"\$thisdir/$objdir\" if test ! -f \"\$progdir/\$program\" || { file=\`ls -1dt \"\$progdir/\$program\" \"\$progdir/../\$program\" 2>/dev/null | ${SED} 1q\`; \\ test \"X\$file\" != \"X\$progdir/\$program\"; }; then file=\"\$\$-\$program\" if test ! -d \"\$progdir\"; then $MKDIR \"\$progdir\" else $RM \"\$progdir/\$file\" fi" $ECHO "\ # relink executable if necessary if test -n \"\$relink_command\"; then if relink_command_output=\`eval \$relink_command 2>&1\`; then : else $ECHO \"\$relink_command_output\" >&2 $RM \"\$progdir/\$file\" exit 1 fi fi $MV \"\$progdir/\$file\" \"\$progdir/\$program\" 2>/dev/null || { $RM \"\$progdir/\$program\"; $MV \"\$progdir/\$file\" \"\$progdir/\$program\"; } $RM \"\$progdir/\$file\" fi" else $ECHO "\ program='$outputname' progdir=\"\$thisdir/$objdir\" " fi $ECHO "\ if test -f \"\$progdir/\$program\"; then" # fixup the dll searchpath if we need to. # # Fix the DLL searchpath if we need to. Do this before prepending # to shlibpath, because on Windows, both are PATH and uninstalled # libraries must come first. if test -n "$dllsearchpath"; then $ECHO "\ # Add the dll search path components to the executable PATH PATH=$dllsearchpath:\$PATH " fi # Export our shlibpath_var if we have one. if test "$shlibpath_overrides_runpath" = yes && test -n "$shlibpath_var" && test -n "$temp_rpath"; then $ECHO "\ # Add our own library path to $shlibpath_var $shlibpath_var=\"$temp_rpath\$$shlibpath_var\" # Some systems cannot cope with colon-terminated $shlibpath_var # The second colon is a workaround for a bug in BeOS R4 sed $shlibpath_var=\`\$ECHO \"\$$shlibpath_var\" | $SED 's/::*\$//'\` export $shlibpath_var " fi $ECHO "\ if test \"\$libtool_execute_magic\" != \"$magic\"; then # Run the actual program with our arguments. func_exec_program \${1+\"\$@\"} fi else # The program doesn't exist. \$ECHO \"\$0: error: \\\`\$progdir/\$program' does not exist\" 1>&2 \$ECHO \"This script is just a wrapper for \$program.\" 1>&2 \$ECHO \"See the $PACKAGE documentation for more information.\" 1>&2 exit 1 fi fi\ " } # func_emit_cwrapperexe_src # emit the source code for a wrapper executable on stdout # Must ONLY be called from within func_mode_link because # it depends on a number of variable set therein. func_emit_cwrapperexe_src () { cat < #include #ifdef _MSC_VER # include # include # include #else # include # include # ifdef __CYGWIN__ # include # endif #endif #include #include #include #include #include #include #include #include /* declarations of non-ANSI functions */ #if defined(__MINGW32__) # ifdef __STRICT_ANSI__ int _putenv (const char *); # endif #elif defined(__CYGWIN__) # ifdef __STRICT_ANSI__ char *realpath (const char *, char *); int putenv (char *); int setenv (const char *, const char *, int); # endif /* #elif defined (other platforms) ... */ #endif /* portability defines, excluding path handling macros */ #if defined(_MSC_VER) # define setmode _setmode # define stat _stat # define chmod _chmod # define getcwd _getcwd # define putenv _putenv # define S_IXUSR _S_IEXEC # ifndef _INTPTR_T_DEFINED # define _INTPTR_T_DEFINED # define intptr_t int # endif #elif defined(__MINGW32__) # define setmode _setmode # define stat _stat # define chmod _chmod # define getcwd _getcwd # define putenv _putenv #elif defined(__CYGWIN__) # define HAVE_SETENV # define FOPEN_WB "wb" /* #elif defined (other platforms) ... */ #endif #if defined(PATH_MAX) # define LT_PATHMAX PATH_MAX #elif defined(MAXPATHLEN) # define LT_PATHMAX MAXPATHLEN #else # define LT_PATHMAX 1024 #endif #ifndef S_IXOTH # define S_IXOTH 0 #endif #ifndef S_IXGRP # define S_IXGRP 0 #endif /* path handling portability macros */ #ifndef DIR_SEPARATOR # define DIR_SEPARATOR '/' # define PATH_SEPARATOR ':' #endif #if defined (_WIN32) || defined (__MSDOS__) || defined (__DJGPP__) || \ defined (__OS2__) # define HAVE_DOS_BASED_FILE_SYSTEM # define FOPEN_WB "wb" # ifndef DIR_SEPARATOR_2 # define DIR_SEPARATOR_2 '\\' # endif # ifndef PATH_SEPARATOR_2 # define PATH_SEPARATOR_2 ';' # endif #endif #ifndef DIR_SEPARATOR_2 # define IS_DIR_SEPARATOR(ch) ((ch) == DIR_SEPARATOR) #else /* DIR_SEPARATOR_2 */ # define IS_DIR_SEPARATOR(ch) \ (((ch) == DIR_SEPARATOR) || ((ch) == DIR_SEPARATOR_2)) #endif /* DIR_SEPARATOR_2 */ #ifndef PATH_SEPARATOR_2 # define IS_PATH_SEPARATOR(ch) ((ch) == PATH_SEPARATOR) #else /* PATH_SEPARATOR_2 */ # define IS_PATH_SEPARATOR(ch) ((ch) == PATH_SEPARATOR_2) #endif /* PATH_SEPARATOR_2 */ #ifndef FOPEN_WB # define FOPEN_WB "w" #endif #ifndef _O_BINARY # define _O_BINARY 0 #endif #define XMALLOC(type, num) ((type *) xmalloc ((num) * sizeof(type))) #define XFREE(stale) do { \ if (stale) { free ((void *) stale); stale = 0; } \ } while (0) #if defined(LT_DEBUGWRAPPER) static int lt_debug = 1; #else static int lt_debug = 0; #endif const char *program_name = "libtool-wrapper"; /* in case xstrdup fails */ void *xmalloc (size_t num); char *xstrdup (const char *string); const char *base_name (const char *name); char *find_executable (const char *wrapper); char *chase_symlinks (const char *pathspec); int make_executable (const char *path); int check_executable (const char *path); char *strendzap (char *str, const char *pat); void lt_debugprintf (const char *file, int line, const char *fmt, ...); void lt_fatal (const char *file, int line, const char *message, ...); static const char *nonnull (const char *s); static const char *nonempty (const char *s); void lt_setenv (const char *name, const char *value); char *lt_extend_str (const char *orig_value, const char *add, int to_end); void lt_update_exe_path (const char *name, const char *value); void lt_update_lib_path (const char *name, const char *value); char **prepare_spawn (char **argv); void lt_dump_script (FILE *f); EOF cat <= 0) && (st.st_mode & (S_IXUSR | S_IXGRP | S_IXOTH))) return 1; else return 0; } int make_executable (const char *path) { int rval = 0; struct stat st; lt_debugprintf (__FILE__, __LINE__, "(make_executable): %s\n", nonempty (path)); if ((!path) || (!*path)) return 0; if (stat (path, &st) >= 0) { rval = chmod (path, st.st_mode | S_IXOTH | S_IXGRP | S_IXUSR); } return rval; } /* Searches for the full path of the wrapper. Returns newly allocated full path name if found, NULL otherwise Does not chase symlinks, even on platforms that support them. */ char * find_executable (const char *wrapper) { int has_slash = 0; const char *p; const char *p_next; /* static buffer for getcwd */ char tmp[LT_PATHMAX + 1]; int tmp_len; char *concat_name; lt_debugprintf (__FILE__, __LINE__, "(find_executable): %s\n", nonempty (wrapper)); if ((wrapper == NULL) || (*wrapper == '\0')) return NULL; /* Absolute path? */ #if defined (HAVE_DOS_BASED_FILE_SYSTEM) if (isalpha ((unsigned char) wrapper[0]) && wrapper[1] == ':') { concat_name = xstrdup (wrapper); if (check_executable (concat_name)) return concat_name; XFREE (concat_name); } else { #endif if (IS_DIR_SEPARATOR (wrapper[0])) { concat_name = xstrdup (wrapper); if (check_executable (concat_name)) return concat_name; XFREE (concat_name); } #if defined (HAVE_DOS_BASED_FILE_SYSTEM) } #endif for (p = wrapper; *p; p++) if (*p == '/') { has_slash = 1; break; } if (!has_slash) { /* no slashes; search PATH */ const char *path = getenv ("PATH"); if (path != NULL) { for (p = path; *p; p = p_next) { const char *q; size_t p_len; for (q = p; *q; q++) if (IS_PATH_SEPARATOR (*q)) break; p_len = q - p; p_next = (*q == '\0' ? q : q + 1); if (p_len == 0) { /* empty path: current directory */ if (getcwd (tmp, LT_PATHMAX) == NULL) lt_fatal (__FILE__, __LINE__, "getcwd failed: %s", nonnull (strerror (errno))); tmp_len = strlen (tmp); concat_name = XMALLOC (char, tmp_len + 1 + strlen (wrapper) + 1); memcpy (concat_name, tmp, tmp_len); concat_name[tmp_len] = '/'; strcpy (concat_name + tmp_len + 1, wrapper); } else { concat_name = XMALLOC (char, p_len + 1 + strlen (wrapper) + 1); memcpy (concat_name, p, p_len); concat_name[p_len] = '/'; strcpy (concat_name + p_len + 1, wrapper); } if (check_executable (concat_name)) return concat_name; XFREE (concat_name); } } /* not found in PATH; assume curdir */ } /* Relative path | not found in path: prepend cwd */ if (getcwd (tmp, LT_PATHMAX) == NULL) lt_fatal (__FILE__, __LINE__, "getcwd failed: %s", nonnull (strerror (errno))); tmp_len = strlen (tmp); concat_name = XMALLOC (char, tmp_len + 1 + strlen (wrapper) + 1); memcpy (concat_name, tmp, tmp_len); concat_name[tmp_len] = '/'; strcpy (concat_name + tmp_len + 1, wrapper); if (check_executable (concat_name)) return concat_name; XFREE (concat_name); return NULL; } char * chase_symlinks (const char *pathspec) { #ifndef S_ISLNK return xstrdup (pathspec); #else char buf[LT_PATHMAX]; struct stat s; char *tmp_pathspec = xstrdup (pathspec); char *p; int has_symlinks = 0; while (strlen (tmp_pathspec) && !has_symlinks) { lt_debugprintf (__FILE__, __LINE__, "checking path component for symlinks: %s\n", tmp_pathspec); if (lstat (tmp_pathspec, &s) == 0) { if (S_ISLNK (s.st_mode) != 0) { has_symlinks = 1; break; } /* search backwards for last DIR_SEPARATOR */ p = tmp_pathspec + strlen (tmp_pathspec) - 1; while ((p > tmp_pathspec) && (!IS_DIR_SEPARATOR (*p))) p--; if ((p == tmp_pathspec) && (!IS_DIR_SEPARATOR (*p))) { /* no more DIR_SEPARATORS left */ break; } *p = '\0'; } else { lt_fatal (__FILE__, __LINE__, "error accessing file \"%s\": %s", tmp_pathspec, nonnull (strerror (errno))); } } XFREE (tmp_pathspec); if (!has_symlinks) { return xstrdup (pathspec); } tmp_pathspec = realpath (pathspec, buf); if (tmp_pathspec == 0) { lt_fatal (__FILE__, __LINE__, "could not follow symlinks for %s", pathspec); } return xstrdup (tmp_pathspec); #endif } char * strendzap (char *str, const char *pat) { size_t len, patlen; assert (str != NULL); assert (pat != NULL); len = strlen (str); patlen = strlen (pat); if (patlen <= len) { str += len - patlen; if (strcmp (str, pat) == 0) *str = '\0'; } return str; } void lt_debugprintf (const char *file, int line, const char *fmt, ...) { va_list args; if (lt_debug) { (void) fprintf (stderr, "%s:%s:%d: ", program_name, file, line); va_start (args, fmt); (void) vfprintf (stderr, fmt, args); va_end (args); } } static void lt_error_core (int exit_status, const char *file, int line, const char *mode, const char *message, va_list ap) { fprintf (stderr, "%s:%s:%d: %s: ", program_name, file, line, mode); vfprintf (stderr, message, ap); fprintf (stderr, ".\n"); if (exit_status >= 0) exit (exit_status); } void lt_fatal (const char *file, int line, const char *message, ...) { va_list ap; va_start (ap, message); lt_error_core (EXIT_FAILURE, file, line, "FATAL", message, ap); va_end (ap); } static const char * nonnull (const char *s) { return s ? s : "(null)"; } static const char * nonempty (const char *s) { return (s && !*s) ? "(empty)" : nonnull (s); } void lt_setenv (const char *name, const char *value) { lt_debugprintf (__FILE__, __LINE__, "(lt_setenv) setting '%s' to '%s'\n", nonnull (name), nonnull (value)); { #ifdef HAVE_SETENV /* always make a copy, for consistency with !HAVE_SETENV */ char *str = xstrdup (value); setenv (name, str, 1); #else int len = strlen (name) + 1 + strlen (value) + 1; char *str = XMALLOC (char, len); sprintf (str, "%s=%s", name, value); if (putenv (str) != EXIT_SUCCESS) { XFREE (str); } #endif } } char * lt_extend_str (const char *orig_value, const char *add, int to_end) { char *new_value; if (orig_value && *orig_value) { int orig_value_len = strlen (orig_value); int add_len = strlen (add); new_value = XMALLOC (char, add_len + orig_value_len + 1); if (to_end) { strcpy (new_value, orig_value); strcpy (new_value + orig_value_len, add); } else { strcpy (new_value, add); strcpy (new_value + add_len, orig_value); } } else { new_value = xstrdup (add); } return new_value; } void lt_update_exe_path (const char *name, const char *value) { lt_debugprintf (__FILE__, __LINE__, "(lt_update_exe_path) modifying '%s' by prepending '%s'\n", nonnull (name), nonnull (value)); if (name && *name && value && *value) { char *new_value = lt_extend_str (getenv (name), value, 0); /* some systems can't cope with a ':'-terminated path #' */ int len = strlen (new_value); while (((len = strlen (new_value)) > 0) && IS_PATH_SEPARATOR (new_value[len-1])) { new_value[len-1] = '\0'; } lt_setenv (name, new_value); XFREE (new_value); } } void lt_update_lib_path (const char *name, const char *value) { lt_debugprintf (__FILE__, __LINE__, "(lt_update_lib_path) modifying '%s' by prepending '%s'\n", nonnull (name), nonnull (value)); if (name && *name && value && *value) { char *new_value = lt_extend_str (getenv (name), value, 0); lt_setenv (name, new_value); XFREE (new_value); } } EOF case $host_os in mingw*) cat <<"EOF" /* Prepares an argument vector before calling spawn(). Note that spawn() does not by itself call the command interpreter (getenv ("COMSPEC") != NULL ? getenv ("COMSPEC") : ({ OSVERSIONINFO v; v.dwOSVersionInfoSize = sizeof(OSVERSIONINFO); GetVersionEx(&v); v.dwPlatformId == VER_PLATFORM_WIN32_NT; }) ? "cmd.exe" : "command.com"). Instead it simply concatenates the arguments, separated by ' ', and calls CreateProcess(). We must quote the arguments since Win32 CreateProcess() interprets characters like ' ', '\t', '\\', '"' (but not '<' and '>') in a special way: - Space and tab are interpreted as delimiters. They are not treated as delimiters if they are surrounded by double quotes: "...". - Unescaped double quotes are removed from the input. Their only effect is that within double quotes, space and tab are treated like normal characters. - Backslashes not followed by double quotes are not special. - But 2*n+1 backslashes followed by a double quote become n backslashes followed by a double quote (n >= 0): \" -> " \\\" -> \" \\\\\" -> \\" */ #define SHELL_SPECIAL_CHARS "\"\\ \001\002\003\004\005\006\007\010\011\012\013\014\015\016\017\020\021\022\023\024\025\026\027\030\031\032\033\034\035\036\037" #define SHELL_SPACE_CHARS " \001\002\003\004\005\006\007\010\011\012\013\014\015\016\017\020\021\022\023\024\025\026\027\030\031\032\033\034\035\036\037" char ** prepare_spawn (char **argv) { size_t argc; char **new_argv; size_t i; /* Count number of arguments. */ for (argc = 0; argv[argc] != NULL; argc++) ; /* Allocate new argument vector. */ new_argv = XMALLOC (char *, argc + 1); /* Put quoted arguments into the new argument vector. */ for (i = 0; i < argc; i++) { const char *string = argv[i]; if (string[0] == '\0') new_argv[i] = xstrdup ("\"\""); else if (strpbrk (string, SHELL_SPECIAL_CHARS) != NULL) { int quote_around = (strpbrk (string, SHELL_SPACE_CHARS) != NULL); size_t length; unsigned int backslashes; const char *s; char *quoted_string; char *p; length = 0; backslashes = 0; if (quote_around) length++; for (s = string; *s != '\0'; s++) { char c = *s; if (c == '"') length += backslashes + 1; length++; if (c == '\\') backslashes++; else backslashes = 0; } if (quote_around) length += backslashes + 1; quoted_string = XMALLOC (char, length + 1); p = quoted_string; backslashes = 0; if (quote_around) *p++ = '"'; for (s = string; *s != '\0'; s++) { char c = *s; if (c == '"') { unsigned int j; for (j = backslashes + 1; j > 0; j--) *p++ = '\\'; } *p++ = c; if (c == '\\') backslashes++; else backslashes = 0; } if (quote_around) { unsigned int j; for (j = backslashes; j > 0; j--) *p++ = '\\'; *p++ = '"'; } *p = '\0'; new_argv[i] = quoted_string; } else new_argv[i] = (char *) string; } new_argv[argc] = NULL; return new_argv; } EOF ;; esac cat <<"EOF" void lt_dump_script (FILE* f) { EOF func_emit_wrapper yes | $SED -n -e ' s/^\(.\{79\}\)\(..*\)/\1\ \2/ h s/\([\\"]\)/\\\1/g s/$/\\n/ s/\([^\n]*\).*/ fputs ("\1", f);/p g D' cat <<"EOF" } EOF } # end: func_emit_cwrapperexe_src # func_win32_import_lib_p ARG # True if ARG is an import lib, as indicated by $file_magic_cmd func_win32_import_lib_p () { $opt_debug case `eval $file_magic_cmd \"\$1\" 2>/dev/null | $SED -e 10q` in *import*) : ;; *) false ;; esac } # func_mode_link arg... func_mode_link () { $opt_debug case $host in *-*-cygwin* | *-*-mingw* | *-*-pw32* | *-*-os2* | *-cegcc*) # It is impossible to link a dll without this setting, and # we shouldn't force the makefile maintainer to figure out # which system we are compiling for in order to pass an extra # flag for every libtool invocation. # allow_undefined=no # FIXME: Unfortunately, there are problems with the above when trying # to make a dll which has undefined symbols, in which case not # even a static library is built. For now, we need to specify # -no-undefined on the libtool link line when we can be certain # that all symbols are satisfied, otherwise we get a static library. allow_undefined=yes ;; *) allow_undefined=yes ;; esac libtool_args=$nonopt base_compile="$nonopt $@" compile_command=$nonopt finalize_command=$nonopt compile_rpath= finalize_rpath= compile_shlibpath= finalize_shlibpath= convenience= old_convenience= deplibs= old_deplibs= compiler_flags= linker_flags= dllsearchpath= lib_search_path=`pwd` inst_prefix_dir= new_inherited_linker_flags= avoid_version=no bindir= dlfiles= dlprefiles= dlself=no export_dynamic=no export_symbols= export_symbols_regex= generated= libobjs= ltlibs= module=no no_install=no objs= non_pic_objects= precious_files_regex= prefer_static_libs=no preload=no prev= prevarg= release= rpath= xrpath= perm_rpath= temp_rpath= thread_safe=no vinfo= vinfo_number=no weak_libs= single_module="${wl}-single_module" func_infer_tag $base_compile # We need to know -static, to get the right output filenames. for arg do case $arg in -shared) test "$build_libtool_libs" != yes && \ func_fatal_configuration "can not build a shared library" build_old_libs=no break ;; -all-static | -static | -static-libtool-libs) case $arg in -all-static) if test "$build_libtool_libs" = yes && test -z "$link_static_flag"; then func_warning "complete static linking is impossible in this configuration" fi if test -n "$link_static_flag"; then dlopen_self=$dlopen_self_static fi prefer_static_libs=yes ;; -static) if test -z "$pic_flag" && test -n "$link_static_flag"; then dlopen_self=$dlopen_self_static fi prefer_static_libs=built ;; -static-libtool-libs) if test -z "$pic_flag" && test -n "$link_static_flag"; then dlopen_self=$dlopen_self_static fi prefer_static_libs=yes ;; esac build_libtool_libs=no build_old_libs=yes break ;; esac done # See if our shared archives depend on static archives. test -n "$old_archive_from_new_cmds" && build_old_libs=yes # Go through the arguments, transforming them on the way. while test "$#" -gt 0; do arg="$1" shift func_quote_for_eval "$arg" qarg=$func_quote_for_eval_unquoted_result func_append libtool_args " $func_quote_for_eval_result" # If the previous option needs an argument, assign it. if test -n "$prev"; then case $prev in output) func_append compile_command " @OUTPUT@" func_append finalize_command " @OUTPUT@" ;; esac case $prev in bindir) bindir="$arg" prev= continue ;; dlfiles|dlprefiles) if test "$preload" = no; then # Add the symbol object into the linking commands. func_append compile_command " @SYMFILE@" func_append finalize_command " @SYMFILE@" preload=yes fi case $arg in *.la | *.lo) ;; # We handle these cases below. force) if test "$dlself" = no; then dlself=needless export_dynamic=yes fi prev= continue ;; self) if test "$prev" = dlprefiles; then dlself=yes elif test "$prev" = dlfiles && test "$dlopen_self" != yes; then dlself=yes else dlself=needless export_dynamic=yes fi prev= continue ;; *) if test "$prev" = dlfiles; then func_append dlfiles " $arg" else func_append dlprefiles " $arg" fi prev= continue ;; esac ;; expsyms) export_symbols="$arg" test -f "$arg" \ || func_fatal_error "symbol file \`$arg' does not exist" prev= continue ;; expsyms_regex) export_symbols_regex="$arg" prev= continue ;; framework) case $host in *-*-darwin*) case "$deplibs " in *" $qarg.ltframework "*) ;; *) func_append deplibs " $qarg.ltframework" # this is fixed later ;; esac ;; esac prev= continue ;; inst_prefix) inst_prefix_dir="$arg" prev= continue ;; objectlist) if test -f "$arg"; then save_arg=$arg moreargs= for fil in `cat "$save_arg"` do # func_append moreargs " $fil" arg=$fil # A libtool-controlled object. # Check to see that this really is a libtool object. if func_lalib_unsafe_p "$arg"; then pic_object= non_pic_object= # Read the .lo file func_source "$arg" if test -z "$pic_object" || test -z "$non_pic_object" || test "$pic_object" = none && test "$non_pic_object" = none; then func_fatal_error "cannot find name of object for \`$arg'" fi # Extract subdirectory from the argument. func_dirname "$arg" "/" "" xdir="$func_dirname_result" if test "$pic_object" != none; then # Prepend the subdirectory the object is found in. pic_object="$xdir$pic_object" if test "$prev" = dlfiles; then if test "$build_libtool_libs" = yes && test "$dlopen_support" = yes; then func_append dlfiles " $pic_object" prev= continue else # If libtool objects are unsupported, then we need to preload. prev=dlprefiles fi fi # CHECK ME: I think I busted this. -Ossama if test "$prev" = dlprefiles; then # Preload the old-style object. func_append dlprefiles " $pic_object" prev= fi # A PIC object. func_append libobjs " $pic_object" arg="$pic_object" fi # Non-PIC object. if test "$non_pic_object" != none; then # Prepend the subdirectory the object is found in. non_pic_object="$xdir$non_pic_object" # A standard non-PIC object func_append non_pic_objects " $non_pic_object" if test -z "$pic_object" || test "$pic_object" = none ; then arg="$non_pic_object" fi else # If the PIC object exists, use it instead. # $xdir was prepended to $pic_object above. non_pic_object="$pic_object" func_append non_pic_objects " $non_pic_object" fi else # Only an error if not doing a dry-run. if $opt_dry_run; then # Extract subdirectory from the argument. func_dirname "$arg" "/" "" xdir="$func_dirname_result" func_lo2o "$arg" pic_object=$xdir$objdir/$func_lo2o_result non_pic_object=$xdir$func_lo2o_result func_append libobjs " $pic_object" func_append non_pic_objects " $non_pic_object" else func_fatal_error "\`$arg' is not a valid libtool object" fi fi done else func_fatal_error "link input file \`$arg' does not exist" fi arg=$save_arg prev= continue ;; precious_regex) precious_files_regex="$arg" prev= continue ;; release) release="-$arg" prev= continue ;; rpath | xrpath) # We need an absolute path. case $arg in [\\/]* | [A-Za-z]:[\\/]*) ;; *) func_fatal_error "only absolute run-paths are allowed" ;; esac if test "$prev" = rpath; then case "$rpath " in *" $arg "*) ;; *) func_append rpath " $arg" ;; esac else case "$xrpath " in *" $arg "*) ;; *) func_append xrpath " $arg" ;; esac fi prev= continue ;; shrext) shrext_cmds="$arg" prev= continue ;; weak) func_append weak_libs " $arg" prev= continue ;; xcclinker) func_append linker_flags " $qarg" func_append compiler_flags " $qarg" prev= func_append compile_command " $qarg" func_append finalize_command " $qarg" continue ;; xcompiler) func_append compiler_flags " $qarg" prev= func_append compile_command " $qarg" func_append finalize_command " $qarg" continue ;; xlinker) func_append linker_flags " $qarg" func_append compiler_flags " $wl$qarg" prev= func_append compile_command " $wl$qarg" func_append finalize_command " $wl$qarg" continue ;; *) eval "$prev=\"\$arg\"" prev= continue ;; esac fi # test -n "$prev" prevarg="$arg" case $arg in -all-static) if test -n "$link_static_flag"; then # See comment for -static flag below, for more details. func_append compile_command " $link_static_flag" func_append finalize_command " $link_static_flag" fi continue ;; -allow-undefined) # FIXME: remove this flag sometime in the future. func_fatal_error "\`-allow-undefined' must not be used because it is the default" ;; -avoid-version) avoid_version=yes continue ;; -bindir) prev=bindir continue ;; -dlopen) prev=dlfiles continue ;; -dlpreopen) prev=dlprefiles continue ;; -export-dynamic) export_dynamic=yes continue ;; -export-symbols | -export-symbols-regex) if test -n "$export_symbols" || test -n "$export_symbols_regex"; then func_fatal_error "more than one -exported-symbols argument is not allowed" fi if test "X$arg" = "X-export-symbols"; then prev=expsyms else prev=expsyms_regex fi continue ;; -framework) prev=framework continue ;; -inst-prefix-dir) prev=inst_prefix continue ;; # The native IRIX linker understands -LANG:*, -LIST:* and -LNO:* # so, if we see these flags be careful not to treat them like -L -L[A-Z][A-Z]*:*) case $with_gcc/$host in no/*-*-irix* | /*-*-irix*) func_append compile_command " $arg" func_append finalize_command " $arg" ;; esac continue ;; -L*) func_stripname "-L" '' "$arg" if test -z "$func_stripname_result"; then if test "$#" -gt 0; then func_fatal_error "require no space between \`-L' and \`$1'" else func_fatal_error "need path for \`-L' option" fi fi func_resolve_sysroot "$func_stripname_result" dir=$func_resolve_sysroot_result # We need an absolute path. case $dir in [\\/]* | [A-Za-z]:[\\/]*) ;; *) absdir=`cd "$dir" && pwd` test -z "$absdir" && \ func_fatal_error "cannot determine absolute directory name of \`$dir'" dir="$absdir" ;; esac case "$deplibs " in *" -L$dir "* | *" $arg "*) # Will only happen for absolute or sysroot arguments ;; *) # Preserve sysroot, but never include relative directories case $dir in [\\/]* | [A-Za-z]:[\\/]* | =*) func_append deplibs " $arg" ;; *) func_append deplibs " -L$dir" ;; esac func_append lib_search_path " $dir" ;; esac case $host in *-*-cygwin* | *-*-mingw* | *-*-pw32* | *-*-os2* | *-cegcc*) testbindir=`$ECHO "$dir" | $SED 's*/lib$*/bin*'` case :$dllsearchpath: in *":$dir:"*) ;; ::) dllsearchpath=$dir;; *) func_append dllsearchpath ":$dir";; esac case :$dllsearchpath: in *":$testbindir:"*) ;; ::) dllsearchpath=$testbindir;; *) func_append dllsearchpath ":$testbindir";; esac ;; esac continue ;; -l*) if test "X$arg" = "X-lc" || test "X$arg" = "X-lm"; then case $host in *-*-cygwin* | *-*-mingw* | *-*-pw32* | *-*-beos* | *-cegcc* | *-*-haiku*) # These systems don't actually have a C or math library (as such) continue ;; *-*-os2*) # These systems don't actually have a C library (as such) test "X$arg" = "X-lc" && continue ;; *-*-openbsd* | *-*-freebsd* | *-*-dragonfly*) # Do not include libc due to us having libc/libc_r. test "X$arg" = "X-lc" && continue ;; *-*-rhapsody* | *-*-darwin1.[012]) # Rhapsody C and math libraries are in the System framework func_append deplibs " System.ltframework" continue ;; *-*-sco3.2v5* | *-*-sco5v6*) # Causes problems with __ctype test "X$arg" = "X-lc" && continue ;; *-*-sysv4.2uw2* | *-*-sysv5* | *-*-unixware* | *-*-OpenUNIX*) # Compiler inserts libc in the correct place for threads to work test "X$arg" = "X-lc" && continue ;; esac elif test "X$arg" = "X-lc_r"; then case $host in *-*-openbsd* | *-*-freebsd* | *-*-dragonfly*) # Do not include libc_r directly, use -pthread flag. continue ;; esac fi func_append deplibs " $arg" continue ;; -module) module=yes continue ;; # Tru64 UNIX uses -model [arg] to determine the layout of C++ # classes, name mangling, and exception handling. # Darwin uses the -arch flag to determine output architecture. -model|-arch|-isysroot|--sysroot) func_append compiler_flags " $arg" func_append compile_command " $arg" func_append finalize_command " $arg" prev=xcompiler continue ;; -mt|-mthreads|-kthread|-Kthread|-pthread|-pthreads|--thread-safe \ |-threads|-fopenmp|-openmp|-mp|-xopenmp|-omp|-qsmp=*) func_append compiler_flags " $arg" func_append compile_command " $arg" func_append finalize_command " $arg" case "$new_inherited_linker_flags " in *" $arg "*) ;; * ) func_append new_inherited_linker_flags " $arg" ;; esac continue ;; -multi_module) single_module="${wl}-multi_module" continue ;; -no-fast-install) fast_install=no continue ;; -no-install) case $host in *-*-cygwin* | *-*-mingw* | *-*-pw32* | *-*-os2* | *-*-darwin* | *-cegcc*) # The PATH hackery in wrapper scripts is required on Windows # and Darwin in order for the loader to find any dlls it needs. func_warning "\`-no-install' is ignored for $host" func_warning "assuming \`-no-fast-install' instead" fast_install=no ;; *) no_install=yes ;; esac continue ;; -no-undefined) allow_undefined=no continue ;; -objectlist) prev=objectlist continue ;; -o) prev=output ;; -precious-files-regex) prev=precious_regex continue ;; -release) prev=release continue ;; -rpath) prev=rpath continue ;; -R) prev=xrpath continue ;; -R*) func_stripname '-R' '' "$arg" dir=$func_stripname_result # We need an absolute path. case $dir in [\\/]* | [A-Za-z]:[\\/]*) ;; =*) func_stripname '=' '' "$dir" dir=$lt_sysroot$func_stripname_result ;; *) func_fatal_error "only absolute run-paths are allowed" ;; esac case "$xrpath " in *" $dir "*) ;; *) func_append xrpath " $dir" ;; esac continue ;; -shared) # The effects of -shared are defined in a previous loop. continue ;; -shrext) prev=shrext continue ;; -static | -static-libtool-libs) # The effects of -static are defined in a previous loop. # We used to do the same as -all-static on platforms that # didn't have a PIC flag, but the assumption that the effects # would be equivalent was wrong. It would break on at least # Digital Unix and AIX. continue ;; -thread-safe) thread_safe=yes continue ;; -version-info) prev=vinfo continue ;; -version-number) prev=vinfo vinfo_number=yes continue ;; -weak) prev=weak continue ;; -Wc,*) func_stripname '-Wc,' '' "$arg" args=$func_stripname_result arg= save_ifs="$IFS"; IFS=',' for flag in $args; do IFS="$save_ifs" func_quote_for_eval "$flag" func_append arg " $func_quote_for_eval_result" func_append compiler_flags " $func_quote_for_eval_result" done IFS="$save_ifs" func_stripname ' ' '' "$arg" arg=$func_stripname_result ;; -Wl,*) func_stripname '-Wl,' '' "$arg" args=$func_stripname_result arg= save_ifs="$IFS"; IFS=',' for flag in $args; do IFS="$save_ifs" func_quote_for_eval "$flag" func_append arg " $wl$func_quote_for_eval_result" func_append compiler_flags " $wl$func_quote_for_eval_result" func_append linker_flags " $func_quote_for_eval_result" done IFS="$save_ifs" func_stripname ' ' '' "$arg" arg=$func_stripname_result ;; -Xcompiler) prev=xcompiler continue ;; -Xlinker) prev=xlinker continue ;; -XCClinker) prev=xcclinker continue ;; # -msg_* for osf cc -msg_*) func_quote_for_eval "$arg" arg="$func_quote_for_eval_result" ;; # Flags to be passed through unchanged, with rationale: # -64, -mips[0-9] enable 64-bit mode for the SGI compiler # -r[0-9][0-9]* specify processor for the SGI compiler # -xarch=*, -xtarget=* enable 64-bit mode for the Sun compiler # +DA*, +DD* enable 64-bit mode for the HP compiler # -q* compiler args for the IBM compiler # -m*, -t[45]*, -txscale* architecture-specific flags for GCC # -F/path path to uninstalled frameworks, gcc on darwin # -p, -pg, --coverage, -fprofile-* profiling flags for GCC # @file GCC response files # -tp=* Portland pgcc target processor selection # --sysroot=* for sysroot support # -O*, -flto*, -fwhopr*, -fuse-linker-plugin GCC link-time optimization -64|-mips[0-9]|-r[0-9][0-9]*|-xarch=*|-xtarget=*|+DA*|+DD*|-q*|-m*| \ -t[45]*|-txscale*|-p|-pg|--coverage|-fprofile-*|-F*|@*|-tp=*|--sysroot=*| \ -O*|-flto*|-fwhopr*|-fuse-linker-plugin) func_quote_for_eval "$arg" arg="$func_quote_for_eval_result" func_append compile_command " $arg" func_append finalize_command " $arg" func_append compiler_flags " $arg" continue ;; # Some other compiler flag. -* | +*) func_quote_for_eval "$arg" arg="$func_quote_for_eval_result" ;; *.$objext) # A standard object. func_append objs " $arg" ;; *.lo) # A libtool-controlled object. # Check to see that this really is a libtool object. if func_lalib_unsafe_p "$arg"; then pic_object= non_pic_object= # Read the .lo file func_source "$arg" if test -z "$pic_object" || test -z "$non_pic_object" || test "$pic_object" = none && test "$non_pic_object" = none; then func_fatal_error "cannot find name of object for \`$arg'" fi # Extract subdirectory from the argument. func_dirname "$arg" "/" "" xdir="$func_dirname_result" if test "$pic_object" != none; then # Prepend the subdirectory the object is found in. pic_object="$xdir$pic_object" if test "$prev" = dlfiles; then if test "$build_libtool_libs" = yes && test "$dlopen_support" = yes; then func_append dlfiles " $pic_object" prev= continue else # If libtool objects are unsupported, then we need to preload. prev=dlprefiles fi fi # CHECK ME: I think I busted this. -Ossama if test "$prev" = dlprefiles; then # Preload the old-style object. func_append dlprefiles " $pic_object" prev= fi # A PIC object. func_append libobjs " $pic_object" arg="$pic_object" fi # Non-PIC object. if test "$non_pic_object" != none; then # Prepend the subdirectory the object is found in. non_pic_object="$xdir$non_pic_object" # A standard non-PIC object func_append non_pic_objects " $non_pic_object" if test -z "$pic_object" || test "$pic_object" = none ; then arg="$non_pic_object" fi else # If the PIC object exists, use it instead. # $xdir was prepended to $pic_object above. non_pic_object="$pic_object" func_append non_pic_objects " $non_pic_object" fi else # Only an error if not doing a dry-run. if $opt_dry_run; then # Extract subdirectory from the argument. func_dirname "$arg" "/" "" xdir="$func_dirname_result" func_lo2o "$arg" pic_object=$xdir$objdir/$func_lo2o_result non_pic_object=$xdir$func_lo2o_result func_append libobjs " $pic_object" func_append non_pic_objects " $non_pic_object" else func_fatal_error "\`$arg' is not a valid libtool object" fi fi ;; *.$libext) # An archive. func_append deplibs " $arg" func_append old_deplibs " $arg" continue ;; *.la) # A libtool-controlled library. func_resolve_sysroot "$arg" if test "$prev" = dlfiles; then # This library was specified with -dlopen. func_append dlfiles " $func_resolve_sysroot_result" prev= elif test "$prev" = dlprefiles; then # The library was specified with -dlpreopen. func_append dlprefiles " $func_resolve_sysroot_result" prev= else func_append deplibs " $func_resolve_sysroot_result" fi continue ;; # Some other compiler argument. *) # Unknown arguments in both finalize_command and compile_command need # to be aesthetically quoted because they are evaled later. func_quote_for_eval "$arg" arg="$func_quote_for_eval_result" ;; esac # arg # Now actually substitute the argument into the commands. if test -n "$arg"; then func_append compile_command " $arg" func_append finalize_command " $arg" fi done # argument parsing loop test -n "$prev" && \ func_fatal_help "the \`$prevarg' option requires an argument" if test "$export_dynamic" = yes && test -n "$export_dynamic_flag_spec"; then eval arg=\"$export_dynamic_flag_spec\" func_append compile_command " $arg" func_append finalize_command " $arg" fi oldlibs= # calculate the name of the file, without its directory func_basename "$output" outputname="$func_basename_result" libobjs_save="$libobjs" if test -n "$shlibpath_var"; then # get the directories listed in $shlibpath_var eval shlib_search_path=\`\$ECHO \"\${$shlibpath_var}\" \| \$SED \'s/:/ /g\'\` else shlib_search_path= fi eval sys_lib_search_path=\"$sys_lib_search_path_spec\" eval sys_lib_dlsearch_path=\"$sys_lib_dlsearch_path_spec\" func_dirname "$output" "/" "" output_objdir="$func_dirname_result$objdir" func_to_tool_file "$output_objdir/" tool_output_objdir=$func_to_tool_file_result # Create the object directory. func_mkdir_p "$output_objdir" # Determine the type of output case $output in "") func_fatal_help "you must specify an output file" ;; *.$libext) linkmode=oldlib ;; *.lo | *.$objext) linkmode=obj ;; *.la) linkmode=lib ;; *) linkmode=prog ;; # Anything else should be a program. esac specialdeplibs= libs= # Find all interdependent deplibs by searching for libraries # that are linked more than once (e.g. -la -lb -la) for deplib in $deplibs; do if $opt_preserve_dup_deps ; then case "$libs " in *" $deplib "*) func_append specialdeplibs " $deplib" ;; esac fi func_append libs " $deplib" done if test "$linkmode" = lib; then libs="$predeps $libs $compiler_lib_search_path $postdeps" # Compute libraries that are listed more than once in $predeps # $postdeps and mark them as special (i.e., whose duplicates are # not to be eliminated). pre_post_deps= if $opt_duplicate_compiler_generated_deps; then for pre_post_dep in $predeps $postdeps; do case "$pre_post_deps " in *" $pre_post_dep "*) func_append specialdeplibs " $pre_post_deps" ;; esac func_append pre_post_deps " $pre_post_dep" done fi pre_post_deps= fi deplibs= newdependency_libs= newlib_search_path= need_relink=no # whether we're linking any uninstalled libtool libraries notinst_deplibs= # not-installed libtool libraries notinst_path= # paths that contain not-installed libtool libraries case $linkmode in lib) passes="conv dlpreopen link" for file in $dlfiles $dlprefiles; do case $file in *.la) ;; *) func_fatal_help "libraries can \`-dlopen' only libtool libraries: $file" ;; esac done ;; prog) compile_deplibs= finalize_deplibs= alldeplibs=no newdlfiles= newdlprefiles= passes="conv scan dlopen dlpreopen link" ;; *) passes="conv" ;; esac for pass in $passes; do # The preopen pass in lib mode reverses $deplibs; put it back here # so that -L comes before libs that need it for instance... if test "$linkmode,$pass" = "lib,link"; then ## FIXME: Find the place where the list is rebuilt in the wrong ## order, and fix it there properly tmp_deplibs= for deplib in $deplibs; do tmp_deplibs="$deplib $tmp_deplibs" done deplibs="$tmp_deplibs" fi if test "$linkmode,$pass" = "lib,link" || test "$linkmode,$pass" = "prog,scan"; then libs="$deplibs" deplibs= fi if test "$linkmode" = prog; then case $pass in dlopen) libs="$dlfiles" ;; dlpreopen) libs="$dlprefiles" ;; link) libs="$deplibs %DEPLIBS% $dependency_libs" ;; esac fi if test "$linkmode,$pass" = "lib,dlpreopen"; then # Collect and forward deplibs of preopened libtool libs for lib in $dlprefiles; do # Ignore non-libtool-libs dependency_libs= func_resolve_sysroot "$lib" case $lib in *.la) func_source "$func_resolve_sysroot_result" ;; esac # Collect preopened libtool deplibs, except any this library # has declared as weak libs for deplib in $dependency_libs; do func_basename "$deplib" deplib_base=$func_basename_result case " $weak_libs " in *" $deplib_base "*) ;; *) func_append deplibs " $deplib" ;; esac done done libs="$dlprefiles" fi if test "$pass" = dlopen; then # Collect dlpreopened libraries save_deplibs="$deplibs" deplibs= fi for deplib in $libs; do lib= found=no case $deplib in -mt|-mthreads|-kthread|-Kthread|-pthread|-pthreads|--thread-safe \ |-threads|-fopenmp|-openmp|-mp|-xopenmp|-omp|-qsmp=*) if test "$linkmode,$pass" = "prog,link"; then compile_deplibs="$deplib $compile_deplibs" finalize_deplibs="$deplib $finalize_deplibs" else func_append compiler_flags " $deplib" if test "$linkmode" = lib ; then case "$new_inherited_linker_flags " in *" $deplib "*) ;; * ) func_append new_inherited_linker_flags " $deplib" ;; esac fi fi continue ;; -l*) if test "$linkmode" != lib && test "$linkmode" != prog; then func_warning "\`-l' is ignored for archives/objects" continue fi func_stripname '-l' '' "$deplib" name=$func_stripname_result if test "$linkmode" = lib; then searchdirs="$newlib_search_path $lib_search_path $compiler_lib_search_dirs $sys_lib_search_path $shlib_search_path" else searchdirs="$newlib_search_path $lib_search_path $sys_lib_search_path $shlib_search_path" fi for searchdir in $searchdirs; do for search_ext in .la $std_shrext .so .a; do # Search the libtool library lib="$searchdir/lib${name}${search_ext}" if test -f "$lib"; then if test "$search_ext" = ".la"; then found=yes else found=no fi break 2 fi done done if test "$found" != yes; then # deplib doesn't seem to be a libtool library if test "$linkmode,$pass" = "prog,link"; then compile_deplibs="$deplib $compile_deplibs" finalize_deplibs="$deplib $finalize_deplibs" else deplibs="$deplib $deplibs" test "$linkmode" = lib && newdependency_libs="$deplib $newdependency_libs" fi continue else # deplib is a libtool library # If $allow_libtool_libs_with_static_runtimes && $deplib is a stdlib, # We need to do some special things here, and not later. if test "X$allow_libtool_libs_with_static_runtimes" = "Xyes" ; then case " $predeps $postdeps " in *" $deplib "*) if func_lalib_p "$lib"; then library_names= old_library= func_source "$lib" for l in $old_library $library_names; do ll="$l" done if test "X$ll" = "X$old_library" ; then # only static version available found=no func_dirname "$lib" "" "." ladir="$func_dirname_result" lib=$ladir/$old_library if test "$linkmode,$pass" = "prog,link"; then compile_deplibs="$deplib $compile_deplibs" finalize_deplibs="$deplib $finalize_deplibs" else deplibs="$deplib $deplibs" test "$linkmode" = lib && newdependency_libs="$deplib $newdependency_libs" fi continue fi fi ;; *) ;; esac fi fi ;; # -l *.ltframework) if test "$linkmode,$pass" = "prog,link"; then compile_deplibs="$deplib $compile_deplibs" finalize_deplibs="$deplib $finalize_deplibs" else deplibs="$deplib $deplibs" if test "$linkmode" = lib ; then case "$new_inherited_linker_flags " in *" $deplib "*) ;; * ) func_append new_inherited_linker_flags " $deplib" ;; esac fi fi continue ;; -L*) case $linkmode in lib) deplibs="$deplib $deplibs" test "$pass" = conv && continue newdependency_libs="$deplib $newdependency_libs" func_stripname '-L' '' "$deplib" func_resolve_sysroot "$func_stripname_result" func_append newlib_search_path " $func_resolve_sysroot_result" ;; prog) if test "$pass" = conv; then deplibs="$deplib $deplibs" continue fi if test "$pass" = scan; then deplibs="$deplib $deplibs" else compile_deplibs="$deplib $compile_deplibs" finalize_deplibs="$deplib $finalize_deplibs" fi func_stripname '-L' '' "$deplib" func_resolve_sysroot "$func_stripname_result" func_append newlib_search_path " $func_resolve_sysroot_result" ;; *) func_warning "\`-L' is ignored for archives/objects" ;; esac # linkmode continue ;; # -L -R*) if test "$pass" = link; then func_stripname '-R' '' "$deplib" func_resolve_sysroot "$func_stripname_result" dir=$func_resolve_sysroot_result # Make sure the xrpath contains only unique directories. case "$xrpath " in *" $dir "*) ;; *) func_append xrpath " $dir" ;; esac fi deplibs="$deplib $deplibs" continue ;; *.la) func_resolve_sysroot "$deplib" lib=$func_resolve_sysroot_result ;; *.$libext) if test "$pass" = conv; then deplibs="$deplib $deplibs" continue fi case $linkmode in lib) # Linking convenience modules into shared libraries is allowed, # but linking other static libraries is non-portable. case " $dlpreconveniencelibs " in *" $deplib "*) ;; *) valid_a_lib=no case $deplibs_check_method in match_pattern*) set dummy $deplibs_check_method; shift match_pattern_regex=`expr "$deplibs_check_method" : "$1 \(.*\)"` if eval "\$ECHO \"$deplib\"" 2>/dev/null | $SED 10q \ | $EGREP "$match_pattern_regex" > /dev/null; then valid_a_lib=yes fi ;; pass_all) valid_a_lib=yes ;; esac if test "$valid_a_lib" != yes; then echo $ECHO "*** Warning: Trying to link with static lib archive $deplib." echo "*** I have the capability to make that library automatically link in when" echo "*** you link to this library. But I can only do this if you have a" echo "*** shared version of the library, which you do not appear to have" echo "*** because the file extensions .$libext of this argument makes me believe" echo "*** that it is just a static archive that I should not use here." else echo $ECHO "*** Warning: Linking the shared library $output against the" $ECHO "*** static library $deplib is not portable!" deplibs="$deplib $deplibs" fi ;; esac continue ;; prog) if test "$pass" != link; then deplibs="$deplib $deplibs" else compile_deplibs="$deplib $compile_deplibs" finalize_deplibs="$deplib $finalize_deplibs" fi continue ;; esac # linkmode ;; # *.$libext *.lo | *.$objext) if test "$pass" = conv; then deplibs="$deplib $deplibs" elif test "$linkmode" = prog; then if test "$pass" = dlpreopen || test "$dlopen_support" != yes || test "$build_libtool_libs" = no; then # If there is no dlopen support or we're linking statically, # we need to preload. func_append newdlprefiles " $deplib" compile_deplibs="$deplib $compile_deplibs" finalize_deplibs="$deplib $finalize_deplibs" else func_append newdlfiles " $deplib" fi fi continue ;; %DEPLIBS%) alldeplibs=yes continue ;; esac # case $deplib if test "$found" = yes || test -f "$lib"; then : else func_fatal_error "cannot find the library \`$lib' or unhandled argument \`$deplib'" fi # Check to see that this really is a libtool archive. func_lalib_unsafe_p "$lib" \ || func_fatal_error "\`$lib' is not a valid libtool archive" func_dirname "$lib" "" "." ladir="$func_dirname_result" dlname= dlopen= dlpreopen= libdir= library_names= old_library= inherited_linker_flags= # If the library was installed with an old release of libtool, # it will not redefine variables installed, or shouldnotlink installed=yes shouldnotlink=no avoidtemprpath= # Read the .la file func_source "$lib" # Convert "-framework foo" to "foo.ltframework" if test -n "$inherited_linker_flags"; then tmp_inherited_linker_flags=`$ECHO "$inherited_linker_flags" | $SED 's/-framework \([^ $]*\)/\1.ltframework/g'` for tmp_inherited_linker_flag in $tmp_inherited_linker_flags; do case " $new_inherited_linker_flags " in *" $tmp_inherited_linker_flag "*) ;; *) func_append new_inherited_linker_flags " $tmp_inherited_linker_flag";; esac done fi dependency_libs=`$ECHO " $dependency_libs" | $SED 's% \([^ $]*\).ltframework% -framework \1%g'` if test "$linkmode,$pass" = "lib,link" || test "$linkmode,$pass" = "prog,scan" || { test "$linkmode" != prog && test "$linkmode" != lib; }; then test -n "$dlopen" && func_append dlfiles " $dlopen" test -n "$dlpreopen" && func_append dlprefiles " $dlpreopen" fi if test "$pass" = conv; then # Only check for convenience libraries deplibs="$lib $deplibs" if test -z "$libdir"; then if test -z "$old_library"; then func_fatal_error "cannot find name of link library for \`$lib'" fi # It is a libtool convenience library, so add in its objects. func_append convenience " $ladir/$objdir/$old_library" func_append old_convenience " $ladir/$objdir/$old_library" elif test "$linkmode" != prog && test "$linkmode" != lib; then func_fatal_error "\`$lib' is not a convenience library" fi tmp_libs= for deplib in $dependency_libs; do deplibs="$deplib $deplibs" if $opt_preserve_dup_deps ; then case "$tmp_libs " in *" $deplib "*) func_append specialdeplibs " $deplib" ;; esac fi func_append tmp_libs " $deplib" done continue fi # $pass = conv # Get the name of the library we link against. linklib= if test -n "$old_library" && { test "$prefer_static_libs" = yes || test "$prefer_static_libs,$installed" = "built,no"; }; then linklib=$old_library else for l in $old_library $library_names; do linklib="$l" done fi if test -z "$linklib"; then func_fatal_error "cannot find name of link library for \`$lib'" fi # This library was specified with -dlopen. if test "$pass" = dlopen; then if test -z "$libdir"; then func_fatal_error "cannot -dlopen a convenience library: \`$lib'" fi if test -z "$dlname" || test "$dlopen_support" != yes || test "$build_libtool_libs" = no; then # If there is no dlname, no dlopen support or we're linking # statically, we need to preload. We also need to preload any # dependent libraries so libltdl's deplib preloader doesn't # bomb out in the load deplibs phase. func_append dlprefiles " $lib $dependency_libs" else func_append newdlfiles " $lib" fi continue fi # $pass = dlopen # We need an absolute path. case $ladir in [\\/]* | [A-Za-z]:[\\/]*) abs_ladir="$ladir" ;; *) abs_ladir=`cd "$ladir" && pwd` if test -z "$abs_ladir"; then func_warning "cannot determine absolute directory name of \`$ladir'" func_warning "passing it literally to the linker, although it might fail" abs_ladir="$ladir" fi ;; esac func_basename "$lib" laname="$func_basename_result" # Find the relevant object directory and library name. if test "X$installed" = Xyes; then if test ! -f "$lt_sysroot$libdir/$linklib" && test -f "$abs_ladir/$linklib"; then func_warning "library \`$lib' was moved." dir="$ladir" absdir="$abs_ladir" libdir="$abs_ladir" else dir="$lt_sysroot$libdir" absdir="$lt_sysroot$libdir" fi test "X$hardcode_automatic" = Xyes && avoidtemprpath=yes else if test ! -f "$ladir/$objdir/$linklib" && test -f "$abs_ladir/$linklib"; then dir="$ladir" absdir="$abs_ladir" # Remove this search path later func_append notinst_path " $abs_ladir" else dir="$ladir/$objdir" absdir="$abs_ladir/$objdir" # Remove this search path later func_append notinst_path " $abs_ladir" fi fi # $installed = yes func_stripname 'lib' '.la' "$laname" name=$func_stripname_result # This library was specified with -dlpreopen. if test "$pass" = dlpreopen; then if test -z "$libdir" && test "$linkmode" = prog; then func_fatal_error "only libraries may -dlpreopen a convenience library: \`$lib'" fi case "$host" in # special handling for platforms with PE-DLLs. *cygwin* | *mingw* | *cegcc* ) # Linker will automatically link against shared library if both # static and shared are present. Therefore, ensure we extract # symbols from the import library if a shared library is present # (otherwise, the dlopen module name will be incorrect). We do # this by putting the import library name into $newdlprefiles. # We recover the dlopen module name by 'saving' the la file # name in a special purpose variable, and (later) extracting the # dlname from the la file. if test -n "$dlname"; then func_tr_sh "$dir/$linklib" eval "libfile_$func_tr_sh_result=\$abs_ladir/\$laname" func_append newdlprefiles " $dir/$linklib" else func_append newdlprefiles " $dir/$old_library" # Keep a list of preopened convenience libraries to check # that they are being used correctly in the link pass. test -z "$libdir" && \ func_append dlpreconveniencelibs " $dir/$old_library" fi ;; * ) # Prefer using a static library (so that no silly _DYNAMIC symbols # are required to link). if test -n "$old_library"; then func_append newdlprefiles " $dir/$old_library" # Keep a list of preopened convenience libraries to check # that they are being used correctly in the link pass. test -z "$libdir" && \ func_append dlpreconveniencelibs " $dir/$old_library" # Otherwise, use the dlname, so that lt_dlopen finds it. elif test -n "$dlname"; then func_append newdlprefiles " $dir/$dlname" else func_append newdlprefiles " $dir/$linklib" fi ;; esac fi # $pass = dlpreopen if test -z "$libdir"; then # Link the convenience library if test "$linkmode" = lib; then deplibs="$dir/$old_library $deplibs" elif test "$linkmode,$pass" = "prog,link"; then compile_deplibs="$dir/$old_library $compile_deplibs" finalize_deplibs="$dir/$old_library $finalize_deplibs" else deplibs="$lib $deplibs" # used for prog,scan pass fi continue fi if test "$linkmode" = prog && test "$pass" != link; then func_append newlib_search_path " $ladir" deplibs="$lib $deplibs" linkalldeplibs=no if test "$link_all_deplibs" != no || test -z "$library_names" || test "$build_libtool_libs" = no; then linkalldeplibs=yes fi tmp_libs= for deplib in $dependency_libs; do case $deplib in -L*) func_stripname '-L' '' "$deplib" func_resolve_sysroot "$func_stripname_result" func_append newlib_search_path " $func_resolve_sysroot_result" ;; esac # Need to link against all dependency_libs? if test "$linkalldeplibs" = yes; then deplibs="$deplib $deplibs" else # Need to hardcode shared library paths # or/and link against static libraries newdependency_libs="$deplib $newdependency_libs" fi if $opt_preserve_dup_deps ; then case "$tmp_libs " in *" $deplib "*) func_append specialdeplibs " $deplib" ;; esac fi func_append tmp_libs " $deplib" done # for deplib continue fi # $linkmode = prog... if test "$linkmode,$pass" = "prog,link"; then if test -n "$library_names" && { { test "$prefer_static_libs" = no || test "$prefer_static_libs,$installed" = "built,yes"; } || test -z "$old_library"; }; then # We need to hardcode the library path if test -n "$shlibpath_var" && test -z "$avoidtemprpath" ; then # Make sure the rpath contains only unique directories. case "$temp_rpath:" in *"$absdir:"*) ;; *) func_append temp_rpath "$absdir:" ;; esac fi # Hardcode the library path. # Skip directories that are in the system default run-time # search path. case " $sys_lib_dlsearch_path " in *" $absdir "*) ;; *) case "$compile_rpath " in *" $absdir "*) ;; *) func_append compile_rpath " $absdir" ;; esac ;; esac case " $sys_lib_dlsearch_path " in *" $libdir "*) ;; *) case "$finalize_rpath " in *" $libdir "*) ;; *) func_append finalize_rpath " $libdir" ;; esac ;; esac fi # $linkmode,$pass = prog,link... if test "$alldeplibs" = yes && { test "$deplibs_check_method" = pass_all || { test "$build_libtool_libs" = yes && test -n "$library_names"; }; }; then # We only need to search for static libraries continue fi fi link_static=no # Whether the deplib will be linked statically use_static_libs=$prefer_static_libs if test "$use_static_libs" = built && test "$installed" = yes; then use_static_libs=no fi if test -n "$library_names" && { test "$use_static_libs" = no || test -z "$old_library"; }; then case $host in *cygwin* | *mingw* | *cegcc*) # No point in relinking DLLs because paths are not encoded func_append notinst_deplibs " $lib" need_relink=no ;; *) if test "$installed" = no; then func_append notinst_deplibs " $lib" need_relink=yes fi ;; esac # This is a shared library # Warn about portability, can't link against -module's on some # systems (darwin). Don't bleat about dlopened modules though! dlopenmodule="" for dlpremoduletest in $dlprefiles; do if test "X$dlpremoduletest" = "X$lib"; then dlopenmodule="$dlpremoduletest" break fi done if test -z "$dlopenmodule" && test "$shouldnotlink" = yes && test "$pass" = link; then echo if test "$linkmode" = prog; then $ECHO "*** Warning: Linking the executable $output against the loadable module" else $ECHO "*** Warning: Linking the shared library $output against the loadable module" fi $ECHO "*** $linklib is not portable!" fi if test "$linkmode" = lib && test "$hardcode_into_libs" = yes; then # Hardcode the library path. # Skip directories that are in the system default run-time # search path. case " $sys_lib_dlsearch_path " in *" $absdir "*) ;; *) case "$compile_rpath " in *" $absdir "*) ;; *) func_append compile_rpath " $absdir" ;; esac ;; esac case " $sys_lib_dlsearch_path " in *" $libdir "*) ;; *) case "$finalize_rpath " in *" $libdir "*) ;; *) func_append finalize_rpath " $libdir" ;; esac ;; esac fi if test -n "$old_archive_from_expsyms_cmds"; then # figure out the soname set dummy $library_names shift realname="$1" shift libname=`eval "\\$ECHO \"$libname_spec\""` # use dlname if we got it. it's perfectly good, no? if test -n "$dlname"; then soname="$dlname" elif test -n "$soname_spec"; then # bleh windows case $host in *cygwin* | mingw* | *cegcc*) func_arith $current - $age major=$func_arith_result versuffix="-$major" ;; esac eval soname=\"$soname_spec\" else soname="$realname" fi # Make a new name for the extract_expsyms_cmds to use soroot="$soname" func_basename "$soroot" soname="$func_basename_result" func_stripname 'lib' '.dll' "$soname" newlib=libimp-$func_stripname_result.a # If the library has no export list, then create one now if test -f "$output_objdir/$soname-def"; then : else func_verbose "extracting exported symbol list from \`$soname'" func_execute_cmds "$extract_expsyms_cmds" 'exit $?' fi # Create $newlib if test -f "$output_objdir/$newlib"; then :; else func_verbose "generating import library for \`$soname'" func_execute_cmds "$old_archive_from_expsyms_cmds" 'exit $?' fi # make sure the library variables are pointing to the new library dir=$output_objdir linklib=$newlib fi # test -n "$old_archive_from_expsyms_cmds" if test "$linkmode" = prog || test "$opt_mode" != relink; then add_shlibpath= add_dir= add= lib_linked=yes case $hardcode_action in immediate | unsupported) if test "$hardcode_direct" = no; then add="$dir/$linklib" case $host in *-*-sco3.2v5.0.[024]*) add_dir="-L$dir" ;; *-*-sysv4*uw2*) add_dir="-L$dir" ;; *-*-sysv5OpenUNIX* | *-*-sysv5UnixWare7.[01].[10]* | \ *-*-unixware7*) add_dir="-L$dir" ;; *-*-darwin* ) # if the lib is a (non-dlopened) module then we can not # link against it, someone is ignoring the earlier warnings if /usr/bin/file -L $add 2> /dev/null | $GREP ": [^:]* bundle" >/dev/null ; then if test "X$dlopenmodule" != "X$lib"; then $ECHO "*** Warning: lib $linklib is a module, not a shared library" if test -z "$old_library" ; then echo echo "*** And there doesn't seem to be a static archive available" echo "*** The link will probably fail, sorry" else add="$dir/$old_library" fi elif test -n "$old_library"; then add="$dir/$old_library" fi fi esac elif test "$hardcode_minus_L" = no; then case $host in *-*-sunos*) add_shlibpath="$dir" ;; esac add_dir="-L$dir" add="-l$name" elif test "$hardcode_shlibpath_var" = no; then add_shlibpath="$dir" add="-l$name" else lib_linked=no fi ;; relink) if test "$hardcode_direct" = yes && test "$hardcode_direct_absolute" = no; then add="$dir/$linklib" elif test "$hardcode_minus_L" = yes; then add_dir="-L$absdir" # Try looking first in the location we're being installed to. if test -n "$inst_prefix_dir"; then case $libdir in [\\/]*) func_append add_dir " -L$inst_prefix_dir$libdir" ;; esac fi add="-l$name" elif test "$hardcode_shlibpath_var" = yes; then add_shlibpath="$dir" add="-l$name" else lib_linked=no fi ;; *) lib_linked=no ;; esac if test "$lib_linked" != yes; then func_fatal_configuration "unsupported hardcode properties" fi if test -n "$add_shlibpath"; then case :$compile_shlibpath: in *":$add_shlibpath:"*) ;; *) func_append compile_shlibpath "$add_shlibpath:" ;; esac fi if test "$linkmode" = prog; then test -n "$add_dir" && compile_deplibs="$add_dir $compile_deplibs" test -n "$add" && compile_deplibs="$add $compile_deplibs" else test -n "$add_dir" && deplibs="$add_dir $deplibs" test -n "$add" && deplibs="$add $deplibs" if test "$hardcode_direct" != yes && test "$hardcode_minus_L" != yes && test "$hardcode_shlibpath_var" = yes; then case :$finalize_shlibpath: in *":$libdir:"*) ;; *) func_append finalize_shlibpath "$libdir:" ;; esac fi fi fi if test "$linkmode" = prog || test "$opt_mode" = relink; then add_shlibpath= add_dir= add= # Finalize command for both is simple: just hardcode it. if test "$hardcode_direct" = yes && test "$hardcode_direct_absolute" = no; then add="$libdir/$linklib" elif test "$hardcode_minus_L" = yes; then add_dir="-L$libdir" add="-l$name" elif test "$hardcode_shlibpath_var" = yes; then case :$finalize_shlibpath: in *":$libdir:"*) ;; *) func_append finalize_shlibpath "$libdir:" ;; esac add="-l$name" elif test "$hardcode_automatic" = yes; then if test -n "$inst_prefix_dir" && test -f "$inst_prefix_dir$libdir/$linklib" ; then add="$inst_prefix_dir$libdir/$linklib" else add="$libdir/$linklib" fi else # We cannot seem to hardcode it, guess we'll fake it. add_dir="-L$libdir" # Try looking first in the location we're being installed to. if test -n "$inst_prefix_dir"; then case $libdir in [\\/]*) func_append add_dir " -L$inst_prefix_dir$libdir" ;; esac fi add="-l$name" fi if test "$linkmode" = prog; then test -n "$add_dir" && finalize_deplibs="$add_dir $finalize_deplibs" test -n "$add" && finalize_deplibs="$add $finalize_deplibs" else test -n "$add_dir" && deplibs="$add_dir $deplibs" test -n "$add" && deplibs="$add $deplibs" fi fi elif test "$linkmode" = prog; then # Here we assume that one of hardcode_direct or hardcode_minus_L # is not unsupported. This is valid on all known static and # shared platforms. if test "$hardcode_direct" != unsupported; then test -n "$old_library" && linklib="$old_library" compile_deplibs="$dir/$linklib $compile_deplibs" finalize_deplibs="$dir/$linklib $finalize_deplibs" else compile_deplibs="-l$name -L$dir $compile_deplibs" finalize_deplibs="-l$name -L$dir $finalize_deplibs" fi elif test "$build_libtool_libs" = yes; then # Not a shared library if test "$deplibs_check_method" != pass_all; then # We're trying link a shared library against a static one # but the system doesn't support it. # Just print a warning and add the library to dependency_libs so # that the program can be linked against the static library. echo $ECHO "*** Warning: This system can not link to static lib archive $lib." echo "*** I have the capability to make that library automatically link in when" echo "*** you link to this library. But I can only do this if you have a" echo "*** shared version of the library, which you do not appear to have." if test "$module" = yes; then echo "*** But as you try to build a module library, libtool will still create " echo "*** a static module, that should work as long as the dlopening application" echo "*** is linked with the -dlopen flag to resolve symbols at runtime." if test -z "$global_symbol_pipe"; then echo echo "*** However, this would only work if libtool was able to extract symbol" echo "*** lists from a program, using \`nm' or equivalent, but libtool could" echo "*** not find such a program. So, this module is probably useless." echo "*** \`nm' from GNU binutils and a full rebuild may help." fi if test "$build_old_libs" = no; then build_libtool_libs=module build_old_libs=yes else build_libtool_libs=no fi fi else deplibs="$dir/$old_library $deplibs" link_static=yes fi fi # link shared/static library? if test "$linkmode" = lib; then if test -n "$dependency_libs" && { test "$hardcode_into_libs" != yes || test "$build_old_libs" = yes || test "$link_static" = yes; }; then # Extract -R from dependency_libs temp_deplibs= for libdir in $dependency_libs; do case $libdir in -R*) func_stripname '-R' '' "$libdir" temp_xrpath=$func_stripname_result case " $xrpath " in *" $temp_xrpath "*) ;; *) func_append xrpath " $temp_xrpath";; esac;; *) func_append temp_deplibs " $libdir";; esac done dependency_libs="$temp_deplibs" fi func_append newlib_search_path " $absdir" # Link against this library test "$link_static" = no && newdependency_libs="$abs_ladir/$laname $newdependency_libs" # ... and its dependency_libs tmp_libs= for deplib in $dependency_libs; do newdependency_libs="$deplib $newdependency_libs" case $deplib in -L*) func_stripname '-L' '' "$deplib" func_resolve_sysroot "$func_stripname_result";; *) func_resolve_sysroot "$deplib" ;; esac if $opt_preserve_dup_deps ; then case "$tmp_libs " in *" $func_resolve_sysroot_result "*) func_append specialdeplibs " $func_resolve_sysroot_result" ;; esac fi func_append tmp_libs " $func_resolve_sysroot_result" done if test "$link_all_deplibs" != no; then # Add the search paths of all dependency libraries for deplib in $dependency_libs; do path= case $deplib in -L*) path="$deplib" ;; *.la) func_resolve_sysroot "$deplib" deplib=$func_resolve_sysroot_result func_dirname "$deplib" "" "." dir=$func_dirname_result # We need an absolute path. case $dir in [\\/]* | [A-Za-z]:[\\/]*) absdir="$dir" ;; *) absdir=`cd "$dir" && pwd` if test -z "$absdir"; then func_warning "cannot determine absolute directory name of \`$dir'" absdir="$dir" fi ;; esac if $GREP "^installed=no" $deplib > /dev/null; then case $host in *-*-darwin*) depdepl= eval deplibrary_names=`${SED} -n -e 's/^library_names=\(.*\)$/\1/p' $deplib` if test -n "$deplibrary_names" ; then for tmp in $deplibrary_names ; do depdepl=$tmp done if test -f "$absdir/$objdir/$depdepl" ; then depdepl="$absdir/$objdir/$depdepl" darwin_install_name=`${OTOOL} -L $depdepl | awk '{if (NR == 2) {print $1;exit}}'` if test -z "$darwin_install_name"; then darwin_install_name=`${OTOOL64} -L $depdepl | awk '{if (NR == 2) {print $1;exit}}'` fi func_append compiler_flags " ${wl}-dylib_file ${wl}${darwin_install_name}:${depdepl}" func_append linker_flags " -dylib_file ${darwin_install_name}:${depdepl}" path= fi fi ;; *) path="-L$absdir/$objdir" ;; esac else eval libdir=`${SED} -n -e 's/^libdir=\(.*\)$/\1/p' $deplib` test -z "$libdir" && \ func_fatal_error "\`$deplib' is not a valid libtool archive" test "$absdir" != "$libdir" && \ func_warning "\`$deplib' seems to be moved" path="-L$absdir" fi ;; esac case " $deplibs " in *" $path "*) ;; *) deplibs="$path $deplibs" ;; esac done fi # link_all_deplibs != no fi # linkmode = lib done # for deplib in $libs if test "$pass" = link; then if test "$linkmode" = "prog"; then compile_deplibs="$new_inherited_linker_flags $compile_deplibs" finalize_deplibs="$new_inherited_linker_flags $finalize_deplibs" else compiler_flags="$compiler_flags "`$ECHO " $new_inherited_linker_flags" | $SED 's% \([^ $]*\).ltframework% -framework \1%g'` fi fi dependency_libs="$newdependency_libs" if test "$pass" = dlpreopen; then # Link the dlpreopened libraries before other libraries for deplib in $save_deplibs; do deplibs="$deplib $deplibs" done fi if test "$pass" != dlopen; then if test "$pass" != conv; then # Make sure lib_search_path contains only unique directories. lib_search_path= for dir in $newlib_search_path; do case "$lib_search_path " in *" $dir "*) ;; *) func_append lib_search_path " $dir" ;; esac done newlib_search_path= fi if test "$linkmode,$pass" != "prog,link"; then vars="deplibs" else vars="compile_deplibs finalize_deplibs" fi for var in $vars dependency_libs; do # Add libraries to $var in reverse order eval tmp_libs=\"\$$var\" new_libs= for deplib in $tmp_libs; do # FIXME: Pedantically, this is the right thing to do, so # that some nasty dependency loop isn't accidentally # broken: #new_libs="$deplib $new_libs" # Pragmatically, this seems to cause very few problems in # practice: case $deplib in -L*) new_libs="$deplib $new_libs" ;; -R*) ;; *) # And here is the reason: when a library appears more # than once as an explicit dependence of a library, or # is implicitly linked in more than once by the # compiler, it is considered special, and multiple # occurrences thereof are not removed. Compare this # with having the same library being listed as a # dependency of multiple other libraries: in this case, # we know (pedantically, we assume) the library does not # need to be listed more than once, so we keep only the # last copy. This is not always right, but it is rare # enough that we require users that really mean to play # such unportable linking tricks to link the library # using -Wl,-lname, so that libtool does not consider it # for duplicate removal. case " $specialdeplibs " in *" $deplib "*) new_libs="$deplib $new_libs" ;; *) case " $new_libs " in *" $deplib "*) ;; *) new_libs="$deplib $new_libs" ;; esac ;; esac ;; esac done tmp_libs= for deplib in $new_libs; do case $deplib in -L*) case " $tmp_libs " in *" $deplib "*) ;; *) func_append tmp_libs " $deplib" ;; esac ;; *) func_append tmp_libs " $deplib" ;; esac done eval $var=\"$tmp_libs\" done # for var fi # Last step: remove runtime libs from dependency_libs # (they stay in deplibs) tmp_libs= for i in $dependency_libs ; do case " $predeps $postdeps $compiler_lib_search_path " in *" $i "*) i="" ;; esac if test -n "$i" ; then func_append tmp_libs " $i" fi done dependency_libs=$tmp_libs done # for pass if test "$linkmode" = prog; then dlfiles="$newdlfiles" fi if test "$linkmode" = prog || test "$linkmode" = lib; then dlprefiles="$newdlprefiles" fi case $linkmode in oldlib) if test -n "$dlfiles$dlprefiles" || test "$dlself" != no; then func_warning "\`-dlopen' is ignored for archives" fi case " $deplibs" in *\ -l* | *\ -L*) func_warning "\`-l' and \`-L' are ignored for archives" ;; esac test -n "$rpath" && \ func_warning "\`-rpath' is ignored for archives" test -n "$xrpath" && \ func_warning "\`-R' is ignored for archives" test -n "$vinfo" && \ func_warning "\`-version-info/-version-number' is ignored for archives" test -n "$release" && \ func_warning "\`-release' is ignored for archives" test -n "$export_symbols$export_symbols_regex" && \ func_warning "\`-export-symbols' is ignored for archives" # Now set the variables for building old libraries. build_libtool_libs=no oldlibs="$output" func_append objs "$old_deplibs" ;; lib) # Make sure we only generate libraries of the form `libNAME.la'. case $outputname in lib*) func_stripname 'lib' '.la' "$outputname" name=$func_stripname_result eval shared_ext=\"$shrext_cmds\" eval libname=\"$libname_spec\" ;; *) test "$module" = no && \ func_fatal_help "libtool library \`$output' must begin with \`lib'" if test "$need_lib_prefix" != no; then # Add the "lib" prefix for modules if required func_stripname '' '.la' "$outputname" name=$func_stripname_result eval shared_ext=\"$shrext_cmds\" eval libname=\"$libname_spec\" else func_stripname '' '.la' "$outputname" libname=$func_stripname_result fi ;; esac if test -n "$objs"; then if test "$deplibs_check_method" != pass_all; then func_fatal_error "cannot build libtool library \`$output' from non-libtool objects on this host:$objs" else echo $ECHO "*** Warning: Linking the shared library $output against the non-libtool" $ECHO "*** objects $objs is not portable!" func_append libobjs " $objs" fi fi test "$dlself" != no && \ func_warning "\`-dlopen self' is ignored for libtool libraries" set dummy $rpath shift test "$#" -gt 1 && \ func_warning "ignoring multiple \`-rpath's for a libtool library" install_libdir="$1" oldlibs= if test -z "$rpath"; then if test "$build_libtool_libs" = yes; then # Building a libtool convenience library. # Some compilers have problems with a `.al' extension so # convenience libraries should have the same extension an # archive normally would. oldlibs="$output_objdir/$libname.$libext $oldlibs" build_libtool_libs=convenience build_old_libs=yes fi test -n "$vinfo" && \ func_warning "\`-version-info/-version-number' is ignored for convenience libraries" test -n "$release" && \ func_warning "\`-release' is ignored for convenience libraries" else # Parse the version information argument. save_ifs="$IFS"; IFS=':' set dummy $vinfo 0 0 0 shift IFS="$save_ifs" test -n "$7" && \ func_fatal_help "too many parameters to \`-version-info'" # convert absolute version numbers to libtool ages # this retains compatibility with .la files and attempts # to make the code below a bit more comprehensible case $vinfo_number in yes) number_major="$1" number_minor="$2" number_revision="$3" # # There are really only two kinds -- those that # use the current revision as the major version # and those that subtract age and use age as # a minor version. But, then there is irix # which has an extra 1 added just for fun # case $version_type in # correct linux to gnu/linux during the next big refactor darwin|linux|osf|windows|none) func_arith $number_major + $number_minor current=$func_arith_result age="$number_minor" revision="$number_revision" ;; freebsd-aout|freebsd-elf|qnx|sunos) current="$number_major" revision="$number_minor" age="0" ;; irix|nonstopux) func_arith $number_major + $number_minor current=$func_arith_result age="$number_minor" revision="$number_minor" lt_irix_increment=no ;; esac ;; no) current="$1" revision="$2" age="$3" ;; esac # Check that each of the things are valid numbers. case $current in 0|[1-9]|[1-9][0-9]|[1-9][0-9][0-9]|[1-9][0-9][0-9][0-9]|[1-9][0-9][0-9][0-9][0-9]) ;; *) func_error "CURRENT \`$current' must be a nonnegative integer" func_fatal_error "\`$vinfo' is not valid version information" ;; esac case $revision in 0|[1-9]|[1-9][0-9]|[1-9][0-9][0-9]|[1-9][0-9][0-9][0-9]|[1-9][0-9][0-9][0-9][0-9]) ;; *) func_error "REVISION \`$revision' must be a nonnegative integer" func_fatal_error "\`$vinfo' is not valid version information" ;; esac case $age in 0|[1-9]|[1-9][0-9]|[1-9][0-9][0-9]|[1-9][0-9][0-9][0-9]|[1-9][0-9][0-9][0-9][0-9]) ;; *) func_error "AGE \`$age' must be a nonnegative integer" func_fatal_error "\`$vinfo' is not valid version information" ;; esac if test "$age" -gt "$current"; then func_error "AGE \`$age' is greater than the current interface number \`$current'" func_fatal_error "\`$vinfo' is not valid version information" fi # Calculate the version variables. major= versuffix= verstring= case $version_type in none) ;; darwin) # Like Linux, but with the current version available in # verstring for coding it into the library header func_arith $current - $age major=.$func_arith_result versuffix="$major.$age.$revision" # Darwin ld doesn't like 0 for these options... func_arith $current + 1 minor_current=$func_arith_result xlcverstring="${wl}-compatibility_version ${wl}$minor_current ${wl}-current_version ${wl}$minor_current.$revision" verstring="-compatibility_version $minor_current -current_version $minor_current.$revision" ;; freebsd-aout) major=".$current" versuffix=".$current.$revision"; ;; freebsd-elf) major=".$current" versuffix=".$current" ;; irix | nonstopux) if test "X$lt_irix_increment" = "Xno"; then func_arith $current - $age else func_arith $current - $age + 1 fi major=$func_arith_result case $version_type in nonstopux) verstring_prefix=nonstopux ;; *) verstring_prefix=sgi ;; esac verstring="$verstring_prefix$major.$revision" # Add in all the interfaces that we are compatible with. loop=$revision while test "$loop" -ne 0; do func_arith $revision - $loop iface=$func_arith_result func_arith $loop - 1 loop=$func_arith_result verstring="$verstring_prefix$major.$iface:$verstring" done # Before this point, $major must not contain `.'. major=.$major versuffix="$major.$revision" ;; linux) # correct to gnu/linux during the next big refactor func_arith $current - $age major=.$func_arith_result versuffix="$major.$age.$revision" ;; osf) func_arith $current - $age major=.$func_arith_result versuffix=".$current.$age.$revision" verstring="$current.$age.$revision" # Add in all the interfaces that we are compatible with. loop=$age while test "$loop" -ne 0; do func_arith $current - $loop iface=$func_arith_result func_arith $loop - 1 loop=$func_arith_result verstring="$verstring:${iface}.0" done # Make executables depend on our current version. func_append verstring ":${current}.0" ;; qnx) major=".$current" versuffix=".$current" ;; sunos) major=".$current" versuffix=".$current.$revision" ;; windows) # Use '-' rather than '.', since we only want one # extension on DOS 8.3 filesystems. func_arith $current - $age major=$func_arith_result versuffix="-$major" ;; *) func_fatal_configuration "unknown library version type \`$version_type'" ;; esac # Clear the version info if we defaulted, and they specified a release. if test -z "$vinfo" && test -n "$release"; then major= case $version_type in darwin) # we can't check for "0.0" in archive_cmds due to quoting # problems, so we reset it completely verstring= ;; *) verstring="0.0" ;; esac if test "$need_version" = no; then versuffix= else versuffix=".0.0" fi fi # Remove version info from name if versioning should be avoided if test "$avoid_version" = yes && test "$need_version" = no; then major= versuffix= verstring="" fi # Check to see if the archive will have undefined symbols. if test "$allow_undefined" = yes; then if test "$allow_undefined_flag" = unsupported; then func_warning "undefined symbols not allowed in $host shared libraries" build_libtool_libs=no build_old_libs=yes fi else # Don't allow undefined symbols. allow_undefined_flag="$no_undefined_flag" fi fi func_generate_dlsyms "$libname" "$libname" "yes" func_append libobjs " $symfileobj" test "X$libobjs" = "X " && libobjs= if test "$opt_mode" != relink; then # Remove our outputs, but don't remove object files since they # may have been created when compiling PIC objects. removelist= tempremovelist=`$ECHO "$output_objdir/*"` for p in $tempremovelist; do case $p in *.$objext | *.gcno) ;; $output_objdir/$outputname | $output_objdir/$libname.* | $output_objdir/${libname}${release}.*) if test "X$precious_files_regex" != "X"; then if $ECHO "$p" | $EGREP -e "$precious_files_regex" >/dev/null 2>&1 then continue fi fi func_append removelist " $p" ;; *) ;; esac done test -n "$removelist" && \ func_show_eval "${RM}r \$removelist" fi # Now set the variables for building old libraries. if test "$build_old_libs" = yes && test "$build_libtool_libs" != convenience ; then func_append oldlibs " $output_objdir/$libname.$libext" # Transform .lo files to .o files. oldobjs="$objs "`$ECHO "$libobjs" | $SP2NL | $SED "/\.${libext}$/d; $lo2o" | $NL2SP` fi # Eliminate all temporary directories. #for path in $notinst_path; do # lib_search_path=`$ECHO "$lib_search_path " | $SED "s% $path % %g"` # deplibs=`$ECHO "$deplibs " | $SED "s% -L$path % %g"` # dependency_libs=`$ECHO "$dependency_libs " | $SED "s% -L$path % %g"` #done if test -n "$xrpath"; then # If the user specified any rpath flags, then add them. temp_xrpath= for libdir in $xrpath; do func_replace_sysroot "$libdir" func_append temp_xrpath " -R$func_replace_sysroot_result" case "$finalize_rpath " in *" $libdir "*) ;; *) func_append finalize_rpath " $libdir" ;; esac done if test "$hardcode_into_libs" != yes || test "$build_old_libs" = yes; then dependency_libs="$temp_xrpath $dependency_libs" fi fi # Make sure dlfiles contains only unique files that won't be dlpreopened old_dlfiles="$dlfiles" dlfiles= for lib in $old_dlfiles; do case " $dlprefiles $dlfiles " in *" $lib "*) ;; *) func_append dlfiles " $lib" ;; esac done # Make sure dlprefiles contains only unique files old_dlprefiles="$dlprefiles" dlprefiles= for lib in $old_dlprefiles; do case "$dlprefiles " in *" $lib "*) ;; *) func_append dlprefiles " $lib" ;; esac done if test "$build_libtool_libs" = yes; then if test -n "$rpath"; then case $host in *-*-cygwin* | *-*-mingw* | *-*-pw32* | *-*-os2* | *-*-beos* | *-cegcc* | *-*-haiku*) # these systems don't actually have a c library (as such)! ;; *-*-rhapsody* | *-*-darwin1.[012]) # Rhapsody C library is in the System framework func_append deplibs " System.ltframework" ;; *-*-netbsd*) # Don't link with libc until the a.out ld.so is fixed. ;; *-*-openbsd* | *-*-freebsd* | *-*-dragonfly*) # Do not include libc due to us having libc/libc_r. ;; *-*-sco3.2v5* | *-*-sco5v6*) # Causes problems with __ctype ;; *-*-sysv4.2uw2* | *-*-sysv5* | *-*-unixware* | *-*-OpenUNIX*) # Compiler inserts libc in the correct place for threads to work ;; *) # Add libc to deplibs on all other systems if necessary. if test "$build_libtool_need_lc" = "yes"; then func_append deplibs " -lc" fi ;; esac fi # Transform deplibs into only deplibs that can be linked in shared. name_save=$name libname_save=$libname release_save=$release versuffix_save=$versuffix major_save=$major # I'm not sure if I'm treating the release correctly. I think # release should show up in the -l (ie -lgmp5) so we don't want to # add it in twice. Is that correct? release="" versuffix="" major="" newdeplibs= droppeddeps=no case $deplibs_check_method in pass_all) # Don't check for shared/static. Everything works. # This might be a little naive. We might want to check # whether the library exists or not. But this is on # osf3 & osf4 and I'm not really sure... Just # implementing what was already the behavior. newdeplibs=$deplibs ;; test_compile) # This code stresses the "libraries are programs" paradigm to its # limits. Maybe even breaks it. We compile a program, linking it # against the deplibs as a proxy for the library. Then we can check # whether they linked in statically or dynamically with ldd. $opt_dry_run || $RM conftest.c cat > conftest.c </dev/null` $nocaseglob else potential_libs=`ls $i/$libnameglob[.-]* 2>/dev/null` fi for potent_lib in $potential_libs; do # Follow soft links. if ls -lLd "$potent_lib" 2>/dev/null | $GREP " -> " >/dev/null; then continue fi # The statement above tries to avoid entering an # endless loop below, in case of cyclic links. # We might still enter an endless loop, since a link # loop can be closed while we follow links, # but so what? potlib="$potent_lib" while test -h "$potlib" 2>/dev/null; do potliblink=`ls -ld $potlib | ${SED} 's/.* -> //'` case $potliblink in [\\/]* | [A-Za-z]:[\\/]*) potlib="$potliblink";; *) potlib=`$ECHO "$potlib" | $SED 's,[^/]*$,,'`"$potliblink";; esac done if eval $file_magic_cmd \"\$potlib\" 2>/dev/null | $SED -e 10q | $EGREP "$file_magic_regex" > /dev/null; then func_append newdeplibs " $a_deplib" a_deplib="" break 2 fi done done fi if test -n "$a_deplib" ; then droppeddeps=yes echo $ECHO "*** Warning: linker path does not have real file for library $a_deplib." echo "*** I have the capability to make that library automatically link in when" echo "*** you link to this library. But I can only do this if you have a" echo "*** shared version of the library, which you do not appear to have" echo "*** because I did check the linker path looking for a file starting" if test -z "$potlib" ; then $ECHO "*** with $libname but no candidates were found. (...for file magic test)" else $ECHO "*** with $libname and none of the candidates passed a file format test" $ECHO "*** using a file magic. 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But I can only do this if you have a" echo "*** shared version of the library, which you do not appear to have" echo "*** because I did check the linker path looking for a file starting" if test -z "$potlib" ; then $ECHO "*** with $libname but no candidates were found. (...for regex pattern test)" else $ECHO "*** with $libname and none of the candidates passed a file format test" $ECHO "*** using a regex pattern. Last file checked: $potlib" fi fi ;; *) # Add a -L argument. func_append newdeplibs " $a_deplib" ;; esac done # Gone through all deplibs. ;; none | unknown | *) newdeplibs="" tmp_deplibs=`$ECHO " $deplibs" | $SED 's/ -lc$//; s/ -[LR][^ ]*//g'` if test "X$allow_libtool_libs_with_static_runtimes" = "Xyes" ; then for i in $predeps $postdeps ; do # can't use Xsed below, because $i might contain '/' tmp_deplibs=`$ECHO " $tmp_deplibs" | $SED "s,$i,,"` done fi case $tmp_deplibs in *[!\ \ ]*) echo if test "X$deplibs_check_method" = "Xnone"; then echo "*** Warning: inter-library dependencies are not supported in this platform." else echo "*** Warning: inter-library dependencies are not known to be supported." fi echo "*** All declared inter-library dependencies are being dropped." droppeddeps=yes ;; esac ;; esac versuffix=$versuffix_save major=$major_save release=$release_save libname=$libname_save name=$name_save case $host in *-*-rhapsody* | *-*-darwin1.[012]) # On Rhapsody replace the C library with the System framework newdeplibs=`$ECHO " $newdeplibs" | $SED 's/ -lc / System.ltframework /'` ;; esac if test "$droppeddeps" = yes; then if test "$module" = yes; then echo echo "*** Warning: libtool could not satisfy all declared inter-library" $ECHO "*** dependencies of module $libname. Therefore, libtool will create" echo "*** a static module, that should work as long as the dlopening" echo "*** application is linked with the -dlopen flag." if test -z "$global_symbol_pipe"; then echo echo "*** However, this would only work if libtool was able to extract symbol" echo "*** lists from a program, using \`nm' or equivalent, but libtool could" echo "*** not find such a program. So, this module is probably useless." echo "*** \`nm' from GNU binutils and a full rebuild may help." fi if test "$build_old_libs" = no; then oldlibs="$output_objdir/$libname.$libext" build_libtool_libs=module build_old_libs=yes else build_libtool_libs=no fi else echo "*** The inter-library dependencies that have been dropped here will be" echo "*** automatically added whenever a program is linked with this library" echo "*** or is declared to -dlopen it." if test "$allow_undefined" = no; then echo echo "*** Since this library must not contain undefined symbols," echo "*** because either the platform does not support them or" echo "*** it was explicitly requested with -no-undefined," echo "*** libtool will only create a static version of it." if test "$build_old_libs" = no; then oldlibs="$output_objdir/$libname.$libext" build_libtool_libs=module build_old_libs=yes else build_libtool_libs=no fi fi fi fi # Done checking deplibs! deplibs=$newdeplibs fi # Time to change all our "foo.ltframework" stuff back to "-framework foo" case $host in *-*-darwin*) newdeplibs=`$ECHO " $newdeplibs" | $SED 's% \([^ $]*\).ltframework% -framework \1%g'` new_inherited_linker_flags=`$ECHO " $new_inherited_linker_flags" | $SED 's% \([^ $]*\).ltframework% -framework \1%g'` deplibs=`$ECHO " $deplibs" | $SED 's% \([^ $]*\).ltframework% -framework \1%g'` ;; esac # move library search paths that coincide with paths to not yet # installed libraries to the beginning of the library search list new_libs= for path in $notinst_path; do case " $new_libs " in *" -L$path/$objdir "*) ;; *) case " $deplibs " in *" -L$path/$objdir "*) func_append new_libs " -L$path/$objdir" ;; esac ;; esac done for deplib in $deplibs; do case $deplib in -L*) case " $new_libs " in *" $deplib "*) ;; *) func_append new_libs " $deplib" ;; esac ;; *) func_append new_libs " $deplib" ;; esac done deplibs="$new_libs" # All the library-specific variables (install_libdir is set above). library_names= old_library= dlname= # Test again, we may have decided not to build it any more if test "$build_libtool_libs" = yes; then # Remove ${wl} instances when linking with ld. # FIXME: should test the right _cmds variable. case $archive_cmds in *\$LD\ *) wl= ;; esac if test "$hardcode_into_libs" = yes; then # Hardcode the library paths hardcode_libdirs= dep_rpath= rpath="$finalize_rpath" test "$opt_mode" != relink && rpath="$compile_rpath$rpath" for libdir in $rpath; do if test -n "$hardcode_libdir_flag_spec"; then if test -n "$hardcode_libdir_separator"; then func_replace_sysroot "$libdir" libdir=$func_replace_sysroot_result if test -z "$hardcode_libdirs"; then hardcode_libdirs="$libdir" else # Just accumulate the unique libdirs. case $hardcode_libdir_separator$hardcode_libdirs$hardcode_libdir_separator in *"$hardcode_libdir_separator$libdir$hardcode_libdir_separator"*) ;; *) func_append hardcode_libdirs "$hardcode_libdir_separator$libdir" ;; esac fi else eval flag=\"$hardcode_libdir_flag_spec\" func_append dep_rpath " $flag" fi elif test -n "$runpath_var"; then case "$perm_rpath " in *" $libdir "*) ;; *) func_append perm_rpath " $libdir" ;; esac fi done # Substitute the hardcoded libdirs into the rpath. if test -n "$hardcode_libdir_separator" && test -n "$hardcode_libdirs"; then libdir="$hardcode_libdirs" eval "dep_rpath=\"$hardcode_libdir_flag_spec\"" fi if test -n "$runpath_var" && test -n "$perm_rpath"; then # We should set the runpath_var. rpath= for dir in $perm_rpath; do func_append rpath "$dir:" done eval "$runpath_var='$rpath\$$runpath_var'; export $runpath_var" fi test -n "$dep_rpath" && deplibs="$dep_rpath $deplibs" fi shlibpath="$finalize_shlibpath" test "$opt_mode" != relink && shlibpath="$compile_shlibpath$shlibpath" if test -n "$shlibpath"; then eval "$shlibpath_var='$shlibpath\$$shlibpath_var'; export $shlibpath_var" fi # Get the real and link names of the library. eval shared_ext=\"$shrext_cmds\" eval library_names=\"$library_names_spec\" set dummy $library_names shift realname="$1" shift if test -n "$soname_spec"; then eval soname=\"$soname_spec\" else soname="$realname" fi if test -z "$dlname"; then dlname=$soname fi lib="$output_objdir/$realname" linknames= for link do func_append linknames " $link" done # Use standard objects if they are pic test -z "$pic_flag" && libobjs=`$ECHO "$libobjs" | $SP2NL | $SED "$lo2o" | $NL2SP` test "X$libobjs" = "X " && libobjs= delfiles= if test -n "$export_symbols" && test -n "$include_expsyms"; then $opt_dry_run || cp "$export_symbols" "$output_objdir/$libname.uexp" export_symbols="$output_objdir/$libname.uexp" func_append delfiles " $export_symbols" fi orig_export_symbols= case $host_os in cygwin* | mingw* | cegcc*) if test -n "$export_symbols" && test -z "$export_symbols_regex"; then # exporting using user supplied symfile if test "x`$SED 1q $export_symbols`" != xEXPORTS; then # and it's NOT already a .def file. Must figure out # which of the given symbols are data symbols and tag # them as such. So, trigger use of export_symbols_cmds. # export_symbols gets reassigned inside the "prepare # the list of exported symbols" if statement, so the # include_expsyms logic still works. orig_export_symbols="$export_symbols" export_symbols= always_export_symbols=yes fi fi ;; esac # Prepare the list of exported symbols if test -z "$export_symbols"; then if test "$always_export_symbols" = yes || test -n "$export_symbols_regex"; then func_verbose "generating symbol list for \`$libname.la'" export_symbols="$output_objdir/$libname.exp" $opt_dry_run || $RM $export_symbols cmds=$export_symbols_cmds save_ifs="$IFS"; IFS='~' for cmd1 in $cmds; do IFS="$save_ifs" # Take the normal branch if the nm_file_list_spec branch # doesn't work or if tool conversion is not needed. case $nm_file_list_spec~$to_tool_file_cmd in *~func_convert_file_noop | *~func_convert_file_msys_to_w32 | ~*) try_normal_branch=yes eval cmd=\"$cmd1\" func_len " $cmd" len=$func_len_result ;; *) try_normal_branch=no ;; esac if test "$try_normal_branch" = yes \ && { test "$len" -lt "$max_cmd_len" \ || test "$max_cmd_len" -le -1; } then func_show_eval "$cmd" 'exit $?' skipped_export=false elif test -n "$nm_file_list_spec"; then func_basename "$output" output_la=$func_basename_result save_libobjs=$libobjs save_output=$output output=${output_objdir}/${output_la}.nm func_to_tool_file "$output" libobjs=$nm_file_list_spec$func_to_tool_file_result func_append delfiles " $output" func_verbose "creating $NM input file list: $output" for obj in $save_libobjs; do func_to_tool_file "$obj" $ECHO "$func_to_tool_file_result" done > "$output" eval cmd=\"$cmd1\" func_show_eval "$cmd" 'exit $?' output=$save_output libobjs=$save_libobjs skipped_export=false else # The command line is too long to execute in one step. func_verbose "using reloadable object file for export list..." skipped_export=: # Break out early, otherwise skipped_export may be # set to false by a later but shorter cmd. break fi done IFS="$save_ifs" if test -n "$export_symbols_regex" && test "X$skipped_export" != "X:"; then func_show_eval '$EGREP -e "$export_symbols_regex" "$export_symbols" > "${export_symbols}T"' func_show_eval '$MV "${export_symbols}T" "$export_symbols"' fi fi fi if test -n "$export_symbols" && test -n "$include_expsyms"; then tmp_export_symbols="$export_symbols" test -n "$orig_export_symbols" && tmp_export_symbols="$orig_export_symbols" $opt_dry_run || eval '$ECHO "$include_expsyms" | $SP2NL >> "$tmp_export_symbols"' fi if test "X$skipped_export" != "X:" && test -n "$orig_export_symbols"; then # The given exports_symbols file has to be filtered, so filter it. func_verbose "filter symbol list for \`$libname.la' to tag DATA exports" # FIXME: $output_objdir/$libname.filter potentially contains lots of # 's' commands which not all seds can handle. GNU sed should be fine # though. Also, the filter scales superlinearly with the number of # global variables. join(1) would be nice here, but unfortunately # isn't a blessed tool. $opt_dry_run || $SED -e '/[ ,]DATA/!d;s,\(.*\)\([ \,].*\),s|^\1$|\1\2|,' < $export_symbols > $output_objdir/$libname.filter func_append delfiles " $export_symbols $output_objdir/$libname.filter" export_symbols=$output_objdir/$libname.def $opt_dry_run || $SED -f $output_objdir/$libname.filter < $orig_export_symbols > $export_symbols fi tmp_deplibs= for test_deplib in $deplibs; do case " $convenience " in *" $test_deplib "*) ;; *) func_append tmp_deplibs " $test_deplib" ;; esac done deplibs="$tmp_deplibs" if test -n "$convenience"; then if test -n "$whole_archive_flag_spec" && test "$compiler_needs_object" = yes && test -z "$libobjs"; then # extract the archives, so we have objects to list. # TODO: could optimize this to just extract one archive. whole_archive_flag_spec= fi if test -n "$whole_archive_flag_spec"; then save_libobjs=$libobjs eval libobjs=\"\$libobjs $whole_archive_flag_spec\" test "X$libobjs" = "X " && libobjs= else gentop="$output_objdir/${outputname}x" func_append generated " $gentop" func_extract_archives $gentop $convenience func_append libobjs " $func_extract_archives_result" test "X$libobjs" = "X " && libobjs= fi fi if test "$thread_safe" = yes && test -n "$thread_safe_flag_spec"; then eval flag=\"$thread_safe_flag_spec\" func_append linker_flags " $flag" fi # Make a backup of the uninstalled library when relinking if test "$opt_mode" = relink; then $opt_dry_run || eval '(cd $output_objdir && $RM ${realname}U && $MV $realname ${realname}U)' || exit $? fi # Do each of the archive commands. if test "$module" = yes && test -n "$module_cmds" ; then if test -n "$export_symbols" && test -n "$module_expsym_cmds"; then eval test_cmds=\"$module_expsym_cmds\" cmds=$module_expsym_cmds else eval test_cmds=\"$module_cmds\" cmds=$module_cmds fi else if test -n "$export_symbols" && test -n "$archive_expsym_cmds"; then eval test_cmds=\"$archive_expsym_cmds\" cmds=$archive_expsym_cmds else eval test_cmds=\"$archive_cmds\" cmds=$archive_cmds fi fi if test "X$skipped_export" != "X:" && func_len " $test_cmds" && len=$func_len_result && test "$len" -lt "$max_cmd_len" || test "$max_cmd_len" -le -1; then : else # The command line is too long to link in one step, link piecewise # or, if using GNU ld and skipped_export is not :, use a linker # script. # Save the value of $output and $libobjs because we want to # use them later. If we have whole_archive_flag_spec, we # want to use save_libobjs as it was before # whole_archive_flag_spec was expanded, because we can't # assume the linker understands whole_archive_flag_spec. # This may have to be revisited, in case too many # convenience libraries get linked in and end up exceeding # the spec. if test -z "$convenience" || test -z "$whole_archive_flag_spec"; then save_libobjs=$libobjs fi save_output=$output func_basename "$output" output_la=$func_basename_result # Clear the reloadable object creation command queue and # initialize k to one. test_cmds= concat_cmds= objlist= last_robj= k=1 if test -n "$save_libobjs" && test "X$skipped_export" != "X:" && test "$with_gnu_ld" = yes; then output=${output_objdir}/${output_la}.lnkscript func_verbose "creating GNU ld script: $output" echo 'INPUT (' > $output for obj in $save_libobjs do func_to_tool_file "$obj" $ECHO "$func_to_tool_file_result" >> $output done echo ')' >> $output func_append delfiles " $output" func_to_tool_file "$output" output=$func_to_tool_file_result elif test -n "$save_libobjs" && test "X$skipped_export" != "X:" && test "X$file_list_spec" != X; then output=${output_objdir}/${output_la}.lnk func_verbose "creating linker input file list: $output" : > $output set x $save_libobjs shift firstobj= if test "$compiler_needs_object" = yes; then firstobj="$1 " shift fi for obj do func_to_tool_file "$obj" $ECHO "$func_to_tool_file_result" >> $output done func_append delfiles " $output" func_to_tool_file "$output" output=$firstobj\"$file_list_spec$func_to_tool_file_result\" else if test -n "$save_libobjs"; then func_verbose "creating reloadable object files..." output=$output_objdir/$output_la-${k}.$objext eval test_cmds=\"$reload_cmds\" func_len " $test_cmds" len0=$func_len_result len=$len0 # Loop over the list of objects to be linked. for obj in $save_libobjs do func_len " $obj" func_arith $len + $func_len_result len=$func_arith_result if test "X$objlist" = X || test "$len" -lt "$max_cmd_len"; then func_append objlist " $obj" else # The command $test_cmds is almost too long, add a # command to the queue. if test "$k" -eq 1 ; then # The first file doesn't have a previous command to add. reload_objs=$objlist eval concat_cmds=\"$reload_cmds\" else # All subsequent reloadable object files will link in # the last one created. reload_objs="$objlist $last_robj" eval concat_cmds=\"\$concat_cmds~$reload_cmds~\$RM $last_robj\" fi last_robj=$output_objdir/$output_la-${k}.$objext func_arith $k + 1 k=$func_arith_result output=$output_objdir/$output_la-${k}.$objext objlist=" $obj" func_len " $last_robj" func_arith $len0 + $func_len_result len=$func_arith_result fi done # Handle the remaining objects by creating one last # reloadable object file. All subsequent reloadable object # files will link in the last one created. test -z "$concat_cmds" || concat_cmds=$concat_cmds~ reload_objs="$objlist $last_robj" eval concat_cmds=\"\${concat_cmds}$reload_cmds\" if test -n "$last_robj"; then eval concat_cmds=\"\${concat_cmds}~\$RM $last_robj\" fi func_append delfiles " $output" else output= fi if ${skipped_export-false}; then func_verbose "generating symbol list for \`$libname.la'" export_symbols="$output_objdir/$libname.exp" $opt_dry_run || $RM $export_symbols libobjs=$output # Append the command to create the export file. test -z "$concat_cmds" || concat_cmds=$concat_cmds~ eval concat_cmds=\"\$concat_cmds$export_symbols_cmds\" if test -n "$last_robj"; then eval concat_cmds=\"\$concat_cmds~\$RM $last_robj\" fi fi test -n "$save_libobjs" && func_verbose "creating a temporary reloadable object file: $output" # Loop through the commands generated above and execute them. save_ifs="$IFS"; IFS='~' for cmd in $concat_cmds; do IFS="$save_ifs" $opt_silent || { func_quote_for_expand "$cmd" eval "func_echo $func_quote_for_expand_result" } $opt_dry_run || eval "$cmd" || { lt_exit=$? # Restore the uninstalled library and exit if test "$opt_mode" = relink; then ( cd "$output_objdir" && \ $RM "${realname}T" && \ $MV "${realname}U" "$realname" ) fi exit $lt_exit } done IFS="$save_ifs" if test -n "$export_symbols_regex" && ${skipped_export-false}; then func_show_eval '$EGREP -e "$export_symbols_regex" "$export_symbols" > "${export_symbols}T"' func_show_eval '$MV "${export_symbols}T" "$export_symbols"' fi fi if ${skipped_export-false}; then if test -n "$export_symbols" && test -n "$include_expsyms"; then tmp_export_symbols="$export_symbols" test -n "$orig_export_symbols" && tmp_export_symbols="$orig_export_symbols" $opt_dry_run || eval '$ECHO "$include_expsyms" | $SP2NL >> "$tmp_export_symbols"' fi if test -n "$orig_export_symbols"; then # The given exports_symbols file has to be filtered, so filter it. func_verbose "filter symbol list for \`$libname.la' to tag DATA exports" # FIXME: $output_objdir/$libname.filter potentially contains lots of # 's' commands which not all seds can handle. GNU sed should be fine # though. Also, the filter scales superlinearly with the number of # global variables. join(1) would be nice here, but unfortunately # isn't a blessed tool. $opt_dry_run || $SED -e '/[ ,]DATA/!d;s,\(.*\)\([ \,].*\),s|^\1$|\1\2|,' < $export_symbols > $output_objdir/$libname.filter func_append delfiles " $export_symbols $output_objdir/$libname.filter" export_symbols=$output_objdir/$libname.def $opt_dry_run || $SED -f $output_objdir/$libname.filter < $orig_export_symbols > $export_symbols fi fi libobjs=$output # Restore the value of output. output=$save_output if test -n "$convenience" && test -n "$whole_archive_flag_spec"; then eval libobjs=\"\$libobjs $whole_archive_flag_spec\" test "X$libobjs" = "X " && libobjs= fi # Expand the library linking commands again to reset the # value of $libobjs for piecewise linking. # Do each of the archive commands. if test "$module" = yes && test -n "$module_cmds" ; then if test -n "$export_symbols" && test -n "$module_expsym_cmds"; then cmds=$module_expsym_cmds else cmds=$module_cmds fi else if test -n "$export_symbols" && test -n "$archive_expsym_cmds"; then cmds=$archive_expsym_cmds else cmds=$archive_cmds fi fi fi if test -n "$delfiles"; then # Append the command to remove temporary files to $cmds. eval cmds=\"\$cmds~\$RM $delfiles\" fi # Add any objects from preloaded convenience libraries if test -n "$dlprefiles"; then gentop="$output_objdir/${outputname}x" func_append generated " $gentop" func_extract_archives $gentop $dlprefiles func_append libobjs " $func_extract_archives_result" test "X$libobjs" = "X " && libobjs= fi save_ifs="$IFS"; IFS='~' for cmd in $cmds; do IFS="$save_ifs" eval cmd=\"$cmd\" $opt_silent || { func_quote_for_expand "$cmd" eval "func_echo $func_quote_for_expand_result" } $opt_dry_run || eval "$cmd" || { lt_exit=$? # Restore the uninstalled library and exit if test "$opt_mode" = relink; then ( cd "$output_objdir" && \ $RM "${realname}T" && \ $MV "${realname}U" "$realname" ) fi exit $lt_exit } done IFS="$save_ifs" # Restore the uninstalled library and exit if test "$opt_mode" = relink; then $opt_dry_run || eval '(cd $output_objdir && $RM ${realname}T && $MV $realname ${realname}T && $MV ${realname}U $realname)' || exit $? if test -n "$convenience"; then if test -z "$whole_archive_flag_spec"; then func_show_eval '${RM}r "$gentop"' fi fi exit $EXIT_SUCCESS fi # Create links to the real library. for linkname in $linknames; do if test "$realname" != "$linkname"; then func_show_eval '(cd "$output_objdir" && $RM "$linkname" && $LN_S "$realname" "$linkname")' 'exit $?' fi done # If -module or -export-dynamic was specified, set the dlname. if test "$module" = yes || test "$export_dynamic" = yes; then # On all known operating systems, these are identical. dlname="$soname" fi fi ;; obj) if test -n "$dlfiles$dlprefiles" || test "$dlself" != no; then func_warning "\`-dlopen' is ignored for objects" fi case " $deplibs" in *\ -l* | *\ -L*) func_warning "\`-l' and \`-L' are ignored for objects" ;; esac test -n "$rpath" && \ func_warning "\`-rpath' is ignored for objects" test -n "$xrpath" && \ func_warning "\`-R' is ignored for objects" test -n "$vinfo" && \ func_warning "\`-version-info' is ignored for objects" test -n "$release" && \ func_warning "\`-release' is ignored for objects" case $output in *.lo) test -n "$objs$old_deplibs" && \ func_fatal_error "cannot build library object \`$output' from non-libtool objects" libobj=$output func_lo2o "$libobj" obj=$func_lo2o_result ;; *) libobj= obj="$output" ;; esac # Delete the old objects. $opt_dry_run || $RM $obj $libobj # Objects from convenience libraries. This assumes # single-version convenience libraries. Whenever we create # different ones for PIC/non-PIC, this we'll have to duplicate # the extraction. reload_conv_objs= gentop= # reload_cmds runs $LD directly, so let us get rid of # -Wl from whole_archive_flag_spec and hope we can get by with # turning comma into space.. wl= if test -n "$convenience"; then if test -n "$whole_archive_flag_spec"; then eval tmp_whole_archive_flags=\"$whole_archive_flag_spec\" reload_conv_objs=$reload_objs\ `$ECHO "$tmp_whole_archive_flags" | $SED 's|,| |g'` else gentop="$output_objdir/${obj}x" func_append generated " $gentop" func_extract_archives $gentop $convenience reload_conv_objs="$reload_objs $func_extract_archives_result" fi fi # If we're not building shared, we need to use non_pic_objs test "$build_libtool_libs" != yes && libobjs="$non_pic_objects" # Create the old-style object. reload_objs="$objs$old_deplibs "`$ECHO "$libobjs" | $SP2NL | $SED "/\.${libext}$/d; /\.lib$/d; $lo2o" | $NL2SP`" $reload_conv_objs" ### testsuite: skip nested quoting test output="$obj" func_execute_cmds "$reload_cmds" 'exit $?' # Exit if we aren't doing a library object file. if test -z "$libobj"; then if test -n "$gentop"; then func_show_eval '${RM}r "$gentop"' fi exit $EXIT_SUCCESS fi if test "$build_libtool_libs" != yes; then if test -n "$gentop"; then func_show_eval '${RM}r "$gentop"' fi # Create an invalid libtool object if no PIC, so that we don't # accidentally link it into a program. # $show "echo timestamp > $libobj" # $opt_dry_run || eval "echo timestamp > $libobj" || exit $? exit $EXIT_SUCCESS fi if test -n "$pic_flag" || test "$pic_mode" != default; then # Only do commands if we really have different PIC objects. reload_objs="$libobjs $reload_conv_objs" output="$libobj" func_execute_cmds "$reload_cmds" 'exit $?' fi if test -n "$gentop"; then func_show_eval '${RM}r "$gentop"' fi exit $EXIT_SUCCESS ;; prog) case $host in *cygwin*) func_stripname '' '.exe' "$output" output=$func_stripname_result.exe;; esac test -n "$vinfo" && \ func_warning "\`-version-info' is ignored for programs" test -n "$release" && \ func_warning "\`-release' is ignored for programs" test "$preload" = yes \ && test "$dlopen_support" = unknown \ && test "$dlopen_self" = unknown \ && test "$dlopen_self_static" = unknown && \ func_warning "\`LT_INIT([dlopen])' not used. Assuming no dlopen support." case $host in *-*-rhapsody* | *-*-darwin1.[012]) # On Rhapsody replace the C library is the System framework compile_deplibs=`$ECHO " $compile_deplibs" | $SED 's/ -lc / System.ltframework /'` finalize_deplibs=`$ECHO " $finalize_deplibs" | $SED 's/ -lc / System.ltframework /'` ;; esac case $host in *-*-darwin*) # Don't allow lazy linking, it breaks C++ global constructors # But is supposedly fixed on 10.4 or later (yay!). if test "$tagname" = CXX ; then case ${MACOSX_DEPLOYMENT_TARGET-10.0} in 10.[0123]) func_append compile_command " ${wl}-bind_at_load" func_append finalize_command " ${wl}-bind_at_load" ;; esac fi # Time to change all our "foo.ltframework" stuff back to "-framework foo" compile_deplibs=`$ECHO " $compile_deplibs" | $SED 's% \([^ $]*\).ltframework% -framework \1%g'` finalize_deplibs=`$ECHO " $finalize_deplibs" | $SED 's% \([^ $]*\).ltframework% -framework \1%g'` ;; esac # move library search paths that coincide with paths to not yet # installed libraries to the beginning of the library search list new_libs= for path in $notinst_path; do case " $new_libs " in *" -L$path/$objdir "*) ;; *) case " $compile_deplibs " in *" -L$path/$objdir "*) func_append new_libs " -L$path/$objdir" ;; esac ;; esac done for deplib in $compile_deplibs; do case $deplib in -L*) case " $new_libs " in *" $deplib "*) ;; *) func_append new_libs " $deplib" ;; esac ;; *) func_append new_libs " $deplib" ;; esac done compile_deplibs="$new_libs" func_append compile_command " $compile_deplibs" func_append finalize_command " $finalize_deplibs" if test -n "$rpath$xrpath"; then # If the user specified any rpath flags, then add them. for libdir in $rpath $xrpath; do # This is the magic to use -rpath. case "$finalize_rpath " in *" $libdir "*) ;; *) func_append finalize_rpath " $libdir" ;; esac done fi # Now hardcode the library paths rpath= hardcode_libdirs= for libdir in $compile_rpath $finalize_rpath; do if test -n "$hardcode_libdir_flag_spec"; then if test -n "$hardcode_libdir_separator"; then if test -z "$hardcode_libdirs"; then hardcode_libdirs="$libdir" else # Just accumulate the unique libdirs. case $hardcode_libdir_separator$hardcode_libdirs$hardcode_libdir_separator in *"$hardcode_libdir_separator$libdir$hardcode_libdir_separator"*) ;; *) func_append hardcode_libdirs "$hardcode_libdir_separator$libdir" ;; esac fi else eval flag=\"$hardcode_libdir_flag_spec\" func_append rpath " $flag" fi elif test -n "$runpath_var"; then case "$perm_rpath " in *" $libdir "*) ;; *) func_append perm_rpath " $libdir" ;; esac fi case $host in *-*-cygwin* | *-*-mingw* | *-*-pw32* | *-*-os2* | *-cegcc*) testbindir=`${ECHO} "$libdir" | ${SED} -e 's*/lib$*/bin*'` case :$dllsearchpath: in *":$libdir:"*) ;; ::) dllsearchpath=$libdir;; *) func_append dllsearchpath ":$libdir";; esac case :$dllsearchpath: in *":$testbindir:"*) ;; ::) dllsearchpath=$testbindir;; *) func_append dllsearchpath ":$testbindir";; esac ;; esac done # Substitute the hardcoded libdirs into the rpath. if test -n "$hardcode_libdir_separator" && test -n "$hardcode_libdirs"; then libdir="$hardcode_libdirs" eval rpath=\" $hardcode_libdir_flag_spec\" fi compile_rpath="$rpath" rpath= hardcode_libdirs= for libdir in $finalize_rpath; do if test -n "$hardcode_libdir_flag_spec"; then if test -n "$hardcode_libdir_separator"; then if test -z "$hardcode_libdirs"; then hardcode_libdirs="$libdir" else # Just accumulate the unique libdirs. case $hardcode_libdir_separator$hardcode_libdirs$hardcode_libdir_separator in *"$hardcode_libdir_separator$libdir$hardcode_libdir_separator"*) ;; *) func_append hardcode_libdirs "$hardcode_libdir_separator$libdir" ;; esac fi else eval flag=\"$hardcode_libdir_flag_spec\" func_append rpath " $flag" fi elif test -n "$runpath_var"; then case "$finalize_perm_rpath " in *" $libdir "*) ;; *) func_append finalize_perm_rpath " $libdir" ;; esac fi done # Substitute the hardcoded libdirs into the rpath. if test -n "$hardcode_libdir_separator" && test -n "$hardcode_libdirs"; then libdir="$hardcode_libdirs" eval rpath=\" $hardcode_libdir_flag_spec\" fi finalize_rpath="$rpath" if test -n "$libobjs" && test "$build_old_libs" = yes; then # Transform all the library objects into standard objects. compile_command=`$ECHO "$compile_command" | $SP2NL | $SED "$lo2o" | $NL2SP` finalize_command=`$ECHO "$finalize_command" | $SP2NL | $SED "$lo2o" | $NL2SP` fi func_generate_dlsyms "$outputname" "@PROGRAM@" "no" # template prelinking step if test -n "$prelink_cmds"; then func_execute_cmds "$prelink_cmds" 'exit $?' fi wrappers_required=yes case $host in *cegcc* | *mingw32ce*) # Disable wrappers for cegcc and mingw32ce hosts, we are cross compiling anyway. wrappers_required=no ;; *cygwin* | *mingw* ) if test "$build_libtool_libs" != yes; then wrappers_required=no fi ;; *) if test "$need_relink" = no || test "$build_libtool_libs" != yes; then wrappers_required=no fi ;; esac if test "$wrappers_required" = no; then # Replace the output file specification. compile_command=`$ECHO "$compile_command" | $SED 's%@OUTPUT@%'"$output"'%g'` link_command="$compile_command$compile_rpath" # We have no uninstalled library dependencies, so finalize right now. exit_status=0 func_show_eval "$link_command" 'exit_status=$?' if test -n "$postlink_cmds"; then func_to_tool_file "$output" postlink_cmds=`func_echo_all "$postlink_cmds" | $SED -e 's%@OUTPUT@%'"$output"'%g' -e 's%@TOOL_OUTPUT@%'"$func_to_tool_file_result"'%g'` func_execute_cmds "$postlink_cmds" 'exit $?' fi # Delete the generated files. if test -f "$output_objdir/${outputname}S.${objext}"; then func_show_eval '$RM "$output_objdir/${outputname}S.${objext}"' fi exit $exit_status fi if test -n "$compile_shlibpath$finalize_shlibpath"; then compile_command="$shlibpath_var=\"$compile_shlibpath$finalize_shlibpath\$$shlibpath_var\" $compile_command" fi if test -n "$finalize_shlibpath"; then finalize_command="$shlibpath_var=\"$finalize_shlibpath\$$shlibpath_var\" $finalize_command" fi compile_var= finalize_var= if test -n "$runpath_var"; then if test -n "$perm_rpath"; then # We should set the runpath_var. rpath= for dir in $perm_rpath; do func_append rpath "$dir:" done compile_var="$runpath_var=\"$rpath\$$runpath_var\" " fi if test -n "$finalize_perm_rpath"; then # We should set the runpath_var. rpath= for dir in $finalize_perm_rpath; do func_append rpath "$dir:" done finalize_var="$runpath_var=\"$rpath\$$runpath_var\" " fi fi if test "$no_install" = yes; then # We don't need to create a wrapper script. link_command="$compile_var$compile_command$compile_rpath" # Replace the output file specification. link_command=`$ECHO "$link_command" | $SED 's%@OUTPUT@%'"$output"'%g'` # Delete the old output file. $opt_dry_run || $RM $output # Link the executable and exit func_show_eval "$link_command" 'exit $?' if test -n "$postlink_cmds"; then func_to_tool_file "$output" postlink_cmds=`func_echo_all "$postlink_cmds" | $SED -e 's%@OUTPUT@%'"$output"'%g' -e 's%@TOOL_OUTPUT@%'"$func_to_tool_file_result"'%g'` func_execute_cmds "$postlink_cmds" 'exit $?' fi exit $EXIT_SUCCESS fi if test "$hardcode_action" = relink; then # Fast installation is not supported link_command="$compile_var$compile_command$compile_rpath" relink_command="$finalize_var$finalize_command$finalize_rpath" func_warning "this platform does not like uninstalled shared libraries" func_warning "\`$output' will be relinked during installation" else if test "$fast_install" != no; then link_command="$finalize_var$compile_command$finalize_rpath" if test "$fast_install" = yes; then relink_command=`$ECHO "$compile_var$compile_command$compile_rpath" | $SED 's%@OUTPUT@%\$progdir/\$file%g'` else # fast_install is set to needless relink_command= fi else link_command="$compile_var$compile_command$compile_rpath" relink_command="$finalize_var$finalize_command$finalize_rpath" fi fi # Replace the output file specification. link_command=`$ECHO "$link_command" | $SED 's%@OUTPUT@%'"$output_objdir/$outputname"'%g'` # Delete the old output files. $opt_dry_run || $RM $output $output_objdir/$outputname $output_objdir/lt-$outputname func_show_eval "$link_command" 'exit $?' if test -n "$postlink_cmds"; then func_to_tool_file "$output_objdir/$outputname" postlink_cmds=`func_echo_all "$postlink_cmds" | $SED -e 's%@OUTPUT@%'"$output_objdir/$outputname"'%g' -e 's%@TOOL_OUTPUT@%'"$func_to_tool_file_result"'%g'` func_execute_cmds "$postlink_cmds" 'exit $?' fi # Now create the wrapper script. func_verbose "creating $output" # Quote the relink command for shipping. if test -n "$relink_command"; then # Preserve any variables that may affect compiler behavior for var in $variables_saved_for_relink; do if eval test -z \"\${$var+set}\"; then relink_command="{ test -z \"\${$var+set}\" || $lt_unset $var || { $var=; export $var; }; }; $relink_command" elif eval var_value=\$$var; test -z "$var_value"; then relink_command="$var=; export $var; $relink_command" else func_quote_for_eval "$var_value" relink_command="$var=$func_quote_for_eval_result; export $var; $relink_command" fi done relink_command="(cd `pwd`; $relink_command)" relink_command=`$ECHO "$relink_command" | $SED "$sed_quote_subst"` fi # Only actually do things if not in dry run mode. $opt_dry_run || { # win32 will think the script is a binary if it has # a .exe suffix, so we strip it off here. case $output in *.exe) func_stripname '' '.exe' "$output" output=$func_stripname_result ;; esac # test for cygwin because mv fails w/o .exe extensions case $host in *cygwin*) exeext=.exe func_stripname '' '.exe' "$outputname" outputname=$func_stripname_result ;; *) exeext= ;; esac case $host in *cygwin* | *mingw* ) func_dirname_and_basename "$output" "" "." output_name=$func_basename_result output_path=$func_dirname_result cwrappersource="$output_path/$objdir/lt-$output_name.c" cwrapper="$output_path/$output_name.exe" $RM $cwrappersource $cwrapper trap "$RM $cwrappersource $cwrapper; exit $EXIT_FAILURE" 1 2 15 func_emit_cwrapperexe_src > $cwrappersource # The wrapper executable is built using the $host compiler, # because it contains $host paths and files. If cross- # compiling, it, like the target executable, must be # executed on the $host or under an emulation environment. $opt_dry_run || { $LTCC $LTCFLAGS -o $cwrapper $cwrappersource $STRIP $cwrapper } # Now, create the wrapper script for func_source use: func_ltwrapper_scriptname $cwrapper $RM $func_ltwrapper_scriptname_result trap "$RM $func_ltwrapper_scriptname_result; exit $EXIT_FAILURE" 1 2 15 $opt_dry_run || { # note: this script will not be executed, so do not chmod. if test "x$build" = "x$host" ; then $cwrapper --lt-dump-script > $func_ltwrapper_scriptname_result else func_emit_wrapper no > $func_ltwrapper_scriptname_result fi } ;; * ) $RM $output trap "$RM $output; exit $EXIT_FAILURE" 1 2 15 func_emit_wrapper no > $output chmod +x $output ;; esac } exit $EXIT_SUCCESS ;; esac # See if we need to build an old-fashioned archive. for oldlib in $oldlibs; do if test "$build_libtool_libs" = convenience; then oldobjs="$libobjs_save $symfileobj" addlibs="$convenience" build_libtool_libs=no else if test "$build_libtool_libs" = module; then oldobjs="$libobjs_save" build_libtool_libs=no else oldobjs="$old_deplibs $non_pic_objects" if test "$preload" = yes && test -f "$symfileobj"; then func_append oldobjs " $symfileobj" fi fi addlibs="$old_convenience" fi if test -n "$addlibs"; then gentop="$output_objdir/${outputname}x" func_append generated " $gentop" func_extract_archives $gentop $addlibs func_append oldobjs " $func_extract_archives_result" fi # Do each command in the archive commands. if test -n "$old_archive_from_new_cmds" && test "$build_libtool_libs" = yes; then cmds=$old_archive_from_new_cmds else # Add any objects from preloaded convenience libraries if test -n "$dlprefiles"; then gentop="$output_objdir/${outputname}x" func_append generated " $gentop" func_extract_archives $gentop $dlprefiles func_append oldobjs " $func_extract_archives_result" fi # POSIX demands no paths to be encoded in archives. We have # to avoid creating archives with duplicate basenames if we # might have to extract them afterwards, e.g., when creating a # static archive out of a convenience library, or when linking # the entirety of a libtool archive into another (currently # not supported by libtool). if (for obj in $oldobjs do func_basename "$obj" $ECHO "$func_basename_result" done | sort | sort -uc >/dev/null 2>&1); then : else echo "copying selected object files to avoid basename conflicts..." gentop="$output_objdir/${outputname}x" func_append generated " $gentop" func_mkdir_p "$gentop" save_oldobjs=$oldobjs oldobjs= counter=1 for obj in $save_oldobjs do func_basename "$obj" objbase="$func_basename_result" case " $oldobjs " in " ") oldobjs=$obj ;; *[\ /]"$objbase "*) while :; do # Make sure we don't pick an alternate name that also # overlaps. newobj=lt$counter-$objbase func_arith $counter + 1 counter=$func_arith_result case " $oldobjs " in *[\ /]"$newobj "*) ;; *) if test ! -f "$gentop/$newobj"; then break; fi ;; esac done func_show_eval "ln $obj $gentop/$newobj || cp $obj $gentop/$newobj" func_append oldobjs " $gentop/$newobj" ;; *) func_append oldobjs " $obj" ;; esac done fi func_to_tool_file "$oldlib" func_convert_file_msys_to_w32 tool_oldlib=$func_to_tool_file_result eval cmds=\"$old_archive_cmds\" func_len " $cmds" len=$func_len_result if test "$len" -lt "$max_cmd_len" || test "$max_cmd_len" -le -1; then cmds=$old_archive_cmds elif test -n "$archiver_list_spec"; then func_verbose "using command file archive linking..." for obj in $oldobjs do func_to_tool_file "$obj" $ECHO "$func_to_tool_file_result" done > $output_objdir/$libname.libcmd func_to_tool_file "$output_objdir/$libname.libcmd" oldobjs=" $archiver_list_spec$func_to_tool_file_result" cmds=$old_archive_cmds else # the command line is too long to link in one step, link in parts func_verbose "using piecewise archive linking..." save_RANLIB=$RANLIB RANLIB=: objlist= concat_cmds= save_oldobjs=$oldobjs oldobjs= # Is there a better way of finding the last object in the list? 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then case " $rmdirs " in *" $odir "*) ;; *) func_append rmdirs " $odir" ;; esac fi # Don't error if the file doesn't exist and rm -f was used. if { test -L "$file"; } >/dev/null 2>&1 || { test -h "$file"; } >/dev/null 2>&1 || test -f "$file"; then : elif test -d "$file"; then exit_status=1 continue elif test "$rmforce" = yes; then continue fi rmfiles="$file" case $name in *.la) # Possibly a libtool archive, so verify it. if func_lalib_p "$file"; then func_source $dir/$name # Delete the libtool libraries and symlinks. for n in $library_names; do func_append rmfiles " $odir/$n" done test -n "$old_library" && func_append rmfiles " $odir/$old_library" case "$opt_mode" in clean) case " $library_names " in *" $dlname "*) ;; *) test -n "$dlname" && func_append rmfiles " $odir/$dlname" ;; esac test -n "$libdir" && func_append rmfiles " $odir/$name $odir/${name}i" ;; uninstall) if test -n "$library_names"; then # Do each command in the postuninstall commands. func_execute_cmds "$postuninstall_cmds" 'test "$rmforce" = yes || exit_status=1' fi if test -n "$old_library"; then # Do each command in the old_postuninstall commands. func_execute_cmds "$old_postuninstall_cmds" 'test "$rmforce" = yes || exit_status=1' fi # FIXME: should reinstall the best remaining shared library. ;; esac fi ;; *.lo) # Possibly a libtool object, so verify it. if func_lalib_p "$file"; then # Read the .lo file func_source $dir/$name # Add PIC object to the list of files to remove. if test -n "$pic_object" && test "$pic_object" != none; then func_append rmfiles " $dir/$pic_object" fi # Add non-PIC object to the list of files to remove. if test -n "$non_pic_object" && test "$non_pic_object" != none; then func_append rmfiles " $dir/$non_pic_object" fi fi ;; *) if test "$opt_mode" = clean ; then noexename=$name case $file in *.exe) func_stripname '' '.exe' "$file" file=$func_stripname_result func_stripname '' '.exe' "$name" noexename=$func_stripname_result # $file with .exe has already been added to rmfiles, # add $file without .exe func_append rmfiles " $file" ;; esac # Do a test to see if this is a libtool program. if func_ltwrapper_p "$file"; then if func_ltwrapper_executable_p "$file"; then func_ltwrapper_scriptname "$file" relink_command= func_source $func_ltwrapper_scriptname_result func_append rmfiles " $func_ltwrapper_scriptname_result" else relink_command= func_source $dir/$noexename fi # note $name still contains .exe if it was in $file originally # as does the version of $file that was added into $rmfiles func_append rmfiles " $odir/$name $odir/${name}S.${objext}" if test "$fast_install" = yes && test -n "$relink_command"; then func_append rmfiles " $odir/lt-$name" fi if test "X$noexename" != "X$name" ; then func_append rmfiles " $odir/lt-${noexename}.c" fi fi fi ;; esac func_show_eval "$RM $rmfiles" 'exit_status=1' done # Try to remove the ${objdir}s in the directories where we deleted files for dir in $rmdirs; do if test -d "$dir"; then func_show_eval "rmdir $dir >/dev/null 2>&1" fi done exit $exit_status } { test "$opt_mode" = uninstall || test "$opt_mode" = clean; } && func_mode_uninstall ${1+"$@"} test -z "$opt_mode" && { help="$generic_help" func_fatal_help "you must specify a MODE" } test -z "$exec_cmd" && \ func_fatal_help "invalid operation mode \`$opt_mode'" if test -n "$exec_cmd"; then eval exec "$exec_cmd" exit $EXIT_FAILURE fi exit $exit_status # The TAGs below are defined such that we never get into a situation # in which we disable both kinds of libraries. Given conflicting # choices, we go for a static library, that is the most portable, # since we can't tell whether shared libraries were disabled because # the user asked for that or because the platform doesn't support # them. This is particularly important on AIX, because we don't # support having both static and shared libraries enabled at the same # time on that platform, so we default to a shared-only configuration. # If a disable-shared tag is given, we'll fallback to a static-only # configuration. But we'll never go from static-only to shared-only. # ### BEGIN LIBTOOL TAG CONFIG: disable-shared build_libtool_libs=no build_old_libs=yes # ### END LIBTOOL TAG CONFIG: disable-shared # ### BEGIN LIBTOOL TAG CONFIG: disable-static build_old_libs=`case $build_libtool_libs in yes) echo no;; *) echo yes;; esac` # ### END LIBTOOL TAG CONFIG: disable-static # Local Variables: # mode:shell-script # sh-indentation:2 # End: # vi:sw=2 pal-0.5.0/Makefile.am000644 000765 000024 00000004535 12366012030 014432 0ustar00timjstaff000000 000000 ## Process this file with automake to produce Makefile.in lib_LTLIBRARIES = libpal.la # Include palOne2One.c separately since it is a combo file libpal_la_SOURCES = $(PUBLIC_C_FILES) palOne2One.c $(PRIVATE_C_FILES) # If we are using a non-standard location libpal_la_CPPFLAGS = $(ERFA_CPPFLAGS) libpal_la_LDFLAGS = $(ERFA_LDFLAGS) # Force a link against ERFA and, optionally, starutil libpal_la_LIBADD = $(ERFA_LIBADD) $(STARUTIL_LIBADD) # Misc files dist_starnews_DATA = pal.news dist_pkgdata_DATA = COPYING COPYING.LESSER README.md # Make all library code position independent. 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See the # GNU General Public License for more details. # You should have received a copy of the GNU General Public License # along with this program. If not, see . # As a special exception to the GNU General Public License, if you # distribute this file as part of a program that contains a # configuration script generated by Autoconf, you may include it under # the same distribution terms that you use for the rest of that program. if test $# -eq 0; then echo 1>&2 "Try '$0 --help' for more information" exit 1 fi case $1 in --is-lightweight) # Used by our autoconf macros to check whether the available missing # script is modern enough. exit 0 ;; --run) # Back-compat with the calling convention used by older automake. shift ;; -h|--h|--he|--hel|--help) echo "\ $0 [OPTION]... PROGRAM [ARGUMENT]... Run 'PROGRAM [ARGUMENT]...', returning a proper advice when this fails due to PROGRAM being missing or too old. 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Define all SLA prototypes in PAL form even * though none are implemented. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, MA 02110-1301 * USA. * Bugs: * {note_any_bugs_here} *- */ #ifdef __cplusplus extern "C" { #endif #include #include void palAddet ( double rm, double dm, double eq, double *rc, double *dc ); void palAfin ( const char *string, int *iptr, float *a, int *j ); double palAirmas ( double zd ); void palAltaz ( double ha, double dec, double phi, double *az, double *azd, double *azdd, double *el, double *eld, double *eldd, double *pa, double *pad, double *padd ); void palAmp ( double ra, double da, double date, double eq, double *rm, double *dm ); void palAmpqk ( double ra, double da, double amprms[21], double *rm, double *dm ); void palAop ( double rap, double dap, double date, double dut, double elongm, double phim, double hm, double xp, double yp, double tdk, double pmb, double rh, double wl, double tlr, double *aob, double *zob, double *hob, double *dob, double *rob ); void palAoppa ( double date, double dut, double elongm, double phim, double hm, double xp, double yp, double tdk, double pmb, double rh, double wl, double tlr, double aoprms[14] ); void palAoppat ( double date, double aoprms[14] ); void palAopqk ( double rap, double dap, const double aoprms[14], double *aob, double *zob, double *hob, double *dob, double *rob ); void palAtmdsp ( double tdk, double pmb, double rh, double wl1, double a1, double b1, double wl2, double *a2, double *b2 ); void palAv2m ( float axvec[3], float rmat[3][3] ); float palBear ( float a1, float b1, float a2, float b2 ); void palCaf2r ( int ideg, int iamin, float asec, float *rad, int *j ); void palCaldj ( int iy, int im, int id, double *djm, int *j ); void palCalyd ( int iy, int im, int id, int *ny, int *nd, int *j ); void palCc2s ( float v[3], float *a, float *b ); void palCc62s ( float v[6], float *a, float *b, float *r, float *ad, float *bd, float *rd ); void palCd2tf ( int ndp, float days, char *sign, int ihmsf[4] ); void palCldj ( int iy, int im, int id, double *djm, int *j ); void palClyd ( int iy, int im, int id, int *ny, int *nd, int *jstat ); void palCombn ( int nsel, int ncand, int list[], int *j ); void palCr2af ( int ndp, float angle, char *sign, int idmsf[4] ); void palCr2tf ( int ndp, float angle, char *sign, int ihmsf[4] ); void palCs2c ( float a, float b, float v[3] ); void palCs2c6 ( float a, float b, float r, float ad, float bd, float rd, float v[6] ); void palCtf2d ( int ihour, int imin, float sec, float *days, int *j ); void palCtf2r ( int ihour, int imin, float sec, float *rad, int *j ); void palDaf2r ( int ideg, int iamin, double asec, double *rad, int *j ); void palDafin ( const char *string, int *iptr, double *a, int *j ); double palDat ( double dju ); void palDav2m ( double axvec[3], double rmat[3][3] ); double palDbear ( double a1, double b1, double a2, double b2 ); void palDbjin ( const char *string, int *nstrt, double *dreslt, int *jf1, int *jf2 ); void palDc62s ( double v[6], double *a, double *b, double *r, double *ad, double *bd, double *rd ); void palDcc2s ( double v[3], double *a, double *b ); void palDcmpf ( double coeffs[6], double *xz, double *yz, double *xs, double *ys, double *perp, double *orient ); void palDcs2c ( double a, double b, double v[3] ); void palDd2tf ( int ndp, double days, char *sign, int ihmsf[4] ); void palDe2h ( double ha, double dec, double phi, double *az, double *el ); void palDeuler ( const char *order, double phi, double theta, double psi, double rmat[3][3] ); void palDfltin ( const char *string, int *nstrt, double *dreslt, int *jflag ); void palDh2e ( double az, double el, double phi, double *ha, double *dec); void palDimxv ( double dm[3][3], double va[3], double vb[3] ); void palDjcal ( int ndp, double djm, int iymdf[4], int *j ); void palDjcl ( double djm, int *iy, int *im, int *id, double *fd, int *j ); void palDm2av ( double rmat[3][3], double axvec[3] ); void palDmat ( int n, double *a, double *y, double *d, int *jf, int *iw ); void palDmoon ( double date, double pv[6] ); void palDmxm ( double a[3][3], double b[3][3], double c[3][3] ); void palDmxv ( double dm[3][3], double va[3], double vb[3] ); double palDpav ( double v1[3], double v2[3] ); void palDr2af ( int ndp, double angle, char *sign, int idmsf[4] ); void palDr2tf ( int ndp, double angle, char *sign, int ihmsf[4] ); double palDrange ( double angle ); double palDranrm ( double angle ); void palDs2c6 ( double a, double b, double r, double ad, double bd, double rd, double v[6] ); void palDs2tp ( double ra, double dec, double raz, double decz, double *xi, double *eta, int *j ); double palDsep ( double a1, double b1, double a2, double b2 ); double palDsepv ( double v1[3], double v2[3] ); double palDt ( double epoch ); void palDtf2d ( int ihour, int imin, double sec, double *days, int *j ); void palDtf2r ( int ihour, int imin, double sec, double *rad, int *j ); void palDtp2s ( double xi, double eta, double raz, double decz, double *ra, double *dec ); void palDtp2v ( double xi, double eta, double v0[3], double v[3] ); void palDtps2c ( double xi, double eta, double ra, double dec, double *raz1, double *decz1, double *raz2, double *decz2, int *n ); void palDtpv2c ( double xi, double eta, double v[3], double v01[3], double v02[3], int *n ); double palDtt ( double dju ); void palDv2tp ( double v[3], double v0[3], double *xi, double *eta, int *j ); double palDvdv ( double va[3], double vb[3] ); void palDvn ( double v[3], double uv[3], double *vm ); void palDvxv ( double va[3], double vb[3], double vc[3] ); void palE2h ( float ha, float dec, float phi, float *az, float *el ); void palEarth ( int iy, int id, float fd, float posvel[6] ); void palEcleq ( double dl, double db, double date, double *dr, double *dd ); void palEcmat ( double date, double rmat[3][3] ); void palEcor ( float rm, float dm, int iy, int id, float fd, float *rv, float *tl ); void palEg50 ( double dr, double dd, double *dl, double *db ); void palEl2ue ( double date, int jform, double epoch, double orbinc, double anode, double perih, double aorq, double e, double aorl, double dm, double u[13], int *jstat ); double palEpb ( double date ); double palEpb2d ( double epb ); double palEpco ( char k0, char k, double e ); double palEpj ( double date ); double palEpj2d ( double epj ); void palEpv( double date, double ph[3], double vh[3], double pb[3], double vb[3] ); void palEqecl ( double dr, double dd, double date, double *dl, double *db ); double palEqeqx ( double date ); void palEqgal ( double dr, double dd, double *dl, double *db ); void palEtrms ( double ep, double ev[3] ); void palEuler ( const char *order, float phi, float theta, float psi, float rmat[3][3] ); void palEvp ( double date, double deqx, double dvb[3], double dpb[3], double dvh[3], double dph[3] ); void palFitxy ( int itype, int np, double xye[][2], double xym[][2], double coeffs[6], int *j ); void palFk425 ( double r1950, double d1950, double dr1950, double dd1950, double p1950, double v1950, double *r2000, double *d2000, double *dr2000, double *dd2000, double *p2000, double *v2000 ); void palFk45z ( double r1950, double d1950, double bepoch, double *r2000, double *d2000 ); void palFk524 ( double r2000, double d2000, double dr2000, double dd2000, double p2000, double v2000, double *r1950, double *d1950, double *dr1950, double *dd1950, double *p1950, double *v1950 ); void palFk52h ( double r5, double d5, double dr5, double dd5, double *dr, double *dh, double *drh, double *ddh ); void palFk54z ( double r2000, double d2000, double bepoch, double *r1950, double *d1950, double *dr1950, double *dd1950 ); void palFk5hz ( double r5, double d5, double epoch, double *rh, double *dh ); void palFlotin ( const char *string, int *nstrt, float *reslt, int *jflag ); void palGaleq ( double dl, double db, double *dr, double *dd ); void palGalsup ( double dl, double db, double *dsl, double *dsb ); void palGe50 ( double dl, double db, double *dr, double *dd ); void palGeoc ( double p, double h, double *r, double *z ); double palGmst ( double ut1 ); double palGmsta ( double date, double ut1 ); void palH2e ( float az, float el, float phi, float *ha, float *dec ); void palH2fk5 ( double dr, double dh, double drh, double ddh, double *r5, double *d5, double *dr5, double *dd5 ); void palHfk5z ( double rh, double dh, double epoch, double *r5, double *d5, double *dr5, double *dd5 ); void palImxv ( float rm[3][3], float va[3], float vb[3] ); void palInt2in ( const char *string, int *nstrt, int *ireslt, int *jflag ); void palIntin ( const char *string, int *nstrt, long *ireslt, int *jflag ); void palInvf ( double fwds[6], double bkwds[6], int *j ); void palKbj ( int jb, double e, char *k, int *j ); void palM2av ( float rmat[3][3], float axvec[3] ); void palMap ( double rm, double dm, double pr, double pd, double px, double rv, double eq, double date, double *ra, double *da ); void palMappa ( double eq, double date, double amprms[21] ); void palMapqk ( double rm, double dm, double pr, double pd, double px, double rv, double amprms[21], double *ra, double *da ); void palMapqkz ( double rm, double dm, double amprms[21], double *ra, double *da ); void palMoon ( int iy, int id, float fd, float posvel[6] ); void palMxm ( float a[3][3], float b[3][3], float c[3][3] ); void palMxv ( float rm[3][3], float va[3], float vb[3] ); void palNut ( double date, double rmatn[3][3] ); void palNutc ( double date, double *dpsi, double *deps, double *eps0 ); void palNutc80 ( double date, double *dpsi, double *deps, double *eps0 ); void palOap ( const char *type, double ob1, double ob2, double date, double dut, double elongm, double phim, double hm, double xp, double yp, double tdk, double pmb, double rh, double wl, double tlr, double *rap, double *dap ); void palOapqk ( const char *type, double ob1, double ob2, const double aoprms[14], double *rap, double *dap ); int palObs( size_t n, const char * c, char * ident, size_t identlen, char * name, size_t namelen, double * w, double * p, double * h ); double palPa ( double ha, double dec, double phi ); double palPav ( float v1[3], float v2[3] ); void palPcd ( double disco, double *x, double *y ); void palPda2h ( double p, double d, double a, double *h1, int *j1, double *h2, int *j2 ); void palPdq2h ( double p, double d, double q, double *h1, int *j1, double *h2, int *j2 ); void palPermut ( int n, int istate[], int iorder[], int *j ); void palPertel (int jform, double date0, double date1, double epoch0, double orbi0, double anode0, double perih0, double aorq0, double e0, double am0, double *epoch1, double *orbi1, double *anode1, double *perih1, double *aorq1, double *e1, double *am1, int *jstat ); void palPertue ( double date, double u[13], int *jstat ); void palPlanel ( double date, int jform, double epoch, double orbinc, double anode, double perih, double aorq, double e, double aorl, double dm, double pv[6], int *jstat ); void palPlanet ( double date, int np, double pv[6], int *j ); void palPlante ( double date, double elong, double phi, int jform, double epoch, double orbinc, double anode, double perih, double aorq, double e, double aorl, double dm, double *ra, double *dec, double *r, int *jstat ); void palPlantu ( double date, double elong, double phi, const double u[13], double *ra, double *dec, double *r, int *jstat ); void palPm ( double r0, double d0, double pr, double pd, double px, double rv, double ep0, double ep1, double *r1, double *d1 ); void palPolmo ( double elongm, double phim, double xp, double yp, double *elong, double *phi, double *daz ); void palPrebn ( double bep0, double bep1, double rmatp[3][3] ); void palPrec ( double ep0, double ep1, double rmatp[3][3] ); void palPrecl ( double ep0, double ep1, double rmatp[3][3] ); void palPreces ( const char sys[3], double ep0, double ep1, double *ra, double *dc ); void palPrenut ( double epoch, double date, double rmatpn[3][3] ); void palPv2el ( const double pv[6], double date, double pmass, int jformr, int *jform, double *epoch, double *orbinc, double *anode, double *perih, double *aorq, double *e, double *aorl, double *dm, int *jstat ); void palPv2ue ( const double pv[6], double date, double pmass, double u[13], int *jstat ); void palPvobs ( double p, double h, double stl, double pv[6] ); void palPxy ( int np, double xye[][2], double xym[][2], double coeffs[6], double xyp[][2], double *xrms, double *yrms, double *rrms ); float palRange ( float angle ); float palRanorm ( float angle ); double palRcc ( double tdb, double ut1, double wl, double u, double v ); void palRdplan ( double date, int np, double elong, double phi, double *ra, double *dec, double *diam ); void palRefco ( double hm, double tdk, double pmb, double rh, double wl, double phi, double tlr, double eps, double *refa, double *refb ); void palRefcoq ( double tdk, double pmb, double rh, double wl, double *refa, double *refb ); void palRefro ( double zobs, double hm, double tdk, double pmb, double rh, double wl, double phi, double tlr, double eps, double *ref ); void palRefv ( double vu[3], double refa, double refb, double vr[3] ); void palRefz ( double zu, double refa, double refb, double *zr ); double palRverot ( double phi, double ra, double da, double st ); double palRvgalc ( double r2000, double d2000 ); double palRvlg ( double r2000, double d2000 ); double palRvlsrd ( double r2000, double d2000 ); double palRvlsrk ( double r2000, double d2000 ); void palS2tp ( float ra, float dec, float raz, float decz, float *xi, float *eta, int *j ); float palSep ( float a1, float b1, float a2, float b2 ); float palSepv ( float v1[3], float v2[3] ); void palSmat ( int n, float *a, float *y, float *d, int *jf, int *iw ); void palSubet ( double rc, double dc, double eq, double *rm, double *dm ); void palSupgal ( double dsl, double dsb, double *dl, double *db ); void palSvd ( int m, int n, int mp, int np, double *a, double *w, double *v, double *work, int *jstat ); void palSvdcov ( int n, int np, int nc, double *w, double *v, double *work, double *cvm ); void palSvdsol ( int m, int n, int mp, int np, double *b, double *u, double *w, double *v, double *work, double *x ); void palTp2s ( float xi, float eta, float raz, float decz, float *ra, float *dec ); void palTp2v ( float xi, float eta, float v0[3], float v[3] ); void palTps2c ( float xi, float eta, float ra, float dec, float *raz1, float *decz1, float *raz2, float *decz2, int *n ); void palTpv2c ( float xi, float eta, float v[3], float v01[3], float v02[3], int *n ); void palUe2el ( const double u[13], int jformr, int *jform, double *epoch, double *orbinc, double *anode, double *perih, double *aorq, double *e, double *aorl, double *dm, int *jstat ); void palUe2pv ( double date, double u[13], double pv[], int *jstat ); void palUnpcd ( double disco, double *x, double *y ); void palV2tp ( float v[3], float v0[3], float *xi, float *eta, int *j ); float palVdv ( float va[3], float vb[3] ); void palVn ( float v[3], float uv[3], float *vm ); void palVxv ( float va[3], float vb[3], float vc[3] ); void palXy2xy ( double x1, double y1, double coeffs[6], double *x2, double *y2 ); double palZd ( double ha, double dec, double phi ); #ifdef __cplusplus } #endif #endif pal-0.5.0/pal.news000644 000765 000024 00000003735 12366007502 014061 0ustar00timjstaff000000 000000 PAL Library The Starlink Positional Astronomy Library (PAL) is a C implementation of the SLALIB API. It is distributed under the GPL and uses the SOFA library wherever possible. V0.5.0 Now works with ERFA . The configure script has been modified to first check for ERFA and then check for SOFA. V0.4.0 New routines ported from SLA: palRefv, palAtmdsp New routine inherited from SOFA: palRefcoq Minimum SOFA version now 2013-12-02 palObs: Now includes telescope positions for APEX and NANTEN2 The autotools build scripts now require autoconf version 2.69. Thanks to Github user @nega0 for some BSD build fixes. A subset of the routines have been relicensed using LGPL to allow them to be included in the AST library. Thanks to Patrick Wallace for giving this permission. A paper on PAL has been published at ADASS: http://adsabs.harvard.edu/abs/2013ASPC..475..307J V0.3.0 Add refraction code and support palOap and palAop. For closer compatibility with SLA for testing purposes the refraction routines internally use clones of slaNutc, slaEqeqx, slaGmst and slaGeoc. Once the code has been verified further the PAL/SOFA routines will be used instead. Switching routines seems to change the results in palTest by about 0.05 arcsec. V0.2.0 Improve configure script when not in a Starlink build environment. Use ./configure --prefix=/path/to/install when Starlink is not available and add --without-starlink if Starlink is present but should not be used. V0.1.5 Explcitly look for libm rather than relying on SOFA to pull it in. V0.1.4 Check for isblank() function and fall back if it is missing. V0.1.3 Improve copysign() detection. V0.1.2 Check for copysign() c99 function and fall back if it is missing. V0.1.1 The palDrange function has been modified so that it now returns +PI if the supplied angle is +PI (previously, it returned -PI in these cases). V0.1.0 Initial release with sufficient SLALIB API for AST and the Astro::Coords perl module. pal-0.5.0/pal1.h000644 000765 000024 00000003522 12360544345 013414 0ustar00timjstaff000000 000000 /* *+ * Name: * pal1.h * Purpose: * Definitions of private PAL functions * Language: * Starlink ANSI C * Type of Module: * Include file * Invocation: * #include "pal1.h" * Description: * Function prototypes for private PAL functions. Will not be * installed. * Authors: * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * History: * 2012-08-24 (TIMJ): * Initial version * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #ifndef PAL1HDEF #define PAL1HDEF void pal1Atms ( double rt, double tt, double dnt, double gamal, double r, double * dn, double * rdndr ); void pal1Atmt ( double r0, double t0, double alpha, double gamm2, double delm2, double c1, double c2, double c3, double c4, double c5, double c6, double r, double *t, double *dn, double *rdndr ); #endif pal-0.5.0/pal1Atms.c000644 000765 000024 00000005017 12366000607 014227 0ustar00timjstaff000000 000000 /* *+ * Name: * pal1Atms * Purpose: * Calculate stratosphere parameters * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void pal1Atms ( double rt, double tt, double dnt, double gamal, * double r, double * dn, double * rdndr ); * Arguments: * rt = double (Given) * Height of the tropopause from centre of the Earth (metre) * tt = double (Given) * Temperature at the tropopause (K) * dnt = double (Given) * Refractive index at the tropopause * gamal = double (Given) * Constant of the atmospheric model = G*MD/R * r = double (Given) * Current distance from the centre of the Earth (metre) * dn = double * (Returned) * Refractive index at r * rdndr = double * (Returned) * r * rate the refractive index is changing at r * Description: * Refractive index and derivative with respect to height for the * stratosphere. * Authors: * TIMJ: Tim Jenness (JAC, Hawaii) * PTW: Patrick T. Wallace * {enter_new_authors_here} * Notes: * - Internal routine used by palRefro. * History: * 2012-08-24 (TIMJ): * Initial version * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2004 Patrick T. Wallace * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include #include "pal1.h" void pal1Atms ( double rt, double tt, double dnt, double gamal, double r, double * dn, double * rdndr ) { double b; double w; b = gamal / tt; w = (dnt - 1.0) * exp( -b * (r-rt) ); *dn = 1.0 + w; *rdndr = -r * b * w; } pal-0.5.0/pal1Atmt.c000644 000765 000024 00000007103 12366000607 014226 0ustar00timjstaff000000 000000 /* *+ * Name: * pal1Atmt * Purpose: * Calculate troposphere parameters * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void pal1Atmt ( double r0, double t0, double alpha, double gamm2, * double delm2, double c1, double c2, double c3, * double c4, double c5, double c6, double r, * double *t, double *dn, double *rdndr ); * Arguments: * r0 = double (Given) * Height of observer from centre of the Earth (metre) * t0 = double (Given) * Temperature of the observer (K) * alpha = double (Given) * Alpha (see HMNAO paper) * gamm2 = double (Given) * Gamma minus 2 (see HMNAO paper) * delm2 = double (Given) * Delta minus 2 (see HMNAO paper) * c1 = double (Given) * Useful term (see palRefro source) * c2 = double (Given) * Useful term (see palRefro source) * c3 = double (Given) * Useful term (see palRefro source) * c4 = double (Given) * Useful term (see palRefro source) * c5 = double (Given) * Useful term (see palRefro source) * c6 = double (Given) * Useful term (see palRefro source) * r = double (Given) * Current distance from the centre of the Earth (metre) * t = double * (Returned) * Temperature at r (K) * dn = double * (Returned) * Refractive index at r. * rdndr = double * (Returned) * r * rate the refractive index is changing at r. * Description: * Refractive index and derivative with respect to height for * the troposphere. * Authors: * TIMJ: Tim Jenness (JAC, Hawaii) * PTW: Patrick T. Wallace * {enter_new_authors_here} * Notes: * - Internal routine used by palRefro * - Note that in the optical case c5 and c6 are zero. * History: * 2012-08-24 (TIMJ): * Initial version, copied from Fortran SLA source. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2004 Patrick T. Wallace * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include #include "palmac.h" #include "pal1.h" void pal1Atmt ( double r0, double t0, double alpha, double gamm2, double delm2, double c1, double c2, double c3, double c4, double c5, double c6, double r, double *t, double *dn, double *rdndr ) { double tt0; double tt0gm2; double tt0dm2; *t = DMAX( DMIN( t0 - alpha*(r-r0), 320.0), 100.0 ); tt0 = *t / t0; tt0gm2 = pow( tt0, gamm2 ); tt0dm2 = pow( tt0, delm2 ); *dn = 1.0 + ( c1 * tt0gm2 - ( c2 - c5 / *t ) * tt0dm2 ) * tt0; *rdndr = r * ( -c3 * tt0gm2 + ( c4 - c6 / tt0 ) * tt0dm2 ); } pal-0.5.0/pal1sofa.h000644 000765 000024 00000006271 12366005320 014260 0ustar00timjstaff000000 000000 /* *+ * Name: * pal1sofa.h * Purpose: * Mappings of ERFA names to SOFA names * Language: * Starlink ANSI C * Type of Module: * Include file * Invocation: * #include "pal1.h" * Description: * PAL will work with both SOFA and ERFA libraries and the * difference is generally a change in prefix. This include * file maps the ERFA form of functions to the SOFA form * and includes the relevant sofa.h vs erfa.h file. * Authors: * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - PAL uses the ERFA form by default. * History: * 2014-07-29 (TIMJ): * Initial version * {enter_further_changes_here} * Copyright: * Copyright (C) 2014 Tim Jenness * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #ifndef PAL1SOFAHDEF #define PAL1SOFAHDEF #include # if HAVE_SOFA_H # include "sofa.h" # include "sofam.h" /* Must replace ERFA with SOFA */ # define eraA2af iauA2af # define eraA2tf iauA2tf # define eraAf2a iauAf2a # define eraAnp iauAnp # define eraAnpm iauAnpm # define eraC2s iauC2s # define eraCal2jd iauCal2jd # define eraD2tf iauD2tf # define eraDat iauDat # define eraEe06a iauEe06a # define eraEpb iauEpb # define eraEpb2jd iauEpb2jd # define eraEpj iauEpj # define eraEpj2jd iauEpj2jd # define eraEpv00 iauEpv00 # define eraFk5hz iauFk5hz # define eraGd2gc iauGd2gc # define eraGmst06 iauGmst06 # define eraHfk5z iauHfk5z # define eraIr iauIr # define eraJd2cal iauJd2cal # define eraNut06a iauNut06a # define eraObl06 iauObl06 # define eraP06e iauP06e # define eraPap iauPap # define eraPas iauPas # define eraPdp iauPdp # define eraPlan94 iauPlan94 # define eraPmat06 iauPmat06 # define eraPn iauPn # define eraPnm06a iauPnm06a # define eraPxp iauPxp # define eraRefco iauRefco # define eraRm2v iauRm2v # define eraRv2m iauRv2m # define eraRx iauRx # define eraRxp iauRxp # define eraRxpv iauRxpv # define eraRxr iauRxr # define eraRy iauRy # define eraRz iauRz # define eraS2c iauS2c # define eraSepp iauSepp # define eraSeps iauSeps # define eraStarpm iauStarpm # define eraTf2a iauTf2a # define eraTf2d iauTf2d # define eraTr iauTr # define eraTrxp iauTrxp /* These are from sofam.h */ # define ERFA_WGS84 WGS84 # define ERFA_DJ00 DJ00 # define ERFA_DJY DJY # define ERFA_DAU DAU # else # include "erfa.h" # include "erfam.h" /* No further action required */ # endif #endif pal-0.5.0/palAddet.c000644 000765 000024 00000005756 12366000612 014271 0ustar00timjstaff000000 000000 /* *+ * Name: * palAddet * Purpose: * Add the E-terms to a pre IAU 1976 mean place * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palAddet ( double rm, double dm, double eq, * double *rc, double *dc ); * Arguments: * rm = double (Given) * RA without E-terms (radians) * dm = double (Given) * Dec without E-terms (radians) * eq = double (Given) * Besselian epoch of mean equator and equinox * rc = double * (Returned) * RA with E-terms included (radians) * dc = double * (Returned) * Dec with E-terms included (radians) * Description: * Add the E-terms (elliptic component of annual aberration) * to a pre IAU 1976 mean place to conform to the old * catalogue convention. * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * Most star positions from pre-1984 optical catalogues (or * derived from astrometry using such stars) embody the * E-terms. If it is necessary to convert a formal mean * place (for example a pulsar timing position) to one * consistent with such a star catalogue, then the RA,Dec * should be adjusted using this routine. * See Also: * Explanatory Supplement to the Astronomical Ephemeris, * section 2D, page 48. * History: * 2012-02-12(TIMJ): * Initial version with documentation taken from Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1999 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "pal1sofa.h" void palAddet ( double rm, double dm, double eq, double *rc, double *dc ) { double a[3]; /* The E-terms */ double v[3]; int i; /* Note the preference for IAU routines */ /* Retrieve the E-terms */ palEtrms( eq, a ); /* Spherical to Cartesian */ eraS2c( rm, dm, v ); /* Include the E-terms */ for (i=0; i<3; i++) { v[i] += a[i]; } /* Cartesian to spherical */ eraC2s( v, rc, dc ); /* Bring RA into conventional range */ *rc = eraAnp( *rc ); } pal-0.5.0/palAirmas.c000644 000765 000024 00000006035 12366000607 014457 0ustar00timjstaff000000 000000 /* *+ * Name: * palAirmas * Purpose: * Air mass at given zenith distance * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * double palAirmas( double zd ); * Arguments: * zd = double (Given) * Observed zenith distance (radians) * Description: * Calculates the airmass at the observed zenith distance. * Authors: * PTW: Patrick Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - The "observed" zenith distance referred to above means "as * affected by refraction". * - Uses Hardie's (1962) polynomial fit to Bemporad's data for * the relative air mass, X, in units of thickness at the zenith * as tabulated by Schoenberg (1929). This is adequate for all * normal needs as it is accurate to better than 0.1% up to X = * 6.8 and better than 1% up to X = 10. Bemporad's tabulated * values are unlikely to be trustworthy to such accuracy * because of variations in density, pressure and other * conditions in the atmosphere from those assumed in his work. * - The sign of the ZD is ignored. * - At zenith distances greater than about ZD = 87 degrees the * air mass is held constant to avoid arithmetic overflows. * See Also: * - Hardie, R.H., 1962, in "Astronomical Techniques" * ed. W.A. Hiltner, University of Chicago Press, p180. * - Schoenberg, E., 1929, Hdb. d. Ap., * Berlin, Julius Springer, 2, 268. * History: * 2012-03-02 (TIMJ): * Initial version from the SLA/F version including documentation. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1999 Rutherford Appleton Laboratory. * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "palmac.h" double palAirmas ( double zd ) { double seczm1; double airmass; /* Have maximum zenith distance of 87 deg */ const double MAXZD = 87.0 * PAL__DD2R; zd = fabs(zd); zd = ( zd > MAXZD ? MAXZD : zd ); seczm1 = (1.0 / cos(zd)) - 1.0; airmass = 1.0 + seczm1*(0.9981833 - seczm1*(0.002875 + 0.0008083*seczm1)); return airmass; } pal-0.5.0/palAmp.c000644 000765 000024 00000004532 12366000607 013760 0ustar00timjstaff000000 000000 /* *+ * Name: * palAmp * Purpose: * Convert star RA,Dec from geocentric apparaent to mean place. * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palAmp ( double ra, double da, double date, double eq, * double *rm, double *dm ); * Arguments: * ra = double (Given) * Apparent RA (radians) * dec = double (Given) * Apparent Dec (radians) * date = double (Given) * TDB for apparent place (JD-2400000.5) * eq = double (Given) * Equinox: Julian epoch of mean place. * rm = double * (Returned) * Mean RA (radians) * dm = double * (Returned) * Mean Dec (radians) * Description: * Convert star RA,Dec from geocentric apparent to mean place. The * mean coordinate system is close to ICRS. See palAmpqk for details. * Authors: * TIMJ: Tim Jenness (JAC, Hawaii) * PTW: Patrick T. Wallace * {enter_new_authors_here} * Notes: * - See palMappa and palAmpqk for details. * History: * 2012-03-02 (TIMJ): * Initial version * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2001 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" void palAmp ( double ra, double da, double date, double eq, double *rm, double *dm ) { double amprms[21]; palMappa( eq, date, amprms ); palAmpqk( ra, da, amprms, rm, dm ); } pal-0.5.0/palAmpqk.c000644 000765 000024 00000007206 12366000612 014311 0ustar00timjstaff000000 000000 /* *+ * Name: * palAmpqk * Purpose: * Convert star RA,Dec from geocentric apparent to mean place. * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palAmpqk ( double ra, double da, double amprms[21], * double *rm, double *dm ) * Arguments: * ra = double (Given) * Apparent RA (radians). * da = double (Given) * Apparent Dec (radians). * amprms = double[21] (Given) * Star-independent mean-to-apparent parameters (see palMappa): * (0) time interval for proper motion (Julian years) * (1-3) barycentric position of the Earth (AU) * (4-6) not used * (7) not used * (8-10) abv: barycentric Earth velocity in units of c * (11) sqrt(1-v*v) where v=modulus(abv) * (12-20) precession/nutation (3,3) matrix * rm = double (Returned) * Mean RA (radians). * dm = double (Returned) * Mean Dec (radians). * Description: * Convert star RA,Dec from geocentric apparent to mean place. The "mean" * coordinate system is in fact close to ICRS. Use of this function * is appropriate when efficiency is important and where many star * positions are all to be transformed for one epoch and equinox. The * star-independent parameters can be obtained by calling the palMappa * function. * Authors: * PTW: Pat Wallace (STFC) * {enter_new_authors_here} * History: * 2012-02-13 (PTW): * Initial version. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2000 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "pal1sofa.h" void palAmpqk ( double ra, double da, double amprms[21], double *rm, double *dm ){ /* Local Variables: */ double ab1; /* sqrt(1-v*v) where v=modulus of Earth vel */ double abv[3]; /* Earth velocity wrt SSB (c, FK5) */ double p1[3], p2[3], p3[3]; /* work vectors */ double ab1p1, p1dv, p1dvp1, w; int i, j; /* Unpack some of the parameters */ ab1 = amprms[11]; for( i = 0; i < 3; i++ ) { abv[i] = amprms[i + 8]; } /* Apparent RA,Dec to Cartesian */ eraS2c( ra, da, p3 ); /* Precession and nutation */ eraTrxp( (double(*)[3]) &rms[12], p3, p2 ); /* Aberration */ ab1p1 = ab1 + 1.0; for( i = 0; i < 3; i++ ) { p1[i] = p2[i]; } for( j = 0; j < 2; j++ ) { p1dv = eraPdp( p1, abv ); p1dvp1 = 1.0 + p1dv; w = 1.0 + p1dv / ab1p1; for( i = 0; i < 3; i++ ) { p1[i] = ( p1dvp1 * p2[i] - w * abv[i] ) / ab1; } eraPn( p1, &w, p3 ); for( i = 0; i < 3; i++ ) { p1[i] = p3[i]; } } /* Mean RA,Dec */ eraC2s( p1, rm, dm ); *rm = eraAnp( *rm ); } pal-0.5.0/palAop.c000644 000765 000024 00000024025 12366000607 013761 0ustar00timjstaff000000 000000 /* *+ * Name: * palAop * Purpose: * Apparent to observed place * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palAop ( double rap, double dap, double date, double dut, * double elongm, double phim, double hm, double xp, * double yp, double tdk, double pmb, double rh, * double wl, double tlr, * double *aob, double *zob, double *hob, * double *dob, double *rob ); * Arguments: * rap = double (Given) * Geocentric apparent right ascension * dap = double (Given) * Geocentirc apparent declination * date = double (Given) * UTC date/time (Modified Julian Date, JD-2400000.5) * dut = double (Given) * delta UT: UT1-UTC (UTC seconds) * elongm = double (Given) * Mean longitude of the observer (radians, east +ve) * phim = double (Given) * Mean geodetic latitude of the observer (radians) * hm = double (Given) * Observer's height above sea level (metres) * xp = double (Given) * Polar motion x-coordinates (radians) * yp = double (Given) * Polar motion y-coordinates (radians) * tdk = double (Given) * Local ambient temperature (K; std=273.15) * pmb = double (Given) * Local atmospheric pressure (mb; std=1013.25) * rh = double (Given) * Local relative humidity (in the range 0.0-1.0) * wl = double (Given) * Effective wavelength (micron, e.g. 0.55) * tlr = double (Given) * Tropospheric laps rate (K/metre, e.g. 0.0065) * aob = double * (Returned) * Observed azimuth (radians: N=0; E=90) * zob = double * (Returned) * Observed zenith distance (radians) * hob = double * (Returned) * Observed Hour Angle (radians) * dob = double * (Returned) * Observed Declination (radians) * rob = double * (Returned) * Observed Right Ascension (radians) * Description: * Apparent to observed place for sources distant from the solar system. * Authors: * PTW: Patrick T. Wallace * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - This routine returns zenith distance rather than elevation * in order to reflect the fact that no allowance is made for * depression of the horizon. * * - The accuracy of the result is limited by the corrections for * refraction. Providing the meteorological parameters are * known accurately and there are no gross local effects, the * predicted apparent RA,Dec should be within about 0.1 arcsec * for a zenith distance of less than 70 degrees. Even at a * topocentric zenith distance of 90 degrees, the accuracy in * elevation should be better than 1 arcmin; useful results * are available for a further 3 degrees, beyond which the * palRefro routine returns a fixed value of the refraction. * The complementary routines palAop (or palAopqk) and palOap * (or palOapqk) are self-consistent to better than 1 micro- * arcsecond all over the celestial sphere. * * - It is advisable to take great care with units, as even * unlikely values of the input parameters are accepted and * processed in accordance with the models used. * * - "Apparent" place means the geocentric apparent right ascension * and declination, which is obtained from a catalogue mean place * by allowing for space motion, parallax, precession, nutation, * annual aberration, and the Sun's gravitational lens effect. For * star positions in the FK5 system (i.e. J2000), these effects can * be applied by means of the palMap etc routines. Starting from * other mean place systems, additional transformations will be * needed; for example, FK4 (i.e. B1950) mean places would first * have to be converted to FK5, which can be done with the * palFk425 etc routines. * * - "Observed" Az,El means the position that would be seen by a * perfect theodolite located at the observer. This is obtained * from the geocentric apparent RA,Dec by allowing for Earth * orientation and diurnal aberration, rotating from equator * to horizon coordinates, and then adjusting for refraction. * The HA,Dec is obtained by rotating back into equatorial * coordinates, using the geodetic latitude corrected for polar * motion, and is the position that would be seen by a perfect * equatorial located at the observer and with its polar axis * aligned to the Earth's axis of rotation (n.b. not to the * refracted pole). Finally, the RA is obtained by subtracting * the HA from the local apparent ST. * * - To predict the required setting of a real telescope, the * observed place produced by this routine would have to be * adjusted for the tilt of the azimuth or polar axis of the * mounting (with appropriate corrections for mount flexures), * for non-perpendicularity between the mounting axes, for the * position of the rotator axis and the pointing axis relative * to it, for tube flexure, for gear and encoder errors, and * finally for encoder zero points. Some telescopes would, of * course, exhibit other properties which would need to be * accounted for at the appropriate point in the sequence. * * - This routine takes time to execute, due mainly to the * rigorous integration used to evaluate the refraction. * For processing multiple stars for one location and time, * call palAoppa once followed by one call per star to palAopqk. * Where a range of times within a limited period of a few hours * is involved, and the highest precision is not required, call * palAoppa once, followed by a call to palAoppat each time the * time changes, followed by one call per star to palAopqk. * * - The DATE argument is UTC expressed as an MJD. This is, * strictly speaking, wrong, because of leap seconds. However, * as long as the delta UT and the UTC are consistent there * are no difficulties, except during a leap second. In this * case, the start of the 61st second of the final minute should * begin a new MJD day and the old pre-leap delta UT should * continue to be used. As the 61st second completes, the MJD * should revert to the start of the day as, simultaneously, * the delta UTC changes by one second to its post-leap new value. * * - The delta UT (UT1-UTC) is tabulated in IERS circulars and * elsewhere. It increases by exactly one second at the end of * each UTC leap second, introduced in order to keep delta UT * within +/- 0.9 seconds. * * - IMPORTANT -- TAKE CARE WITH THE LONGITUDE SIGN CONVENTION. * The longitude required by the present routine is east-positive, * in accordance with geographical convention (and right-handed). * In particular, note that the longitudes returned by the * palObs routine are west-positive, following astronomical * usage, and must be reversed in sign before use in the present * routine. * * - The polar coordinates XP,YP can be obtained from IERS * circulars and equivalent publications. The maximum amplitude * is about 0.3 arcseconds. If XP,YP values are unavailable, * use XP=YP=0.0. See page B60 of the 1988 Astronomical Almanac * for a definition of the two angles. * * - The height above sea level of the observing station, HM, * can be obtained from the Astronomical Almanac (Section J * in the 1988 edition), or via the routine palObs. If P, * the pressure in millibars, is available, an adequate * estimate of HM can be obtained from the expression * * HM ~ -29.3*TSL*LOG(P/1013.25). * * where TSL is the approximate sea-level air temperature in K * (see Astrophysical Quantities, C.W.Allen, 3rd edition, * section 52). Similarly, if the pressure P is not known, * it can be estimated from the height of the observing * station, HM, as follows: * * P ~ 1013.25*EXP(-HM/(29.3*TSL)). * * Note, however, that the refraction is nearly proportional to the * pressure and that an accurate P value is important for precise * work. * * - The azimuths etc produced by the present routine are with * respect to the celestial pole. Corrections to the terrestrial * pole can be computed using palPolmo. * History: * 2012-08-25 (TIMJ): * Initial version * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2005 Patrick T. Wallace * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" void palAop ( double rap, double dap, double date, double dut, double elongm, double phim, double hm, double xp, double yp, double tdk, double pmb, double rh, double wl, double tlr, double *aob, double *zob, double *hob, double *dob, double *rob ) { double aoprms[14]; palAoppa(date,dut,elongm,phim,hm,xp,yp,tdk,pmb,rh,wl,tlr, aoprms); palAopqk(rap,dap,aoprms,aob,zob,hob,dob,rob); } pal-0.5.0/palAoppa.c000644 000765 000024 00000255350 12366000607 014311 0ustar00timjstaff000000 000000 /* *+ * Name: * palAoppa * Purpose: * Precompute apparent to observed place parameters * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palAoppa ( double date, double dut, double elongm, double phim, * double hm, double xp, double yp, double tdk, double pmb, * double rh, double wl, double tlr, double aoprms[14] ); * Arguments: * date = double (Given) * UTC date/time (modified Julian Date, JD-2400000.5) * dut = double (Given) * delta UT: UT1-UTC (UTC seconds) * elongm = double (Given) * mean longitude of the observer (radians, east +ve) * phim = double (Given) * mean geodetic latitude of the observer (radians) * hm = double (Given) * observer's height above sea level (metres) * xp = double (Given) * polar motion x-coordinate (radians) * yp = double (Given) * polar motion y-coordinate (radians) * tdk = double (Given) * local ambient temperature (K; std=273.15) * pmb = double (Given) * local atmospheric pressure (mb; std=1013.25) * rh = double (Given) * local relative humidity (in the range 0.0-1.0) * wl = double (Given) * effective wavelength (micron, e.g. 0.55) * tlr = double (Given) * tropospheric lapse rate (K/metre, e.g. 0.0065) * aoprms = double [14] (Returned) * Star-independent apparent-to-observed parameters * * (0) geodetic latitude (radians) * (1,2) sine and cosine of geodetic latitude * (3) magnitude of diurnal aberration vector * (4) height (hm) * (5) ambient temperature (tdk) * (6) pressure (pmb) * (7) relative humidity (rh) * (8) wavelength (wl) * (9) lapse rate (tlr) * (10,11) refraction constants A and B (radians) * (12) longitude + eqn of equinoxes + sidereal DUT (radians) * (13) local apparent sidereal time (radians) * Description: * Precompute apparent to observed place parameters required by palAopqk * and palOapqk. * Authors: * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - It is advisable to take great care with units, as even * unlikely values of the input parameters are accepted and * processed in accordance with the models used. * * - The DATE argument is UTC expressed as an MJD. This is, * strictly speaking, improper, because of leap seconds. However, * as long as the delta UT and the UTC are consistent there * are no difficulties, except during a leap second. In this * case, the start of the 61st second of the final minute should * begin a new MJD day and the old pre-leap delta UT should * continue to be used. As the 61st second completes, the MJD * should revert to the start of the day as, simultaneously, * the delta UTC changes by one second to its post-leap new value. * * - The delta UT (UT1-UTC) is tabulated in IERS circulars and * elsewhere. It increases by exactly one second at the end of * each UTC leap second, introduced in order to keep delta UT * within +/- 0.9 seconds. * * - IMPORTANT -- TAKE CARE WITH THE LONGITUDE SIGN CONVENTION. * The longitude required by the present routine is east-positive, * in accordance with geographical convention (and right-handed). * In particular, note that the longitudes returned by the * palObs routine are west-positive, following astronomical * usage, and must be reversed in sign before use in the present * routine. * * - The polar coordinates XP,YP can be obtained from IERS * circulars and equivalent publications. The maximum amplitude * is about 0.3 arcseconds. If XP,YP values are unavailable, * use XP=YP=0.0. See page B60 of the 1988 Astronomical Almanac * for a definition of the two angles. * * - The height above sea level of the observing station, HM, * can be obtained from the Astronomical Almanac (Section J * in the 1988 edition), or via the routine palObs. If P, * the pressure in millibars, is available, an adequate * estimate of HM can be obtained from the expression * * HM ~ -29.3*TSL*log(P/1013.25). * * where TSL is the approximate sea-level air temperature in K * (see Astrophysical Quantities, C.W.Allen, 3rd edition, * section 52). Similarly, if the pressure P is not known, * it can be estimated from the height of the observing * station, HM, as follows: * * P ~ 1013.25*exp(-HM/(29.3*TSL)). * * Note, however, that the refraction is nearly proportional to the * pressure and that an accurate P value is important for precise * work. * * - Repeated, computationally-expensive, calls to palAoppa for * times that are very close together can be avoided by calling * palAoppa just once and then using palAoppat for the subsequent * times. Fresh calls to palAoppa will be needed only when * changes in the precession have grown to unacceptable levels or * when anything affecting the refraction has changed. * History: * 2012-08-24 (TIMJ): * Initial version, ported directly from Fortran SLA. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include "math.h" #include "pal.h" #include "palmac.h" /* These are local SLA implementations to aid in testing. Switch * to native PAL implementations when tests are complete. */ static void pal__Geoc( double p, double h, double *r, double * z ); static void pal__Nutc ( double date, double * dpsi, double *deps, double * eps0 ); static double pal__Eqeqx( double date ); void palAoppa ( double date, double dut, double elongm, double phim, double hm, double xp, double yp, double tdk, double pmb, double rh, double wl, double tlr, double aoprms[14] ) { /* Constants */ const double C = 173.14463331; /* Speed of light (AU per day) */ const double SOLSID = 1.0027379093; /* Ratio between solar and sidereal time */ /* Local variables */ double cphim,xt,yt,zt,xc,yc,zc,elong,phi,uau,vau; /* Observer's location corrected for polar motion */ cphim = cos(phim); xt = cos(elongm)*cphim; yt = sin(elongm)*cphim; zt = sin(phim); xc = xt-xp*zt; yc = yt+yp*zt; zc = xp*xt-yp*yt+zt; if (xc == 0.0 && yc == 0.0) { elong = 0.0; } else { elong = atan2(yc,xc); } phi = atan2(zc,sqrt(xc*xc+yc*yc)); aoprms[0] = phi; aoprms[1] = sin(phi); aoprms[2] = cos(phi); /* magnitude of the diurnal aberration vector */ pal__Geoc(phi,hm,&uau,&vau); aoprms[3] = PAL__D2PI*uau*SOLSID/C; /* copy the refraction parameters and compute the a & b constants */ aoprms[4] = hm; aoprms[5] = tdk; aoprms[6] = pmb; aoprms[7] = rh; aoprms[8] = wl; aoprms[9] = tlr; palRefco(hm,tdk,pmb,rh,wl,phi,tlr,1e-10, &aoprms[10],&aoprms[11]); /* longitude + equation of the equinoxes + sidereal equivalent of DUT * (ignoring change in equation of the equinoxes between UTC and TDB) */ aoprms[12] = elong+pal__Eqeqx(date)+dut*SOLSID*PAL__DS2R; /* sidereal time */ palAoppat(date,aoprms); } /* Private reimplementation of slaEqeqx for testing the algorithm */ #include static void pal__Geoc( double p, double h, double *r, double * z ) { /* earth equatorial radius (metres) */ const double A0=6378140.0; /* reference spheroid flattening factor and useful function */ const double f = 1.0/298.257; double b; /* astronomical unit in metres */ const double AU = 1.49597870e11; double sp,cp,c,s; b = pow( 1.0-f, 2.0 ); /* geodetic to geocentric conversion */ sp = sin(p); cp = cos(p); c = 1.0/sqrt(cp*cp+b*sp*sp); s = b*c; *r = (A0*c+h)*cp/AU; *z = (A0*s+h)*sp/AU; } static double pal__Eqeqx( double date ) { const double T2AS=1296000.0; double sla_eqeqx; double t, om, dpsi, deps, eps0; /* interval between basic epoch j2000.0 and current epoch (jc) */ t=(date-51544.5)/36525.0; /* longitude of the mean ascending node of the lunar orbit on the * ecliptic, measured from the mean equinox of date */ om=PAL__DAS2R*(450160.280+(-5.0*T2AS-482890.539 +(7.455+0.008*t)*t)*t); /* nutation */ pal__Nutc(date,&dpsi,&deps,&eps0); /* equation of the equinoxes */ sla_eqeqx=dpsi*cos(eps0)+PAL__DAS2R*(0.00264*sin(om)+ 0.000063*sin(om+om)); return sla_eqeqx; } #include "palmac.h" static void pal__Nutc ( double date, double * dpsi, double *deps, double * eps0 ) { const double DJC = 36525.0; const double DJM0 = 51544.5; const double TURNAS = 1296000.0; #define NTERMS 194 int j; double t,el,elp,f,d,om,ve,ma,ju,sa,theta,c,s,dp,de; int na[ 194 ][9] = { { 0 , 0 , 0 , 0 , -1 , 0 , 0 , 0 , 0 }, { 0 , 0 , 2 , -2 , 2 , 0 , 0 , 0 , 0 }, { 0 , 0 , 2 , 0 , 2 , 0 , 0 , 0 , 0 }, { 0 , 0 , 0 , 0 , -2 , 0 , 0 , 0 , 0 }, { 0 , 1 , 0 , 0 , 0 , 0 , 0 , 0 , 0 }, { 0 , 1 , 2 , -2 , 2 , 0 , 0 , 0 , 0 }, { 1 , 0 , 0 , 0 , 0 , 0 , 0 , 0 , 0 }, { 0 , 0 , 2 , 0 , 1 , 0 , 0 , 0 , 0 }, { 1 , 0 , 2 , 0 , 2 , 0 , 0 , 0 , 0 }, { 0 , -1 , 2 , -2 , 2 , 0 , 0 , 0 , 0 }, { 0 , 0 , 2 , -2 , 1 , 0 , 0 , 0 , 0 }, { -1 , 0 , 2 , 0 , 2 , 0 , 0 , 0 , 0 }, { -1 , 0 , 0 , 2 , 0 , 0 , 0 , 0 , 0 }, { 1 , 0 , 0 , 0 , 1 , 0 , 0 , 0 , 0 }, { 1 , 0 , 0 , 0 , -1 , 0 , 0 , 0 , 0 }, { -1 , 0 , 2 , 2 , 2 , 0 , 0 , 0 , 0 }, { 1 , 0 , 2 , 0 , 1 , 0 , 0 , 0 , 0 }, { -2 , 0 , 2 , 0 , 1 , 0 , 0 , 0 , 0 }, { 0 , 0 , 0 , 2 , 0 , 0 , 0 , 0 , 0 }, { 0 , 0 , 2 , 2 , 2 , 0 , 0 , 0 , 0 }, { 2 , 0 , 0 , -2 , 0 , 0 , 0 , 0 , 0 }, { 2 , 0 , 2 , 0 , 2 , 0 , 0 , 0 , 0 }, { 1 , 0 , 2 , -2 , 2 , 0 , 0 , 0 , 0 }, { -1 , 0 , 2 , 0 , 1 , 0 , 0 , 0 , 0 }, { 2 , 0 , 0 , 0 , 0 , 0 , 0 , 0 , 0 }, { 0 , 0 , 2 , 0 , 0 , 0 , 0 , 0 , 0 }, { 0 , 1 , 0 , 0 , 1 , 0 , 0 , 0 , 0 }, { -1 , 0 , 0 , 2 , 1 , 0 , 0 , 0 , 0 }, { 0 , 2 , 2 , -2 , 2 , 0 , 0 , 0 , 0 }, { 0 , 0 , 2 , -2 , 0 , 0 , 0 , 0 , 0 }, { -1 , 0 , 0 , 2 , -1 , 0 , 0 , 0 , 0 }, { 0 , 1 , 0 , 0 , -1 , 0 , 0 , 0 , 0 }, { 0 , 2 , 0 , 0 , 0 , 0 , 0 , 0 , 0 }, { -1 , 0 , 2 , 2 , 1 , 0 , 0 , 0 , 0 }, { 1 , 0 , 2 , 2 , 2 , 0 , 0 , 0 , 0 }, { 0 , 1 , 2 , 0 , 2 , 0 , 0 , 0 , 0 }, { -2 , 0 , 2 , 0 , 0 , 0 , 0 , 0 , 0 }, { 0 , 0 , 2 , 2 , 1 , 0 , 0 , 0 , 0 }, { 0 , -1 , 2 , 0 , 2 , 0 , 0 , 0 , 0 }, { 0 , 0 , 0 , 2 , 1 , 0 , 0 , 0 , 0 }, { 1 , 0 , 2 , -2 , 1 , 0 , 0 , 0 , 0 }, { 2 , 0 , 0 , -2 , -1 , 0 , 0 , 0 , 0 }, { 2 , 0 , 2 , -2 , 2 , 0 , 0 , 0 , 0 }, { 2 , 0 , 2 , 0 , 1 , 0 , 0 , 0 , 0 }, { 0 , 0 , 0 , 2 , -1 , 0 , 0 , 0 , 0 }, { 0 , -1 , 2 , -2 , 1 , 0 , 0 , 0 , 0 }, { -1 , -1 , 0 , 2 , 0 , 0 , 0 , 0 , 0 }, { 2 , 0 , 0 , -2 , 1 , 0 , 0 , 0 , 0 }, { 1 , 0 , 0 , 2 , 0 , 0 , 0 , 0 , 0 }, { 0 , 1 , 2 , -2 , 1 , 0 , 0 , 0 , 0 }, { 1 , -1 , 0 , 0 , 0 , 0 , 0 , 0 , 0 }, { -2 , 0 , 2 , 0 , 2 , 0 , 0 , 0 , 0 }, { 0 , -1 , 0 , 2 , 0 , 0 , 0 , 0 , 0 }, { 3 , 0 , 2 , 0 , 2 , 0 , 0 , 0 , 0 }, { 0 , 0 , 0 , 1 , 0 , 0 , 0 , 0 , 0 }, { 1 , -1 , 2 , 0 , 2 , 0 , 0 , 0 , 0 }, { 1 , 0 , 0 , -1 , 0 , 0 , 0 , 0 , 0 }, { -1 , -1 , 2 , 2 , 2 , 0 , 0 , 0 , 0 }, { -1 , 0 , 2 , 0 , 0 , 0 , 0 , 0 , 0 }, { 2 , 0 , 0 , 0 , -1 , 0 , 0 , 0 , 0 }, { 0 , -1 , 2 , 2 , 2 , 0 , 0 , 0 , 0 }, { 1 , 1 , 2 , 0 , 2 , 0 , 0 , 0 , 0 }, { 2 , 0 , 0 , 0 , 1 , 0 , 0 , 0 , 0 }, { 1 , 1 , 0 , 0 , 0 , 0 , 0 , 0 , 0 }, { 1 , 0 , -2 , 2 , -1 , 0 , 0 , 0 , 0 }, { 1 , 0 , 2 , 0 , 0 , 0 , 0 , 0 , 0 }, { -1 , 1 , 0 , 1 , 0 , 0 , 0 , 0 , 0 }, { 1 , 0 , 0 , 0 , 2 , 0 , 0 , 0 , 0 }, { -1 , 0 , 1 , 0 , 1 , 0 , 0 , 0 , 0 }, { 0 , 0 , 2 , 1 , 2 , 0 , 0 , 0 , 0 }, { -1 , 1 , 0 , 1 , 1 , 0 , 0 , 0 , 0 }, { -1 , 0 , 2 , 4 , 2 , 0 , 0 , 0 , 0 }, { 0 , -2 , 2 , -2 , 1 , 0 , 0 , 0 , 0 }, { 1 , 0 , 2 , 2 , 1 , 0 , 0 , 0 , 0 }, { 1 , 0 , 0 , 0 , -2 , 0 , 0 , 0 , 0 }, { -2 , 0 , 2 , 2 , 2 , 0 , 0 , 0 , 0 }, { 1 , 1 , 2 , -2 , 2 , 0 , 0 , 0 , 0 }, { -2 , 0 , 2 , 4 , 2 , 0 , 0 , 0 , 0 }, { -1 , 0 , 4 , 0 , 2 , 0 , 0 , 0 , 0 }, { 2 , 0 , 2 , -2 , 1 , 0 , 0 , 0 , 0 }, { 1 , 0 , 0 , -1 , -1 , 0 , 0 , 0 , 0 }, { 2 , 0 , 2 , 2 , 2 , 0 , 0 , 0 , 0 }, { 1 , 0 , 0 , 2 , 1 , 0 , 0 , 0 , 0 }, { 3 , 0 , 0 , 0 , 0 , 0 , 0 , 0 , 0 }, { 0 , 0 , 2 , -2 , -1 , 0 , 0 , 0 , 0 }, { 3 , 0 , 2 , -2 , 2 , 0 , 0 , 0 , 0 }, { 0 , 0 , 4 , -2 , 2 , 0 , 0 , 0 , 0 }, { -1 , 0 , 0 , 4 , 0 , 0 , 0 , 0 , 0 }, { 0 , 1 , 2 , 0 , 1 , 0 , 0 , 0 , 0 }, { 0 , 0 , 2 , -2 , 3 , 0 , 0 , 0 , 0 }, { -2 , 0 , 0 , 4 , 0 , 0 , 0 , 0 , 0 }, { -1 , -1 , 0 , 2 , 1 , 0 , 0 , 0 , 0 }, { -2 , 0 , 2 , 0 , -1 , 0 , 0 , 0 , 0 }, { 0 , 0 , 2 , 0 , -1 , 0 , 0 , 0 , 0 }, { 0 , -1 , 2 , 0 , 1 , 0 , 0 , 0 , 0 }, { 0 , 1 , 0 , 0 , 2 , 0 , 0 , 0 , 0 }, { 0 , 0 , 2 , -1 , 2 , 0 , 0 , 0 , 0 }, { 2 , 1 , 0 , -2 , 0 , 0 , 0 , 0 , 0 }, { 0 , 0 , 2 , 4 , 2 , 0 , 0 , 0 , 0 }, { -1 , -1 , 0 , 2 , -1 , 0 , 0 , 0 , 0 }, { -1 , 1 , 0 , 2 , 0 , 0 , 0 , 0 , 0 }, { 1 , -1 , 0 , 0 , 1 , 0 , 0 , 0 , 0 }, { 0 , -1 , 2 , -2 , 0 , 0 , 0 , 0 , 0 }, { 0 , 1 , 0 , 0 , -2 , 0 , 0 , 0 , 0 }, { 1 , -1 , 2 , 2 , 2 , 0 , 0 , 0 , 0 }, { 1 , 0 , 0 , 2 , -1 , 0 , 0 , 0 , 0 }, { -1 , 1 , 2 , 2 , 2 , 0 , 0 , 0 , 0 }, { 3 , 0 , 2 , 0 , 1 , 0 , 0 , 0 , 0 }, { 0 , 1 , 2 , 2 , 2 , 0 , 0 , 0 , 0 }, { 1 , 0 , 2 , -2 , 0 , 0 , 0 , 0 , 0 }, { -1 , 0 , -2 , 4 , -1 , 0 , 0 , 0 , 0 }, { -1 , -1 , 2 , 2 , 1 , 0 , 0 , 0 , 0 }, { 0 , -1 , 2 , 2 , 1 , 0 , 0 , 0 , 0 }, { 2 , -1 , 2 , 0 , 2 , 0 , 0 , 0 , 0 }, { 0 , 0 , 0 , 2 , 2 , 0 , 0 , 0 , 0 }, { 1 , -1 , 2 , 0 , 1 , 0 , 0 , 0 , 0 }, { -1 , 1 , 2 , 0 , 2 , 0 , 0 , 0 , 0 }, { 0 , 1 , 0 , 2 , 0 , 0 , 0 , 0 , 0 }, { 0 , 1 , 2 , -2 , 0 , 0 , 0 , 0 , 0 }, { 0 , 3 , 2 , -2 , 2 , 0 , 0 , 0 , 0 }, { 0 , 0 , 0 , 1 , 1 , 0 , 0 , 0 , 0 }, { -1 , 0 , 2 , 2 , 0 , 0 , 0 , 0 , 0 }, { 2 , 1 , 2 , 0 , 2 , 0 , 0 , 0 , 0 }, { 1 , 1 , 0 , 0 , 1 , 0 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0.90000000000000002 , 1.2000000000000000 , 0.0000000000000000 , 0.0000000000000000 }, { -11.900000000000000 , -0.50000000000000000 , 0.0000000000000000 , 0.29999999999999999 }, { 0.40000000000000002 , 12.000000000000000 , 0.29999999999999999 , -0.20000000000000001 }, { 8.3000000000000007 , 6.0999999999999996 , -0.10000000000000001 , 0.10000000000000001 }, { 0.0000000000000000 , 0.0000000000000000 , 0.0000000000000000 , 0.0000000000000000 }, { 0.40000000000000002 , -10.800000000000001 , 0.29999999999999999 , 0.0000000000000000 }, { 9.5999999999999996 , 2.2000000000000002 , 0.29999999999999999 , -1.2000000000000000 } }; /* interval between fundamental epoch j2000.0 and given epoch (jc). */ t = (date-DJM0)/DJC; /* mean anomaly of the moon. */ el = 134.96340251*PAL__DD2R+ fmod(t*(1717915923.2178+ t*( 31.8792+ t*( 0.051635+ t*( - 0.00024470)))),TURNAS)*PAL__DAS2R; /* mean anomaly of the sun. */ elp = 357.52910918*PAL__DD2R+ fmod(t*( 129596581.0481+ t*( - 0.5532+ t*( 0.000136+ t*( - 0.00001149)))),TURNAS)*PAL__DAS2R; /* mean argument of the latitude of the moon. */ f = 93.27209062*PAL__DD2R+ fmod(t*(1739527262.8478+ t*( - 12.7512+ t*( - 0.001037+ t*( 0.00000417)))),TURNAS)*PAL__DAS2R; /* mean elongation of the moon from the sun. */ d = 297.85019547*PAL__DD2R+ fmod(t*(1602961601.2090+ t*( - 6.3706+ t*( 0.006539+ t*( - 0.00003169)))),TURNAS)*PAL__DAS2R; /* mean longitude of the ascending node of the moon. */ om = 125.04455501*PAL__DD2R+ fmod(t*( - 6962890.5431+ t*( 7.4722+ t*( 0.007702+ t*( - 0.00005939)))),TURNAS)*PAL__DAS2R; /* mean longitude of venus. */ ve = 181.97980085*PAL__DD2R+fmod(210664136.433548*t,TURNAS)*PAL__DAS2R; /* mean longitude of mars.*/ ma = 355.43299958*PAL__DD2R+fmod( 68905077.493988*t,TURNAS)*PAL__DAS2R; /* mean longitude of jupiter. */ ju = 34.35151874*PAL__DD2R+fmod( 10925660.377991*t,TURNAS)*PAL__DAS2R; /* mean longitude of saturn. */ sa = 50.07744430*PAL__DD2R+fmod( 4399609.855732*t,TURNAS)*PAL__DAS2R; /* geodesic nutation (fukushima 1991) in microarcsec. */ dp = -153.1*sin(elp)-1.9*sin(2*elp); de = 0.0; /* shirai & fukushima (2001) nutation series. */ for (j=NTERMS-1; j >= 0; j--) { theta = ((double)na[j][0])*el+ ((double)na[j][1])*elp+ ((double)na[j][2])*f+ ((double)na[j][3])*d+ ((double)na[j][4])*om+ ((double)na[j][5])*ve+ ((double)na[j][6])*ma+ ((double)na[j][7])*ju+ ((double)na[j][8])*sa; c = cos(theta); s = sin(theta); dp += (psi[j][0] + psi[j][2]*t)*c + (psi[j][1] + psi[j][3]*t)*s; de += (eps[j][0] + eps[j][2]*t)*c + (eps[j][1] + eps[j][3]*t)*s; } /* change of units, and addition of the precession correction.*/ *dpsi = (dp*1e-6-0.042888-0.29856*t)*PAL__DAS2R; *deps = (de*1e-6-0.005171-0.02408*t)*PAL__DAS2R; /* mean obliquity of date (simon et al. 1994). */ *eps0 = (84381.412+ (-46.80927+ (-0.000152+ (0.0019989+ (-0.00000051+ (-0.000000025)*t)*t)*t)*t)*t)*PAL__DAS2R; } pal-0.5.0/palAoppat.c000644 000765 000024 00000006032 12366000607 014464 0ustar00timjstaff000000 000000 /* *+ * Name: * palAoppat * Purpose: * Recompute sidereal time to support apparent to observed place * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palAoppat( double date, double aoprms[14] ); * Arguments: * date = double (Given) * UTC date/time (modified Julian Date, JD-2400000.5) * (see palAoppa description for comments on leap seconds) * aoprms = double[14] (Given & Returned) * Star-independent apparent-to-observed parameters. Updated * by this routine. Requires element 12 to be the longitude + * eqn of equinoxes + sidereal DUT and fills in element 13 * with the local apparent sidereal time (in radians). * Description: * This routine recomputes the sidereal time in the apparent to * observed place star-independent parameter block. * Authors: * TIMJ: Tim Jenness (JAC, Hawaii) * PTW: Patrick T. Wallace * {enter_new_authors_here} * Notes: * - See palAoppa for more information. * - The star-independent parameters are not treated as an opaque * struct in order to retain compatibility with SLA. * History: * 2012-08-24 (TIMJ): * Initial version, ported from Fortran SLA source. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1995 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" static double pal__Gmst( double ut1 ); void palAoppat( double date, double aoprms[14] ) { aoprms[13] = pal__Gmst(date) + aoprms[12]; } /* Use a private implementation of palGmst for testing that matches the SLA rather than SOFA implementation. This is used for comparing SLA with PAL refraction code. */ #include "math.h" #include "palmac.h" static double pal__Gmst( double ut1 ) { double tu; double gmst; /* Julian centuries from fundamental epoch J2000 to this UT */ tu=(ut1-51544.5)/36525; /* GMST at this UT */ gmst=palDranrm(fmod(ut1,1.0)*PAL__D2PI+ (24110.54841+ (8640184.812866+ (0.093104-6.2e-6*tu)*tu)*tu)*PAL__DS2R); return gmst; } pal-0.5.0/palAopqk.c000644 000765 000024 00000024035 12366000607 014316 0ustar00timjstaff000000 000000 /* *+ * Name: * palAopqk * Purpose: * Quick apparent to observed place * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palAopqk ( double rap, double dap, const double aoprms[14], * double *aob, double *zob, double *hob, * double *dob, double *rob ); * Arguments: * rap = double (Given) * Geocentric apparent right ascension * dap = double (Given) * Geocentric apparent declination * aoprms = const double [14] (Given) * Star-independent apparent-to-observed parameters. * * [0] geodetic latitude (radians) * [1,2] sine and cosine of geodetic latitude * [3] magnitude of diurnal aberration vector * [4] height (HM) * [5] ambient temperature (T) * [6] pressure (P) * [7] relative humidity (RH) * [8] wavelength (WL) * [9] lapse rate (TLR) * [10,11] refraction constants A and B (radians) * [12] longitude + eqn of equinoxes + sidereal DUT (radians) * [13] local apparent sidereal time (radians) * aob = double * (Returned) * Observed azimuth (radians: N=0,E=90) * zob = double * (Returned) * Observed zenith distance (radians) * hob = double * (Returned) * Observed Hour Angle (radians) * dob = double * (Returned) * Observed Declination (radians) * rob = double * (Returned) * Observed Right Ascension (radians) * Description: * Quick apparent to observed place. * Authors: * TIMJ: Tim Jenness (JAC, Hawaii) * PTW: Patrick T. Wallace * {enter_new_authors_here} * Notes: * - This routine returns zenith distance rather than elevation * in order to reflect the fact that no allowance is made for * depression of the horizon. * * - The accuracy of the result is limited by the corrections for * refraction. Providing the meteorological parameters are * known accurately and there are no gross local effects, the * observed RA,Dec predicted by this routine should be within * about 0.1 arcsec for a zenith distance of less than 70 degrees. * Even at a topocentric zenith distance of 90 degrees, the * accuracy in elevation should be better than 1 arcmin; useful * results are available for a further 3 degrees, beyond which * the palRefro routine returns a fixed value of the refraction. * The complementary routines palAop (or palAopqk) and palOap * (or palOapqk) are self-consistent to better than 1 micro- * arcsecond all over the celestial sphere. * * - It is advisable to take great care with units, as even * unlikely values of the input parameters are accepted and * processed in accordance with the models used. * * - "Apparent" place means the geocentric apparent right ascension * and declination, which is obtained from a catalogue mean place * by allowing for space motion, parallax, precession, nutation, * annual aberration, and the Sun's gravitational lens effect. For * star positions in the FK5 system (i.e. J2000), these effects can * be applied by means of the palMap etc routines. Starting from * other mean place systems, additional transformations will be * needed; for example, FK4 (i.e. B1950) mean places would first * have to be converted to FK5, which can be done with the * palFk425 etc routines. * * - "Observed" Az,El means the position that would be seen by a * perfect theodolite located at the observer. This is obtained * from the geocentric apparent RA,Dec by allowing for Earth * orientation and diurnal aberration, rotating from equator * to horizon coordinates, and then adjusting for refraction. * The HA,Dec is obtained by rotating back into equatorial * coordinates, using the geodetic latitude corrected for polar * motion, and is the position that would be seen by a perfect * equatorial located at the observer and with its polar axis * aligned to the Earth's axis of rotation (n.b. not to the * refracted pole). Finally, the RA is obtained by subtracting * the HA from the local apparent ST. * * - To predict the required setting of a real telescope, the * observed place produced by this routine would have to be * adjusted for the tilt of the azimuth or polar axis of the * mounting (with appropriate corrections for mount flexures), * for non-perpendicularity between the mounting axes, for the * position of the rotator axis and the pointing axis relative * to it, for tube flexure, for gear and encoder errors, and * finally for encoder zero points. Some telescopes would, of * course, exhibit other properties which would need to be * accounted for at the appropriate point in the sequence. * * - The star-independent apparent-to-observed-place parameters * in AOPRMS may be computed by means of the palAoppa routine. * If nothing has changed significantly except the time, the * palAoppat routine may be used to perform the requisite * partial recomputation of AOPRMS. * * - At zenith distances beyond about 76 degrees, the need for * special care with the corrections for refraction causes a * marked increase in execution time. Moreover, the effect * gets worse with increasing zenith distance. Adroit * programming in the calling application may allow the * problem to be reduced. Prepare an alternative AOPRMS array, * computed for zero air-pressure; this will disable the * refraction corrections and cause rapid execution. Using * this AOPRMS array, a preliminary call to the present routine * will, depending on the application, produce a rough position * which may be enough to establish whether the full, slow * calculation (using the real AOPRMS array) is worthwhile. * For example, there would be no need for the full calculation * if the preliminary call had already established that the * source was well below the elevation limits for a particular * telescope. * * - The azimuths etc produced by the present routine are with * respect to the celestial pole. Corrections to the terrestrial * pole can be computed using palPolmo. * History: * 2012-08-25 (TIMJ): * Initial version, copied from Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2003 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include #include "pal.h" void palAopqk ( double rap, double dap, const double aoprms[14], double *aob, double *zob, double *hob, double *dob, double *rob ) { /* Breakpoint for fast/slow refraction algorithm: * ZD greater than arctan(4), (see palRefco routine) * or vector Z less than cosine(arctan(Z)) = 1/sqrt(17) */ const double zbreak = 0.242535625; int i; double sphi,cphi,st,v[3],xhd,yhd,zhd,diurab,f, xhdt,yhdt,zhdt,xaet,yaet,zaet,azobs, zdt,refa,refb,zdobs,dzd,dref,ce, xaeo,yaeo,zaeo,hmobs,dcobs,raobs; /* sin, cos of latitude */ sphi = aoprms[1]; cphi = aoprms[2]; /* local apparent sidereal time */ st = aoprms[13]; /* apparent ra,dec to cartesian -ha,dec */ palDcs2c( rap-st, dap, v ); xhd = v[0]; yhd = v[1]; zhd = v[2]; /* diurnal aberration */ diurab = aoprms[3]; f = (1.0-diurab*yhd); xhdt = f*xhd; yhdt = f*(yhd+diurab); zhdt = f*zhd; /* cartesian -ha,dec to cartesian az,el (s=0,e=90) */ xaet = sphi*xhdt-cphi*zhdt; yaet = yhdt; zaet = cphi*xhdt+sphi*zhdt; /* azimuth (n=0,e=90) */ if (xaet == 0.0 && yaet == 0.0) { azobs = 0.0; } else { azobs = atan2(yaet,-xaet); } /* topocentric zenith distance */ zdt = atan2(sqrt(xaet*xaet+yaet*yaet),zaet); /* * refraction * ---------- */ /* fast algorithm using two constant model */ refa = aoprms[10]; refb = aoprms[11]; palRefz(zdt,refa,refb,&zdobs); /* large zenith distance? */ if (cos(zdobs) < zbreak) { /* yes: use rigorous algorithm */ /* initialize loop (maximum of 10 iterations) */ i = 1; dzd = 1.0e1; while (abs(dzd) > 1e-10 && i <= 10) { /* compute refraction using current estimate of observed zd */ palRefro(zdobs,aoprms[4],aoprms[5],aoprms[6], aoprms[7],aoprms[8],aoprms[0], aoprms[9],1e-8,&dref); /* remaining discrepancy */ dzd = zdobs+dref-zdt; /* update the estimate */ zdobs = zdobs-dzd; /* increment the iteration counter */ i++; } } /* to cartesian az/zd */ ce = sin(zdobs); xaeo = -cos(azobs)*ce; yaeo = sin(azobs)*ce; zaeo = cos(zdobs); /* cartesian az/zd to cartesian -ha,dec */ v[0] = sphi*xaeo+cphi*zaeo; v[1] = yaeo; v[2] = -cphi*xaeo+sphi*zaeo; /* to spherical -ha,dec */ palDcc2s(v,&hmobs,&dcobs); /* right ascension */ raobs = palDranrm(st+hmobs); /* return the results */ *aob = azobs; *zob = zdobs; *hob = -hmobs; *dob = dcobs; *rob = raobs; } pal-0.5.0/palAtmdsp.c000644 000765 000024 00000013742 12366000607 014476 0ustar00timjstaff000000 000000 /* *+ * Name: * palAtmdsp * Purpose: * Apply atmospheric-dispersion adjustments to refraction coefficients * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palAtmdsp( double tdk, double pmb, double rh, double wl1, * double a1, double b1, double wl2, double *a2, double *b2 ); * Arguments: * tdk = double (Given) * Ambient temperature, K * pmb = double (Given) * Ambient pressure, millibars * rh = double (Given) * Ambient relative humidity, 0-1 * wl1 = double (Given) * Reference wavelength, micrometre (0.4 recommended) * a1 = double (Given) * Refraction coefficient A for wavelength wl1 (radians) * b1 = double (Given) * Refraction coefficient B for wavelength wl1 (radians) * wl2 = double (Given) * Wavelength for which adjusted A,B required * a2 = double * (Returned) * Refraction coefficient A for wavelength WL2 (radians) * b2 = double * (Returned) * Refraction coefficient B for wavelength WL2 (radians) * Description: * Apply atmospheric-dispersion adjustments to refraction coefficients. * Authors: * TIMJ: Tim Jenness * PTW: Patrick Wallace * {enter_new_authors_here} * Notes: * - To use this routine, first call palRefco specifying WL1 as the * wavelength. This yields refraction coefficients A1,B1, correct * for that wavelength. Subsequently, calls to palAtmdsp specifying * different wavelengths will produce new, slightly adjusted * refraction coefficients which apply to the specified wavelength. * * - Most of the atmospheric dispersion happens between 0.7 micrometre * and the UV atmospheric cutoff, and the effect increases strongly * towards the UV end. For this reason a blue reference wavelength * is recommended, for example 0.4 micrometres. * * - The accuracy, for this set of conditions: * * height above sea level 2000 m * latitude 29 deg * pressure 793 mb * temperature 17 degC * humidity 50% * lapse rate 0.0065 degC/m * reference wavelength 0.4 micrometre * star elevation 15 deg * * is about 2.5 mas RMS between 0.3 and 1.0 micrometres, and stays * within 4 mas for the whole range longward of 0.3 micrometres * (compared with a total dispersion from 0.3 to 20.0 micrometres * of about 11 arcsec). These errors are typical for ordinary * conditions and the given elevation; in extreme conditions values * a few times this size may occur, while at higher elevations the * errors become much smaller. * * - If either wavelength exceeds 100 micrometres, the radio case * is assumed and the returned refraction coefficients are the * same as the given ones. Note that radio refraction coefficients * cannot be turned into optical values using this routine, nor * vice versa. * * - The algorithm consists of calculation of the refractivity of the * air at the observer for the two wavelengths, using the methods * of the palRefro routine, and then scaling of the two refraction * coefficients according to classical refraction theory. This * amounts to scaling the A coefficient in proportion to (n-1) and * the B coefficient almost in the same ratio (see R.M.Green, * "Spherical Astronomy", Cambridge University Press, 1985). * History: * 2014-07-15 (TIMJ): * Initial version. A direct copy of the Fortran SLA implementation. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2014 Tim Jenness * Copyright (C) 2005 Patrick Wallace * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "palmac.h" #include void palAtmdsp ( double tdk, double pmb, double rh, double wl1, double a1, double b1, double wl2, double *a2, double *b2 ) { double f,tdkok,pmbok,rhok; double psat,pwo,w1,wlok,wlsq,w2,dn1,dn2; /* Check for radio wavelengths */ if (wl1 > 100.0 || wl2 > 100.0) { /* Radio: no dispersion */ *a2 = a1; *b2 = b1; } else { /* Optical: keep arguments within safe bounds */ tdkok = DMIN(DMAX(tdk,100.0),500.0); pmbok = DMIN(DMAX(pmb,0.0),10000.0); rhok = DMIN(DMAX(rh,0.0),1.0); /* Atmosphere parameters at the observer */ psat = pow(10.0, -8.7115+0.03477*tdkok); pwo = rhok*psat; w1 = 11.2684e-6*pwo; /* Refractivity at the observer for first wavelength */ wlok = DMAX(wl1,0.1); wlsq = wlok*wlok; w2 = 77.5317e-6+(0.43909e-6+0.00367e-6/wlsq)/wlsq; dn1 = (w2*pmbok-w1)/tdkok; /* Refractivity at the observer for second wavelength */ wlok = DMAX(wl2,0.1); wlsq = wlok*wlok; w2 = 77.5317e-6+(0.43909e-6+0.00367e-6/wlsq)/wlsq; dn2 = (w2*pmbok-w1)/tdkok; /* Scale the refraction coefficients (see Green 4.31, p93) */ if (dn1 != 0.0) { f = dn2/dn1; *a2 = a1*f; *b2 = b1*f; if (dn1 != a1) { *b2 *= (1.0+dn1*(dn1-dn2)/(2.0*(dn1-a1))); } } else { *a2 = a1; *b2 = b1; } } } pal-0.5.0/palCaldj.c000644 000765 000024 00000005467 12366000612 014264 0ustar00timjstaff000000 000000 /* *+ * Name: * palCaldj * Purpose: * Gregorian Calendar to Modified Julian Date * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palCaldj ( int iy, int im, int id, double *djm, int *j ); * Arguments: * iy = int (Given) * Year in the Gregorian calendar * im = int (Given) * Month in the Gergorian calendar * id = int (Given) * Day in the Gregorian calendar * djm = double * (Returned) * Modified Julian Date (JD-2400000.5) for 0 hrs * j = status (Returned) * 0 = OK. See eraCal2jd for other values. * Description: * Modified Julian Date to Gregorian Calendar with special * behaviour for 2-digit years relating to 1950 to 2049. * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * History: * 2012-02-11 (TIMJ): * Initial version with documentation taken from Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Notes: * - Uses eraCal2jd * - Unlike eraCal2jd this routine treats the years 0-100 as * referring to the end of the 20th Century and beginning of * the 21st Century. If this behaviour is not acceptable * use the SOFA routine directly or palCldj. * Acceptable years are 00-49, interpreted as 2000-2049, * 50-99, " " 1950-1999, * all others, interpreted literally. * - Unlike SLA this routine will work with negative years. * Copyright: * Copyright (C) 1995 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "palmac.h" #include "pal1sofa.h" void palCaldj ( int iy, int im, int id, double *djm, int *j ) { int adj = 0; /* Year adjustment */ double djm0; if (iy >= 0 && iy <= 49) { adj = 2000; } else if (iy >= 50 && iy <= 99) { adj = 1900; } iy += adj; *j = eraCal2jd( iy, im, id, &djm0, djm ); } pal-0.5.0/palDafin.c000644 000765 000024 00000014536 12366000612 014265 0ustar00timjstaff000000 000000 /* *+ * Name: * palDafin * Purpose: * Sexagesimal character string to angle * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palDafin ( const char *string, int *ipos, double *a, int *j ); * Arguments: * string = const char * (Given) * String containing deg, arcmin, arcsec fields * ipos = int * (Given & Returned) * Position to start decoding "string". First character * is position 1 for compatibility with SLA. After * calling this routine "iptr" will be positioned after * the sexagesimal string. * a = double * (Returned) * Angle in radians. * j = int * (Returned) * status: 0 = OK * +1 = default, A unchanged * -1 = bad degrees ) * -2 = bad arcminutes ) (note 3) * -3 = bad arcseconds ) * Description: * Extracts an angle from a sexagesimal string with degrees, arcmin, * arcsec fields using space or comma delimiters. * Authors: * TIMJ: Tim Jenness (JAC, Hawaii) * PTW: Patrick T. Wallace * {enter_new_authors_here} * Example: * argument before after * * STRING '-57 17 44.806 12 34 56.7' unchanged * IPTR 1 16 (points to 12...) * A ? -1.00000D0 * J ? 0 * Notes: * - The first three "fields" in STRING are degrees, arcminutes, * arcseconds, separated by spaces or commas. The degrees field * may be signed, but not the others. The decoding is carried * out by the palDfltin routine and is free-format. * - Successive fields may be absent, defaulting to zero. For * zero status, the only combinations allowed are degrees alone, * degrees and arcminutes, and all three fields present. If all * three fields are omitted, a status of +1 is returned and A is * unchanged. In all other cases A is changed. * - Range checking: * * The degrees field is not range checked. However, it is * expected to be integral unless the other two fields are absent. * * The arcminutes field is expected to be 0-59, and integral if * the arcseconds field is present. If the arcseconds field * is absent, the arcminutes is expected to be 0-59.9999... * * The arcseconds field is expected to be 0-59.9999... * * - Decoding continues even when a check has failed. Under these * circumstances the field takes the supplied value, defaulting * to zero, and the result A is computed and returned. * - Further fields after the three expected ones are not treated * as an error. The pointer IPOS is left in the correct state * for further decoding with the present routine or with palDfltin * etc. See the example, above. * - If STRING contains hours, minutes, seconds instead of degrees * etc, or if the required units are turns (or days) instead of * radians, the result A should be multiplied as follows: * * for to obtain multiply * STRING A in A by * * d ' " radians 1 = 1.0 * d ' " turns 1/2pi = 0.1591549430918953358 * h m s radians 15 = 15.0 * h m s days 15/2pi = 2.3873241463784300365 * History: * 2012-03-08 (TIMJ): * Initial version from SLA/F using Fortran documentation * Adapted with permission from the Fortran SLALIB library. * 2012-10-17 (TIMJ): * Fix range check on arcminute value. * {enter_further_changes_here} * Copyright: * Copyright (C) 1996 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "palmac.h" #include "pal1sofa.h" #include void palDafin ( const char *string, int *ipos, double *a, int *j ) { int jd = 0; /* Status for degree parsing */ int jm = 0; /* Status for arcmin parsing */ int js = 0; /* Status for arcsec parsing */ int jf = 0; /* Internal copy of status */ double deg = 0.0; double arcmin = 0.0; double arcsec = 0.0; /* Decode degrees, arcminutes, arcseconds */ palDfltin( string, ipos, °, &jd ); if (jd > 1) { jf = -1; } else { palDfltin( string, ipos, &arcmin, &jm ); if ( jm < 0 || jm > 1 ) { jf = -2; } else { palDfltin( string, ipos, &arcsec, &js ); if (js < 0 || js > 1) { jf = -3; } else if (jd > 0) { /* See if combination of fields is credible */ /* No degrees: arcmin, arcsec ought also to be absent */ if (jm == 0) { /* Suspect arcmin */ jf = -2; } else if (js == 0) { /* Suspect arcsec */ jf = -3; } else { /* All three fields absent */ jf = 1; } } else if (jm != 0 && js == 0) { /* Deg present: if arcsec present should have arcmin */ jf = -3; /* Tests for range and integrality */ } else if (jm == 0 && DINT(deg) != deg) { /* Degrees */ jf = -1; } else if ( (js == 0 && DINT(arcmin) != arcmin) || arcmin >= 60.0 ) { /* Arcmin */ jf = -2; } else if (arcsec >= 60.0) { /* Arcsec */ jf = -3; } } } /* Unless all three fields absent, compute angle value */ if (jf <= 0) { *a = PAL__DAS2R * ( 60.0 * ( 60.0 * fabs(deg) + arcmin) + arcsec ); if ( jd < 0 ) *a *= -1.; } *j = jf; } pal-0.5.0/palDat.c000644 000765 000024 00000004770 12366000612 013753 0ustar00timjstaff000000 000000 /* *+ * Name: * palDtt * Purpose: * Return offset between UTC and TT * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * dat = palDat( double utc ); * Arguments: * utc = double (Given) * UTC date as a modified JD (JD-2400000.5) * Returned Value: * dat = double * TAI-UTC in seconds * Description: * Increment to be applied to Coordinated Universal Time UTC to give * International Atomic Time (TAI). * Authors: * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - This routine converts the MJD argument to calendar date before calling * the SOFA eraDat function. * - This routine matches the slaDat interface which differs from the eraDat * interface. Consider coding directly to the SOFA interface. * - See eraDat for a description of error conditions when calling this function * with a time outside of the UTC range. * - The status argument from eraDat is ignored. This is reasonable since the * error codes are mainly related to incorrect calendar dates when calculating * the JD internally. * History: * 2012-02-08 (TIMJ): * Initial version * Adapted with permission from the Fortran SLALIB library * although the core algorithm is now from SOFA. * {enter_further_changes_here} * Copyright: * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "palmac.h" #include "pal1sofa.h" double palDat ( double dju ) { int iy; int im; int id; int status; double fd; double deltat; eraJd2cal( PAL__MJD0, dju, &iy, &im, &id, &fd ); status = eraDat( iy, im, id, fd, &deltat ); return deltat; } pal-0.5.0/palDe2h.c000644 000765 000024 00000007446 12366000607 014034 0ustar00timjstaff000000 000000 /* *+ * Name: * palDe2h * Purpose: * Equatorial to horizon coordinates: HA,Dec to Az,E * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * palDe2h( double ha, double dec, double phi, double * az, double * el ); * Arguments: * ha = double * (Given) * Hour angle (radians) * dec = double * (Given) * Declination (radians) * phi = double (Given) * Observatory latitude (radians) * az = double * (Returned) * Azimuth (radians) * el = double * (Returned) * Elevation (radians) * Description: * Convert equatorial to horizon coordinates. * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - All the arguments are angles in radians. * - Azimuth is returned in the range 0-2pi; north is zero, * and east is +pi/2. Elevation is returned in the range * +/-pi/2. * - The latitude must be geodetic. In critical applications, * corrections for polar motion should be applied. * - In some applications it will be important to specify the * correct type of hour angle and declination in order to * produce the required type of azimuth and elevation. In * particular, it may be important to distinguish between * elevation as affected by refraction, which would * require the "observed" HA,Dec, and the elevation * in vacuo, which would require the "topocentric" HA,Dec. * If the effects of diurnal aberration can be neglected, the * "apparent" HA,Dec may be used instead of the topocentric * HA,Dec. * - No range checking of arguments is carried out. * - In applications which involve many such calculations, rather * than calling the present routine it will be more efficient to * use inline code, having previously computed fixed terms such * as sine and cosine of latitude, and (for tracking a star) * sine and cosine of declination. * History: * 2012-02-08 (TIMJ): * Initial version with documentation taken from Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1995 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "palmac.h" #include void palDe2h ( double ha, double dec, double phi, double *az, double *el) { double sh; double ch; double sd; double cd; double sp; double cp; double a; double x; double y; double z; double r; /* Useful trig functions */ sh = sin(ha); ch = cos(ha); sd = sin(dec); cd = cos(dec); sp = sin(phi); cp = cos(phi); /* Az,El as x,y,z */ x = -ch * cd * sp + sd * cp; y = -sh * cd; z = ch * cd * cp + sd * sp; /* To spherical */ r = sqrt(x * x + y * y); if (r == 0.) { a = 0.; } else { a = atan2(y, x); } if (a < 0.) { a += PAL__D2PI; } *az = a; *el = atan2(z, r); return; } pal-0.5.0/palDeuler.c000644 000765 000024 00000007562 12366000612 014465 0ustar00timjstaff000000 000000 /* *+ * Name: * palDeuler * Purpose: * Form a rotation matrix from the Euler angles * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palDeuler ( const char *order, double phi, double theta, double psi, * double rmat[3][3] ); * Arguments: * order = const char[] (Given) * Specifies about which axes the rotation occurs * phi = double (Given) * 1st rotation (radians) * theta = double (Given) * 2nd rotation (radians) * psi = double (Given) * 3rd rotation (radians) * rmat = double[3][3] (Given & Returned) * Rotation matrix * Description: * A rotation is positive when the reference frame rotates * anticlockwise as seen looking towards the origin from the * positive region of the specified axis. * * The characters of ORDER define which axes the three successive * rotations are about. A typical value is 'ZXZ', indicating that * RMAT is to become the direction cosine matrix corresponding to * rotations of the reference frame through PHI radians about the * old Z-axis, followed by THETA radians about the resulting X-axis, * then PSI radians about the resulting Z-axis. * * The axis names can be any of the following, in any order or * combination: X, Y, Z, uppercase or lowercase, 1, 2, 3. Normal * axis labelling/numbering conventions apply; the xyz (=123) * triad is right-handed. Thus, the 'ZXZ' example given above * could be written 'zxz' or '313' (or even 'ZxZ' or '3xZ'). ORDER * is terminated by length or by the first unrecognized character. * * Fewer than three rotations are acceptable, in which case the later * angle arguments are ignored. If all rotations are zero, the * identity matrix is produced. * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * History: * 2012-02-08 (TIMJ): * Initial version with documentation taken from Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1997 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "pal1sofa.h" void palDeuler( const char *order, double phi, double theta, double psi, double rmat[3][3] ) { int i = 0; double rotations[3]; /* Initialise rmat */ eraIr( rmat ); /* copy the rotations into an array */ rotations[0] = phi; rotations[1] = theta; rotations[2] = psi; /* maximum three rotations */ while (i < 3 && order[i] != '\0') { switch (order[i]) { case 'X': case 'x': case '1': eraRx( rotations[i], rmat ); break; case 'Y': case 'y': case '2': eraRy( rotations[i], rmat ); break; case 'Z': case 'z': case '3': eraRz( rotations[i], rmat ); break; default: /* break out the loop if we do not recognize something */ i = 3; } /* Go to the next position */ i++; } return; } pal-0.5.0/palDfltin.c000644 000765 000024 00000016321 12366007151 014463 0ustar00timjstaff000000 000000 /* *+ * Name: * palDfltin * Purpose: * Convert free-format input into double precision floating point * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palDfltin( const char * string, int *nstrt, * double *dreslt, int *jflag ); * Arguments: * string = const char * (Given) * String containing number to be decoded. * nstrt = int * (Given and Returned) * Character number indicating where decoding should start. * On output its value is updated to be the location of the * possible next value. For compatibility with SLA the first * character is index 1. * dreslt = double * (Returned) * Result. Not updated when jflag=1. * jflag = int * (Returned) * status: -1 = -OK, 0 = +OK, 1 = null, 2 = error * Description: * Extracts a number from an input string starting at the specified * index. * Authors: * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - Uses the strtod() system call to do the parsing. This may lead to * subtle differences when compared to the SLA/F parsing. * - All "D" characters are converted to "E" to handle fortran exponents. * - Commas are recognized as a special case and are skipped if one happens * to be the next character when updating nstrt. Additionally the output * nstrt position will skip past any trailing space. * - If no number can be found flag will be set to 1. * - If the number overflows or underflows jflag will be set to 2. For overflow * the returned result will have the value HUGE_VAL, for underflow it * will have the value 0.0. * - For compatiblity with SLA/F -0 will be returned as "0" with jflag == -1. * - Unlike slaDfltin a standalone "E" will return status 1 (could not find * a number) rather than 2 (bad number). * Implementation Status: * - The code is more robust if the C99 copysign() function is available. * This can recognize the -0.0 values returned by strtod. If copysign() is * missing we try to scan the string looking for minus signs. * History: * 2012-03-08 (TIMJ): * Initial version based on strtod * Adapted with permission from the Fortran SLALIB library * although this is a completely distinct implementation of the SLA API. * 2012-06-21 (TIMJ): * Provide a backup for missing copysign. * 2012-06-22 (TIMJ): * Check __STDC_VERSION__ * {enter_further_changes_here} * Copyright: * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ /* Use the config file if we have one, else look at compiler defines to see if we have C99 */ #if HAVE_CONFIG_H #include #else #ifdef __STDC_VERSION__ # if (__STDC_VERSION__ >= 199901L) # define HAVE_COPYSIGN 1 # endif #endif #endif /* isblank() is a C99 feature so we just reimplement it if it is missing */ #if HAVE_ISBLANK #define _POSIX_C_SOURCE 200112L #define _ISOC99_SOURCE #include # define ISBLANK isblank #else static int ISBLANK( int c ) { return ( c == ' ' || c == '\t' ); } #endif /* System include files */ #include #include #include #include #include "pal.h" #if HAVE_COPYSIGN # define SCAN_FOR_MINUS 0 #else # define SCAN_FOR_MINUS 1 #endif /* We prefer to use the starutil package */ #if HAVE_STAR_UTIL_H # include "star/util.h" #else #endif void palDfltin( const char * string, int *nstrt, double *dreslt, int *jflag ) { char * ctemp = NULL; /* Pointer into string */ char * endptr = NULL;/* Pointer to string after number */ double retval; /* Return value from strtod */ /* We have to copy the string in order to modify the exponents from Fortran style. Rather than using malloc we have a static buffer. Technically we only have to do the copy if we have a D or d in the string. */ char tempbuf[256]; #if SCAN_FOR_MINUS int dreslt_sign = 1; int ipos = *nstrt; const char * cctemp = NULL; /* Scan the string looking for a minus sign. Then update the start position for the subsequent copy iff we find a '-'. Note that commas are a special delimiter so we stop looking for a minus if we find one or if we find a digit. */ cctemp = &(string[ipos-1]); while (!isdigit(*cctemp) && (*cctemp != ',') && (*cctemp != '\0')) { if (*cctemp == '-') { *nstrt = ipos; dreslt_sign = -1; break; } ipos++; cctemp++; } #endif /* Correct for SLA use of fortran convention */ #if HAVE_STAR_UTIL_H star_strlcpy( tempbuf, &(string[*nstrt-1]), sizeof(tempbuf) ); #else # if HAVE_STRLCPY strlcpy( tempbuf, &(string[*nstrt-1]), sizeof(tempbuf) ); # else /* Use standard C interface */ strncpy( tempbuf, &(string[*nstrt-1]), sizeof(tempbuf)); tempbuf[sizeof(tempbuf)-1] = '\0'; # endif #endif /* Convert d or D to E */ ctemp = tempbuf; while (*ctemp != '\0') { if (*ctemp == 'd' || *ctemp == 'D') *ctemp = 'E'; ctemp++; } /* strtod man page indicates that we should reset errno before calling strtod */ errno = 0; /* We know we are starting at the beginning of the string now */ retval = strtod( tempbuf, &endptr ); if (retval == 0.0 && endptr == tempbuf) { /* conversion did not find anything */ *jflag = 1; /* but SLA compatibility requires that we step through to remove leading spaces. We also step through alphabetic characters since they can never be numbers standalone (no number starts with an 'E') */ while (ISBLANK(*endptr) || isalpha(*endptr) ) { endptr++; } } else if ( errno == ERANGE ) { *jflag = 2; } else { #if SCAN_FOR_MINUS *jflag = (dreslt_sign < 0 ? -1 : 0); #else if ( retval < 0.0 ) { *jflag = -1; } else if ( retval == 0.0 ) { /* Need to distinguish -0 from +0 */ double test = copysign( 1.0, retval ); if ( test < 0.0 ) { *jflag = -1; } else { *jflag = 0; } } else { *jflag = 0; } #endif } /* Sort out the position for the next index */ *nstrt += endptr - tempbuf; /* Skip a comma */ if (*endptr == ',') { (*nstrt)++; } else { /* jump past any leading spaces for the next part of the string */ ctemp = endptr; while ( ISBLANK(*ctemp) ) { (*nstrt)++; ctemp++; } } /* And the result unless we found nothing */ if (*jflag != 1) *dreslt = retval; } pal-0.5.0/palDh2e.c000644 000765 000024 00000007211 12366000607 014022 0ustar00timjstaff000000 000000 /* *+ * Name: * palDh2e * Purpose: * Horizon to equatorial coordinates: Az,El to HA,Dec * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * palDh2e( double az, double el, double phi, double * ha, double * dec ); * Arguments: * az = double (Given) * Azimuth (radians) * el = double (Given) * Elevation (radians) * phi = double (Given) * Observatory latitude (radians) * ha = double * (Returned) * Hour angle (radians) * dec = double * (Returned) * Declination (radians) * Description: * Convert horizon to equatorial coordinates. * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - All the arguments are angles in radians. * - The sign convention for azimuth is north zero, east +pi/2. * - HA is returned in the range +/-pi. Declination is returned * in the range +/-pi/2. * - The latitude is (in principle) geodetic. In critical * applications, corrections for polar motion should be applied. * - In some applications it will be important to specify the * correct type of elevation in order to produce the required * type of HA,Dec. In particular, it may be important to * distinguish between the elevation as affected by refraction, * which will yield the "observed" HA,Dec, and the elevation * in vacuo, which will yield the "topocentric" HA,Dec. If the * effects of diurnal aberration can be neglected, the * topocentric HA,Dec may be used as an approximation to the * "apparent" HA,Dec. * - No range checking of arguments is done. * - In applications which involve many such calculations, rather * than calling the present routine it will be more efficient to * use inline code, having previously computed fixed terms such * as sine and cosine of latitude. * History: * 2012-02-08 (TIMJ): * Initial version with documentation taken from Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1996 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include void palDh2e ( double az, double el, double phi, double *ha, double *dec) { double sa; double ca; double se; double ce; double sp; double cp; double x; double y; double z; double r; /* Useful trig functions */ sa = sin(az); ca = cos(az); se = sin(el); ce = cos(el); sp = sin(phi); cp = cos(phi); /* HA,Dec as x,y,z */ x = -ca * ce * sp + se * cp; y = -sa * ce; z = ca * ce * cp + se * sp; /* To HA,Dec */ r = sqrt(x * x + y * y); if (r == 0.) { *ha = 0.; } else { *ha = atan2(y, x); } *dec = atan2(z, r); return; } pal-0.5.0/palDjcal.c000644 000765 000024 00000004770 12366000612 014260 0ustar00timjstaff000000 000000 /* *+ * Name: * palDjcal * Purpose: * Modified Julian Date to Gregorian Calendar * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palDjcal ( int ndp, double djm, int iymdf[4], int *j ); * Arguments: * ndp = int (Given) * Number of decimal places of days in fraction. * djm = double (Given) * Modified Julian Date (JD-2400000.5) * iymdf[4] = int[] (Returned) * Year, month, day, fraction in Gregorian calendar. * j = status (Returned) * 0 = OK. See eraJd2cal for other values. * Description: * Modified Julian Date to Gregorian Calendar, expressed * in a form convenient for formatting messages (namely * rounded to a specified precision, and with the fields * stored in a single array) * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * History: * 2012-02-10 (TIMJ): * Initial version with documentation taken from Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Notes: * - Uses eraJd2cal * Copyright: * Copyright (C) 2004 Patrick T. Wallace * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include #include "pal.h" #include "palmac.h" #include "pal1sofa.h" void palDjcal ( int ndp, double djm, int iymdf[4], int *j ) { double frac = 0.0; double nfd; *j = eraJd2cal( PAL__MJD0, djm, &(iymdf[0]), &(iymdf[1]), &(iymdf[2]), &frac); /* Convert ndp to a power of 10 */ nfd = pow( 10., (double)ndp ); /* Multiply the fraction */ frac *= nfd; /* and now we want to round to the nearest integer */ iymdf[3] = (int)DNINT(frac); } pal-0.5.0/palDmat.c000644 000765 000024 00000010300 12365762531 014130 0ustar00timjstaff000000 000000 /* *+ * Name: * palDmat * Purpose: * Matrix inversion & solution of simultaneous equations * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palDmat( int n, double *a, double *y, double *d, int *jf, * int *iw ); * Arguments: * n = int (Given) * Number of simultaneous equations and number of unknowns. * a = double[] (Given & Returned) * A non-singular NxN matrix (implemented as a contiguous block * of memory). After calling this routine "a" contains the * inverse of the matrix. * y = double[] (Given & Returned) * On input the vector of N knowns. On exit this vector contains the * N solutions. * d = double * (Returned) * The determinant. * jf = int * (Returned) * The singularity flag. If the matrix is non-singular, jf=0 * is returned. If the matrix is singular, jf=-1 & d=0.0 are * returned. In the latter case, the contents of array "a" on * return are undefined. * iw = int[] (Given) * Integer workspace of size N. * Description: * Matrix inversion & solution of simultaneous equations * For the set of n simultaneous equations in n unknowns: * A.Y = X * this routine calculates the inverse of A, the determinant * of matrix A and the vector of N unknowns. * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * History: * 2012-02-11 (TIMJ): * Combination of a port of the Fortran and a comparison * with the obfuscated GPL C routine. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Notes: * - Implemented using Gaussian elimination with partial pivoting. * - Optimized for speed rather than accuracy with errors 1 to 4 * times those of routines optimized for accuracy. * Copyright: * Copyright (C) 2001 Rutherford Appleton Laboratory. * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" void palDmat ( int n, double *a, double *y, double *d, int *jf, int *iw ) { const double SFA = 1e-20; int k; double*aoff; *jf=0; *d=1.0; for(k=0,aoff=a; kamx){ amx=t; imx=i; aoff2=apos2; } } } if(amx0;){ int ki=iw[k]; if(k!=ki){ int i; double *apos = a; for(i=0;i=0; N--) { /* DO N=NL, 1, -1 */ COEFF=TL[N]; EMN=(double)(ITL[N][0]); EMPN=(double)(ITL[N][1]); DN=(double)(ITL[N][2]); FN=(double)(ITL[N][3]); I=ITL[N][4]; if (I == 0) { EN=1.; DEN=0.; } else if (I == 1) { EN=E; DEN=DE; } else { EN=ESQ; DEN=DESQ; } THETA=EMN*EM+EMPN*EMP+DN*D+FN*F; DTHETA=EMN*DEM+EMPN*DEMP+DN*DD+FN*DF; FTHETA=sin(THETA); V=V+COEFF*FTHETA*EN; DV=DV+COEFF*(cos(THETA)*DTHETA*EN+FTHETA*DEN); } EL=ELP+PAL__DD2R*V; DEL=(DELP+PAL__DD2R*DV)/CJ; /* Latitude */ V=0.; DV=0.; for (N=NB-1; N>=0; N--) { /* DO N=NB,1,-1 */ COEFF=TB[N]; EMN=(double)(ITB[N][0]); EMPN=(double)(ITB[N][1]); DN=(double)(ITB[N][2]); FN=(double)(ITB[N][3]); I=ITB[N][4]; if (I == 0 ) { EN=1.; DEN=0.; } else if (I == 1) { EN=E; DEN=DE; } else { EN=ESQ; DEN=DESQ; } THETA=EMN*EM+EMPN*EMP+DN*D+FN*F; DTHETA=EMN*DEM+EMPN*DEMP+DN*DD+FN*DF; FTHETA=sin(THETA); V=V+COEFF*FTHETA*EN; DV=DV+COEFF*(cos(THETA)*DTHETA*EN+FTHETA*DEN); } BF=1.-CW1*COSOM-CW2*COSWOM; DBF=CW1*DOM*SINOM+CW2*DWOM*SINWOM; B=PAL__DD2R*V*BF; DB=PAL__DD2R*(DV*BF+V*DBF)/CJ; /* Parallax */ V=0.; DV=0.; for (N=NP-1; N>=0; N--) { /* DO N=NP,1,-1 */ COEFF=TP[N]; EMN=(double)(ITP[N][0]); EMPN=(double)(ITP[N][1]); DN=(double)(ITP[N][2]); FN=(double)(ITP[N][3]); I=ITP[N][4]; if (I == 0) { EN=1.; DEN=0.; } else if (I == 1) { EN=E; DEN=DE; } else { EN=ESQ; DEN=DESQ; } THETA=EMN*EM+EMPN*EMP+DN*D+FN*F; DTHETA=EMN*DEM+EMPN*DEMP+DN*DD+FN*DF; FTHETA=cos(THETA); V=V+COEFF*FTHETA*EN; DV=DV+COEFF*(-sin(THETA)*DTHETA*EN+FTHETA*DEN); } P=PAL__DD2R*V; DP=PAL__DD2R*DV/CJ; /* * Transformation into final form */ /* Parallax to distance (AU, AU/sec) */ SP=sin(P); R=ERADAU/SP; DR=-R*DP*cos(P)/SP; /* Longitude, latitude to x,y,z (AU) */ SEL=sin(EL); CEL=cos(EL); SB=sin(B); CB=cos(B); RCB=R*CB; RBD=R*DB; W=RBD*SB-CB*DR; X=RCB*CEL; Y=RCB*SEL; Z=R*SB; XD=-Y*DEL-W*CEL; YD=X*DEL-W*SEL; ZD=RBD*CB+SB*DR; /* Julian centuries since J2000 */ T=(date-51544.5)/36525.; /* Fricke equinox correction */ EPJ=2000.+T*100.; EQCOR=PAL__DS2R*(0.035+0.00085*(EPJ-B1950)); /* Mean obliquity (IAU 1976) */ EPS=PAL__DAS2R*(84381.448+(-46.8150+(-0.00059+0.001813*T)*T)*T); /* To the equatorial system, mean of date, FK5 system */ SINEPS=sin(EPS); COSEPS=cos(EPS); ES=EQCOR*SINEPS; EC=EQCOR*COSEPS; pv[0]=X-EC*Y+ES*Z; pv[1]=EQCOR*X+Y*COSEPS-Z*SINEPS; pv[2]=Y*SINEPS+Z*COSEPS; pv[3]=XD-EC*YD+ES*ZD; pv[4]=EQCOR*XD+YD*COSEPS-ZD*SINEPS; pv[5]=YD*SINEPS+ZD*COSEPS; } pal-0.5.0/palDrange.c000644 000765 000024 00000003667 12366000607 014453 0ustar00timjstaff000000 000000 /* *+ * Name: * palDrange * Purpose: * Normalize angle into range +/- pi * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * palDrange( double angle ) * Arguments: * angle = double (Given) * The angle in radians. * Description: * The result is "angle" expressed in the range +/- pi. If the * supplied value for "angle" is equal to +/- pi, it is returned * unchanged. * Authors: * DSB: David S Berry (JAC, Hawaii) * PTW: Patrick T. Wallace * {enter_new_authors_here} * History: * 2012-05-09 (DSB): * Initial version with documentation taken from Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1995 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "palmac.h" #include double palDrange( double angle ){ double result = fmod( angle, PAL__D2PI ); if( result > PAL__DPI ) { result -= PAL__D2PI; } else if( result < -PAL__DPI ) { result += PAL__D2PI; } return result; } pal-0.5.0/palDs2tp.c000644 000765 000024 00000006600 12366000607 014235 0ustar00timjstaff000000 000000 /* *+ * Name: * palDs2tp * Purpose: * Spherical to tangent plane projection * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * palDs2tp( double ra, double dec, double raz, double decz, * double *xi, double *eta, int *j ); * Arguments: * ra = double (Given) * RA spherical coordinate of point to be projected (radians) * dec = double (Given) * Dec spherical coordinate of point to be projected (radians) * raz = double (Given) * RA spherical coordinate of tangent point (radians) * decz = double (Given) * Dec spherical coordinate of tangent point (radians) * xi = double * (Returned) * First rectangular coordinate on tangent plane (radians) * eta = double * (Returned) * Second rectangular coordinate on tangent plane (radians) * j = int * (Returned) * status: 0 = OK, star on tangent plane * 1 = error, star too far from axis * 2 = error, antistar on tangent plane * 3 = error, antistar too far from axis * Description: * Projection of spherical coordinates onto tangent plane: * "gnomonic" projection - "standard coordinates" * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * History: * 2012-02-08 (TIMJ): * Initial version with documentation taken from Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1996 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include void palDs2tp ( double ra, double dec, double raz, double decz, double *xi, double *eta, int *j ) { const double TINY = 1.0e-6; double cdec; double sdec; double radif; double cdecz; double denom; double sdecz; double cradif; double sradif; /* Trig functions */ sdecz = sin(decz); sdec = sin(dec); cdecz = cos(decz); cdec = cos(dec); radif = ra - raz; sradif = sin(radif); cradif = cos(radif); /* Reciprocal of star vector length to tangent plane */ denom = sdec * sdecz + cdec * cdecz * cradif; /* Handle vectors too far from axis */ if (denom > TINY) { *j = 0; } else if (denom >= 0.) { *j = 1; denom = TINY; } else if (denom > -TINY) { *j = 2; denom = -TINY; } else { *j = 3; } /* Compute tangent plane coordinates (even in dubious cases) */ *xi = cdec * sradif / denom; *eta = (sdec * cdecz - cdec * sdecz * cradif) / denom; return; } pal-0.5.0/palDt.c000644 000765 000024 00000007057 12366000607 013617 0ustar00timjstaff000000 000000 /* *+ * Name: * palDt * Purpose: * Estimate the offset between dynamical time and UT * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * double palDt( double epoch ); * Arguments: * epoch = double (Given) * Julian epoch (e.g. 1850.0) * Returned Value: * palDt = double * Rough estimate of ET-UT (after 1984, TT-UT) at the * given epoch, in seconds. * Description: * Estimate the offset between dynamical time and Universal Time * for a given historical epoch. * Authors: * TIMJ: Tim Jenness (JAC, Hawaii) * PTW: Patrick T. Wallace * {enter_new_authors_here} * Notes: * - Depending on the epoch, one of three parabolic approximations * is used: * * before 979 Stephenson & Morrison's 390 BC to AD 948 model * 979 to 1708 Stephenson & Morrison's 948 to 1600 model * after 1708 McCarthy & Babcock's post-1650 model * * The breakpoints are chosen to ensure continuity: they occur * at places where the adjacent models give the same answer as * each other. * - The accuracy is modest, with errors of up to 20 sec during * the interval since 1650, rising to perhaps 30 min by 1000 BC. * Comparatively accurate values from AD 1600 are tabulated in * the Astronomical Almanac (see section K8 of the 1995 AA). * - The use of double-precision for both argument and result is * purely for compatibility with other SLALIB time routines. * - The models used are based on a lunar tidal acceleration value * of -26.00 arcsec per century. * * See Also: * Explanatory Supplement to the Astronomical Almanac, * ed P.K.Seidelmann, University Science Books (1992), * section 2.553, p83. This contains references to * the Stephenson & Morrison and McCarthy & Babcock * papers. * History: * 2012-03-08 (TIMJ): * Initial version with documentation from SLA/F. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1995 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" double palDt ( double epoch ) { double t,w,s; /* Centuries since 1800 */ t = (epoch - 1800.0) / 100.0; /* Select model */ if ( epoch >= 1708.185161980887 ) { /* Post-1708: use McCarthy & Babcock */ w = t - 0.19; s = 5.156 + 13.3066 * w * w; } else if ( epoch >= 979.0258204760233 ) { /* 978-1708: use Stephenson & Morrison's 948-1600 model */ s = 25.5 * t * t; } else { /* Pre-979: use Stephenson & Morrison's 390 BC to AD 948 model */ s = 1360.0 + (320.0 + 44.3*t) * t; } return s; } pal-0.5.0/palDtp2s.c000644 000765 000024 00000005056 12366000612 014235 0ustar00timjstaff000000 000000 /* *+ * Name: * palDtp2s * Purpose: * Tangent plane to spherical coordinates * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * palDtp2s( double xi, double eta, double raz, double decz, * double *ra, double *dec); * Arguments: * xi = double (Given) * First rectangular coordinate on tangent plane (radians) * eta = double (Given) * Second rectangular coordinate on tangent plane (radians) * raz = double (Given) * RA spherical coordinate of tangent point (radians) * decz = double (Given) * Dec spherical coordinate of tangent point (radians) * ra = double * (Returned) * RA spherical coordinate of point to be projected (radians) * dec = double * (Returned) * Dec spherical coordinate of point to be projected (radians) * Description: * Transform tangent plane coordinates into spherical. * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * History: * 2012-02-08 (TIMJ): * Initial version with documentation taken from Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1995 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "pal1sofa.h" #include void palDtp2s ( double xi, double eta, double raz, double decz, double *ra, double *dec ) { double cdecz; double denom; double sdecz; double d; sdecz = sin(decz); cdecz = cos(decz); denom = cdecz - eta * sdecz; d = atan2(xi, denom) + raz; *ra = eraAnp(d); *dec = atan2(sdecz + eta * cdecz, sqrt(xi * xi + denom * denom)); return; } pal-0.5.0/palDtps2c.c000644 000765 000024 00000011153 12366000612 014373 0ustar00timjstaff000000 000000 /* *+ * Name: * palDtps2c * Purpose: * Determine RA,Dec of tangent point from coordinates * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * palDtps2c( double xi, double eta, double ra, double dec, * double * raz1, double decz1, * double * raz2, double decz2, int *n); * Arguments: * xi = double (Given) * First rectangular coordinate on tangent plane (radians) * eta = double (Given) * Second rectangular coordinate on tangent plane (radians) * ra = double (Given) * RA spherical coordinate of star (radians) * dec = double (Given) * Dec spherical coordinate of star (radians) * raz1 = double * (Returned) * RA spherical coordinate of tangent point, solution 1 (radians) * decz1 = double * (Returned) * Dec spherical coordinate of tangent point, solution 1 (radians) * raz2 = double * (Returned) * RA spherical coordinate of tangent point, solution 2 (radians) * decz2 = double * (Returned) * Dec spherical coordinate of tangent point, solution 2 (radians) * n = int * (Returned) * number of solutions: 0 = no solutions returned (note 2) * 1 = only the first solution is useful (note 3) * 2 = both solutions are useful (note 3) * Description: * From the tangent plane coordinates of a star of known RA,Dec, * determine the RA,Dec of the tangent point. * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - The RAZ1 and RAZ2 values are returned in the range 0-2pi. * - Cases where there is no solution can only arise near the poles. * For example, it is clearly impossible for a star at the pole * itself to have a non-zero XI value, and hence it is * meaningless to ask where the tangent point would have to be * to bring about this combination of XI and DEC. * - Also near the poles, cases can arise where there are two useful * solutions. The argument N indicates whether the second of the * two solutions returned is useful. N=1 indicates only one useful * solution, the usual case; under these circumstances, the second * solution corresponds to the "over-the-pole" case, and this is * reflected in the values of RAZ2 and DECZ2 which are returned. * - The DECZ1 and DECZ2 values are returned in the range +/-pi, but * in the usual, non-pole-crossing, case, the range is +/-pi/2. * - This routine is the spherical equivalent of the routine sla_DTPV2C. * History: * 2012-02-08 (TIMJ): * Initial version with documentation taken from Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1995 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "pal1sofa.h" #include void palDtps2c( double xi, double eta, double ra, double dec, double * raz1, double * decz1, double * raz2, double * decz2, int *n) { double x2; double y2; double sd; double cd; double sdf; double r2; x2 = xi * xi; y2 = eta * eta; sd = sin(dec); cd = cos(dec); sdf = sd * sqrt(x2 + 1. + y2); r2 = cd * cd * (y2 + 1.) - sd * sd * x2; if (r2 >= 0.) { double r; double s; double c; r = sqrt(r2); s = sdf - eta * r; c = sdf * eta + r; if (xi == 0. && r == 0.) { r = 1.; } *raz1 = eraAnp(ra - atan2(xi, r)); *decz1 = atan2(s, c); r = -r; s = sdf - eta * r; c = sdf * eta + r; *raz2 = eraAnp(ra - atan2(xi, r)); *decz2 = atan2(s, c); if (fabs(sdf) < 1.) { *n = 1; } else { *n = 2; } } else { *n = 0; } return; } pal-0.5.0/palDtt.c000644 000765 000024 00000004102 12366000612 013763 0ustar00timjstaff000000 000000 /* *+ * Name: * palDtt * Purpose: * Return offset between UTC and TT * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * dtt = palDtt( double utc ); * Arguments: * utc = double (Given) * UTC date as a modified JD (JD-2400000.5) * Returned Value: * dtt = double * TT-UTC in seconds * Description: * Increment to be applied to Coordinated Universal Time UTC to give * Terrestrial Time TT (formerly Ephemeris Time ET) * Authors: * TIMJ: Tim Jenness (JAC, Hawaii) * PTW: Patrick T. Wallace * {enter_new_authors_here} * Notes: * - Consider a comprehensive upgrade to use the time transformations in SOFA's time * cookbook: http://www.erasofa.org/sofa_ts_c.pdf. * - See eraDat for a description of error conditions when calling this function * with a time outside of the UTC range. This behaviour differs from slaDtt. * History: * 2012-02-08 (TIMJ): * Initial version * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1995 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" double palDtt( double utc ) { return 32.184 + palDat( utc ); } pal-0.5.0/palEcmat.c000644 000765 000024 00000004377 12366000612 014277 0ustar00timjstaff000000 000000 /* *+ * Name: * palEcmat * Purpose: * Form the equatorial to ecliptic rotation matrix - IAU 2006 * precession model. * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * palEcmat( double date, double rmat[3][3] ) * Arguments: * date = double (Given) * TT as Modified Julian Date (JD-2400000.5). The difference * between TT and TDB is of the order of a millisecond or two * (i.e. about 0.02 arc-seconds). * rmat = double[3][3] (Returned) * Rotation matrix * Description: * The equatorial to ecliptic rotation matrix is found and returned. * The matrix is in the sense V(ecl) = RMAT * V(equ); the * equator, equinox and ecliptic are mean of date. * Authors: * PTW: Pat Wallace (STFC) * DSB: David Berry (JAC, Hawaii) * {enter_new_authors_here} * History: * 2012-02-10 (DSB): * Initial version with documentation taken from Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1996 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "palmac.h" #include "pal1sofa.h" void palEcmat( double date, double rmat[3][3] ) { /* Mean obliquity (the angle between the ecliptic and mean equator of date). */ double eps0 = eraObl06( PAL__MJD0, date ); /* Matrix */ palDeuler( "X", eps0, 0.0, 0.0, rmat ); } pal-0.5.0/palEl2ue.c000644 000765 000024 00000025334 12366000607 014222 0ustar00timjstaff000000 000000 /* *+ * Name: * palEl2ue * Purpose: * Transform conventional elements into "universal" form * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palEl2ue ( double date, int jform, double epoch, double orbinc, * double anode, double perih, double aorq, double e, * double aorl, double dm, double u[13], int *jstat ); * Arguments: * date = double (Given) * Epoch (TT MJD) of osculation (Note 3) * jform = int (Given) * Element set actually returned (1-3; Note 6) * epoch = double (Given) * Epoch of elements (TT MJD) * orbinc = double (Given) * inclination (radians) * anode = double (Given) * longitude of the ascending node (radians) * perih = double (Given) * longitude or argument of perihelion (radians) * aorq = double (Given) * mean distance or perihelion distance (AU) * e = double (Given) * eccentricity * aorl = double (Given) * mean anomaly or longitude (radians, JFORM=1,2 only) * dm = double (Given) * daily motion (radians, JFORM=1 only) * u = double [13] (Returned) * Universal orbital elements (Note 1) * - (0) combined mass (M+m) * - (1) total energy of the orbit (alpha) * - (2) reference (osculating) epoch (t0) * - (3-5) position at reference epoch (r0) * - (6-8) velocity at reference epoch (v0) * - (9) heliocentric distance at reference epoch * - (10) r0.v0 * - (11) date (t) * - (12) universal eccentric anomaly (psi) of date, approx * jstat = int * (Returned) * status: 0 = OK * - -1 = illegal JFORM * - -2 = illegal E * - -3 = illegal AORQ * - -4 = illegal DM * - -5 = numerical error * Description: * Transform conventional osculating elements into "universal" form. * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - The "universal" elements are those which define the orbit for the * purposes of the method of universal variables (see reference). * They consist of the combined mass of the two bodies, an epoch, * and the position and velocity vectors (arbitrary reference frame) * at that epoch. The parameter set used here includes also various * quantities that can, in fact, be derived from the other * information. This approach is taken to avoiding unnecessary * computation and loss of accuracy. The supplementary quantities * are (i) alpha, which is proportional to the total energy of the * orbit, (ii) the heliocentric distance at epoch, (iii) the * outwards component of the velocity at the given epoch, (iv) an * estimate of psi, the "universal eccentric anomaly" at a given * date and (v) that date. * - The companion routine is palUe2pv. This takes the set of numbers * that the present routine outputs and uses them to derive the * object's position and velocity. A single prediction requires one * call to the present routine followed by one call to palUe2pv; * for convenience, the two calls are packaged as the routine * palPlanel. Multiple predictions may be made by again calling the * present routine once, but then calling palUe2pv multiple times, * which is faster than multiple calls to palPlanel. * - DATE is the epoch of osculation. It is in the TT timescale * (formerly Ephemeris Time, ET) and is a Modified Julian Date * (JD-2400000.5). * - The supplied orbital elements are with respect to the J2000 * ecliptic and equinox. The position and velocity parameters * returned in the array U are with respect to the mean equator and * equinox of epoch J2000, and are for the perihelion prior to the * specified epoch. * - The universal elements returned in the array U are in canonical * units (solar masses, AU and canonical days). * - Three different element-format options are available: * * Option JFORM=1, suitable for the major planets: * * EPOCH = epoch of elements (TT MJD) * ORBINC = inclination i (radians) * ANODE = longitude of the ascending node, big omega (radians) * PERIH = longitude of perihelion, curly pi (radians) * AORQ = mean distance, a (AU) * E = eccentricity, e (range 0 to <1) * AORL = mean longitude L (radians) * DM = daily motion (radians) * * Option JFORM=2, suitable for minor planets: * * EPOCH = epoch of elements (TT MJD) * ORBINC = inclination i (radians) * ANODE = longitude of the ascending node, big omega (radians) * PERIH = argument of perihelion, little omega (radians) * AORQ = mean distance, a (AU) * E = eccentricity, e (range 0 to <1) * AORL = mean anomaly M (radians) * * Option JFORM=3, suitable for comets: * * EPOCH = epoch of perihelion (TT MJD) * ORBINC = inclination i (radians) * ANODE = longitude of the ascending node, big omega (radians) * PERIH = argument of perihelion, little omega (radians) * AORQ = perihelion distance, q (AU) * E = eccentricity, e (range 0 to 10) * * - Unused elements (DM for JFORM=2, AORL and DM for JFORM=3) are * not accessed. * - The algorithm was originally adapted from the EPHSLA program of * D.H.P.Jones (private communication, 1996). The method is based * on Stumpff's Universal Variables. * * See Also: * Everhart & Pitkin, Am.J.Phys. 51, 712 (1983). * History: * 2012-03-12 (TIMJ): * Initial version taken directly from SLA/F. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2005 Patrick T. Wallace * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include #include "pal.h" #include "palmac.h" void palEl2ue ( double date, int jform, double epoch, double orbinc, double anode, double perih, double aorq, double e, double aorl, double dm, double u[13], int *jstat ) { /* Sin and cos of J2000 mean obliquity (IAU 1976) */ const double SE=0.3977771559319137; const double CE=0.9174820620691818; int J; double PHT,ARGPH,Q,W,CM,ALPHA,PHS,SW,CW,SI,CI,SO,CO, X,Y,Z,PX,PY,PZ,VX,VY,VZ,DT,FC,FP,PSI, UL[13],PV[6]; /* Validate arguments. */ if (jform < 1 || jform > 3) { *jstat = -1; return; } if (e < 0.0 || e > 10.0 || (e >= 1.0 && jform != 3)) { *jstat = -2; return; } if (aorq <= 0.0) { *jstat = -3; return; } if (jform == 1 && dm <= 0.0) { *jstat = -4; return; } /* * Transform elements into standard form: * * PHT = epoch of perihelion passage * ARGPH = argument of perihelion (little omega) * Q = perihelion distance (q) * CM = combined mass, M+m (mu) */ if (jform == 1) { /* Major planet. */ PHT = epoch-(aorl-perih)/dm; ARGPH = perih-anode; Q = aorq*(1.0-e); W = dm/PAL__GCON; CM = W*W*aorq*aorq*aorq; } else if (jform == 2) { /* Minor planet. */ PHT = epoch-aorl*sqrt(aorq*aorq*aorq)/PAL__GCON; ARGPH = perih; Q = aorq*(1.0-e); CM = 1.0; } else { /* Comet. */ PHT = epoch; ARGPH = perih; Q = aorq; CM = 1.0; } /* The universal variable alpha. This is proportional to the total * energy of the orbit: -ve for an ellipse, zero for a parabola, * +ve for a hyperbola. */ ALPHA = CM*(e-1.0)/Q; /* Speed at perihelion. */ PHS = sqrt(ALPHA+2.0*CM/Q); /* In a Cartesian coordinate system which has the x-axis pointing * to perihelion and the z-axis normal to the orbit (such that the * object orbits counter-clockwise as seen from +ve z), the * perihelion position and velocity vectors are: * * position [Q,0,0] * velocity [0,PHS,0] * * To express the results in J2000 equatorial coordinates we make a * series of four rotations of the Cartesian axes: * * axis Euler angle * * 1 z argument of perihelion (little omega) * 2 x inclination (i) * 3 z longitude of the ascending node (big omega) * 4 x J2000 obliquity (epsilon) * * In each case the rotation is clockwise as seen from the +ve end of * the axis concerned. */ /* Functions of the Euler angles. */ SW = sin(ARGPH); CW = cos(ARGPH); SI = sin(orbinc); CI = cos(orbinc); SO = sin(anode); CO = cos(anode); /* Position at perihelion (AU). */ X = Q*CW; Y = Q*SW; Z = Y*SI; Y = Y*CI; PX = X*CO-Y*SO; Y = X*SO+Y*CO; PY = Y*CE-Z*SE; PZ = Y*SE+Z*CE; /* Velocity at perihelion (AU per canonical day). */ X = -PHS*SW; Y = PHS*CW; Z = Y*SI; Y = Y*CI; VX = X*CO-Y*SO; Y = X*SO+Y*CO; VY = Y*CE-Z*SE; VZ = Y*SE+Z*CE; /* Time from perihelion to date (in Canonical Days: a canonical day * is 58.1324409... days, defined as 1/PAL__GCON). */ DT = (date-PHT)*PAL__GCON; /* First approximation to the Universal Eccentric Anomaly, PSI, * based on the circle (FC) and parabola (FP) values. */ FC = DT/Q; W = pow(3.0*DT+sqrt(9.0*DT*DT+8.0*Q*Q*Q), 1.0/3.0); FP = W-2.0*Q/W; PSI = (1.0-e)*FC+e*FP; /* Assemble local copy of element set. */ UL[0] = CM; UL[1] = ALPHA; UL[2] = PHT; UL[3] = PX; UL[4] = PY; UL[5] = PZ; UL[6] = VX; UL[7] = VY; UL[8] = VZ; UL[9] = Q; UL[10] = 0.0; UL[11] = date; UL[12] = PSI; /* Predict position+velocity at epoch of osculation. */ palUe2pv( date, UL, PV, &J ); if (J != 0) { *jstat = -5; return; } /* Convert back to universal elements. */ palPv2ue( PV, date, CM-1.0, u, &J ); if (J != 0) { *jstat = -5; return; } /* OK exit. */ *jstat = 0; } pal-0.5.0/palEpco.c000644 000765 000024 00000005432 12366000612 014125 0ustar00timjstaff000000 000000 /* *+ * Name: * palEpco * Purpose: * Convert an epoch into the appropriate form - 'B' or 'J' * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * double palEpco( char k0, char k, double e ); * Arguments: * k0 = char (Given) * Form of result: 'B'=Besselian, 'J'=Julian * k = char (Given) * Form of given epoch: 'B' or 'J'. * Description: * Converts a Besselian or Julian epoch to a Julian or Besselian * epoch. * Authors: * PTW: Patrick T. Wallace * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - The result is always either equal to or very close to * the given epoch E. The routine is required only in * applications where punctilious treatment of heterogeneous * mixtures of star positions is necessary. * - k and k0 are case insensitive. This differes slightly from the * Fortran SLA implementation. * - k and k0 are not validated. They are interpreted as follows: * o If k0 and k are the same the result is e * o If k0 is 'b' or 'B' and k isn't the conversion is J to B. * o In all other cases, the conversion is B to J. * History: * 2012-03-01 (TIMJ): * Initial version. Documentation from SLA/F. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1995 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, MA 02110-1301 * USA. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "pal1sofa.h" #include double palEpco( char k0, char k, double e ) { double new_epoch = 0.0; double djm; double djm0; /* Use upper case */ k0 = toupper( k0 ); k = toupper( k ); if (k == k0) { new_epoch = e; } else if (k0 == 'B') { eraEpj2jd( e, &djm0, &djm ); new_epoch = eraEpb( djm0, djm ); } else { eraEpb2jd( e, &djm0, &djm ); new_epoch = eraEpj( djm0, djm ); } return new_epoch; } pal-0.5.0/palEpv.c000644 000765 000024 00000005037 12366000611 013771 0ustar00timjstaff000000 000000 /* *+ * Name: * palEpv * Purpose: * Earth position and velocity with respect to the BCRS * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palEpv( double date, double ph[3], double vh[3], * double pb[3], double vb[3] ); * Arguments: * date = double (Given) * Date, TDB Modified Julian Date (JD-2400000.5) * ph = double [3] (Returned) * Heliocentric Earth position (AU) * vh = double [3] (Returned) * Heliocentric Earth velocity (AU/day) * pb = double [3] (Returned) * Barycentric Earth position (AU) * vb = double [3] (Returned) * Barycentric Earth velocity (AU/day) * Description: * Earth position and velocity, heliocentric and barycentric, with * respect to the Barycentric Celestial Reference System. * Authors: * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - See eraEpv00 for details on accuracy * - Note that the status argument from eraEpv00 is ignored * History: * 2012-03-12 (TIMJ): * Initial version * Adapted with permission from the Fortran SLALIB library * but now mainly calls SOFA routines. * {enter_further_changes_here} * Copyright: * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include "palmac.h" #include "pal.h" #include "pal1sofa.h" void palEpv( double date, double ph[3], double vh[3], double pb[3], double vb[3] ) { int i; double pvh[2][3]; double pvb[2][3]; eraEpv00( PAL__MJD0, date, pvh, pvb ); /* Copy into output arrays */ for (i=0; i<3; i++) { ph[i] = pvh[0][i]; vh[i] = pvh[1][i]; pb[i] = pvb[0][i]; vb[i] = pvb[1][i]; } } pal-0.5.0/palEqecl.c000644 000765 000024 00000005151 12366000611 014265 0ustar00timjstaff000000 000000 /* *+ * Name: * palEqecl * Purpose: * Transform from J2000.0 equatorial coordinates to ecliptic coordinates * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palEqecl( double dr, double dd, double date, * double *dl, double *db); * Arguments: * dr = double (Given) * J2000.0 mean RA (radians) * dd = double (Given) * J2000.0 mean Dec (Radians) * date = double (Given) * TT as Modified Julian Date (JD-2400000.5). The difference * between TT and TDB is of the order of a millisecond or two * (i.e. about 0.02 arc-seconds). * dl = double * (Returned) * Ecliptic longitude (mean of date, IAU 1980 theory, radians) * db = double * (Returned) * Ecliptic latitude (mean of date, IAU 1980 theory, radians) * Description: * Transform from J2000.0 equatorial coordinates to ecliptic coordinates. * Authors: * PTW: Patrick T. Wallace * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * History: * 2012-03-02 (TIMJ): * Initial version * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1995 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "pal1sofa.h" void palEqecl ( double dr, double dd, double date, double *dl, double *db ) { double v1[3], v2[3]; double rmat[3][3]; /* Spherical to Cartesian */ eraS2c( dr, dd, v1 ); /* Mean J2000 to mean of date */ palPrec( 2000.0, palEpj(date), rmat ); eraRxp( rmat, v1, v2 ); /* Equatorial to ecliptic */ palEcmat( date, rmat ); eraRxp( rmat, v2, v1 ); /* Cartesian to spherical */ eraC2s( v1, dl, db ); } pal-0.5.0/palEqgal.c000644 000765 000024 00000006150 12366000611 014265 0ustar00timjstaff000000 000000 /* *+ * Name: * palEqgal * Purpose: * Convert from J2000.0 equatorial coordinates to Galactic * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palEqgal ( double dr, double dd, double *dl, double *db ); * Arguments: * dr = double (Given) * J2000.0 RA (radians) * dd = double (Given) * J2000.0 Dec (radians * dl = double * (Returned) * Galactic longitude (radians). * db = double * (Returned) * Galactic latitude (radians). * Description: * Transformation from J2000.0 equatorial coordinates * to IAU 1958 galactic coordinates. * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * The equatorial coordinates are J2000.0. Use the routine * palGe50 if conversion to B1950.0 'FK4' coordinates is * required. * See Also: * Blaauw et al, Mon.Not.R.Astron.Soc.,121,123 (1960) * History: * 2012-02-12(TIMJ): * Initial version with documentation taken from Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1998 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "pal1sofa.h" void palEqgal ( double dr, double dd, double *dl, double *db ) { double v1[3]; double v2[3]; /* * L2,B2 system of galactic coordinates * * P = 192.25 RA of galactic north pole (mean B1950.0) * Q = 62.6 inclination of galactic to mean B1950.0 equator * R = 33 longitude of ascending node * * P,Q,R are degrees * * Equatorial to galactic rotation matrix (J2000.0), obtained by * applying the standard FK4 to FK5 transformation, for zero proper * motion in FK5, to the columns of the B1950 equatorial to * galactic rotation matrix: */ double rmat[3][3] = { { -0.054875539726,-0.873437108010,-0.483834985808 }, { +0.494109453312,-0.444829589425,+0.746982251810 }, { -0.867666135858,-0.198076386122,+0.455983795705 } }; /* Spherical to Cartesian */ eraS2c( dr, dd, v1 ); /* Equatorial to Galactic */ eraRxp( rmat, v1, v2 ); /* Cartesian to spherical */ eraC2s( v2, dl, db ); /* Express in conventional ranges */ *dl = eraAnp( *dl ); *db = eraAnpm( *db ); } pal-0.5.0/palEtrms.c000644 000765 000024 00000005427 12366000607 014341 0ustar00timjstaff000000 000000 /* *+ * Name: * palEtrms * Purpose: * Compute the E-terms vector * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palEtrms ( double ep, double ev[3] ); * Arguments: * ep = double (Given) * Besselian epoch * ev = double [3] (Returned) * E-terms as (dx,dy,dz) * Description: * Computes the E-terms (elliptic component of annual aberration) * vector. * * Note the use of the J2000 aberration constant (20.49552 arcsec). * This is a reflection of the fact that the E-terms embodied in * existing star catalogues were computed from a variety of * aberration constants. Rather than adopting one of the old * constants the latest value is used here. * * See also: * - Smith, C.A. et al., 1989. Astr.J. 97, 265. * - Yallop, B.D. et al., 1989. Astr.J. 97, 274. * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * History: * 2012-02-12 (TIMJ): * Initial version with documentation taken from Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1996 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "palmac.h" void palEtrms ( double ep, double ev[3] ) { /* Use the J2000 aberration constant */ const double ABCONST = 20.49552; double t, e, e0, p, ek, cp; /* Julian centuries since B1950 */ t = (ep - 1950.) * .0100002135903; /* Eccentricity */ e = .01673011 - (t * 1.26e-7 + 4.193e-5) * t; /* Mean obliquity */ e0 = (84404.836 - ((t * .00181 + .00319) * t + 46.8495) * t) * PAL__DAS2R; /* Mean longitude of perihelion */ p = (((t * .012 + 1.65) * t + 6190.67) * t + 1015489.951) * PAL__DAS2R; /* E-terms */ ek = e * ABCONST * PAL__DAS2R; cp = cos(p); ev[0] = ek * sin(p); ev[1] = -ek * cp * cos(e0); ev[2] = -ek * cp * sin(e0); } pal-0.5.0/palEvp.c000644 000765 000024 00000006166 12366000611 013775 0ustar00timjstaff000000 000000 /* *+ * Name: * palEvp * Purpose: * Returns the barycentric and heliocentric velocity and position of the * Earth. * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palEvp( double date, double deqx, double dvb[3], double dpb[3], * double dvh[3], double dph[3] ) * Arguments: * date = double (Given) * TDB (loosely ET) as a Modified Julian Date (JD-2400000.5) * deqx = double (Given) * Julian epoch (e.g. 2000.0) of mean equator and equinox of the * vectors returned. If deqx <= 0.0, all vectors are referred to the * mean equator and equinox (FK5) of epoch date. * dvb = double[3] (Returned) * Barycentric velocity (AU/s, AU) * dpb = double[3] (Returned) * Barycentric position (AU/s, AU) * dvh = double[3] (Returned) * heliocentric velocity (AU/s, AU) * dph = double[3] (Returned) * Heliocentric position (AU/s, AU) * Description: * Returns the barycentric and heliocentric velocity and position of the * Earth at a given epoch, given with respect to a specified equinox. * For information about accuracy, see the function eraEpv00. * Authors: * PTW: Pat Wallace (STFC) * {enter_new_authors_here} * History: * 2012-02-13 (PTW): * Initial version. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2005 Patrick T. Wallace * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "palmac.h" #include "pal1sofa.h" void palEvp( double date, double deqx, double dvb[3], double dpb[3], double dvh[3], double dph[3] ){ /* Local Variables; */ int i; double pvh[2][3], pvb[2][3], d1, d2, r[3][3]; /* BCRS PV-vectors. */ eraEpv00 ( 2400000.5, date, pvh, pvb ); /* Was precession to another equinox requested? */ if ( deqx > 0.0 ) { /* Yes: compute precession matrix from J2000.0 to deqx. */ eraEpj2jd ( deqx, &d1, &d2 ); eraPmat06 ( d1, d2, r ); /* Rotate the PV-vectors. */ eraRxpv ( r, pvh, pvh ); eraRxpv ( r, pvb, pvb ); } /* Return the required vectors. */ for ( i = 0; i < 3; i++ ) { dvh[i] = pvh[1][i] / PAL__SPD; dvb[i] = pvb[1][i] / PAL__SPD; dph[i] = pvh[0][i]; dpb[i] = pvb[0][i]; } } pal-0.5.0/palFk45z.c000644 000765 000024 00000014352 12366000611 014142 0ustar00timjstaff000000 000000 /* *+ * Name: * palFk45z * Purpose: * Convert B1950.0 FK4 star data to J2000.0 FK5 assuming zero * proper motion in the FK5 frame * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * palFk45z( double r1950, double d1950, double bepoch, double *r2000, * double *d2000 ) * Arguments: * r1950 = double (Given) * B1950.0 FK4 RA at epoch (radians). * d1950 = double (Given) * B1950.0 FK4 Dec at epoch (radians). * bepoch = double (Given) * Besselian epoch (e.g. 1979.3) * r2000 = double (Returned) * J2000.0 FK5 RA (Radians). * d2000 = double (Returned) * J2000.0 FK5 Dec(Radians). * Description: * Convert B1950.0 FK4 star data to J2000.0 FK5 assuming zero * proper motion in the FK5 frame (double precision) * * This function converts stars from the Bessel-Newcomb, FK4 * system to the IAU 1976, FK5, Fricke system, in such a * way that the FK5 proper motion is zero. Because such a star * has, in general, a non-zero proper motion in the FK4 system, * the routine requires the epoch at which the position in the * FK4 system was determined. * * The method is from Appendix 2 of Ref 1, but using the constants * of Ref 4. * Notes: * - The epoch BEPOCH is strictly speaking Besselian, but if a * Julian epoch is supplied the result will be affected only to * a negligible extent. * * - Conversion from Besselian epoch 1950.0 to Julian epoch 2000.0 * only is provided for. Conversions involving other epochs will * require use of the appropriate precession, proper motion, and * E-terms routines before and/or after palFk45z is called. * * - In the FK4 catalogue the proper motions of stars within 10 * degrees of the poles do not embody the differential E-term effect * and should, strictly speaking, be handled in a different manner * from stars outside these regions. However, given the general lack * of homogeneity of the star data available for routine astrometry, * the difficulties of handling positions that may have been * determined from astrometric fields spanning the polar and non-polar * regions, the likelihood that the differential E-terms effect was not * taken into account when allowing for proper motion in past * astrometry, and the undesirability of a discontinuity in the * algorithm, the decision has been made in this routine to include the * effect of differential E-terms on the proper motions for all stars, * whether polar or not. At epoch 2000, and measuring on the sky rather * than in terms of dRA, the errors resulting from this simplification * are less than 1 milliarcsecond in position and 1 milliarcsecond per * century in proper motion. * * References: * - Aoki,S., et al, 1983. Astron.Astrophys., 128, 263. * - Smith, C.A. et al, 1989. "The transformation of astrometric * catalog systems to the equinox J2000.0". Astron.J. 97, 265. * - Yallop, B.D. et al, 1989. "Transformation of mean star places * from FK4 B1950.0 to FK5 J2000.0 using matrices in 6-space". * Astron.J. 97, 274. * - Seidelmann, P.K. (ed), 1992. "Explanatory Supplement to * the Astronomical Almanac", ISBN 0-935702-68-7. * Authors: * PTW: Pat Wallace (STFC) * DSB: David Berry (JAC, Hawaii) * {enter_new_authors_here} * History: * 2012-02-10 (DSB): * Initial version with documentation taken from Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1998 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "palmac.h" #include "pal1sofa.h" void palFk45z( double r1950, double d1950, double bepoch, double *r2000, double *d2000 ){ /* Local Variables: */ double w; int i; int j; double r0[3], a1[3], v1[3], v2[6]; /* Position and position+velocity vectors */ /* CANONICAL CONSTANTS (see references) */ /* Vector A. */ double a[3] = { -1.62557E-6, -0.31919E-6, -0.13843E-6 }; /* Vectors Adot. */ double ad[3] = { 1.245E-3, -1.580E-3, -0.659E-3 }; /* Matrix M (only half of which is needed here). */ double em[6][3] = { {0.9999256782, -0.0111820611, -0.0048579477}, {0.0111820610, 0.9999374784, -0.0000271765}, {0.0048579479, -0.0000271474, 0.9999881997}, {-0.000551, -0.238565, 0.435739}, {0.238514, -0.002667, -0.008541}, {-0.435623, 0.012254, 0.002117} }; /* Spherical to Cartesian. */ eraS2c( r1950, d1950, r0 ); /* Adjust vector A to give zero proper motion in FK5. */ w = ( bepoch - 1950.0 )/PAL__PMF; for( i = 0; i < 3; i++ ) { a1[ i ] = a[ i ] + w*ad[ i ]; } /* Remove e-terms. */ w = r0[ 0 ]*a1[ 0 ] + r0[ 1 ]*a1[ 1 ] + r0[ 2 ]*a1[ 2 ]; for( i = 0; i < 3; i++ ) { v1[ i ] = r0[ i ] - a1[ i ] + w*r0[ i ]; } /* Convert position vector to Fricke system. */ for( i = 0; i < 6; i++ ) { w = 0.0; for( j = 0; j < 3; j++ ) { w += em[ i ][ j ]*v1[ j ]; } v2[ i ] = w; } /* Allow for fictitious proper motion in FK4. */ w = ( palEpj( palEpb2d( bepoch ) ) - 2000.0 )/PAL__PMF; for( i = 0; i < 3; i++ ) { v2[ i ] += w*v2[ i + 3 ]; } /* Revert to spherical coordinates. */ eraC2s( v2, &w, d2000 ); *r2000 = eraAnp( w ); } pal-0.5.0/palFk524.c000644 000765 000024 00000021010 12366000607 014024 0ustar00timjstaff000000 000000 /* *+ * Name: * palFk524 * Purpose: * Convert J2000.0 FK5 star data to B1950.0 FK4. * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * palFk524( double r2000, double d2000, double dr2000, double dd2000, * double p2000, double v2000, double *r1950, double *d1950, * double *dr1950, double *dd1950, double *p1950, double *v1950 ) * Arguments: * r2000 = double (Given) * J2000.0 FK5 RA (radians). * d2000 = double (Given) * J2000.0 FK5 Dec (radians). * dr2000 = double (Given) * J2000.0 FK5 RA proper motion (rad/Jul.yr) * dd2000 = double (Given) * J2000.0 FK5 Dec proper motion (rad/Jul.yr) * p2000 = double (Given) * J2000.0 FK5 parallax (arcsec) * v2000 = double (Given) * J2000.0 FK5 radial velocity (km/s, +ve = moving away) * r1950 = double * (Returned) * B1950.0 FK4 RA (radians). * d1950 = double * (Returned) * B1950.0 FK4 Dec (radians). * dr1950 = double * (Returned) * B1950.0 FK4 RA proper motion (rad/Jul.yr) * dd1950 = double * (Returned) * B1950.0 FK4 Dec proper motion (rad/Jul.yr) * p1950 = double * (Returned) * B1950.0 FK4 parallax (arcsec) * v1950 = double * (Returned) * B1950.0 FK4 radial velocity (km/s, +ve = moving away) * Description: * This function converts stars from the IAU 1976, FK5, Fricke * system, to the Bessel-Newcomb, FK4 system. The precepts * of Smith et al (Ref 1) are followed, using the implementation * by Yallop et al (Ref 2) of a matrix method due to Standish. * Kinoshita's development of Andoyer's post-Newcomb precession is * used. The numerical constants from Seidelmann et al (Ref 3) are * used canonically. * Notes: * - The proper motions in RA are dRA/dt rather than * cos(Dec)*dRA/dt, and are per year rather than per century. * - Note that conversion from Julian epoch 2000.0 to Besselian * epoch 1950.0 only is provided for. Conversions involving * other epochs will require use of the appropriate precession, * proper motion, and E-terms routines before and/or after * FK524 is called. * - In the FK4 catalogue the proper motions of stars within * 10 degrees of the poles do not embody the differential * E-term effect and should, strictly speaking, be handled * in a different manner from stars outside these regions. * However, given the general lack of homogeneity of the star * data available for routine astrometry, the difficulties of * handling positions that may have been determined from * astrometric fields spanning the polar and non-polar regions, * the likelihood that the differential E-terms effect was not * taken into account when allowing for proper motion in past * astrometry, and the undesirability of a discontinuity in * the algorithm, the decision has been made in this routine to * include the effect of differential E-terms on the proper * motions for all stars, whether polar or not. At epoch 2000, * and measuring on the sky rather than in terms of dRA, the * errors resulting from this simplification are less than * 1 milliarcsecond in position and 1 milliarcsecond per * century in proper motion. * * References: * - Smith, C.A. et al, 1989. "The transformation of astrometric * catalog systems to the equinox J2000.0". Astron.J. 97, 265. * - Yallop, B.D. et al, 1989. "Transformation of mean star places * from FK4 B1950.0 to FK5 J2000.0 using matrices in 6-space". * Astron.J. 97, 274. * - Seidelmann, P.K. (ed), 1992. "Explanatory Supplement to * the Astronomical Almanac", ISBN 0-935702-68-7. * Authors: * PTW: Pat Wallace (STFC) * DSB: David Berry (JAC, Hawaii) * {enter_new_authors_here} * History: * 2012-02-13 (DSB): * Initial version with documentation taken from Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1995 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "palmac.h" #include "math.h" void palFk524( double r2000, double d2000, double dr2000, double dd2000, double p2000, double v2000, double *r1950, double *d1950, double *dr1950, double *dd1950, double *p1950, double *v1950 ){ /* Local Variables; */ double r, d, ur, ud, px, rv; double sr, cr, sd, cd, x, y, z, w; double v1[ 6 ], v2[ 6 ]; double xd, yd, zd; double rxyz, wd, rxysq, rxy; int i, j; /* Small number to avoid arithmetic problems. */ static const double tiny = 1.0-30; /* Canonical constants (see references). Constant vector and matrix. */ double a[ 6 ] = { -1.62557E-6, -0.31919E-6, -0.13843E-6, +1.245E-3, -1.580E-3, -0.659E-3 }; double emi[ 6 ][ 6 ] = { { 0.9999256795, 0.0111814828, 0.0048590039, -0.00000242389840, -0.00000002710544, -0.00000001177742}, {-0.0111814828, 0.9999374849, -0.0000271771, 0.00000002710544, -0.00000242392702, 0.00000000006585 }, {-0.0048590040, -0.0000271557, 0.9999881946, 0.00000001177742, 0.00000000006585, -0.00000242404995 }, {-0.000551, 0.238509, -0.435614, 0.99990432, 0.01118145, 0.00485852 }, {-0.238560, -0.002667, 0.012254, -0.01118145, 0.99991613, -0.00002717}, { 0.435730, -0.008541, 0.002117, -0.00485852, -0.00002716, 0.99996684 } }; /* Pick up J2000 data (units radians and arcsec/JC). */ r = r2000; d = d2000; ur = dr2000*PAL__PMF; ud = dd2000*PAL__PMF; px = p2000; rv = v2000; /* Spherical to Cartesian. */ sr = sin( r ); cr = cos( r ); sd = sin( d ); cd = cos( d ); x = cr*cd; y = sr*cd; z = sd; w = PAL__VF*rv*px; v1[ 0 ] = x; v1[ 1 ] = y; v1[ 2 ] = z; v1[ 3 ] = -ur*y - cr*sd*ud + w*x; v1[ 4 ] = ur*x - sr*sd*ud + w*y; v1[ 5 ] = cd*ud + w*z; /* Convert position+velocity vector to BN system. */ for( i = 0; i < 6; i++ ) { w = 0.0; for( j = 0; j < 6; j++ ) { w += emi[ i ][ j ]*v1[ j ]; } v2[ i ] = w; } /* Position vector components and magnitude. */ x = v2[ 0 ]; y = v2[ 1 ]; z = v2[ 2 ]; rxyz = sqrt( x*x + y*y + z*z ); /* Apply E-terms to position. */ w = x*a[ 0 ] + y*a[ 1 ] + z*a[ 2 ]; x += a[ 0 ]*rxyz - w*x; y += a[ 1 ]*rxyz - w*y; z += a[ 2 ]*rxyz - w*z; /* Recompute magnitude. */ rxyz = sqrt( x*x + y*y + z*z ); /* Apply E-terms to both position and velocity. */ x = v2[ 0 ]; y = v2[ 1 ]; z = v2[ 2 ]; w = x*a[ 0 ] + y*a[ 1 ] + z*a[ 2 ]; wd = x*a[ 3 ] + y*a[ 4 ] + z*a[ 5 ]; x += a[ 0 ]*rxyz - w*x; y += a[ 1 ]*rxyz - w*y; z += a[ 2 ]*rxyz - w*z; xd = v2[ 3 ] + a[ 3 ]*rxyz - wd*x; yd = v2[ 4 ] + a[ 4 ]*rxyz - wd*y; zd = v2[ 5 ] + a[ 5 ]*rxyz - wd*z; /* Convert to spherical. */ rxysq = x*x + y*y; rxy = sqrt( rxysq ); if( x == 0.0 && y == 0.0 ) { r = 0.0; } else { r = atan2( y, x ); if( r < 0.0 ) r += PAL__D2PI; } d = atan2( z, rxy ); if( rxy > tiny ) { ur = ( x*yd - y*xd )/rxysq; ud = ( zd*rxysq - z*( x*xd + y*yd ) )/( ( rxysq + z*z )*rxy ); } /* Radial velocity and parallax. */ if( px > tiny ) { rv = ( x*xd + y*yd + z*zd )/( px*PAL__VF*rxyz ); px /= rxyz; } /* Return results. */ *r1950 = r; *d1950 = d; *dr1950 = ur/PAL__PMF; *dd1950 = ud/PAL__PMF; *p1950 = px; *v1950 = rv; } pal-0.5.0/palFk54z.c000644 000765 000024 00000007273 12366000611 014146 0ustar00timjstaff000000 000000 /* *+ * Name: * palFk54z * Purpose: * Convert a J2000.0 FK5 star position to B1950.0 FK4 assuming * zero proper motion and parallax. * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * palFk54z( double r2000, double d2000, double bepoch, double *r1950, * double *d1950, double *dr1950, double *dd1950 ) * Arguments: * r2000 = double (Given) * J2000.0 FK5 RA (radians). * d2000 = double (Given) * J2000.0 FK5 Dec (radians). * bepoch = double (Given) * Besselian epoch (e.g. 1950.0). * r1950 = double * (Returned) * B1950 FK4 RA (radians) at epoch "bepoch". * d1950 = double * (Returned) * B1950 FK4 Dec (radians) at epoch "bepoch". * dr1950 = double * (Returned) * B1950 FK4 proper motion (RA) (radians/trop.yr)). * dr1950 = double * (Returned) * B1950 FK4 proper motion (Dec) (radians/trop.yr)). * Description: * This function converts star positions from the IAU 1976, * FK5, Fricke system to the Bessel-Newcomb, FK4 system. * Notes: * - The proper motion in RA is dRA/dt rather than cos(Dec)*dRA/dt. * - Conversion from Julian epoch 2000.0 to Besselian epoch 1950.0 * only is provided for. Conversions involving other epochs will * require use of the appropriate precession functions before and * after this function is called. * - The FK5 proper motions, the parallax and the radial velocity * are presumed zero. * - It is the intention that FK5 should be a close approximation * to an inertial frame, so that distant objects have zero proper * motion; such objects have (in general) non-zero proper motion * in FK4, and this function returns those fictitious proper * motions. * - The position returned by this function is in the B1950 * reference frame but at Besselian epoch BEPOCH. For comparison * with catalogues the "bepoch" argument will frequently be 1950.0. * Authors: * PTW: Pat Wallace (STFC) * DSB: David Berry (JAC, Hawaii) * {enter_new_authors_here} * History: * 2012-02-13 (DSB): * Initial version with documentation taken from Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1995 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "pal1sofa.h" void palFk54z( double r2000, double d2000, double bepoch, double *r1950, double *d1950, double *dr1950, double *dd1950 ){ /* Local Variables: */ double r, d, px, rv, y; /* FK5 equinox J2000 (any epoch) to FK4 equinox B1950 epoch B1950. */ palFk524( r2000, d2000, 0.0, 0.0, 0.0, 0.0, &r, &d, dr1950, dd1950, &px, &rv ); /* Fictitious proper motion to epoch "bepoch". */ y = bepoch - 1950.0; *r1950 = r + *dr1950*y; *d1950 = d + *dd1950*y; } pal-0.5.0/palGaleq.c000644 000765 000024 00000006152 12366000611 014267 0ustar00timjstaff000000 000000 /* *+ * Name: * palGaleq * Purpose: * Convert from galactic to J2000.0 equatorial coordinates * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palGaleq ( double dl, double db, double *dr, double *dd ); * Arguments: * dl = double (Given) * Galactic longitude (radians). * db = double (Given) * Galactic latitude (radians). * dr = double * (Returned) * J2000.0 RA (radians) * dd = double * (Returned) * J2000.0 Dec (radians) * Description: * Transformation from IAU 1958 galactic coordinates to * J2000.0 equatorial coordinates. * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * The equatorial coordinates are J2000.0. Use the routine * palGe50 if conversion to B1950.0 'FK4' coordinates is * required. * See Also: * Blaauw et al, Mon.Not.R.Astron.Soc.,121,123 (1960) * History: * 2012-02-12(TIMJ): * Initial version with documentation taken from Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1998 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "pal1sofa.h" void palGaleq ( double dl, double db, double *dr, double *dd ) { double v1[3]; double v2[3]; /* * L2,B2 system of galactic coordinates * * P = 192.25 RA of galactic north pole (mean B1950.0) * Q = 62.6 inclination of galactic to mean B1950.0 equator * R = 33 longitude of ascending node * * P,Q,R are degrees * * Equatorial to galactic rotation matrix (J2000.0), obtained by * applying the standard FK4 to FK5 transformation, for zero proper * motion in FK5, to the columns of the B1950 equatorial to * galactic rotation matrix: */ double rmat[3][3] = { { -0.054875539726,-0.873437108010,-0.483834985808 }, { +0.494109453312,-0.444829589425,+0.746982251810 }, { -0.867666135858,-0.198076386122,+0.455983795705 } }; /* Spherical to Cartesian */ eraS2c( dl, db, v1 ); /* Galactic to equatorial */ eraTrxp( rmat, v1, v2 ); /* Cartesian to spherical */ eraC2s( v2, dr, dd ); /* Express in conventional ranges */ *dr = eraAnp( *dr ); *dd = eraAnpm( *dd ); } pal-0.5.0/palGalsup.c000644 000765 000024 00000006122 12366000611 014466 0ustar00timjstaff000000 000000 /* *+ * Name: * palGalsup * Purpose: * Convert from galactic to supergalactic coordinates * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palGalsup ( double dl, double db, double *dsl, double *dsb ); * Arguments: * dl = double (Given) * Galactic longitude. * db = double (Given) * Galactic latitude. * dsl = double * (Returned) * Supergalactic longitude. * dsb = double * (Returned) * Supergalactic latitude. * Description: * Transformation from IAU 1958 galactic coordinates to * de Vaucouleurs supergalactic coordinates. * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * See Also: * - de Vaucouleurs, de Vaucouleurs, & Corwin, Second Reference * Catalogue of Bright Galaxies, U. Texas, page 8. * - Systems & Applied Sciences Corp., Documentation for the * machine-readable version of the above catalogue, * Contract NAS 5-26490. * * (These two references give different values for the galactic * longitude of the supergalactic origin. Both are wrong; the * correct value is L2=137.37.) * History: * 2012-02-12(TIMJ): * Initial version with documentation taken from Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1999 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "pal1sofa.h" void palGalsup ( double dl, double db, double *dsl, double *dsb ) { double v1[3]; double v2[3]; /* * System of supergalactic coordinates: * * SGL SGB L2 B2 (deg) * - +90 47.37 +6.32 * 0 0 - 0 * * Galactic to supergalactic rotation matrix: */ double rmat[3][3] = { { -0.735742574804,+0.677261296414,+0.000000000000 }, { -0.074553778365,-0.080991471307,+0.993922590400 }, { +0.673145302109,+0.731271165817,+0.110081262225 } }; /* Spherical to Cartesian */ eraS2c( dl, db, v1 ); /* Galactic to Supergalactic */ eraRxp( rmat, v1, v2 ); /* Cartesian to spherical */ eraC2s( v2, dsl, dsb ); /* Express in conventional ranges */ *dsl = eraAnp( *dsl ); *dsb = eraAnpm( *dsb ); } pal-0.5.0/palGe50.c000644 000765 000024 00000006400 12366000611 013732 0ustar00timjstaff000000 000000 /* *+ * Name: * palGe50 * Purpose: * Transform Galactic Coordinate to B1950 FK4 * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * palGe50( double dl, double db, double *dr, double *dd ); * Arguments: * dl = double (Given) * Galactic longitude (radians) * db = double (Given) * Galactic latitude (radians) * dr = double * (Returned) * B9150.0 FK4 RA. * dd = double * (Returned) * B1950.0 FK4 Dec. * Description: * Transformation from IAU 1958 galactic coordinates to * B1950.0 'FK4' equatorial coordinates. * Authors: * PTW: Patrick T. Wallace * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - The equatorial coordinates are B1950.0 'FK4'. Use the routine * palGaleq if conversion to J2000.0 coordinates is required. * See Also: * - Blaauw et al, Mon.Not.R.Astron.Soc.,121,123 (1960) * History: * 2012-03-23 (TIMJ): * Initial version * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1995 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "pal1sofa.h" void palGe50 ( double dl, double db, double * dr, double * dd ) { /* * L2,B2 system of galactic coordinates * * P = 192.25 RA of galactic north pole (mean B1950.0) * Q = 62.6 inclination of galactic to mean B1950.0 equator * R = 33 longitude of ascending node * * P,Q,R are degrees * * * Equatorial to galactic rotation matrix * * The Euler angles are P, Q, 90-R, about the z then y then * z axes. * * +CP.CQ.SR-SP.CR +SP.CQ.SR+CP.CR -SQ.SR * * -CP.CQ.CR-SP.SR -SP.CQ.CR+CP.SR +SQ.CR * * +CP.SQ +SP.SQ +CQ * */ double rmat[3][3] = { { -0.066988739415,-0.872755765852,-0.483538914632 }, { +0.492728466075,-0.450346958020,+0.744584633283 }, { -0.867600811151,-0.188374601723,+0.460199784784 } }; double v1[3], v2[3], r, d, re, de; /* Spherical to cartesian */ eraS2c( dl, db, v1 ); /* Rotate to mean B1950.0 */ eraTrxp( rmat, v1, v2 ); /* Cartesian to spherical */ eraC2s( v2, &r, &d ); /* Introduce E-terms */ palAddet( r, d, 1950.0, &re, &de ); /* Express in conventional ranges */ *dr = eraAnp( re ); *dd = eraAnpm( de ); } pal-0.5.0/palGeoc.c000644 000765 000024 00000004406 12366000713 014116 0ustar00timjstaff000000 000000 /* *+ * Name: * palGeoc * Purpose: * Convert geodetic position to geocentric * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palGeoc( double p, double h, double * r, double *z ); * Arguments: * p = double (Given) * latitude (radians) * h = double (Given) * height above reference spheroid (geodetic, metres) * r = double * (Returned) * distance from Earth axis (AU) * z = double * (Returned) * distance from plane of Earth equator (AU) * Description: * Convert geodetic position to geocentric. * Authors: * PTW: Patrick T. Wallace * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - Geocentric latitude can be obtained by evaluating atan2(z,r) * - Uses WGS84 reference ellipsoid and calls eraGd2gc * History: * 2012-03-01 (TIMJ): * Initial version moved from palOne2One * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2004 Patrick T. Wallace * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "pal1sofa.h" void palGeoc ( double p, double h, double *r, double *z ) { double xyz[3]; const double elong = 0.0; /* Use zero longitude */ const double AU = 1.49597870E11; /* WGS84 looks to be the closest match */ eraGd2gc( ERFA_WGS84, elong, p, h, xyz ); *r = xyz[0] / (AU * cos(elong) ); *z = xyz[2] / AU; } pal-0.5.0/palIntin.c000644 000765 000024 00000011651 12366000607 014324 0ustar00timjstaff000000 000000 /* *+ * Name: * palIntin * Purpose: * Convert free-format input into an integer * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palIntin( const char * string, int *nstrt, * long *ireslt, int *jflag ); * Arguments: * string = const char * (Given) * String containing number to be decoded. * nstrt = int * (Given and Returned) * Character number indicating where decoding should start. * On output its value is updated to be the location of the * possible next value. For compatibility with SLA the first * character is index 1. * ireslt = long * (Returned) * Result. Not updated when jflag=1. * jflag = int * (Returned) * status: -1 = -OK, 0 = +OK, 1 = null, 2 = error * Description: * Extracts a number from an input string starting at the specified * index. * Authors: * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - Uses the strtol() system call to do the parsing. This may lead to * subtle differences when compared to the SLA/F parsing. * - Commas are recognized as a special case and are skipped if one happens * to be the next character when updating nstrt. Additionally the output * nstrt position will skip past any trailing space. * - If no number can be found flag will be set to 1. * - If the number overflows or underflows jflag will be set to 2. For overflow * the returned result will have the value LONG_MAX, for underflow it * will have the value LONG_MIN. * History: * 2012-03-15 (TIMJ): * Initial version * Matches the SLALIB interface but brand new implementation using * C library calls and not a direct port of the Fortran. * {enter_further_changes_here} * Copyright: * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ /* Shenanigans for isblank() which is C99 only */ #define _POSIX_C_SOURCE 200112L #define _ISOC99_SOURCE #include #include #include #include "pal.h" void palIntin( const char * string, int *nstrt, long *ireslt, int *jflag ) { const char *strstart = NULL; /* Pointer to start of search */ const char * ctemp = NULL; /* Pointer into string */ char * endptr = NULL;/* Pointer to string after number */ int retval; /* Return value from strtol */ int hasminus; /* is this a -0 */ /* strtol man page indicates that we should reset errno before calling strtod */ errno = 0; /* Locate the start postion */ strstart = &(string[*nstrt-1]); /* We have to be able to deal with -0 so we have to search the string first and look for the negative */ hasminus = 0; ctemp = strstart; while ( ctemp != '\0' ) { if (isdigit(*ctemp)) break; /* Reset so that - 12345 is not a negative number */ hasminus = 0; /* Flag that we have found a minus */ if (*ctemp == '-') hasminus = 1; ctemp++; } /* Look for the number using the system call, offsetting using 1-based counter. */ retval = strtol( strstart, &endptr, 10 ); if (retval == 0.0 && endptr == strstart) { /* conversion did not find anything */ *jflag = 1; /* but SLA compatibility requires that we step through to remove leading spaces. We also step through alphabetic characters since they can never be numbers. Skip past a "+" since it doesn't gain us anything and matches slalib. */ while (isblank(*endptr) || isalpha(*endptr) || *endptr == '+' ) { endptr++; } } else if ( errno == ERANGE ) { *jflag = 2; } else { if ( retval < 0 || hasminus ) { *jflag = -1; } else { *jflag = 0; } } /* Sort out the position for the next index */ *nstrt = endptr - string + 1; /* Skip a comma */ if (*endptr == ',') { (*nstrt)++; } else { /* jump past any leading spaces for the next part of the string */ ctemp = endptr; while ( isblank(*ctemp) ) { (*nstrt)++; ctemp++; } } /* And the result unless we found nothing */ if (*jflag != 1) *ireslt = retval; } pal-0.5.0/palmac.h000644 000765 000024 00000010302 12366000611 013773 0ustar00timjstaff000000 000000 #ifndef PALMACDEF #define PALMACDEF /* *+ * Name: * palmac.h * Purpose: * Macros used by the PAL library * Language: * Starlink ANSI C * Type of Module: * Include file * Description: * A collection of useful macros provided and used by the PAL library * Authors: * TIMJ: Tim Jenness (JAC, Hawaii) * DSB: David Berry (JAC, Hawaii) * {enter_new_authors_here} * Notes: * * History: * 2012-02-08 (TIMJ): * Initial version. * Adapted with permission from the Fortran SLALIB library. * 2012-04-13 (DSB): * Added PAL__DR2H and PAL__DR2S * {enter_further_changes_here} * Copyright: * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, MA 02110-1301 * USA. * Bugs: * {note_any_bugs_here} *- */ /* Pi */ static const double PAL__DPI = 3.1415926535897932384626433832795028841971693993751; /* 2Pi */ static const double PAL__D2PI = 6.2831853071795864769252867665590057683943387987502; /* pi/2: 90 degrees in radians */ static const double PAL__DPIBY2 = 1.5707963267948966192313216916397514420985846996876; /* pi/180: degrees to radians */ static const double PAL__DD2R = 0.017453292519943295769236907684886127134428718885417; /* Radians to arcseconds */ static const double PAL__DR2AS = 2.0626480624709635515647335733077861319665970087963e5; /* Arcseconds to radians */ static const double PAL__DAS2R = 4.8481368110953599358991410235794797595635330237270e-6; /* Radians to degrees */ static const double PAL__DR2D = 57.295779513082320876798154814105170332405472466564; /* Hours to radians */ static const double PAL__DH2R = 0.26179938779914943653855361527329190701643078328126; /* Radians to hours */ static const double PAL__DR2H = 3.8197186342054880584532103209403446888270314977709; /* Radians to seconds of time */ static const double PAL__DR2S = 1.3750987083139757010431557155385240879777313391975e4; /* Seconds of time to radians */ static const double PAL__DS2R = 7.272205216643039903848712e-5; /* Start of SLA modified Julian date epoch */ static const double PAL__MJD0 = 2400000.5; /* Light time for 1 AU (sec) */ static const double PAL__CR = 499.004782; /* Seconds per day */ static const double PAL__SPD = 86400.0; /* Km per sec to AU per tropical century = 86400 * 36524.2198782 / 149597870 */ static const double PAL__VF = 21.095; /* Radians per year to arcsec per century. This needs to be a macro since it is an expression including other constants. */ #define PAL__PMF (100.0*60.0*60.0*360.0/PAL__D2PI); /* Mean sidereal rate - the rotational angular velocity of Earth in radians/sec from IERS Conventions (2003). */ static const double PAL__SR = 7.2921150e-5; /* Gaussian gravitational constant (exact) */ static const double PAL__GCON = 0.01720209895; /* DINR(A) - truncate to nearest whole number towards zero (double) */ #define DINT(A) ((A)<0.0?ceil(A):floor(A)) /* DNINT(A) - round to nearest whole number (double) */ #define DNINT(A) ((A)<0.0?ceil((A)-0.5):floor((A)+0.5)) /* DMAX(A,B) - return maximum value - evaluates arguments multiple times */ #define DMAX(A,B) ((A) > (B) ? (A) : (B) ) /* DMIN(A,B) - return minimum value - evaluates arguments multiple times */ #define DMIN(A,B) ((A) < (B) ? (A) : (B) ) /* We actually prefer to use C99 copysign() but we define this here as a backup but it will not detect -0.0 so is not useful for palDfltin. */ /* DSIGN(A,B) - magnitude of A with sign of B (double) */ #define DSIGN(A,B) ((B)<0.0?-fabs(A):fabs(A)) #endif pal-0.5.0/palMap.c000644 000765 000024 00000010227 12366001307 013754 0ustar00timjstaff000000 000000 /* *+ * Name: * palMap * Purpose: * Convert star RA,Dec from mean place to geocentric apparent * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palMap( double rm, double dm, double pr, double pd, * double px, double rv, double eq, double date, * double *ra, double *da ); * Arguments: * rm = double (Given) * Mean RA (radians) * dm = double (Given) * Mean declination (radians) * pr = double (Given) * RA proper motion, changes per Julian year (radians) * pd = double (Given) * Dec proper motion, changes per Julian year (radians) * px = double (Given) * Parallax (arcsec) * rv = double (Given) * Radial velocity (km/s, +ve if receding) * eq = double (Given) * Epoch and equinox of star data (Julian) * date = double (Given) * TDB for apparent place (JD-2400000.5) * ra = double * (Returned) * Apparent RA (radians) * dec = double * (Returned) * Apparent dec (radians) * Description: * Convert star RA,Dec from mean place to geocentric apparent. * Authors: * PTW: Patrick T. Wallace * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - Calls palMappa and palMapqk * - The reference systems and timescales used are IAU 2006. * - EQ is the Julian epoch specifying both the reference frame and * the epoch of the position - usually 2000. For positions where * the epoch and equinox are different, use the routine palPm to * apply proper motion corrections before using this routine. * * - The distinction between the required TDB and TT is always * negligible. Moreover, for all but the most critical * applications UTC is adequate. * * - The proper motions in RA are dRA/dt rather than cos(Dec)*dRA/dt. * * - This routine may be wasteful for some applications because it * recomputes the Earth position/velocity and the precession- * nutation matrix each time, and because it allows for parallax * and proper motion. Where multiple transformations are to be * carried out for one epoch, a faster method is to call the * palMappa routine once and then either the palMapqk routine * (which includes parallax and proper motion) or palMapqkz (which * assumes zero parallax and proper motion). * * - The accuracy is sub-milliarcsecond, limited by the * precession-nutation model (see palPrenut for details). * * - The accuracy is further limited by the routine palEvp, called * by palMappa, which computes the Earth position and velocity. * See eraEpv00 for details on that calculation. * History: * 2012-03-01 (TIMJ): * Initial version * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2001 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, MA 02110-1301 * USA. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" void palMap( double rm, double dm, double pr, double pd, double px, double rv, double eq, double date, double *ra, double *da ) { double amprms[21]; /* Star independent parameters */ palMappa( eq, date, amprms ); /* Mean to apparent */ palMapqk( rm, dm, pr, pd, px, rv, amprms, ra, da ); } pal-0.5.0/palMappa.c000644 000765 000024 00000007575 12366000611 014306 0ustar00timjstaff000000 000000 /* *+ * Name: * palMappa * Purpose: * Compute parameters needed by palAmpqk and palMapqk. * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palMappa( double eq, double date, double amprms[21] ) * Arguments: * eq = double (Given) * epoch of mean equinox to be used (Julian) * date = double (Given) * TDB (JD-2400000.5) * amprms = double[21] (Returned) * star-independent mean-to-apparent parameters: * - (0) time interval for proper motion (Julian years) * - (1-3) barycentric position of the Earth (AU) * - (4-6) heliocentric direction of the Earth (unit vector) * - (7) (grav rad Sun)*2/(Sun-Earth distance) * - (8-10) abv: barycentric Earth velocity in units of c * - (11) sqrt(1-v**2) where v=modulus(abv) * - (12-20) precession/nutation (3,3) matrix * Description: * Compute star-independent parameters in preparation for * transformations between mean place and geocentric apparent place. * * The parameters produced by this function are required in the * parallax, aberration, and nutation/bias/precession parts of the * mean/apparent transformations. * * The reference systems and timescales used are IAU 2006. * Notes: * - For date, the distinction between the required TDB and TT * is always negligible. Moreover, for all but the most * critical applications UTC is adequate. * - The vector amprms(1-3) is referred to the mean equinox and * equator of epoch eq. * - The parameters amprms produced by this function are used by * palAmpqk, palMapqk and palMapqkz. * Authors: * PTW: Pat Wallace (STFC) * {enter_new_authors_here} * History: * 2012-02-13 (PTW): * Initial version. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2003 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "palmac.h" #include "pal1sofa.h" #include void palMappa( double eq, double date, double amprms[21] ){ /* Local constants */ /* Gravitational radius of the Sun x 2 (2*mu/c**2, AU) */ const double GR2 = 2.0 * 9.87063e-9; /* Local Variables; */ int i; double ebd[ 3 ], ehd[ 3 ], eh[ 3 ], e, vn[ 3 ], vm; /* Initialise so that unsused values are returned holding zero */ memset( amprms, 0, 21*sizeof( *amprms ) ); /* Time interval for proper motion correction. */ amprms[ 0 ] = eraEpj( PAL__MJD0, date ) - eq; /* Get Earth barycentric and heliocentric position and velocity. */ palEvp( date, eq, ebd, &rms[ 1 ], ehd, eh ); /* Heliocentric direction of Earth (normalized) and modulus. */ eraPn( eh, &e, &rms[ 4 ] ); /* Light deflection parameter */ amprms[7] = GR2 / e; /* Aberration parameters. */ for( i = 0; i < 3; i++ ) { amprms[ i + 8 ] = ebd[ i ]*PAL__CR; } eraPn( &rms[8], &vm, vn ); amprms[ 11 ] = sqrt( 1.0 - vm*vm ); /* NPB matrix. */ palPrenut( eq, date, (double(*)[ 3 ]) &rms[ 12 ] ); } pal-0.5.0/palMapqk.c000644 000765 000024 00000011151 12366000611 014302 0ustar00timjstaff000000 000000 /* *+ * Name: * palMapqk * Purpose: * Quick mean to apparent place * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palMapqk ( double rm, double dm, double pr, double pd, * double px, double rv, double amprms[21], * double *ra, double *da ); * Arguments: * rm = double (Given) * Mean RA (radians) * dm = double (Given) * Mean declination (radians) * pr = double (Given) * RA proper motion, changes per Julian year (radians) * pd = double (Given) * Dec proper motion, changes per Julian year (radians) * px = double (Given) * Parallax (arcsec) * rv = double (Given) * Radial velocity (km/s, +ve if receding) * amprms = double [21] (Given) * Star-independent mean-to-apparent parameters (see palMappa). * ra = double * (Returned) * Apparent RA (radians) * dec = double * (Returned) * Apparent dec (radians) * Description: * Quick mean to apparent place: transform a star RA,Dec from * mean place to geocentric apparent place, given the * star-independent parameters. * * Use of this routine is appropriate when efficiency is important * and where many star positions, all referred to the same equator * and equinox, are to be transformed for one epoch. The * star-independent parameters can be obtained by calling the * palMappa routine. * * If the parallax and proper motions are zero the palMapqkz * routine can be used instead. * Authors: * PTW: Patrick T. Wallace * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - The reference frames and timescales used are post IAU 2006. * History: * 2012-03-01 (TIMJ): * Initial version with documentation from SLA/F * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2000 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "palmac.h" #include "pal1sofa.h" void palMapqk ( double rm, double dm, double pr, double pd, double px, double rv, double amprms[21], double *ra, double *da ) { /* local constants */ const double VF = 0.21094502; /* Km/s to AU/year */ /* Local Variables: */ int i; double ab1, abv[3], p[3], w, p1dv, p2[3], p3[3]; double pmt, gr2e, eb[3], q[3], pxr, em[3]; double pde, pdep1, p1[3], ehn[3], pn[3]; /* Unpack scalar and vector parameters. */ pmt = amprms[0]; gr2e = amprms[7]; ab1 = amprms[11]; for( i = 0; i < 3; i++ ) { eb[i] = amprms[i+1]; ehn[i] = amprms[i+4]; abv[i] = amprms[i+8]; } /* Spherical to x,y,z. */ eraS2c( rm, dm, q); /* Space motion (radians per year) */ pxr = px * PAL__DAS2R; w = VF * rv * pxr; em[0] = -pr * q[1] - pd * cos(rm) * sin(dm) + w * q[0]; em[1] = pr * q[0] - pd * sin(rm) * sin(dm) + w * q[1]; em[2] = pd * cos(dm) + w * q[2]; /* Geocentric direction of star (normalised) */ for( i = 0; i < 3; i++ ) { p[i] = q[i] + pmt * em[i] - pxr * eb[i]; } eraPn( p, &w, pn ); /* Light deflection (restrained within the Sun's disc) */ pde = eraPdp( pn, ehn ); pdep1 = pde + 1.0; w = gr2e / ( pdep1 > 1.0e-5 ? pdep1 : 1.0e-5 ); for( i = 0; i < 3; i++) { p1[i] = pn[i] + w * ( ehn[i] - pde * pn[i] ); } /* Aberration (normalisation omitted). */ p1dv = eraPdp( p, abv ); w = 1.0 + p1dv / ( ab1 + 1.0 ); for( i = 0; i < 3; i++ ) { p2[i] = ( ab1 * p1[i] ) + ( w * abv[i] ); } /* Precession and nutation. */ eraRxp( (double(*)[3]) &rms[12], p2, p3 ); /* Geocentric apparent RA,dec. */ eraC2s( p3, ra, da ); *ra = eraAnp( *ra ); } pal-0.5.0/palMapqkz.c000644 000765 000024 00000007232 12366000611 014501 0ustar00timjstaff000000 000000 /* *+ * Name: * palMapqkz * Purpose: * Quick mean to apparent place. * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palMapqkz( double rm, double dm, double amprms[21], * double *ra, double *da ) * Arguments: * rm = double (Given) * Mean RA (radians). * dm = double (Given) * Mean Dec (radians). * amprms = double[21] (Given) * Star-independent mean-to-apparent parameters (see palMappa): * (0-3) not used * (4-6) not used * (7) not used * (8-10) abv: barycentric Earth velocity in units of c * (11) sqrt(1-v**2) where v=modulus(abv) * (12-20) precession/nutation (3,3) matrix * ra = double * (Returned) * Apparent RA (radians). * da = double * (Returned) * Apparent Dec (radians). * Description: * Quick mean to apparent place: transform a star RA,dec from * mean place to geocentric apparent place, given the * star-independent parameters, and assuming zero parallax * and proper motion. * * Use of this function is appropriate when efficiency is important * and where many star positions, all with parallax and proper * motion either zero or already allowed for, and all referred to * the same equator and equinox, are to be transformed for one * epoch. The star-independent parameters can be obtained by * calling the palMappa function. * * The corresponding function for the case of non-zero parallax * and proper motion is palMapqk. * * The reference systems and timescales used are IAU 2006. * * Strictly speaking, the function is not valid for solar-system * sources, though the error will usually be extremely small. * Authors: * PTW: Pat Wallace (STFC) * {enter_new_authors_here} * History: * 2012-02-13 (PTW): * Initial version. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1999 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "pal1sofa.h" void palMapqkz ( double rm, double dm, double amprms[21], double *ra, double *da ){ /* Local Variables: */ int i; double ab1, abv[3], p[3], w, p1dv, p1dvp1, p2[3], p3[3]; /* Unpack scalar and vector parameters. */ ab1 = amprms[11]; for( i = 0; i < 3; i++ ) { abv[i] = amprms[i+8]; } /* Spherical to x,y,z. */ eraS2c( rm, dm, p ); /* Aberration. */ p1dv = eraPdp( p, abv ); p1dvp1 = p1dv + 1.0; w = 1.0 + p1dv / ( ab1 + 1.0 ); for( i = 0; i < 3; i++ ) { p2[i] = ( ( ab1 * p[i] ) + ( w * abv[i] ) ) / p1dvp1; } /* Precession and nutation. */ eraRxp( (double(*)[3]) &rms[12], p2, p3 ); /* Geocentric apparent RA,dec. */ eraC2s( p3, ra, da ); *ra = eraAnp( *ra ); } pal-0.5.0/palNut.c000644 000765 000024 00000004561 12366000611 014006 0ustar00timjstaff000000 000000 /* *+ * Name: * palNut * Purpose: * Form the matrix of nutation * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palNut( double date, double rmatn[3][3] ); * Arguments: * date = double (Given) * TT as modified Julian date (JD-2400000.5) * rmatn = double [3][3] (Returned) * Nutation matrix in the sense v(true)=rmatn * v(mean) * where v(true) is the star vector relative to the * true equator and equinox of date and v(mean) is the * star vector relative to the mean equator and equinox * of date. * Description: * Form the matrix of nutation for a given date using * the IAU 2006 nutation model and palDeuler. * Authors: * PTW: Patrick T. Wallace * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - Uses eraNut06a via palNutc * - The distinction between TDB and TT is negligible. For all but * the most critical applications UTC is adequate. * History: * 2012-03-07 (TIMJ): * Initial version * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2005 Patrick T. Wallace * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include void palNut( double date, double rmatn[3][3]) { double dpsi, deps, eps0; /* Nutation component and mean obliquity */ palNutc( date, &dpsi, &deps, &eps0 ); /* Rotation matrix */ palDeuler( "XZX", eps0, -dpsi, -(eps0+deps), rmatn ); } pal-0.5.0/palNutc.c000644 000765 000024 00000004326 12366001330 014147 0ustar00timjstaff000000 000000 /* *+ * Name: * palNutc * Purpose: * Calculate nutation longitude & obliquoty components * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palNutc( double date, double * dpsi, double *deps, double *eps0 ); * Arguments: * date = double (Given) * TT as modified Julian date (JD-2400000.5) * dpsi = double * (Returned) * Nutation in longitude * deps = double * (Returned) * Nutation in obliquity * eps0 = double * (Returned) * Mean obliquity. * Description: * Calculates the longitude * obliquity components and mean obliquity * using the SOFA library. * Authors: * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - Calls eraObl06 and eraNut06a and therefore uses the IAU 206 * precession/nutation model. * - Note the change from SLA/F regarding the date. TT is used * rather than TDB. * History: * 2012-03-05 (TIMJ): * Initial version * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "palmac.h" #include "pal1sofa.h" void palNutc( double date, double * dpsi, double *deps, double *eps0 ) { eraNut06a( PAL__MJD0, date, dpsi, deps ); *eps0 = eraObl06( PAL__MJD0, date ); } pal-0.5.0/palOap.c000644 000765 000024 00000023463 12366000607 013766 0ustar00timjstaff000000 000000 /* *+ * Name: * palOap * Purpose: * Observed to apparent place * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palOap ( const char *type, double ob1, double ob2, double date, * double dut, double elongm, double phim, double hm, * double xp, double yp, double tdk, double pmb, * double rh, double wl, double tlr, * double *rap, double *dap ); * Arguments: * type = const char * (Given) * Type of coordinates - 'R', 'H' or 'A' (see below) * ob1 = double (Given) * Observed Az, HA or RA (radians; Az is N=0;E=90) * ob2 = double (Given) * Observed ZD or Dec (radians) * date = double (Given) * UTC date/time (Modified Julian Date, JD-2400000.5) * dut = double (Given) * delta UT: UT1-UTC (UTC seconds) * elongm = double (Given) * Mean longitude of the observer (radians, east +ve) * phim = double (Given) * Mean geodetic latitude of the observer (radians) * hm = double (Given) * Observer's height above sea level (metres) * xp = double (Given) * Polar motion x-coordinates (radians) * yp = double (Given) * Polar motion y-coordinates (radians) * tdk = double (Given) * Local ambient temperature (K; std=273.15) * pmb = double (Given) * Local atmospheric pressure (mb; std=1013.25) * rh = double (Given) * Local relative humidity (in the range 0.0-1.0) * wl = double (Given) * Effective wavelength (micron, e.g. 0.55) * tlr = double (Given) * Tropospheric laps rate (K/metre, e.g. 0.0065) * rap = double * (Given) * Geocentric apparent right ascension * dap = double * (Given) * Geocentric apparent declination * Description: * Observed to apparent place. * Authors: * PTW: Patrick T. Wallace * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - Only the first character of the TYPE argument is significant. * 'R' or 'r' indicates that OBS1 and OBS2 are the observed right * ascension and declination; 'H' or 'h' indicates that they are * hour angle (west +ve) and declination; anything else ('A' or * 'a' is recommended) indicates that OBS1 and OBS2 are azimuth * (north zero, east 90 deg) and zenith distance. (Zenith * distance is used rather than elevation in order to reflect the * fact that no allowance is made for depression of the horizon.) * * - The accuracy of the result is limited by the corrections for * refraction. Providing the meteorological parameters are * known accurately and there are no gross local effects, the * predicted apparent RA,Dec should be within about 0.1 arcsec * for a zenith distance of less than 70 degrees. Even at a * topocentric zenith distance of 90 degrees, the accuracy in * elevation should be better than 1 arcmin; useful results * are available for a further 3 degrees, beyond which the * palRefro routine returns a fixed value of the refraction. * The complementary routines palAop (or palAopqk) and palOap * (or palOapqk) are self-consistent to better than 1 micro- * arcsecond all over the celestial sphere. * * - It is advisable to take great care with units, as even * unlikely values of the input parameters are accepted and * processed in accordance with the models used. * * - "Observed" Az,El means the position that would be seen by a * perfect theodolite located at the observer. This is * related to the observed HA,Dec via the standard rotation, using * the geodetic latitude (corrected for polar motion), while the * observed HA and RA are related simply through the local * apparent ST. "Observed" RA,Dec or HA,Dec thus means the * position that would be seen by a perfect equatorial located * at the observer and with its polar axis aligned to the * Earth's axis of rotation (n.b. not to the refracted pole). * By removing from the observed place the effects of * atmospheric refraction and diurnal aberration, the * geocentric apparent RA,Dec is obtained. * * - Frequently, mean rather than apparent RA,Dec will be required, * in which case further transformations will be necessary. The * palAmp etc routines will convert the apparent RA,Dec produced * by the present routine into an "FK5" (J2000) mean place, by * allowing for the Sun's gravitational lens effect, annual * aberration, nutation and precession. Should "FK4" (1950) * coordinates be needed, the routines palFk524 etc will also * need to be applied. * * - To convert to apparent RA,Dec the coordinates read from a * real telescope, corrections would have to be applied for * encoder zero points, gear and encoder errors, tube flexure, * the position of the rotator axis and the pointing axis * relative to it, non-perpendicularity between the mounting * axes, and finally for the tilt of the azimuth or polar axis * of the mounting (with appropriate corrections for mount * flexures). Some telescopes would, of course, exhibit other * properties which would need to be accounted for at the * appropriate point in the sequence. * * - This routine takes time to execute, due mainly to the rigorous * integration used to evaluate the refraction. For processing * multiple stars for one location and time, call palAoppa once * followed by one call per star to palOapqk. Where a range of * times within a limited period of a few hours is involved, and the * highest precision is not required, call palAoppa once, followed * by a call to palAoppat each time the time changes, followed by * one call per star to palOapqk. * * - The DATE argument is UTC expressed as an MJD. This is, strictly * speaking, wrong, because of leap seconds. However, as long as * the delta UT and the UTC are consistent there are no * difficulties, except during a leap second. In this case, the * start of the 61st second of the final minute should begin a new * MJD day and the old pre-leap delta UT should continue to be used. * As the 61st second completes, the MJD should revert to the start * of the day as, simultaneously, the delta UTC changes by one * second to its post-leap new value. * * - The delta UT (UT1-UTC) is tabulated in IERS circulars and * elsewhere. It increases by exactly one second at the end of * each UTC leap second, introduced in order to keep delta UT * within +/- 0.9 seconds. * * - IMPORTANT -- TAKE CARE WITH THE LONGITUDE SIGN CONVENTION. * The longitude required by the present routine is east-positive, * in accordance with geographical convention (and right-handed). * In particular, note that the longitudes returned by the * palOBS routine are west-positive, following astronomical * usage, and must be reversed in sign before use in the present * routine. * * - The polar coordinates XP,YP can be obtained from IERS * circulars and equivalent publications. The maximum amplitude * is about 0.3 arcseconds. If XP,YP values are unavailable, * use XP=YP=0D0. See page B60 of the 1988 Astronomical Almanac * for a definition of the two angles. * * - The height above sea level of the observing station, HM, * can be obtained from the Astronomical Almanac (Section J * in the 1988 edition), or via the routine palOBS. If P, * the pressure in millibars, is available, an adequate * estimate of HM can be obtained from the expression * * HM ~ -29.3*TSL*LOG(P/1013.25). * * where TSL is the approximate sea-level air temperature in K * (see Astrophysical Quantities, C.W.Allen, 3rd edition, * section 52). Similarly, if the pressure P is not known, * it can be estimated from the height of the observing * station, HM, as follows: * * P ~ 1013.25*EXP(-HM/(29.3*TSL)). * * Note, however, that the refraction is nearly proportional to the * pressure and that an accurate P value is important for precise * work. * * - The azimuths etc. used by the present routine are with respect * to the celestial pole. Corrections from the terrestrial pole * can be computed using palPolmo. * History: * 2012-08-27 (TIMJ): * Initial version, copied from Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2005 Patrick T. Wallace * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" void palOap ( const char *type, double ob1, double ob2, double date, double dut, double elongm, double phim, double hm, double xp, double yp, double tdk, double pmb, double rh, double wl, double tlr, double *rap, double *dap ) { double aoprms[14]; palAoppa(date,dut,elongm,phim,hm,xp,yp,tdk,pmb,rh,wl,tlr, aoprms); palOapqk(type,ob1,ob2,aoprms,rap,dap); } pal-0.5.0/palOapqk.c000644 000765 000024 00000020565 12366000607 014322 0ustar00timjstaff000000 000000 /* *+ * Name: * palOapqk * Purpose: * Quick observed to apparent place * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palOapqk ( const char *type, double ob1, double ob2, * const double aoprms[14], double *rap, double *dap ); * Arguments: * Quick observed to apparent place. * Description: * type = const char * (Given) * Type of coordinates - 'R', 'H' or 'A' (see below) * ob1 = double (Given) * Observed Az, HA or RA (radians; Az is N=0;E=90) * ob2 = double (Given) * Observed ZD or Dec (radians) * aoprms = const double [14] (Given) * Star-independent apparent-to-observed parameters. * See palAopqk for details. * rap = double * (Given) * Geocentric apparent right ascension * dap = double * (Given) * Geocentric apparent declination * Authors: * PTW: Patrick T. Wallace * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - Only the first character of the TYPE argument is significant. * 'R' or 'r' indicates that OBS1 and OBS2 are the observed right * ascension and declination; 'H' or 'h' indicates that they are * hour angle (west +ve) and declination; anything else ('A' or * 'a' is recommended) indicates that OBS1 and OBS2 are azimuth * (north zero, east 90 deg) and zenith distance. (Zenith distance * is used rather than elevation in order to reflect the fact that * no allowance is made for depression of the horizon.) * * - The accuracy of the result is limited by the corrections for * refraction. Providing the meteorological parameters are * known accurately and there are no gross local effects, the * predicted apparent RA,Dec should be within about 0.1 arcsec * for a zenith distance of less than 70 degrees. Even at a * topocentric zenith distance of 90 degrees, the accuracy in * elevation should be better than 1 arcmin; useful results * are available for a further 3 degrees, beyond which the * palREFRO routine returns a fixed value of the refraction. * The complementary routines palAop (or palAopqk) and palOap * (or palOapqk) are self-consistent to better than 1 micro- * arcsecond all over the celestial sphere. * * - It is advisable to take great care with units, as even * unlikely values of the input parameters are accepted and * processed in accordance with the models used. * * - "Observed" Az,El means the position that would be seen by a * perfect theodolite located at the observer. This is * related to the observed HA,Dec via the standard rotation, using * the geodetic latitude (corrected for polar motion), while the * observed HA and RA are related simply through the local * apparent ST. "Observed" RA,Dec or HA,Dec thus means the * position that would be seen by a perfect equatorial located * at the observer and with its polar axis aligned to the * Earth's axis of rotation (n.b. not to the refracted pole). * By removing from the observed place the effects of * atmospheric refraction and diurnal aberration, the * geocentric apparent RA,Dec is obtained. * * - Frequently, mean rather than apparent RA,Dec will be required, * in which case further transformations will be necessary. The * palAmp etc routines will convert the apparent RA,Dec produced * by the present routine into an "FK5" (J2000) mean place, by * allowing for the Sun's gravitational lens effect, annual * aberration, nutation and precession. Should "FK4" (1950) * coordinates be needed, the routines palFk524 etc will also * need to be applied. * * - To convert to apparent RA,Dec the coordinates read from a * real telescope, corrections would have to be applied for * encoder zero points, gear and encoder errors, tube flexure, * the position of the rotator axis and the pointing axis * relative to it, non-perpendicularity between the mounting * axes, and finally for the tilt of the azimuth or polar axis * of the mounting (with appropriate corrections for mount * flexures). Some telescopes would, of course, exhibit other * properties which would need to be accounted for at the * appropriate point in the sequence. * * - The star-independent apparent-to-observed-place parameters * in AOPRMS may be computed by means of the palAoppa routine. * If nothing has changed significantly except the time, the * palAoppat routine may be used to perform the requisite * partial recomputation of AOPRMS. * * - The azimuths etc used by the present routine are with respect * to the celestial pole. Corrections from the terrestrial pole * can be computed using palPolmo. * History: * 2012-08-27 (TIMJ): * Initial version, direct copy of Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2004 Patrick T. Wallace * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include #include "pal.h" #include "palmac.h" void palOapqk ( const char *type, double ob1, double ob2, const double aoprms[14], double *rap, double *dap ) { /* breakpoint for fast/slow refraction algorithm: * zd greater than arctan(4), (see sla_refco routine) * or vector z less than cosine(arctan(z)) = 1/sqrt(17) */ const double zbreak = 0.242535625; char c; double c1,c2,sphi,cphi,st,ce,xaeo,yaeo,zaeo,v[3], xmhdo,ymhdo,zmhdo,az,sz,zdo,tz,dref,zdt, xaet,yaet,zaet,xmhda,ymhda,zmhda,diurab,f,hma; /* coordinate type */ c = type[0]; /* coordinates */ c1 = ob1; c2 = ob2; /* sin, cos of latitude */ sphi = aoprms[1]; cphi = aoprms[2]; /* local apparent sidereal time */ st = aoprms[13]; /* standardise coordinate type */ if (c == 'r' || c == 'R') { c = 'r'; } else if (c == 'h' || c == 'H') { c = 'h'; } else { c = 'a'; } /* if az,zd convert to cartesian (s=0,e=90) */ if (c == 'a') { ce = sin(c2); xaeo = -cos(c1)*ce; yaeo = sin(c1)*ce; zaeo = cos(c2); } else { /* if ra,dec convert to ha,dec */ if (c == 'r') { c1 = st-c1; } /* to cartesian -ha,dec */ palDcs2c( -c1, c2, v ); xmhdo = v[0]; ymhdo = v[1]; zmhdo = v[2]; /* to cartesian az,el (s=0,e=90) */ xaeo = sphi*xmhdo-cphi*zmhdo; yaeo = ymhdo; zaeo = cphi*xmhdo+sphi*zmhdo; } /* azimuth (s=0,e=90) */ if (xaeo != 0.0 || yaeo != 0.0) { az = atan2(yaeo,xaeo); } else { az = 0.0; } /* sine of observed zd, and observed zd */ sz = sqrt(xaeo*xaeo+yaeo*yaeo); zdo = atan2(sz,zaeo); /* * refraction * ---------- */ /* large zenith distance? */ if (zaeo >= zbreak) { /* fast algorithm using two constant model */ tz = sz/zaeo; dref = (aoprms[10]+aoprms[11]*tz*tz)*tz; } else { /* rigorous algorithm for large zd */ palRefro(zdo,aoprms[4],aoprms[5],aoprms[6],aoprms[7], aoprms[8],aoprms[0],aoprms[9],1e-8,&dref); } zdt = zdo+dref; /* to cartesian az,zd */ ce = sin(zdt); xaet = cos(az)*ce; yaet = sin(az)*ce; zaet = cos(zdt); /* cartesian az,zd to cartesian -ha,dec */ xmhda = sphi*xaet+cphi*zaet; ymhda = yaet; zmhda = -cphi*xaet+sphi*zaet; /* diurnal aberration */ diurab = -aoprms[3]; f = (1.0-diurab*ymhda); v[0] = f*xmhda; v[1] = f*(ymhda+diurab); v[2] = f*zmhda; /* to spherical -ha,dec */ palDcc2s(v,&hma,dap); /* Right Ascension */ *rap = palDranrm(st+hma); } pal-0.5.0/palObs.c000644 000765 000024 00000061654 12366003553 014001 0ustar00timjstaff000000 000000 /* *+ * Name: * palObs * Purpose: * Parameters of selected ground-based observing stations * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * int palObs( size_t n, const char * c, * char * ident, size_t identlen, * char * name, size_t namelen, * double * w, double * p, double * h ); * Arguments: * n = size_t (Given) * Number specifying the observing station. If 0 * the identifier in "c" is used to determine the * observing station to use. * c = const char * (Given) * Identifier specifying the observing station for * which the parameters should be returned. Only used * if n is 0. Can be NULL for n>0. Case insensitive. * ident = char * (Returned) * Identifier of the observing station selected. Will be * identical to "c" if n==0. Unchanged if "n" or "c" * do not match an observing station. Should be at least * 11 characters (including the trailing nul). * identlen = size_t (Given) * Size of the buffer "ident" including trailing nul. * name = char * (Returned) * Full name of the specified observing station. Contains "?" * if "n" or "c" did not correspond to a valid station. Should * be at least 41 characters (including the trailing nul). * w = double * (Returned) * Longitude (radians, West +ve). Unchanged if observing * station could not be identified. * p = double * (Returned) * Geodetic latitude (radians, North +ve). Unchanged if observing * station could not be identified. * h = double * (Returned) * Height above sea level (metres). Unchanged if observing * station could not be identified. * Returned Value: * palObs = int * 0 if an observing station was returned. -1 if no match was * found. * Description: * Station numbers, identifiers, names and other details are * subject to change and should not be hardwired into * application programs. * * All characters in "c" up to the first space are * checked; thus an abbreviated ID will return the parameters * for the first station in the list which matches the * abbreviation supplied, and no station in the list will ever * contain embedded spaces. "c" must not have leading spaces. * * IMPORTANT -- BEWARE OF THE LONGITUDE SIGN CONVENTION. The * longitude returned by sla_OBS is west-positive in accordance * with astronomical usage. However, this sign convention is * left-handed and is the opposite of the one used by geographers; * elsewhere in PAL the preferable east-positive convention is * used. In particular, note that for use in palAop, palAoppa * and palOap the sign of the longitude must be reversed. * * Users are urged to inform the author of any improvements * they would like to see made. For example: * * typographical corrections * more accurate parameters * better station identifiers or names * additional stations * Authors: * PTW: Patrick T. Wallace * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - Differs from the SLA interface in that the output short name * is not the same variable as the input short name. This simplifies * consting. Additionally the size of the output buffers are now * specified in the API and a status integer is returned. * History: * 2012-03-06 (TIMJ): * Initial version containing entries from SLA/F as of 15 March 2002 * with a 2008 tweak to the JCMT GPS position. * Adapted with permission from the Fortran SLALIB library. * 2014-04-08 (TIMJ): * Add APEX and NANTEN2 * {enter_further_changes_here} * Copyright: * Copyright (C) 2002 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * Copyright (C) 2014 Cornell University. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #if HAVE_CONFIG_H # include #endif #include /* We prefer to use the starutil package. */ #if HAVE_STAR_UTIL_H #include "star/util.h" #else /* This version is just a straight copy without putting ellipsis on the end. */ static void star__strellcpy( char * dest, const char * src, size_t size ) { # if HAVE_STRLCPY strlcpy( dest, src, size ); # else strncpy( dest, src, size ); dest[size-1] = '\0'; # endif } #define star_strellcpy(dest, src, size) star__strellcpy(dest, src, size) #endif #include "pal.h" #include "palmac.h" /* Helper macros to convert degrees to radians in longitude and latitude */ #define WEST(ID,IAM,AS) PAL__DAS2R*((60.0*(60.0*(double)ID+(double)IAM))+(double)AS) #define NORTH(ID,IAM,AS) WEST(ID,IAM,AS) #define EAST(ID,IAM,AS) -1.0*WEST(ID,IAM,AS) #define SOUTH(ID,IAM,AS) -1.0*WEST(ID,IAM,AS) struct telData { double w; double p; double h; char shortname[11]; char longname[41]; }; int palObs( size_t n, const char * c, char * ident, size_t identlen, char * name, size_t namelen, double * w, double * p, double * h ) { const struct telData telData[] = { /* AAT (Observer's Guide) AAT */ { EAST(149,3,57.91), SOUTH(31,16,37.34), 1164E0, "AAT", "Anglo-Australian 3.9m Telescope" }, /* WHT (Gemini, April 1987) LPO4.2 */ { WEST(17,52,53.9), NORTH(28,45,38.1), 2332E0, "LPO4.2", "William Herschel 4.2m Telescope" }, /* INT (Gemini, April 1987) LPO2.5 */ { WEST(17,52,39.5), NORTH(28,45,43.2), 2336E0, "LPO2.5", "Isaac Newton 2.5m Telescope" }, /* JKT (Gemini, April 1987) LPO1 */ { WEST(17,52,41.2), NORTH(28,45,39.9), 2364E0, "LPO1", "Jacobus Kapteyn 1m Telescope" }, /* Lick 120" (S.L.Allen, private communication, 2002) LICK120 */ { WEST(121,38,13.689), NORTH(37,20,34.931), 1286E0, "LICK120", "Lick 120 inch" }, /* MMT 6.5m conversion (MMT Observatory website) MMT */ { WEST(110,53,4.4), NORTH(31,41,19.6), 2608E0, "MMT", "MMT 6.5m, Mt Hopkins" }, /* Victoria B.C. 1.85m (1984 Almanac) DAO72 */ { WEST(123,25,1.18), NORTH(48,31,11.9), 238E0, "DAO72", "DAO Victoria BC 1.85 metre" }, /* Las Campanas (1983 Almanac) DUPONT */ { WEST(70,42,9.), SOUTH(29,0,11.), 2280E0, "DUPONT", "Du Pont 2.5m Telescope, Las Campanas" }, /* Mt Hopkins 1.5m (1983 Almanac) MTHOP1.5 */ { WEST(110,52,39.00), NORTH(31,40,51.4), 2344E0, "MTHOP1.5", "Mt Hopkins 1.5 metre" }, /* Mt Stromlo 74" (1983 Almanac) STROMLO74 */ { EAST(149,0,27.59), SOUTH(35,19,14.3), 767E0, "STROMLO74", "Mount Stromlo 74 inch" }, /* ANU 2.3m, SSO (Gary Hovey) ANU2.3 */ { EAST(149,3,40.3), SOUTH(31,16,24.1), 1149E0, "ANU2.3", "Siding Spring 2.3 metre" }, /* Greenbank 140' (1983 Almanac) GBVA140 */ { WEST(79,50,9.61), NORTH(38,26,15.4), 881E0, "GBVA140", "Greenbank 140 foot" }, /* Cerro Tololo 4m (1982 Almanac) TOLOLO4M */ { WEST(70,48,53.6), SOUTH(30,9,57.8), 2235E0, "TOLOLO4M", "Cerro Tololo 4 metre" }, /* Cerro Tololo 1.5m (1982 Almanac) TOLOLO1.5M */ { WEST(70,48,54.5), SOUTH(30,9,56.3), 2225E0, "TOLOLO1.5M", "Cerro Tololo 1.5 metre" }, /* Tidbinbilla 64m (1982 Almanac) TIDBINBLA */ { EAST(148,58,48.20), SOUTH(35,24,14.3), 670E0, "TIDBINBLA", "Tidbinbilla 64 metre" }, /* Bloemfontein 1.52m (1981 Almanac) BLOEMF */ { EAST(26,24,18.), SOUTH(29,2,18.), 1387E0, "BLOEMF", "Bloemfontein 1.52 metre" }, /* Bosque Alegre 1.54m (1981 Almanac) BOSQALEGRE */ { WEST(64,32,48.0), SOUTH(31,35,53.), 1250E0, "BOSQALEGRE", "Bosque Alegre 1.54 metre" }, /* USNO 61" astrographic reflector, Flagstaff (1981 Almanac) FLAGSTF61 */ { WEST(111,44,23.6), NORTH(35,11,2.5), 2316E0, "FLAGSTF61", "USNO 61 inch astrograph, Flagstaff" }, /* Lowell 72" (1981 Almanac) LOWELL72 */ { WEST(111,32,9.3), NORTH(35,5,48.6), 2198E0, "LOWELL72", "Perkins 72 inch, Lowell" }, /* Harvard 1.55m (1981 Almanac) HARVARD */ { WEST(71,33,29.32), NORTH(42,30,19.0), 185E0, "HARVARD", "Harvard College Observatory 1.55m" }, /* Okayama 1.88m (1981 Almanac) OKAYAMA */ { EAST(133,35,47.29), NORTH(34,34,26.1), 372E0, "OKAYAMA", "Okayama 1.88 metre" }, /* Kitt Peak Mayall 4m (1981 Almanac) KPNO158 */ { WEST(111,35,57.61), NORTH(31,57,50.3), 2120E0, "KPNO158", "Kitt Peak 158 inch" }, /* Kitt Peak 90 inch (1981 Almanac) KPNO90 */ { WEST(111,35,58.24), NORTH(31,57,46.9), 2071E0, "KPNO90", "Kitt Peak 90 inch" }, /* Kitt Peak 84 inch (1981 Almanac) KPNO84 */ { WEST(111,35,51.56), NORTH(31,57,29.2), 2096E0, "KPNO84", "Kitt Peak 84 inch" }, /* Kitt Peak 36 foot (1981 Almanac) KPNO36FT */ { WEST(111,36,51.12), NORTH(31,57,12.1), 1939E0, "KPNO36FT", "Kitt Peak 36 foot" }, /* Kottamia 74" (1981 Almanac) KOTTAMIA */ { EAST(31,49,30.), NORTH(29,55,54.), 476E0, "KOTTAMIA", "Kottamia 74 inch" }, /* La Silla 3.6m (1981 Almanac) ESO3.6 */ { WEST(70,43,36.), SOUTH(29,15,36.), 2428E0, "ESO3.6", "ESO 3.6 metre" }, /* Mauna Kea 88 inch MAUNAK88 */ /* (IfA website, Richard Wainscoat) */ { WEST(155,28,9.96), NORTH(19,49,22.77), 4213.6E0, "MAUNAK88", "Mauna Kea 88 inch" }, /* UKIRT (IfA website, Richard Wainscoat) UKIRT */ { WEST(155,28,13.18), NORTH(19,49,20.75), 4198.5E0, "UKIRT", "UK Infra Red Telescope" }, /* Quebec 1.6m (1981 Almanac) QUEBEC1.6 */ { WEST(71,9,9.7), NORTH(45,27,20.6), 1114E0, "QUEBEC1.6", "Quebec 1.6 metre" }, /* Mt Ekar 1.82m (1981 Almanac) MTEKAR */ { EAST(11,34,15.), NORTH(45,50,48.), 1365E0, "MTEKAR", "Mt Ekar 1.82 metre" }, /* Mt Lemmon 60" (1981 Almanac) MTLEMMON60 */ { WEST(110,42,16.9), NORTH(32,26,33.9), 2790E0, "MTLEMMON60", "Mt Lemmon 60 inch" }, /* Mt Locke 2.7m (1981 Almanac) MCDONLD2.7 */ { WEST(104,1,17.60), NORTH(30,40,17.7), 2075E0, "MCDONLD2.7", "McDonald 2.7 metre" }, /* Mt Locke 2.1m (1981 Almanac) MCDONLD2.1 */ { WEST(104,1,20.10), NORTH(30,40,17.7), 2075E0, "MCDONLD2.1", "McDonald 2.1 metre" }, /* Palomar 200" (1981 Almanac) PALOMAR200 */ { WEST(116,51,50.), NORTH(33,21,22.), 1706E0, "PALOMAR200", "Palomar 200 inch" }, /* Palomar 60" (1981 Almanac) PALOMAR60 */ { WEST(116,51,31.), NORTH(33,20,56.), 1706E0, "PALOMAR60", "Palomar 60 inch" }, /* David Dunlap 74" (1981 Almanac) DUNLAP74 */ { WEST(79,25,20.), NORTH(43,51,46.), 244E0, "DUNLAP74", "David Dunlap 74 inch" }, /* Haute Provence 1.93m (1981 Almanac) HPROV1.93 */ { EAST(5,42,46.75), NORTH(43,55,53.3), 665E0, "HPROV1.93", "Haute Provence 1.93 metre" }, /* Haute Provence 1.52m (1981 Almanac) HPROV1.52 */ { EAST(5,42,43.82), NORTH(43,56,0.2), 667E0, "HPROV1.52", "Haute Provence 1.52 metre" }, /* San Pedro Martir 83" (1981 Almanac) SANPM83 */ { WEST(115,27,47.), NORTH(31,2,38.), 2830E0, "SANPM83", "San Pedro Martir 83 inch" }, /* Sutherland 74" (1981 Almanac) SAAO74 */ { EAST(20,48,44.3), SOUTH(32,22,43.4), 1771E0, "SAAO74", "Sutherland 74 inch" }, /* Tautenburg 2m (1981 Almanac) TAUTNBG */ { EAST(11,42,45.), NORTH(50,58,51.), 331E0, "TAUTNBG", "Tautenburg 2 metre" }, /* Catalina 61" (1981 Almanac) CATALINA61 */ { WEST(110,43,55.1), NORTH(32,25,0.7), 2510E0, "CATALINA61", "Catalina 61 inch" }, /* Steward 90" (1981 Almanac) STEWARD90 */ { WEST(111,35,58.24), NORTH(31,57,46.9), 2071E0, "STEWARD90", "Steward 90 inch" }, /* Russian 6m (1981 Almanac) USSR6 */ { EAST(41,26,30.0), NORTH(43,39,12.), 2100E0, "USSR6", "USSR 6 metre" }, /* Arecibo 1000' (1981 Almanac) ARECIBO */ { WEST(66,45,11.1), NORTH(18,20,36.6), 496E0, "ARECIBO", "Arecibo 1000 foot" }, /* Cambridge 5km (1981 Almanac) CAMB5KM */ { EAST(0,2,37.23), NORTH(52,10,12.2), 17E0, "CAMB5KM", "Cambridge 5km" }, /* Cambridge 1 mile (1981 Almanac) CAMB1MILE */ { EAST(0,2,21.64), NORTH(52,9,47.3), 17E0, "CAMB1MILE", "Cambridge 1 mile" }, /* Bonn 100m (1981 Almanac) EFFELSBERG */ { EAST(6,53,1.5), NORTH(50,31,28.6), 366E0, "EFFELSBERG", "Effelsberg 100 metre" }, /* Greenbank 300' (1981 Almanac) GBVA300 (R.I.P.) */ { WEST(79,50,56.36), NORTH(38,25,46.3), 894E0, "(R.I.P.)", "Greenbank 300 foot" }, /* Jodrell Bank Mk 1 (1981 Almanac) JODRELL1 */ { WEST(2,18,25.), NORTH(53,14,10.5), 78E0, "JODRELL1", "Jodrell Bank 250 foot" }, /* Australia Telescope Parkes Observatory PARKES */ /* (Peter te Lintel Hekkert) */ { EAST(148,15,44.3591), SOUTH(32,59,59.8657), 391.79E0, "PARKES", "Parkes 64 metre" }, /* VLA (1981 Almanac) VLA */ { WEST(107,37,3.82), NORTH(34,4,43.5), 2124E0, "VLA", "Very Large Array" }, /* Sugar Grove 150' (1981 Almanac) SUGARGROVE */ { WEST(79,16,23.), NORTH(38,31,14.), 705E0, "SUGARGROVE", "Sugar Grove 150 foot" }, /* Russian 600' (1981 Almanac) USSR600 */ { EAST(41,35,25.5), NORTH(43,49,32.), 973E0, "USSR600", "USSR 600 foot" }, /* Nobeyama 45 metre mm dish (based on 1981 Almanac entry) NOBEYAMA */ { EAST(138,29,12.), NORTH(35,56,19.), 1350E0, "NOBEYAMA", "Nobeyama 45 metre" }, /* James Clerk Maxwell 15 metre mm telescope, Mauna Kea JCMT */ /* From GPS measurements on 11Apr2007 for eSMA setup (R. Tilanus) */ { WEST(155,28,37.30), NORTH(19,49,22.22), 4124.75E0, "JCMT", "JCMT 15 metre" }, /* ESO 3.5 metre NTT, La Silla (K.Wirenstrand) ESONTT */ { WEST(70,43,7.), SOUTH(29,15,30.), 2377E0, "ESONTT", "ESO 3.5 metre NTT" }, /* St Andrews University Observatory (1982 Almanac) ST.ANDREWS */ { WEST(2,48,52.5), NORTH(56,20,12.), 30E0, "ST.ANDREWS", "St Andrews" }, /* Apache Point 3.5 metre (R.Owen) APO3.5 */ { WEST(105,49,11.56), NORTH(32,46,48.96), 2809E0, "APO3.5", "Apache Point 3.5m" }, /* W.M.Keck Observatory, Telescope 1 KECK1 */ /* (William Lupton) */ { WEST(155,28,28.99), NORTH(19,49,33.41), 4160E0, "KECK1", "Keck 10m Telescope #1" }, /* Tautenberg Schmidt (1983 Almanac) TAUTSCHM */ { EAST(11,42,45.0), NORTH(50,58,51.0), 331E0, "TAUTSCHM", "Tautenberg 1.34 metre Schmidt" }, /* Palomar Schmidt (1981 Almanac) PALOMAR48 */ { WEST(116,51,32.0), NORTH(33,21,26.0), 1706E0, "PALOMAR48", "Palomar 48-inch Schmidt" }, /* UK Schmidt, Siding Spring (1983 Almanac) UKST */ { EAST(149,4,12.8), SOUTH(31,16,27.8), 1145E0, "UKST", "UK 1.2 metre Schmidt, Siding Spring" }, /* Kiso Schmidt, Japan (1981 Almanac) KISO */ { EAST(137,37,42.2), NORTH(35,47,38.7), 1130E0, "KISO", "Kiso 1.05 metre Schmidt, Japan" }, /* ESO Schmidt, La Silla (1981 Almanac) ESOSCHM */ { WEST(70,43,46.5), SOUTH(29,15,25.8), 2347E0, "ESOSCHM", "ESO 1 metre Schmidt, La Silla" }, /* Australia Telescope Compact Array ATCA */ /* (WGS84 coordinates of Station 35, Mark Calabretta) */ { EAST(149,33,0.500), SOUTH(30,18,46.385), 236.9E0, "ATCA", "Australia Telescope Compact Array" }, /* Australia Telescope Mopra Observatory MOPRA */ /* (Peter te Lintel Hekkert) */ { EAST(149,5,58.732), SOUTH(31,16,4.451), 850E0, "MOPRA", "ATNF Mopra Observatory" }, /* Subaru telescope, Mauna Kea SUBARU */ /* (IfA website, Richard Wainscoat) */ { WEST(155,28,33.67), NORTH(19,49,31.81), 4163E0, "SUBARU", "Subaru 8m telescope" }, /* Canada-France-Hawaii Telescope, Mauna Kea CFHT */ /* (IfA website, Richard Wainscoat) */ { WEST(155,28,7.95), NORTH(19,49,30.91), 4204.1E0, "CFHT", "Canada-France-Hawaii 3.6m Telescope" }, /* W.M.Keck Observatory, Telescope 2 KECK2 */ /* (William Lupton) */ { WEST(155,28,27.24), NORTH(19,49,35.62), 4159.6E0, "KECK2", "Keck 10m Telescope #2" }, /* Gemini North, Mauna Kea GEMININ */ /* (IfA website, Richard Wainscoat) */ { WEST(155,28,8.57), NORTH(19,49,25.69), 4213.4E0, "GEMININ", "Gemini North 8-m telescope" }, /* Five College Radio Astronomy Observatory FCRAO */ /* (Tim Jenness) */ { WEST(72,20,42.0), NORTH(42,23,30.0), 314E0, "FCRAO", "Five College Radio Astronomy Obs" }, /* NASA Infra Red Telescope Facility IRTF */ /* (IfA website, Richard Wainscoat) */ { WEST(155,28,19.20), NORTH(19,49,34.39), 4168.1E0, "IRTF", "NASA IR Telescope Facility, Mauna Kea" }, /* Caltech Submillimeter Observatory CSO */ /* (IfA website, Richard Wainscoat; height estimated) */ { WEST(155,28,31.79), NORTH(19,49,20.78), 4080E0, "CSO", "Caltech Sub-mm Observatory, Mauna Kea" }, /* ESO VLT, UT1 VLT1 */ /* (ESO website, VLT Whitebook Chapter 2) */ { WEST(70,24,11.642), SOUTH(24,37,33.117), 2635.43, "VLT1", "ESO VLT, Paranal, Chile: UT1" }, /* ESO VLT, UT2 VLT2 */ /* (ESO website, VLT Whitebook Chapter 2) */ { WEST(70,24,10.855), SOUTH(24,37,31.465), 2635.43, "VLT2", "ESO VLT, Paranal, Chile: UT2" }, /* ESO VLT, UT3 VLT3 */ /* (ESO website, VLT Whitebook Chapter 2) */ { WEST(70,24,9.896), SOUTH(24,37,30.300), 2635.43, "VLT3", "ESO VLT, Paranal, Chile: UT3" }, /* ESO VLT, UT4 VLT4 */ /* (ESO website, VLT Whitebook Chapter 2) */ { WEST(70,24,8.000), SOUTH(24,37,31.000), 2635.43, "VLT4", "ESO VLT, Paranal, Chile: UT4" }, /* Gemini South, Cerro Pachon GEMINIS */ /* (GPS readings by Patrick Wallace) */ { WEST(70,44,11.5), SOUTH(30,14,26.7), 2738E0, "GEMINIS", "Gemini South 8-m telescope" }, /* Cologne Observatory for Submillimeter Astronomy (KOSMA) KOSMA3M */ /* (Holger Jakob) */ { EAST(7,47,3.48), NORTH(45,58,59.772), 3141E0, "KOSMA3M", "KOSMA 3m telescope, Gornergrat" }, /* Magellan 1, 6.5m telescope at Las Campanas, Chile MAGELLAN1 */ /* (Skip Schaller) */ { WEST(70,41,31.9), SOUTH(29,0,51.7), 2408E0, "MAGELLAN1", "Magellan 1, 6.5m, Las Campanas" }, /* Magellan 2, 6.5m telescope at Las Campanas, Chile MAGELLAN2 */ /* (Skip Schaller) */ { WEST(70,41,33.5), SOUTH(29,0,50.3), 2408E0, "MAGELLAN2", "Magellan 2, 6.5m, Las Campanas" }, /* APEX - Atacama Pathfinder EXperiment, Llano de Chajnantor APEX */ /* (APEX web site) */ { WEST(67,45,33.0), SOUTH(23,0,20.8), 5105E0, "APEX", "APEX 12m telescope, Llano de Chajnantor" }, /* NANTEN2 Submillimeter Observatory, 4m telescope Atacame desert NANTEN2 */ /* (NANTEN2 web site) */ { WEST(67,42,8.0), SOUTH(22,57,47.0), 4865E0, "NANTEN2", "NANTEN2 4m telescope, Pampa la Bola" } }; int retval = -1; /* Return status. 0 if found. -1 if no match */ /* Work out the number of telescopes */ const size_t NTEL = sizeof(telData) / sizeof(struct telData); /* Prefill the return buffer in a pessimistic manner */ star_strellcpy( name, "?", namelen ); if (n > 0) { if (n <= NTEL) { /* Index into telData with correction for zero-based indexing */ struct telData thistel; thistel = telData[n-1]; *w = thistel.w; *p = thistel.p; *h = thistel.h; star_strellcpy( ident, thistel.shortname, identlen ); star_strellcpy( name, thistel.longname, namelen ); retval = 0; } } else { /* Searching */ size_t i; for (i=0; i. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "palmac.h" #include "pal1sofa.h" void palCldj ( int iy, int im, int id, double *djm, int *j ) { double djm0; *j = eraCal2jd( iy, im, id, &djm0, djm ); } double palDbear ( double a1, double b1, double a2, double b2 ) { return eraPas( a1, b1, a2, b2 ); } /* Arguments differ slightly. Assumes that the sign is always positive and dealt with externally. */ void palDaf2r ( int ideg, int iamin, double asec, double *rad, int *j ) { *j = eraAf2a( ' ', ideg, iamin, asec, rad ); } void palDav2m ( double axvec[3], double rmat[3][3] ) { eraRv2m( axvec, rmat ); } void palDcc2s ( double v[3], double *a, double *b ) { eraC2s( v, a, b ); } void palDcs2c ( double a, double b, double v[3] ) { eraS2c( a, b, v ); } void palDd2tf ( int ndp, double days, char *sign, int ihmsf[4] ) { eraD2tf( ndp, days, sign, ihmsf ); } void palDimxv ( double dm[3][3], double va[3], double vb[3] ) { eraTrxp( dm, va, vb ); } void palDm2av ( double rmat[3][3], double axvec[3] ) { eraRm2v( rmat, axvec ); } /* Requires additional SLA MJD reference date */ void palDjcl ( double djm, int *iy, int *im, int *id, double *fd, int *j ) { *j = eraJd2cal( PAL__MJD0, djm, iy, im, id, fd ); } void palDmxm ( double a[3][3], double b[3][3], double c[3][3] ) { eraRxr( a, b, c ); } void palDmxv ( double dm[3][3], double va[3], double vb[3] ) { eraRxp( dm, va, vb ); } double palDpav ( double v1[3], double v2[3] ) { return eraPap( v1, v2 ); } void palDr2af ( int ndp, double angle, char *sign, int idmsf[4] ) { eraA2af( ndp, angle, sign, idmsf ); } void palDr2tf( int ndp, double angle, char *sign, int ihmsf[4] ) { eraA2tf( ndp, angle, sign, ihmsf ); } double palDranrm ( double angle ) { return eraAnp( angle ); } double palDsep ( double a1, double b1, double a2, double b2 ) { return eraSeps( a1, b1, a2, b2 ); } double palDsepv ( double v1[3], double v2[3] ) { return eraSepp( v1, v2 ); } /* Assumes that the sign is always positive and is dealt with externally */ void palDtf2d ( int ihour, int imin, double sec, double *days, int *j ) { *j = eraTf2d( ' ', ihour, imin, sec, days ); } /* Assumes that the sign is dealt with outside this routine */ void palDtf2r ( int ihour, int imin, double sec, double *rad, int *j ) { *j = eraTf2a( ' ', ihour, imin, sec, rad ); } double palDvdv ( double va[3], double vb[3] ) { return eraPdp( va, vb ); } /* Note that the arguments are flipped */ void palDvn ( double v[3], double uv[3], double *vm ) { eraPn( v, vm, uv ); } void palDvxv ( double va[3], double vb[3], double vc[3] ) { eraPxp( va, vb, vc ); } /* Requires additional SLA MJD reference date */ double palEpb ( double date ) { return eraEpb( PAL__MJD0, date ); } double palEpb2d ( double epb ) { double djm0, djm; eraEpb2jd( epb, &djm0, &djm ); return djm; } /* Requires additional SLA MJD reference date */ double palEpj ( double date ) { return eraEpj( PAL__MJD0, date ); } double palEpj2d ( double epj ) { double djm0, djm; eraEpj2jd( epj, &djm0, &djm ); return djm; } /* Requires additional SLA MJD reference date */ double palEqeqx ( double date ) { return eraEe06a( PAL__MJD0, date ); } /* Do not use palEvp just yet */ void palFk5hz ( double r5, double d5, double epoch, double *rh, double *dh ) { /* Need to convert epoch to Julian date first */ double date1, date2; eraEpj2jd( epoch, &date1, &date2 ); eraFk5hz( r5, d5, date1, date2, rh, dh ); } /* Note that SOFA has more accurate time arguments and we use the 2006 precession model */ double palGmst ( double ut1 ) { return eraGmst06( PAL__MJD0, ut1, PAL__MJD0, ut1 ); } /* Slightly better but still not as accurate as SOFA */ double palGmsta( double date, double ut ) { date += PAL__MJD0; return eraGmst06( date, ut, date, ut ); } void palHfk5z ( double rh, double dh, double epoch, double *r5, double *d5, double *dr5, double *dd5 ) { /* Need to convert epoch to Julian date first */ double date1, date2; eraEpj2jd( epoch, &date1, &date2 ); eraHfk5z( rh, dh, date1, date2, r5, d5, dr5, dd5 ); } void palRefcoq ( double tdk, double pmb, double rh, double wl, double *refa, double *refb ) { /* Note that SLA (and therefore PAL) uses units of kelvin but SOFA uses deg C */ eraRefco( pmb, tdk - 273.15, rh, wl, refa, refb ); } pal-0.5.0/palPa.c000644 000765 000024 00000005062 12366000607 013602 0ustar00timjstaff000000 000000 /* *+ * Name: * palPa * Purpose: * HA, Dec to Parallactic Angle * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * double palPa( double ha, double dec, double phi ); * Arguments: * ha = double (Given) * Hour angle in radians (Geocentric apparent) * dec = double (Given) * Declination in radians (Geocentric apparent) * phi = double (Given) * Observatory latitude in radians (geodetic) * Returned Value: * palPa = double * Parallactic angle in the range -pi to +pi. * Description: * Converts HA, Dec to Parallactic Angle. * Authors: * PTW: Patrick T. Wallace * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - The parallactic angle at a point in the sky is the position * angle of the vertical, i.e. the angle between the direction to * the pole and to the zenith. In precise applications care must * be taken only to use geocentric apparent HA,Dec and to consider * separately the effects of atmospheric refraction and telescope * mount errors. * - At the pole a zero result is returned. * History: * 2012-03-02 (TIMJ): * Initial version * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1995 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include double palPa( double ha, double dec, double phi ) { double cp, sqsz, cqsz; cp = cos(phi); sqsz = cp * sin(ha); cqsz = sin(phi) * cos(dec) - cp * sin(dec) * cos(ha); if (sqsz == 0.0 && cqsz == 0.0) cqsz = 1.0; return atan2( sqsz, cqsz ); } pal-0.5.0/palPertel.c000644 000765 000024 00000017057 12366000607 014504 0ustar00timjstaff000000 000000 /* *+ * Name: * palPertel * Purpose: * Update elements by applying planetary perturbations * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palPertel (int jform, double date0, double date1, * double epoch0, double orbi0, double anode0, * double perih0, double aorq0, double e0, double am0, * double *epoch1, double *orbi1, double *anode1, * double *perih1, double *aorq1, double *e1, double *am1, * int *jstat ); * Arguments: * jform = int (Given) * Element set actually returned (1-3; Note 6) * date0 = double (Given) * Date of osculation (TT MJD) for the given elements. * date1 = double (Given) * Date of osculation (TT MJD) for the updated elements. * epoch0 = double (Given) * Epoch of elements (TT MJD) * orbi0 = double (Given) * inclination (radians) * anode0 = double (Given) * longitude of the ascending node (radians) * perih0 = double (Given) * longitude or argument of perihelion (radians) * aorq0 = double (Given) * mean distance or perihelion distance (AU) * e0 = double (Given) * eccentricity * am0 = double (Given) * mean anomaly (radians, JFORM=2 only) * epoch1 = double * (Returned) * Epoch of elements (TT MJD) * orbi1 = double * (Returned) * inclination (radians) * anode1 = double * (Returned) * longitude of the ascending node (radians) * perih1 = double * (Returned) * longitude or argument of perihelion (radians) * aorq1 = double * (Returned) * mean distance or perihelion distance (AU) * e1 = double * (Returned) * eccentricity * am1 = double * (Returned) * mean anomaly (radians, JFORM=2 only) * jstat = int * (Returned) * status: * - +102 = warning, distant epoch * - +101 = warning, large timespan ( > 100 years) * - +1 to +10 = coincident with planet (Note 6) * - 0 = OK * - -1 = illegal JFORM * - -2 = illegal E0 * - -3 = illegal AORQ0 * - -4 = internal error * - -5 = numerical error * Description: * Update the osculating orbital elements of an asteroid or comet by * applying planetary perturbations. * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - Two different element-format options are available: * * Option JFORM=2, suitable for minor planets: * * EPOCH = epoch of elements (TT MJD) * ORBI = inclination i (radians) * ANODE = longitude of the ascending node, big omega (radians) * PERIH = argument of perihelion, little omega (radians) * AORQ = mean distance, a (AU) * E = eccentricity, e * AM = mean anomaly M (radians) * * Option JFORM=3, suitable for comets: * * EPOCH = epoch of perihelion (TT MJD) * ORBI = inclination i (radians) * ANODE = longitude of the ascending node, big omega (radians) * PERIH = argument of perihelion, little omega (radians) * AORQ = perihelion distance, q (AU) * E = eccentricity, e * * - DATE0, DATE1, EPOCH0 and EPOCH1 are all instants of time in * the TT timescale (formerly Ephemeris Time, ET), expressed * as Modified Julian Dates (JD-2400000.5). * * DATE0 is the instant at which the given (i.e. unperturbed) * osculating elements are correct. * * DATE1 is the specified instant at which the updated osculating * elements are correct. * * EPOCH0 and EPOCH1 will be the same as DATE0 and DATE1 * (respectively) for the JFORM=2 case, normally used for minor * planets. For the JFORM=3 case, the two epochs will refer to * perihelion passage and so will not, in general, be the same as * DATE0 and/or DATE1 though they may be similar to one another. * - The elements are with respect to the J2000 ecliptic and equinox. * - Unused elements (AM0 and AM1 for JFORM=3) are not accessed. * - See the palPertue routine for details of the algorithm used. * - This routine is not intended to be used for major planets, which * is why JFORM=1 is not available and why there is no opportunity * to specify either the longitude of perihelion or the daily * motion. However, if JFORM=2 elements are somehow obtained for a * major planet and supplied to the routine, sensible results will, * in fact, be produced. This happens because the sla_PERTUE routine * that is called to perform the calculations checks the separation * between the body and each of the planets and interprets a * suspiciously small value (0.001 AU) as an attempt to apply it to * the planet concerned. If this condition is detected, the * contribution from that planet is ignored, and the status is set to * the planet number (1-10 = Mercury, Venus, EMB, Mars, Jupiter, * Saturn, Uranus, Neptune, Earth, Moon) as a warning. * * See Also: * - Sterne, Theodore E., "An Introduction to Celestial Mechanics", * Interscience Publishers Inc., 1960. Section 6.7, p199. * History: * 2012-03-12 (TIMJ): * Initial version direct conversion of SLA/F. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2004 Patrick T. Wallace * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" void palPertel (int jform, double date0, double date1, double epoch0, double orbi0, double anode0, double perih0, double aorq0, double e0, double am0, double *epoch1, double *orbi1, double *anode1, double *perih1, double *aorq1, double *e1, double *am1, int *jstat ) { double u[13], dm; int j, jf; /* Check that the elements are either minor-planet or comet format. */ if (jform < 2 || jform > 3) { *jstat = -1; return; } else { /* Provisionally set the status to OK. */ *jstat = 0; } /* Transform the elements from conventional to universal form. */ palEl2ue(date0,jform,epoch0,orbi0,anode0,perih0, aorq0,e0,am0,0.0,u,&j); if (j != 0) { *jstat = j; return; } /* Update the universal elements. */ palPertue(date1,u,&j); if (j > 0) { *jstat = j; } else if (j < 0) { *jstat = -5; return; } /* Transform from universal to conventional elements. */ palUe2el(u, jform, &jf, epoch1, orbi1, anode1, perih1, aorq1, e1, am1, &dm, &j); if (jf != jform || j != 0) *jstat = -5; } pal-0.5.0/palPertue.c000644 000765 000024 00000047671 12366000611 014515 0ustar00timjstaff000000 000000 /* *+ * Name: * palPertue * Purpose: * Update the universal elements by applying planetary perturbations * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palPertue( double date, double u[13], int *jstat ); * Arguments: * date = double (Given) * Final epoch (TT MJD) for the update elements. * u = const double [13] (Given & Returned) * Universal orbital elements (Note 1) * (0) combined mass (M+m) * (1) total energy of the orbit (alpha) * (2) reference (osculating) epoch (t0) * (3-5) position at reference epoch (r0) * (6-8) velocity at reference epoch (v0) * (9) heliocentric distance at reference epoch * (10) r0.v0 * (11) date (t) * (12) universal eccentric anomaly (psi) of date, approx * jstat = int * (Returned) * status: * +102 = warning, distant epoch * +101 = warning, large timespan ( > 100 years) * +1 to +10 = coincident with major planet (Note 5) * 0 = OK * -1 = numerical error * Description: * Update the universal elements of an asteroid or comet by applying * planetary perturbations. * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - The "universal" elements are those which define the orbit for the * purposes of the method of universal variables (see reference 2). * They consist of the combined mass of the two bodies, an epoch, * and the position and velocity vectors (arbitrary reference frame) * at that epoch. The parameter set used here includes also various * quantities that can, in fact, be derived from the other * information. This approach is taken to avoiding unnecessary * computation and loss of accuracy. The supplementary quantities * are (i) alpha, which is proportional to the total energy of the * orbit, (ii) the heliocentric distance at epoch, (iii) the * outwards component of the velocity at the given epoch, (iv) an * estimate of psi, the "universal eccentric anomaly" at a given * date and (v) that date. * - The universal elements are with respect to the J2000 equator and * equinox. * - The epochs DATE, U(3) and U(12) are all Modified Julian Dates * (JD-2400000.5). * - The algorithm is a simplified form of Encke's method. It takes as * a basis the unperturbed motion of the body, and numerically * integrates the perturbing accelerations from the major planets. * The expression used is essentially Sterne's 6.7-2 (reference 1). * Everhart and Pitkin (reference 2) suggest rectifying the orbit at * each integration step by propagating the new perturbed position * and velocity as the new universal variables. In the present * routine the orbit is rectified less frequently than this, in order * to gain a slight speed advantage. However, the rectification is * done directly in terms of position and velocity, as suggested by * Everhart and Pitkin, bypassing the use of conventional orbital * elements. * * The f(q) part of the full Encke method is not used. The purpose * of this part is to avoid subtracting two nearly equal quantities * when calculating the "indirect member", which takes account of the * small change in the Sun's attraction due to the slightly displaced * position of the perturbed body. A simpler, direct calculation in * double precision proves to be faster and not significantly less * accurate. * * Apart from employing a variable timestep, and occasionally * "rectifying the orbit" to keep the indirect member small, the * integration is done in a fairly straightforward way. The * acceleration estimated for the middle of the timestep is assumed * to apply throughout that timestep; it is also used in the * extrapolation of the perturbations to the middle of the next * timestep, to predict the new disturbed position. There is no * iteration within a timestep. * * Measures are taken to reach a compromise between execution time * and accuracy. The starting-point is the goal of achieving * arcsecond accuracy for ordinary minor planets over a ten-year * timespan. This goal dictates how large the timesteps can be, * which in turn dictates how frequently the unperturbed motion has * to be recalculated from the osculating elements. * * Within predetermined limits, the timestep for the numerical * integration is varied in length in inverse proportion to the * magnitude of the net acceleration on the body from the major * planets. * * The numerical integration requires estimates of the major-planet * motions. Approximate positions for the major planets (Pluto * alone is omitted) are obtained from the routine palPlanet. Two * levels of interpolation are used, to enhance speed without * significantly degrading accuracy. At a low frequency, the routine * palPlanet is called to generate updated position+velocity "state * vectors". The only task remaining to be carried out at the full * frequency (i.e. at each integration step) is to use the state * vectors to extrapolate the planetary positions. In place of a * strictly linear extrapolation, some allowance is made for the * curvature of the orbit by scaling back the radius vector as the * linear extrapolation goes off at a tangent. * * Various other approximations are made. For example, perturbations * by Pluto and the minor planets are neglected and relativistic * effects are not taken into account. * * In the interests of simplicity, the background calculations for * the major planets are carried out en masse. The mean elements and * state vectors for all the planets are refreshed at the same time, * without regard for orbit curvature, mass or proximity. * * The Earth-Moon system is treated as a single body when the body is * distant but as separate bodies when closer to the EMB than the * parameter RNE, which incurs a time penalty but improves accuracy * for near-Earth objects. * * - This routine is not intended to be used for major planets. * However, if major-planet elements are supplied, sensible results * will, in fact, be produced. This happens because the routine * checks the separation between the body and each of the planets and * interprets a suspiciously small value (0.001 AU) as an attempt to * apply the routine to the planet concerned. If this condition is * detected, the contribution from that planet is ignored, and the * status is set to the planet number (1-10 = Mercury, Venus, EMB, * Mars, Jupiter, Saturn, Uranus, Neptune, Earth, Moon) as a warning. * See Also: * - Sterne, Theodore E., "An Introduction to Celestial Mechanics", * Interscience Publishers Inc., 1960. Section 6.7, p199. * - Everhart, E. & Pitkin, E.T., Am.J.Phys. 51, 712, 1983. * History: * 2012-03-12 (TIMJ): * Initial version direct conversion of SLA/F. * Adapted with permission from the Fortran SLALIB library. * 2012-06-21 (TIMJ): * Support a lack of copysign() function. * 2012-06-22 (TIMJ): * Check __STDC_VERSION__ * {enter_further_changes_here} * Copyright: * Copyright (C) 2004 Patrick T. Wallace * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ /* Use the config file if we have one, else look at compiler defines to see if we have C99 */ #if HAVE_CONFIG_H #include #else #ifdef __STDC_VERSION__ # if (__STDC_VERSION__ >= 199901L) # define HAVE_COPYSIGN 1 # endif #endif #endif #include #include "pal.h" #include "palmac.h" #include "pal1sofa.h" /* copysign is C99 */ #if HAVE_COPYSIGN # define COPYSIGN copysign #else # define COPYSIGN(a,b) DSIGN(a,b) #endif void palPertue( double date, double u[13], int *jstat ) { /* Distance from EMB at which Earth and Moon are treated separately */ const double RNE=1.0; /* Coincidence with major planet distance */ const double COINC=0.0001; /* Coefficient relating timestep to perturbing force */ const double TSC=1e-4; /* Minimum and maximum timestep (days) */ const double TSMIN = 0.01; const double TSMAX = 10.0; /* Age limit for major-planet state vector (days) */ const double AGEPMO=5.0; /* Age limit for major-planet mean elements (days) */ const double AGEPEL=50.0; /* Margin for error when deciding whether to renew the planetary data */ const double TINY=1e-6; /* Age limit for the body's osculating elements (before rectification) */ const double AGEBEL=100.0; /* Gaussian gravitational constant squared */ const double GCON2 = PAL__GCON * PAL__GCON; /* The final epoch */ double TFINAL; /* The body's current universal elements */ double UL[13]; /* Current reference epoch */ double T0; /* Timespan from latest orbit rectification to final epoch (days) */ double TSPAN; /* Time left to go before integration is complete */ double TLEFT; /* Time direction flag: +1=forwards, -1=backwards */ double FB; /* First-time flag */ int FIRST = 0; /* * The current perturbations */ /* Epoch (days relative to current reference epoch) */ double RTN; /* Position (AU) */ double PERP[3]; /* Velocity (AU/d) */ double PERV[3]; /* Acceleration (AU/d/d) */ double PERA[3]; /* Length of current timestep (days), and half that */ double TS,HTS; /* Epoch of middle of timestep */ double T; /* Epoch of planetary mean elements */ double TPEL = 0.0; /* Planet number (1=Mercury, 2=Venus, 3=EMB...8=Neptune) */ int NP; /* Planetary universal orbital elements */ double UP[8][13]; /* Epoch of planetary state vectors */ double TPMO = 0.0; /* State vectors for the major planets (AU,AU/s) */ double PVIN[8][6]; /* Earth velocity and position vectors (AU,AU/s) */ double VB[3],PB[3],VH[3],PE[3]; /* Moon geocentric state vector (AU,AU/s) and position part */ double PVM[6],PM[3]; /* Date to J2000 de-precession matrix */ double PMAT[3][3]; /* * Correction terms for extrapolated major planet vectors */ /* Sun-to-planet distances squared multiplied by 3 */ double R2X3[8]; /* Sunward acceleration terms, G/2R^3 */ double GC[8]; /* Tangential-to-circular correction factor */ double FC; /* Radial correction factor due to Sunwards acceleration */ double FG; /* The body's unperturbed and perturbed state vectors (AU,AU/s) */ double PV0[6],PV[6]; /* The body's perturbed and unperturbed heliocentric distances (AU) cubed */ double R03,R3; /* The perturbating accelerations, indirect and direct */ double FI[3],FD[3]; /* Sun-to-planet vector, and distance cubed */ double RHO[3],RHO3; /* Body-to-planet vector, and distance cubed */ double DELTA[3],DELTA3; /* Miscellaneous */ int I,J; double R2,W,DT,DT2,R,FT; int NE; /* Planetary inverse masses, Mercury through Neptune then Earth and Moon */ const double AMAS[10] = { 6023600., 408523.5, 328900.5, 3098710., 1047.355, 3498.5, 22869., 19314., 332946.038, 27068709. }; /* Preset the status to OK. */ *jstat = 0; /* Copy the final epoch. */ TFINAL = date; /* Copy the elements (which will be periodically updated). */ for (I=0; I<13; I++) { UL[I] = u[I]; } /* Initialize the working reference epoch. */ T0=UL[2]; /* Total timespan (days) and hence time left. */ TSPAN = TFINAL-T0; TLEFT = TSPAN; /* Warn if excessive. */ if (fabs(TSPAN) > 36525.0) *jstat=101; /* Time direction: +1 for forwards, -1 for backwards. */ FB = COPYSIGN(1.0,TSPAN); /* Initialize relative epoch for start of current timestep. */ RTN = 0.0; /* Reset the perturbations (position, velocity, acceleration). */ for (I=0; I<3; I++) { PERP[I] = 0.0; PERV[I] = 0.0; PERA[I] = 0.0; } /* Set "first iteration" flag. */ FIRST = 1; /* Step through the time left. */ while (FB*TLEFT > 0.0) { /* Magnitude of current acceleration due to planetary attractions. */ if (FIRST) { TS = TSMIN; } else { R2 = 0.0; for (I=0; I<3; I++) { W = FD[I]; R2 = R2+W*W; } W = sqrt(R2); /* Use the acceleration to decide how big a timestep can be tolerated. */ if (W != 0.0) { TS = DMIN(TSMAX,DMAX(TSMIN,TSC/W)); } else { TS = TSMAX; } } TS = TS*FB; /* Override if final epoch is imminent. */ TLEFT = TSPAN-RTN; if (fabs(TS) > fabs(TLEFT)) TS=TLEFT; /* Epoch of middle of timestep. */ HTS = TS/2.0; T = T0+RTN+HTS; /* Is it time to recompute the major-planet elements? */ if (FIRST || fabs(T-TPEL)-AGEPEL >= TINY) { /* Yes: go forward in time by just under the maximum allowed. */ TPEL = T+FB*AGEPEL; /* Compute the state vector for the new epoch. */ for (NP=1; NP<=8; NP++) { palPlanet(TPEL,NP,PV,&J); /* Warning if remote epoch, abort if error. */ if (J == 1) { *jstat = 102; } else if (J != 0) { goto ABORT; } /* Transform the vector into universal elements. */ palPv2ue(PV,TPEL,0.0,&(UP[NP-1][0]),&J); if (J != 0) goto ABORT; } } /* Is it time to recompute the major-planet motions? */ if (FIRST || fabs(T-TPMO)-AGEPMO >= TINY) { /* Yes: look ahead. */ TPMO = T+FB*AGEPMO; /* Compute the motions of each planet (AU,AU/d). */ for (NP=1; NP<=8; NP++) { /* The planet's position and velocity (AU,AU/s). */ palUe2pv(TPMO,&(UP[NP-1][0]),&(PVIN[NP-1][0]),&J); if (J != 0) goto ABORT; /* Scale velocity to AU/d. */ for (J=3; J<6; J++) { PVIN[NP-1][J] = PVIN[NP-1][J]*PAL__SPD; } /* Precompute also the extrapolation correction terms. */ R2 = 0.0; for (I=0; I<3; I++) { W = PVIN[NP-1][I]; R2 = R2+W*W; } R2X3[NP-1] = R2*3.0; GC[NP-1] = GCON2/(2.0*R2*sqrt(R2)); } } /* Reset the first-time flag. */ FIRST = 0; /* Unperturbed motion of the body at middle of timestep (AU,AU/s). */ palUe2pv(T,UL,PV0,&J); if (J != 0) goto ABORT; /* Perturbed position of the body (AU) and heliocentric distance cubed. */ R2 = 0.0; for (I=0; I<3; I++) { W = PV0[I]+PERP[I]+(PERV[I]+PERA[I]*HTS/2.0)*HTS; PV[I] = W; R2 = R2+W*W; } R3 = R2*sqrt(R2); /* The body's unperturbed heliocentric distance cubed. */ R2 = 0.0; for (I=0; I<3; I++) { W = PV0[I]; R2 = R2+W*W; } R03 = R2*sqrt(R2); /* Compute indirect and initialize direct parts of the perturbation. */ for (I=0; I<3; I++) { FI[I] = PV0[I]/R03-PV[I]/R3; FD[I] = 0.0; } /* Ready to compute the direct planetary effects. */ /* Reset the "near-Earth" flag. */ NE = 0; /* Interval from state-vector epoch to middle of current timestep. */ DT = T-TPMO; DT2 = DT*DT; /* Planet by planet, including separate Earth and Moon. */ for (NP=1; NP<10; NP++) { /* Which perturbing body? */ if (NP <= 8) { /* Planet: compute the extrapolation in longitude (squared). */ R2 = 0.0; for (J=3; J<6; J++) { W = PVIN[NP-1][J]*DT; R2 = R2+W*W; } /* Hence the tangential-to-circular correction factor. */ FC = 1.0+R2/R2X3[NP-1]; /* The radial correction factor due to the inwards acceleration. */ FG = 1.0-GC[NP-1]*DT2; /* Planet's position. */ for (I=0; I<3; I++) { RHO[I] = FG*(PVIN[NP-1][I]+FC*PVIN[NP-1][I+3]*DT); } } else if (NE) { /* Near-Earth and either Earth or Moon. */ if (NP == 9) { /* Earth: position. */ palEpv(T,PE,VH,PB,VB); for (I=0; I<3; I++) { RHO[I] = PE[I]; } } else { /* Moon: position. */ palPrec(palEpj(T),2000.0,PMAT); palDmoon(T,PVM); eraRxp(PMAT,PVM,PM); for (I=0; I<3; I++) { RHO[I] = PM[I]+PE[I]; } } } /* Proceed unless Earth or Moon and not the near-Earth case. */ if (NP <= 8 || NE) { /* Heliocentric distance cubed. */ R2 = 0.0; for (I=0; I<3; I++) { W = RHO[I]; R2 = R2+W*W; } R = sqrt(R2); RHO3 = R2*R; /* Body-to-planet vector, and distance. */ R2 = 0.0; for (I=0; I<3; I++) { W = RHO[I]-PV[I]; DELTA[I] = W; R2 = R2+W*W; } R = sqrt(R2); /* If this is the EMB, set the near-Earth flag appropriately. */ if (NP == 3 && R < RNE) NE = 1; /* Proceed unless EMB and this is the near-Earth case. */ if ( ! (NE && NP == 3) ) { /* If too close, ignore this planet and set a warning. */ if (R < COINC) { *jstat = NP; } else { /* Accumulate "direct" part of perturbation acceleration. */ DELTA3 = R2*R; W = AMAS[NP-1]; for (I=0; I<3; I++) { FD[I] = FD[I]+(DELTA[I]/DELTA3-RHO[I]/RHO3)/W; } } } } } /* Update the perturbations to the end of the timestep. */ RTN += TS; for (I=0; I<3; I++) { W = (FI[I]+FD[I])*GCON2; FT = W*TS; PERP[I] = PERP[I]+(PERV[I]+FT/2.0)*TS; PERV[I] = PERV[I]+FT; PERA[I] = W; } /* Time still to go. */ TLEFT = TSPAN-RTN; /* Is it either time to rectify the orbit or the last time through? */ if (fabs(RTN) >= AGEBEL || FB*TLEFT <= 0.0) { /* Yes: update to the end of the current timestep. */ T0 += RTN; RTN = 0.0; /* The body's unperturbed motion (AU,AU/s). */ palUe2pv(T0,UL,PV0,&J); if (J != 0) goto ABORT; /* Add and re-initialize the perturbations. */ for (I=0; I<3; I++) { J = I+3; PV[I] = PV0[I]+PERP[I]; PV[J] = PV0[J]+PERV[I]/PAL__SPD; PERP[I] = 0.0; PERV[I] = 0.0; PERA[I] = FD[I]*GCON2; } /* Use the position and velocity to set up new universal elements. */ palPv2ue(PV,T0,0.0,UL,&J); if (J != 0) goto ABORT; /* Adjust the timespan and time left. */ TSPAN = TFINAL-T0; TLEFT = TSPAN; } /* Next timestep. */ } /* Return the updated universal-element set. */ for (I=0; I<13; I++) { u[I] = UL[I]; } /* Finished. */ return; /* Miscellaneous numerical error. */ ABORT: *jstat = -1; return; } pal-0.5.0/palPlanel.c000644 000765 000024 00000020206 12366000607 014452 0ustar00timjstaff000000 000000 /* *+ * Name: * palPlanel * Purpose: * Transform conventional elements into position and velocity * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palPlanel ( double date, int jform, double epoch, double orbinc, * double anode, double perih, double aorq, double e, * double aorl, double dm, double pv[6], int *jstat ); * Arguments: * date = double (Given) * Epoch (TT MJD) of osculation (Note 1) * jform = int (Given) * Element set actually returned (1-3; Note 3) * epoch = double (Given) * Epoch of elements (TT MJD) (Note 4) * orbinc = double (Given) * inclination (radians) * anode = double (Given) * longitude of the ascending node (radians) * perih = double (Given) * longitude or argument of perihelion (radians) * aorq = double (Given) * mean distance or perihelion distance (AU) * e = double (Given) * eccentricity * aorl = double (Given) * mean anomaly or longitude (radians, JFORM=1,2 only) * dm = double (Given) * daily motion (radians, JFORM=1 only) * u = double [13] (Returned) * Universal orbital elements (Note 1) * (0) combined mass (M+m) * (1) total energy of the orbit (alpha) * (2) reference (osculating) epoch (t0) * (3-5) position at reference epoch (r0) * (6-8) velocity at reference epoch (v0) * (9) heliocentric distance at reference epoch * (10) r0.v0 * (11) date (t) * (12) universal eccentric anomaly (psi) of date, approx * jstat = int * (Returned) * status: 0 = OK * - -1 = illegal JFORM * - -2 = illegal E * - -3 = illegal AORQ * - -4 = illegal DM * - -5 = numerical error * Description: * Heliocentric position and velocity of a planet, asteroid or comet, * starting from orbital elements. * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - DATE is the instant for which the prediction is required. It is * in the TT timescale (formerly Ephemeris Time, ET) and is a * Modified Julian Date (JD-2400000.5). * - The elements are with respect to the J2000 ecliptic and equinox. * - A choice of three different element-set options is available: * * Option JFORM = 1, suitable for the major planets: * * EPOCH = epoch of elements (TT MJD) * ORBINC = inclination i (radians) * ANODE = longitude of the ascending node, big omega (radians) * PERIH = longitude of perihelion, curly pi (radians) * AORQ = mean distance, a (AU) * E = eccentricity, e (range 0 to <1) * AORL = mean longitude L (radians) * DM = daily motion (radians) * * Option JFORM = 2, suitable for minor planets: * * EPOCH = epoch of elements (TT MJD) * ORBINC = inclination i (radians) * ANODE = longitude of the ascending node, big omega (radians) * PERIH = argument of perihelion, little omega (radians) * AORQ = mean distance, a (AU) * E = eccentricity, e (range 0 to <1) * AORL = mean anomaly M (radians) * * Option JFORM = 3, suitable for comets: * * EPOCH = epoch of elements and perihelion (TT MJD) * ORBINC = inclination i (radians) * ANODE = longitude of the ascending node, big omega (radians) * PERIH = argument of perihelion, little omega (radians) * AORQ = perihelion distance, q (AU) * E = eccentricity, e (range 0 to 10) * * Unused arguments (DM for JFORM=2, AORL and DM for JFORM=3) are not * accessed. * - Each of the three element sets defines an unperturbed heliocentric * orbit. For a given epoch of observation, the position of the body * in its orbit can be predicted from these elements, which are * called "osculating elements", using standard two-body analytical * solutions. However, due to planetary perturbations, a given set * of osculating elements remains usable for only as long as the * unperturbed orbit that it describes is an adequate approximation * to reality. Attached to such a set of elements is a date called * the "osculating epoch", at which the elements are, momentarily, * a perfect representation of the instantaneous position and * velocity of the body. * * Therefore, for any given problem there are up to three different * epochs in play, and it is vital to distinguish clearly between * them: * * . The epoch of observation: the moment in time for which the * position of the body is to be predicted. * * . The epoch defining the position of the body: the moment in time * at which, in the absence of purturbations, the specified * position (mean longitude, mean anomaly, or perihelion) is * reached. * * . The osculating epoch: the moment in time at which the given * elements are correct. * * For the major-planet and minor-planet cases it is usual to make * the epoch that defines the position of the body the same as the * epoch of osculation. Thus, only two different epochs are * involved: the epoch of the elements and the epoch of observation. * * For comets, the epoch of perihelion fixes the position in the * orbit and in general a different epoch of osculation will be * chosen. Thus, all three types of epoch are involved. * * For the present routine: * * . The epoch of observation is the argument DATE. * * . The epoch defining the position of the body is the argument * EPOCH. * * . The osculating epoch is not used and is assumed to be close * enough to the epoch of observation to deliver adequate accuracy. * If not, a preliminary call to sla_PERTEL may be used to update * the element-set (and its associated osculating epoch) by * applying planetary perturbations. * - The reference frame for the result is with respect to the mean * equator and equinox of epoch J2000. * - The algorithm was originally adapted from the EPHSLA program of * D.H.P.Jones (private communication, 1996). The method is based * on Stumpff's Universal Variables. * See Also: * Everhart, E. & Pitkin, E.T., Am.J.Phys. 51, 712, 1983. * History: * 2012-03-12 (TIMJ): * Initial version taken directly from SLA/F. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2002 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" void palPlanel ( double date, int jform, double epoch, double orbinc, double anode, double perih, double aorq, double e, double aorl, double dm, double pv[6], int *jstat ) { int j; double u[13]; /* Validate elements and convert to "universal variables" parameters. */ palEl2ue( date, jform, epoch, orbinc, anode, perih, aorq, e, aorl, dm, u, &j ); /* Determine the position and velocity */ if (j == 0) { palUe2pv( date, u, pv, &j); if (j != 0) j = -5; } /* Wrap up */ *jstat = j; } pal-0.5.0/palPlanet.c000644 000765 000024 00000005443 12366000611 014463 0ustar00timjstaff000000 000000 /* *+ * Name: * palPlanet * Purpose: * Approximate heliocentric position and velocity of major planet * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palPlanet ( double date, int np, double pv[6], int *j ); * Arguments: * date = double (Given) * TDB Modified Julian Date (JD-2400000.5). * np = int (Given) * planet (1=Mercury, 2=Venus, 3=EMB, 4=Mars, * 5=Jupiter, 6=Saturn, 7=Uranus, 8=Neptune) * pv = double [6] (Returned) * heliocentric x,y,z,xdot,ydot,zdot, J2000, equatorial triad * in units AU and AU/s. * j = int * (Returned) * - -2 = solution didn't converge. * - -1 = illegal np (1-8) * - 0 = OK * - +1 = warning: year outside 1000-3000 * Description: * Calculates the approximate heliocentric position and velocity of * the specified major planet. * Authors: * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - See SOFA eraPlan94 for details * - Note that Pluto is supported in SLA/F but not in this routine * - Status -2 is equivalent to eraPlan94 status +2. * - Note that velocity units here match the SLA/F documentation. * History: * 2012-03-07 (TIMJ): * Initial version * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "palmac.h" #include "pal1sofa.h" void palPlanet ( double date, int np, double pv[6], int *j ) { double erapv[2][3]; *j = eraPlan94( PAL__MJD0, date, np, erapv ); /* Convert the outputs to the correct form and also correct AU/d to AU/s */ pv[0] = erapv[0][0]; pv[1] = erapv[0][1]; pv[2] = erapv[0][2]; pv[3] = erapv[1][0] / PAL__SPD; pv[4] = erapv[1][1] / PAL__SPD; pv[5] = erapv[1][2] / PAL__SPD; /* SLA compatibility for status */ if (*j == 2) *j = -2; } pal-0.5.0/palPlante.c000644 000765 000024 00000023624 12366000607 014471 0ustar00timjstaff000000 000000 /* *+ * Name: * palPlante * Purpose: * Topocentric RA,Dec of a Solar-System object from heliocentric orbital elements * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palPlante ( double date, double elong, double phi, int jform, * double epoch, double orbinc, double anode, double perih, * double aorq, double e, double aorl, double dm, * double *ra, double *dec, double *r, int *jstat ); * Description: * Topocentric apparent RA,Dec of a Solar-System object whose * heliocentric orbital elements are known. * Arguments: * date = double (Given) * TT MJD of observation (JD-2400000.5) * elong = double (Given) * Observer's east longitude (radians) * phi = double (Given) * Observer's geodetic latitude (radians) * jform = int (Given) * Element set actually returned (1-3; Note 6) * epoch = double (Given) * Epoch of elements (TT MJD) * orbinc = double (Given) * inclination (radians) * anode = double (Given) * longitude of the ascending node (radians) * perih = double (Given) * longitude or argument of perihelion (radians) * aorq = double (Given) * mean distance or perihelion distance (AU) * e = double (Given) * eccentricity * aorl = double (Given) * mean anomaly or longitude (radians, JFORM=1,2 only) * dm = double (Given) * daily motion (radians, JFORM=1 only) * ra = double * (Returned) * Topocentric apparent RA (radians) * dec = double * (Returned) * Topocentric apparent Dec (radians) * r = double * (Returned) * Distance from observer (AU) * jstat = int * (Returned) * status: 0 = OK * - -1 = illegal jform * - -2 = illegal e * - -3 = illegal aorq * - -4 = illegal dm * - -5 = numerical error * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - DATE is the instant for which the prediction is required. It is * in the TT timescale (formerly Ephemeris Time, ET) and is a * Modified Julian Date (JD-2400000.5). * - The longitude and latitude allow correction for geocentric * parallax. This is usually a small effect, but can become * important for near-Earth asteroids. Geocentric positions can be * generated by appropriate use of routines palEpv (or palEvp) and * palUe2pv. * - The elements are with respect to the J2000 ecliptic and equinox. * - A choice of three different element-set options is available: * * Option JFORM = 1, suitable for the major planets: * * EPOCH = epoch of elements (TT MJD) * ORBINC = inclination i (radians) * ANODE = longitude of the ascending node, big omega (radians) * PERIH = longitude of perihelion, curly pi (radians) * AORQ = mean distance, a (AU) * E = eccentricity, e (range 0 to <1) * AORL = mean longitude L (radians) * DM = daily motion (radians) * * Option JFORM = 2, suitable for minor planets: * * EPOCH = epoch of elements (TT MJD) * ORBINC = inclination i (radians) * ANODE = longitude of the ascending node, big omega (radians) * PERIH = argument of perihelion, little omega (radians) * AORQ = mean distance, a (AU) * E = eccentricity, e (range 0 to <1) * AORL = mean anomaly M (radians) * * Option JFORM = 3, suitable for comets: * * EPOCH = epoch of elements and perihelion (TT MJD) * ORBINC = inclination i (radians) * ANODE = longitude of the ascending node, big omega (radians) * PERIH = argument of perihelion, little omega (radians) * AORQ = perihelion distance, q (AU) * E = eccentricity, e (range 0 to 10) * * Unused arguments (DM for JFORM=2, AORL and DM for JFORM=3) are not * accessed. * - Each of the three element sets defines an unperturbed heliocentric * orbit. For a given epoch of observation, the position of the body * in its orbit can be predicted from these elements, which are * called "osculating elements", using standard two-body analytical * solutions. However, due to planetary perturbations, a given set * of osculating elements remains usable for only as long as the * unperturbed orbit that it describes is an adequate approximation * to reality. Attached to such a set of elements is a date called * the "osculating epoch", at which the elements are, momentarily, * a perfect representation of the instantaneous position and * velocity of the body. * * Therefore, for any given problem there are up to three different * epochs in play, and it is vital to distinguish clearly between * them: * * . The epoch of observation: the moment in time for which the * position of the body is to be predicted. * * . The epoch defining the position of the body: the moment in time * at which, in the absence of purturbations, the specified * position (mean longitude, mean anomaly, or perihelion) is * reached. * * . The osculating epoch: the moment in time at which the given * elements are correct. * * For the major-planet and minor-planet cases it is usual to make * the epoch that defines the position of the body the same as the * epoch of osculation. Thus, only two different epochs are * involved: the epoch of the elements and the epoch of observation. * * For comets, the epoch of perihelion fixes the position in the * orbit and in general a different epoch of osculation will be * chosen. Thus, all three types of epoch are involved. * * For the present routine: * * . The epoch of observation is the argument DATE. * * . The epoch defining the position of the body is the argument * EPOCH. * * . The osculating epoch is not used and is assumed to be close * enough to the epoch of observation to deliver adequate accuracy. * If not, a preliminary call to sla_PERTEL may be used to update * the element-set (and its associated osculating epoch) by * applying planetary perturbations. * - Two important sources for orbital elements are Horizons, operated * by the Jet Propulsion Laboratory, Pasadena, and the Minor Planet * Center, operated by the Center for Astrophysics, Harvard. * * The JPL Horizons elements (heliocentric, J2000 ecliptic and * equinox) correspond to SLALIB arguments as follows. * * Major planets: * * JFORM = 1 * EPOCH = JDCT-2400000.5 * ORBINC = IN (in radians) * ANODE = OM (in radians) * PERIH = OM+W (in radians) * AORQ = A * E = EC * AORL = MA+OM+W (in radians) * DM = N (in radians) * * Epoch of osculation = JDCT-2400000.5 * * Minor planets: * * JFORM = 2 * EPOCH = JDCT-2400000.5 * ORBINC = IN (in radians) * ANODE = OM (in radians) * PERIH = W (in radians) * AORQ = A * E = EC * AORL = MA (in radians) * * Epoch of osculation = JDCT-2400000.5 * * Comets: * * JFORM = 3 * EPOCH = Tp-2400000.5 * ORBINC = IN (in radians) * ANODE = OM (in radians) * PERIH = W (in radians) * AORQ = QR * E = EC * * Epoch of osculation = JDCT-2400000.5 * * The MPC elements correspond to SLALIB arguments as follows. * * Minor planets: * * JFORM = 2 * EPOCH = Epoch-2400000.5 * ORBINC = Incl. (in radians) * ANODE = Node (in radians) * PERIH = Perih. (in radians) * AORQ = a * E = e * AORL = M (in radians) * * Epoch of osculation = Epoch-2400000.5 * * Comets: * * JFORM = 3 * EPOCH = T-2400000.5 * ORBINC = Incl. (in radians) * ANODE = Node. (in radians) * PERIH = Perih. (in radians) * AORQ = q * E = e * * Epoch of osculation = Epoch-2400000.5 * History: * 2012-03-12 (TIMJ): * Initial version direct conversion of SLA/F. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2004 Patrick T. Wallace * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" void palPlante ( double date, double elong, double phi, int jform, double epoch, double orbinc, double anode, double perih, double aorq, double e, double aorl, double dm, double *ra, double *dec, double *r, int *jstat ) { double u[13]; /* Transform conventional elements to universal elements */ palEl2ue( date, jform, epoch, orbinc, anode, perih, aorq, e, aorl, dm, u, jstat ); /* If succcessful, make the prediction */ if (*jstat == 0) palPlantu( date, elong, phi, u, ra, dec, r, jstat ); } pal-0.5.0/palPlantu.c000644 000765 000024 00000013765 12366000611 014511 0ustar00timjstaff000000 000000 /* *+ * Name: * palPlantu * Purpose: * Topocentric RA,Dec of a Solar-System object from universal elements * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palPlantu ( double date, double elong, double phi, const double u[13], * double *ra, double *dec, double *r, int *jstat ) { * Description: * Topocentric apparent RA,Dec of a Solar-System object whose * heliocentric universal elements are known. * Arguments: * date = double (Given) * TT MJD of observation (JD-2400000.5) * elong = double (Given) * Observer's east longitude (radians) * phi = double (Given) * Observer's geodetic latitude (radians) * u = const double [13] (Given) * Universal orbital elements * - (0) combined mass (M+m) * - (1) total energy of the orbit (alpha) * - (2) reference (osculating) epoch (t0) * - (3-5) position at reference epoch (r0) * - (6-8) velocity at reference epoch (v0) * - (9) heliocentric distance at reference epoch * - (10) r0.v0 * - (11) date (t) * - (12) universal eccentric anomaly (psi) of date, approx * ra = double * (Returned) * Topocentric apparent RA (radians) * dec = double * (Returned) * Topocentric apparent Dec (radians) * r = double * (Returned) * Distance from observer (AU) * jstat = int * (Returned) * status: 0 = OK * - -1 = radius vector zero * - -2 = failed to converge * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - DATE is the instant for which the prediction is required. It is * in the TT timescale (formerly Ephemeris Time, ET) and is a * Modified Julian Date (JD-2400000.5). * - The longitude and latitude allow correction for geocentric * parallax. This is usually a small effect, but can become * important for near-Earth asteroids. Geocentric positions can be * generated by appropriate use of routines palEpv (or palEvp) and * palUe2pv. * - The "universal" elements are those which define the orbit for the * purposes of the method of universal variables (see reference 2). * They consist of the combined mass of the two bodies, an epoch, * and the position and velocity vectors (arbitrary reference frame) * at that epoch. The parameter set used here includes also various * quantities that can, in fact, be derived from the other * information. This approach is taken to avoiding unnecessary * computation and loss of accuracy. The supplementary quantities * are (i) alpha, which is proportional to the total energy of the * orbit, (ii) the heliocentric distance at epoch, (iii) the * outwards component of the velocity at the given epoch, (iv) an * estimate of psi, the "universal eccentric anomaly" at a given * date and (v) that date. * - The universal elements are with respect to the J2000 equator and * equinox. * See Also: * - Sterne, Theodore E., "An Introduction to Celestial Mechanics", * Interscience Publishers Inc., 1960. Section 6.7, p199. * - Everhart, E. & Pitkin, E.T., Am.J.Phys. 51, 712, 1983. * History: * 2012-03-12 (TIMJ): * Initial version direct conversion of SLA/F. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2005 Patrick T. Wallace * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include #include "pal.h" #include "palmac.h" #include "pal1sofa.h" void palPlantu ( double date, double elong, double phi, const double u[13], double *ra, double *dec, double *r, int *jstat ) { int i; double dvb[3], dpb[3], vsg[6], vsp[6], v[6], rmat[3][3], vgp[6], stl, vgo[6], dx, dy, dz, d, tl; double ucp[13]; /* To retain the stated const API and conform to the documentation we must copy the contents of the u array as palUe2pv updates the final two elements */ for (i=0;i<13;i++) { ucp[i] = u[i]; } /* Sun to geocentre (J2000, velocity in AU/s) */ palEpv( date, vsg, &(vsg[3]), dpb, dvb ); for (i=3; i < 6; i++) { vsg[i] /= PAL__SPD; } /* Sun to planet (J2000) */ palUe2pv( date, ucp, vsp, jstat ); /* Geocentre to planet (J2000) */ for (i=0; i<6; i++) { v[i] = vsp[i] - vsg[i]; } /* Precession and nutation to date */ palPrenut( 2000.0, date, rmat ); eraRxp(rmat, v, vgp); eraRxp( rmat, &(v[3]), &(vgp[3]) ); /* Geocentre to observer (date) */ stl = palGmst( date - palDt( palEpj(date) ) / PAL__SPD ) + elong; palPvobs( phi, 0.0, stl, vgo ); /* Observer to planet (date) */ for (i=0; i<6; i++) { v[i] = vgp[i] - vgo[i]; } /* Geometric distance (AU) */ dx = v[0]; dy = v[1]; dz = v[2]; d = sqrt( dx*dx + dy*dy + dz*dz ); /* Light time (sec) */ tl = PAL__CR * d; /* Correct position for planetary aberration */ for (i=0; i<3; i++) { v[i] -= tl * v[i+3]; } /* To RA,Dec */ eraC2s( v, ra, dec ); *ra = eraAnp( *ra ); *r = d; } pal-0.5.0/palPm.c000644 000765 000024 00000006265 12366000611 013617 0ustar00timjstaff000000 000000 /* *+ * Name: * palPm * Purpose: * Apply corrections for proper motion a star RA,Dec * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palPm ( double r0, double d0, double pr, double pd, * double px, double rv, double ep0, double ep1, * double *r1, double *d1 ); * Arguments: * r0 = double (Given) * RA at epoch ep0 (radians) * d0 = double (Given) * Dec at epoch ep0 (radians) * pr = double (Given) * RA proper motion in radians per year. * pd = double (Given) * Dec proper motion in radians per year. * px = double (Given) * Parallax (arcsec) * rv = double (Given) * Radial velocity (km/sec +ve if receding) * ep0 = double (Given) * Start epoch in years, assumed to be Julian. * ep1 = double (Given) * End epoch in years, assumed to be Julian. * r1 = double * (Returned) * RA at epoch ep1 (radians) * d1 = double * (Returned) * Dec at epoch ep1 (radians) * Description: * Apply corrections for proper motion to a star RA,Dec using the * SOFA routine eraStarpm. * Authors: * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - Uses eraStarpm but ignores the status returns from that routine. * In particular note that parallax should not be zero when the * proper motions are non-zero. SLA/F allows parallax to be zero. * - Assumes all epochs are Julian epochs. * History: * 2012-03-02 (TIMJ): * Initial version * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "pal1sofa.h" void palPm ( double r0, double d0, double pr, double pd, double px, double rv, double ep0, double ep1, double *r1, double *d1 ) { int status; double ep1a, ep1b, ep2a, ep2b; double pmr2, pmd2, px2, rv2; /* SOFA requires the epochs in TDB MJD so we have to assume that the supplied epochs are Julian years */ eraEpj2jd( ep0, &ep1a, &ep1b ); eraEpj2jd( ep1, &ep2a, &ep2b ); status = eraStarpm( r0, d0, pr, pd, px, rv, ep1a, ep1b, ep2a, ep2b, r1, d1, &pmr2, &pmd2, &px2, &rv2 ); } pal-0.5.0/palPrebn.c000644 000765 000024 00000005533 12366000607 014313 0ustar00timjstaff000000 000000 /* *+ * Name: * palPrebn * Purpose: * Generate the matrix of precession between two objects (old) * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palPrebn ( double bep0, double bep1, double rmatp[3][3] ); * Arguments: * bep0 = double (Given) * Beginning Besselian epoch. * bep1 = double (Given) * Ending Besselian epoch * rmatp = double[3][3] (Returned) * precession matrix in the sense V(BEP1) = RMATP * V(BEP0) * Description: * Generate the matrix of precession between two epochs, * using the old, pre-IAU1976, Bessel-Newcomb model, using * Kinoshita's formulation * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * See Also: * Kinoshita, H. (1975) 'Formulas for precession', SAO Special * Report No. 364, Smithsonian Institution Astrophysical * Observatory, Cambridge, Massachusetts. * History: * 2012-02-12(TIMJ): * Initial version with documentation taken from Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1996 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "palmac.h" void palPrebn ( double bep0, double bep1, double rmatp[3][3] ) { double t,bigt, zeta, theta, z, tas2r, w; /* Interval between basic epoch B1850.0 and beginning epoch in TC */ bigt = (bep0-1850)/100.; /* Interval over which precession required, in tropical centuries */ t = (bep1-bep0)/100.; /* Euler angles */ tas2r = t * PAL__DAS2R; w = 2303.5548 + ( 1.39720 + 0.000059 * bigt) * bigt; zeta = ( w + ( 0.30242 - 0.000269 * bigt + 0.017996 * t ) * t ) * tas2r; z = ( w + ( 1.09478 + 0.000387 * bigt + 0.018324 * t ) * t ) * tas2r; theta = ( 2005.1125 + ( -0.85294 - 0.000365 * bigt ) * bigt + (-0.42647 - 0.000365 * bigt - 0.041802 * t ) * t ) * tas2r; /* Rotation matrix */ palDeuler("ZYZ", -zeta, theta, -z, rmatp); } pal-0.5.0/palPrec.c000644 000765 000024 00000006051 12366000611 014125 0ustar00timjstaff000000 000000 /* *+ * Name: * palPrec * Purpose: * Form the matrix of precession between two epochs (IAU 2006) * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * palPrec( double ep0, double ep1, double rmatp[3][3] ) * Arguments: * ep0 = double (Given) * Beginning epoch * ep1 = double (Given) * Ending epoch * rmatp = double[3][3] (Returned) * Precession matrix * Description: * The IAU 2006 precession matrix from ep0 to ep1 is found and * returned. The matrix is in the sense V(EP1) = RMATP * V(EP0). * The epochs are TDB (loosely TT) Julian epochs. * * Though the matrix method itself is rigorous, the precession * angles are expressed through canonical polynomials which are * valid only for a limited time span of a few hundred years around * the current epoch. * Authors: * PTW: Pat Wallace (STFC) * DSB: David Berry (JAC, Hawaii) * {enter_new_authors_here} * History: * 2012-02-10 (DSB): * Initial version with documentation taken from Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1996 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "pal1sofa.h" void palPrec( double ep0, double ep1, double rmatp[3][3] ){ /* Local Variables: */ double rmatq[3][3]; double ep0_days; double ep1_days; /* Convert supplied dates to days since J2000 */ ep0_days = ( ep0 - 2000.0 )*ERFA_DJY; ep1_days = ( ep1 - 2000.0 )*ERFA_DJY; /* If beginning epoch is J2000, just return the rotation matrix from J2000 to EP1. */ if( ep0 == 2000.0 ) { eraPmat06( ERFA_DJ00, ep1_days, rmatp ); /* If end epoch is J2000, get the rotation matrix from J2000 to EP0 and then transpose it to get the rotation matrix from EP0 to J2000. */ } else if( ep1 == 2000.0 ) { eraPmat06( ERFA_DJ00, ep0_days, rmatp ); eraTr( rmatp, rmatp ); /* Otherwise. get the two matrices used above and multiply them together. */ } else { eraPmat06( ERFA_DJ00, ep0_days, rmatp ); eraTr( rmatp, rmatp ); eraPmat06( ERFA_DJ00, ep1_days, rmatq ); eraRxr( rmatp, rmatq, rmatp ); } } pal-0.5.0/palPreces.c000644 000765 000024 00000006641 12366000611 014462 0ustar00timjstaff000000 000000 /* *+ * Name: * palPreces * Purpose: * Precession - either FK4 or FK5 as required. * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palPreces ( const char sys[3], double ep0, double ep1, * double *ra, double *dc ); * Arguments: * sys = const char [3] (Given) * Precession to be applied: FK4 or FK5. Case insensitive. * ep0 = double (Given) * Starting epoch. * ep1 = double (Given) * Ending epoch * ra = double * (Given & Returned) * On input the RA mean equator & equinox at epoch ep0. On exit * the RA mean equator & equinox of epoch ep1. * dec = double * (Given & Returned) * On input the dec mean equator & equinox at epoch ep0. On exit * the dec mean equator & equinox of epoch ep1. * Description: * Precess coordinates using the appropriate system and epochs. * Authors: * PTW: Patrick T. Wallace * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - Uses palPrec for FK5 data and palPrebn for FK4 data. * - The epochs are Besselian if SYSTEM='FK4' and Julian if 'FK5'. * For example, to precess coordinates in the old system from * equinox 1900.0 to 1950.0 the call would be: * palPreces( "FK4", 1900.0, 1950.0, &ra, &dc ); * - This routine will NOT correctly convert between the old and * the new systems - for example conversion from B1950 to J2000. * For these purposes see palFk425, palFk524, palFk45z and * palFk54z. * - If an invalid SYSTEM is supplied, values of -99D0,-99D0 will * be returned for both RA and DC. * History: * 2012-03-02 (TIMJ): * Initial version * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1995 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "pal1sofa.h" #include void palPreces ( const char sys[3], double ep0, double ep1, double *ra, double *dc ) { double pm[3][3]; double v1[3]; double v2[3]; /* Generate appropriate precession matrix */ if ( strncasecmp( "FK4", sys, 3 ) == 0 ) { palPrebn( ep0, ep1, pm ); } else if (strncasecmp( "FK5", sys, 3 ) == 0 ) { palPrec( ep0, ep1, pm ); } else { *ra = -99.0; *dc = -99.0; return; } /* Convert RA,Dec to x,y,z */ eraS2c( *ra, *dc, v1 ); /* Precess */ eraRxp( pm, v1, v2 ); /* Back to RA,Dec */ eraC2s( v2, ra, dc ); *ra = eraAnp( *ra ); } pal-0.5.0/palPrenut.c000644 000765 000024 00000005444 12366000611 014516 0ustar00timjstaff000000 000000 /* *+ * Name: * palPrenut * Purpose: * Form the matrix of bias-precession-nutation (IAU 2006/2000A) * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palPrenut( double epoch, double date, double rmatpn[3][3] ) * Arguments: * epoch = double (Returned) * Julian epoch for mean coordinates. * date = double (Returned) * Modified Julian Date (JD-2400000.5) for true coordinates. * rmatpn = double[3][3] (Returned) * combined NPB matrix * Description: * Form the matrix of bias-precession-nutation (IAU 2006/2000A). * The epoch and date are TT (but TDB is usually close enough). * The matrix is in the sense v(true) = rmatpn * v(mean). * Authors: * PTW: Pat Wallace (STFC) * {enter_new_authors_here} * History: * 2012-02-10 (PTW): * Initial version. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "palmac.h" #include "pal1sofa.h" void palPrenut ( double epoch, double date, double rmatpn[3][3] ){ /* Local Variables: */ double bpa; double bpia; double bqa; double chia; double d1; double d2; double eps0; double epsa; double gam; double oma; double pa; double phi; double pia; double psi; double psia; double r1[3][3]; double r2[3][3]; double thetaa; double za; double zetaa; /* Specified Julian epoch as a 2-part JD. */ eraEpj2jd( epoch, &d1, &d2 ); /* P matrix, from specified epoch to J2000.0. */ eraP06e( d1, d2, &eps0, &psia, &oma, &bpa, &bqa, &pia, &bpia, &epsa, &chia, &za, &zetaa, &thetaa, &pa, &gam, &phi, &psi ); eraIr( r1 ); eraRz( -chia, r1 ); eraRx( oma, r1 ); eraRz( psia, r1 ); eraRx( -eps0, r1 ); /* NPB matrix, from J2000.0 to date. */ eraPnm06a( PAL__MJD0, date, r2 ); /* NPB matrix, from specified epoch to date. */ eraRxr( r2, r1, rmatpn ); } pal-0.5.0/palPv2el.c000644 000765 000024 00000027424 12366000611 014233 0ustar00timjstaff000000 000000 /* *+ * Name: * palPv2el * Purpose: * Position velocity to heliocentirc osculating elements * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palPv2el ( const double pv[6], double date, double pmass, int jformr, * int *jform, double *epoch, double *orbinc, * double *anode, double *perih, double *aorq, double *e, * double *aorl, double *dm, int *jstat ); * Arguments: * pv = const double [6] (Given) * Heliocentric x,y,z,xdot,ydot,zdot of date, * J2000 equatorial triad (AU,AU/s; Note 1) * date = double (Given) * Date (TT Modified Julian Date = JD-2400000.5) * pmass = double (Given) * Mass of the planet (Sun=1; Note 2) * jformr = int (Given) * Requested element set (1-3; Note 3) * jform = int * (Returned) * Element set actually returned (1-3; Note 4) * epoch = double * (Returned) * Epoch of elements (TT MJD) * orbinc = double * (Returned) * inclination (radians) * anode = double * (Returned) * longitude of the ascending node (radians) * perih = double * (Returned) * longitude or argument of perihelion (radians) * aorq = double * (Returned) * mean distance or perihelion distance (AU) * e = double * (Returned) * eccentricity * aorl = double * (Returned) * mean anomaly or longitude (radians, JFORM=1,2 only) * dm = double * (Returned) * daily motion (radians, JFORM=1 only) * jstat = int * (Returned) * status: 0 = OK * - -1 = illegal PMASS * - -2 = illegal JFORMR * - -3 = position/velocity out of range * Description: * Heliocentric osculating elements obtained from instantaneous position * and velocity. * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - The PV 6-vector is with respect to the mean equator and equinox of * epoch J2000. The orbital elements produced are with respect to * the J2000 ecliptic and mean equinox. * - The mass, PMASS, is important only for the larger planets. For * most purposes (e.g. asteroids) use 0D0. Values less than zero * are illegal. * - Three different element-format options are supported: * * Option JFORM=1, suitable for the major planets: * * EPOCH = epoch of elements (TT MJD) * ORBINC = inclination i (radians) * ANODE = longitude of the ascending node, big omega (radians) * PERIH = longitude of perihelion, curly pi (radians) * AORQ = mean distance, a (AU) * E = eccentricity, e * AORL = mean longitude L (radians) * DM = daily motion (radians) * * Option JFORM=2, suitable for minor planets: * * EPOCH = epoch of elements (TT MJD) * ORBINC = inclination i (radians) * ANODE = longitude of the ascending node, big omega (radians) * PERIH = argument of perihelion, little omega (radians) * AORQ = mean distance, a (AU) * E = eccentricity, e * AORL = mean anomaly M (radians) * * Option JFORM=3, suitable for comets: * * EPOCH = epoch of perihelion (TT MJD) * ORBINC = inclination i (radians) * ANODE = longitude of the ascending node, big omega (radians) * PERIH = argument of perihelion, little omega (radians) * AORQ = perihelion distance, q (AU) * E = eccentricity, e * * - It may not be possible to generate elements in the form * requested through JFORMR. The caller is notified of the form * of elements actually returned by means of the JFORM argument: * JFORMR JFORM meaning * * 1 1 OK - elements are in the requested format * 1 2 never happens * 1 3 orbit not elliptical * * 2 1 never happens * 2 2 OK - elements are in the requested format * 2 3 orbit not elliptical * * 3 1 never happens * 3 2 never happens * 3 3 OK - elements are in the requested format * * - The arguments returned for each value of JFORM (cf Note 5: JFORM * may not be the same as JFORMR) are as follows: * * JFORM 1 2 3 * EPOCH t0 t0 T * ORBINC i i i * ANODE Omega Omega Omega * PERIH curly pi omega omega * AORQ a a q * E e e e * AORL L M - * DM n - - * * where: * * t0 is the epoch of the elements (MJD, TT) * T " epoch of perihelion (MJD, TT) * i " inclination (radians) * Omega " longitude of the ascending node (radians) * curly pi " longitude of perihelion (radians) * omega " argument of perihelion (radians) * a " mean distance (AU) * q " perihelion distance (AU) * e " eccentricity * L " longitude (radians, 0-2pi) * M " mean anomaly (radians, 0-2pi) * n " daily motion (radians) * - means no value is set * * - At very small inclinations, the longitude of the ascending node * ANODE becomes indeterminate and under some circumstances may be * set arbitrarily to zero. Similarly, if the orbit is close to * circular, the true anomaly becomes indeterminate and under some * circumstances may be set arbitrarily to zero. In such cases, * the other elements are automatically adjusted to compensate, * and so the elements remain a valid description of the orbit. * - The osculating epoch for the returned elements is the argument * DATE. * * - Reference: Sterne, Theodore E., "An Introduction to Celestial * Mechanics", Interscience Publishers, 1960 * History: * 2012-03-09 (TIMJ): * Initial version converted from SLA/F. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2005 Patrick T. Wallace * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include #include "pal1sofa.h" #include "pal.h" #include "palmac.h" void palPv2el ( const double pv[6], double date, double pmass, int jformr, int *jform, double *epoch, double *orbinc, double *anode, double *perih, double *aorq, double *e, double *aorl, double *dm, int *jstat ) { /* Sin and cos of J2000 mean obliquity (IAU 1976) */ const double SE = 0.3977771559319137; const double CE = 0.9174820620691818; /* Minimum allowed distance (AU) and speed (AU/day) */ const double RMIN = 1e-3; const double VMIN = 1e-8; /* How close to unity the eccentricity has to be to call it a parabola */ const double PARAB = 1.0e-8; double X,Y,Z,XD,YD,ZD,R,V2,V,RDV,GMU,HX,HY,HZ, HX2PY2,H2,H,OI,BIGOM,AR,ECC,S,C,AT,U,OM, GAR3,EM1,EP1,HAT,SHAT,CHAT,AE,AM,DN,PL, EL,Q,TP,THAT,THHF,F; int JF; /* Validate arguments PMASS and JFORMR.*/ if (pmass < 0.0) { *jstat = -1; return; } if (jformr < 1 || jformr > 3) { *jstat = -2; return; } /* Provisionally assume the elements will be in the chosen form. */ JF = jformr; /* Rotate the position from equatorial to ecliptic coordinates. */ X = pv[0]; Y = pv[1]*CE+pv[2]*SE; Z = -pv[1]*SE+pv[2]*CE; /* Rotate the velocity similarly, scaling to AU/day. */ XD = PAL__SPD*pv[3]; YD = PAL__SPD*(pv[4]*CE+pv[5]*SE); ZD = PAL__SPD*(-pv[4]*SE+pv[5]*CE); /* Distance and speed. */ R = sqrt(X*X+Y*Y+Z*Z); V2 = XD*XD+YD*YD+ZD*ZD; V = sqrt(V2); /* Reject unreasonably small values. */ if (R < RMIN || V < VMIN) { *jstat = -3; return; } /* R dot V. */ RDV = X*XD+Y*YD+Z*ZD; /* Mu. */ GMU = (1.0+pmass)*PAL__GCON*PAL__GCON; /* Vector angular momentum per unit reduced mass. */ HX = Y*ZD-Z*YD; HY = Z*XD-X*ZD; HZ = X*YD-Y*XD; /* Areal constant. */ HX2PY2 = HX*HX+HY*HY; H2 = HX2PY2+HZ*HZ; H = sqrt(H2); /* Inclination. */ OI = atan2(sqrt(HX2PY2),HZ); /* Longitude of ascending node. */ if (HX != 0.0 || HY != 0.0) { BIGOM = atan2(HX,-HY); } else { BIGOM=0.0; } /* Reciprocal of mean distance etc. */ AR = 2.0/R-V2/GMU; /* Eccentricity. */ ECC = sqrt(DMAX(1.0-AR*H2/GMU,0.0)); /* True anomaly. */ S = H*RDV; C = H2-R*GMU; if (S != 0.0 || C != 0.0) { AT = atan2(S,C); } else { AT = 0.0; } /* Argument of the latitude. */ S = sin(BIGOM); C = cos(BIGOM); U = atan2((-X*S+Y*C)*cos(OI)+Z*sin(OI),X*C+Y*S); /* Argument of perihelion. */ OM = U-AT; /* Capture near-parabolic cases. */ if (fabs(ECC-1.0) < PARAB) ECC=1.0; /* Comply with JFORMR = 1 or 2 only if orbit is elliptical. */ if (ECC > 1.0) JF=3; /* Functions. */ GAR3 = GMU*AR*AR*AR; EM1 = ECC-1.0; EP1 = ECC+1.0; HAT = AT/2.0; SHAT = sin(HAT); CHAT = cos(HAT); /* Variable initializations to avoid compiler warnings. */ AM = 0.0; DN = 0.0; PL = 0.0; EL = 0.0; Q = 0.0; TP = 0.0; /* Ellipse? */ if (ECC < 1.0 ) { /* Eccentric anomaly. */ AE = 2.0*atan2(sqrt(-EM1)*SHAT,sqrt(EP1)*CHAT); /* Mean anomaly. */ AM = AE-ECC*sin(AE); /* Daily motion. */ DN = sqrt(GAR3); } /* "Major planet" element set? */ if (JF == 1) { /* Longitude of perihelion. */ PL = BIGOM+OM; /* Longitude at epoch. */ EL = PL+AM; } /* "Comet" element set? */ if (JF == 3) { /* Perihelion distance. */ Q = H2/(GMU*EP1); /* Ellipse, parabola, hyperbola? */ if (ECC < 1.0) { /* Ellipse: epoch of perihelion. */ TP = date-AM/DN; } else { /* Parabola or hyperbola: evaluate tan ( ( true anomaly ) / 2 ) */ THAT = SHAT/CHAT; if (ECC == 1.0) { /* Parabola: epoch of perihelion. */ TP = date-THAT*(1.0+THAT*THAT/3.0)*H*H2/(2.0*GMU*GMU); } else { /* Hyperbola: epoch of perihelion. */ THHF = sqrt(EM1/EP1)*THAT; F = log(1.0+THHF)-log(1.0-THHF); TP = date-(ECC*sinh(F)-F)/sqrt(-GAR3); } } } /* Return the appropriate set of elements. */ *jform = JF; *orbinc = OI; *anode = eraAnp(BIGOM); *e = ECC; if (JF == 1) { *perih = eraAnp(PL); *aorl = eraAnp(EL); *dm = DN; } else { *perih = eraAnp(OM); if (JF == 2) *aorl = eraAnp(AM); } if (JF != 3) { *epoch = date; *aorq = 1.0/AR; } else { *epoch = TP; *aorq = Q; } *jstat = 0; } pal-0.5.0/palPv2ue.c000644 000765 000024 00000012530 12366000607 014241 0ustar00timjstaff000000 000000 /* *+ * Name: * palPv2ue * Purpose: * Universal elements to position and velocity. * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palPv2ue( const double pv[6], double date, double pmass, * double u[13], int * jstat ); * Arguments: * pv = double [6] (Given) * Heliocentric x,y,z,xdot,ydot,zdot of date, (AU,AU/s; Note 1) * date = double (Given) * Date (TT modified Julian Date = JD-2400000.5) * pmass = double (Given) * Mass of the planet (Sun=1; note 2) * u = double [13] (Returned) * Universal orbital elements (Note 3) * * - (0) combined mass (M+m) * - (1) total energy of the orbit (alpha) * - (2) reference (osculating) epoch (t0) * - (3-5) position at reference epoch (r0) * - (6-8) velocity at reference epoch (v0) * - (9) heliocentric distance at reference epoch * - (10) r0.v0 * - (11) date (t) * - (12) universal eccentric anomaly (psi) of date, approx * jstat = int * (Returned) * status: 0 = OK * - -1 = illegal PMASS * - -2 = too close to Sun * - -3 = too slow * Description: * Construct a universal element set based on an instantaneous position * and velocity. * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - The PV 6-vector can be with respect to any chosen inertial frame, * and the resulting universal-element set will be with respect to * the same frame. A common choice will be mean equator and ecliptic * of epoch J2000. * - The mass, PMASS, is important only for the larger planets. For * most purposes (e.g. asteroids) use 0D0. Values less than zero * are illegal. * - The "universal" elements are those which define the orbit for the * purposes of the method of universal variables (see reference). * They consist of the combined mass of the two bodies, an epoch, * and the position and velocity vectors (arbitrary reference frame) * at that epoch. The parameter set used here includes also various * quantities that can, in fact, be derived from the other * information. This approach is taken to avoiding unnecessary * computation and loss of accuracy. The supplementary quantities * are (i) alpha, which is proportional to the total energy of the * orbit, (ii) the heliocentric distance at epoch, (iii) the * outwards component of the velocity at the given epoch, (iv) an * estimate of psi, the "universal eccentric anomaly" at a given * date and (v) that date. * - Reference: Everhart, E. & Pitkin, E.T., Am.J.Phys. 51, 712, 1983. * History: * 2012-03-09 (TIMJ): * Initial version from the SLA/F implementation. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1999 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include #include "pal.h" #include "palmac.h" void palPv2ue( const double pv[6], double date, double pmass, double u[13], int * jstat ) { /* Canonical days to seconds */ const double CD2S = PAL__GCON / PAL__SPD; /* Minimum allowed distance (AU) and speed (AU per canonical day) */ const double RMIN = 1e-3; const double VMIN = 1e-3; double T0,CM,X,Y,Z,XD,YD,ZD,R,V2,V,ALPHA,RDV; /* Reference epoch. */ T0 = date; /* Combined mass (mu=M+m). */ if (pmass < 0.0 ) { /* Negative planet mass */ *jstat = -1; return; } CM = 1.0+pmass; /* Unpack the state vector, expressing velocity in AU per canonical day. */ X = pv[0]; Y = pv[1]; Z = pv[2]; XD = pv[3]/CD2S; YD = pv[4]/CD2S; ZD = pv[5]/CD2S; /* Heliocentric distance, and speed. */ R = sqrt(X*X+Y*Y+Z*Z); V2 = XD*XD+YD*YD+ZD*ZD; V = sqrt(V2); /* Reject unreasonably small values. */ if (R < RMIN) { /* Too close */ *jstat = -2; return; } if (V < VMIN) { /* Too slow */ *jstat = -3; return; } /* Total energy of the orbit. */ ALPHA = V2-2.0*CM/R; /* Outward component of velocity. */ RDV = X*XD+Y*YD+Z*ZD; /* Construct the universal-element set. */ u[0] = CM; u[1] = ALPHA; u[2] = T0; u[3] = X; u[4] = Y; u[5] = Z; u[6] = XD; u[7] = YD; u[8] = ZD; u[9] = R; u[10] = RDV; u[11] = T0; u[12] = 0.0; *jstat = 0; return; } pal-0.5.0/palPvobs.c000644 000765 000024 00000005077 12366000653 014342 0ustar00timjstaff000000 000000 /* *+ * Name: * palPvobs * Purpose: * Position and velocity of an observing station. * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * palPvobs( double p, double h, double stl, double pv[6] ) * Arguments: * p = double (Given) * Latitude (geodetic, radians). * h = double (Given) * Height above reference spheroid (geodetic, metres). * stl = double (Given) * Local apparent sidereal time (radians). * pv = double[ 6 ] (Returned) * position/velocity 6-vector (AU, AU/s, true equator * and equinox of date). * Description: * Returns the position and velocity of an observing station. * Notes: * - The WGS84 reference ellipsoid is used. * Authors: * PTW: Pat Wallace (STFC) * DSB: David Berry (JAC, Hawaii) * {enter_new_authors_here} * History: * 2012-02-16 (DSB): * Initial version. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1995 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "palmac.h" #include "palmac.h" #include "pal1sofa.h" void palPvobs( double p, double h, double stl, double pv[6] ){ /* Local Variables: */ double xyz[3], z, r, s, c, v; /* Geodetic to geocentric conversion (WGS84 reference ellipsoid). */ eraGd2gc( ERFA_WGS84, 0.0, p, h, xyz ); /* Convert from metres to AU */ r = xyz[ 0 ]/ERFA_DAU; z = xyz[ 2 ]/ERFA_DAU; /* Functions of ST. */ s = sin( stl ); c = cos( stl ); /* Speed. */ v = PAL__SR*r; /* Position. */ pv[ 0 ] = r*c; pv[ 1 ] = r*s; pv[ 2 ] = z; /* Velocity. */ pv[ 3 ] = -v*s; pv[ 4 ] = v*c; pv[ 5 ] = 0.0; } pal-0.5.0/palRdplan.c000644 000765 000024 00000012733 12366000611 014460 0ustar00timjstaff000000 000000 /* *+ * Name: * palRdplan * Purpose: * Approximate topocentric apparent RA,Dec of a planet * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palRdplan( double date, int np, double elong, double phi, * double * ra, double * dec, double * diam ); * Arguments: * date = double (Given) * MJD of observation (JD-2400000.5) in TDB. For all practical * purposes TT can be used instead of TDB, and for many applications * UT will do (except for the Moon). * np = int (Given) * Planet: 1 = Mercury * 2 = Venus * 3 = Moon * 4 = Mars * 5 = Jupiter * 6 = Saturn * 7 = Uranus * 8 = Neptune * else = Sun * elong = double (Given) * Observer's east longitude (radians) * phi = double (Given) * Observer's geodetic latitude (radians) * ra = double * (Returned) * RA (topocentric apparent, radians) * dec = double * (Returned) * Dec (topocentric apparent, radians) * diam = double * (Returned) * Angular diameter (equatorial, radians) * Description: * Approximate topocentric apparent RA,Dec of a planet, and its * angular diameter. * Authors: * PTW: Patrick T. Wallace * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - Unlike with slaRdplan, Pluto is not supported. * - The longitude and latitude allow correction for geocentric * parallax. This is a major effect for the Moon, but in the * context of the limited accuracy of the present routine its * effect on planetary positions is small (negligible for the * outer planets). Geocentric positions can be generated by * appropriate use of the routines palDmoon and eraPlan94. * History: * 2012-03-07 (TIMJ): * Initial version, with some documentation from SLA/F. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1997 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include #include "pal.h" #include "palmac.h" #include "pal1sofa.h" void palRdplan( double date, int np, double elong, double phi, double * ra, double * dec, double * diam ) { /* AU in km */ const double AUKM = 1.49597870e8; /* Equatorial radii (km) */ const double EQRAU[] = { 696000.0, /* Sun */ 2439.7, 6051.9, 1738, 3397, 71492, 60268, 25559, 24764 }; /* Local variables */ int i, j; double stl; double vgm[6]; double v[6]; double rmat[3][3]; double vse[6]; double vsg[6]; double vsp[6]; double vgo[6]; double dx,dy,dz,r,tl; /* Classify np */ if (np < 0 || np > 8 ) np=0; /* Sun */ /* Approximate local sidereal time */ stl = palGmst( date - palDt( palEpj(date)) / 86400.0) + elong; /* Geocentre to Moon (mean of date) */ palDmoon( date, v ); /* Nutation to true of date */ palNut( date, rmat ); eraRxp( rmat, v, vgm ); eraRxp( rmat, &(v[3]), &(vgm[3]) ); /* Moon? */ if (np == 3) { /* geocentre to Moon (true of date) */ for (i=0; i<6; i++) { v[i] = vgm[i]; } } else { /* Not moon: precession/nutation matrix J2000 to date */ palPrenut( 2000.0, date, rmat ); /* Sun to Earth-Moon Barycentre (J2000) */ palPlanet( date, 3, v, &j ); /* Precession and nutation to date */ eraRxp( rmat, v, vse ); eraRxp( rmat, &(v[3]), &(vse[3]) ); /* Sun to geocentre (true of date) */ for (i=0; i<6; i++) { vsg[i] = vse[i] - 0.012150581 * vgm[i]; } /* Sun ? */ if (np == 0) { /* Geocentre to Sun */ for (i=0; i<6; i++) { v[i] = -vsg[i]; } } else { /* Sun to Planet (J2000) */ palPlanet( date, np, v, &j ); /* Precession and nutation to date */ eraRxp( rmat, v, vsp ); eraRxp( rmat, &(v[3]), &(vsp[3]) ); /* Geocentre to planet */ for (i=0; i<6; i++) { v[i] = vsp[i] - vsg[i]; } } } /* Refer to origina at the observer */ palPvobs( phi, 0.0, stl, vgo ); for (i=0; i<6; i++) { v[i] -= vgo[i]; } /* Geometric distance (AU) */ dx = v[0]; dy = v[1]; dz = v[2]; r = sqrt( dx*dx + dy*dy + dz*dz ); /* Light time */ tl = PAL__CR * r; /* Correct position for planetary aberration */ for (i=0; i<3; i++) { v[i] -= tl * v[i+3]; } /* To RA,Dec */ eraC2s( v, ra, dec ); *ra = eraAnp( *ra ); /* Angular diameter (radians) */ *diam = 2.0 * asin( EQRAU[np] / (r * AUKM ) ); } pal-0.5.0/palRefco.c000644 000765 000024 00000007617 12366000607 014310 0ustar00timjstaff000000 000000 /* *+ * Name: * palRefco * Purpose: * Determine constants in atmospheric refraction model * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palRefco ( double hm, double tdk, double pmb, double rh, * double wl, double phi, double tlr, double eps, * double *refa, double *refb ); * Arguments: * hm = double (Given) * Height of the observer above sea level (metre) * tdk = double (Given) * Ambient temperature at the observer (K) * pmb = double (Given) * Pressure at the observer (millibar) * rh = double (Given) * Relative humidity at the observer (range 0-1) * wl = double (Given) * Effective wavelength of the source (micrometre) * phi = double (Given) * Latitude of the observer (radian, astronomical) * tlr = double (Given) * Temperature lapse rate in the troposphere (K/metre) * eps = double (Given) * Precision required to terminate iteration (radian) * refa = double * (Returned) * tan Z coefficient (radian) * refb = double * (Returned) * tan**3 Z coefficient (radian) * Description: * Determine the constants A and B in the atmospheric refraction * model dZ = A tan Z + B tan**3 Z. * * Z is the "observed" zenith distance (i.e. affected by refraction) * and dZ is what to add to Z to give the "topocentric" (i.e. in vacuo) * zenith distance. * Authors: * PTW: Patrick T. Wallace * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - Typical values for the TLR and EPS arguments might be 0.0065 and * 1E-10 respectively. * * - The radio refraction is chosen by specifying WL > 100 micrometres. * * - The routine is a slower but more accurate alternative to the * palRefcoq routine. The constants it produces give perfect * agreement with palRefro at zenith distances arctan(1) (45 deg) * and arctan(4) (about 76 deg). It achieves 0.5 arcsec accuracy * for ZD < 80 deg, 0.01 arcsec accuracy for ZD < 60 deg, and * 0.001 arcsec accuracy for ZD < 45 deg. * History: * 2012-08-24 (TIMJ): * Initial version. A direct copy of the Fortran SLA implementation. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2004 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" void palRefco ( double hm, double tdk, double pmb, double rh, double wl, double phi, double tlr, double eps, double *refa, double *refb ) { double r1, r2; /* Sample zenith distances: arctan(1) and arctan(4) */ const double ATN1 = 0.7853981633974483; const double ATN4 = 1.325817663668033; /* Determine refraction for the two sample zenith distances */ palRefro(ATN1,hm,tdk,pmb,rh,wl,phi,tlr,eps,&r1); palRefro(ATN4,hm,tdk,pmb,rh,wl,phi,tlr,eps,&r2); /* Solve for refraction constants */ *refa = (64.0*r1-r2)/60.0; *refb = (r2-4.0*r1)/60.0; } pal-0.5.0/palRefro.c000644 000765 000024 00000033713 12366000607 014323 0ustar00timjstaff000000 000000 /* *+ * Name: * palRefro * Purpose: * Atmospheric refraction for radio and optical/IR wavelengths * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palRefro( double zobs, double hm, double tdk, double pmb, double rh, double wl, double phi, double tlr, double eps, double * ref ) { * Arguments: * zobs = double (Given) * Observed zenith distance of the source (radian) * hm = double (Given) * Height of the observer above sea level (metre) * tdk = double (Given) * Ambient temperature at the observer (K) * pmb = double (Given) * Pressure at the observer (millibar) * rh = double (Given) * Relative humidity at the observer (range 0-1) * wl = double (Given) * Effective wavelength of the source (micrometre) * phi = double (Given) * Latitude of the observer (radian, astronomical) * tlr = double (Given) * Temperature lapse rate in the troposphere (K/metre) * eps = double (Given) * Precision required to terminate iteration (radian) * ref = double * (Returned) * Refraction: in vacuao ZD minus observed ZD (radian) * Description: * Calculates the atmospheric refraction for radio and optical/IR * wavelengths. * Authors: * PTW: Patrick T. Wallace * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - A suggested value for the TLR argument is 0.0065. The * refraction is significantly affected by TLR, and if studies * of the local atmosphere have been carried out a better TLR * value may be available. The sign of the supplied TLR value * is ignored. * * - A suggested value for the EPS argument is 1E-8. The result is * usually at least two orders of magnitude more computationally * precise than the supplied EPS value. * * - The routine computes the refraction for zenith distances up * to and a little beyond 90 deg using the method of Hohenkerk * and Sinclair (NAO Technical Notes 59 and 63, subsequently adopted * in the Explanatory Supplement, 1992 edition - see section 3.281). * * - The code is a development of the optical/IR refraction subroutine * AREF of C.Hohenkerk (HMNAO, September 1984), with extensions to * support the radio case. Apart from merely cosmetic changes, the * following modifications to the original HMNAO optical/IR refraction * code have been made: * * . The angle arguments have been changed to radians. * * . Any value of ZOBS is allowed (see note 6, below). * * . Other argument values have been limited to safe values. * * . Murray's values for the gas constants have been used * (Vectorial Astrometry, Adam Hilger, 1983). * * . The numerical integration phase has been rearranged for * extra clarity. * * . A better model for Ps(T) has been adopted (taken from * Gill, Atmosphere-Ocean Dynamics, Academic Press, 1982). * * . More accurate expressions for Pwo have been adopted * (again from Gill 1982). * * . The formula for the water vapour pressure, given the * saturation pressure and the relative humidity, is from * Crane (1976), expression 2.5.5. * . Provision for radio wavelengths has been added using * expressions devised by A.T.Sinclair, RGO (private * communication 1989). The refractivity model currently * used is from J.M.Rueger, "Refractive Index Formulae for * Electronic Distance Measurement with Radio and Millimetre * Waves", in Unisurv Report S-68 (2002), School of Surveying * and Spatial Information Systems, University of New South * Wales, Sydney, Australia. * * . The optical refractivity for dry air is from Resolution 3 of * the International Association of Geodesy adopted at the XXIIth * General Assembly in Birmingham, UK, 1999. * * . Various small changes have been made to gain speed. * * - The radio refraction is chosen by specifying WL > 100 micrometres. * Because the algorithm takes no account of the ionosphere, the * accuracy deteriorates at low frequencies, below about 30 MHz. * * - Before use, the value of ZOBS is expressed in the range +/- pi. * If this ranged ZOBS is -ve, the result REF is computed from its * absolute value before being made -ve to match. In addition, if * it has an absolute value greater than 93 deg, a fixed REF value * equal to the result for ZOBS = 93 deg is returned, appropriately * signed. * * - As in the original Hohenkerk and Sinclair algorithm, fixed values * of the water vapour polytrope exponent, the height of the * tropopause, and the height at which refraction is negligible are * used. * * - The radio refraction has been tested against work done by * Iain Coulson, JACH, (private communication 1995) for the * James Clerk Maxwell Telescope, Mauna Kea. For typical conditions, * agreement at the 0.1 arcsec level is achieved for moderate ZD, * worsening to perhaps 0.5-1.0 arcsec at ZD 80 deg. At hot and * humid sea-level sites the accuracy will not be as good. * * - It should be noted that the relative humidity RH is formally * defined in terms of "mixing ratio" rather than pressures or * densities as is often stated. It is the mass of water per unit * mass of dry air divided by that for saturated air at the same * temperature and pressure (see Gill 1982). * - The algorithm is designed for observers in the troposphere. The * supplied temperature, pressure and lapse rate are assumed to be * for a point in the troposphere and are used to define a model * atmosphere with the tropopause at 11km altitude and a constant * temperature above that. However, in practice, the refraction * values returned for stratospheric observers, at altitudes up to * 25km, are quite usable. * History: * 2012-08-24 (TIMJ): * Initial version, direct port of SLA Fortran source. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2005 Patrick T. Wallace * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include #include "pal.h" #include "pal1.h" #include "palmac.h" void palRefro( double zobs, double hm, double tdk, double pmb, double rh, double wl, double phi, double tlr, double eps, double * ref ) { /* * Fixed parameters */ /* 93 degrees in radians */ const double D93 = 1.623156204; /* Universal gas constant */ const double GCR = 8314.32; /* Molecular weight of dry air */ const double DMD = 28.9644; /* Molecular weight of water vapour */ const double DMW = 18.0152; /* Mean Earth radius (metre) */ const double S = 6378120.; /* Exponent of temperature dependence of water vapour pressure */ const double DELTA = 18.36; /* Height of tropopause (metre) */ const double HT = 11000.; /* Upper limit for refractive effects (metre) */ const double HS = 80000.; /* Numerical integration: maximum number of strips. */ const int ISMAX=16384l; /* Local variables */ int is, k, n, i, j; int optic, loop; /* booleans */ double zobs1,zobs2,hmok,tdkok,pmbok,rhok,wlok,alpha, tol,wlsq,gb,a,gamal,gamma,gamm2,delm2, tdc,psat,pwo,w, c1,c2,c3,c4,c5,c6,r0,tempo,dn0,rdndr0,sk0,f0, rt,tt,dnt,rdndrt,sine,zt,ft,dnts,rdndrp,zts,fts, rs,dns,rdndrs,zs,fs,refold,z0,zrange,fb,ff,fo,fe, h,r,sz,rg,dr,tg,dn,rdndr,t,f,refp,reft; /* The refraction integrand */ #define refi(DN,RDNDR) RDNDR/(DN+RDNDR) /* Transform ZOBS into the normal range. */ zobs1 = palDrange(zobs); zobs2 = DMIN(fabs(zobs1),D93); /* keep other arguments within safe bounds. */ hmok = DMIN(DMAX(hm,-1e3),HS); tdkok = DMIN(DMAX(tdk,100.0),500.0); pmbok = DMIN(DMAX(pmb,0.0),10000.0); rhok = DMIN(DMAX(rh,0.0),1.0); wlok = DMAX(wl,0.1); alpha = DMIN(DMAX(fabs(tlr),0.001),0.01); /* tolerance for iteration. */ tol = DMIN(DMAX(fabs(eps),1e-12),0.1)/2.0; /* decide whether optical/ir or radio case - switch at 100 microns. */ optic = wlok < 100.0; /* set up model atmosphere parameters defined at the observer. */ wlsq = wlok*wlok; gb = 9.784*(1.0-0.0026*cos(phi+phi)-0.00000028*hmok); if (optic) { a = (287.6155+(1.62887+0.01360/wlsq)/wlsq) * 273.15e-6/1013.25; } else { a = 77.6890e-6; } gamal = (gb*DMD)/GCR; gamma = gamal/alpha; gamm2 = gamma-2.0; delm2 = DELTA-2.0; tdc = tdkok-273.15; psat = pow(10.0,(0.7859+0.03477*tdc)/(1.0+0.00412*tdc)) * (1.0+pmbok*(4.5e-6+6.0e-10*tdc*tdc)); if (pmbok > 0.0) { pwo = rhok*psat/(1.0-(1.0-rhok)*psat/pmbok); } else { pwo = 0.0; } w = pwo*(1.0-DMW/DMD)*gamma/(DELTA-gamma); c1 = a*(pmbok+w)/tdkok; if (optic) { c2 = (a*w+11.2684e-6*pwo)/tdkok; } else { c2 = (a*w+6.3938e-6*pwo)/tdkok; } c3 = (gamma-1.0)*alpha*c1/tdkok; c4 = (DELTA-1.0)*alpha*c2/tdkok; if (optic) { c5 = 0.0; c6 = 0.0; } else { c5 = 375463e-6*pwo/tdkok; c6 = c5*delm2*alpha/(tdkok*tdkok); } /* conditions at the observer. */ r0 = S+hmok; pal1Atmt(r0,tdkok,alpha,gamm2,delm2,c1,c2,c3,c4,c5,c6, r0,&tempo,&dn0,&rdndr0); sk0 = dn0*r0*sin(zobs2); f0 = refi(dn0,rdndr0); /* conditions in the troposphere at the tropopause. */ rt = S+DMAX(HT,hmok); pal1Atmt(r0,tdkok,alpha,gamm2,delm2,c1,c2,c3,c4,c5,c6, rt,&tt,&dnt,&rdndrt); sine = sk0/(rt*dnt); zt = atan2(sine,sqrt(DMAX(1.0-sine*sine,0.0))); ft = refi(dnt,rdndrt); /* conditions in the stratosphere at the tropopause. */ pal1Atms(rt,tt,dnt,gamal,rt,&dnts,&rdndrp); sine = sk0/(rt*dnts); zts = atan2(sine,sqrt(DMAX(1.0-sine*sine,0.0))); fts = refi(dnts,rdndrp); /* conditions at the stratosphere limit. */ rs = S+HS; pal1Atms(rt,tt,dnt,gamal,rs,&dns,&rdndrs); sine = sk0/(rs*dns); zs = atan2(sine,sqrt(DMAX(1.0-sine*sine,0.0))); fs = refi(dns,rdndrs); /* variable initialization to avoid compiler warning. */ reft = 0.0; /* integrate the refraction integral in two parts; first in the * troposphere (k=1), then in the stratosphere (k=2). */ for (k=1; k<=2; k++) { /* initialize previous refraction to ensure at least two iterations. */ refold = 1.0; /* start off with 8 strips. */ is = 8; /* start z, z range, and start and end values. */ if (k==1) { z0 = zobs2; zrange = zt-z0; fb = f0; ff = ft; } else { z0 = zts; zrange = zs-z0; fb = fts; ff = fs; } /* sums of odd and even values. */ fo = 0.0; fe = 0.0; /* first time through the loop we have to do every point. */ n = 1; /* start of iteration loop (terminates at specified precision). */ loop = 1; while (loop) { /* strip width. */ h = zrange/((double)is); /* initialize distance from earth centre for quadrature pass. */ if (k == 1) { r = r0; } else { r = rt; } /* one pass (no need to compute evens after first time). */ for (i=1; i 1e-20) { w = sk0/sz; rg = r; dr = 1.0e6; j = 0; while ( fabs(dr) > 1.0 && j < 4 ) { j++; if (k==1) { pal1Atmt(r0,tdkok,alpha,gamm2,delm2, c1,c2,c3,c4,c5,c6,rg,&tg,&dn,&rdndr); } else { pal1Atms(rt,tt,dnt,gamal,rg,&dn,&rdndr); } dr = (rg*dn-w)/(dn+rdndr); rg = rg-dr; } r = rg; } /* find the refractive index and integrand at r. */ if (k==1) { pal1Atmt(r0,tdkok,alpha,gamm2,delm2, c1,c2,c3,c4,c5,c6,r,&t,&dn,&rdndr); } else { pal1Atms(rt,tt,dnt,gamal,r,&dn,&rdndr); } f = refi(dn,rdndr); /* accumulate odd and (first time only) even values. */ if (n==1 && i%2 == 0) { fe += f; } else { fo += f; } } /* evaluate the integrand using simpson's rule. */ refp = h*(fb+4.0*fo+2.0*fe+ff)/3.0; /* has the required precision been achieved (or can't be)? */ if (fabs(refp-refold) > tol && is < ISMAX) { /* no: prepare for next iteration.*/ /* save current value for convergence test. */ refold = refp; /* double the number of strips. */ is += is; /* sum of all current values = sum of next pass's even values. */ fe += fo; /* prepare for new odd values. */ fo = 0.0; /* skip even values next time. */ n = 2; } else { /* yes: save troposphere component and terminate the loop. */ if (k==1) reft = refp; loop = 0; } } } /* result. */ *ref = reft+refp; if (zobs1 < 0.0) *ref = -(*ref); } pal-0.5.0/palRefv.c000644 000765 000024 00000012110 12366000607 014134 0ustar00timjstaff000000 000000 /* *+ * Name: * palRefv * Purpose: * Adjust an unrefracted Cartesian vector to include the effect of atmospheric refraction * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palRefv ( double vu[3], double refa, double refb, double vr[3] ); * Arguments: * vu[3] = double (Given) * Unrefracted position of the source (Az/El 3-vector) * refa = double (Given) * tan Z coefficient (radian) * refb = double (Given) * tan**3 Z coefficient (radian) * vr[3] = double (Returned) * Refracted position of the source (Az/El 3-vector) * Description: * Adjust an unrefracted Cartesian vector to include the effect of * atmospheric refraction, using the simple A tan Z + B tan**3 Z * model. * Authors: * TIMJ: Tim Jenness * PTW: Patrick Wallace * {enter_new_authors_here} * Notes: * - This routine applies the adjustment for refraction in the * opposite sense to the usual one - it takes an unrefracted * (in vacuo) position and produces an observed (refracted) * position, whereas the A tan Z + B tan**3 Z model strictly * applies to the case where an observed position is to have the * refraction removed. The unrefracted to refracted case is * harder, and requires an inverted form of the text-book * refraction models; the algorithm used here is equivalent to * one iteration of the Newton-Raphson method applied to the above * formula. * * - Though optimized for speed rather than precision, the present * routine achieves consistency with the refracted-to-unrefracted * A tan Z + B tan**3 Z model at better than 1 microarcsecond within * 30 degrees of the zenith and remains within 1 milliarcsecond to * beyond ZD 70 degrees. The inherent accuracy of the model is, of * course, far worse than this - see the documentation for sla_REFCO * for more information. * * - At low elevations (below about 3 degrees) the refraction * correction is held back to prevent arithmetic problems and * wildly wrong results. For optical/IR wavelengths, over a wide * range of observer heights and corresponding temperatures and * pressures, the following levels of accuracy (arcsec, worst case) * are achieved, relative to numerical integration through a model * atmosphere: * * ZD error * * 80 0.7 * 81 1.3 * 82 2.5 * 83 5 * 84 10 * 85 20 * 86 55 * 87 160 * 88 360 * 89 640 * 90 1100 * 91 1700 } relevant only to * 92 2600 } high-elevation sites * * The results for radio are slightly worse over most of the range, * becoming significantly worse below ZD=88 and unusable beyond * ZD=90. * * - See also the routine palRefz, which performs the adjustment to * the zenith distance rather than in Cartesian Az/El coordinates. * The present routine is faster than palRefz and, except very low down, * is equally accurate for all practical purposes. However, beyond * about ZD 84 degrees palRefz should be used, and for the utmost * accuracy iterative use of palRefro should be considered. * History: * 2014-07-15 (TIMJ): * Initial version. A direct copy of the Fortran SLA implementation. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2014 Tim Jenness * Copyright (C) 2004 Patrick Wallace * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "palmac.h" #include void palRefv ( double vu[3], double refa, double refb, double vr[3] ) { double x,y,z1,z,zsq,rsq,r,wb,wt,d,cd,f; /* Initial estimate = unrefracted vector */ x = vu[0]; y = vu[1]; z1 = vu[2]; /* Keep correction approximately constant below about 3 deg elevation */ z = DMAX(z1,0.05); /* One Newton-Raphson iteration */ zsq = z*z; rsq = x*x+y*y; r = sqrt(rsq); wb = refb*rsq/zsq; wt = (refa+wb)/(1.0+(refa+3.0*wb)*(zsq+rsq)/zsq); d = wt*r/z; cd = 1.0-d*d/2.0; f = cd*(1.0-wt); /* Post-refraction x,y,z */ vr[0] = x*f; vr[1] = y*f; vr[2] = cd*(z+d*r)+(z1-z); } pal-0.5.0/palRefz.c000644 000765 000024 00000013775 12366000607 014162 0ustar00timjstaff000000 000000 /* *+ * Name: * palRefz * Purpose: * Adjust unrefracted zenith distance * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palRefz ( double zu, double refa, double refb, double *zr ); * Arguments: * zu = double (Given) * Unrefracted zenith distance of the source (radians) * refa = double (Given) * tan Z coefficient (radians) * refb = double (Given) * tan**3 Z coefficient (radian) * zr = double * (Returned) * Refracted zenith distance (radians) * Description: * Adjust an unrefracted zenith distance to include the effect of * atmospheric refraction, using the simple A tan Z + B tan**3 Z * model (plus special handling for large ZDs). * Authors: * PTW: Patrick T. Wallace * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - This routine applies the adjustment for refraction in the * opposite sense to the usual one - it takes an unrefracted * (in vacuo) position and produces an observed (refracted) * position, whereas the A tan Z + B tan**3 Z model strictly * applies to the case where an observed position is to have the * refraction removed. The unrefracted to refracted case is * harder, and requires an inverted form of the text-book * refraction models; the formula used here is based on the * Newton-Raphson method. For the utmost numerical consistency * with the refracted to unrefracted model, two iterations are * carried out, achieving agreement at the 1D-11 arcseconds level * for a ZD of 80 degrees. The inherent accuracy of the model * is, of course, far worse than this - see the documentation for * palRefco for more information. * * - At ZD 83 degrees, the rapidly-worsening A tan Z + B tan^3 Z * model is abandoned and an empirical formula takes over. For * optical/IR wavelengths, over a wide range of observer heights and * corresponding temperatures and pressures, the following levels of * accuracy (arcsec, worst case) are achieved, relative to numerical * integration through a model atmosphere: * * ZR error * * 80 0.7 * 81 1.3 * 82 2.4 * 83 4.7 * 84 6.2 * 85 6.4 * 86 8 * 87 10 * 88 15 * 89 30 * 90 60 * 91 150 } relevant only to * 92 400 } high-elevation sites * * For radio wavelengths the errors are typically 50% larger than * the optical figures and by ZD 85 deg are twice as bad, worsening * rapidly below that. To maintain 1 arcsec accuracy down to ZD=85 * at the Green Bank site, Condon (2004) has suggested amplifying * the amount of refraction predicted by palRefz below 10.8 deg * elevation by the factor (1+0.00195*(10.8-E_t)), where E_t is the * unrefracted elevation in degrees. * * The high-ZD model is scaled to match the normal model at the * transition point; there is no glitch. * * - Beyond 93 deg zenith distance, the refraction is held at its * 93 deg value. * * - See also the routine palRefv, which performs the adjustment in * Cartesian Az/El coordinates, and with the emphasis on speed * rather than numerical accuracy. * References: * Condon,J.J., Refraction Corrections for the GBT, PTCS/PN/35.2, * NRAO Green Bank, 2004. * History: * 2012-08-24 (TIMJ): * Initial version, ported directly from Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2004 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include #include "pal.h" #include "palmac.h" void palRefz ( double zu, double refa, double refb, double *zr ) { /* Constants */ /* Largest usable ZD (deg) */ const double D93 = 93.0; /* ZD at which one model hands over to the other (radians) */ const double Z83 = 83.0 * PAL__DD2R; /* coefficients for high ZD model (used beyond ZD 83 deg) */ const double C1 = +0.55445; const double C2 = -0.01133; const double C3 = +0.00202; const double C4 = +0.28385; const double C5 = +0.02390; /* High-ZD-model prefiction (deg) for that point */ const double REF83 = (C1+C2*7.0+C3*49.0)/(1.0+C4*7.0+C5*49.0); double zu1,zl,s,c,t,tsq,tcu,ref,e,e2; /* perform calculations for zu or 83 deg, whichever is smaller */ zu1 = DMIN(zu,Z83); /* functions of ZD */ zl = zu1; s = sin(zl); c = cos(zl); t = s/c; tsq = t*t; tcu = t*tsq; /* refracted zd (mathematically to better than 1 mas at 70 deg) */ zl = zl-(refa*t+refb*tcu)/(1.0+(refa+3.0*refb*tsq)/(c*c)); /* further iteration */ s = sin(zl); c = cos(zl); t = s/c; tsq = t*t; tcu = t*tsq; ref = zu1-zl+ (zl-zu1+refa*t+refb*tcu)/(1.0+(refa+3.0*refb*tsq)/(c*c)); /* special handling for large zu */ if (zu > zu1) { e = 90.0-DMIN(D93,zu*PAL__DR2D); e2 = e*e; ref = (ref/REF83)*(C1+C2*e+C3*e2)/(1.0+C4*e+C5*e2); } /* return refracted zd */ *zr = zu-ref; } pal-0.5.0/palRverot.c000644 000765 000024 00000005217 12366000607 014525 0ustar00timjstaff000000 000000 /* *+ * Name: * palRverot * Purpose: * Velocity component in a given direction due to Earth rotation * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * double palRverot ( double phi, double ra, double da, double st ); * Arguments: * phi = double (Given) * latitude of observing station (geodetic) (radians) * ra = double (Given) * apparent RA (radians) * da = double (Given) * apparent Dec (radians) * st = double (Given) 8 Local apparent sidereal time. * Returned Value: * palRverot = double * Component of Earth rotation in direction RA,DA (km/s). * The result is +ve when the observatory is receding from the * given point on the sky. * Description: * Calculate the velocity component in a given direction due to Earth * rotation. * * The simple algorithm used assumes a spherical Earth, of * a radius chosen to give results accurate to about 0.0005 km/s * for observing stations at typical latitudes and heights. For * applications requiring greater precision, use the routine * palPvobs. * Authors: * PTW: Patrick T. Wallace * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * History: * 2012-03-02 (TIMJ): * Initial version * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1995 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include double palRverot ( double phi, double ra, double da, double st ) { /* Nominal mean sidereal speed of Earth equator in km/s (the actual * value is about 0.4651) */ const double espeed = 0.4655; return espeed * cos(phi) * sin(st-ra) * cos(da); } pal-0.5.0/palRvgalc.c000644 000765 000024 00000006016 12366000611 014453 0ustar00timjstaff000000 000000 /* *+ * Name: * palRvgalc * Purpose: * Velocity component in a given direction due to the rotation * of the Galaxy. * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * double palRvgalc( double r2000, double d2000 ) * Arguments: * r2000 = double (Given) * J2000.0 mean RA (radians) * d2000 = double (Given) * J2000.0 mean Dec (radians) * Returned Value: * Component of dynamical LSR motion in direction R2000,D2000 (km/s). * Description: * This function returns the Component of dynamical LSR motion in * the direction of R2000,D2000. The result is +ve when the dynamical * LSR is receding from the given point on the sky. * * Notes: * - The Local Standard of Rest used here is a point in the * vicinity of the Sun which is in a circular orbit around * the Galactic centre. Sometimes called the "dynamical" LSR, * it is not to be confused with a "kinematical" LSR, which * is the mean standard of rest of star catalogues or stellar * populations. * * Reference: * - The orbital speed of 220 km/s used here comes from Kerr & * Lynden-Bell (1986), MNRAS, 221, p1023. * Authors: * PTW: Pat Wallace (STFC) * DSB: David Berry (JAC, Hawaii) * {enter_new_authors_here} * History: * 2012-02-16 (DSB): * Initial version. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1995 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "pal1sofa.h" double palRvgalc( double r2000, double d2000 ){ /* Local Variables: */ double vb[ 3 ]; /* * LSR velocity due to Galactic rotation * * Speed = 220 km/s * Apex = L2,B2 90deg, 0deg * = RA,Dec 21 12 01.1 +48 19 47 J2000.0 * * This is expressed in the form of a J2000.0 x,y,z vector: * * VA(1) = X = -SPEED*COS(RA)*COS(DEC) * VA(2) = Y = -SPEED*SIN(RA)*COS(DEC) * VA(3) = Z = -SPEED*SIN(DEC) */ double va[ 3 ] = { -108.70408, +97.86251, -164.33610 }; /* Convert given J2000 RA,Dec to x,y,z. */ eraS2c( r2000, d2000, vb ); /* Compute dot product with LSR motion vector. */ return eraPdp( va, vb ); } pal-0.5.0/palRvlg.c000644 000765 000024 00000005355 12366000611 014154 0ustar00timjstaff000000 000000 /* *+ * Name: * palRvlg * Purpose: * Velocity component in a given direction due to Galactic rotation * and motion of the local group. * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * double palRvlg( double r2000, double d2000 ) * Arguments: * r2000 = double (Given) * J2000.0 mean RA (radians) * d2000 = double (Given) * J2000.0 mean Dec (radians) * Returned Value: * Component of SOLAR motion in direction R2000,D2000 (km/s). * Description: * This function returns the velocity component in a given * direction due to the combination of the rotation of the * Galaxy and the motion of the Galaxy relative to the mean * motion of the local group. The result is +ve when the Sun * is receding from the given point on the sky. * * Reference: * - IAU Trans 1976, 168, p201. * Authors: * PTW: Pat Wallace (STFC) * DSB: David Berry (JAC, Hawaii) * {enter_new_authors_here} * History: * 2012-02-16 (DSB): * Initial version. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1995 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "pal1sofa.h" double palRvlg( double r2000, double d2000 ){ /* Local Variables: */ double vb[ 3 ]; /* * * Solar velocity due to Galactic rotation and translation * * Speed = 300 km/s * * Apex = L2,B2 90deg, 0deg * = RA,Dec 21 12 01.1 +48 19 47 J2000.0 * * This is expressed in the form of a J2000.0 x,y,z vector: * * VA(1) = X = -SPEED*COS(RA)*COS(DEC) * VA(2) = Y = -SPEED*SIN(RA)*COS(DEC) * VA(3) = Z = -SPEED*SIN(DEC) */ double va[ 3 ] = { -148.23284, +133.44888, -224.09467 }; /* Convert given J2000 RA,Dec to x,y,z. */ eraS2c( r2000, d2000, vb ); /* Compute dot product with Solar motion vector. */ return eraPdp( va, vb ); } pal-0.5.0/palRvlsrd.c000644 000765 000024 00000007122 12366000611 014510 0ustar00timjstaff000000 000000 /* *+ * Name: * palRvlsrd * Purpose: * Velocity component in a given direction due to the Sun's motion * with respect to the dynamical Local Standard of Rest. * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * double palRvlsrd( double r2000, double d2000 ) * Arguments: * r2000 = double (Given) * J2000.0 mean RA (radians) * d2000 = double (Given) * J2000.0 mean Dec (radians) * Returned Value: * Component of "peculiar" solar motion in direction R2000,D2000 (km/s). * Description: * This function returns the velocity component in a given direction * due to the Sun's motion with respect to the dynamical Local Standard * of Rest. The result is +ve when the Sun is receding from the given * point on the sky. * Notes: * - The Local Standard of Rest used here is the "dynamical" LSR, * a point in the vicinity of the Sun which is in a circular orbit * around the Galactic centre. The Sun's motion with respect to the * dynamical LSR is called the "peculiar" solar motion. * - There is another type of LSR, called a "kinematical" LSR. A * kinematical LSR is the mean standard of rest of specified star * catalogues or stellar populations, and several slightly different * kinematical LSRs are in use. The Sun's motion with respect to an * agreed kinematical LSR is known as the "standard" solar motion. * To obtain a radial velocity correction with respect to an adopted * kinematical LSR use the routine sla_RVLSRK. * Reference: * - Delhaye (1965), in "Stars and Stellar Systems", vol 5, p73. * Authors: * PTW: Pat Wallace (STFC) * DSB: David Berry (JAC, Hawaii) * {enter_new_authors_here} * History: * 2012-02-16 (DSB): * Initial version. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1995 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "pal1sofa.h" double palRvlsrd( double r2000, double d2000 ){ /* Local Variables: */ double vb[ 3 ]; /* * Peculiar solar motion from Delhaye 1965: in Galactic Cartesian * coordinates (+9,+12,+7) km/s. This corresponds to about 16.6 km/s * towards Galactic coordinates L2 = 53 deg, B2 = +25 deg, or RA,Dec * 17 49 58.7 +28 07 04 J2000. * * The solar motion is expressed here in the form of a J2000.0 * equatorial Cartesian vector: * * VA(1) = X = -SPEED*COS(RA)*COS(DEC) * VA(2) = Y = -SPEED*SIN(RA)*COS(DEC) * VA(3) = Z = -SPEED*SIN(DEC) */ double va[ 3 ] = { +0.63823, +14.58542, -7.80116 }; /* Convert given J2000 RA,Dec to x,y,z. */ eraS2c( r2000, d2000, vb ); /* Compute dot product with Solar motion vector. */ return eraPdp( va, vb ); } pal-0.5.0/palRvlsrk.c000644 000765 000024 00000006745 12366000611 014531 0ustar00timjstaff000000 000000 /* *+ * Name: * palRvlsrk * Purpose: * Velocity component in a given direction due to the Sun's motion * with respect to an adopted kinematic Local Standard of Rest. * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * double palRvlsrk( double r2000, double d2000 ) * Arguments: * r2000 = double (Given) * J2000.0 mean RA (radians) * d2000 = double (Given) * J2000.0 mean Dec (radians) * Returned Value: * Component of "standard" solar motion in direction R2000,D2000 (km/s). * Description: * This function returns the velocity component in a given direction * due to the Sun's motion with respect to an adopted kinematic * Local Standard of Rest. The result is +ve when the Sun is receding * from the given point on the sky. * Notes: * - The Local Standard of Rest used here is one of several * "kinematical" LSRs in common use. A kinematical LSR is the mean * standard of rest of specified star catalogues or stellar * populations. The Sun's motion with respect to a kinematical LSR * is known as the "standard" solar motion. * - There is another sort of LSR, the "dynamical" LSR, which is a * point in the vicinity of the Sun which is in a circular orbit * around the Galactic centre. The Sun's motion with respect to * the dynamical LSR is called the "peculiar" solar motion. To * obtain a radial velocity correction with respect to the * dynamical LSR use the routine sla_RVLSRD. * Reference: * - Delhaye (1965), in "Stars and Stellar Systems", vol 5, p73. * Authors: * PTW: Pat Wallace (STFC) * DSB: David Berry (JAC, Hawaii) * {enter_new_authors_here} * History: * 2012-02-16 (DSB): * Initial version. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1995 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "pal1sofa.h" double palRvlsrk( double r2000, double d2000 ){ /* Local Variables: */ double vb[ 3 ]; /* * Standard solar motion (from Methods of Experimental Physics, ed Meeks, * vol 12, part C, sec 6.1.5.2, p281): * * 20 km/s towards RA 18h Dec +30d (1900). * * The solar motion is expressed here in the form of a J2000.0 * equatorial Cartesian vector: * * VA(1) = X = -SPEED*COS(RA)*COS(DEC) * VA(2) = Y = -SPEED*SIN(RA)*COS(DEC) * VA(3) = Z = -SPEED*SIN(DEC) */ double va[ 3 ] = { -0.29000, +17.31726, -10.00141 }; /* Convert given J2000 RA,Dec to x,y,z. */ eraS2c( r2000, d2000, vb ); /* Compute dot product with Solar motion vector. */ return eraPdp( va, vb ); } pal-0.5.0/palSubet.c000644 000765 000024 00000005724 12366000611 014324 0ustar00timjstaff000000 000000 /* *+ * Name: * palSubet * Purpose: * Remove the E-terms from a pre IAU 1976 catalogue RA,Dec * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palSubet ( double rc, double dc, double eq, * double *rm, double *dm ); * Arguments: * rc = double (Given) * RA with E-terms included (radians) * dc = double (Given) * Dec with E-terms included (radians) * eq = double (Given) * Besselian epoch of mean equator and equinox * rm = double * (Returned) * RA without E-terms (radians) * dm = double * (Returned) * Dec without E-terms (radians) * Description: * Remove the E-terms (elliptic component of annual aberration) * from a pre IAU 1976 catalogue RA,Dec to give a mean place. * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * Most star positions from pre-1984 optical catalogues (or * derived from astrometry using such stars) embody the * E-terms. This routine converts such a position to a * formal mean place (allowing, for example, comparison with a * pulsar timing position). * See Also: * Explanatory Supplement to the Astronomical Ephemeris, * section 2D, page 48. * History: * 2012-02-12(TIMJ): * Initial version with documentation taken from Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1995 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "pal1sofa.h" void palSubet ( double rc, double dc, double eq, double *rm, double *dm ) { double a[3]; /* The E-terms */ double v[3]; double f; int i; /* Note the preference for IAU routines */ /* Retrieve the E-terms */ palEtrms( eq, a ); /* Spherical to Cartesian */ eraS2c( rc, dc, v ); /* Include the E-terms */ f = 1.0 + eraPdp( v, a ); for (i=0; i<3; i++) { v[i] = f*v[i] - a[i]; } /* Cartesian to spherical */ eraC2s( v, rm, dm ); /* Bring RA into conventional range */ *rm = eraAnp( *rm ); } pal-0.5.0/palSupgal.c000644 000765 000024 00000006116 12366000611 014471 0ustar00timjstaff000000 000000 /* *+ * Name: * palSupgal * Purpose: * Convert from supergalactic to galactic coordinates * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palSupgal ( double dsl, double dsb, double *dl, double *db ); * Arguments: * dsl = double (Given) * Supergalactic longitude. * dsb = double (Given) * Supergalactic latitude. * dl = double * (Returned) * Galactic longitude. * db = double * (Returned) * Galactic latitude. * Description: * Transformation from de Vaucouleurs supergalactic coordinates * to IAU 1958 galactic coordinates * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * See Also: * - de Vaucouleurs, de Vaucouleurs, & Corwin, Second Reference * Catalogue of Bright Galaxies, U. Texas, page 8. * - Systems & Applied Sciences Corp., Documentation for the * machine-readable version of the above catalogue, * Contract NAS 5-26490. * * (These two references give different values for the galactic * longitude of the supergalactic origin. Both are wrong; the * correct value is L2=137.37.) * History: * 2012-02-12(TIMJ): * Initial version with documentation taken from Fortran SLA * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1995 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software: you can redistribute it and/or * modify it under the terms of the GNU Lesser General Public * License as published by the Free Software Foundation, either * version 3 of the License, or (at your option) any later * version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU Lesser General Public License for more details. * * You should have received a copy of the GNU Lesser General * License along with this program. If not, see * . * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "pal1sofa.h" void palSupgal ( double dsl, double dsb, double *dl, double *db ) { double v1[3]; double v2[3]; /* * System of supergalactic coordinates: * * SGL SGB L2 B2 (deg) * - +90 47.37 +6.32 * 0 0 - 0 * * Galactic to supergalactic rotation matrix: */ double rmat[3][3] = { { -0.735742574804,+0.677261296414,+0.000000000000 }, { -0.074553778365,-0.080991471307,+0.993922590400 }, { +0.673145302109,+0.731271165817,+0.110081262225 } }; /* Spherical to Cartesian */ eraS2c( dsl, dsb, v1 ); /* Supergalactic to galactic */ eraTrxp( rmat, v1, v2 ); /* Cartesian to spherical */ eraC2s( v2, dl, db ); /* Express in conventional ranges */ *dl = eraAnp( *dl ); *db = eraAnpm( *db ); } pal-0.5.0/palTest.c000644 000765 000024 00000157312 12366000607 014167 0ustar00timjstaff000000 000000 /* *+ * Name: * palTest * Purpose: * Test the PAL library * Language: * Starlink ANSI C * Type of Module: * Application * Description: * Test the PAL library is functioning correctly. Uses some of the SLA test code. * Authors: * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * History: * 2012-02-08 (TIMJ): * Initial version * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, MA 02110-1301 * USA. * Bugs: * {note_any_bugs_here} *- */ #include #include #include #include "pal.h" #include "palmac.h" static int verbose = 1; /* Support functions to allow to test results. viv and vvd match the SOFA implementations */ static void viv(int ival, int ivalok, const char *func, const char *test, int *status) /* ** - - - - ** v i v ** - - - - ** ** Validate an integer result. ** ** Internal function used by t_sofa_c program. ** ** Given: ** ival int value computed by function under test ** ivalok int correct value ** func char[] name of function under test ** test char[] name of individual test ** ** Given and returned: ** status int set to FALSE if test fails ** ** This revision: 2009 November 4 */ { if (ival != ivalok) { *status = 1; printf("%s failed: %s want %d got %d\n", func, test, ivalok, ival); } else if (verbose) { printf("%s passed: %s want %d got %d\n", func, test, ivalok, ival); } return; } static void vvd(double val, double valok, double dval, const char *func, const char *test, int *status) /* ** - - - - ** v v d ** - - - - ** ** Validate a double result. ** ** Internal function used by t_sofa_c program. ** ** Given: ** val double value computed by function under test ** valok double expected value ** dval double maximum allowable error ** func char[] name of function under test ** test char[] name of individual test ** ** Given and returned: ** status int set to FALSE if test fails ** ** This revision: 2008 June 8 */ { double a, f; /* absolute and fractional error */ a = val - valok; if (fabs(a) > dval) { f = fabs(valok / a); *status = 1; printf("%s failed: %s want %.20g got %.20g (1/%.3g)\n", func, test, valok, val, f); } else if (verbose) { printf("%s passed: %s want %.20g got %.20g\n", func, test, valok, val); } return; } /* Verify a string */ static void vcs( const char * val, const char * valok, const char * func, const char * test, int *status ) { if (strcmp(val, valok) != 0) { *status = 1; printf("%s failed: %s want %s got %s\n", func, test, valok, val ); } else if (verbose) { printf("%s passed: %s want %s got %s\n", func, test, valok, val ); } return; } /* Verify the 3x3 rmat matrix */ static void vrmat( double rmat[3][3], double expected[3][3], const char * func, double dval, int * status ) { int i; char buf[10]; for( i = 0; i < 3; i++ ) { int j; for( j = 0; j < 3; j++ ) { sprintf( buf, "%d,%d", i, j ); vvd( rmat[i][j], expected[i][j], dval, func, buf, status ); } } } /* Verify a vector */ static void vvec( int len, double *vec, double *expected, const char *func, int *status ) { int i; char buf[10]; for( i = 0; i < len; i++ ) { sprintf( buf, "%d", i ); vvd( vec[i], expected[i], 1e-12, func, buf, status ); } } /******************************************************************/ /* TEST FUNCTIONS */ /* Adding E-terms */ static void t_addet( int *status ) { double r1,d1,r2,d2; double rm = 2.; double dm = -1.; double eq = 1975.; palAddet ( rm, dm, eq, &r1, &d1 ); vvd ( r1 - rm, 2.983864874295250e-6, 1e-12, "palAddet", "R", status ); vvd ( d1 - dm, 2.379650804185118e-7, 1e-12, "palAddet", "D", status ); palSubet ( r1, d1, eq, &r2, &d2 ); vvd ( r2 - rm, 0, 1e-12, "palSubet", "R", status ); vvd ( d2 - dm, 0, 1e-12, "palSubet", "D", status ); } static void t_afin( int * status ) { int j; int i = 1; double d = 0.0; const char * s = "12 34 56.7 |"; const char * s2 = "45 00 00.000 "; palDafin (s, &i, &d, &j); viv ( i, 12, "palDafin", "I", status ); vvd ( d, 0.2196045986911432, 1e-12, "palDafin", "A", status ); viv ( j, 0, "palDafin", "J", status ); i = 1; palDafin (s2, &i, &d, &j); viv ( i, 14, "palDafin", "I", status ); vvd ( d, PAL__DPI/4.0, 1e-12, "palDafin", "A", status ); viv ( j, 0, "palDafin", "J", status ); } /* Airmass */ static void t_airmas( int *status ) { vvd ( palAirmas ( 1.2354 ), 3.015698990074724, 1e-12, "palAirmas", " ", status ); } /* Apparent to mean place */ static void t_amp ( int *status ) { double rm, dm; /* Original SLA test is not accurate since palMapqk differs from slaMapqk */ palAmp ( 2.345, -1.234, 50100, 1990, &rm, &dm ); vvd ( rm, 2.344472180027961, 1e-6, "palAmp", "R", status ); vvd ( dm, -1.233573099847705, 1e-7, "palAmp", "D", status ); /* This is the palMapqk test */ palAmp( 1.234, -0.567, 55927.0, 2010.0, &rm, &dm ); vvd( rm, 1.2335120411026936349, 1.0E-12, "palAmp", "rm", status ); vvd( dm, -0.56702908706930343907, 1.0E-12, "palAmp", "dm", status ); } /* Apparent to Observed place */ static void t_aop ( int *status ) { int i; double rap, dap, date, dut, elongm, phim, hm, xp, yp, tdk, pmb, rh, wl, tlr, aob, zob, hob, dob, rob, aoprms[14]; dap = -0.1234; date = 51000.1; dut = 25.0; elongm = 2.1; phim = 0.5; hm = 3000.0; xp = -0.5e-6; yp = 1.0e-6; tdk = 280.0; pmb = 550.0; rh = 0.6; tlr = 0.006; for (i=1; i<=3; i++) { if ( i == 1 ) { rap = 2.7; wl = 0.45; } else if ( i == 2 ) { rap = 2.345; } else { wl = 1.0e6; } palAop ( rap, dap, date, dut, elongm, phim, hm, xp, yp, tdk, pmb, rh, wl, tlr, &aob, &zob, &hob, &dob, &rob ); if ( i == 1 ) { vvd( aob, 1.812817787123283034, 1e-10, "palAop", "lo aob", status ); vvd( zob, 1.393860816635714034, 1e-8, "palAop", "lo zob", status ); vvd( hob, -1.297808009092456683, 1e-8, "palAop", "lo hob", status ); vvd( dob, -0.122967060534561, 1e-8, "palAop", "lo dob", status ); vvd( rob, 2.699270287872084, 1e-8, "palAop", "lo rob", status ); } else if ( i == 2 ) { vvd( aob, 2.019928026670621442, 1e-10, "palAop", "aob/o", status ); vvd( zob, 1.101316172427482466, 1e-10, "palAop", "zob/o", status ); vvd( hob, -0.9432923558497740862, 1e-10, "palAop", "hob/o", status ); vvd( dob, -0.1232144708194224, 1e-10, "palAop", "dob/o", status ); vvd( rob, 2.344754634629428, 1e-10, "palAop", "rob/o", status ); } else { vvd( aob, 2.019928026670621442, 1e-10, "palAop", "aob/r", status ); vvd( zob, 1.101267532198003760, 1e-10, "palAop", "zob/r", status ); vvd( hob, -0.9432533138143315937, 1e-10, "palAop", "hob/r", status ); vvd( dob, -0.1231850665614878, 1e-10, "palAop", "dob/r", status ); vvd( rob, 2.344715592593984, 1e-10, "palAop", "rob/r", status ); } } date = 48000.3; wl = 0.45; palAoppa ( date, dut, elongm, phim, hm, xp, yp, tdk, pmb, rh, wl, tlr, aoprms ); vvd( aoprms[0], 0.4999993892136306, 1e-13, "palAoppa", "0", status ); vvd( aoprms[1], 0.4794250025886467, 1e-13, "palAoppa", "1", status ); vvd( aoprms[2], 0.8775828547167932, 1e-13, "palAoppa", "2", status ); vvd( aoprms[3], 1.363180872136126e-6, 1e-13, "palAoppa", "3", status ); vvd( aoprms[4], 3000.0, 1e-10, "palAoppa", "4", status ); vvd( aoprms[5], 280.0, 1e-11, "palAoppa", "5", status ); vvd( aoprms[6], 550.0, 1e-11, "palAoppa", "6", status ); vvd( aoprms[7], 0.6, 1e-13, "palAoppa", "7", status ); vvd( aoprms[8], 0.45, 1e-13, "palAoppa", "8", status ); vvd( aoprms[9], 0.006, 1e-15, "palAoppa", "9", status ); vvd( aoprms[10], 0.0001562803328459898, 1e-13, "palAoppa", "10", status ); vvd( aoprms[11], -1.792293660141e-7, 1e-13, "palAoppa", "11", status ); vvd( aoprms[12], 2.101874231495843, 1e-13, "palAoppa", "12", status ); vvd( aoprms[13], 7.601916802079765, 1e-8, "palAoppa", "13", status ); palOap ( "r", 1.6, -1.01, date, dut, elongm, phim, hm, xp, yp, tdk, pmb, rh, wl, tlr, &rap, &dap ); vvd( rap, 1.601197569844787, 1e-10, "palOap", "rr", status ); vvd( dap, -1.012528566544262, 1e-10, "palOap", "rd", status ); palOap ( "h", -1.234, 2.34, date, dut, elongm, phim, hm, xp, yp, tdk, pmb, rh, wl, tlr, &rap, &dap ); vvd( rap, 5.693087688154886463, 1e-10, "palOap", "hr", status ); vvd( dap, 0.8010281167405444, 1e-10, "palOap", "hd", status ); palOap ( "a", 6.1, 1.1, date, dut, elongm, phim, hm, xp, yp, tdk, pmb, rh, wl, tlr, &rap, &dap ); vvd( rap, 5.894305175192448940, 1e-10, "palOap", "ar", status ); vvd( dap, 1.406150707974922, 1e-10, "palOap", "ad", status ); palOapqk ( "r", 2.1, -0.345, aoprms, &rap, &dap ); vvd( rap, 2.10023962776202, 1e-10, "palOapqk", "rr", status ); vvd( dap, -0.3452428692888919, 1e-10, "palOapqk", "rd", status ); palOapqk ( "h", -0.01, 1.03, aoprms, &rap, &dap ); vvd( rap, 1.328731933634564995, 1e-10, "palOapqk", "hr", status ); vvd( dap, 1.030091538647746, 1e-10, "palOapqk", "hd", status ); palOapqk ( "a", 4.321, 0.987, aoprms, &rap, &dap ); vvd( rap, 0.4375507112075065923, 1e-10, "palOapqk", "ar", status ); vvd( dap, -0.01520898480744436, 1e-10, "palOapqk", "ad", status ); palAoppat ( date + PAL__DS2R, aoprms ); vvd( aoprms[13], 7.602374979243502, 1e-8, "palAoppat", " ", status ); } /* Bearings */ static void t_bear( int *status ) { double a1 = 1.234; double b1 = -0.123; double a2 = 2.345; double b2 = 0.789; double d1[3]; double d2[3]; vvd ( palDbear ( a1, b1, a2, b2 ), 0.7045970341781791, 1e-12, "palDbear", " ", status ); palDcs2c ( a1, b1, d1 ); palDcs2c ( a2, b2, d2 ); vvd ( palDpav ( d1, d2 ), 0.7045970341781791, 1e-12, "palDpav", " ", status ); } /* Calendar to MJD */ static void t_caldj( int *status ) { int j; double djm; palCaldj ( 1999, 12, 31, &djm, &j ); vvd ( djm, 51543, 0, "palCaldj", " ", status ); viv ( j, 0, "palCaldj", "J", status ); } /* palDaf2r */ static void t_caf2r( int * status ) { int j; double dr; palDaf2r ( 76, 54, 32.1, &dr, &j ); vvd ( dr, 1.342313819975276, 1e-12, "palDaf2r", "r", status ); viv ( j, 0, "palDaf2r", "j", status ); } /* Test palDcc2s routines */ static void t_cc2s( int * status ) { double dv[3] = { 100., -50., 25. }; double da, db; palDcc2s ( dv, &da, &db ); vvd ( da, -0.4636476090008061, 1e-12, "palDcc2s", "A", status ); vvd ( db, 0.2199879773954594, 1e-12, "palDcc2s", "B", status ); } /* palDd2tf */ static void t_cd2tf( int *status ) { int ihmsf[4]; char s; palDd2tf ( 4, -0.987654321, &s, ihmsf ); viv ( s, '-', "palDd2tf", "S", status ); viv ( ihmsf[0], 23, "palDd2tf", "(1)", status ); viv ( ihmsf[1], 42, "palDd2tf", "(2)", status ); viv ( ihmsf[2], 13, "palDd2tf", "(3)", status ); viv ( ihmsf[3], 3333, "palDd2tf", "(4)", status ); } /* Calendar to MJD */ static void t_cldj( int *status ) { double d; int j; palCldj ( 1899, 12, 31, &d, &j ); vvd ( d, 15019, 0, "palCldj", "D", status ); viv ( j, 0, "palCldj", "J", status ); } /* palDr2af */ static void t_cr2af( int *status ) { char s; int idmsf[4]; palDr2af ( 4, 2.345, &s, idmsf ); viv ( s, '+', "palDr2af", "S", status ); viv ( idmsf[0], 134, "palDr2af", "(1)", status ); viv ( idmsf[1], 21, "palDr2af", "(2)", status ); viv ( idmsf[2], 30, "palDr2af", "(3)", status ); viv ( idmsf[3], 9706, "palDr2af", "(4)", status ); } /* palDr2tf */ static void t_cr2tf( int *status ) { char s; int ihmsf[4]; palDr2tf ( 4, -3.01234, &s, ihmsf ); viv ( s, '-', "palDr2tf", "S", status ); viv ( ihmsf[0], 11, "palDr2tf", "(1)", status ); viv ( ihmsf[1], 30, "palDr2tf", "(2)", status ); viv ( ihmsf[2], 22, "palDr2tf", "(3)", status ); viv ( ihmsf[3], 6484, "palDr2tf", "(4)", status ); } /* palDtf2d */ static void t_ctf2d( int *status ) { double dd; int j; palDtf2d (23, 56, 59.1, &dd, &j); vvd ( dd, 0.99790625, 1e-12, "palDtf2d", "D", status ); viv ( j, 0, "palDtf2d", "J", status ); } /* palDtf2r */ static void t_ctf2r( int *status ) { double dr; int j; palDtf2r (23, 56, 59.1, &dr, &j); vvd ( dr, 6.270029887942679, 1e-12, "palDtf2r", "R", status ); viv ( j, 0, "palDtf2r", "J", status ); } static void t_dat ( int *status ) { vvd ( palDat ( 43900 ), 18, 0, "palDat", " ", status ); vvd ( palDtt ( 40404 ), 39.709746, 1e-12, "palDtt", " ", status ); vvd ( palDt ( 500 ), 4686.7, 1e-10, "palDt", "500", status ); vvd ( palDt ( 1400 ), 408, 1e-11, "palDt", "1400", status ); vvd ( palDt ( 1950 ), 27.99145626, 1e-12, "palDt", "1950", status ); } /* Dates */ static void t_djcal( int *status ) { const double djm = 50123.9999; int iy, im, id; int iydmf[4]; int j; double f; palDjcal ( 4, djm, iydmf, &j ); viv ( iydmf[0], 1996, "palDjcal", "Y", status ); viv ( iydmf[1], 2, "palDjcal", "M", status ); viv ( iydmf[2], 10, "palDjcal", "D", status ); viv ( iydmf[3], 9999, "palDjcal", "F", status ); viv ( j, 0, "palDjcal", "J", status ); palDjcl ( djm, &iy, &im, &id, &f, &j ); viv ( iy, 1996, "palDjcl", "Y", status ); viv ( im, 2, "palDjcl", "M", status ); viv ( id, 10, "palDjcl", "D", status ); vvd ( f, 0.9999, 1e-7, "palDjcl", "F", status ); viv ( j, 0, "palDjcl", "J", status ); } /* Matrix inversion */ static void t_dmat( int *status ) { int j; int iw[3]; double dd; double da[9] = { 2.22, 1.6578, 1.380522, 1.6578, 1.380522, 1.22548578, 1.380522, 1.22548578, 1.1356276122 }; double dv[3] = { 2.28625, 1.7128825, 1.429432225 }; palDmat( 3, da, dv, &dd, &j, iw ); vvd ( da[0], 18.02550629769198, 1e-10, "palDmat", "a[0]", status ); vvd ( da[1], -52.16386644917280607, 1e-10, "palDmat", "a[1]", status ); vvd ( da[2], 34.37875949717850495, 1e-10, "palDmat", "a[2]", status ); vvd ( da[3], -52.16386644917280607, 1e-10, "palDmat", "a[3]", status ); vvd ( da[4], 168.1778099099805627, 1e-10, "palDmat", "a[4]", status ); vvd ( da[5], -118.0722869694232670, 1e-10, "palDmat", "a[5]", status ); vvd ( da[6], 34.37875949717850495, 1e-10, "palDmat", "a[6]", status ); vvd ( da[7], -118.0722869694232670, 1e-10, "palDmat", "a[7]", status ); vvd ( da[8], 86.50307003740151262, 1e-10, "palDmat", "a[8]", status ); vvd ( dv[0], 1.002346480763383, 1e-12, "palDmat", "v[0]", status ); vvd ( dv[1], 0.03285594016974583489, 1e-12, "palDmat", "v[1]", status ); vvd ( dv[2], 0.004760688414885247309, 1e-12, "palDmat", "v[2]", status ); vvd ( dd, 0.003658344147359863, 1e-12, "palDmat", "D", status ); viv ( j, 0, "palDmat", "J", status ); } /* Test palDe2h and palDh2e routines */ static void t_e2h( int *status ) { double dh, dd, dp, da, de; dh = -0.3; dd = -1.1; dp = -0.7; palDe2h( dh, dd, dp, &da, &de ); vvd( da, 2.820087515852369, 1e-12, "palDe2h", "AZ", status); vvd( de, 1.132711866443304, 1e-12, "palDe2h", "EL", status ); palDh2e( da, de, dp, &dh, &dd ); vvd( dh, -0.3, 1e-12, "palDh2e", "HA", status); vvd( dd, -1.1, 1e-12, "palDh2e", "DEC", status ); } /* Epochs */ static void t_epb( int *status ) { vvd ( palEpb( 45123 ), 1982.419793168669, 1e-8, "palEpb", " ", status ); } static void t_epb2d( int *status ) { vvd ( palEpb2d( 1975.5 ), 42595.5995279655, 1e-7, "palEpb2d", " ", status ); } static void t_epco( int *status ) { vvd ( palEpco ( 'B', 'J', 2000 ), 2000.001277513665, 1e-7, "palEpco", "BJ", status ); vvd ( palEpco ( 'J', 'B', 1950 ), 1949.999790442300, 1e-7, "palEpco", "JB", status ); vvd ( palEpco ( 'J', 'j', 2000 ), 2000, 1e-7, "palEpco", "JJ", status ); } static void t_epj( int *status ) { vvd ( palEpj( 42999 ), 1976.603696098563, 1e-7, "palEpj", " ", status ); } static void t_epj2d( int *status ) { vvd ( palEpj2d( 2010.077 ), 55225.124250, 1e-6, "palEpj2d", " ", status ); } /* Equation of the equinoxes */ /* Use SOFA test because of change in precession model */ static void t_eqeqx (int *status ) { vvd ( palEqeqx( 53736. ), -0.8834195072043790156e-5, 1e-15, "palEqeqx", " ", status ); } /* E-terms */ static void t_etrms( int * status ) { double ev[3]; palEtrms ( 1976.9, ev ); vvd ( ev[0], -1.621617102537041e-6, 1e-18, "palEtrms", "X", status ); vvd ( ev[1], -3.310070088507914e-7, 1e-18, "palEtrms", "Y", status ); vvd ( ev[2], -1.435296627515719e-7, 1e-18, "palEtrms", "Z", status ); } /* J2000 to Galactic */ static void t_eqgal( int *status ) { double dl, db; palEqgal ( 5.67, -1.23, &dl, &db ); vvd ( dl, 5.612270780904526, 1e-12, "palEqgal", "DL", status ); vvd ( db, -0.6800521449061520, 1e-12, "palEqgal", "DB", status ); } /* Galactic to J2000 equatorial */ static void t_galeq( int *status ) { double dr, dd; palGaleq ( 5.67, -1.23, &dr, &dd ); vvd ( dr, 0.04729270418071426, 1e-12, "palGaleq", "DR", status ); vvd ( dd, -0.7834003666745548, 1e-12, "palGaleq", "DD", status ); } /* Galactic to supergalactic */ static void t_galsup(int *status ) { double dsl, dsb; palGalsup ( 6.1, -1.4, &dsl, &dsb ); vvd ( dsl, 4.567933268859171, 1e-12, "palGalsup", "DSL", status ); vvd ( dsb, -0.01862369899731829, 1e-12, "palGalsup", "DSB", status ); } /* Geocentric coordinates */ /* This is not from sla_test.f */ static void t_geoc( int *status ) { double r; double z; /* JCMT */ const double lat = 19.822838905884 * PAL__DD2R; const double alt = 4120.0; palGeoc( lat, alt, &r, &z ); /* Note the lower tolerance than normal since the models in SLA differ from the more up to date model in SOFA */ vvd( r, 4.01502667039618e-05, 1e-10, "palGeoc", "R", status ); vvd( z, 1.43762411970295e-05, 1e-10, "palGeoc", "Z", status ); } /* Galactic to Fk4 */ static void t_ge50 ( int *status ) { double dr, dd; palGe50( 6.1, -1.55, &dr, &dd ); vvd ( dr, 0.1966825219934508, 1e-12, "palGe50", "DR", status ); vvd ( dd, -0.4924752701678960, 1e-12, "palGe50", "DD", status ); } /* GMST */ /* We use the SOFA test values rather than the values from SLA because the precession models have changed */ static void t_gmst( int *status ) { vvd ( palGmst( 53736. ), 1.754174971870091203, 1e-12, "palGmst", " ", status ); vvd ( palGmsta( 53736., 0.0 ), 1.754174971870091203, 1e-12, "palGmsta", " ", status ); } /* FK5 */ static void t_fk52h ( int *status ) { double r5, d5, dr5, dd5, rh, dh; palFk5hz ( 1.234, -0.987, 1980, &rh, &dh ); vvd ( rh, 1.234000136713611301, 1e-13, "palFk5hz", "R", status ); vvd ( dh, -0.9869999702020807601, 1e-13, "palFk5hz", "D", status ); palHfk5z ( rh, dh, 1980, &r5, &d5, &dr5, &dd5 ); vvd ( r5, 1.234, 1e-13, "palHfk5z", "R", status ); vvd ( d5, -0.987, 1e-13, "palHfk5z", "D", status ); vvd ( dr5, 0.000000006822074, 1e-13, "palHfk5z", "DR", status ); vvd ( dd5, -0.000000002334012, 1e-13, "palHfk5z", "DD", status ); } static void t_intin( int *status ) { const char s[] = " -12345, , -0 2000 + "; /* 1234567890123456789012345678 */ int i = 1; long n = 0; int j; palIntin ( s, &i, &n, &j ); viv ( i, 10, "palIntin", "I1", status ); viv ( n, -12345, "palIntin", "V1", status ); viv ( j, -1, "palIntin", "J1", status ); palIntin ( s, &i, &n, &j ); viv ( i, 12, "palIntin", "I2", status ); viv ( n, -12345, "palIntin", "V2", status ); viv ( j, 1, "palIntin", "J2", status ); palIntin ( s, &i, &n, &j ); viv ( i, 17, "palIntin", "I3", status ); viv ( n, 0, "palIntin", "V3", status ); viv ( j, -1, "palIntin", "J3", status ); palIntin ( s, &i, &n, &j ); viv ( i, 23, "palIntin", "I4", status ); viv ( n, 2000, "palIntin", "V4", status ); viv ( j, 0, "palIntin", "J4", status ); palIntin ( s, &i, &n, &j ); viv ( i, 29, "palIntin", "I5", status ); viv ( n, 2000, "palIntin", "V5", status ); viv ( j, 1, "palIntin", "J5", status ); /* Note that strtol does not care about a + */ } /* Moon */ static void t_moon ( int *status ) { double pv[6]; double expected1[] = { 0.00229161514616454, 0.000973912029208393, 0.000669931538978146, -3.44709700068209e-09, 5.44477533462392e-09, 2.11785724844417e-09 }; /* SLA test only include slaMoon so we use the example from SUN/67 */ palDmoon( 48634.4687174074, pv ); vvec( 6, pv, expected1, "palDmoon", status ); } /* Nutation */ static void t_nut( int *status ) { double dpsi, deps, eps0; double expected[3][3] = { { 9.999999969492166e-1, 7.166577986249302e-5, 3.107382973077677e-5 }, { -7.166503970900504e-5, 9.999999971483732e-1, -2.381965032461830e-5 }, { -3.107553669598237e-5, 2.381742334472628e-5, 9.999999992335206818e-1 } }; double rmatn[3][3]; /* SLA tests with low precision */ palNut( 46012.32, rmatn ); vrmat( rmatn, expected, "palNut", 1.0e-3, status ); /* Use the SOFA tests */ palNutc( 54388.0, &dpsi, &deps, &eps0 ); vvd( eps0, 0.4090749229387258204, 1e-14, "palNutc", "eps0", status); palNutc( 53736.0, &dpsi, &deps, &eps0 ); vvd(dpsi, -0.9630912025820308797e-5, 1e-13, "palNutc", "dpsi", status); vvd(deps, 0.4063238496887249798e-4, 1e-13, "palNutc", "deps", status); } /* palPrebn */ static void t_prebn( int *status ) { double rmatp[3][3]; double prebn_expected[3][3] = { { 9.999257613786738e-1, -1.117444640880939e-2, -4.858341150654265e-3 }, { 1.117444639746558e-2, 9.999375635561940e-1, -2.714797892626396e-5 }, { 4.858341176745641e-3, -2.714330927085065e-5, 9.999881978224798e-1 }, }; palPrebn ( 1925., 1975., rmatp ); vrmat( rmatp, prebn_expected, "palPrebn", 1.0e-12, status ); } /* Range */ static void t_range( int *status ) { vvd ( palDrange ( -4 ), 2.283185307179586, 1e-12, "palDrange", " ", status ); } static void t_ranorm( int *status ) { vvd ( palDranrm ( -0.1 ), 6.183185307179587, 1e-12, "palDranrm", "2", status ); } /* Separation routines */ static void t_sep( int *status ) { double d1[3] = { 1.0, 0.1, 0.2 }; double d2[3] = { -3.0, 1e-3, 0.2 }; double ad1, bd1, ad2, bd2; palDcc2s( d1, &ad1, &bd1 ); palDcc2s( d2, &ad2, &bd2 ); vvd ( palDsep ( ad1, bd1, ad2, bd2 ), 2.8603919190246608, 1e-7, "palDsep", " ", status ); vvd ( palDsepv ( d1, d2 ), 2.8603919190246608, 1e-7, "palDsepv", " ", status ); } /* Supergalactic */ static void t_supgal( int *status ) { double dl, db; palSupgal ( 6.1, -1.4, &dl, &db ); vvd ( dl, 3.798775860769474, 1e-12, "palSupgal", "DL", status ); vvd ( db, -0.1397070490669407, 1e-12, "palSupgal", "DB", status ); } /* Test spherical tangent-plane-projection routines */ static void t_tp( int *status ) { int j; double dr0, dd0, dr1, dd1, dx, dy, dr2, dd2, dr01, dd01, dr02, dd02; dr0 = 3.1; dd0 = -0.9; dr1 = dr0 + 0.2; dd1 = dd0 - 0.1; palDs2tp( dr1, dd1, dr0, dd0, &dx, &dy, &j ); vvd( dx, 0.1086112301590404, 1e-12, "palDs2tp", "x", status ); vvd( dy, -0.1095506200711452, 1e-12, "palDs2tp", "y", status ); viv( j, 0, "palDs2tp", "j", status ); palDtp2s( dx, dy, dr0, dd0, &dr2, &dd2 ); vvd( dr2 - dr1, 0., 1e-12, "palDtp2s", "r", status ); vvd( dd2 - dd1, 0., 1e-12, "palDtp2s", "d", status ); palDtps2c( dx, dy, dr2, dd2, &dr01, &dd01, &dr02, &dd02, &j ); vvd( dr01, 3.1, 1e-12, "palDtps2c", "r1", status); vvd( dd01, -0.9, 1e-12, "palDtps2c", "d1", status); vvd( dr02, 0.3584073464102072, 1e-12, "palDtps2c", "r2", status); vvd( dd02, -2.023361658234722, 1e-12, "palDtps2c", "d2", status ); viv( j, 1, "palDtps2c", "n", status ); } /* Test all the 3-vector and 3x3 matrix routines. */ static void t_vecmat( int * status ) { int i; /* palDav2m */ double drm1[3][3]; double dav[3] = { -0.123, 0.0987, 0.0654 }; double dav2m_expected[3][3] = { { 0.9930075842721269, 0.05902743090199868, -0.1022335560329612 }, { -0.07113807138648245, 0.9903204657727545, -0.1191836812279541 }, { 0.09420887631983825, 0.1256229973879967, 0.9875948309655174 }, }; /* palDeuler */ double drm2[3][3]; double deuler_expected[3][3] = { { -0.1681574770810878, 0.1981362273264315, 0.9656423242187410 }, { -0.2285369373983370, 0.9450659587140423, -0.2337117924378156 }, { -0.9589024617479674, -0.2599853247796050, -0.1136384607117296 } }; /* palDmxm */ double drm[3][3]; double dmxm_expected[3][3] = { { -0.09010460088585805, 0.3075993402463796, 0.9472400998581048 }, { -0.3161868071070688, 0.8930686362478707, -0.3200848543149236 }, { -0.9444083141897035, -0.3283459407855694, 0.01678926022795169 }, }; /* palDcs2c et al */ double dv1[3]; double dv2[3]; double dv3[3]; double dv4[3]; double dv5[3]; double dv6[3]; double dv7[3]; double dvm; /* palDav2m */ palDav2m( dav, drm1 ); vrmat( drm1, dav2m_expected, "palDav2m", 1.0e-12, status ); /* Test palDeuler */ palDeuler( "YZY", 2.345, -0.333, 2.222, drm2 ); vrmat( drm2, deuler_expected, "palDeuler", 1.0e-12, status ); /* palDmxm */ palDmxm( drm2, drm1, drm ); vrmat( drm, dmxm_expected, "palDmxm", 1.0e-12, status ); /* palDcs2c */ palDcs2c( 3.0123, -0.999, dv1 ); vvd ( dv1[0], -0.5366267667260525, 1e-12, "palDcs2c", "x", status ); vvd ( dv1[1], 0.06977111097651444, 1e-12, "palDcs2c", "y", status ); vvd ( dv1[2], -0.8409302618566215, 1e-12, "palDcs2c", "z", status ); /* palDmxv */ palDmxv( drm1, dv1, dv2 ); palDmxv( drm2, dv2, dv3 ); vvd ( dv3[0], -0.7267487768696160, 1e-12, "palDmxv", "x", status ); vvd ( dv3[1], 0.5011537352639822, 1e-12, "palDmxv", "y", status ); vvd ( dv3[2], 0.4697671220397141, 1e-12, "palDmxv", "z", status ); /* palDimxv */ palDimxv( drm, dv3, dv4 ); vvd ( dv4[0], -0.5366267667260526, 1e-12, "palDimxv", "X", status ); vvd ( dv4[1], 0.06977111097651445, 1e-12, "palDimxv", "Y", status ); vvd ( dv4[2], -0.8409302618566215, 1e-12, "palDimxv", "Z", status ); /* palDm2av */ palDm2av( drm, dv5 ); vvd ( dv5[0], 0.006889040510209034, 1e-12, "palDm2av", "X", status ); vvd ( dv5[1], -1.577473205461961, 1e-12, "palDm2av", "Y", status ); vvd ( dv5[2], 0.5201843672856759, 1e-12, "palDm2av", "Z", status ); for (i=0; i<3; i++) { dv5[i] *= 1000.0; } /* palDvn */ palDvn( dv5, dv6, &dvm ); vvd ( dv6[0], 0.004147420704640065, 1e-12, "palDvn", "X", status ); vvd ( dv6[1], -0.9496888606842218, 1e-12, "palDvn", "Y", status ); vvd ( dv6[2], 0.3131674740355448, 1e-12, "palDvn", "Z", status ); vvd ( dvm, 1661.042127339937, 1e-9, "palDvn", "M", status ); vvd ( palDvdv ( dv6, dv1 ), -0.3318384698006295, 1e-12, "palDvn", " ", status ); /* palDvxv */ palDvxv( dv6, dv1, dv7 ); vvd ( dv7[0], 0.7767720597123304, 1e-12, "palDvxv", "X", status ); vvd ( dv7[1], -0.1645663574562769, 1e-12, "palDvxv", "Y", status ); vvd ( dv7[2], -0.5093390925544726, 1e-12, "palDvxv", "Z", status ); } static void t_ecmat( int *status ) { double rmat[3][3]; double expected[3][3] = { { 1.0, 0.0, 0.0 }, { 0.0, 0.91749307789883549624, 0.3977517467060596168 }, { 0.0, -0.3977517467060596168, 0.91749307789883549624 } }; palEcmat( 55966.46, rmat ); vrmat( rmat, expected, "palEcmat", 1.0e-12, status ); } static void t_eqecl ( int *status ) { double dl, db; palEqecl ( 0.789, -0.123, 46555, &dl, &db ); /* Slight changes from SLA for 2006 precession/nutation */ vvd ( dl, 0.7036566430349022, 1e-6, "palEqecl", "L", status ); vvd ( db, -0.4036047164116848, 1e-6, "palEqecl", "B", status ); } static void t_prec( int *status ) { double rmat[3][3]; double expected[3][3] = { { 0.9999856154510, -0.0049192906204, -0.0021376320580 }, { 0.0049192906805, 0.9999879002027, -5.2297405698747e-06 }, { 0.0021376319197, -5.2859681191735e-06, 0.9999977152483 } }; palPrec( 1990.0, 2012.0, rmat ); vrmat( rmat, expected, "palPrec", 1.0e-12, status ); } static void t_preces( int *status ) { double ra; double dc; ra = 6.28; dc = -1.123; palPreces ( "FK4", 1925, 1950, &ra, &dc ); vvd ( ra, 0.002403604864728447, 1e-12, "palPreces", "R", status ); vvd ( dc, -1.120570643322045, 1e-12, "palPreces", "D", status ); /* This is the SLA test but PAL now uses the IAU 2006 precession model so we need to loosen the comparison */ ra = 0.0123; dc = 1.0987; palPreces ( "FK5", 2050, 1990, &ra, &dc ); vvd ( ra, 6.282003602708382, 1e-6, "palPreces", "R", status ); vvd ( dc, 1.092870326188383, 1e-6, "palPreces", "D", status ); } static void t_evp( int *status ) { double dvb[3],dpb[3],dvh[3],dph[3]; double vbex[3] = { 1.6957348127008098514e-07, -9.1093446116039685966e-08, -3.9528532243991863036e-08 }; double pbex[3] = {-0.49771075259730546136, -0.80273812396332311359, -0.34851593942866060383 }; double vhex[3] = { 1.6964379181455713805e-07, -9.1147224045727438391e-08, -3.9553158272334222497e-08 }; double phex[3] = { -0.50169124421419830639, -0.80650980174901798492, -0.34997162028527262212 }; double vbex2[3] = { -0.0109187426811683, -0.0124652546173285, -0.0054047731809662 }; double pbex2[3] = { -0.7714104440491060, +0.5598412061824225, +0.2425996277722475 }; double vhex2[3] = { -0.0109189182414732, -0.0124718726844084, -0.0054075694180650 }; double phex2[3] = { -0.7757238809297653, +0.5598052241363390, +0.2426998466481708 }; palEvp( 2010.0, 2012.0, dvb, dpb, dvh, dph ); vvec( 3, dvb, vbex, "palEvp", status ); vvec( 3, dpb, pbex, "palEvp", status ); vvec( 3, dvh, vhex, "palEvp", status ); vvec( 3, dph, phex, "palEvp", status ); palEpv ( 53411.52501161, dph, dvh, dpb, dvb ); vvec( 3, dvb, vbex2, "palEpv", status ); vvec( 3, dpb, pbex2, "palEpv", status ); vvec( 3, dvh, vhex2, "palEpv", status ); vvec( 3, dph, phex2, "palEpv", status ); } static void t_map( int *status ) { double ra, da; palMap ( 6.123, -0.999, 1.23e-5, -0.987e-5, 0.123, 32.1, 1999, 43210.9, &ra, &da ); /* These are the SLA tests but and they agree to 0.1 arcsec with PAL/SOFA. We expect a slight difference from the change to nutation models. */ vvd ( ra, 6.117130429775647, 1e-6, "palMap", "RA", status ); vvd ( da, -1.000880769038632, 1e-8, "palMap", "DA", status ); } static void t_mappa( int *status ) { double amprms[21]; double expected[21] = {1.9986310746064646082, -0.1728200754134739392, 0.88745394651412767839, 0.38472374350184274094, -0.17245634725219796679, 0.90374808622520386159, 0.3917884696321610738, 2.0075929387510784968e-08, -9.9464149073251757597e-05, -1.6125306981057062306e-05, -6.9897255793245634435e-06, 0.99999999489900059935, 0.99999983777998024959, -0.00052248206600935195865, -0.00022683144398381763045, 0.00052248547063364874764, 0.99999986339269864022, 1.4950491424992534218e-05, 0.00022682360163333854623, -1.5069005133483779417e-05, 0.99999997416198904698}; palMappa( 2010.0, 55927.0, amprms ); vvec( 21, amprms, expected, "palMappa", status ); } static void t_mapqkz( int *status ) { double amprms[21], ra, da; palMappa( 2010.0, 55927.0, amprms ); palMapqkz( 1.234, -0.567, amprms, &ra, &da ); vvd( ra, 1.2344879748414849807, 1.0E-12, "palMapqkz", "ra", status ); vvd( da, -0.56697099554368701746, 1.0E-12, "palMapqkz", "da", status ); /* Try the same with palMapqk and zero parallax and proper motion */ palMapqk( 1.234, -0.567, 0., 0., 0., 0., amprms, &ra, &da ); vvd( ra, 1.2344879748414849807, 1.0E-7, "palMapqkz", "ra", status ); vvd( da, -0.56697099554368701746, 1.0E-7, "palMapqkz", "da", status ); } static void t_ampqk( int *status ) { double amprms[21], rm, dm; palMappa( 2010.0, 55927.0, amprms ); palAmpqk( 1.234, -0.567, amprms, &rm, &dm ); vvd( rm, 1.2335120411026936349, 1.0E-12, "palAmpqk", "rm", status ); vvd( dm, -0.56702908706930343907, 1.0E-12, "palAmpqk", "dm", status ); } static void t_fk45z( int *status ) { double r2000, d2000; palFk45z( 1.2, -0.3, 1960.0, &r2000, &d2000 ); vvd( r2000, 1.2097812228966762227, 1.0E-12, "palFk45z", "r2000", status ); vvd( d2000, -0.29826111711331398935, 1.0E-12, "palFk45z", "d2000", status ); } static void t_fk54z( int *status ) { double r1950, d1950, dr1950, dd1950; palFk54z( 1.2, -0.3, 1960.0, &r1950, &d1950, &dr1950, &dd1950 ); vvd( r1950, 1.1902221805755279771, 1.0E-12, "palFk54z", "r1950", status ); vvd( d1950, -0.30178317645793828472, 1.0E-12, "palFk54z", "d1950", status ); vvd( dr1950, -1.7830874775952945507e-08, 1.0E-12, "palFk54z", "dr1950", status ); vvd( dd1950, 7.196059425334821089e-09, 1.0E-12, "palFk54z", "dd1950", status ); } static void t_flotin( int * status ) { int j; const char * s = " 12.345, , -0 1E3-4 2000 E "; /* 123456789012345678901234567890123 */ int i = 1; double dv = 0.0; palDfltin ( s, &i, &dv, &j ); viv ( i, 10, "palDfltin", "I1", status ); vvd ( dv, 12.345, 1e-12, "palDfltin", "V1", status ); viv ( j, 0, "palDfltin", "J1", status ); palDfltin ( s, &i, &dv, &j ); viv ( i, 12, "palDfltin", "I2", status ); vvd ( dv, 12.345, 1e-12, "palDfltin", "V2", status ); viv ( j, 1, "palDfltin", "J2", status ); palDfltin ( s, &i, &dv, &j ); viv ( i, 16, "palDfltin", "I3", status ); vvd ( dv, 0, 0, "palDfltin", "V3", status ); viv ( j, -1, "palDfltin", "J3", status ); palDfltin ( s, &i, &dv, &j ); viv ( i, 19, "palDfltin", "I4", status ); vvd ( dv, 1000, 0, "palDfltin", "V4", status ); viv ( j, 0, "palDfltin", "J4", status ); palDfltin ( s, &i, &dv, &j ); viv ( i, 22, "palDfltin", "I5", status ); vvd ( dv, -4, 0, "palDfltin", "V5", status ); viv ( j, -1, "palDfltin", "J5", status ); palDfltin ( s, &i, &dv, &j ); viv ( i, 28, "palDfltin", "I6", status ); vvd ( dv, 2000, 0, "palDfltin", "V6", status ); viv ( j, 0, "palDfltin", "J6", status ); palDfltin ( s, &i, &dv, &j ); viv ( i, 34, "palDfltin", "I7", status ); vvd ( dv, 2000, 0, "palDfltin", "V7", status ); viv ( j, 1, "palDfltin", "J7", status ); /* differs from slaDfltin */ /* Now test overflow and underflow */ i = 1; palDfltin( " 1D600 ", &i, &dv, &j ); viv ( i, 8, "palDfltin", "I8", status ); vvd ( dv, HUGE_VAL, 0, "palDfltin", "V8", status ); viv ( j, 2, "palDfltin", "J8", status ); } static void t_obs( int * status ) { char shortname[11]; char longname[41]; double w, p, h; int lstat; lstat = palObs( 0, "MMT", shortname, sizeof(shortname), longname, sizeof(longname), &w, &p, &h ); vcs ( shortname, "MMT", "palObs", "1/C", status ); vcs ( longname, "MMT 6.5m, Mt Hopkins", "palObs", "1/NAME", status ); vvd ( w, 1.935300584055477, 1e-8, "palObs", "1/W", status ); vvd ( p, 0.5530735081550342238, 1e-10, "palObs", "1/P", status ); vvd ( h, 2608, 1e-10, "palObs", "1/H", status ); viv( lstat, 0, "palObs", "retval", status ); lstat = palObs ( 61, NULL, shortname, sizeof(shortname), longname, sizeof(longname), &w, &p, &h ); vcs ( shortname, "KECK1", "palObs", "2/C", status ); vcs ( longname, "Keck 10m Telescope #1", "palObs", "2/NAME", status ); vvd ( w, 2.713545757918895, 1e-8, "palObs", "2/W", status ); vvd ( p, 0.3460280563536619, 1e-8, "palObs", "2/P", status ); vvd ( h, 4160, 1e-10, "palObs", "2/H", status ); viv( lstat, 0, "palObs", "retval", status ); lstat = palObs ( 83, NULL, shortname, sizeof(shortname), longname, sizeof(longname), &w, &p, &h ); vcs ( shortname, "MAGELLAN2", "palObs", "3/C", status ); vcs ( longname, "Magellan 2, 6.5m, Las Campanas", "palObs", "3/NAME", status ); vvd ( w, 1.233819305534497, 1e-8, "palObs", "3/W", status ); vvd ( p, -0.506389344359954, 1e-8, "palObs", "3/P", status ); vvd ( h, 2408, 1e-10, "palObs", "3/H", status ); viv( lstat, 0, "palObs", "retval", status ); /* the first argument here should be 1 greater than the number of items * in const struct telData defined in palObs.c */ lstat = palObs ( 86, NULL, shortname, sizeof(shortname), longname, sizeof(longname), &w, &p, &h ); vcs ( longname, "?", "palObs", "4/NAME", status ); viv( lstat, -1, "palObs", "retval", status ); lstat = palObs ( 0, "MISSING", shortname, sizeof(shortname), longname, sizeof(longname), &w, &p, &h ); vcs ( longname, "?", "palObs", "5/NAME", status ); viv( lstat, -1, "palObs", "retval", status ); lstat = palObs( 0, "mmt", shortname, sizeof(shortname), longname, sizeof(longname), &w, &p, &h ); vcs ( shortname, "MMT", "palObs", "6/C", status ); vcs ( longname, "MMT 6.5m, Mt Hopkins", "palObs", "6/NAME", status ); vvd ( w, 1.935300584055477, 1e-8, "palObs", "6/W", status ); vvd ( p, 0.5530735081550342238, 1e-10, "palObs", "6/P", status ); vvd ( h, 2608, 1e-10, "palObs", "6/H", status ); viv( lstat, 0, "palObs", "retval", status ); } static void t_pa( int *status ) { vvd ( palPa ( -1.567, 1.5123, 0.987 ), -1.486288540423851, 1e-12, "palPa", " ", status ); vvd ( palPa ( 0, 0.789, 0.789 ), 0, 0, "palPa", "zenith", status ); } static void t_planet( int * status ) { int j; double pv[6]; double u[13]; double expected1[6] = { 0., 0., 0., 0., 0., 0. }; double expectedue1[13] = { 1.000878908362435284, -0.3336263027874777288, 50000., 2.840425801310305210, 0.1264380368035014224, -0.2287711835229143197, -0.01301062595106185195, 0.5657102158104651697, 0.2189745287281794885, 2.852427310959998500, -0.01552349065435120900, 50000., 0.0 }; double expectedue2[13] = { 1.00006, -4.856142884511782, 50000., 0.3, -0.2, 0.1, -0.4520378601821727, 0.4018114312730424, -.3515850023639121, 0.3741657386773941, -0.2511321445456515, 50000., 0. }; double expectedue3[13] = { 1.000000000000000, -0.3329769417028020949, 50100., 2.638884303608524597, 1.070994304747824305, 0.1544112080167568589, -0.2188240619161439344, 0.5207557453451906385, 0.2217782439275216936, 2.852118859689216658, 0.01452010174371893229, 50100. }; double expectedpv[6] = { 0.07944764084631667011, -0.04118141077419014775, 0.002915180702063625400, -0.6890132370721108608e-6, 0.4326690733487621457e-6, -0.1763249096254134306e-6, }; double expectedpv2[6] = { 1.947628959288897677, -1.013736058752235271, -0.3536409947732733647, 2.742247411571786194e-8, 1.170467244079075911e-7, 3.709878268217564005e-8 }; double ra,dec,diam, r; int jform; double epoch, orbinc, anode, perih, aorq, e, aorl, dm; /* palEl2ue */ palEl2ue ( 50000, 1, 49000, 0.1, 2, 0.2, 3, 0.05, 3, 0.003312, u, &j ); vvec( 13, u, expectedue1, "palEl2ue", status ); viv ( j, 0, "palEl2ue", "J", status ); /* palPertel */ palPertel ( 2, 43000., 43200., 43000., 0.2, 3, 4, 5, 0.02, 6, &epoch, &orbinc, &anode, &perih, &aorq, &e, &aorl, &j ); vvd ( epoch, 43200., 1e-10, "palPertel", "EPOCH", status ); vvd ( orbinc, 0.1995661466545422381, 1e-7, "palPertel", "ORBINC", status ); vvd ( anode, 2.998052737821591215, 1e-7, "palPertel", "ANODE", status ); vvd ( perih, 4.009516448441143636, 1e-6, "palPertel", "PERIH", status ); vvd ( aorq, 5.014216294790922323, 1e-7, "palPertel", "AORQ", status ); vvd ( e, 0.02281386258309823607, 1e-7, "palPertel", "E", status ); vvd ( aorl, 0.01735248648779583748, 1e-6, "palPertel", "AORL", status ); viv ( j, 0, "palPertel", "J", status ); /* palPertue */ palPertue ( 50100, u, &j ); vvec( 13, u, expectedue3, "palPertue", status ); viv ( j, 0, "palPertue", "J", status ); /* palPlanel */ palPlanel ( 50600, 2, 50500, 0.1, 3, 5, 2, 0.3, 4, 0, pv, &j ); vvec( 6, pv, expectedpv2, "palPlanel", status ); viv ( j, 0, "palPlanel", "J", status ); /* palPlanet */ palPlanet( 1e6, 0, pv, &j ); vvec( 6, pv, expected1, "palPlanet 1", status ); viv ( j, -1, "palPlanet", "J 1", status ); palPlanet( 1e6, 9, pv, &j); viv ( j, -1, "palPlanet", "J 2", status ); palPlanet ( -320000, 3, pv, &j ); vvd ( pv[0], 0.9308038666827242603, 1e-11, "palPlanet", "pv[0] 3", status ); vvd ( pv[1], 0.3258319040252137618, 1e-11, "palPlanet", "pv[1] 3", status ); vvd ( pv[2], 0.1422794544477122021, 1e-11, "palPlanet", "pv[2] 3", status ); vvd ( pv[3], -7.441503423889371696e-8, 1e-17, "palPlanet", "pv[3] 3", status ); vvd ( pv[4], 1.699734557528650689e-7, 1e-17, "palPlanet", "pv[4] 3", status ); vvd ( pv[5], 7.415505123001430864e-8, 1e-17, "palPlanet", "pv[5] 3", status ); viv ( j, 1, "palPlanet", "J 3", status ); palPlanet ( 43999.9, 1, pv, &j ); vvd ( pv[0], 0.2945293959257422246, 1e-11, "palPlanet", "pv[0] 4", status ); vvd ( pv[1], -0.2452204176601052181, 1e-11, "palPlanet", "pv[1] 4", status ); vvd ( pv[2], -0.1615427700571978643, 1e-11, "palPlanet", "pv[2] 4", status ); vvd ( pv[3], 1.636421147459047057e-7, 1e-18, "palPlanet", "pv[3] 4", status ); vvd ( pv[4], 2.252949422574889753e-7, 1e-18, "palPlanet", "pv[4] 4", status ); vvd ( pv[5], 1.033542799062371839e-7, 1e-18, "palPlanet", "pv[5] 4", status ); viv ( j, 0, "palPlanet", "J 4", status ); /* palPlante test would go here */ palPlante ( 50600., -1.23, 0.456, 2, 50500., 0.1, 3., 5., 2., 0.3, 4., 0., &ra, &dec, &r, &j ); vvd ( ra, 6.222958101333794007, 1e-6, "palPlante", "RA", status ); vvd ( dec, 0.01142220305739771601, 1e-6, "palPlante", "DEC", status ); vvd ( r, 2.288902494080167624, 1e-8, "palPlante", "R", status ); viv ( j, 0, "palPlante", "J", status ); u[0] = 1.0005; u[1] = -0.3; u[2] = 55000.; u[3] = 2.8; u[4] = 0.1; u[5] = -0.2; u[6] = -0.01; u[7] = 0.5; u[8] = 0.22; u[9] = 2.8; u[10] = -0.015; u[11] = 55001.; u[12] = 0; /* palPlantu */ palPlantu ( 55001., -1.23, 0.456, u, &ra, &dec, &r, &j ); vvd ( ra, 0.3531814831241686647, 1e-6, "palPlantu", "RA", status ); vvd ( dec, 0.06940344580567131328, 1e-6, "palPlantu", "DEC", status ); vvd ( r, 3.031687170873274464, 1e-8, "palPlantu", "R", status ); viv ( j, 0, "palPlantu", "J", status ); /* palPv2el */ pv[0] = 0.3; pv[1] = -0.2; pv[2] = 0.1; pv[3] = -0.9e-7; pv[4] = 0.8e-7; pv[5] = -0.7e-7; palPv2el ( pv, 50000, 0.00006, 1, &jform, &epoch, &orbinc, &anode, &perih, &aorq, &e, &aorl, &dm, &j ); viv ( jform, 1, "palPv2el", "JFORM", status ); vvd ( epoch, 50000, 1e-10, "palPv2el", "EPOCH", status ); vvd ( orbinc, 1.52099895268912, 1e-12, "palPv2el", "ORBINC", status ); vvd ( anode, 2.720503180538650, 1e-12, "palPv2el", "ANODE", status ); vvd ( perih, 2.194081512031836, 1e-12, "palPv2el", "PERIH", status ); vvd ( aorq, 0.2059371035373771, 1e-12, "palPv2el", "AORQ", status ); vvd ( e, 0.9866822985810528, 1e-12, "palPv2el", "E", status ); vvd ( aorl, 0.2012758344836794, 1e-12, "palPv2el", "AORL", status ); vvd ( dm, 0.1840740507951820, 1e-12, "palPv2el", "DM", status ); viv ( j, 0, "palPv2el", "J", status ); /* palPv2ue */ palPv2ue ( pv, 50000., 0.00006, u, &j ); vvec( 13, u, expectedue2, "palPv2ue", status ); viv ( j, 0, "palPv2ue", "J", status ); /* Planets */ palRdplan ( 40999.9, 0, 0.1, -0.9, &ra, &dec, &diam ); vvd ( ra, 5.772270359389275837, 1e-6, "palRdplan", "ra 0", status ); vvd ( dec, -0.2089207338795416192, 1e-7, "palRdplan", "dec 0", status ); vvd ( diam, 9.415338935229717875e-3, 1e-10, "palRdplan", "diam 0", status ); palRdplan ( 41999.9, 1, 1.1, -0.9, &ra, &dec, &diam ); vvd ( ra, 3.866363420052936653, 1e-6, "palRdplan", "ra 1", status ); vvd ( dec, -0.2594430577550113130, 1e-7, "palRdplan", "dec 1", status ); vvd ( diam, 4.638468996795023071e-5, 1e-14, "palRdplan", "diam 1", status ); palRdplan ( 42999.9, 2, 2.1, 0.9, &ra, &dec, &diam ); vvd ( ra, 2.695383203184077378, 1e-6, "palRdplan", "ra 2", status ); vvd ( dec, 0.2124044506294805126, 1e-7, "palRdplan", "dec 2", status ); vvd ( diam, 4.892222838681000389e-5, 1e-14, "palRdplan", "diam 2", status ); palRdplan ( 43999.9, 3, 3.1, 0.9, &ra, &dec, &diam ); vvd ( ra, 2.908326678461540165, 1e-7, "palRdplan", "ra 3", status ); vvd ( dec, 0.08729783126905579385, 1e-7, "palRdplan", "dec 3", status ); vvd ( diam, 8.581305866034962476e-3, 1e-7, "palRdplan", "diam 3", status ); palRdplan ( 44999.9, 4, -0.1, 1.1, &ra, &dec, &diam ); vvd ( ra, 3.429840787472851721, 1e-6, "palRdplan", "ra 4", status ); vvd ( dec, -0.06979851055261161013, 1e-7, "palRdplan", "dec 4", status ); vvd ( diam, 4.540536678439300199e-5, 1e-14, "palRdplan", "diam 4", status ); palRdplan ( 45999.9, 5, -1.1, 0.1, &ra, &dec, &diam ); vvd ( ra, 4.864669466449422548, 1e-6, "palRdplan", "ra 5", status ); vvd ( dec, -0.4077714497908953354, 1e-7, "palRdplan", "dec 5", status ); vvd ( diam, 1.727945579027815576e-4, 1e-14, "palRdplan", "diam 5", status ); palRdplan ( 46999.9, 6, -2.1, -0.1, &ra, &dec, &diam ); vvd ( ra, 4.432929829176388766, 1e-6, "palRdplan", "ra 6", status ); vvd ( dec, -0.3682820877854730530, 1e-7, "palRdplan", "dec 6", status ); vvd ( diam, 8.670829016099083311e-5, 1e-14, "palRdplan", "diam 6", status ); palRdplan ( 47999.9, 7, -3.1, -1.1, &ra, &dec, &diam ); vvd ( ra, 4.894972492286818487, 1e-6, "palRdplan", "ra 7", status ); vvd ( dec, -0.4084068901053653125, 1e-7, "palRdplan", "dec 7", status ); vvd ( diam, 1.793916783975974163e-5, 1e-14, "palRdplan", "diam 7", status ); palRdplan ( 48999.9, 8, 0, 0, &ra, &dec, &diam ); vvd ( ra, 5.066050284760144000, 1e-6, "palRdplan", "ra 8", status ); vvd ( dec, -0.3744690779683850609, 1e-7, "palRdplan", "dec 8", status ); vvd ( diam, 1.062210086082700563e-5, 1e-14, "palRdplan", "diam 8", status ); /* palUe2el */ palUe2el ( u, 1, &jform, &epoch, &orbinc, &anode, &perih, &aorq, &e, &aorl, &dm, &j ); viv ( jform, 1, "palUe2el", "JFORM", status ); vvd ( epoch, 50000.00000000000, 1e-10, "palUe2el", "EPOCH", status ); vvd ( orbinc, 1.520998952689120, 1e-12, "palUe2el", "ORBINC", status ); vvd ( anode, 2.720503180538650, 1e-12, "palUe2el", "ANODE", status ); vvd ( perih, 2.194081512031836, 1e-12, "palUe2el", "PERIH", status ); vvd ( aorq, 0.2059371035373771, 1e-12, "palUe2el", "AORQ", status ); vvd ( e, 0.9866822985810528, 1e-12, "palUe2el", "E", status ); vvd ( aorl, 0.2012758344836794, 1e-12, "palUe2el", "AORL", status ); viv ( j, 0, "palUe2el", "J", status ); /* palUe2pv */ palUe2pv( 50010., u, pv, &j ); /* Update the final two elements of the expecte UE array */ expectedue2[11] = 50010.; expectedue2[12] = 0.7194308220038886856; vvec( 13, u, expectedue2, "palUe2pv", status ); vvec( 6, pv, expectedpv, "palUe2pv", status ); viv ( j, 0, "palUe2pv", "J", status ); } static void t_pm( int * status ) { double ra2, dec2; double ra1, dec1, pmr1, pmd1, px1, rv1; ra1 = 5.43; dec1 = -0.87; pmr1 = -0.33e-5; pmd1 = 0.77e-5; px1 = 0.7; rv1 = 50.3*365.2422/365.25; palPm ( ra1, dec1, pmr1, pmd1, px1, rv1, 1899, 1943, &ra2, &dec2 ); vvd ( ra2, 5.429855087793875, 1e-10, "palPm", "R", status ); vvd ( dec2, -0.8696617307805072, 1e-10, "palPm", "D", status ); /* SOFA test */ ra1 = 0.01686756; dec1 = -1.093989828; pmr1 = -1.78323516e-5; pmd1 = 2.336024047e-6; px1 = 0.74723; rv1 = -21.6; palPm(ra1, dec1, pmr1, pmd1, px1, rv1, palEpj(50083.0), palEpj(53736.0), &ra2, &dec2); vvd(ra2, 0.01668919069414242368, 1e-13, "palPm", "ra", status); vvd(dec2, -1.093966454217127879, 1e-13, "palPm", "dec", status); } static void t_pvobs( int *status ) { double pv[6]; double expected[6] = { -4.7683600138836167813e-06, 1.0419056712717953176e-05, 4.099831053320363277e-05, -7.5976959740661272483e-10, -3.4771429582640930371e-10, 0.0}; palPvobs( 1.3, 10000.0, 2.0, pv ); vvec( 6, pv, expected, "palPvobs", status ); } static void t_rv( int *status ) { vvd ( palRverot ( -0.777, 5.67, -0.3, 3.19 ), -0.1948098355075913, 1e-6, "palRverot", " ", status ); vvd ( palRvgalc ( 1.11E0, -0.99E0 ), 158.9630759840254, 1e-3, "palRvgalc", " ", status ); vvd ( palRvlg ( 3.97E0, 1.09E0 ), -197.818762175363, 1e-3, "palRvlg", " ", status ); vvd ( palRvlsrd ( 6.01E0, 0.1E0 ), -4.082811335150567, 1e-4, "palRvlsrd", " ", status ); vvd ( palRvlsrk ( 6.01E0, 0.1E0 ), -5.925180579830265, 1e-4, "palRvlsrk", " ", status ); } static void t_rvgalc( int *status ) { double rv; rv = palRvgalc( 2.7, -1.0 ); vvd( rv, 213.98084425751144977, 1.0E-12, "palRvgalc", "rv", status ); } static void t_rvlg( int *status ) { double rv; rv = palRvlg( 2.7, -1.0 ); vvd( rv, 291.79205281252404802, 1.0E-12, "palRvlg", "rv", status ); } static void t_rvlsrd( int *status ) { double rv; rv = palRvlsrd( 2.7, -1.0 ); vvd( rv, 9.620674692097630043, 1.0E-12, "palRvlsrd", "rv", status ); } static void t_rvlsrk( int *status ) { double rv; rv = palRvlsrk( 2.7, -1.0 ); vvd( rv, 12.556356851411955233, 1.0E-12, "palRvlsrk", "rv", status ); } static void t_refco( int *status ) { double phpa, tc, rh, wl, refa, refb; phpa = 800.0; tc = 10.0 + 273.15; /* SLA uses kelvin */ rh = 0.9; wl = 0.4; palRefcoq(tc, phpa, rh, wl, &refa, &refb); vvd(refa, 0.2264949956241415009e-3, 1e-15, "palRefcoq", "refa", status); vvd(refb, -0.2598658261729343970e-6, 1e-18, "palRefcoq", "refb", status); } static void t_ref( int *status ) { double ref, refa, refb, refa2, refb2, vu[3], vr[3], zr; palRefro( 1.4, 3456.7, 280, 678.9, 0.9, 0.55, -0.3, 0.006, 1e-9, &ref ); vvd( ref, 0.00106715763018568, 1e-12, "palRefro", "o", status ); palRefro( 1.4, 3456.7, 280, 678.9, 0.9, 1000, -0.3, 0.006, 1e-9, &ref ); vvd( ref, 0.001296416185295403, 1e-12, "palRefro", "r", status ); palRefcoq( 275.9, 709.3, 0.9, 101, &refa, &refb ); vvd( refa, 2.324736903790639e-4, 1e-12, "palRefcoq", "a/r", status ); vvd( refb, -2.442884551059e-7, 1e-15, "palRefcoq", "b/r", status ); palRefco( 2111.1, 275.9, 709.3, 0.9, 101, -1.03, 0.0067, 1e-12, &refa, &refb ); vvd( refa, 2.324673985217244e-4, 1e-12, "palRefco", "a/r", status ); vvd( refb, -2.265040682496e-7, 1e-15, "palRefco", "b/r", status ); palRefcoq( 275.9, 709.3, 0.9, 0.77, &refa, &refb ); vvd( refa, 2.007406521596588e-4, 1e-12, "palRefcoq", "a", status ); vvd( refb, -2.264210092590e-7, 1e-15, "palRefcoq", "b", status ); palRefco( 2111.1, 275.9, 709.3, 0.9, 0.77, -1.03, 0.0067, 1e-12, &refa, &refb ); vvd( refa, 2.007202720084551e-4, 1e-12, "palRefco", "a", status ); vvd( refb, -2.223037748876e-7, 1e-15, "palRefco", "b", status ); palAtmdsp ( 275.9, 709.3, 0.9, 0.77, refa, refb, 0.5, &refa2, &refb2 ); vvd ( refa2, 2.034523658888048e-4, 1e-12, "palAtmdsp", "a", status ); vvd ( refb2, -2.250855362179e-7, 1e-15, "palAtmdsp", "b", status ); palDcs2c ( 0.345, 0.456, vu ); palRefv ( vu, refa, refb, vr ); vvd ( vr[0], 0.8447487047790478, 1e-12, "palRefv", "x1", status ); vvd ( vr[1], 0.3035794890562339, 1e-12, "palRefv", "y1", status ); vvd ( vr[2], 0.4407256738589851, 1e-12, "palRefv", "z1", status ); palDcs2c ( 3.7, 0.03, vu ); palRefv ( vu, refa, refb, vr ); vvd ( vr[0], -0.8476187691681673, 1e-12, "palRefv", "x2", status ); vvd ( vr[1], -0.5295354802804889, 1e-12, "palRefv", "y2", status ); vvd ( vr[2], 0.0322914582168426, 1e-12, "palRefv", "z2", status ); palRefz ( 0.567, refa, refb, &zr ); vvd ( zr, 0.566872285910534, 1e-12, "palRefz", "hi el", status ); palRefz ( 1.55, refa, refb, &zr ); vvd ( zr, 1.545697350690958, 1e-12, "palRefz", "lo el", status ); } /**********************************************************************/ int main (void) { /* Use the SLA and SOFA conventions */ int status = 0; /* Unix and SAE convention */ t_addet(&status); t_afin(&status); t_ampqk(&status); t_aop(&status); t_airmas(&status); t_amp(&status); t_bear(&status); t_caf2r(&status); t_caldj(&status); t_cc2s(&status); t_cd2tf(&status); t_cldj(&status); t_cr2af(&status); t_cr2tf(&status); t_ctf2d(&status); t_ctf2r(&status); t_dat(&status); t_djcal(&status); t_dmat(&status); t_epb(&status); t_epb2d(&status); t_epco(&status); t_epj(&status); t_epj2d(&status); t_eqecl(&status); t_eqeqx(&status); t_etrms(&status); t_eqgal(&status); t_evp(&status); t_fk45z(&status); t_fk54z(&status); t_flotin(&status); t_galeq(&status); t_galsup(&status); t_ge50(&status); t_geoc(&status); t_gmst(&status); t_fk52h(&status); t_intin(&status); t_prec(&status); t_preces(&status); t_ecmat(&status); t_e2h(&status); t_map(&status); t_mappa(&status); t_mapqkz(&status); t_moon(&status); t_nut(&status); t_obs(&status); t_pa(&status); t_planet(&status); t_pm(&status); t_prebn(&status); t_pvobs(&status); t_range(&status); t_ranorm(&status); t_ref(&status); t_refco(&status); t_rv(&status); t_rvgalc(&status); t_rvlg(&status); t_rvlsrd(&status); t_rvlsrk(&status); t_sep(&status); t_supgal(&status); t_tp(&status); t_vecmat(&status); return status; } pal-0.5.0/palUe2el.c000644 000765 000024 00000021774 12366000607 014226 0ustar00timjstaff000000 000000 /* *+ * Name: * palUe2el * Purpose: * Universal elements to heliocentric osculating elements * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palUe2el ( const double u[13], int jformr, * int *jform, double *epoch, double *orbinc, * double *anode, double *perih, double *aorq, double *e, * double *aorl, double *dm, int *jstat ); * Arguments: * u = const double [13] (Given) * Universal orbital elements (Note 1) * (0) combined mass (M+m) * (1) total energy of the orbit (alpha) * (2) reference (osculating) epoch (t0) * (3-5) position at reference epoch (r0) * (6-8) velocity at reference epoch (v0) * (9) heliocentric distance at reference epoch * (10) r0.v0 * (11) date (t) * (12) universal eccentric anomaly (psi) of date, approx * jformr = int (Given) * Requested element set (1-3; Note 3) * jform = int * (Returned) * Element set actually returned (1-3; Note 4) * epoch = double * (Returned) * Epoch of elements (TT MJD) * orbinc = double * (Returned) * inclination (radians) * anode = double * (Returned) * longitude of the ascending node (radians) * perih = double * (Returned) * longitude or argument of perihelion (radians) * aorq = double * (Returned) * mean distance or perihelion distance (AU) * e = double * (Returned) * eccentricity * aorl = double * (Returned) * mean anomaly or longitude (radians, JFORM=1,2 only) * dm = double * (Returned) * daily motion (radians, JFORM=1 only) * jstat = int * (Returned) * status: 0 = OK * -1 = illegal combined mass * -2 = illegal JFORMR * -3 = position/velocity out of range * Description: * Transform universal elements into conventional heliocentric * osculating elements. * Authors: * PTW: Patrick T. Wallace * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - The "universal" elements are those which define the orbit for the * purposes of the method of universal variables (see reference 2). * They consist of the combined mass of the two bodies, an epoch, * and the position and velocity vectors (arbitrary reference frame) * at that epoch. The parameter set used here includes also various * quantities that can, in fact, be derived from the other * information. This approach is taken to avoiding unnecessary * computation and loss of accuracy. The supplementary quantities * are (i) alpha, which is proportional to the total energy of the * orbit, (ii) the heliocentric distance at epoch, (iii) the * outwards component of the velocity at the given epoch, (iv) an * estimate of psi, the "universal eccentric anomaly" at a given * date and (v) that date. * - The universal elements are with respect to the mean equator and * equinox of epoch J2000. The orbital elements produced are with * respect to the J2000 ecliptic and mean equinox. * - Three different element-format options are supported: * * Option JFORM=1, suitable for the major planets: * * EPOCH = epoch of elements (TT MJD) * ORBINC = inclination i (radians) * ANODE = longitude of the ascending node, big omega (radians) * PERIH = longitude of perihelion, curly pi (radians) * AORQ = mean distance, a (AU) * E = eccentricity, e * AORL = mean longitude L (radians) * DM = daily motion (radians) * * Option JFORM=2, suitable for minor planets: * * EPOCH = epoch of elements (TT MJD) * ORBINC = inclination i (radians) * ANODE = longitude of the ascending node, big omega (radians) * PERIH = argument of perihelion, little omega (radians) * AORQ = mean distance, a (AU) * E = eccentricity, e * AORL = mean anomaly M (radians) * * Option JFORM=3, suitable for comets: * * EPOCH = epoch of perihelion (TT MJD) * ORBINC = inclination i (radians) * ANODE = longitude of the ascending node, big omega (radians) * PERIH = argument of perihelion, little omega (radians) * AORQ = perihelion distance, q (AU) * E = eccentricity, e * * - It may not be possible to generate elements in the form * requested through JFORMR. The caller is notified of the form * of elements actually returned by means of the JFORM argument: * * JFORMR JFORM meaning * * 1 1 OK - elements are in the requested format * 1 2 never happens * 1 3 orbit not elliptical * * 2 1 never happens * 2 2 OK - elements are in the requested format * 2 3 orbit not elliptical * * 3 1 never happens * 3 2 never happens * 3 3 OK - elements are in the requested format * * - The arguments returned for each value of JFORM (cf Note 6: JFORM * may not be the same as JFORMR) are as follows: * * JFORM 1 2 3 * EPOCH t0 t0 T * ORBINC i i i * ANODE Omega Omega Omega * PERIH curly pi omega omega * AORQ a a q * E e e e * AORL L M - * DM n - - * * where: * * t0 is the epoch of the elements (MJD, TT) * T " epoch of perihelion (MJD, TT) * i " inclination (radians) * Omega " longitude of the ascending node (radians) * curly pi " longitude of perihelion (radians) * omega " argument of perihelion (radians) * a " mean distance (AU) * q " perihelion distance (AU) * e " eccentricity * L " longitude (radians, 0-2pi) * M " mean anomaly (radians, 0-2pi) * n " daily motion (radians) * - means no value is set * * - At very small inclinations, the longitude of the ascending node * ANODE becomes indeterminate and under some circumstances may be * set arbitrarily to zero. Similarly, if the orbit is close to * circular, the true anomaly becomes indeterminate and under some * circumstances may be set arbitrarily to zero. In such cases, * the other elements are automatically adjusted to compensate, * and so the elements remain a valid description of the orbit. * See Also: * - Sterne, Theodore E., "An Introduction to Celestial Mechanics", * Interscience Publishers Inc., 1960. Section 6.7, p199. * - Everhart, E. & Pitkin, E.T., Am.J.Phys. 51, 712, 1983. * History: * 2012-03-09 (TIMJ): * Initial version * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 1999 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include "pal.h" #include "palmac.h" void palUe2el ( const double u[], int jformr, int *jform, double *epoch, double *orbinc, double *anode, double *perih, double *aorq, double *e, double *aorl, double *dm, int *jstat ) { /* Canonical days to seconds */ const double CD2S = PAL__GCON / PAL__SPD; int i; double pmass, date, pv[6]; /* Unpack the universal elements */ pmass = u[0] - 1.0; date = u[2]; for (i=0; i<3; i++) { pv[i] = u[i+3]; pv[i+3] = u[i+6] * CD2S; } /* Convert the position and velocity etc into conventional elements */ palPv2el( pv, date, pmass, jformr, jform, epoch, orbinc, anode, perih, aorq, e, aorl, dm, jstat ); } pal-0.5.0/palUe2pv.c000644 000765 000024 00000020442 12366000607 014242 0ustar00timjstaff000000 000000 /* *+ * Name: * palUe2pv * Purpose: * Heliocentric position and velocity of a planet, asteroid or comet, from universal elements * Language: * Starlink ANSI C * Type of Module: * Library routine * Invocation: * void palUe2pv( double date, double u[13], double pv[6], int *jstat ); * Arguments: * date = double (Given) * TT Modified Julian date (JD-2400000.5). * u = double [13] (Given & Returned) * Universal orbital elements (updated, see note 1) * given (0) combined mass (M+m) * " (1) total energy of the orbit (alpha) * " (2) reference (osculating) epoch (t0) * " (3-5) position at reference epoch (r0) * " (6-8) velocity at reference epoch (v0) * " (9) heliocentric distance at reference epoch * " (10) r0.v0 * returned (11) date (t) * " (12) universal eccentric anomaly (psi) of date * jstat = int * (Returned) * status: 0 = OK * -1 = radius vector zero * -2 = failed to converge * Description: * Heliocentric position and velocity of a planet, asteroid or comet, * starting from orbital elements in the "universal variables" form. * Authors: * PTW: Pat Wallace (STFC) * TIMJ: Tim Jenness (JAC, Hawaii) * {enter_new_authors_here} * Notes: * - The "universal" elements are those which define the orbit for the * purposes of the method of universal variables (see reference). * They consist of the combined mass of the two bodies, an epoch, * and the position and velocity vectors (arbitrary reference frame) * at that epoch. The parameter set used here includes also various * quantities that can, in fact, be derived from the other * information. This approach is taken to avoiding unnecessary * computation and loss of accuracy. The supplementary quantities * are (i) alpha, which is proportional to the total energy of the * orbit, (ii) the heliocentric distance at epoch, (iii) the * outwards component of the velocity at the given epoch, (iv) an * estimate of psi, the "universal eccentric anomaly" at a given * date and (v) that date. * - The companion routine is palEl2ue. This takes the conventional * orbital elements and transforms them into the set of numbers * needed by the present routine. A single prediction requires one * one call to palEl2ue followed by one call to the present routine; * for convenience, the two calls are packaged as the routine * sla_PLANEL. Multiple predictions may be made by again * calling palEl2ue once, but then calling the present routine * multiple times, which is faster than multiple calls to palPlanel. * - It is not obligatory to use palEl2ue to obtain the parameters. * However, it should be noted that because palEl2ue performs its * own validation, no checks on the contents of the array U are made * by the present routine. - DATE is the instant for which the prediction is required. It is * in the TT timescale (formerly Ephemeris Time, ET) and is a * Modified Julian Date (JD-2400000.5). - The universal elements supplied in the array U are in canonical * units (solar masses, AU and canonical days). The position and * velocity are not sensitive to the choice of reference frame. The * palEl2ue routine in fact produces coordinates with respect to the * J2000 equator and equinox. * - The algorithm was originally adapted from the EPHSLA program of * D.H.P.Jones (private communication, 1996). The method is based * on Stumpff's Universal Variables. * - Reference: Everhart, E. & Pitkin, E.T., Am.J.Phys. 51, 712, 1983. * History: * 2012-03-09 (TIMJ): * Initial version cloned from SLA/F. * Adapted with permission from the Fortran SLALIB library. * {enter_further_changes_here} * Copyright: * Copyright (C) 2005 Rutherford Appleton Laboratory * Copyright (C) 2012 Science and Technology Facilities Council. * All Rights Reserved. * Licence: * This program is free software; you can redistribute it and/or * modify it under the terms of the GNU General Public License as * published by the Free Software Foundation; either version 3 of * the License, or (at your option) any later version. * * This program is distributed in the hope that it will be * useful, but WITHOUT ANY WARRANTY; without even the implied * warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR * PURPOSE. See the GNU General Public License for more details. * * You should have received a copy of the GNU General Public License * along with this program; if not, write to the Free Software * Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, * MA 02110-1301, USA. * Bugs: * {note_any_bugs_here} *- */ #include #include "pal.h" #include "palmac.h" void palUe2pv( double date, double u[13], double pv[6], int *jstat ) { /* Canonical days to seconds */ const double CD2S = PAL__GCON / PAL__SPD; /* Test value for solution and maximum number of iterations */ const double TEST = 1e-13; const int NITMAX = 25; int I, NIT, N; double CM,ALPHA,T0,P0[3],V0[3],R0,SIGMA0,T,PSI,DT,W, TOL,PSJ,PSJ2,BETA,S0,S1,S2,S3, FF,R,F,G,FD,GD; double PLAST = 0.0; double FLAST = 0.0; /* Unpack the parameters. */ CM = u[0]; ALPHA = u[1]; T0 = u[2]; for (I=0; I<3; I++) { P0[I] = u[I+3]; V0[I] = u[I+6]; } R0 = u[9]; SIGMA0 = u[10]; T = u[11]; PSI = u[12]; /* Approximately update the universal eccentric anomaly. */ PSI = PSI+(date-T)*PAL__GCON/R0; /* Time from reference epoch to date (in Canonical Days: a canonical * day is 58.1324409... days, defined as 1/PAL__GCON). */ DT = (date-T0)*PAL__GCON; /* Refine the universal eccentric anomaly, psi. */ NIT = 1; W = 1.0; TOL = 0.0; while (fabs(W) >= TOL) { /* Form half angles until BETA small enough. */ N = 0; PSJ = PSI; PSJ2 = PSJ*PSJ; BETA = ALPHA*PSJ2; while (fabs(BETA) > 0.7) { N = N+1; BETA = BETA/4.0; PSJ = PSJ/2.0; PSJ2 = PSJ2/4.0; } /* Calculate Universal Variables S0,S1,S2,S3 by nested series. */ S3 = PSJ*PSJ2*((((((BETA/210.0+1.0) *BETA/156.0+1.0) *BETA/110.0+1.0) *BETA/72.0+1.0) *BETA/42.0+1.0) *BETA/20.0+1.0)/6.0; S2 = PSJ2*((((((BETA/182.0+1.0) *BETA/132.0+1.0) *BETA/90.0+1.0) *BETA/56.0+1.0) *BETA/30.0+1.0) *BETA/12.0+1.0)/2.0; S1 = PSJ+ALPHA*S3; S0 = 1.0+ALPHA*S2; /* Undo the angle-halving. */ TOL = TEST; while (N > 0) { S3 = 2.0*(S0*S3+PSJ*S2); S2 = 2.0*S1*S1; S1 = 2.0*S0*S1; S0 = 2.0*S0*S0-1.0; PSJ = PSJ+PSJ; TOL += TOL; N--; } /* Values of F and F' corresponding to the current value of psi. */ FF = R0*S1+SIGMA0*S2+CM*S3-DT; R = R0*S0+SIGMA0*S1+CM*S2; /* If first iteration, create dummy "last F". */ if ( NIT == 1) FLAST = FF; /* Check for sign change. */ if ( FF*FLAST < 0.0 ) { /* Sign change: get psi adjustment using secant method. */ W = FF*(PLAST-PSI)/(FLAST-FF); } else { /* No sign change: use Newton-Raphson method instead. */ if (R == 0.0) { /* Null radius vector */ *jstat = -1; return; } W = FF/R; } /* Save the last psi and F values. */ PLAST = PSI; FLAST = FF; /* Apply the Newton-Raphson or secant adjustment to psi. */ PSI = PSI-W; /* Next iteration, unless too many already. */ if (NIT > NITMAX) { *jstat = -2; /* Failed to converge */ return; } NIT++; } /* Project the position and velocity vectors (scaling velocity to AU/s). */ W = CM*S2; F = 1.0-W/R0; G = DT-CM*S3; FD = -CM*S1/(R0*R); GD = 1.0-W/R; for (I=0; I<3; I++) { pv[I] = P0[I]*F+V0[I]*G; pv[I+3] = CD2S*(P0[I]*FD+V0[I]*GD); } /* Update the parameters to allow speedy prediction of PSI next time. */ u[11] = date; u[12] = PSI; /* OK exit. */ *jstat = 0; return; } pal-0.5.0/._README.md000644 000765 000024 00000000265 12366007414 014100 0ustar00timjstaff000000 000000 Mac OS X  2ƒµATTRµ˜˜com.apple.quarantineq/0002;53d80137;Marked\x202;pal-0.5.0/README.md000644 000765 000024 00000005214 12366007414 013662 0ustar00timjstaff000000 000000 PAL - Positional Astronomy Library ================================== The PAL library is a partial re-implementation of Pat Wallace's popular SLALIB library written in C using a Gnu GPL license and layered on top of the IAU's SOFA library (or the BSD-licensed ERFA) where appropriate. PAL attempts to stick to the SLA C API where possible although `palObs()` has a more C-like API than the equivalent `slaObs()` function. In most cases it is enough to simply change the function prefix of a routine in order to link against PAL rather than SLALIB. Routines calling SOFA use modern nutation and precession models so will return slightly different answers than native SLALIB. PAL functions not available in SOFA were ported from the Fortran version of SLALIB that ships as part of the Starlink software and uses a GPL licence. See `pal.news` for release notes. Building -------- A simple `configure` script is provided: ./configure --prefix=/usr/local make make install The tests can be run using `make check`. Use `--prefix` to specify an install location. Given the history of the source code as a Starlink library the default will be `/star`. Requirements ------------ Requires that either the SOFA C library or the ERFA library variant (which has a more permissive license than SOFA) be installed. The `configure` script will abort if neither SOFA nor ERFA can be found. SOFA can be obtained either from or from an unofficial github repository (with a configure script) at . ERFA can be downloaded from . Missing Functions ----------------- Not all SLALIB functions have been added. New routines are added to PAL as demand arises. Language Bindings ----------------- A Perl binding of PAL is available () named `Astro::PAL` and is available from CPAN at . This is a standalone distribution that comes with its own copies of PAL and SOFA and so can be installed directly from the `cpan` shell. A Python binding of PAL is available (). This is a standalone distribution that comes with its own copies of PAL and SOFA. The Starlink AST () library now uses PAL and can be built either with a private PAL or with an external PAL. Documentation ------------- The description paper for PAL is: ["_PAL: A Positional Astronomy Library_"](http://adsabs.harvard.edu/abs/2013ASPC..475..307J), Jenness, T. & Berry, D. S., in _Astronomical Data Anaysis Software and Systems XXII_, Friedel, D. N. (ed), ASP Conf. Ser. **475**, p307. pal-0.5.0/sun267.htx_tar000644 000765 000024 00003053000 12365763733 015055 0ustar00timjstaff000000 000000 sun267.htx/000755 000765 000024 00000000000 12365763733 013051 5ustar00timjstaff000000 000000 sun267.htx/.star2html-init000644 000765 000024 00000004460 12365763500 015727 0ustar00timjstaff000000 000000 # Star2html latex2html defaults file. $ADDRESS = 'PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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$noresave{$key} = "$nosave"; $key = q/palRverot/; $external_labels{$key} = "$URL/" . q|node66.html|; $noresave{$key} = "$nosave"; $key = q/____palDt_/; $external_labels{$key} = "$URL/" . q|node23.html|; $noresave{$key} = "$nosave"; $key = q/palGeoc/; $external_labels{$key} = "$URL/" . q|node41.html|; $noresave{$key} = "$nosave"; $key = q/xref_palEcmat/; $external_labels{$key} = "$URL/" . q|node27.html|; $noresave{$key} = "$nosave"; $key = q/palGe50/; $external_labels{$key} = "$URL/" . q|node40.html|; $noresave{$key} = "$nosave"; $key = q/xref_palRdplan/; $external_labels{$key} = "$URL/" . q|node65.html|; $noresave{$key} = "$nosave"; $key = q/xref_palDfltin/; $external_labels{$key} = "$URL/" . q|node15.html|; $noresave{$key} = "$nosave"; $key = q/xref_palPv2el/; $external_labels{$key} = "$URL/" . q|node62.html|; $noresave{$key} = "$nosave"; $key = q/palPlante/; $external_labels{$key} = "$URL/" . q|node55.html|; $noresave{$key} = "$nosave"; $key = q/____palGalsup_/; $external_labels{$key} = "$URL/" . q|node39.html|; $noresave{$key} = "$nosave"; $key = q/palRvgalc/; $external_labels{$key} = "$URL/" . q|node67.html|; $noresave{$key} = "$nosave"; $key = q/xref_palUe2el/; $external_labels{$key} = "$URL/" . q|node73.html|; $noresave{$key} = "$nosave"; $key = q/xref_palDafin/; $external_labels{$key} = "$URL/" . q|node12.html|; $noresave{$key} = "$nosave"; $key = q/xref_palMap/; $external_labels{$key} = "$URL/" . q|node43.html|; $noresave{$key} = "$nosave"; $key = q/palEqgal/; $external_labels{$key} = "$URL/" . q|node33.html|; $noresave{$key} = "$nosave"; $key = q/____palEqgal_/; $external_labels{$key} = "$URL/" . q|node33.html|; $noresave{$key} = "$nosave"; $key = q/palDh2e/; $external_labels{$key} = "$URL/" . q|node16.html|; $noresave{$key} = "$nosave"; $key = q/palMappa/; $external_labels{$key} = "$URL/" . q|node44.html|; $noresave{$key} = "$nosave"; $key = q/xref_palAirmas/; $external_labels{$key} = "$URL/" . q|node8.html|; $noresave{$key} = "$nosave"; $key = q/xref_palUe2pv/; $external_labels{$key} = "$URL/" . q|node74.html|; $noresave{$key} = "$nosave"; $key = q/____palMap_/; $external_labels{$key} = "$URL/" . q|node43.html|; $noresave{$key} = "$nosave"; $key = q/palUe2pv/; $external_labels{$key} = "$URL/" . q|node74.html|; $noresave{$key} = "$nosave"; $key = q/palPm/; $external_labels{$key} = "$URL/" . q|node57.html|; $noresave{$key} = "$nosave"; $key = q/____palRverot_/; $external_labels{$key} = "$URL/" . q|node66.html|; $noresave{$key} = "$nosave"; $key = q/palMapqkz/; $external_labels{$key} = "$URL/" . q|node46.html|; $noresave{$key} = "$nosave"; $key = q/xref_palPertel/; $external_labels{$key} = "$URL/" . q|node51.html|; $noresave{$key} = "$nosave"; $key = q/xref_palFk54z/; $external_labels{$key} = "$URL/" . q|node37.html|; $noresave{$key} = "$nosave"; $key = q/xref_palPv2ue/; $external_labels{$key} = "$URL/" . q|node63.html|; $noresave{$key} = "$nosave"; $key = q/palGaleq/; $external_labels{$key} = "$URL/" . q|node38.html|; $noresave{$key} = "$nosave"; $key = q/xref_palRvgalc/; $external_labels{$key} = "$URL/" . q|node67.html|; $noresave{$key} = "$nosave"; $key = q/palEl2ue/; $external_labels{$key} = "$URL/" . q|node28.html|; $noresave{$key} = "$nosave"; $key = q/____palDjcal_/; $external_labels{$key} = "$URL/" . q|node17.html|; $noresave{$key} = "$nosave"; $key = q/____palDe2h_/; $external_labels{$key} = "$URL/" . q|node13.html|; $noresave{$key} = "$nosave"; $key = q/xref_palPreces/; $external_labels{$key} = "$URL/" . q|node60.html|; $noresave{$key} = "$nosave"; $key = q/xref_palAddet/; $external_labels{$key} = "$URL/" . q|node7.html|; $noresave{$key} = "$nosave"; $key = q/xref_palPrenut/; $external_labels{$key} = "$URL/" . q|node61.html|; $noresave{$key} = "$nosave"; $key = q/xref_palRvlsrk/; $external_labels{$key} = "$URL/" . q|node70.html|; $noresave{$key} = "$nosave"; $key = q/xref_palDh2e/; $external_labels{$key} = "$URL/" . q|node16.html|; $noresave{$key} = "$nosave"; $key = q/____palDtps2c_/; $external_labels{$key} = "$URL/" . q|node25.html|; $noresave{$key} = "$nosave"; $key = q/____palEpv_/; $external_labels{$key} = "$URL/" . q|node30.html|; $noresave{$key} = "$nosave"; $key = q/xref_palPm/; $external_labels{$key} = "$URL/" . q|node57.html|; $noresave{$key} = "$nosave"; $key = q/____palRvlg_/; $external_labels{$key} = "$URL/" . q|node68.html|; $noresave{$key} = "$nosave"; $key = q/xref_palSubet/; $external_labels{$key} = "$URL/" . q|node71.html|; $noresave{$key} = "$nosave"; $key = q/palDs2tp/; $external_labels{$key} = "$URL/" . q|node19.html|; $noresave{$key} = "$nosave"; $key = q/____palNutc_/; $external_labels{$key} = "$URL/" . q|node48.html|; $noresave{$key} = "$nosave"; 1; # LaTeX2HTML 2012-Starlink (1.2) # labels from external_latex_labels array. 1; sun267.htx/next.png000644 000765 000024 00000000365 12365763733 014541 0ustar00timjstaff000000 000000 ‰PNG  IHDR%wìu PLTE¿¿¿oooççç[Íã¹tRNS@æØf—IDATxœmŽ1 Ã0 EQF >ŠÁk >B‡ú>†¬…NÙ3û¯=Œ¡k¡•äШ¾Ÿ?²d”Œ M53–—³³ˆkARMê9®êNÈlúà :CÕü5¥t•·¥læ¸]o¦÷ÁDª­×/ûÜ¡_ç\lŽEÄ6¶ãtÄUˆê›é¬è{Ccs=Ëßû@ªuwÿû¡®·ˆz Abstract

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Abstract

PAL provides a subset of the Fortran SLALIB library but written in C using the SLALIB C API. Where possible the PAL routines are implemented using the C SOFA library. It is provided with a GPL license.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node10.html000644 000765 000024 00000011701 12365763733 015025 0ustar00timjstaff000000 000000 palAmpqk - Convert star RA,Dec from geocentric apparent to mean place
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palAmpqk - Convert star RA,Dec from geocentric apparent to mean place

Description:
Convert star RA,Dec from geocentric apparent to mean place. The "mean" coordinate system is in fact close to ICRS. Use of this function is appropriate when efficiency is important and where many star positions are all to be transformed for one epoch and equinox. The star-independent parameters can be obtained by calling the palMappa function.

Invocation:
void palAmpqk ( double ra, double da, double amprms[21], double rm, double dm )

Arguments:

ra = double (Given)
Apparent RA (radians).
da = double (Given)
Apparent Dec (radians).
amprms = double[21] (Given)
Star-independent mean-to-apparent parameters (see palMappa): (0) time interval for proper motion (Julian years) (1-3) barycentric position of the Earth (AU) (4-6) not used (7) not used (8-10) abv: barycentric Earth velocity in units of c (11) sqrt(1-vv) where v=modulus(abv) (12-20) precession/nutation (3,3) matrix
rm = double (Returned)
Mean RA (radians).
dm = double (Returned)
Mean Dec (radians).


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node11.html000644 000765 000024 00000011614 12365763733 015031 0ustar00timjstaff000000 000000 palCaldj - Gregorian Calendar to Modified Julian Date
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palCaldj - Gregorian Calendar to Modified Julian Date

Description:
Modified Julian Date to Gregorian Calendar with special behaviour for 2-digit years relating to 1950 to 2049.

Invocation:
void palCaldj ( int iy, int im, int id, double djm, int j );

Arguments:

iy = int (Given)
Year in the Gregorian calendar
im = int (Given)
Month in the Gergorian calendar
id = int (Given)
Day in the Gregorian calendar
djm = double (Returned)
Modified Julian Date (JD-2400000.5) for 0 hrs
j = status (Returned)
0 = OK. See iauCal2jd for other values.

Notes:
  • Uses iauCal2jd

  • Unlike iauCal2jd this routine treats the years 0-100 as referring to the end of the 20th Century and beginning of the 21st Century. If this behaviour is not acceptable use the SOFA routine directly or palCldj. Acceptable years are 00-49, interpreted as 2000-2049, 50-99, " " 1950-1999, all others, interpreted literally.

  • Unlike SLA this routine will work with negative years.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node12.html000644 000765 000024 00000016015 12365763733 015032 0ustar00timjstaff000000 000000 palDafin - Sexagesimal character string to angle
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palDafin - Sexagesimal character string to angle

Description:
Extracts an angle from a sexagesimal string with degrees, arcmin, arcsec fields using space or comma delimiters.

Invocation:
void palDafin ( const char string, int ipos, double a, int j );

Arguments:

string = const char (Given)
String containing deg, arcmin, arcsec fields
ipos = int (Given & Returned)
Position to start decoding "string". First character is position 1 for compatibility with SLA. After calling this routine "iptr" will be positioned after the sexagesimal string.
a = double (Returned)
Angle in radians.
j = int (Returned)
status: 0 = OK 1 = default, A unchanged
  • 1 = bad degrees )

  • 2 = bad arcminutes ) (note 3)

  • 3 = bad arcseconds )


Notes:
  • The first three "fields" in STRING are degrees, arcminutes, arcseconds, separated by spaces or commas. The degrees field may be signed, but not the others. The decoding is carried out by the palDfltin routine and is free-format.

  • Successive fields may be absent, defaulting to zero. For zero status, the only combinations allowed are degrees alone, degrees and arcminutes, and all three fields present. If all three fields are omitted, a status of 1 is returned and A is unchanged. In all other cases A is changed.

  • Range checking:


The degrees field is not range checked. However, it is expected to be integral unless the other two fields are absent.

The arcminutes field is expected to be 0-59, and integral if the arcseconds field is present. If the arcseconds field is absent, the arcminutes is expected to be 0-59.9999...

The arcseconds field is expected to be 0-59.9999...

  • Decoding continues even when a check has failed. Under these circumstances the field takes the supplied value, defaulting to zero, and the result A is computed and returned.

  • Further fields after the three expected ones are not treated as an error. The pointer IPOS is left in the correct state for further decoding with the present routine or with palDfltin etc. See the example, above.

  • If STRING contains hours, minutes, seconds instead of degrees etc, or if the required units are turns (or days) instead of radians, the result A should be multiplied as follows:


for to obtain multiply STRING A in A by

d ' " radians 1 = 1.0 d ' " turns 1/2pi = 0.1591549430918953358 h m s radians 15 = 15.0 h m s days 15/2pi = 2.3873241463784300365

Example
argument before after

STRING '-57 17 44.806 12 34 56.7' unchanged IPTR 1 16 (points to 12...) A ? -1.00000D0 J ? 0


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node13.html000644 000765 000024 00000013117 12365763733 015033 0ustar00timjstaff000000 000000 palDe2h - Equatorial to horizon coordinates: HA,Dec to Az,E
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palDe2h - Equatorial to horizon coordinates: HA,Dec to Az,E

Description:
Convert equatorial to horizon coordinates.

Invocation:
palDe2h( double ha, double dec, double phi, double az, double el );

Arguments:

ha = double (Given)
Hour angle (radians)
dec = double (Given)
Declination (radians)
phi = double (Given)
Observatory latitude (radians)
az = double (Returned)
Azimuth (radians)
el = double (Returned)
Elevation (radians)

Notes:
  • All the arguments are angles in radians.

  • Azimuth is returned in the range 0-2pi; north is zero, and east is pi/2. Elevation is returned in the range /-pi/2.

  • The latitude must be geodetic. In critical applications, corrections for polar motion should be applied.

  • In some applications it will be important to specify the correct type of hour angle and declination in order to produce the required type of azimuth and elevation. In particular, it may be important to distinguish between elevation as affected by refraction, which would require the "observed" HA,Dec, and the elevation in vacuo, which would require the "topocentric" HA,Dec. If the effects of diurnal aberration can be neglected, the "apparent" HA,Dec may be used instead of the topocentric HA,Dec.

  • No range checking of arguments is carried out.

  • In applications which involve many such calculations, rather than calling the present routine it will be more efficient to use inline code, having previously computed fixed terms such as sine and cosine of latitude, and (for tracking a star) sine and cosine of declination.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node14.html000644 000765 000024 00000012730 12365763733 015034 0ustar00timjstaff000000 000000 palDeuler - Form a rotation matrix from the Euler angles
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palDeuler - Form a rotation matrix from the Euler angles

Description:
A rotation is positive when the reference frame rotates anticlockwise as seen looking towards the origin from the positive region of the specified axis.

The characters of ORDER define which axes the three successive rotations are about. A typical value is 'ZXZ', indicating that RMAT is to become the direction cosine matrix corresponding to rotations of the reference frame through PHI radians about the old Z-axis, followed by THETA radians about the resulting X-axis, then PSI radians about the resulting Z-axis.

The axis names can be any of the following, in any order or combination: X, Y, Z, uppercase or lowercase, 1, 2, 3. Normal axis labelling/numbering conventions apply; the xyz (=123) triad is right-handed. Thus, the 'ZXZ' example given above could be written 'zxz' or '313' (or even 'ZxZ' or '3xZ'). ORDER is terminated by length or by the first unrecognized character.

Fewer than three rotations are acceptable, in which case the later angle arguments are ignored. If all rotations are zero, the identity matrix is produced.


Invocation:
void palDeuler ( const char order, double phi, double theta, double psi, double rmat[3][3] );

Arguments:

order = const char[] (Given)
Specifies about which axes the rotation occurs
phi = double (Given)
1st rotation (radians)
theta = double (Given)
2nd rotation (radians)
psi = double (Given)
3rd rotation (radians)
rmat = double[3][3] (Given & Returned)
Rotation matrix


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node15.html000644 000765 000024 00000012761 12365763733 015041 0ustar00timjstaff000000 000000 palDfltin - Convert free-format input into double precision floating point
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palDfltin - Convert free-format input into double precision floating point

Description:
Extracts a number from an input string starting at the specified index.

Invocation:
void palDfltin( const char string, int nstrt, double dreslt, int jflag );

Arguments:

string = const char (Given)
String containing number to be decoded.
nstrt = int (Given and Returned)
Character number indicating where decoding should start. On output its value is updated to be the location of the possible next value. For compatibility with SLA the first character is index 1.
dreslt = double (Returned)
Result. Not updated when jflag=1.
jflag = int (Returned)
status: -1 = -OK, 0 = OK, 1 = null, 2 = error

Notes:
  • Uses the strtod() system call to do the parsing. This may lead to subtle differences when compared to the SLA/F parsing.

  • All "D" characters are converted to "E" to handle fortran exponents.

  • Commas are recognized as a special case and are skipped if one happens to be the next character when updating nstrt. Additionally the output nstrt position will skip past any trailing space.

  • If no number can be found flag will be set to 1.

  • If the number overflows or underflows jflag will be set to 2. For overflow the returned result will have the value HUGE_VAL, for underflow it will have the value 0.0.

  • For compatiblity with SLA/F -0 will be returned as "0" with jflag == -1.

  • Unlike slaDfltin a standalone "E" will return status 1 (could not find a number) rather than 2 (bad number).


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node16.html000644 000765 000024 00000013065 12365763733 015040 0ustar00timjstaff000000 000000 palDh2e - Horizon to equatorial coordinates: Az,El to HA,Dec
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palDh2e - Horizon to equatorial coordinates: Az,El to HA,Dec

Description:
Convert horizon to equatorial coordinates.

Invocation:
palDh2e( double az, double el, double phi, double ha, double dec );

Arguments:

az = double (Given)
Azimuth (radians)
el = double (Given)
Elevation (radians)
phi = double (Given)
Observatory latitude (radians)
ha = double (Returned)
Hour angle (radians)
dec = double (Returned)
Declination (radians)

Notes:
  • All the arguments are angles in radians.

  • The sign convention for azimuth is north zero, east pi/2.

  • HA is returned in the range /-pi. Declination is returned in the range /-pi/2.

  • The latitude is (in principle) geodetic. In critical applications, corrections for polar motion should be applied.

  • In some applications it will be important to specify the correct type of elevation in order to produce the required type of HA,Dec. In particular, it may be important to distinguish between the elevation as affected by refraction, which will yield the "observed" HA,Dec, and the elevation in vacuo, which will yield the "topocentric" HA,Dec. If the effects of diurnal aberration can be neglected, the topocentric HA,Dec may be used as an approximation to the "apparent" HA,Dec.

  • No range checking of arguments is done.

  • In applications which involve many such calculations, rather than calling the present routine it will be more efficient to use inline code, having previously computed fixed terms such as sine and cosine of latitude.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node17.html000644 000765 000024 00000010575 12365763733 015044 0ustar00timjstaff000000 000000 palDjcal - Modified Julian Date to Gregorian Calendar
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palDjcal - Modified Julian Date to Gregorian Calendar

Description:
Modified Julian Date to Gregorian Calendar, expressed in a form convenient for formatting messages (namely rounded to a specified precision, and with the fields stored in a single array)

Invocation:
void palDjcal ( int ndp, double djm, int iymdf[4], int j );

Arguments:

ndp = int (Given)
Number of decimal places of days in fraction.
djm = double (Given)
Modified Julian Date (JD-2400000.5)
iymdf[4] = int[] (Returned)
Year, month, day, fraction in Gregorian calendar.
j = status (Returned)
0 = OK. See iauJd2cal for other values.

Notes:
  • Uses iauJd2cal


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palDmat - Matrix inversion & solution of simultaneous equations

Description:
Matrix inversion & solution of simultaneous equations For the set of n simultaneous equations in n unknowns: A.Y = X this routine calculates the inverse of A, the determinant of matrix A and the vector of N unknowns.

Invocation:
void palDmat( int n, double a, double y, double d, int jf, int iw );

Arguments:

n = int (Given)
Number of simultaneous equations and number of unknowns.
a = double[] (Given & Returned)
A non-singular NxN matrix (implemented as a contiguous block of memory). After calling this routine "a" contains the inverse of the matrix.
y = double[] (Given & Returned)
The vector of N unknowns. On exit this vector contains the N solutions.
d = double (Returned)
The determinant.
jf = int (Returned)
The singularity flag. If the matrix is non-singular, jf=0 is returned. If the matrix is singular, jf=-1 & d=0.0 are returned. In the latter case, the contents of array "a" on return are undefined.

Notes:
  • Implemented using Gaussian elimination with partial pivoting.

  • Optimized for speed rather than accuracy with errors 1 to 4 times those of routines optimized for accuracy.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node19.html000644 000765 000024 00000011547 12365763733 015046 0ustar00timjstaff000000 000000 palDs2tp - Spherical to tangent plane projection
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palDs2tp - Spherical to tangent plane projection

Description:
Projection of spherical coordinates onto tangent plane: "gnomonic" projection - "standard coordinates"

Invocation:
palDs2tp( double ra, double dec, double raz, double decz, double xi, double eta, int j );

Arguments:

ra = double (Given)
RA spherical coordinate of point to be projected (radians)
dec = double (Given)
Dec spherical coordinate of point to be projected (radians)
raz = double (Given)
RA spherical coordinate of tangent point (radians)
decz = double (Given)
Dec spherical coordinate of tangent point (radians)
xi = double (Returned)
First rectangular coordinate on tangent plane (radians)
eta = double (Returned)
Second rectangular coordinate on tangent plane (radians)
j = int (Returned)
status: 0 = OK, star on tangent plane 1 = error, star too far from axis 2 = error, antistar on tangent plane 3 = error, antistar too far from axis


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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Introduction

This library provides a C library designed as a API-compatible replacement for the C SLALIB library (SUN/67) and uses a GPL licence so is freely redistributable. Where possible the functions call equivalent SOFA routines (Hohenkerk, C., 2011, Scholarpedia, 6, 11404) and use current IAU 2006 standards. This means that any functions that rely on nutation or precession will return slightly different answers to the SLA functions.

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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node20.html000644 000765 000024 00000011034 12365763733 015025 0ustar00timjstaff000000 000000 palDtt - Return offset between UTC and TT
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palDtt - Return offset between UTC and TT

Description:
Increment to be applied to Coordinated Universal Time UTC to give International Atomic Time (TAI).

Invocation:
dat = palDat( double utc );

Arguments:

utc = double (Given)
UTC date as a modified JD (JD-2400000.5)

Returned Value:

dat = double
TAI-UTC in seconds

Notes:
  • This routine converts the MJD argument to calendar date before calling the SOFA iauDat function.

  • This routine matches the slaDat interface which differs from the iauDat interface. Consider coding directly to the SOFA interface.

  • See iauDat for a description of error conditions when calling this function with a time outside of the UTC range.

  • The status argument from iauDat is ignored. This is reasonable since the error codes are mainly related to incorrect calendar dates when calculating the JD internally.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palDmoon - Approximate geocentric position and velocity of the Moon

Description:
Calculate the approximate geocentric position of the Moon using a full implementation of the algorithm published by Meeus (l'Astronomie, June 1984, p348).

Invocation:
void palDmoon( double date, double pv[6] );

Arguments:

date = double (Given)
TDB as a Modified Julian Date (JD-2400000.5)
pv = double [6] (Returned)
Moon x,y,z,xdot,ydot,zdot, mean equator and equinox of date (AU, AU/s)

Notes:
  • Meeus quotes accuracies of 10 arcsec in longitude, 3 arcsec in latitude and 0.2 arcsec in HP (equivalent to about 20 km in distance). Comparison with JPL DE200 over the interval 1960-2025 gives RMS errors of 3.7 arcsec and 83 mas/hour in longitude, 2.3 arcsec and 48 mas/hour in latitude, 11 km and 81 mm/s in distance. The maximum errors over the same interval are 18 arcsec and 0.50 arcsec/hour in longitude, 11 arcsec and 0.24 arcsec/hour in latitude, 40 km and 0.29 m/s in distance.

  • The original algorithm is expressed in terms of the obsolete timescale Ephemeris Time. Either TDB or TT can be used, but not UT without incurring significant errors (30 arcsec at the present time) due to the Moon's 0.5 arcsec/sec movement.

  • The algorithm is based on pre IAU 1976 standards. However, the result has been moved onto the new (FK5) equinox, an adjustment which is in any case much smaller than the intrinsic accuracy of the procedure.

  • Velocity is obtained by a complete analytical differentiation of the Meeus model.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palDrange - Normalize angle into range /- pi

Description:
The result is "angle" expressed in the range /- pi. If the supplied value for "angle" is equal to /- pi, it is returned unchanged.

Invocation:
palDrange( double angle )

Arguments:

angle = double (Given)
The angle in radians.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node23.html000644 000765 000024 00000012446 12365763733 015040 0ustar00timjstaff000000 000000 palDt - Estimate the offset between dynamical time and UT
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palDt - Estimate the offset between dynamical time and UT

Description:
Estimate the offset between dynamical time and Universal Time for a given historical epoch.

Invocation:
double palDt( double epoch );

Arguments:

epoch = double (Given)
Julian epoch (e.g. 1850.0)

Returned Value:

palDt = double
Rough estimate of ET-UT (after 1984, TT-UT) at the given epoch, in seconds.

Notes:
  • Depending on the epoch, one of three parabolic approximations is used:


before 979 Stephenson & Morrison's 390 BC to AD 948 model 979 to 1708 Stephenson & Morrison's 948 to 1600 model after 1708 McCarthy & Babcock's post-1650 model

The breakpoints are chosen to ensure continuity: they occur at places where the adjacent models give the same answer as each other.

  • The accuracy is modest, with errors of up to 20 sec during the interval since 1650, rising to perhaps 30 min by 1000 BC. Comparatively accurate values from AD 1600 are tabulated in the Astronomical Almanac (see section K8 of the 1995 AA).

  • The use of double-precision for both argument and result is purely for compatibility with other SLALIB time routines.

  • The models used are based on a lunar tidal acceleration value of -26.00 arcsec per century.

See Also
Explanatory Supplement to the Astronomical Almanac, ed P.K.Seidelmann, University Science Books (1992), section 2.553, p83. This contains references to the Stephenson & Morrison and McCarthy & Babcock papers.

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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node24.html000644 000765 000024 00000010764 12365763733 015042 0ustar00timjstaff000000 000000 palDtp2s - Tangent plane to spherical coordinates
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palDtp2s - Tangent plane to spherical coordinates

Description:
Transform tangent plane coordinates into spherical.

Invocation:
palDtp2s( double xi, double eta, double raz, double decz, double ra, double dec);

Arguments:

xi = double (Given)
First rectangular coordinate on tangent plane (radians)
eta = double (Given)
Second rectangular coordinate on tangent plane (radians)
raz = double (Given)
RA spherical coordinate of tangent point (radians)
decz = double (Given)
Dec spherical coordinate of tangent point (radians)
ra = double (Returned)
RA spherical coordinate of point to be projected (radians)
dec = double (Returned)
Dec spherical coordinate of point to be projected (radians)


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node25.html000644 000765 000024 00000014552 12365763733 015042 0ustar00timjstaff000000 000000 palDtps2c - Determine RA,Dec of tangent point from coordinates
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palDtps2c - Determine RA,Dec of tangent point from coordinates

Description:
From the tangent plane coordinates of a star of known RA,Dec, determine the RA,Dec of the tangent point.

Invocation:
palDtps2c( double xi, double eta, double ra, double dec, double raz1, double decz1, double raz2, double decz2, int n);

Arguments:

xi = double (Given)
First rectangular coordinate on tangent plane (radians)
eta = double (Given)
Second rectangular coordinate on tangent plane (radians)
ra = double (Given)
RA spherical coordinate of star (radians)
dec = double (Given)
Dec spherical coordinate of star (radians)
raz1 = double (Returned)
RA spherical coordinate of tangent point, solution 1 (radians)
decz1 = double (Returned)
Dec spherical coordinate of tangent point, solution 1 (radians)
raz2 = double (Returned)
RA spherical coordinate of tangent point, solution 2 (radians)
decz2 = double (Returned)
Dec spherical coordinate of tangent point, solution 2 (radians)
n = int (Returned)
number of solutions: 0 = no solutions returned (note 2) 1 = only the first solution is useful (note 3) 2 = both solutions are useful (note 3)

Notes:
  • The RAZ1 and RAZ2 values are returned in the range 0-2pi.

  • Cases where there is no solution can only arise near the poles. For example, it is clearly impossible for a star at the pole itself to have a non-zero XI value, and hence it is meaningless to ask where the tangent point would have to be to bring about this combination of XI and DEC.

  • Also near the poles, cases can arise where there are two useful solutions. The argument N indicates whether the second of the two solutions returned is useful. N=1 indicates only one useful solution, the usual case; under these circumstances, the second solution corresponds to the "over-the-pole" case, and this is reflected in the values of RAZ2 and DECZ2 which are returned.

  • The DECZ1 and DECZ2 values are returned in the range /-pi, but in the usual, non-pole-crossing, case, the range is /-pi/2.

  • This routine is the spherical equivalent of the routine sla_DTPV2C.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palDtt - Return offset between UTC and TT

Description:
Increment to be applied to Coordinated Universal Time UTC to give Terrestrial Time TT (formerly Ephemeris Time ET)

Invocation:
dtt = palDtt( double utc );

Arguments:

utc = double (Given)
UTC date as a modified JD (JD-2400000.5)

Returned Value:

dtt = double
TT-UTC in seconds

Notes:
  • Consider a comprehensive upgrade to use the time transformations in SOFA's time cookbook: http://www.iausofa.org/sofa_ts_c.pdf.

  • See iauDat for a description of error conditions when calling this function with a time outside of the UTC range. This behaviour differs from slaDtt.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palEcmat - Form the equatorial to ecliptic rotation matrix - IAU 2006 precession model

Description:
The equatorial to ecliptic rotation matrix is found and returned. The matrix is in the sense V(ecl) = RMAT V(equ); the equator, equinox and ecliptic are mean of date.

Invocation:
palEcmat( double date, double rmat[3][3] )

Arguments:

date = double (Given)
TT as Modified Julian Date (JD-2400000.5). The difference between TT and TDB is of the order of a millisecond or two (i.e. about 0.02 arc-seconds).
rmat = double[3][3] (Returned)
Rotation matrix


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palEl2ue - Transform conventional elements into "universal" form

Description:
Transform conventional osculating elements into "universal" form.

Invocation:
void palEl2ue ( double date, int jform, double epoch, double orbinc, double anode, double perih, double aorq, double e, double aorl, double dm, double u[13], int jstat );

Arguments:

date = double (Given)
Epoch (TT MJD) of osculation (Note 3)
jform = int (Given)
Element set actually returned (1-3; Note 6)
epoch = double (Given)
Epoch of elements (TT MJD)
orbinc = double (Given)
inclination (radians)
anode = double (Given)
longitude of the ascending node (radians)
perih = double (Given)
longitude or argument of perihelion (radians)
aorq = double (Given)
mean distance or perihelion distance (AU)
e = double (Given)
eccentricity
aorl = double (Given)
mean anomaly or longitude (radians, JFORM=1,2 only)
dm = double (Given)
daily motion (radians, JFORM=1 only)
u = double [13] (Returned)
Universal orbital elements (Note 1) (0) combined mass (Mm) (1) total energy of the orbit (alpha) (2) reference (osculating) epoch (t0) (3-5) position at reference epoch (r0) (6-8) velocity at reference epoch (v0) (9) heliocentric distance at reference epoch (10) r0.v0 (11) date (t) (12) universal eccentric anomaly (psi) of date, approx
jstat = int (Returned)
status: 0 = OK
  • 1 = illegal JFORM

  • 2 = illegal E

  • 3 = illegal AORQ

  • 4 = illegal DM

  • 5 = numerical error


Notes:
  • The "universal" elements are those which define the orbit for the purposes of the method of universal variables (see reference). They consist of the combined mass of the two bodies, an epoch, and the position and velocity vectors (arbitrary reference frame) at that epoch. The parameter set used here includes also various quantities that can, in fact, be derived from the other information. This approach is taken to avoiding unnecessary computation and loss of accuracy. The supplementary quantities are (i) alpha, which is proportional to the total energy of the orbit, (ii) the heliocentric distance at epoch, (iii) the outwards component of the velocity at the given epoch, (iv) an estimate of psi, the "universal eccentric anomaly" at a given date and (v) that date.

  • The companion routine is palUe2pv. This takes the set of numbers that the present routine outputs and uses them to derive the object's position and velocity. A single prediction requires one call to the present routine followed by one call to palUe2pv; for convenience, the two calls are packaged as the routine palPlanel. Multiple predictions may be made by again calling the present routine once, but then calling palUe2pv multiple times, which is faster than multiple calls to palPlanel.

  • DATE is the epoch of osculation. It is in the TT timescale (formerly Ephemeris Time, ET) and is a Modified Julian Date (JD-2400000.5).

  • The supplied orbital elements are with respect to the J2000 ecliptic and equinox. The position and velocity parameters returned in the array U are with respect to the mean equator and equinox of epoch J2000, and are for the perihelion prior to the specified epoch.

  • The universal elements returned in the array U are in canonical units (solar masses, AU and canonical days).

  • Three different element-format options are available:


Option JFORM=1, suitable for the major planets:

EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = longitude of perihelion, curly pi (radians) AORQ = mean distance, a (AU) E = eccentricity, e (range 0 to 1) AORL = mean longitude L (radians) DM = daily motion (radians)

Option JFORM=2, suitable for minor planets:

EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = mean distance, a (AU) E = eccentricity, e (range 0 to 1) AORL = mean anomaly M (radians)

Option JFORM=3, suitable for comets:

EPOCH = epoch of perihelion (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = perihelion distance, q (AU) E = eccentricity, e (range 0 to 10)

  • Unused elements (DM for JFORM=2, AORL and DM for JFORM=3) are not accessed.

  • The algorithm was originally adapted from the EPHSLA program of D.H.P.Jones (private communication, 1996). The method is based on Stumpff's Universal Variables.

See Also
Everhart & Pitkin, Am.J.Phys. 51, 712 (1983).

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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palEpco - Convert an epoch into the appropriate form - 'B' or 'J'

Description:
Converts a Besselian or Julian epoch to a Julian or Besselian epoch.

Invocation:
double palEpco( char k0, char k, double e );

Arguments:

k0 = char (Given)
Form of result: 'B'=Besselian, 'J'=Julian
k = char (Given)
Form of given epoch: 'B' or 'J'.

Notes:
  • The result is always either equal to or very close to the given epoch E. The routine is required only in applications where punctilious treatment of heterogeneous mixtures of star positions is necessary.

  • k and k0 are case insensitive. This differes slightly from the Fortran SLA implementation.

  • k and k0 are not validated. They are interpreted as follows: o If k0 and k are the same the result is e o If k0 is 'b' or 'B' and k isn't the conversion is J to B. o In all other cases, the conversion is B to J.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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Citing PAL

If you use PAL in your work please consider citing it. The description paper for PAL is: PAL: A Positional Astronomy Library, Jenness, T. & Berry, D. S., in Astronomoical Data Anaysis Software and Systems XXII, Friedel, D. N. (ed), ASP Conf. Ser. 475, p307.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palEpv - Earth position and velocity with respect to the BCRS

Description:
Earth position and velocity, heliocentric and barycentric, with respect to the Barycentric Celestial Reference System.

Invocation:
void palEpv( double date, double ph[3], double vh[3], double pb[3], double vb[3] );

Arguments:

date = double (Given)
Date, TDB Modified Julian Date (JD-2400000.5)
ph = double [3] (Returned)
Heliocentric Earth position (AU)
vh = double [3] (Returned)
Heliocentric Earth velocity (AU/day)
pb = double [3] (Returned)
Barycentric Earth position (AU)
vb = double [3] (Returned)
Barycentric Earth velocity (AU/day)

Notes:
  • See iauEpv00 for details on accuracy

  • Note that the status argument from iauEpv00 is ignored


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palEtrms - Compute the E-terms vector

Description:
Computes the E-terms (elliptic component of annual aberration) vector.

Note the use of the J2000 aberration constant (20.49552 arcsec). This is a reflection of the fact that the E-terms embodied in existing star catalogues were computed from a variety of aberration constants. Rather than adopting one of the old constants the latest value is used here.


Invocation:
void palEtrms ( double ep, double ev[3] );

Arguments:

ep = double (Given)
Besselian epoch
ev = double [3] (Returned)
E-terms as (dx,dy,dz)

See also
  • Smith, C.A. et al., 1989. Astr.J. 97, 265.

  • Yallop, B.D. et al., 1989. Astr.J. 97, 274.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palEqecl - Transform from J2000.0 equatorial coordinates to ecliptic coordinates

Description:
Transform from J2000.0 equatorial coordinates to ecliptic coordinates.

Invocation:
void palEqecl( double dr, double dd, double date, double dl, double db);

Arguments:

dr = double (Given)
J2000.0 mean RA (radians)
dd = double (Given)
J2000.0 mean Dec (Radians)
date = double (Given)
TT as Modified Julian Date (JD-2400000.5). The difference between TT and TDB is of the order of a millisecond or two (i.e. about 0.02 arc-seconds).
dl = double (Returned)
Ecliptic longitude (mean of date, IAU 1980 theory, radians)
db = double (Returned)
Ecliptic latitude (mean of date, IAU 1980 theory, radians)


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palEqgal - Convert from J2000.0 equatorial coordinates to Galactic

Description:
Transformation from J2000.0 equatorial coordinates to IAU 1958 galactic coordinates.

Invocation:
void palEqgal ( double dr, double dd, double dl, double db );

Arguments:

dr = double (Given)
J2000.0 RA (radians)
dd = double (Given)
J2000.0 Dec (radians
dl = double (Returned)
Galactic longitude (radians).
db = double (Returned)
Galactic latitude (radians).

Notes:
The equatorial coordinates are J2000.0. Use the routine palGe50 if conversion to B1950.0 'FK4' coordinates is required.
See Also
Blaauw et al, Mon.Not.R.Astron.Soc.,121,123 (1960)

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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node34.html000644 000765 000024 00000011653 12365763733 015041 0ustar00timjstaff000000 000000 palEvp - Returns the barycentric and heliocentric velocity and position of the Earth
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palEvp - Returns the barycentric and heliocentric velocity and position of the Earth

Description:
Returns the barycentric and heliocentric velocity and position of the Earth at a given epoch, given with respect to a specified equinox. For information about accuracy, see the function iauEpv00.

Invocation:
void palEvp( double date, double deqx, double dvb[3], double dpb[3], double dvh[3], double dph[3] )

Arguments:

date = double (Given)
TDB (loosely ET) as a Modified Julian Date (JD-2400000.5)
deqx = double (Given)
Julian epoch (e.g. 2000.0) of mean equator and equinox of the vectors returned. If deqx = 0.0, all vectors are referred to the mean equator and equinox (FK5) of epoch date.
dvb = double[3] (Returned)
Barycentric velocity (AU/s, AU)
dpb = double[3] (Returned)
Barycentric position (AU/s, AU)
dvh = double[3] (Returned)
heliocentric velocity (AU/s, AU)
dph = double[3] (Returned)
Heliocentric position (AU/s, AU)


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node35.html000644 000765 000024 00000016305 12365763733 015041 0ustar00timjstaff000000 000000 palFk45z - Convert B1950.0 FK4 star data to J2000.0 FK5 assuming zero proper motion in the FK5 frame
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palFk45z - Convert B1950.0 FK4 star data to J2000.0 FK5 assuming zero proper motion in the FK5 frame

Description:
Convert B1950.0 FK4 star data to J2000.0 FK5 assuming zero proper motion in the FK5 frame (double precision)

This function converts stars from the Bessel-Newcomb, FK4 system to the IAU 1976, FK5, Fricke system, in such a way that the FK5 proper motion is zero. Because such a star has, in general, a non-zero proper motion in the FK4 system, the routine requires the epoch at which the position in the FK4 system was determined.

The method is from Appendix 2 of Ref 1, but using the constants of Ref 4.


Invocation:
palFk45z( double r1950, double d1950, double bepoch, double r2000, double d2000 )

Arguments:

r1950 = double (Given)
B1950.0 FK4 RA at epoch (radians).
d1950 = double (Given)
B1950.0 FK4 Dec at epoch (radians).
bepoch = double (Given)
Besselian epoch (e.g. 1979.3)
r2000 = double (Returned)
J2000.0 FK5 RA (Radians).
d2000 = double (Returned)
J2000.0 FK5 Dec(Radians).

Notes:
  • The epoch BEPOCH is strictly speaking Besselian, but if a Julian epoch is supplied the result will be affected only to a negligible extent.

  • Conversion from Besselian epoch 1950.0 to Julian epoch 2000.0 only is provided for. Conversions involving other epochs will require use of the appropriate precession, proper motion, and E-terms routines before and/or after palFk45z is called.

  • In the FK4 catalogue the proper motions of stars within 10 degrees of the poles do not embody the differential E-term effect and should, strictly speaking, be handled in a different manner from stars outside these regions. However, given the general lack of homogeneity of the star data available for routine astrometry, the difficulties of handling positions that may have been determined from astrometric fields spanning the polar and non-polar regions, the likelihood that the differential E-terms effect was not taken into account when allowing for proper motion in past astrometry, and the undesirability of a discontinuity in the algorithm, the decision has been made in this routine to include the effect of differential E-terms on the proper motions for all stars, whether polar or not. At epoch 2000, and measuring on the sky rather than in terms of dRA, the errors resulting from this simplification are less than 1 milliarcsecond in position and 1 milliarcsecond per century in proper motion.

References
  • Aoki,S., et al, 1983. Astron.Astrophys., 128, 263.

  • Smith, C.A. et al, 1989. "The transformation of astrometric catalog systems to the equinox J2000.0". Astron.J. 97, 265.

  • Yallop, B.D. et al, 1989. "Transformation of mean star places from FK4 B1950.0 to FK5 J2000.0 using matrices in 6-space". Astron.J. 97, 274.

  • Seidelmann, P.K. (ed), 1992. "Explanatory Supplement to the Astronomical Almanac", ISBN 0-935702-68-7.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node36.html000644 000765 000024 00000020140 12365763733 015032 0ustar00timjstaff000000 000000 palFk524 - Convert J2000.0 FK5 star data to B1950.0 FK4
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palFk524 - Convert J2000.0 FK5 star data to B1950.0 FK4

Description:
This function converts stars from the IAU 1976, FK5, Fricke system, to the Bessel-Newcomb, FK4 system. The precepts of Smith et al (Ref 1) are followed, using the implementation by Yallop et al (Ref 2) of a matrix method due to Standish. Kinoshita's development of Andoyer's post-Newcomb precession is used. The numerical constants from Seidelmann et al (Ref 3) are used canonically.

Invocation:
palFk524( double r2000, double d2000, double dr2000, double dd2000, double p2000, double v2000, double r1950, double d1950, double dr1950, double dd1950, double p1950, double v1950 )

Arguments:

r2000 = double (Given)
J2000.0 FK5 RA (radians).
d2000 = double (Given)
J2000.0 FK5 Dec (radians).
dr2000 = double (Given)
J2000.0 FK5 RA proper motion (rad/Jul.yr)
dd2000 = double (Given)
J2000.0 FK5 Dec proper motion (rad/Jul.yr)
p2000 = double (Given)
J2000.0 FK5 parallax (arcsec)
v2000 = double (Given)
J2000.0 FK5 radial velocity (km/s, ve = moving away)
r1950 = double (Returned)
B1950.0 FK4 RA (radians).
d1950 = double (Returned)
B1950.0 FK4 Dec (radians).
dr1950 = double (Returned)
B1950.0 FK4 RA proper motion (rad/Jul.yr)
dd1950 = double (Returned)
B1950.0 FK4 Dec proper motion (rad/Jul.yr)
p1950 = double (Returned)
B1950.0 FK4 parallax (arcsec)
v1950 = double (Returned)
B1950.0 FK4 radial velocity (km/s, ve = moving away)

Notes:
  • The proper motions in RA are dRA/dt rather than cos(Dec)dRA/dt, and are per year rather than per century.

  • Note that conversion from Julian epoch 2000.0 to Besselian epoch 1950.0 only is provided for. Conversions involving other epochs will require use of the appropriate precession, proper motion, and E-terms routines before and/or after FK524 is called.

  • In the FK4 catalogue the proper motions of stars within 10 degrees of the poles do not embody the differential E-term effect and should, strictly speaking, be handled in a different manner from stars outside these regions. However, given the general lack of homogeneity of the star data available for routine astrometry, the difficulties of handling positions that may have been determined from astrometric fields spanning the polar and non-polar regions, the likelihood that the differential E-terms effect was not taken into account when allowing for proper motion in past astrometry, and the undesirability of a discontinuity in the algorithm, the decision has been made in this routine to include the effect of differential E-terms on the proper motions for all stars, whether polar or not. At epoch 2000, and measuring on the sky rather than in terms of dRA, the errors resulting from this simplification are less than 1 milliarcsecond in position and 1 milliarcsecond per century in proper motion.

References
  • Smith, C.A. et al, 1989. "The transformation of astrometric catalog systems to the equinox J2000.0". Astron.J. 97, 265.

  • Yallop, B.D. et al, 1989. "Transformation of mean star places from FK4 B1950.0 to FK5 J2000.0 using matrices in 6-space". Astron.J. 97, 274.

  • Seidelmann, P.K. (ed), 1992. "Explanatory Supplement to the Astronomical Almanac", ISBN 0-935702-68-7.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node37.html000644 000765 000024 00000013561 12365763733 015044 0ustar00timjstaff000000 000000 palFk54z - Convert a J2000.0 FK5 star position to B1950.0 FK4 assuming zero proper motion and parallax
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palFk54z - Convert a J2000.0 FK5 star position to B1950.0 FK4 assuming zero proper motion and parallax

Description:
This function converts star positions from the IAU 1976, FK5, Fricke system to the Bessel-Newcomb, FK4 system.

Invocation:
palFk54z( double r2000, double d2000, double bepoch, double r1950, double d1950, double dr1950, double dd1950 )

Arguments:

r2000 = double (Given)
J2000.0 FK5 RA (radians).
d2000 = double (Given)
J2000.0 FK5 Dec (radians).
bepoch = double (Given)
Besselian epoch (e.g. 1950.0).
r1950 = double (Returned)
B1950 FK4 RA (radians) at epoch "bepoch".
d1950 = double (Returned)
B1950 FK4 Dec (radians) at epoch "bepoch".
dr1950 = double (Returned)
B1950 FK4 proper motion (RA) (radians/trop.yr)).
dr1950 = double (Returned)
B1950 FK4 proper motion (Dec) (radians/trop.yr)).

Notes:
  • The proper motion in RA is dRA/dt rather than cos(Dec)dRA/dt.

  • Conversion from Julian epoch 2000.0 to Besselian epoch 1950.0 only is provided for. Conversions involving other epochs will require use of the appropriate precession functions before and after this function is called.

  • The FK5 proper motions, the parallax and the radial velocity are presumed zero.

  • It is the intention that FK5 should be a close approximation to an inertial frame, so that distant objects have zero proper motion; such objects have (in general) non-zero proper motion in FK4, and this function returns those fictitious proper motions.

  • The position returned by this function is in the B1950 reference frame but at Besselian epoch BEPOCH. For comparison with catalogues the "bepoch" argument will frequently be 1950.0.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node38.html000644 000765 000024 00000011011 12365763733 015031 0ustar00timjstaff000000 000000 palGaleq - Convert from galactic to J2000.0 equatorial coordinates
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palGaleq - Convert from galactic to J2000.0 equatorial coordinates

Description:
Transformation from IAU 1958 galactic coordinates to J2000.0 equatorial coordinates.

Invocation:
void palGaleq ( double dl, double db, double dr, double dd );

Arguments:

dl = double (Given)
Galactic longitude (radians).
db = double (Given)
Galactic latitude (radians).
dr = double (Returned)
J2000.0 RA (radians)
dd = double (Returned)
J2000.0 Dec (radians)

Notes:
The equatorial coordinates are J2000.0. Use the routine palGe50 if conversion to B1950.0 'FK4' coordinates is required.
See Also
Blaauw et al, Mon.Not.R.Astron.Soc.,121,123 (1960)

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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node39.html000644 000765 000024 00000011247 12365763733 015045 0ustar00timjstaff000000 000000 palGalsup - Convert from galactic to supergalactic coordinates
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palGalsup - Convert from galactic to supergalactic coordinates

Description:
Transformation from IAU 1958 galactic coordinates to de Vaucouleurs supergalactic coordinates.

Invocation:
void palGalsup ( double dl, double db, double dsl, double dsb );

Arguments:

dl = double (Given)
Galactic longitude.
db = double (Given)
Galactic latitude.
dsl = double (Returned)
Supergalactic longitude.
dsb = double (Returned)
Supergalactic latitude.

See Also
  • de Vaucouleurs, de Vaucouleurs, & Corwin, Second Reference Catalogue of Bright Galaxies, U. Texas, page 8.

  • Systems & Applied Sciences Corp., Documentation for the machine-readable version of the above catalogue, Contract NAS 5-26490.


(These two references give different values for the galactic longitude of the supergalactic origin. Both are wrong; the correct value is L2=137.37.)

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Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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Function Descriptions


Subsections
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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node40.html000644 000765 000024 00000010671 12365763733 015035 0ustar00timjstaff000000 000000 palGe50 - Transform Galactic Coordinate to B1950 FK4
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palGe50 - Transform Galactic Coordinate to B1950 FK4

Description:
Transformation from IAU 1958 galactic coordinates to B1950.0 'FK4' equatorial coordinates.

Invocation:
palGe50( double dl, double db, double dr, double dd );

Arguments:

dl = double (Given)
Galactic longitude (radians)
db = double (Given)
Galactic latitude (radians)
dr = double (Returned)
B9150.0 FK4 RA.
dd = double (Returned)
B1950.0 FK4 Dec.

Notes:
  • The equatorial coordinates are B1950.0 'FK4'. Use the routine palGaleq if conversion to J2000.0 coordinates is required.

See Also
  • Blaauw et al, Mon.Not.R.Astron.Soc.,121,123 (1960)


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node41.html000644 000765 000024 00000010346 12365763733 015035 0ustar00timjstaff000000 000000 palGeoc - Convert geodetic position to geocentric
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palGeoc - Convert geodetic position to geocentric

Description:
Convert geodetic position to geocentric.

Invocation:
void palGeoc( double p, double h, double r, double z );

Arguments:

p = double (Given)
latitude (radians)
h = double (Given)
height above reference spheroid (geodetic, metres)
r = double (Returned)
distance from Earth axis (AU)
z = double (Returned)
distance from plane of Earth equator (AU)

Notes:
  • Geocentric latitude can be obtained by evaluating atan2(z,r)

  • Uses WGS84 reference ellipsoid and calls iauGd2gc


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node42.html000644 000765 000024 00000012062 12365763733 015033 0ustar00timjstaff000000 000000 palIntin - Convert free-format input into an integer
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palIntin - Convert free-format input into an integer

Description:
Extracts a number from an input string starting at the specified index.

Invocation:
void palIntin( const char string, int nstrt, long ireslt, int jflag );

Arguments:

string = const char (Given)
String containing number to be decoded.
nstrt = int (Given and Returned)
Character number indicating where decoding should start. On output its value is updated to be the location of the possible next value. For compatibility with SLA the first character is index 1.
ireslt = long (Returned)
Result. Not updated when jflag=1.
jflag = int (Returned)
status: -1 = -OK, 0 = OK, 1 = null, 2 = error

Notes:
  • Uses the strtol() system call to do the parsing. This may lead to subtle differences when compared to the SLA/F parsing.

  • Commas are recognized as a special case and are skipped if one happens to be the next character when updating nstrt. Additionally the output nstrt position will skip past any trailing space.

  • If no number can be found flag will be set to 1.

  • If the number overflows or underflows jflag will be set to 2. For overflow the returned result will have the value LONG_MAX, for underflow it will have the value LONG_MIN.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node43.html000644 000765 000024 00000012231 12365763733 015032 0ustar00timjstaff000000 000000 palMap - Convert star RA,Dec from mean place to geocentric apparent
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palMap - Convert star RA,Dec from mean place to geocentric apparent

Description:
Convert star RA,Dec from mean place to geocentric apparent.

Invocation:
void palMap( double rm, double dm, double pr, double pd, double px, double rv, double eq, double date, double ra, double da );

Arguments:

rm = double (Given)
Mean RA (radians)
dm = double (Given)
Mean declination (radians)
pr = double (Given)
RA proper motion, changes per Julian year (radians)
pd = double (Given)
Dec proper motion, changes per Julian year (radians)
px = double (Given)
Parallax (arcsec)
rv = double (Given)
Radial velocity (km/s, ve if receding)
eq = double (Given)
Epoch and equinox of star data (Julian)
date = double (Given)
TDB for apparent place (JD-2400000.5)
ra = double (Returned)
Apparent RA (radians)
dec = double (Returned)
Apparent dec (radians)

Notes:
  • Calls palMappa and palMapqk

  • The reference systems and timescales used are IAU 2006.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node44.html000644 000765 000024 00000012276 12365763733 015044 0ustar00timjstaff000000 000000 palMappa - Compute parameters needed by palAmpqk and palMapqk
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palMappa - Compute parameters needed by palAmpqk and palMapqk

Description:
Compute star-independent parameters in preparation for transformations between mean place and geocentric apparent place.

The parameters produced by this function are required in the parallax, aberration, and nutation/bias/precession parts of the mean/apparent transformations.

The reference systems and timescales used are IAU 2006.


Invocation:
void palMappa( double eq, double date, double amprms[21] )

Arguments:

eq = double (Given)
epoch of mean equinox to be used (Julian)
date = double (Given)
TDB (JD-2400000.5)
amprms = double[21] (Returned)
star-independent mean-to-apparent parameters:
  • (0) time interval for proper motion (Julian years)

  • (1-3) barycentric position of the Earth (AU)

  • (4-6) heliocentric direction of the Earth (unit vector)

  • (7) (grav rad Sun)2/(Sun-Earth distance)

  • (8-10) abv: barycentric Earth velocity in units of c

  • (11) sqrt(1-v2) where v=modulus(abv)

  • (12-20) precession/nutation (3,3) matrix


Notes:
  • For date, the distinction between the required TDB and TT is always negligible. Moreover, for all but the most critical applications UTC is adequate.

  • The vector amprms(1-3) is referred to the mean equinox and equator of epoch eq.

  • The parameters amprms produced by this function are used by palAmpqk, palMapqk and palMapqkz.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node45.html000644 000765 000024 00000012602 12365763733 015036 0ustar00timjstaff000000 000000 palMapqk - Quick mean to apparent place
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palMapqk - Quick mean to apparent place

Description:
Quick mean to apparent place: transform a star RA,Dec from mean place to geocentric apparent place, given the star-independent parameters.

Use of this routine is appropriate when efficiency is important and where many star positions, all referred to the same equator and equinox, are to be transformed for one epoch. The star-independent parameters can be obtained by calling the palMappa routine.

If the parallax and proper motions are zero the palMapqkz routine can be used instead.


Invocation:
void palMapqk ( double rm, double dm, double pr, double pd, double px, double rv, double amprms[21], double ra, double da );

Arguments:

rm = double (Given)
Mean RA (radians)
dm = double (Given)
Mean declination (radians)
pr = double (Given)
RA proper motion, changes per Julian year (radians)
pd = double (Given)
Dec proper motion, changes per Julian year (radians)
px = double (Given)
Parallax (arcsec)
rv = double (Given)
Radial velocity (km/s, ve if receding)
amprms = double [21] (Given)
Star-independent mean-to-apparent parameters (see palMappa).
ra = double (Returned)
Apparent RA (radians)
dec = double (Returned)
Apparent dec (radians)

Notes:
  • The reference frames and timescales used are post IAU 2006.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node46.html000644 000765 000024 00000012230 12365763733 015034 0ustar00timjstaff000000 000000 palMapqkz - Quick mean to apparent place
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palMapqkz - Quick mean to apparent place

Description:
Quick mean to apparent place: transform a star RA,dec from mean place to geocentric apparent place, given the star-independent parameters, and assuming zero parallax and proper motion.

Use of this function is appropriate when efficiency is important and where many star positions, all with parallax and proper motion either zero or already allowed for, and all referred to the same equator and equinox, are to be transformed for one epoch. The star-independent parameters can be obtained by calling the palMappa function.

The corresponding function for the case of non-zero parallax and proper motion is palMapqk.

The reference systems and timescales used are IAU 2006.

Strictly speaking, the function is not valid for solar-system sources, though the error will usually be extremely small.


Invocation:
void palMapqkz( double rm, double dm, double amprms[21], double ra, double da )

Arguments:

rm = double (Given)
Mean RA (radians).
dm = double (Given)
Mean Dec (radians).
amprms = double[21] (Given)
Star-independent mean-to-apparent parameters (see palMappa): (0-3) not used (4-6) not used (7) not used (8-10) abv: barycentric Earth velocity in units of c (11) sqrt(1-v2) where v=modulus(abv) (12-20) precession/nutation (3,3) matrix
ra = double (Returned)
Apparent RA (radians).
da = double (Returned)
Apparent Dec (radians).


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Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palNut - Form the matrix of nutation

Description:
Form the matrix of nutation for a given date using the IAU 2006 nutation model and palDeuler.

Invocation:
void palNut( double date, double rmatn[3][3] );

Arguments:

date = double (Given)
TT as modified Julian date (JD-2400000.5)
rmatn = double [3][3] (Returned)
Nutation matrix in the sense v(true)=rmatn v(mean) where v(true) is the star vector relative to the true equator and equinox of date and v(mean) is the star vector relative to the mean equator and equinox of date.

Notes:
  • Uses iauNut06a via palNutc

  • The distinction between TDB and TT is negligible. For all but the most critical applications UTC is adequate.


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Starlink User Note 267
Tim Jenness
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palNutc - Calculate nutation longitude & obliquoty components

Description:
Calculates the longitude obliquity components and mean obliquity using the SOFA library.

Invocation:
void palNutc( double date, double dpsi, double deps, double eps0 );

Arguments:

date = double (Given)
TT as modified Julian date (JD-2400000.5)
dpsi = double (Returned)
Nutation in longitude
deps = double (Returned)
Nutation in obliquity
eps0 = double (Returned)
Mean obliquity.

Notes:
  • Calls iauObl06 and iauNut06a and therefore uses the IAU 206 precession/nutation model.

  • Note the change from SLA/F regarding the date. TT is used rather than TDB.


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Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palObs - Parameters of selected ground-based observing stations

Description:
Station numbers, identifiers, names and other details are subject to change and should not be hardwired into application programs.

All characters in "c" up to the first space are checked; thus an abbreviated ID will return the parameters for the first station in the list which matches the abbreviation supplied, and no station in the list will ever contain embedded spaces. "c" must not have leading spaces.

IMPORTANT - BEWARE OF THE LONGITUDE SIGN CONVENTION. The longitude returned by sla_OBS is west-positive in accordance with astronomical usage. However, this sign convention is left-handed and is the opposite of the one used by geographers; elsewhere in PAL the preferable east-positive convention is used. In particular, note that for use in palAop, palAoppa and palOap the sign of the longitude must be reversed.

Users are urged to inform the author of any improvements they would like to see made. For example:

typographical corrections more accurate parameters better station identifiers or names additional stations


Invocation:
int palObs( size_t n, const char c, char ident, size_t identlen, char name, size_t namelen, double w, double p, double h );

Arguments:

n = size_t (Given)
Number specifying the observing station. If 0 the identifier in "c" is used to determine the observing station to use.
c = const char (Given)
Identifier specifying the observing station for which the parameters should be returned. Only used if n is 0. Can be NULL for n0. Case insensitive.
ident = char (Returned)
Identifier of the observing station selected. Will be identical to "c" if n==0. Unchanged if "n" or "c" do not match an observing station. Should be at least 11 characters (including the trailing nul).
identlen = size_t (Given)
Size of the buffer "ident" including trailing nul.
name = char (Returned)
Full name of the specified observing station. Contains "?" if "n" or "c" did not correspond to a valid station. Should be at least 41 characters (including the trailing nul).
w = double (Returned)
Longitude (radians, West ve). Unchanged if observing station could not be identified.
p = double (Returned)
Geodetic latitude (radians, North ve). Unchanged if observing station could not be identified.
h = double (Returned)
Height above sea level (metres). Unchanged if observing station could not be identified.

Returned Value:

palObs = int
0 if an observing station was returned. -1 if no match was found.

Notes:
  • Differs from the SLA interface in that the output short name is not the same variable as the input short name. This simplifies consting. Additionally the size of the output buffers are now specified in the API and a status integer is returned.


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Tim Jenness
2012 March 23
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SOFA Mappings

The following table lists PAL/SLA functions that have direct replacements in SOFA. Whilst these routines are implemented in the PAL library using SOFA new code should probably call SOFA directly.

SLA/PAL SOFA
palCldj iauCal2jd
palDbear iauPas
palDaf2r iauAf2a
palDav2m iauRv2m
palDcc2s iauC2s
palDcs2c iauS2c
palDd2tf iauD2tf
palDimxv iauTrxp
palDm2av iauRm2v
palDjcl iauJd2cal
palDmxm iauRxr
palDmxv iauRxp
palDpav iauPap
palDr2af iauA2af
palDr2tf iauA2tf
palDranrm iauAnp
palDsep iauSeps
palDsepv iauSepp
palDtf2d iauTf2d
palDtf2r iauTf2a
palDvdv iauPdp
palDvn iauPn
palDvxv iauPxp
palEpb iauEpb
palEpb2d iauEpb2d
palEpj iauEpj
palEpj2d iauEpj2jd
palEqeqx iauEe06a
palFk5hz iauFk5hz also calls iauEpj2jd
palGmst iauGmst06
palGmsta iauGmst06
palHfk5z iauHfk5z also calls iauEpj2jd

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Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

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palPa - HA, Dec to Parallactic Angle

Description:
Converts HA, Dec to Parallactic Angle.

Invocation:
double palPa( double ha, double dec, double phi );

Arguments:

ha = double (Given)
Hour angle in radians (Geocentric apparent)
dec = double (Given)
Declination in radians (Geocentric apparent)
phi = double (Given)
Observatory latitude in radians (geodetic)

Returned Value:

palPa = double
Parallactic angle in the range -pi to pi.

Notes:
  • The parallactic angle at a point in the sky is the position angle of the vertical, i.e. the angle between the direction to the pole and to the zenith. In precise applications care must be taken only to use geocentric apparent HA,Dec and to consider separately the effects of atmospheric refraction and telescope mount errors.

  • At the pole a zero result is returned.


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Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palPertel - Update elements by applying planetary perturbations

Description:
Update the osculating orbital elements of an asteroid or comet by applying planetary perturbations.

Invocation:
void palPertel (int jform, double date0, double date1, double epoch0, double orbi0, double anode0, double perih0, double aorq0, double e0, double am0, double epoch1, double orbi1, double anode1, double perih1, double aorq1, double e1, double am1, int jstat );

Arguments:

jform = int (Given)
Element set actually returned (1-3; Note 6)
date0 = double (Given)
Date of osculation (TT MJD) for the given elements.
date1 = double (Given)
Date of osculation (TT MJD) for the updated elements.
epoch0 = double (Given)
Epoch of elements (TT MJD)
orbi0 = double (Given)
inclination (radians)
anode0 = double (Given)
longitude of the ascending node (radians)
perih0 = double (Given)
longitude or argument of perihelion (radians)
aorq0 = double (Given)
mean distance or perihelion distance (AU)
e0 = double (Given)
eccentricity
am0 = double (Given)
mean anomaly (radians, JFORM=2 only)
epoch1 = double (Returned)
Epoch of elements (TT MJD)
orbi1 = double (Returned)
inclination (radians)
anode1 = double (Returned)
longitude of the ascending node (radians)
perih1 = double (Returned)
longitude or argument of perihelion (radians)
aorq1 = double (Returned)
mean distance or perihelion distance (AU)
e1 = double (Returned)
eccentricity
am1 = double (Returned)
mean anomaly (radians, JFORM=2 only)
jstat = int (Returned)
status:
  • 102 = warning, distant epoch

  • 101 = warning, large timespan ( 100 years)

  • 1 to 10 = coincident with planet (Note 6)

  • 0 = OK

  • -1 = illegal JFORM

  • -2 = illegal E0

  • -3 = illegal AORQ0

  • -4 = internal error

  • -5 = numerical error


Notes:
  • Two different element-format options are available:


Option JFORM=2, suitable for minor planets:

EPOCH = epoch of elements (TT MJD) ORBI = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = mean distance, a (AU) E = eccentricity, e AM = mean anomaly M (radians)

Option JFORM=3, suitable for comets:

EPOCH = epoch of perihelion (TT MJD) ORBI = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = perihelion distance, q (AU) E = eccentricity, e

  • DATE0, DATE1, EPOCH0 and EPOCH1 are all instants of time in the TT timescale (formerly Ephemeris Time, ET), expressed as Modified Julian Dates (JD-2400000.5).


DATE0 is the instant at which the given (i.e. unperturbed) osculating elements are correct.

DATE1 is the specified instant at which the updated osculating elements are correct.

EPOCH0 and EPOCH1 will be the same as DATE0 and DATE1 (respectively) for the JFORM=2 case, normally used for minor planets. For the JFORM=3 case, the two epochs will refer to perihelion passage and so will not, in general, be the same as DATE0 and/or DATE1 though they may be similar to one another.

  • The elements are with respect to the J2000 ecliptic and equinox.

  • Unused elements (AM0 and AM1 for JFORM=3) are not accessed.

  • See the palPertue routine for details of the algorithm used.

  • This routine is not intended to be used for major planets, which is why JFORM=1 is not available and why there is no opportunity to specify either the longitude of perihelion or the daily motion. However, if JFORM=2 elements are somehow obtained for a major planet and supplied to the routine, sensible results will, in fact, be produced. This happens because the sla_PERTUE routine that is called to perform the calculations checks the separation between the body and each of the planets and interprets a suspiciously small value (0.001 AU) as an attempt to apply it to the planet concerned. If this condition is detected, the contribution from that planet is ignored, and the status is set to the planet number (1-10 = Mercury, Venus, EMB, Mars, Jupiter, Saturn, Uranus, Neptune, Earth, Moon) as a warning.

See Also
  • Sterne, Theodore E., "An Introduction to Celestial Mechanics", Interscience Publishers Inc., 1960. Section 6.7, p199.


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Tim Jenness
2012 March 23
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Copyright © 2012 Science and Technology Facilities Council
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palPertue - Update the universal elements by applying planetary perturbations

Description:
Update the universal elements of an asteroid or comet by applying planetary perturbations.

Invocation:
void palPertue( double date, double u[13], int jstat );

Arguments:

date = double (Given)
Final epoch (TT MJD) for the update elements.
u = const double [13] (Given & Returned)
Universal orbital elements (Note 1) (0) combined mass (Mm) (1) total energy of the orbit (alpha) (2) reference (osculating) epoch (t0) (3-5) position at reference epoch (r0) (6-8) velocity at reference epoch (v0) (9) heliocentric distance at reference epoch (10) r0.v0 (11) date (t) (12) universal eccentric anomaly (psi) of date, approx
jstat = int (Returned)
status: 102 = warning, distant epoch 101 = warning, large timespan ( 100 years) 1 to 10 = coincident with major planet (Note 5) 0 = OK
  • 1 = numerical error


Notes:
  • The "universal" elements are those which define the orbit for the purposes of the method of universal variables (see reference 2). They consist of the combined mass of the two bodies, an epoch, and the position and velocity vectors (arbitrary reference frame) at that epoch. The parameter set used here includes also various quantities that can, in fact, be derived from the other information. This approach is taken to avoiding unnecessary computation and loss of accuracy. The supplementary quantities are (i) alpha, which is proportional to the total energy of the orbit, (ii) the heliocentric distance at epoch, (iii) the outwards component of the velocity at the given epoch, (iv) an estimate of psi, the "universal eccentric anomaly" at a given date and (v) that date.

  • The universal elements are with respect to the J2000 equator and equinox.

  • The epochs DATE, U(3) and U(12) are all Modified Julian Dates (JD-2400000.5).

  • The algorithm is a simplified form of Encke's method. It takes as a basis the unperturbed motion of the body, and numerically integrates the perturbing accelerations from the major planets. The expression used is essentially Sterne's 6.7-2 (reference 1). Everhart and Pitkin (reference 2) suggest rectifying the orbit at each integration step by propagating the new perturbed position and velocity as the new universal variables. In the present routine the orbit is rectified less frequently than this, in order to gain a slight speed advantage. However, the rectification is done directly in terms of position and velocity, as suggested by Everhart and Pitkin, bypassing the use of conventional orbital elements.


The f(q) part of the full Encke method is not used. The purpose of this part is to avoid subtracting two nearly equal quantities when calculating the "indirect member", which takes account of the small change in the Sun's attraction due to the slightly displaced position of the perturbed body. A simpler, direct calculation in double precision proves to be faster and not significantly less accurate.

Apart from employing a variable timestep, and occasionally "rectifying the orbit" to keep the indirect member small, the integration is done in a fairly straightforward way. The acceleration estimated for the middle of the timestep is assumed to apply throughout that timestep; it is also used in the extrapolation of the perturbations to the middle of the next timestep, to predict the new disturbed position. There is no iteration within a timestep.

Measures are taken to reach a compromise between execution time and accuracy. The starting-point is the goal of achieving arcsecond accuracy for ordinary minor planets over a ten-year timespan. This goal dictates how large the timesteps can be, which in turn dictates how frequently the unperturbed motion has to be recalculated from the osculating elements.

Within predetermined limits, the timestep for the numerical integration is varied in length in inverse proportion to the magnitude of the net acceleration on the body from the major planets.

The numerical integration requires estimates of the major-planet motions. Approximate positions for the major planets (Pluto alone is omitted) are obtained from the routine palPlanet. Two levels of interpolation are used, to enhance speed without significantly degrading accuracy. At a low frequency, the routine palPlanet is called to generate updated positionvelocity "state vectors". The only task remaining to be carried out at the full frequency (i.e. at each integration step) is to use the state vectors to extrapolate the planetary positions. In place of a strictly linear extrapolation, some allowance is made for the curvature of the orbit by scaling back the radius vector as the linear extrapolation goes off at a tangent.

Various other approximations are made. For example, perturbations by Pluto and the minor planets are neglected and relativistic effects are not taken into account.

In the interests of simplicity, the background calculations for the major planets are carried out en masse. The mean elements and state vectors for all the planets are refreshed at the same time, without regard for orbit curvature, mass or proximity.

The Earth-Moon system is treated as a single body when the body is distant but as separate bodies when closer to the EMB than the parameter RNE, which incurs a time penalty but improves accuracy for near-Earth objects.

  • This routine is not intended to be used for major planets. However, if major-planet elements are supplied, sensible results will, in fact, be produced. This happens because the routine checks the separation between the body and each of the planets and interprets a suspiciously small value (0.001 AU) as an attempt to apply the routine to the planet concerned. If this condition is detected, the contribution from that planet is ignored, and the status is set to the planet number (1-10 = Mercury, Venus, EMB, Mars, Jupiter, Saturn, Uranus, Neptune, Earth, Moon) as a warning.

See Also
  • Sterne, Theodore E., "An Introduction to Celestial Mechanics", Interscience Publishers Inc., 1960. Section 6.7, p199.

  • Everhart, E. & Pitkin, E.T., Am.J.Phys. 51, 712, 1983.


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Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

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palPlanel - Transform conventional elements into position and velocity

Description:
Heliocentric position and velocity of a planet, asteroid or comet, starting from orbital elements.

Invocation:
void palPlanel ( double date, int jform, double epoch, double orbinc, double anode, double perih, double aorq, double e, double aorl, double dm, double pv[6], int jstat );

Arguments:

date = double (Given)
Epoch (TT MJD) of osculation (Note 1)
jform = int (Given)
Element set actually returned (1-3; Note 3)
epoch = double (Given)
Epoch of elements (TT MJD) (Note 4)
orbinc = double (Given)
inclination (radians)
anode = double (Given)
longitude of the ascending node (radians)
perih = double (Given)
longitude or argument of perihelion (radians)
aorq = double (Given)
mean distance or perihelion distance (AU)
e = double (Given)
eccentricity
aorl = double (Given)
mean anomaly or longitude (radians, JFORM=1,2 only)
dm = double (Given)
daily motion (radians, JFORM=1 only)
u = double [13] (Returned)
Universal orbital elements (Note 1) (0) combined mass (Mm) (1) total energy of the orbit (alpha) (2) reference (osculating) epoch (t0) (3-5) position at reference epoch (r0) (6-8) velocity at reference epoch (v0) (9) heliocentric distance at reference epoch (10) r0.v0 (11) date (t) (12) universal eccentric anomaly (psi) of date, approx
jstat = int (Returned)
status: 0 = OK
  • -1 = illegal JFORM

  • -2 = illegal E

  • -3 = illegal AORQ

  • -4 = illegal DM

  • -5 = numerical error


Notes:
  • DATE is the instant for which the prediction is required. It is in the TT timescale (formerly Ephemeris Time, ET) and is a Modified Julian Date (JD-2400000.5).

  • The elements are with respect to the J2000 ecliptic and equinox.

  • A choice of three different element-set options is available:


Option JFORM = 1, suitable for the major planets:

EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = longitude of perihelion, curly pi (radians) AORQ = mean distance, a (AU) E = eccentricity, e (range 0 to 1) AORL = mean longitude L (radians) DM = daily motion (radians)

Option JFORM = 2, suitable for minor planets:

EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = mean distance, a (AU) E = eccentricity, e (range 0 to 1) AORL = mean anomaly M (radians)

Option JFORM = 3, suitable for comets:

EPOCH = epoch of elements and perihelion (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = perihelion distance, q (AU) E = eccentricity, e (range 0 to 10)

Unused arguments (DM for JFORM=2, AORL and DM for JFORM=3) are not accessed.

  • Each of the three element sets defines an unperturbed heliocentric orbit. For a given epoch of observation, the position of the body in its orbit can be predicted from these elements, which are called "osculating elements", using standard two-body analytical solutions. However, due to planetary perturbations, a given set of osculating elements remains usable for only as long as the unperturbed orbit that it describes is an adequate approximation to reality. Attached to such a set of elements is a date called the "osculating epoch", at which the elements are, momentarily, a perfect representation of the instantaneous position and velocity of the body.


Therefore, for any given problem there are up to three different epochs in play, and it is vital to distinguish clearly between them:

. The epoch of observation: the moment in time for which the position of the body is to be predicted.

. The epoch defining the position of the body: the moment in time at which, in the absence of purturbations, the specified position (mean longitude, mean anomaly, or perihelion) is reached.

. The osculating epoch: the moment in time at which the given elements are correct.

For the major-planet and minor-planet cases it is usual to make the epoch that defines the position of the body the same as the epoch of osculation. Thus, only two different epochs are involved: the epoch of the elements and the epoch of observation.

For comets, the epoch of perihelion fixes the position in the orbit and in general a different epoch of osculation will be chosen. Thus, all three types of epoch are involved.

For the present routine:

. The epoch of observation is the argument DATE.

. The epoch defining the position of the body is the argument EPOCH.

. The osculating epoch is not used and is assumed to be close enough to the epoch of observation to deliver adequate accuracy. If not, a preliminary call to sla_PERTEL may be used to update the element-set (and its associated osculating epoch) by applying planetary perturbations.

  • The reference frame for the result is with respect to the mean equator and equinox of epoch J2000.

  • The algorithm was originally adapted from the EPHSLA program of D.H.P.Jones (private communication, 1996). The method is based on Stumpff's Universal Variables.

See Also
Everhart, E. & Pitkin, E.T., Am.J.Phys. 51, 712, 1983.

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Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palPlanet - Approximate heliocentric position and velocity of major planet

Description:
Calculates the approximate heliocentric position and velocity of the specified major planet.

Invocation:
void palPlanet ( double date, int np, double pv[6], int j );

Arguments:

date = double (Given)
TDB Modified Julian Date (JD-2400000.5).
np = int (Given)
planet (1=Mercury, 2=Venus, 3=EMB, 4=Mars, 5=Jupiter, 6=Saturn, 7=Uranus, 8=Neptune)
pv = double [6] (Returned)
heliocentric x,y,z,xdot,ydot,zdot, J2000, equatorial triad in units AU and AU/s.
j = int (Returned)
  • -2 = solution didn't converge.

  • -1 = illegal np (1-8)

  • 0 = OK

  • 1 = warning: year outside 1000-3000


Notes:
  • See SOFA iauPlan94 for details

  • Note that Pluto is supported in SLA/F but not in this routine

  • Status -2 is equivalent to iauPlan94 status 2.

  • Note that velocity units here match the SLA/F documentation.


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Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palPlante - Topocentric RA,Dec of a Solar-System object from heliocentric orbital elements

Description:
Topocentric apparent RA,Dec of a Solar-System object whose heliocentric orbital elements are known.

Invocation:
void palPlante ( double date, double elong, double phi, int jform, double epoch, double orbinc, double anode, double perih, double aorq, double e, double aorl, double dm, double ra, double dec, double r, int jstat );

Arguments:

date = double (Given)
TT MJD of observation (JD-2400000.5)
elong = double (Given)
Observer's east longitude (radians)
phi = double (Given)
Observer's geodetic latitude (radians)
jform = int (Given)
Element set actually returned (1-3; Note 6)
epoch = double (Given)
Epoch of elements (TT MJD)
orbinc = double (Given)
inclination (radians)
anode = double (Given)
longitude of the ascending node (radians)
perih = double (Given)
longitude or argument of perihelion (radians)
aorq = double (Given)
mean distance or perihelion distance (AU)
e = double (Given)
eccentricity
aorl = double (Given)
mean anomaly or longitude (radians, JFORM=1,2 only)
dm = double (Given)
daily motion (radians, JFORM=1 only)
ra = double (Returned)
Topocentric apparent RA (radians)
dec = double (Returned)
Topocentric apparent Dec (radians)
r = double (Returned)
Distance from observer (AU)
jstat = int (Returned)
status: 0 = OK
  • -1 = illegal jform

  • -2 = illegal e

  • -3 = illegal aorq

  • -4 = illegal dm

  • -5 = numerical error


Notes:
  • DATE is the instant for which the prediction is required. It is in the TT timescale (formerly Ephemeris Time, ET) and is a Modified Julian Date (JD-2400000.5).

  • The longitude and latitude allow correction for geocentric parallax. This is usually a small effect, but can become important for near-Earth asteroids. Geocentric positions can be generated by appropriate use of routines palEpv (or palEvp) and palUe2pv.

  • The elements are with respect to the J2000 ecliptic and equinox.

  • A choice of three different element-set options is available:


Option JFORM = 1, suitable for the major planets:

EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = longitude of perihelion, curly pi (radians) AORQ = mean distance, a (AU) E = eccentricity, e (range 0 to 1) AORL = mean longitude L (radians) DM = daily motion (radians)

Option JFORM = 2, suitable for minor planets:

EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = mean distance, a (AU) E = eccentricity, e (range 0 to 1) AORL = mean anomaly M (radians)

Option JFORM = 3, suitable for comets:

EPOCH = epoch of elements and perihelion (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = perihelion distance, q (AU) E = eccentricity, e (range 0 to 10)

Unused arguments (DM for JFORM=2, AORL and DM for JFORM=3) are not accessed.

  • Each of the three element sets defines an unperturbed heliocentric orbit. For a given epoch of observation, the position of the body in its orbit can be predicted from these elements, which are called "osculating elements", using standard two-body analytical solutions. However, due to planetary perturbations, a given set of osculating elements remains usable for only as long as the unperturbed orbit that it describes is an adequate approximation to reality. Attached to such a set of elements is a date called the "osculating epoch", at which the elements are, momentarily, a perfect representation of the instantaneous position and velocity of the body.


Therefore, for any given problem there are up to three different epochs in play, and it is vital to distinguish clearly between them:

. The epoch of observation: the moment in time for which the position of the body is to be predicted.

. The epoch defining the position of the body: the moment in time at which, in the absence of purturbations, the specified position (mean longitude, mean anomaly, or perihelion) is reached.

. The osculating epoch: the moment in time at which the given elements are correct.

For the major-planet and minor-planet cases it is usual to make the epoch that defines the position of the body the same as the epoch of osculation. Thus, only two different epochs are involved: the epoch of the elements and the epoch of observation.

For comets, the epoch of perihelion fixes the position in the orbit and in general a different epoch of osculation will be chosen. Thus, all three types of epoch are involved.

For the present routine:

. The epoch of observation is the argument DATE.

. The epoch defining the position of the body is the argument EPOCH.

. The osculating epoch is not used and is assumed to be close enough to the epoch of observation to deliver adequate accuracy. If not, a preliminary call to sla_PERTEL may be used to update the element-set (and its associated osculating epoch) by applying planetary perturbations.

  • Two important sources for orbital elements are Horizons, operated by the Jet Propulsion Laboratory, Pasadena, and the Minor Planet Center, operated by the Center for Astrophysics, Harvard.


The JPL Horizons elements (heliocentric, J2000 ecliptic and equinox) correspond to SLALIB arguments as follows.

Major planets:

JFORM = 1 EPOCH = JDCT-2400000.5 ORBINC = IN (in radians) ANODE = OM (in radians) PERIH = OMW (in radians) AORQ = A E = EC AORL = MAOMW (in radians) DM = N (in radians)

Epoch of osculation = JDCT-2400000.5

Minor planets:

JFORM = 2 EPOCH = JDCT-2400000.5 ORBINC = IN (in radians) ANODE = OM (in radians) PERIH = W (in radians) AORQ = A E = EC AORL = MA (in radians)

Epoch of osculation = JDCT-2400000.5

Comets:

JFORM = 3 EPOCH = Tp-2400000.5 ORBINC = IN (in radians) ANODE = OM (in radians) PERIH = W (in radians) AORQ = QR E = EC

Epoch of osculation = JDCT-2400000.5

The MPC elements correspond to SLALIB arguments as follows.

Minor planets:

JFORM = 2 EPOCH = Epoch-2400000.5 ORBINC = Incl. (in radians) ANODE = Node (in radians) PERIH = Perih. (in radians) AORQ = a E = e AORL = M (in radians)

Epoch of osculation = Epoch-2400000.5

Comets:

JFORM = 3 EPOCH = T-2400000.5 ORBINC = Incl. (in radians) ANODE = Node. (in radians) PERIH = Perih. (in radians) AORQ = q E = e

Epoch of osculation = Epoch-2400000.5


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palPlantu - Topocentric RA,Dec of a Solar-System object from universal elements

Description:
Topocentric apparent RA,Dec of a Solar-System object whose heliocentric universal elements are known.

Invocation:
void palPlantu ( double date, double elong, double phi, const double u[13], double ra, double dec, double r, int jstat ) {

Arguments:

date = double (Given)
TT MJD of observation (JD-2400000.5)
elong = double (Given)
Observer's east longitude (radians)
phi = double (Given)
Observer's geodetic latitude (radians)
u = const double [13] (Given)
Universal orbital elements
  • (0) combined mass (Mm)

  • (1) total energy of the orbit (alpha)

  • (2) reference (osculating) epoch (t0)

  • (3-5) position at reference epoch (r0)

  • (6-8) velocity at reference epoch (v0)

  • (9) heliocentric distance at reference epoch

  • (10) r0.v0

  • (11) date (t)

  • (12) universal eccentric anomaly (psi) of date, approx

ra = double (Returned)
Topocentric apparent RA (radians)
dec = double (Returned)
Topocentric apparent Dec (radians)
r = double (Returned)
Distance from observer (AU)
jstat = int (Returned)
status: 0 = OK
  • -1 = radius vector zero

  • -2 = failed to converge


Notes:
  • DATE is the instant for which the prediction is required. It is in the TT timescale (formerly Ephemeris Time, ET) and is a Modified Julian Date (JD-2400000.5).

  • The longitude and latitude allow correction for geocentric parallax. This is usually a small effect, but can become important for near-Earth asteroids. Geocentric positions can be generated by appropriate use of routines palEpv (or palEvp) and palUe2pv.

  • The "universal" elements are those which define the orbit for the purposes of the method of universal variables (see reference 2). They consist of the combined mass of the two bodies, an epoch, and the position and velocity vectors (arbitrary reference frame) at that epoch. The parameter set used here includes also various quantities that can, in fact, be derived from the other information. This approach is taken to avoiding unnecessary computation and loss of accuracy. The supplementary quantities are (i) alpha, which is proportional to the total energy of the orbit, (ii) the heliocentric distance at epoch, (iii) the outwards component of the velocity at the given epoch, (iv) an estimate of psi, the "universal eccentric anomaly" at a given date and (v) that date.

  • The universal elements are with respect to the J2000 equator and equinox.

See Also
  • Sterne, Theodore E., "An Introduction to Celestial Mechanics", Interscience Publishers Inc., 1960. Section 6.7, p199.

  • Everhart, E. & Pitkin, E.T., Am.J.Phys. 51, 712, 1983.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palPm - Apply corrections for proper motion a star RA,Dec

Description:
Apply corrections for proper motion to a star RA,Dec using the SOFA routine iauStarpm.

Invocation:
void palPm ( double r0, double d0, double pr, double pd, double px, double rv, double ep0, double ep1, double r1, double d1 );

Arguments:

r0 = double (Given)
RA at epoch ep0 (radians)
d0 = double (Given)
Dec at epoch ep0 (radians)
pr = double (Given)
RA proper motion in radians per year.
pd = double (Given)
Dec proper motion in radians per year.
px = double (Given)
Parallax (arcsec)
rv = double (Given)
Radial velocity (km/sec ve if receding)
ep0 = double (Given)
Start epoch in years, assumed to be Julian.
ep1 = double (Given)
End epoch in years, assumed to be Julian.
r1 = double (Returned)
RA at epoch ep1 (radians)
d1 = double (Returned)
Dec at epoch ep1 (radians)

Notes:
  • Uses iauStarpm but ignores the status returns from that routine. In particular note that parallax should not be zero when the proper motions are non-zero. SLA/F allows parallax to be zero.

  • Assumes all epochs are Julian epochs.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palPrebn - Generate the matrix of precession between two objects (old)

Description:
Generate the matrix of precession between two epochs, using the old, pre-IAU1976, Bessel-Newcomb model, using Kinoshita's formulation

Invocation:
void palPrebn ( double bep0, double bep1, double rmatp[3][3] );

Arguments:

bep0 = double (Given)
Beginning Besselian epoch.
bep1 = double (Given)
Ending Besselian epoch
rmatp = double[3][3] (Returned)
precession matrix in the sense V(BEP1) = RMATP V(BEP0)

See Also
Kinoshita, H. (1975) 'Formulas for precession', SAO Special Report No. 364, Smithsonian Institution Astrophysical Observatory, Cambridge, Massachusetts.

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Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palPrec - Form the matrix of precession between two epochs (IAU 2006)

Description:
The IAU 2006 precession matrix from ep0 to ep1 is found and returned. The matrix is in the sense V(EP1) = RMATP V(EP0). The epochs are TDB (loosely TT) Julian epochs.

Though the matrix method itself is rigorous, the precession angles are expressed through canonical polynomials which are valid only for a limited time span of a few hundred years around the current epoch.


Invocation:
palPrec( double ep0, double ep1, double rmatp[3][3] )

Arguments:

ep0 = double (Given)
Beginning epoch
ep1 = double (Given)
Ending epoch
rmatp = double[3][3] (Returned)
Precession matrix


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Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node6.html000644 000765 000024 00000006053 12365763733 014756 0ustar00timjstaff000000 000000 More complex functions
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Previous: SOFA Mappings

More complex functions

These functions do not have a simple equivalent in SOFA so are reimplemented either completely standalone or using multiple SOFA functions.


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Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palPreces - Precession - either FK4 or FK5 as required

Description:
Precess coordinates using the appropriate system and epochs.

Invocation:
void palPreces ( const char sys[3], double ep0, double ep1, double ra, double dc );

Arguments:

sys = const char [3] (Given)
Precession to be applied: FK4 or FK5. Case insensitive.
ep0 = double (Given)
Starting epoch.
ep1 = double (Given)
Ending epoch
ra = double (Given & Returned)
On input the RA mean equator & equinox at epoch ep0. On exit the RA mean equator & equinox of epoch ep1.
dec = double (Given & Returned)
On input the dec mean equator & equinox at epoch ep0. On exit the dec mean equator & equinox of epoch ep1.

Notes:
  • Uses palPrec for FK5 data and palPrebn for FK4 data.

  • The epochs are Besselian if SYSTEM='FK4' and Julian if 'FK5'. For example, to precess coordinates in the old system from equinox 1900.0 to 1950.0 the call would be: palPreces( "FK4", 1900.0, 1950.0, &ra, &dc );

  • This routine will NOT correctly convert between the old and the new systems - for example conversion from B1950 to J2000. For these purposes see palFk425, palFk524, palFk45z and palFk54z.

  • If an invalid SYSTEM is supplied, values of -99D0,-99D0 will be returned for both RA and DC.


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Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palPrenut - Form the matrix of bias-precession-nutation (IAU 2006/2000A)

Description:
Form the matrix of bias-precession-nutation (IAU 2006/2000A). The epoch and date are TT (but TDB is usually close enough). The matrix is in the sense v(true) = rmatpn v(mean).

Invocation:
void palPrenut( double epoch, double date, double rmatpn[3][3] )

Arguments:

epoch = double (Returned)
Julian epoch for mean coordinates.
date = double (Returned)
Modified Julian Date (JD-2400000.5) for true coordinates.
rmatpn = double[3][3] (Returned)
combined NPB matrix


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Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palPv2el - Position velocity to heliocentirc osculating elements

Description:
Heliocentric osculating elements obtained from instantaneous position and velocity.

Invocation:
void palPv2el ( const double pv[6], double date, double pmass, int jformr, int jform, double epoch, double orbinc, double anode, double perih, double aorq, double e, double aorl, double dm, int jstat );

Arguments:

pv = const double [6] (Given)
Heliocentric x,y,z,xdot,ydot,zdot of date, J2000 equatorial triad (AU,AU/s; Note 1)
date = double (Given)
Date (TT Modified Julian Date = JD-2400000.5)
pmass = double (Given)
Mass of the planet (Sun=1; Note 2)
jformr = int (Given)
Requested element set (1-3; Note 3)
jform = int (Returned)
Element set actually returned (1-3; Note 4)
epoch = double (Returned)
Epoch of elements (TT MJD)
orbinc = double (Returned)
inclination (radians)
anode = double (Returned)
longitude of the ascending node (radians)
perih = double (Returned)
longitude or argument of perihelion (radians)
aorq = double (Returned)
mean distance or perihelion distance (AU)
e = double (Returned)
eccentricity
aorl = double (Returned)
mean anomaly or longitude (radians, JFORM=1,2 only)
dm = double (Returned)
daily motion (radians, JFORM=1 only)
jstat = int (Returned)
status: 0 = OK
  • -1 = illegal PMASS

  • -2 = illegal JFORMR

  • -3 = position/velocity out of range


Notes:
  • The PV 6-vector is with respect to the mean equator and equinox of epoch J2000. The orbital elements produced are with respect to the J2000 ecliptic and mean equinox.

  • The mass, PMASS, is important only for the larger planets. For most purposes (e.g. asteroids) use 0D0. Values less than zero are illegal.

  • Three different element-format options are supported:


Option JFORM=1, suitable for the major planets:

EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = longitude of perihelion, curly pi (radians) AORQ = mean distance, a (AU) E = eccentricity, e AORL = mean longitude L (radians) DM = daily motion (radians)

Option JFORM=2, suitable for minor planets:

EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = mean distance, a (AU) E = eccentricity, e AORL = mean anomaly M (radians)

Option JFORM=3, suitable for comets:

EPOCH = epoch of perihelion (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = perihelion distance, q (AU) E = eccentricity, e

  • It may not be possible to generate elements in the form requested through JFORMR. The caller is notified of the form of elements actually returned by means of the JFORM argument:


JFORMR JFORM meaning

1 1 OK - elements are in the requested format 1 2 never happens 1 3 orbit not elliptical

2 1 never happens 2 2 OK - elements are in the requested format 2 3 orbit not elliptical

3 1 never happens 3 2 never happens 3 3 OK - elements are in the requested format

  • The arguments returned for each value of JFORM (cf Note 5: JFORM may not be the same as JFORMR) are as follows:


JFORM 1 2 3 EPOCH t0 t0 T ORBINC i i i ANODE Omega Omega Omega PERIH curly pi omega omega AORQ a a q E e e e AORL L M - DM n - -

where:

t0 is the epoch of the elements (MJD, TT) T " epoch of perihelion (MJD, TT) i " inclination (radians) Omega " longitude of the ascending node (radians) curly pi " longitude of perihelion (radians) omega " argument of perihelion (radians) a " mean distance (AU) q " perihelion distance (AU) e " eccentricity L " longitude (radians, 0-2pi) M " mean anomaly (radians, 0-2pi) n " daily motion (radians)

  • means no value is set

  • At very small inclinations, the longitude of the ascending node ANODE becomes indeterminate and under some circumstances may be set arbitrarily to zero. Similarly, if the orbit is close to circular, the true anomaly becomes indeterminate and under some circumstances may be set arbitrarily to zero. In such cases, the other elements are automatically adjusted to compensate, and so the elements remain a valid description of the orbit.

  • The osculating epoch for the returned elements is the argument DATE.

  • Reference: Sterne, Theodore E., "An Introduction to Celestial Mechanics", Interscience Publishers, 1960


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Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palPv2ue - Universal elements to position and velocity

Description:
Construct a universal element set based on an instantaneous position and velocity.

Invocation:
void palPv2ue( const double pv[6], double date, double pmass, double u[13], int jstat );

Arguments:

pv = double [6] (Given)
Heliocentric x,y,z,xdot,ydot,zdot of date, (AU,AU/s; Note 1)
date = double (Given)
Date (TT modified Julian Date = JD-2400000.5)
pmass = double (Given)
Mass of the planet (Sun=1; note 2)
u = double [13] (Returned)
Universal orbital elements (Note 3)

  • (0) combined mass (Mm)

  • (1) total energy of the orbit (alpha)

  • (2) reference (osculating) epoch (t0)

  • (3-5) position at reference epoch (r0)

  • (6-8) velocity at reference epoch (v0)

  • (9) heliocentric distance at reference epoch

  • (10) r0.v0

  • (11) date (t)

  • (12) universal eccentric anomaly (psi) of date, approx

jstat = int (Returned)
status: 0 = OK
  • -1 = illegal PMASS

  • -2 = too close to Sun

  • -3 = too slow


Notes:
  • The PV 6-vector can be with respect to any chosen inertial frame, and the resulting universal-element set will be with respect to the same frame. A common choice will be mean equator and ecliptic of epoch J2000.

  • The mass, PMASS, is important only for the larger planets. For most purposes (e.g. asteroids) use 0D0. Values less than zero are illegal.

  • The "universal" elements are those which define the orbit for the purposes of the method of universal variables (see reference). They consist of the combined mass of the two bodies, an epoch, and the position and velocity vectors (arbitrary reference frame) at that epoch. The parameter set used here includes also various quantities that can, in fact, be derived from the other information. This approach is taken to avoiding unnecessary computation and loss of accuracy. The supplementary quantities are (i) alpha, which is proportional to the total energy of the orbit, (ii) the heliocentric distance at epoch, (iii) the outwards component of the velocity at the given epoch, (iv) an estimate of psi, the "universal eccentric anomaly" at a given date and (v) that date.

  • Reference: Everhart, E. & Pitkin, E.T., Am.J.Phys. 51, 712, 1983.


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Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node64.html000644 000765 000024 00000010457 12365763733 015045 0ustar00timjstaff000000 000000 palPvobs - Position and velocity of an observing station
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palPvobs - Position and velocity of an observing station

Description:
Returns the position and velocity of an observing station.

Invocation:
palPvobs( double p, double h, double stl, double pv[6] )

Arguments:

p = double (Given)
Latitude (geodetic, radians).
h = double (Given)
Height above reference spheroid (geodetic, metres).
stl = double (Given)
Local apparent sidereal time (radians).
pv = double[ 6 ] (Returned)
position/velocity 6-vector (AU, AU/s, true equator and equinox of date).

Notes:
  • The WGS84 reference ellipsoid is used.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node65.html000644 000765 000024 00000013032 12365763733 015036 0ustar00timjstaff000000 000000 palRdplan - Approximate topocentric apparent RA,Dec of a planet
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palRdplan - Approximate topocentric apparent RA,Dec of a planet

Description:
Approximate topocentric apparent RA,Dec of a planet, and its angular diameter.

Invocation:
void palRdplan( double date, int np, double elong, double phi, double ra, double dec, double diam );

Arguments:

date = double (Given)
MJD of observation (JD-2400000.5) in TDB. For all practical purposes TT can be used instead of TDB, and for many applications UT will do (except for the Moon).
np = int (Given)
Planet: 1 = Mercury 2 = Venus 3 = Moon 4 = Mars 5 = Jupiter 6 = Saturn 7 = Uranus 8 = Neptune else = Sun
elong = double (Given)
Observer's east longitude (radians)
phi = double (Given)
Observer's geodetic latitude (radians)
ra = double (Returned)
RA (topocentric apparent, radians)
dec = double (Returned)
Dec (topocentric apparent, radians)
diam = double (Returned)
Angular diameter (equatorial, radians)

Notes:
  • Unlike with slaRdplan, Pluto is not supported.

  • The longitude and latitude allow correction for geocentric parallax. This is a major effect for the Moon, but in the context of the limited accuracy of the present routine its effect on planetary positions is small (negligible for the outer planets). Geocentric positions can be generated by appropriate use of the routines palDmoon and iauPlan94.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node66.html000644 000765 000024 00000011423 12365763733 015041 0ustar00timjstaff000000 000000 palRverot - Velocity component in a given direction due to Earth rotation
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palRverot - Velocity component in a given direction due to Earth rotation

Description:
Calculate the velocity component in a given direction due to Earth rotation.

The simple algorithm used assumes a spherical Earth, of a radius chosen to give results accurate to about 0.0005 km/s for observing stations at typical latitudes and heights. For applications requiring greater precision, use the routine palPvobs.


Invocation:
double palRverot ( double phi, double ra, double da, double st );

Arguments:

phi = double (Given)
latitude of observing station (geodetic) (radians)
ra = double (Given)
apparent RA (radians)
da = double (Given)
apparent Dec (radians)
st = double (Given)

Returned Value:

palRverot = double
Component of Earth rotation in direction RA,DA (km/s). The result is ve when the observatory is receding from the given point on the sky.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node67.html000644 000765 000024 00000011776 12365763733 015055 0ustar00timjstaff000000 000000 palRvgalc - Velocity component in a given direction due to the rotation of the Galaxy
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palRvgalc - Velocity component in a given direction due to the rotation of the Galaxy

Description:
This function returns the Component of dynamical LSR motion in the direction of R2000,D2000. The result is ve when the dynamical LSR is receding from the given point on the sky.

Invocation:
double palRvgalc( double r2000, double d2000 )

Arguments:

r2000 = double (Given)
J2000.0 mean RA (radians)
d2000 = double (Given)
J2000.0 mean Dec (radians)

Returned Value:

Component of dynamical LSR motion in direction R2000,D2000 (km/s).

Notes:
  • The Local Standard of Rest used here is a point in the vicinity of the Sun which is in a circular orbit around the Galactic centre. Sometimes called the "dynamical" LSR, it is not to be confused with a "kinematical" LSR, which is the mean standard of rest of star catalogues or stellar populations.

Reference
  • The orbital speed of 220 km/s used here comes from Kerr & Lynden-Bell (1986), MNRAS, 221, p1023.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node68.html000644 000765 000024 00000011254 12365763733 015045 0ustar00timjstaff000000 000000 palRvlg - Velocity component in a given direction due to Galactic rotation and motion of the local group
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palRvlg - Velocity component in a given direction due to Galactic rotation and motion of the local group

Description:
This function returns the velocity component in a given direction due to the combination of the rotation of the Galaxy and the motion of the Galaxy relative to the mean motion of the local group. The result is ve when the Sun is receding from the given point on the sky.

Invocation:
double palRvlg( double r2000, double d2000 )

Arguments:

r2000 = double (Given)
J2000.0 mean RA (radians)
d2000 = double (Given)
J2000.0 mean Dec (radians)

Returned Value:

Component of SOLAR motion in direction R2000,D2000 (km/s).

Reference
  • IAU Trans 1976, 168, p201.


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Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node69.html000644 000765 000024 00000013356 12365763733 015053 0ustar00timjstaff000000 000000 palRvlsrd - Velocity component in a given direction due to the Sun's motion with respect to the dynamical Local Standard of Rest
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palRvlsrd - Velocity component in a given direction due to the Sun's motion with respect to the dynamical Local Standard of Rest

Description:
This function returns the velocity component in a given direction due to the Sun's motion with respect to the dynamical Local Standard of Rest. The result is ve when the Sun is receding from the given point on the sky.

Invocation:
double palRvlsrd( double r2000, double d2000 )

Arguments:

r2000 = double (Given)
J2000.0 mean RA (radians)
d2000 = double (Given)
J2000.0 mean Dec (radians)

Returned Value:

Component of "peculiar" solar motion in direction R2000,D2000 (km/s).

Notes:
  • The Local Standard of Rest used here is the "dynamical" LSR, a point in the vicinity of the Sun which is in a circular orbit around the Galactic centre. The Sun's motion with respect to the dynamical LSR is called the "peculiar" solar motion.

  • There is another type of LSR, called a "kinematical" LSR. A kinematical LSR is the mean standard of rest of specified star catalogues or stellar populations, and several slightly different kinematical LSRs are in use. The Sun's motion with respect to an agreed kinematical LSR is known as the "standard" solar motion. To obtain a radial velocity correction with respect to an adopted kinematical LSR use the routine sla_RVLSRK.

Reference
  • Delhaye (1965), in "Stars and Stellar Systems", vol 5, p73.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node7.html000644 000765 000024 00000011363 12365763733 014757 0ustar00timjstaff000000 000000 palAddet - Add the E-terms to a pre IAU 1976 mean place
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palAddet - Add the E-terms to a pre IAU 1976 mean place

Description:
Add the E-terms (elliptic component of annual aberration) to a pre IAU 1976 mean place to conform to the old catalogue convention.

Invocation:
void palAddet ( double rm, double dm, double eq, double rc, double dc );

Arguments:

rm = double (Given)
RA without E-terms (radians)
dm = double (Given)
Dec without E-terms (radians)
eq = double (Given)
Besselian epoch of mean equator and equinox
rc = double (Returned)
RA with E-terms included (radians)
dc = double (Returned)
Dec with E-terms included (radians)

Notes:
Most star positions from pre-1984 optical catalogues (or derived from astrometry using such stars) embody the E-terms. If it is necessary to convert a formal mean place (for example a pulsar timing position) to one consistent with such a star catalogue, then the RA,Dec should be adjusted using this routine.
See Also
Explanatory Supplement to the Astronomical Ephemeris, section 2D, page 48.

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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node70.html000644 000765 000024 00000013224 12365763733 015035 0ustar00timjstaff000000 000000 palRvlsrk - Velocity component in a given direction due to the Sun's motion with respect to an adopted kinematic Local Standard of Rest
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palRvlsrk - Velocity component in a given direction due to the Sun's motion with respect to an adopted kinematic Local Standard of Rest

Description:
This function returns the velocity component in a given direction due to the Sun's motion with respect to an adopted kinematic Local Standard of Rest. The result is ve when the Sun is receding from the given point on the sky.

Invocation:
double palRvlsrk( double r2000, double d2000 )

Arguments:

r2000 = double (Given)
J2000.0 mean RA (radians)
d2000 = double (Given)
J2000.0 mean Dec (radians)

Returned Value:

Component of "standard" solar motion in direction R2000,D2000 (km/s).

Notes:
  • The Local Standard of Rest used here is one of several "kinematical" LSRs in common use. A kinematical LSR is the mean standard of rest of specified star catalogues or stellar populations. The Sun's motion with respect to a kinematical LSR is known as the "standard" solar motion.

  • There is another sort of LSR, the "dynamical" LSR, which is a point in the vicinity of the Sun which is in a circular orbit around the Galactic centre. The Sun's motion with respect to the dynamical LSR is called the "peculiar" solar motion. To obtain a radial velocity correction with respect to the dynamical LSR use the routine sla_RVLSRD.

Reference
  • Delhaye (1965), in "Stars and Stellar Systems", vol 5, p73.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node71.html000644 000765 000024 00000011655 12365763733 015044 0ustar00timjstaff000000 000000 palSubet - Remove the E-terms from a pre IAU 1976 catalogue RA,Dec
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palSubet - Remove the E-terms from a pre IAU 1976 catalogue RA,Dec

Description:
Remove the E-terms (elliptic component of annual aberration) from a pre IAU 1976 catalogue RA,Dec to give a mean place.

Invocation:
void palSubet ( double rc, double dc, double eq, double rm, double dm );

Arguments:

rc = double (Given)
RA with E-terms included (radians)
dc = double (Given)
Dec with E-terms included (radians)
eq = double (Given)
Besselian epoch of mean equator and equinox
rm = double (Returned)
RA without E-terms (radians)
dm = double (Returned)
Dec without E-terms (radians)

Notes:
Most star positions from pre-1984 optical catalogues (or derived from astrometry using such stars) embody the E-terms. This routine converts such a position to a formal mean place (allowing, for example, comparison with a pulsar timing position).
See Also
Explanatory Supplement to the Astronomical Ephemeris, section 2D, page 48.

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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node72.html000644 000765 000024 00000011300 12365763733 015030 0ustar00timjstaff000000 000000 palSupgal - Convert from supergalactic to galactic coordinates
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palSupgal - Convert from supergalactic to galactic coordinates

Description:
Transformation from de Vaucouleurs supergalactic coordinates to IAU 1958 galactic coordinates

Invocation:
void palSupgal ( double dsl, double dsb, double dl, double db );

Arguments:

dsl = double (Given)
Supergalactic longitude.
dsb = double (Given)
Supergalactic latitude.
dl = double (Returned)
Galactic longitude.
db = double (Returned)
Galactic latitude.

See Also
  • de Vaucouleurs, de Vaucouleurs, & Corwin, Second Reference Catalogue of Bright Galaxies, U. Texas, page 8.

  • Systems & Applied Sciences Corp., Documentation for the machine-readable version of the above catalogue, Contract NAS 5-26490.


(These two references give different values for the galactic longitude of the supergalactic origin. Both are wrong; the correct value is L2=137.37.)

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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node73.html000644 000765 000024 00000027077 12365763733 015053 0ustar00timjstaff000000 000000 palUe2el - Universal elements to heliocentric osculating elements
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palUe2el - Universal elements to heliocentric osculating elements

Description:
Transform universal elements into conventional heliocentric osculating elements.

Invocation:
void palUe2el ( const double u[13], int jformr, int jform, double epoch, double orbinc, double anode, double perih, double aorq, double e, double aorl, double dm, int jstat );

Arguments:

u = const double [13] (Given)
Universal orbital elements (Note 1) (0) combined mass (Mm) (1) total energy of the orbit (alpha) (2) reference (osculating) epoch (t0) (3-5) position at reference epoch (r0) (6-8) velocity at reference epoch (v0) (9) heliocentric distance at reference epoch (10) r0.v0 (11) date (t) (12) universal eccentric anomaly (psi) of date, approx
jformr = int (Given)
Requested element set (1-3; Note 3)
jform = int (Returned)
Element set actually returned (1-3; Note 4)
epoch = double (Returned)
Epoch of elements (TT MJD)
orbinc = double (Returned)
inclination (radians)
anode = double (Returned)
longitude of the ascending node (radians)
perih = double (Returned)
longitude or argument of perihelion (radians)
aorq = double (Returned)
mean distance or perihelion distance (AU)
e = double (Returned)
eccentricity
aorl = double (Returned)
mean anomaly or longitude (radians, JFORM=1,2 only)
dm = double (Returned)
daily motion (radians, JFORM=1 only)
jstat = int (Returned)
status: 0 = OK
  • 1 = illegal combined mass

  • 2 = illegal JFORMR

  • 3 = position/velocity out of range


Notes:
  • The "universal" elements are those which define the orbit for the purposes of the method of universal variables (see reference 2). They consist of the combined mass of the two bodies, an epoch, and the position and velocity vectors (arbitrary reference frame) at that epoch. The parameter set used here includes also various quantities that can, in fact, be derived from the other information. This approach is taken to avoiding unnecessary computation and loss of accuracy. The supplementary quantities are (i) alpha, which is proportional to the total energy of the orbit, (ii) the heliocentric distance at epoch, (iii) the outwards component of the velocity at the given epoch, (iv) an estimate of psi, the "universal eccentric anomaly" at a given date and (v) that date.

  • The universal elements are with respect to the mean equator and equinox of epoch J2000. The orbital elements produced are with respect to the J2000 ecliptic and mean equinox.

  • Three different element-format options are supported:


Option JFORM=1, suitable for the major planets:

EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = longitude of perihelion, curly pi (radians) AORQ = mean distance, a (AU) E = eccentricity, e AORL = mean longitude L (radians) DM = daily motion (radians)

Option JFORM=2, suitable for minor planets:

EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = mean distance, a (AU) E = eccentricity, e AORL = mean anomaly M (radians)

Option JFORM=3, suitable for comets:

EPOCH = epoch of perihelion (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = perihelion distance, q (AU) E = eccentricity, e

  • It may not be possible to generate elements in the form requested through JFORMR. The caller is notified of the form of elements actually returned by means of the JFORM argument:


JFORMR JFORM meaning

1 1 OK - elements are in the requested format 1 2 never happens 1 3 orbit not elliptical

2 1 never happens 2 2 OK - elements are in the requested format 2 3 orbit not elliptical

3 1 never happens 3 2 never happens 3 3 OK - elements are in the requested format

  • The arguments returned for each value of JFORM (cf Note 6: JFORM may not be the same as JFORMR) are as follows:


JFORM 1 2 3 EPOCH t0 t0 T ORBINC i i i ANODE Omega Omega Omega PERIH curly pi omega omega AORQ a a q E e e e AORL L M - DM n - -

where:

t0 is the epoch of the elements (MJD, TT) T " epoch of perihelion (MJD, TT) i " inclination (radians) Omega " longitude of the ascending node (radians) curly pi " longitude of perihelion (radians) omega " argument of perihelion (radians) a " mean distance (AU) q " perihelion distance (AU) e " eccentricity L " longitude (radians, 0-2pi) M " mean anomaly (radians, 0-2pi) n " daily motion (radians)

  • means no value is set

  • At very small inclinations, the longitude of the ascending node ANODE becomes indeterminate and under some circumstances may be set arbitrarily to zero. Similarly, if the orbit is close to circular, the true anomaly becomes indeterminate and under some circumstances may be set arbitrarily to zero. In such cases, the other elements are automatically adjusted to compensate, and so the elements remain a valid description of the orbit.


See Also:
  • Sterne, Theodore E., "An Introduction to Celestial Mechanics", Interscience Publishers Inc., 1960. Section 6.7, p199.

  • Everhart, E. & Pitkin, E.T., Am.J.Phys. 51, 712, 1983.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/node74.html000644 000765 000024 00000016363 12365763733 015050 0ustar00timjstaff000000 000000 palUe2pv - Heliocentric position and velocity of a planet, asteroid or comet, from universal elements
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palUe2pv - Heliocentric position and velocity of a planet, asteroid or comet, from universal elements

Description:
Heliocentric position and velocity of a planet, asteroid or comet, starting from orbital elements in the "universal variables" form.

Invocation:
void palUe2pv( double date, double u[13], double pv[6], int jstat );

Arguments:

date = double (Given)
TT Modified Julian date (JD-2400000.5).
u = double [13] (Given & Returned)
Universal orbital elements (updated, see note 1) given (0) combined mass (Mm) " (1) total energy of the orbit (alpha) " (2) reference (osculating) epoch (t0) " (3-5) position at reference epoch (r0) " (6-8) velocity at reference epoch (v0) " (9) heliocentric distance at reference epoch " (10) r0.v0 returned (11) date (t) " (12) universal eccentric anomaly (psi) of date
jstat = int (Returned)
status: 0 = OK
  • 1 = radius vector zero

  • 2 = failed to converge


Notes:
  • The "universal" elements are those which define the orbit for the purposes of the method of universal variables (see reference). They consist of the combined mass of the two bodies, an epoch, and the position and velocity vectors (arbitrary reference frame) at that epoch. The parameter set used here includes also various quantities that can, in fact, be derived from the other information. This approach is taken to avoiding unnecessary computation and loss of accuracy. The supplementary quantities are (i) alpha, which is proportional to the total energy of the orbit, (ii) the heliocentric distance at epoch, (iii) the outwards component of the velocity at the given epoch, (iv) an estimate of psi, the "universal eccentric anomaly" at a given date and (v) that date.

  • The companion routine is palEl2ue. This takes the conventional orbital elements and transforms them into the set of numbers needed by the present routine. A single prediction requires one one call to palEl2ue followed by one call to the present routine; for convenience, the two calls are packaged as the routine sla_PLANEL. Multiple predictions may be made by again calling palEl2ue once, but then calling the present routine multiple times, which is faster than multiple calls to palPlanel.

  • It is not obligatory to use palEl2ue to obtain the parameters. However, it should be noted that because palEl2ue performs its own validation, no checks on the contents of the array U are made by the present routine. in the TT timescale (formerly Ephemeris Time, ET) and is a Modified Julian Date (JD-2400000.5). units (solar masses, AU and canonical days). The position and velocity are not sensitive to the choice of reference frame. The palEl2ue routine in fact produces coordinates with respect to the J2000 equator and equinox.

  • The algorithm was originally adapted from the EPHSLA program of D.H.P.Jones (private communication, 1996). The method is based on Stumpff's Universal Variables.

  • Reference: Everhart, E. & Pitkin, E.T., Am.J.Phys. 51, 712, 1983.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palAirmas - Air mass at given zenith distance

Description:
Calculates the airmass at the observed zenith distance.

Invocation:
double palAirmas( double zd );

Arguments:

zd = double (Given)
Observed zenith distance (radians)

Notes:
  • The "observed" zenith distance referred to above means "as affected by refraction".

  • Uses Hardie's (1962) polynomial fit to Bemporad's data for the relative air mass, X, in units of thickness at the zenith as tabulated by Schoenberg (1929). This is adequate for all normal needs as it is accurate to better than 0.1% up to X = 6.8 and better than 1% up to X = 10. Bemporad's tabulated values are unlikely to be trustworthy to such accuracy because of variations in density, pressure and other conditions in the atmosphere from those assumed in his work.

  • The sign of the ZD is ignored.

  • At zenith distances greater than about ZD = 87 degrees the air mass is held constant to avoid arithmetic overflows.

See Also
  • Hardie, R.H., 1962, in "Astronomical Techniques" ed. W.A. Hiltner, University of Chicago Press, p180.

  • Schoenberg, E., 1929, Hdb. d. Ap., Berlin, Julius Springer, 2, 268.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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palAmp - Convert star RA,Dec from geocentric apparaent to mean place

Description:
Convert star RA,Dec from geocentric apparent to mean place. The mean coordinate system is close to ICRS. See palAmpqk for details.

Invocation:
void palAmp ( double ra, double da, double date, double eq, double rm, double dm );

Arguments:

ra = double (Given)
Apparent RA (radians)
dec = double (Given)
Apparent Dec (radians)
date = double (Given)
TDB for apparent place (JD-2400000.5)
eq = double (Given)
Equinox: Julian epoch of mean place.
rm = double (Returned)
Mean RA (radians)
dm = double (Returned)
Mean Dec (radians)

Notes:
  • See palMappa and palAmpqk for details.


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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
sun267.htx/prev.png000644 000765 000024 00000000427 12365763733 014536 0ustar00timjstaff000000 000000 ‰PNG  IHDR?GŸýT PLTE¿¿¿oooççç[Íã¹tRNS@æØf¹IDATxœ…= Ã0 …_pF—Dà5àK¤÷ t têÞ¡Cñ)éèät-´ªÓ}ñüYÒ#% À¡Æ4”ÒÍ¥d/Çùªåvµë`3 v3tâE$ Sãà™ù£ç°5•ªs}jßf/‹¹šÀŒˆˆ”hQ!žÜäÛ•=KV_³ªN8âK›Àþ8’!û™)Š‚x'‡Éë‘ÒȸÙD˜ˆ¹^Kù ê-êŸþsNH¼!%³IEND®B`‚sun267.htx/prev_g.png000644 000765 000024 00000000507 12365763733 015043 0ustar00timjstaff000000 000000 ‰PNG  IHDR?šJtRNS¿-Mc%IDATxœÍ”ÁuÄ D?~´5ým9î`ÓD:p9€cÇäm.™ÂBBb$9d¾b`Hí¨ž°UI:Bu:±éΓE»-'ƒ}› Øã²ØC|,¤÷tÇ%ì„}yF²sP©ª=šT¯’„¨Â.¢+—9döGƒ+WZ­~paòâÛnP8ðã9ÔâÔ5îil u9ä'»öͩβ ý²‘ÁÖ’á_¼ÿ¹+þxež ôŒUþ+Ôi„Îÿþ@i’ZfG-Κ6)nsU~!ÃL,À’cšˆÔwámP,ßv®zSßñ§Hµ¹Ë=hy™êW:þCý>Gæõ'ÿoå²i=Q)ÂIEND®B`‚sun267.htx/section0.tex000644 000765 000024 00000000727 12365763500 015315 0ustar00timjstaff000000 000000 \section{Introduction} This library provides a C library designed as a API-compatible replacement for the C SLALIB library (SUN/67) and uses a GPL licence so is freely redistributable. Where possible the functions call equivalent SOFA routines (Hohenkerk, C., 2011, Scholarpedia, \textbf{6}, \emph{11404}) and use current IAU 2006 standards. This means that any functions that rely on nutation or precession will return slightly different answers to the SLA functions. sun267.htx/section1.tex000644 000765 000024 00000000507 12365763500 015312 0ustar00timjstaff000000 000000 \section{Citing PAL} If you use PAL in your work please consider citing it. The description paper for PAL is: \emph{PAL: A Positional Astronomy Library}, Jenness, T. \& Berry, D. S., in \emph{Astronomoical Data Anaysis Software and Systems XXII}, Friedel, D. N. (ed), ASP Conf.\ Ser. \textbf{475}, p307. \clearpage \appendix sun267.htx/section10.tex000644 000765 000024 00000007544 12365763500 015402 0ustar00timjstaff000000 000000 \sstroutine{ palDafin }{ Sexagesimal character string to angle }{ \sstdescription{ Extracts an angle from a sexagesimal string with degrees, arcmin, arcsec fields using space or comma delimiters. } \sstinvocation{ void palDafin ( const char $*$string, int $*$ipos, double $*$a, int $*$j ); } \sstarguments{ \sstsubsection{ string = const char $*$ (Given) }{ String containing deg, arcmin, arcsec fields } \sstsubsection{ ipos = int $*$ (Given \& Returned) }{ Position to start decoding {\tt "}string{\tt "}. First character is position 1 for compatibility with SLA. After calling this routine {\tt "}iptr{\tt "} will be positioned after the sexagesimal string. } \sstsubsection{ a = double $*$ (Returned) }{ Angle in radians. } \sstsubsection{ j = int $*$ (Returned) }{ status: 0 = OK $+$1 = default, A unchanged \sstitemlist{ \sstitem 1 = bad degrees ) \sstitem 2 = bad arcminutes ) (note 3) \sstitem 3 = bad arcseconds ) } } } \sstnotes{ \sstitemlist{ \sstitem The first three {\tt "}fields{\tt "} in STRING are degrees, arcminutes, arcseconds, separated by spaces or commas. The degrees field may be signed, but not the others. The decoding is carried out by the palDfltin routine and is free-format. \sstitem Successive fields may be absent, defaulting to zero. For zero status, the only combinations allowed are degrees alone, degrees and arcminutes, and all three fields present. If all three fields are omitted, a status of $+$1 is returned and A is unchanged. In all other cases A is changed. \sstitem Range checking: } The degrees field is not range checked. However, it is expected to be integral unless the other two fields are absent. The arcminutes field is expected to be 0-59, and integral if the arcseconds field is present. If the arcseconds field is absent, the arcminutes is expected to be 0-59.9999... The arcseconds field is expected to be 0-59.9999... \sstitemlist{ \sstitem Decoding continues even when a check has failed. Under these circumstances the field takes the supplied value, defaulting to zero, and the result A is computed and returned. \sstitem Further fields after the three expected ones are not treated as an error. The pointer IPOS is left in the correct state for further decoding with the present routine or with palDfltin etc. See the example, above. \sstitem If STRING contains hours, minutes, seconds instead of degrees etc, or if the required units are turns (or days) instead of radians, the result A should be multiplied as follows: } for to obtain multiply STRING A in A by d {\tt '} {\tt "} radians 1 = 1.0 d {\tt '} {\tt "} turns 1/2pi = 0.1591549430918953358 h m s radians 15 = 15.0 h m s days 15/2pi = 2.3873241463784300365 } \sstdiytopic{ Example }{ argument before after STRING {\tt '}-57 17 44.806 12 34 56.7{\tt '} unchanged IPTR 1 16 (points to 12...) A ? -1.00000D0 J ? 0 } } sun267.htx/section11.tex000644 000765 000024 00000004431 12365763500 015373 0ustar00timjstaff000000 000000 \sstroutine{ palDe2h }{ Equatorial to horizon coordinates: HA,Dec to Az,E }{ \sstdescription{ Convert equatorial to horizon coordinates. } \sstinvocation{ palDe2h( double ha, double dec, double phi, double $*$ az, double $*$ el ); } \sstarguments{ \sstsubsection{ ha = double $*$ (Given) }{ Hour angle (radians) } \sstsubsection{ dec = double $*$ (Given) }{ Declination (radians) } \sstsubsection{ phi = double (Given) }{ Observatory latitude (radians) } \sstsubsection{ az = double $*$ (Returned) }{ Azimuth (radians) } \sstsubsection{ el = double $*$ (Returned) }{ Elevation (radians) } } \sstnotes{ \sstitemlist{ \sstitem All the arguments are angles in radians. \sstitem Azimuth is returned in the range 0-2pi; north is zero, and east is $+$pi/2. Elevation is returned in the range $+$/-pi/2. \sstitem The latitude must be geodetic. In critical applications, corrections for polar motion should be applied. \sstitem In some applications it will be important to specify the correct type of hour angle and declination in order to produce the required type of azimuth and elevation. In particular, it may be important to distinguish between elevation as affected by refraction, which would require the {\tt "}observed{\tt "} HA,Dec, and the elevation in vacuo, which would require the {\tt "}topocentric{\tt "} HA,Dec. If the effects of diurnal aberration can be neglected, the {\tt "}apparent{\tt "} HA,Dec may be used instead of the topocentric HA,Dec. \sstitem No range checking of arguments is carried out. \sstitem In applications which involve many such calculations, rather than calling the present routine it will be more efficient to use inline code, having previously computed fixed terms such as sine and cosine of latitude, and (for tracking a star) sine and cosine of declination. } } } sun267.htx/section12.tex000644 000765 000024 00000004015 12365763500 015372 0ustar00timjstaff000000 000000 \sstroutine{ palDeuler }{ Form a rotation matrix from the Euler angles }{ \sstdescription{ A rotation is positive when the reference frame rotates anticlockwise as seen looking towards the origin from the positive region of the specified axis. The characters of ORDER define which axes the three successive rotations are about. A typical value is {\tt '}ZXZ{\tt '}, indicating that RMAT is to become the direction cosine matrix corresponding to rotations of the reference frame through PHI radians about the old Z-axis, followed by THETA radians about the resulting X-axis, then PSI radians about the resulting Z-axis. The axis names can be any of the following, in any order or combination: X, Y, Z, uppercase or lowercase, 1, 2, 3. Normal axis labelling/numbering conventions apply; the xyz (=123) triad is right-handed. Thus, the {\tt '}ZXZ{\tt '} example given above could be written {\tt '}zxz{\tt '} or {\tt '}313{\tt '} (or even {\tt '}ZxZ{\tt '} or {\tt '}3xZ{\tt '}). ORDER is terminated by length or by the first unrecognized character. Fewer than three rotations are acceptable, in which case the later angle arguments are ignored. If all rotations are zero, the identity matrix is produced. } \sstinvocation{ void palDeuler ( const char $*$order, double phi, double theta, double psi, double rmat[3][3] ); } \sstarguments{ \sstsubsection{ order = const char[] (Given) }{ Specifies about which axes the rotation occurs } \sstsubsection{ phi = double (Given) }{ 1st rotation (radians) } \sstsubsection{ theta = double (Given) }{ 2nd rotation (radians) } \sstsubsection{ psi = double (Given) }{ 3rd rotation (radians) } \sstsubsection{ rmat = double[3][3] (Given \& Returned) }{ Rotation matrix } } } sun267.htx/section13.tex000644 000765 000024 00000004237 12365763500 015401 0ustar00timjstaff000000 000000 \sstroutine{ palDfltin }{ Convert free-format input into double precision floating point }{ \sstdescription{ Extracts a number from an input string starting at the specified index. } \sstinvocation{ void palDfltin( const char $*$ string, int $*$nstrt, double $*$dreslt, int $*$jflag ); } \sstarguments{ \sstsubsection{ string = const char $*$ (Given) }{ String containing number to be decoded. } \sstsubsection{ nstrt = int $*$ (Given and Returned) }{ Character number indicating where decoding should start. On output its value is updated to be the location of the possible next value. For compatibility with SLA the first character is index 1. } \sstsubsection{ dreslt = double $*$ (Returned) }{ Result. Not updated when jflag=1. } \sstsubsection{ jflag = int $*$ (Returned) }{ status: -1 = -OK, 0 = $+$OK, 1 = null, 2 = error } } \sstnotes{ \sstitemlist{ \sstitem Uses the strtod() system call to do the parsing. This may lead to subtle differences when compared to the SLA/F parsing. \sstitem All {\tt "}D{\tt "} characters are converted to {\tt "}E{\tt "} to handle fortran exponents. \sstitem Commas are recognized as a special case and are skipped if one happens to be the next character when updating nstrt. Additionally the output nstrt position will skip past any trailing space. \sstitem If no number can be found flag will be set to 1. \sstitem If the number overflows or underflows jflag will be set to 2. For overflow the returned result will have the value HUGE\_VAL, for underflow it will have the value 0.0. \sstitem For compatiblity with SLA/F -0 will be returned as {\tt "}0{\tt "} with jflag == -1. \sstitem Unlike slaDfltin a standalone {\tt "}E{\tt "} will return status 1 (could not find a number) rather than 2 (bad number). } } } sun267.htx/section14.tex000644 000765 000024 00000004330 12365763500 015374 0ustar00timjstaff000000 000000 \sstroutine{ palDh2e }{ Horizon to equatorial coordinates: Az,El to HA,Dec }{ \sstdescription{ Convert horizon to equatorial coordinates. } \sstinvocation{ palDh2e( double az, double el, double phi, double $*$ ha, double $*$ dec ); } \sstarguments{ \sstsubsection{ az = double (Given) }{ Azimuth (radians) } \sstsubsection{ el = double (Given) }{ Elevation (radians) } \sstsubsection{ phi = double (Given) }{ Observatory latitude (radians) } \sstsubsection{ ha = double $*$ (Returned) }{ Hour angle (radians) } \sstsubsection{ dec = double $*$ (Returned) }{ Declination (radians) } } \sstnotes{ \sstitemlist{ \sstitem All the arguments are angles in radians. \sstitem The sign convention for azimuth is north zero, east $+$pi/2. \sstitem HA is returned in the range $+$/-pi. Declination is returned in the range $+$/-pi/2. \sstitem The latitude is (in principle) geodetic. In critical applications, corrections for polar motion should be applied. \sstitem In some applications it will be important to specify the correct type of elevation in order to produce the required type of HA,Dec. In particular, it may be important to distinguish between the elevation as affected by refraction, which will yield the {\tt "}observed{\tt "} HA,Dec, and the elevation in vacuo, which will yield the {\tt "}topocentric{\tt "} HA,Dec. If the effects of diurnal aberration can be neglected, the topocentric HA,Dec may be used as an approximation to the {\tt "}apparent{\tt "} HA,Dec. \sstitem No range checking of arguments is done. \sstitem In applications which involve many such calculations, rather than calling the present routine it will be more efficient to use inline code, having previously computed fixed terms such as sine and cosine of latitude. } } } sun267.htx/section15.tex000644 000765 000024 00000001762 12365763500 015403 0ustar00timjstaff000000 000000 \sstroutine{ palDjcal }{ Modified Julian Date to Gregorian Calendar }{ \sstdescription{ Modified Julian Date to Gregorian Calendar, expressed in a form convenient for formatting messages (namely rounded to a specified precision, and with the fields stored in a single array) } \sstinvocation{ void palDjcal ( int ndp, double djm, int iymdf[4], int $*$j ); } \sstarguments{ \sstsubsection{ ndp = int (Given) }{ Number of decimal places of days in fraction. } \sstsubsection{ djm = double (Given) }{ Modified Julian Date (JD-2400000.5) } \sstsubsection{ iymdf[4] = int[] (Returned) }{ Year, month, day, fraction in Gregorian calendar. } \sstsubsection{ j = status (Returned) }{ 0 = OK. See iauJd2cal for other values. } } \sstnotes{ \sstitemlist{ \sstitem Uses iauJd2cal } } } sun267.htx/section16.tex000644 000765 000024 00000003400 12365763500 015373 0ustar00timjstaff000000 000000 \sstroutine{ palDmat }{ Matrix inversion \& solution of simultaneous equations }{ \sstdescription{ Matrix inversion \& solution of simultaneous equations For the set of n simultaneous equations in n unknowns: A.Y = X this routine calculates the inverse of A, the determinant of matrix A and the vector of N unknowns. } \sstinvocation{ void palDmat( int n, double $*$a, double $*$y, double $*$d, int $*$jf, int $*$iw ); } \sstarguments{ \sstsubsection{ n = int (Given) }{ Number of simultaneous equations and number of unknowns. } \sstsubsection{ a = double[] (Given \& Returned) }{ A non-singular NxN matrix (implemented as a contiguous block of memory). After calling this routine {\tt "}a{\tt "} contains the inverse of the matrix. } \sstsubsection{ y = double[] (Given \& Returned) }{ The vector of N unknowns. On exit this vector contains the N solutions. } \sstsubsection{ d = double $*$ (Returned) }{ The determinant. } \sstsubsection{ jf = int $*$ (Returned) }{ The singularity flag. If the matrix is non-singular, jf=0 is returned. If the matrix is singular, jf=-1 \& d=0.0 are returned. In the latter case, the contents of array {\tt "}a{\tt "} on return are undefined. } } \sstnotes{ \sstitemlist{ \sstitem Implemented using Gaussian elimination with partial pivoting. \sstitem Optimized for speed rather than accuracy with errors 1 to 4 times those of routines optimized for accuracy. } } } sun267.htx/section17.tex000644 000765 000024 00000002734 12365763500 015405 0ustar00timjstaff000000 000000 \sstroutine{ palDs2tp }{ Spherical to tangent plane projection }{ \sstdescription{ Projection of spherical coordinates onto tangent plane: {\tt "}gnomonic{\tt "} projection - {\tt "}standard coordinates{\tt "} } \sstinvocation{ palDs2tp( double ra, double dec, double raz, double decz, double $*$xi, double $*$eta, int $*$j ); } \sstarguments{ \sstsubsection{ ra = double (Given) }{ RA spherical coordinate of point to be projected (radians) } \sstsubsection{ dec = double (Given) }{ Dec spherical coordinate of point to be projected (radians) } \sstsubsection{ raz = double (Given) }{ RA spherical coordinate of tangent point (radians) } \sstsubsection{ decz = double (Given) }{ Dec spherical coordinate of tangent point (radians) } \sstsubsection{ xi = double $*$ (Returned) }{ First rectangular coordinate on tangent plane (radians) } \sstsubsection{ eta = double $*$ (Returned) }{ Second rectangular coordinate on tangent plane (radians) } \sstsubsection{ j = int $*$ (Returned) }{ status: 0 = OK, star on tangent plane 1 = error, star too far from axis 2 = error, antistar on tangent plane 3 = error, antistar too far from axis } } } sun267.htx/section18.tex000644 000765 000024 00000002333 12365763500 015401 0ustar00timjstaff000000 000000 \sstroutine{ palDtt }{ Return offset between UTC and TT }{ \sstdescription{ Increment to be applied to Coordinated Universal Time UTC to give International Atomic Time (TAI). } \sstinvocation{ dat = palDat( double utc ); } \sstarguments{ \sstsubsection{ utc = double (Given) }{ UTC date as a modified JD (JD-2400000.5) } } \sstreturnedvalue{ \sstsubsection{ dat = double }{ TAI-UTC in seconds } } \sstnotes{ \sstitemlist{ \sstitem This routine converts the MJD argument to calendar date before calling the SOFA iauDat function. \sstitem This routine matches the slaDat interface which differs from the iauDat interface. Consider coding directly to the SOFA interface. \sstitem See iauDat for a description of error conditions when calling this function with a time outside of the UTC range. \sstitem The status argument from iauDat is ignored. This is reasonable since the error codes are mainly related to incorrect calendar dates when calculating the JD internally. } } } sun267.htx/section19.tex000644 000765 000024 00000003760 12365763500 015407 0ustar00timjstaff000000 000000 \sstroutine{ palDmoon }{ Approximate geocentric position and velocity of the Moon }{ \sstdescription{ Calculate the approximate geocentric position of the Moon using a full implementation of the algorithm published by Meeus (l{\tt '}Astronomie, June 1984, p348). } \sstinvocation{ void palDmoon( double date, double pv[6] ); } \sstarguments{ \sstsubsection{ date = double (Given) }{ TDB as a Modified Julian Date (JD-2400000.5) } \sstsubsection{ pv = double [6] (Returned) }{ Moon x,y,z,xdot,ydot,zdot, mean equator and equinox of date (AU, AU/s) } } \sstnotes{ \sstitemlist{ \sstitem Meeus quotes accuracies of 10 arcsec in longitude, 3 arcsec in latitude and 0.2 arcsec in HP (equivalent to about 20 km in distance). Comparison with JPL DE200 over the interval 1960-2025 gives RMS errors of 3.7 arcsec and 83 mas/hour in longitude, 2.3 arcsec and 48 mas/hour in latitude, 11 km and 81 mm/s in distance. The maximum errors over the same interval are 18 arcsec and 0.50 arcsec/hour in longitude, 11 arcsec and 0.24 arcsec/hour in latitude, 40 km and 0.29 m/s in distance. \sstitem The original algorithm is expressed in terms of the obsolete timescale Ephemeris Time. Either TDB or TT can be used, but not UT without incurring significant errors (30 arcsec at the present time) due to the Moon{\tt '}s 0.5 arcsec/sec movement. \sstitem The algorithm is based on pre IAU 1976 standards. However, the result has been moved onto the new (FK5) equinox, an adjustment which is in any case much smaller than the intrinsic accuracy of the procedure. \sstitem Velocity is obtained by a complete analytical differentiation of the Meeus model. } } } sun267.htx/section2.tex000644 000765 000024 00000000061 12365763500 015306 0ustar00timjstaff000000 000000 \section{\label{APP:SPEC}Function Descriptions} sun267.htx/section20.tex000644 000765 000024 00000000712 12365763500 015371 0ustar00timjstaff000000 000000 \sstroutine{ palDrange }{ Normalize angle into range $+$/- pi }{ \sstdescription{ The result is {\tt "}angle{\tt "} expressed in the range $+$/- pi. If the supplied value for {\tt "}angle{\tt "} is equal to $+$/- pi, it is returned unchanged. } \sstinvocation{ palDrange( double angle ) } \sstarguments{ \sstsubsection{ angle = double (Given) }{ The angle in radians. } } } sun267.htx/section21.tex000644 000765 000024 00000003746 12365763500 015404 0ustar00timjstaff000000 000000 \sstroutine{ palDt }{ Estimate the offset between dynamical time and UT }{ \sstdescription{ Estimate the offset between dynamical time and Universal Time for a given historical epoch. } \sstinvocation{ double palDt( double epoch ); } \sstarguments{ \sstsubsection{ epoch = double (Given) }{ Julian epoch (e.g. 1850.0) } } \sstreturnedvalue{ \sstsubsection{ palDt = double }{ Rough estimate of ET-UT (after 1984, TT-UT) at the given epoch, in seconds. } } \sstnotes{ \sstitemlist{ \sstitem Depending on the epoch, one of three parabolic approximations is used: } before 979 Stephenson \& Morrison{\tt '}s 390 BC to AD 948 model 979 to 1708 Stephenson \& Morrison{\tt '}s 948 to 1600 model after 1708 McCarthy \& Babcock{\tt '}s post-1650 model The breakpoints are chosen to ensure continuity: they occur at places where the adjacent models give the same answer as each other. \sstitemlist{ \sstitem The accuracy is modest, with errors of up to 20 sec during the interval since 1650, rising to perhaps 30 min by 1000 BC. Comparatively accurate values from AD 1600 are tabulated in the Astronomical Almanac (see section K8 of the 1995 AA). \sstitem The use of double-precision for both argument and result is purely for compatibility with other SLALIB time routines. \sstitem The models used are based on a lunar tidal acceleration value of -26.00 arcsec per century. } } \sstdiytopic{ See Also }{ Explanatory Supplement to the Astronomical Almanac, ed P.K.Seidelmann, University Science Books (1992), section 2.553, p83. This contains references to the Stephenson \& Morrison and McCarthy \& Babcock papers. } } sun267.htx/section22.tex000644 000765 000024 00000002153 12365763500 015374 0ustar00timjstaff000000 000000 \sstroutine{ palDtp2s }{ Tangent plane to spherical coordinates }{ \sstdescription{ Transform tangent plane coordinates into spherical. } \sstinvocation{ palDtp2s( double xi, double eta, double raz, double decz, double $*$ra, double $*$dec); } \sstarguments{ \sstsubsection{ xi = double (Given) }{ First rectangular coordinate on tangent plane (radians) } \sstsubsection{ eta = double (Given) }{ Second rectangular coordinate on tangent plane (radians) } \sstsubsection{ raz = double (Given) }{ RA spherical coordinate of tangent point (radians) } \sstsubsection{ decz = double (Given) }{ Dec spherical coordinate of tangent point (radians) } \sstsubsection{ ra = double $*$ (Returned) }{ RA spherical coordinate of point to be projected (radians) } \sstsubsection{ dec = double $*$ (Returned) }{ Dec spherical coordinate of point to be projected (radians) } } } sun267.htx/section23.tex000644 000765 000024 00000005773 12365763500 015410 0ustar00timjstaff000000 000000 \sstroutine{ palDtps2c }{ Determine RA,Dec of tangent point from coordinates }{ \sstdescription{ From the tangent plane coordinates of a star of known RA,Dec, determine the RA,Dec of the tangent point. } \sstinvocation{ palDtps2c( double xi, double eta, double ra, double dec, double $*$ raz1, double decz1, double $*$ raz2, double decz2, int $*$n); } \sstarguments{ \sstsubsection{ xi = double (Given) }{ First rectangular coordinate on tangent plane (radians) } \sstsubsection{ eta = double (Given) }{ Second rectangular coordinate on tangent plane (radians) } \sstsubsection{ ra = double (Given) }{ RA spherical coordinate of star (radians) } \sstsubsection{ dec = double (Given) }{ Dec spherical coordinate of star (radians) } \sstsubsection{ raz1 = double $*$ (Returned) }{ RA spherical coordinate of tangent point, solution 1 (radians) } \sstsubsection{ decz1 = double $*$ (Returned) }{ Dec spherical coordinate of tangent point, solution 1 (radians) } \sstsubsection{ raz2 = double $*$ (Returned) }{ RA spherical coordinate of tangent point, solution 2 (radians) } \sstsubsection{ decz2 = double $*$ (Returned) }{ Dec spherical coordinate of tangent point, solution 2 (radians) } \sstsubsection{ n = int $*$ (Returned) }{ number of solutions: 0 = no solutions returned (note 2) 1 = only the first solution is useful (note 3) 2 = both solutions are useful (note 3) } } \sstnotes{ \sstitemlist{ \sstitem The RAZ1 and RAZ2 values are returned in the range 0-2pi. \sstitem Cases where there is no solution can only arise near the poles. For example, it is clearly impossible for a star at the pole itself to have a non-zero XI value, and hence it is meaningless to ask where the tangent point would have to be to bring about this combination of XI and DEC. \sstitem Also near the poles, cases can arise where there are two useful solutions. The argument N indicates whether the second of the two solutions returned is useful. N=1 indicates only one useful solution, the usual case; under these circumstances, the second solution corresponds to the {\tt "}over-the-pole{\tt "} case, and this is reflected in the values of RAZ2 and DECZ2 which are returned. \sstitem The DECZ1 and DECZ2 values are returned in the range $+$/-pi, but in the usual, non-pole-crossing, case, the range is $+$/-pi/2. \sstitem This routine is the spherical equivalent of the routine sla\_DTPV2C. } } } sun267.htx/section24.tex000644 000765 000024 00000001662 12365763500 015402 0ustar00timjstaff000000 000000 \sstroutine{ palDtt }{ Return offset between UTC and TT }{ \sstdescription{ Increment to be applied to Coordinated Universal Time UTC to give Terrestrial Time TT (formerly Ephemeris Time ET) } \sstinvocation{ dtt = palDtt( double utc ); } \sstarguments{ \sstsubsection{ utc = double (Given) }{ UTC date as a modified JD (JD-2400000.5) } } \sstreturnedvalue{ \sstsubsection{ dtt = double }{ TT-UTC in seconds } } \sstnotes{ \sstitemlist{ \sstitem Consider a comprehensive upgrade to use the time transformations in SOFA{\tt '}s time cookbook: http://www.iausofa.org/sofa\_ts\_c.pdf. \sstitem See iauDat for a description of error conditions when calling this function with a time outside of the UTC range. This behaviour differs from slaDtt. } } } sun267.htx/section25.tex000644 000765 000024 00000001413 12365763500 015375 0ustar00timjstaff000000 000000 \sstroutine{ palEcmat }{ Form the equatorial to ecliptic rotation matrix - IAU 2006 precession model }{ \sstdescription{ The equatorial to ecliptic rotation matrix is found and returned. The matrix is in the sense V(ecl) = RMAT $*$ V(equ); the equator, equinox and ecliptic are mean of date. } \sstinvocation{ palEcmat( double date, double rmat[3][3] ) } \sstarguments{ \sstsubsection{ date = double (Given) }{ TT as Modified Julian Date (JD-2400000.5). The difference between TT and TDB is of the order of a millisecond or two (i.e. about 0.02 arc-seconds). } \sstsubsection{ rmat = double[3][3] (Returned) }{ Rotation matrix } } } sun267.htx/section26.tex000644 000765 000024 00000014764 12365763500 015413 0ustar00timjstaff000000 000000 \sstroutine{ palEl2ue }{ Transform conventional elements into {\tt "}universal{\tt "} form }{ \sstdescription{ Transform conventional osculating elements into {\tt "}universal{\tt "} form. } \sstinvocation{ void palEl2ue ( double date, int jform, double epoch, double orbinc, double anode, double perih, double aorq, double e, double aorl, double dm, double u[13], int $*$jstat ); } \sstarguments{ \sstsubsection{ date = double (Given) }{ Epoch (TT MJD) of osculation (Note 3) } \sstsubsection{ jform = int (Given) }{ Element set actually returned (1-3; Note 6) } \sstsubsection{ epoch = double (Given) }{ Epoch of elements (TT MJD) } \sstsubsection{ orbinc = double (Given) }{ inclination (radians) } \sstsubsection{ anode = double (Given) }{ longitude of the ascending node (radians) } \sstsubsection{ perih = double (Given) }{ longitude or argument of perihelion (radians) } \sstsubsection{ aorq = double (Given) }{ mean distance or perihelion distance (AU) } \sstsubsection{ e = double (Given) }{ eccentricity } \sstsubsection{ aorl = double (Given) }{ mean anomaly or longitude (radians, JFORM=1,2 only) } \sstsubsection{ dm = double (Given) }{ daily motion (radians, JFORM=1 only) } \sstsubsection{ u = double [13] (Returned) }{ Universal orbital elements (Note 1) (0) combined mass (M$+$m) (1) total energy of the orbit (alpha) (2) reference (osculating) epoch (t0) (3-5) position at reference epoch (r0) (6-8) velocity at reference epoch (v0) (9) heliocentric distance at reference epoch (10) r0.v0 (11) date (t) (12) universal eccentric anomaly (psi) of date, approx } \sstsubsection{ jstat = int $*$ (Returned) }{ status: 0 = OK \sstitemlist{ \sstitem 1 = illegal JFORM \sstitem 2 = illegal E \sstitem 3 = illegal AORQ \sstitem 4 = illegal DM \sstitem 5 = numerical error } } } \sstnotes{ \sstitemlist{ \sstitem The {\tt "}universal{\tt "} elements are those which define the orbit for the purposes of the method of universal variables (see reference). They consist of the combined mass of the two bodies, an epoch, and the position and velocity vectors (arbitrary reference frame) at that epoch. The parameter set used here includes also various quantities that can, in fact, be derived from the other information. This approach is taken to avoiding unnecessary computation and loss of accuracy. The supplementary quantities are (i) alpha, which is proportional to the total energy of the orbit, (ii) the heliocentric distance at epoch, (iii) the outwards component of the velocity at the given epoch, (iv) an estimate of psi, the {\tt "}universal eccentric anomaly{\tt "} at a given date and (v) that date. \sstitem The companion routine is palUe2pv. This takes the set of numbers that the present routine outputs and uses them to derive the object{\tt '}s position and velocity. A single prediction requires one call to the present routine followed by one call to palUe2pv; for convenience, the two calls are packaged as the routine palPlanel. Multiple predictions may be made by again calling the present routine once, but then calling palUe2pv multiple times, which is faster than multiple calls to palPlanel. \sstitem DATE is the epoch of osculation. It is in the TT timescale (formerly Ephemeris Time, ET) and is a Modified Julian Date (JD-2400000.5). \sstitem The supplied orbital elements are with respect to the J2000 ecliptic and equinox. The position and velocity parameters returned in the array U are with respect to the mean equator and equinox of epoch J2000, and are for the perihelion prior to the specified epoch. \sstitem The universal elements returned in the array U are in canonical units (solar masses, AU and canonical days). \sstitem Three different element-format options are available: } Option JFORM=1, suitable for the major planets: EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = longitude of perihelion, curly pi (radians) AORQ = mean distance, a (AU) E = eccentricity, e (range 0 to $<$1) AORL = mean longitude L (radians) DM = daily motion (radians) Option JFORM=2, suitable for minor planets: EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = mean distance, a (AU) E = eccentricity, e (range 0 to $<$1) AORL = mean anomaly M (radians) Option JFORM=3, suitable for comets: EPOCH = epoch of perihelion (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = perihelion distance, q (AU) E = eccentricity, e (range 0 to 10) \sstitemlist{ \sstitem Unused elements (DM for JFORM=2, AORL and DM for JFORM=3) are not accessed. \sstitem The algorithm was originally adapted from the EPHSLA program of D.H.P.Jones (private communication, 1996). The method is based on Stumpff{\tt '}s Universal Variables. } } \sstdiytopic{ See Also }{ Everhart \& Pitkin, Am.J.Phys. 51, 712 (1983). } } sun267.htx/section27.tex000644 000765 000024 00000002471 12365763500 015404 0ustar00timjstaff000000 000000 \sstroutine{ palEpco }{ Convert an epoch into the appropriate form - {\tt '}B{\tt '} or {\tt '}J{\tt '} }{ \sstdescription{ Converts a Besselian or Julian epoch to a Julian or Besselian epoch. } \sstinvocation{ double palEpco( char k0, char k, double e ); } \sstarguments{ \sstsubsection{ k0 = char (Given) }{ Form of result: {\tt '}B{\tt '}=Besselian, {\tt '}J{\tt '}=Julian } \sstsubsection{ k = char (Given) }{ Form of given epoch: {\tt '}B{\tt '} or {\tt '}J{\tt '}. } } \sstnotes{ \sstitemlist{ \sstitem The result is always either equal to or very close to the given epoch E. The routine is required only in applications where punctilious treatment of heterogeneous mixtures of star positions is necessary. \sstitem k and k0 are case insensitive. This differes slightly from the Fortran SLA implementation. \sstitem k and k0 are not validated. They are interpreted as follows: o If k0 and k are the same the result is e o If k0 is {\tt '}b{\tt '} or {\tt '}B{\tt '} and k isn{\tt '}t the conversion is J to B. o In all other cases, the conversion is B to J. } } } sun267.htx/section28.tex000644 000765 000024 00000002251 12365763500 015401 0ustar00timjstaff000000 000000 \sstroutine{ palEpv }{ Earth position and velocity with respect to the BCRS }{ \sstdescription{ Earth position and velocity, heliocentric and barycentric, with respect to the Barycentric Celestial Reference System. } \sstinvocation{ void palEpv( double date, double ph[3], double vh[3], double pb[3], double vb[3] ); } \sstarguments{ \sstsubsection{ date = double (Given) }{ Date, TDB Modified Julian Date (JD-2400000.5) } \sstsubsection{ ph = double [3] (Returned) }{ Heliocentric Earth position (AU) } \sstsubsection{ vh = double [3] (Returned) }{ Heliocentric Earth velocity (AU/day) } \sstsubsection{ pb = double [3] (Returned) }{ Barycentric Earth position (AU) } \sstsubsection{ vb = double [3] (Returned) }{ Barycentric Earth velocity (AU/day) } } \sstnotes{ \sstitemlist{ \sstitem See iauEpv00 for details on accuracy \sstitem Note that the status argument from iauEpv00 is ignored } } } sun267.htx/section29.tex000644 000765 000024 00000001745 12365763500 015411 0ustar00timjstaff000000 000000 \sstroutine{ palEtrms }{ Compute the E-terms vector }{ \sstdescription{ Computes the E-terms (elliptic component of annual aberration) vector. Note the use of the J2000 aberration constant (20.49552 arcsec). This is a reflection of the fact that the E-terms embodied in existing star catalogues were computed from a variety of aberration constants. Rather than adopting one of the old constants the latest value is used here. } \sstinvocation{ void palEtrms ( double ep, double ev[3] ); } \sstarguments{ \sstsubsection{ ep = double (Given) }{ Besselian epoch } \sstsubsection{ ev = double [3] (Returned) }{ E-terms as (dx,dy,dz) } } \sstdiytopic{ See also }{ \sstitemlist{ \sstitem Smith, C.A. et al., 1989. Astr.J. 97, 265. \sstitem Yallop, B.D. et al., 1989. Astr.J. 97, 274. } } } sun267.htx/section3.tex000644 000765 000024 00000003056 12365763500 015316 0ustar00timjstaff000000 000000 \subsection{SOFA Mappings} The following table lists PAL/SLA functions that have direct replacements in SOFA. Whilst these routines are implemented in the PAL library using SOFA new code should probably call SOFA directly. \begin{tabular}{ll} SLA/PAL & SOFA \\ \texttt{palCldj} & \texttt{iauCal2jd} \\ \texttt{palDbear} & \texttt{iauPas} \\ \texttt{palDaf2r} & \texttt{iauAf2a} \\ \texttt{palDav2m} & \texttt{iauRv2m} \\ \texttt{palDcc2s} & \texttt{iauC2s} \\ \texttt{palDcs2c} & \texttt{iauS2c} \\ \texttt{palDd2tf} & \texttt{iauD2tf}\\ \texttt{palDimxv} & \texttt{iauTrxp}\\ \texttt{palDm2av} & \texttt{iauRm2v}\\ \texttt{palDjcl} & \texttt{iauJd2cal}\\ \texttt{palDmxm} & \texttt{iauRxr}\\ \texttt{palDmxv} & \texttt{iauRxp}\\ \texttt{palDpav} & \texttt{iauPap}\\ \texttt{palDr2af} & \texttt{iauA2af}\\ \texttt{palDr2tf} & \texttt{iauA2tf}\\ \texttt{palDranrm} & \texttt{iauAnp}\\ \texttt{palDsep} & \texttt{iauSeps}\\ \texttt{palDsepv} & \texttt{iauSepp}\\ \texttt{palDtf2d} & \texttt{iauTf2d}\\ \texttt{palDtf2r} & \texttt{iauTf2a}\\ \texttt{palDvdv} & \texttt{iauPdp}\\ \texttt{palDvn} & \texttt{iauPn}\\ \texttt{palDvxv} & \texttt{iauPxp}\\ \texttt{palEpb} & \texttt{iauEpb}\\ \texttt{palEpb2d} & \texttt{iauEpb2d}\\ \texttt{palEpj} & \texttt{iauEpj}\\ \texttt{palEpj2d} & \texttt{iauEpj2jd}\\ \texttt{palEqeqx} & \texttt{iauEe06a}\\ \texttt{palFk5hz} & \texttt{iauFk5hz} \textit{also calls iauEpj2jd}\\ \texttt{palGmst} & \texttt{iauGmst06}\\ \texttt{palGmsta} & \texttt{iauGmst06}\\ \texttt{palHfk5z} & \texttt{iauHfk5z} \textit{also calls iauEpj2jd}\\ \end{tabular} sun267.htx/section30.tex000644 000765 000024 00000002114 12365763500 015370 0ustar00timjstaff000000 000000 \sstroutine{ palEqecl }{ Transform from J2000.0 equatorial coordinates to ecliptic coordinates }{ \sstdescription{ Transform from J2000.0 equatorial coordinates to ecliptic coordinates. } \sstinvocation{ void palEqecl( double dr, double dd, double date, double $*$dl, double $*$db); } \sstarguments{ \sstsubsection{ dr = double (Given) }{ J2000.0 mean RA (radians) } \sstsubsection{ dd = double (Given) }{ J2000.0 mean Dec (Radians) } \sstsubsection{ date = double (Given) }{ TT as Modified Julian Date (JD-2400000.5). The difference between TT and TDB is of the order of a millisecond or two (i.e. about 0.02 arc-seconds). } \sstsubsection{ dl = double $*$ (Returned) }{ Ecliptic longitude (mean of date, IAU 1980 theory, radians) } \sstsubsection{ db = double $*$ (Returned) }{ Ecliptic latitude (mean of date, IAU 1980 theory, radians) } } } sun267.htx/section31.tex000644 000765 000024 00000002004 12365763500 015367 0ustar00timjstaff000000 000000 \sstroutine{ palEqgal }{ Convert from J2000.0 equatorial coordinates to Galactic }{ \sstdescription{ Transformation from J2000.0 equatorial coordinates to IAU 1958 galactic coordinates. } \sstinvocation{ void palEqgal ( double dr, double dd, double $*$dl, double $*$db ); } \sstarguments{ \sstsubsection{ dr = double (Given) }{ J2000.0 RA (radians) } \sstsubsection{ dd = double (Given) }{ J2000.0 Dec (radians } \sstsubsection{ dl = double $*$ (Returned) }{ Galactic longitude (radians). } \sstsubsection{ db = double $*$ (Returned) }{ Galactic latitude (radians). } } \sstnotes{ The equatorial coordinates are J2000.0. Use the routine palGe50 if conversion to B1950.0 {\tt '}FK4{\tt '} coordinates is required. } \sstdiytopic{ See Also }{ Blaauw et al, Mon.Not.R.Astron.Soc.,121,123 (1960) } } sun267.htx/section32.tex000644 000765 000024 00000002571 12365763500 015401 0ustar00timjstaff000000 000000 \sstroutine{ palEvp }{ Returns the barycentric and heliocentric velocity and position of the Earth }{ \sstdescription{ Returns the barycentric and heliocentric velocity and position of the Earth at a given epoch, given with respect to a specified equinox. For information about accuracy, see the function iauEpv00. } \sstinvocation{ void palEvp( double date, double deqx, double dvb[3], double dpb[3], double dvh[3], double dph[3] ) } \sstarguments{ \sstsubsection{ date = double (Given) }{ TDB (loosely ET) as a Modified Julian Date (JD-2400000.5) } \sstsubsection{ deqx = double (Given) }{ Julian epoch (e.g. 2000.0) of mean equator and equinox of the vectors returned. If deqx $<$= 0.0, all vectors are referred to the mean equator and equinox (FK5) of epoch date. } \sstsubsection{ dvb = double[3] (Returned) }{ Barycentric velocity (AU/s, AU) } \sstsubsection{ dpb = double[3] (Returned) }{ Barycentric position (AU/s, AU) } \sstsubsection{ dvh = double[3] (Returned) }{ heliocentric velocity (AU/s, AU) } \sstsubsection{ dph = double[3] (Returned) }{ Heliocentric position (AU/s, AU) } } } sun267.htx/section33.tex000644 000765 000024 00000007356 12365763500 015410 0ustar00timjstaff000000 000000 \sstroutine{ palFk45z }{ Convert B1950.0 FK4 star data to J2000.0 FK5 assuming zero proper motion in the FK5 frame }{ \sstdescription{ Convert B1950.0 FK4 star data to J2000.0 FK5 assuming zero proper motion in the FK5 frame (double precision) This function converts stars from the Bessel-Newcomb, FK4 system to the IAU 1976, FK5, Fricke system, in such a way that the FK5 proper motion is zero. Because such a star has, in general, a non-zero proper motion in the FK4 system, the routine requires the epoch at which the position in the FK4 system was determined. The method is from Appendix 2 of Ref 1, but using the constants of Ref 4. } \sstinvocation{ palFk45z( double r1950, double d1950, double bepoch, double $*$r2000, double $*$d2000 ) } \sstarguments{ \sstsubsection{ r1950 = double (Given) }{ B1950.0 FK4 RA at epoch (radians). } \sstsubsection{ d1950 = double (Given) }{ B1950.0 FK4 Dec at epoch (radians). } \sstsubsection{ bepoch = double (Given) }{ Besselian epoch (e.g. 1979.3) } \sstsubsection{ r2000 = double (Returned) }{ J2000.0 FK5 RA (Radians). } \sstsubsection{ d2000 = double (Returned) }{ J2000.0 FK5 Dec(Radians). } } \sstnotes{ \sstitemlist{ \sstitem The epoch BEPOCH is strictly speaking Besselian, but if a Julian epoch is supplied the result will be affected only to a negligible extent. \sstitem Conversion from Besselian epoch 1950.0 to Julian epoch 2000.0 only is provided for. Conversions involving other epochs will require use of the appropriate precession, proper motion, and E-terms routines before and/or after palFk45z is called. \sstitem In the FK4 catalogue the proper motions of stars within 10 degrees of the poles do not embody the differential E-term effect and should, strictly speaking, be handled in a different manner from stars outside these regions. However, given the general lack of homogeneity of the star data available for routine astrometry, the difficulties of handling positions that may have been determined from astrometric fields spanning the polar and non-polar regions, the likelihood that the differential E-terms effect was not taken into account when allowing for proper motion in past astrometry, and the undesirability of a discontinuity in the algorithm, the decision has been made in this routine to include the effect of differential E-terms on the proper motions for all stars, whether polar or not. At epoch 2000, and measuring on the sky rather than in terms of dRA, the errors resulting from this simplification are less than 1 milliarcsecond in position and 1 milliarcsecond per century in proper motion. } } \sstdiytopic{ References }{ \sstitemlist{ \sstitem Aoki,S., et al, 1983. Astron.Astrophys., 128, 263. \sstitem Smith, C.A. et al, 1989. {\tt "}The transformation of astrometric catalog systems to the equinox J2000.0{\tt "}. Astron.J. 97, 265. \sstitem Yallop, B.D. et al, 1989. {\tt "}Transformation of mean star places from FK4 B1950.0 to FK5 J2000.0 using matrices in 6-space{\tt "}. Astron.J. 97, 274. \sstitem Seidelmann, P.K. (ed), 1992. {\tt "}Explanatory Supplement to the Astronomical Almanac{\tt "}, ISBN 0-935702-68-7. } } } sun267.htx/section34.tex000644 000765 000024 00000010751 12365763500 015402 0ustar00timjstaff000000 000000 \sstroutine{ palFk524 }{ Convert J2000.0 FK5 star data to B1950.0 FK4 }{ \sstdescription{ This function converts stars from the IAU 1976, FK5, Fricke system, to the Bessel-Newcomb, FK4 system. The precepts of Smith et al (Ref 1) are followed, using the implementation by Yallop et al (Ref 2) of a matrix method due to Standish. Kinoshita{\tt '}s development of Andoyer{\tt '}s post-Newcomb precession is used. The numerical constants from Seidelmann et al (Ref 3) are used canonically. } \sstinvocation{ palFk524( double r2000, double d2000, double dr2000, double dd2000, double p2000, double v2000, double $*$r1950, double $*$d1950, double $*$dr1950, double $*$dd1950, double $*$p1950, double $*$v1950 ) } \sstarguments{ \sstsubsection{ r2000 = double (Given) }{ J2000.0 FK5 RA (radians). } \sstsubsection{ d2000 = double (Given) }{ J2000.0 FK5 Dec (radians). } \sstsubsection{ dr2000 = double (Given) }{ J2000.0 FK5 RA proper motion (rad/Jul.yr) } \sstsubsection{ dd2000 = double (Given) }{ J2000.0 FK5 Dec proper motion (rad/Jul.yr) } \sstsubsection{ p2000 = double (Given) }{ J2000.0 FK5 parallax (arcsec) } \sstsubsection{ v2000 = double (Given) }{ J2000.0 FK5 radial velocity (km/s, $+$ve = moving away) } \sstsubsection{ r1950 = double $*$ (Returned) }{ B1950.0 FK4 RA (radians). } \sstsubsection{ d1950 = double $*$ (Returned) }{ B1950.0 FK4 Dec (radians). } \sstsubsection{ dr1950 = double $*$ (Returned) }{ B1950.0 FK4 RA proper motion (rad/Jul.yr) } \sstsubsection{ dd1950 = double $*$ (Returned) }{ B1950.0 FK4 Dec proper motion (rad/Jul.yr) } \sstsubsection{ p1950 = double $*$ (Returned) }{ B1950.0 FK4 parallax (arcsec) } \sstsubsection{ v1950 = double $*$ (Returned) }{ B1950.0 FK4 radial velocity (km/s, $+$ve = moving away) } } \sstnotes{ \sstitemlist{ \sstitem The proper motions in RA are dRA/dt rather than cos(Dec)$*$dRA/dt, and are per year rather than per century. \sstitem Note that conversion from Julian epoch 2000.0 to Besselian epoch 1950.0 only is provided for. Conversions involving other epochs will require use of the appropriate precession, proper motion, and E-terms routines before and/or after FK524 is called. \sstitem In the FK4 catalogue the proper motions of stars within 10 degrees of the poles do not embody the differential E-term effect and should, strictly speaking, be handled in a different manner from stars outside these regions. However, given the general lack of homogeneity of the star data available for routine astrometry, the difficulties of handling positions that may have been determined from astrometric fields spanning the polar and non-polar regions, the likelihood that the differential E-terms effect was not taken into account when allowing for proper motion in past astrometry, and the undesirability of a discontinuity in the algorithm, the decision has been made in this routine to include the effect of differential E-terms on the proper motions for all stars, whether polar or not. At epoch 2000, and measuring on the sky rather than in terms of dRA, the errors resulting from this simplification are less than 1 milliarcsecond in position and 1 milliarcsecond per century in proper motion. } } \sstdiytopic{ References }{ \sstitemlist{ \sstitem Smith, C.A. et al, 1989. {\tt "}The transformation of astrometric catalog systems to the equinox J2000.0{\tt "}. Astron.J. 97, 265. \sstitem Yallop, B.D. et al, 1989. {\tt "}Transformation of mean star places from FK4 B1950.0 to FK5 J2000.0 using matrices in 6-space{\tt "}. Astron.J. 97, 274. \sstitem Seidelmann, P.K. (ed), 1992. {\tt "}Explanatory Supplement to the Astronomical Almanac{\tt "}, ISBN 0-935702-68-7. } } } sun267.htx/section35.tex000644 000765 000024 00000004616 12365763500 015406 0ustar00timjstaff000000 000000 \sstroutine{ palFk54z }{ Convert a J2000.0 FK5 star position to B1950.0 FK4 assuming zero proper motion and parallax }{ \sstdescription{ This function converts star positions from the IAU 1976, FK5, Fricke system to the Bessel-Newcomb, FK4 system. } \sstinvocation{ palFk54z( double r2000, double d2000, double bepoch, double $*$r1950, double $*$d1950, double $*$dr1950, double $*$dd1950 ) } \sstarguments{ \sstsubsection{ r2000 = double (Given) }{ J2000.0 FK5 RA (radians). } \sstsubsection{ d2000 = double (Given) }{ J2000.0 FK5 Dec (radians). } \sstsubsection{ bepoch = double (Given) }{ Besselian epoch (e.g. 1950.0). } \sstsubsection{ r1950 = double $*$ (Returned) }{ B1950 FK4 RA (radians) at epoch {\tt "}bepoch{\tt "}. } \sstsubsection{ d1950 = double $*$ (Returned) }{ B1950 FK4 Dec (radians) at epoch {\tt "}bepoch{\tt "}. } \sstsubsection{ dr1950 = double $*$ (Returned) }{ B1950 FK4 proper motion (RA) (radians/trop.yr)). } \sstsubsection{ dr1950 = double $*$ (Returned) }{ B1950 FK4 proper motion (Dec) (radians/trop.yr)). } } \sstnotes{ \sstitemlist{ \sstitem The proper motion in RA is dRA/dt rather than cos(Dec)$*$dRA/dt. \sstitem Conversion from Julian epoch 2000.0 to Besselian epoch 1950.0 only is provided for. Conversions involving other epochs will require use of the appropriate precession functions before and after this function is called. \sstitem The FK5 proper motions, the parallax and the radial velocity are presumed zero. \sstitem It is the intention that FK5 should be a close approximation to an inertial frame, so that distant objects have zero proper motion; such objects have (in general) non-zero proper motion in FK4, and this function returns those fictitious proper motions. \sstitem The position returned by this function is in the B1950 reference frame but at Besselian epoch BEPOCH. For comparison with catalogues the {\tt "}bepoch{\tt "} argument will frequently be 1950.0. } } } sun267.htx/section36.tex000644 000765 000024 00000002005 12365763500 015375 0ustar00timjstaff000000 000000 \sstroutine{ palGaleq }{ Convert from galactic to J2000.0 equatorial coordinates }{ \sstdescription{ Transformation from IAU 1958 galactic coordinates to J2000.0 equatorial coordinates. } \sstinvocation{ void palGaleq ( double dl, double db, double $*$dr, double $*$dd ); } \sstarguments{ \sstsubsection{ dl = double (Given) }{ Galactic longitude (radians). } \sstsubsection{ db = double (Given) }{ Galactic latitude (radians). } \sstsubsection{ dr = double $*$ (Returned) }{ J2000.0 RA (radians) } \sstsubsection{ dd = double $*$ (Returned) }{ J2000.0 Dec (radians) } } \sstnotes{ The equatorial coordinates are J2000.0. Use the routine palGe50 if conversion to B1950.0 {\tt '}FK4{\tt '} coordinates is required. } \sstdiytopic{ See Also }{ Blaauw et al, Mon.Not.R.Astron.Soc.,121,123 (1960) } } sun267.htx/section37.tex000644 000765 000024 00000002461 12365763500 015404 0ustar00timjstaff000000 000000 \sstroutine{ palGalsup }{ Convert from galactic to supergalactic coordinates }{ \sstdescription{ Transformation from IAU 1958 galactic coordinates to de Vaucouleurs supergalactic coordinates. } \sstinvocation{ void palGalsup ( double dl, double db, double $*$dsl, double $*$dsb ); } \sstarguments{ \sstsubsection{ dl = double (Given) }{ Galactic longitude. } \sstsubsection{ db = double (Given) }{ Galactic latitude. } \sstsubsection{ dsl = double $*$ (Returned) }{ Supergalactic longitude. } \sstsubsection{ dsb = double $*$ (Returned) }{ Supergalactic latitude. } } \sstdiytopic{ See Also }{ \sstitemlist{ \sstitem de Vaucouleurs, de Vaucouleurs, \& Corwin, Second Reference Catalogue of Bright Galaxies, U. Texas, page 8. \sstitem Systems \& Applied Sciences Corp., Documentation for the machine-readable version of the above catalogue, Contract NAS 5-26490. } (These two references give different values for the galactic longitude of the supergalactic origin. Both are wrong; the correct value is L2=137.37.) } } sun267.htx/section38.tex000644 000765 000024 00000002127 12365763500 015404 0ustar00timjstaff000000 000000 \sstroutine{ palGe50 }{ Transform Galactic Coordinate to B1950 FK4 }{ \sstdescription{ Transformation from IAU 1958 galactic coordinates to B1950.0 {\tt '}FK4{\tt '} equatorial coordinates. } \sstinvocation{ palGe50( double dl, double db, double $*$dr, double $*$dd ); } \sstarguments{ \sstsubsection{ dl = double (Given) }{ Galactic longitude (radians) } \sstsubsection{ db = double (Given) }{ Galactic latitude (radians) } \sstsubsection{ dr = double $*$ (Returned) }{ B9150.0 FK4 RA. } \sstsubsection{ dd = double $*$ (Returned) }{ B1950.0 FK4 Dec. } } \sstnotes{ \sstitemlist{ \sstitem The equatorial coordinates are B1950.0 {\tt '}FK4{\tt '}. Use the routine palGaleq if conversion to J2000.0 coordinates is required. } } \sstdiytopic{ See Also }{ \sstitemlist{ \sstitem Blaauw et al, Mon.Not.R.Astron.Soc.,121,123 (1960) } } } sun267.htx/section39.tex000644 000765 000024 00000001651 12365763500 015406 0ustar00timjstaff000000 000000 \sstroutine{ palGeoc }{ Convert geodetic position to geocentric }{ \sstdescription{ Convert geodetic position to geocentric. } \sstinvocation{ void palGeoc( double p, double h, double $*$ r, double $*$z ); } \sstarguments{ \sstsubsection{ p = double (Given) }{ latitude (radians) } \sstsubsection{ h = double (Given) }{ height above reference spheroid (geodetic, metres) } \sstsubsection{ r = double $*$ (Returned) }{ distance from Earth axis (AU) } \sstsubsection{ z = double $*$ (Returned) }{ distance from plane of Earth equator (AU) } } \sstnotes{ \sstitemlist{ \sstitem Geocentric latitude can be obtained by evaluating atan2(z,r) \sstitem Uses WGS84 reference ellipsoid and calls iauGd2gc } } } sun267.htx/section4.tex000644 000765 000024 00000000662 12365763500 015317 0ustar00timjstaff000000 000000 \subsection{More complex functions} These functions do not have a simple equivalent in SOFA so are reimplemented either completely standalone or using multiple SOFA functions. %% Regenerate everything after this from the prologues using SST by %% running "make palsun.tex". We do not build this automatically as %% there is no particular need for an SST dependency. %% Some manual tweaking is required after creating the SST tex. sun267.htx/section40.tex000644 000765 000024 00000003400 12365763500 015370 0ustar00timjstaff000000 000000 \sstroutine{ palIntin }{ Convert free-format input into an integer }{ \sstdescription{ Extracts a number from an input string starting at the specified index. } \sstinvocation{ void palIntin( const char $*$ string, int $*$nstrt, long $*$ireslt, int $*$jflag ); } \sstarguments{ \sstsubsection{ string = const char $*$ (Given) }{ String containing number to be decoded. } \sstsubsection{ nstrt = int $*$ (Given and Returned) }{ Character number indicating where decoding should start. On output its value is updated to be the location of the possible next value. For compatibility with SLA the first character is index 1. } \sstsubsection{ ireslt = long $*$ (Returned) }{ Result. Not updated when jflag=1. } \sstsubsection{ jflag = int $*$ (Returned) }{ status: -1 = -OK, 0 = $+$OK, 1 = null, 2 = error } } \sstnotes{ \sstitemlist{ \sstitem Uses the strtol() system call to do the parsing. This may lead to subtle differences when compared to the SLA/F parsing. \sstitem Commas are recognized as a special case and are skipped if one happens to be the next character when updating nstrt. Additionally the output nstrt position will skip past any trailing space. \sstitem If no number can be found flag will be set to 1. \sstitem If the number overflows or underflows jflag will be set to 2. For overflow the returned result will have the value LONG\_MAX, for underflow it will have the value LONG\_MIN. } } } sun267.htx/section41.tex000644 000765 000024 00000003263 12365763500 015400 0ustar00timjstaff000000 000000 \sstroutine{ palMap }{ Convert star RA,Dec from mean place to geocentric apparent }{ \sstdescription{ Convert star RA,Dec from mean place to geocentric apparent. } \sstinvocation{ void palMap( double rm, double dm, double pr, double pd, double px, double rv, double eq, double date, double $*$ra, double $*$da ); } \sstarguments{ \sstsubsection{ rm = double (Given) }{ Mean RA (radians) } \sstsubsection{ dm = double (Given) }{ Mean declination (radians) } \sstsubsection{ pr = double (Given) }{ RA proper motion, changes per Julian year (radians) } \sstsubsection{ pd = double (Given) }{ Dec proper motion, changes per Julian year (radians) } \sstsubsection{ px = double (Given) }{ Parallax (arcsec) } \sstsubsection{ rv = double (Given) }{ Radial velocity (km/s, $+$ve if receding) } \sstsubsection{ eq = double (Given) }{ Epoch and equinox of star data (Julian) } \sstsubsection{ date = double (Given) }{ TDB for apparent place (JD-2400000.5) } \sstsubsection{ ra = double $*$ (Returned) }{ Apparent RA (radians) } \sstsubsection{ dec = double $*$ (Returned) }{ Apparent dec (radians) } } \sstnotes{ \sstitemlist{ \sstitem Calls palMappa and palMapqk \sstitem The reference systems and timescales used are IAU 2006. } } } sun267.htx/section42.tex000644 000765 000024 00000004025 12365763500 015376 0ustar00timjstaff000000 000000 \sstroutine{ palMappa }{ Compute parameters needed by palAmpqk and palMapqk }{ \sstdescription{ Compute star-independent parameters in preparation for transformations between mean place and geocentric apparent place. The parameters produced by this function are required in the parallax, aberration, and nutation/bias/precession parts of the mean/apparent transformations. The reference systems and timescales used are IAU 2006. } \sstinvocation{ void palMappa( double eq, double date, double amprms[21] ) } \sstarguments{ \sstsubsection{ eq = double (Given) }{ epoch of mean equinox to be used (Julian) } \sstsubsection{ date = double (Given) }{ TDB (JD-2400000.5) } \sstsubsection{ amprms = double[21] (Returned) }{ star-independent mean-to-apparent parameters: \sstitemlist{ \sstitem (0) time interval for proper motion (Julian years) \sstitem (1-3) barycentric position of the Earth (AU) \sstitem (4-6) heliocentric direction of the Earth (unit vector) \sstitem (7) (grav rad Sun)$*$2/(Sun-Earth distance) \sstitem (8-10) abv: barycentric Earth velocity in units of c \sstitem (11) sqrt(1-v$*$$*$2) where v=modulus(abv) \sstitem (12-20) precession/nutation (3,3) matrix } } } \sstnotes{ \sstitemlist{ \sstitem For date, the distinction between the required TDB and TT is always negligible. Moreover, for all but the most critical applications UTC is adequate. \sstitem The vector amprms(1-3) is referred to the mean equinox and equator of epoch eq. \sstitem The parameters amprms produced by this function are used by palAmpqk, palMapqk and palMapqkz. } } } sun267.htx/section43.tex000644 000765 000024 00000003763 12365763500 015407 0ustar00timjstaff000000 000000 \sstroutine{ palMapqk }{ Quick mean to apparent place }{ \sstdescription{ Quick mean to apparent place: transform a star RA,Dec from mean place to geocentric apparent place, given the star-independent parameters. Use of this routine is appropriate when efficiency is important and where many star positions, all referred to the same equator and equinox, are to be transformed for one epoch. The star-independent parameters can be obtained by calling the palMappa routine. If the parallax and proper motions are zero the palMapqkz routine can be used instead. } \sstinvocation{ void palMapqk ( double rm, double dm, double pr, double pd, double px, double rv, double amprms[21], double $*$ra, double $*$da ); } \sstarguments{ \sstsubsection{ rm = double (Given) }{ Mean RA (radians) } \sstsubsection{ dm = double (Given) }{ Mean declination (radians) } \sstsubsection{ pr = double (Given) }{ RA proper motion, changes per Julian year (radians) } \sstsubsection{ pd = double (Given) }{ Dec proper motion, changes per Julian year (radians) } \sstsubsection{ px = double (Given) }{ Parallax (arcsec) } \sstsubsection{ rv = double (Given) }{ Radial velocity (km/s, $+$ve if receding) } \sstsubsection{ amprms = double [21] (Given) }{ Star-independent mean-to-apparent parameters (see palMappa). } \sstsubsection{ ra = double $*$ (Returned) }{ Apparent RA (radians) } \sstsubsection{ dec = double $*$ (Returned) }{ Apparent dec (radians) } } \sstnotes{ \sstitemlist{ \sstitem The reference frames and timescales used are post IAU 2006. } } } sun267.htx/section44.tex000644 000765 000024 00000003631 12365763500 015402 0ustar00timjstaff000000 000000 \sstroutine{ palMapqkz }{ Quick mean to apparent place }{ \sstdescription{ Quick mean to apparent place: transform a star RA,dec from mean place to geocentric apparent place, given the star-independent parameters, and assuming zero parallax and proper motion. Use of this function is appropriate when efficiency is important and where many star positions, all with parallax and proper motion either zero or already allowed for, and all referred to the same equator and equinox, are to be transformed for one epoch. The star-independent parameters can be obtained by calling the palMappa function. The corresponding function for the case of non-zero parallax and proper motion is palMapqk. The reference systems and timescales used are IAU 2006. Strictly speaking, the function is not valid for solar-system sources, though the error will usually be extremely small. } \sstinvocation{ void palMapqkz( double rm, double dm, double amprms[21], double $*$ra, double $*$da ) } \sstarguments{ \sstsubsection{ rm = double (Given) }{ Mean RA (radians). } \sstsubsection{ dm = double (Given) }{ Mean Dec (radians). } \sstsubsection{ amprms = double[21] (Given) }{ Star-independent mean-to-apparent parameters (see palMappa): (0-3) not used (4-6) not used (7) not used (8-10) abv: barycentric Earth velocity in units of c (11) sqrt(1-v$*$$*$2) where v=modulus(abv) (12-20) precession/nutation (3,3) matrix } \sstsubsection{ ra = double $*$ (Returned) }{ Apparent RA (radians). } \sstsubsection{ da = double $*$ (Returned) }{ Apparent Dec (radians). } } } sun267.htx/section45.tex000644 000765 000024 00000001762 12365763500 015406 0ustar00timjstaff000000 000000 \sstroutine{ palNut }{ Form the matrix of nutation }{ \sstdescription{ Form the matrix of nutation for a given date using the IAU 2006 nutation model and palDeuler. } \sstinvocation{ void palNut( double date, double rmatn[3][3] ); } \sstarguments{ \sstsubsection{ date = double (Given) }{ TT as modified Julian date (JD-2400000.5) } \sstsubsection{ rmatn = double [3][3] (Returned) }{ Nutation matrix in the sense v(true)=rmatn $*$ v(mean) where v(true) is the star vector relative to the true equator and equinox of date and v(mean) is the star vector relative to the mean equator and equinox of date. } } \sstnotes{ \sstitemlist{ \sstitem Uses iauNut06a via palNutc \sstitem The distinction between TDB and TT is negligible. For all but the most critical applications UTC is adequate. } } } sun267.htx/section46.tex000644 000765 000024 00000002063 12365763500 015402 0ustar00timjstaff000000 000000 \sstroutine{ palNutc }{ Calculate nutation longitude \& obliquoty components }{ \sstdescription{ Calculates the longitude $*$ obliquity components and mean obliquity using the SOFA library. } \sstinvocation{ void palNutc( double date, double $*$ dpsi, double $*$deps, double $*$eps0 ); } \sstarguments{ \sstsubsection{ date = double (Given) }{ TT as modified Julian date (JD-2400000.5) } \sstsubsection{ dpsi = double $*$ (Returned) }{ Nutation in longitude } \sstsubsection{ deps = double $*$ (Returned) }{ Nutation in obliquity } \sstsubsection{ eps0 = double $*$ (Returned) }{ Mean obliquity. } } \sstnotes{ \sstitemlist{ \sstitem Calls iauObl06 and iauNut06a and therefore uses the IAU 206 precession/nutation model. \sstitem Note the change from SLA/F regarding the date. TT is used rather than TDB. } } } sun267.htx/section47.tex000644 000765 000024 00000007547 12365763500 015417 0ustar00timjstaff000000 000000 \sstroutine{ palObs }{ Parameters of selected ground-based observing stations }{ \sstdescription{ Station numbers, identifiers, names and other details are subject to change and should not be hardwired into application programs. All characters in {\tt "}c{\tt "} up to the first space are checked; thus an abbreviated ID will return the parameters for the first station in the list which matches the abbreviation supplied, and no station in the list will ever contain embedded spaces. {\tt "}c{\tt "} must not have leading spaces. IMPORTANT -- BEWARE OF THE LONGITUDE SIGN CONVENTION. The longitude returned by sla\_OBS is west-positive in accordance with astronomical usage. However, this sign convention is left-handed and is the opposite of the one used by geographers; elsewhere in PAL the preferable east-positive convention is used. In particular, note that for use in palAop, palAoppa and palOap the sign of the longitude must be reversed. Users are urged to inform the author of any improvements they would like to see made. For example: typographical corrections more accurate parameters better station identifiers or names additional stations } \sstinvocation{ int palObs( size\_t n, const char $*$ c, char $*$ ident, size\_t identlen, char $*$ name, size\_t namelen, double $*$ w, double $*$ p, double $*$ h ); } \sstarguments{ \sstsubsection{ n = size\_t (Given) }{ Number specifying the observing station. If 0 the identifier in {\tt "}c{\tt "} is used to determine the observing station to use. } \sstsubsection{ c = const char $*$ (Given) }{ Identifier specifying the observing station for which the parameters should be returned. Only used if n is 0. Can be NULL for n$>$0. Case insensitive. } \sstsubsection{ ident = char $*$ (Returned) }{ Identifier of the observing station selected. Will be identical to {\tt "}c{\tt "} if n==0. Unchanged if {\tt "}n{\tt "} or {\tt "}c{\tt "} do not match an observing station. Should be at least 11 characters (including the trailing nul). } \sstsubsection{ identlen = size\_t (Given) }{ Size of the buffer {\tt "}ident{\tt "} including trailing nul. } \sstsubsection{ name = char $*$ (Returned) }{ Full name of the specified observing station. Contains {\tt "}?{\tt "} if {\tt "}n{\tt "} or {\tt "}c{\tt "} did not correspond to a valid station. Should be at least 41 characters (including the trailing nul). } \sstsubsection{ w = double $*$ (Returned) }{ Longitude (radians, West $+$ve). Unchanged if observing station could not be identified. } \sstsubsection{ p = double $*$ (Returned) }{ Geodetic latitude (radians, North $+$ve). Unchanged if observing station could not be identified. } \sstsubsection{ h = double $*$ (Returned) }{ Height above sea level (metres). Unchanged if observing station could not be identified. } } \sstreturnedvalue{ \sstsubsection{ palObs = int }{ 0 if an observing station was returned. -1 if no match was found. } } \sstnotes{ \sstitemlist{ \sstitem Differs from the SLA interface in that the output short name is not the same variable as the input short name. This simplifies consting. Additionally the size of the output buffers are now specified in the API and a status integer is returned. } } } sun267.htx/section48.tex000644 000765 000024 00000002365 12365763500 015411 0ustar00timjstaff000000 000000 \sstroutine{ palPa }{ HA, Dec to Parallactic Angle }{ \sstdescription{ Converts HA, Dec to Parallactic Angle. } \sstinvocation{ double palPa( double ha, double dec, double phi ); } \sstarguments{ \sstsubsection{ ha = double (Given) }{ Hour angle in radians (Geocentric apparent) } \sstsubsection{ dec = double (Given) }{ Declination in radians (Geocentric apparent) } \sstsubsection{ phi = double (Given) }{ Observatory latitude in radians (geodetic) } } \sstreturnedvalue{ \sstsubsection{ palPa = double }{ Parallactic angle in the range -pi to $+$pi. } } \sstnotes{ \sstitemlist{ \sstitem The parallactic angle at a point in the sky is the position angle of the vertical, i.e. the angle between the direction to the pole and to the zenith. In precise applications care must be taken only to use geocentric apparent HA,Dec and to consider separately the effects of atmospheric refraction and telescope mount errors. \sstitem At the pole a zero result is returned. } } } sun267.htx/section49.tex000644 000765 000024 00000014615 12365763500 015413 0ustar00timjstaff000000 000000 \sstroutine{ palPertel }{ Update elements by applying planetary perturbations }{ \sstdescription{ Update the osculating orbital elements of an asteroid or comet by applying planetary perturbations. } \sstinvocation{ void palPertel (int jform, double date0, double date1, double epoch0, double orbi0, double anode0, double perih0, double aorq0, double e0, double am0, double $*$epoch1, double $*$orbi1, double $*$anode1, double $*$perih1, double $*$aorq1, double $*$e1, double $*$am1, int $*$jstat ); } \sstarguments{ \sstsubsection{ jform = int (Given) }{ Element set actually returned (1-3; Note 6) } \sstsubsection{ date0 = double (Given) }{ Date of osculation (TT MJD) for the given elements. } \sstsubsection{ date1 = double (Given) }{ Date of osculation (TT MJD) for the updated elements. } \sstsubsection{ epoch0 = double (Given) }{ Epoch of elements (TT MJD) } \sstsubsection{ orbi0 = double (Given) }{ inclination (radians) } \sstsubsection{ anode0 = double (Given) }{ longitude of the ascending node (radians) } \sstsubsection{ perih0 = double (Given) }{ longitude or argument of perihelion (radians) } \sstsubsection{ aorq0 = double (Given) }{ mean distance or perihelion distance (AU) } \sstsubsection{ e0 = double (Given) }{ eccentricity } \sstsubsection{ am0 = double (Given) }{ mean anomaly (radians, JFORM=2 only) } \sstsubsection{ epoch1 = double $*$ (Returned) }{ Epoch of elements (TT MJD) } \sstsubsection{ orbi1 = double $*$ (Returned) }{ inclination (radians) } \sstsubsection{ anode1 = double $*$ (Returned) }{ longitude of the ascending node (radians) } \sstsubsection{ perih1 = double $*$ (Returned) }{ longitude or argument of perihelion (radians) } \sstsubsection{ aorq1 = double $*$ (Returned) }{ mean distance or perihelion distance (AU) } \sstsubsection{ e1 = double $*$ (Returned) }{ eccentricity } \sstsubsection{ am1 = double $*$ (Returned) }{ mean anomaly (radians, JFORM=2 only) } \sstsubsection{ jstat = int $*$ (Returned) }{ status: \sstitemlist{ \sstitem $+$102 = warning, distant epoch \sstitem $+$101 = warning, large timespan ( $>$ 100 years) \sstitem $+$1 to $+$10 = coincident with planet (Note 6) \sstitem 0 = OK \sstitem -1 = illegal JFORM \sstitem -2 = illegal E0 \sstitem -3 = illegal AORQ0 \sstitem -4 = internal error \sstitem -5 = numerical error } } } \sstnotes{ \sstitemlist{ \sstitem Two different element-format options are available: } Option JFORM=2, suitable for minor planets: EPOCH = epoch of elements (TT MJD) ORBI = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = mean distance, a (AU) E = eccentricity, e AM = mean anomaly M (radians) Option JFORM=3, suitable for comets: EPOCH = epoch of perihelion (TT MJD) ORBI = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = perihelion distance, q (AU) E = eccentricity, e \sstitemlist{ \sstitem DATE0, DATE1, EPOCH0 and EPOCH1 are all instants of time in the TT timescale (formerly Ephemeris Time, ET), expressed as Modified Julian Dates (JD-2400000.5). } DATE0 is the instant at which the given (i.e. unperturbed) osculating elements are correct. DATE1 is the specified instant at which the updated osculating elements are correct. EPOCH0 and EPOCH1 will be the same as DATE0 and DATE1 (respectively) for the JFORM=2 case, normally used for minor planets. For the JFORM=3 case, the two epochs will refer to perihelion passage and so will not, in general, be the same as DATE0 and/or DATE1 though they may be similar to one another. \sstitemlist{ \sstitem The elements are with respect to the J2000 ecliptic and equinox. \sstitem Unused elements (AM0 and AM1 for JFORM=3) are not accessed. \sstitem See the palPertue routine for details of the algorithm used. \sstitem This routine is not intended to be used for major planets, which is why JFORM=1 is not available and why there is no opportunity to specify either the longitude of perihelion or the daily motion. However, if JFORM=2 elements are somehow obtained for a major planet and supplied to the routine, sensible results will, in fact, be produced. This happens because the sla\_PERTUE routine that is called to perform the calculations checks the separation between the body and each of the planets and interprets a suspiciously small value (0.001 AU) as an attempt to apply it to the planet concerned. If this condition is detected, the contribution from that planet is ignored, and the status is set to the planet number (1-10 = Mercury, Venus, EMB, Mars, Jupiter, Saturn, Uranus, Neptune, Earth, Moon) as a warning. } } \sstdiytopic{ See Also }{ \sstitemlist{ \sstitem Sterne, Theodore E., {\tt "}An Introduction to Celestial Mechanics{\tt "}, Interscience Publishers Inc., 1960. Section 6.7, p199. } } } sun267.htx/section5.tex000644 000765 000024 00000002705 12365763500 015320 0ustar00timjstaff000000 000000 \sstroutine{ palAddet }{ Add the E-terms to a pre IAU 1976 mean place }{ \sstdescription{ Add the E-terms (elliptic component of annual aberration) to a pre IAU 1976 mean place to conform to the old catalogue convention. } \sstinvocation{ void palAddet ( double rm, double dm, double eq, double $*$rc, double $*$dc ); } \sstarguments{ \sstsubsection{ rm = double (Given) }{ RA without E-terms (radians) } \sstsubsection{ dm = double (Given) }{ Dec without E-terms (radians) } \sstsubsection{ eq = double (Given) }{ Besselian epoch of mean equator and equinox } \sstsubsection{ rc = double $*$ (Returned) }{ RA with E-terms included (radians) } \sstsubsection{ dc = double $*$ (Returned) }{ Dec with E-terms included (radians) } } \sstnotes{ Most star positions from pre-1984 optical catalogues (or derived from astrometry using such stars) embody the E-terms. If it is necessary to convert a formal mean place (for example a pulsar timing position) to one consistent with such a star catalogue, then the RA,Dec should be adjusted using this routine. } \sstdiytopic{ See Also }{ Explanatory Supplement to the Astronomical Ephemeris, section 2D, page 48. } } sun267.htx/section50.tex000644 000765 000024 00000017227 12365763500 015405 0ustar00timjstaff000000 000000 \sstroutine{ palPertue }{ Update the universal elements by applying planetary perturbations }{ \sstdescription{ Update the universal elements of an asteroid or comet by applying planetary perturbations. } \sstinvocation{ void palPertue( double date, double u[13], int $*$jstat ); } \sstarguments{ \sstsubsection{ date = double (Given) }{ Final epoch (TT MJD) for the update elements. } \sstsubsection{ u = const double [13] (Given \& Returned) }{ Universal orbital elements (Note 1) (0) combined mass (M$+$m) (1) total energy of the orbit (alpha) (2) reference (osculating) epoch (t0) (3-5) position at reference epoch (r0) (6-8) velocity at reference epoch (v0) (9) heliocentric distance at reference epoch (10) r0.v0 (11) date (t) (12) universal eccentric anomaly (psi) of date, approx } \sstsubsection{ jstat = int $*$ (Returned) }{ status: $+$102 = warning, distant epoch $+$101 = warning, large timespan ( $>$ 100 years) $+$1 to $+$10 = coincident with major planet (Note 5) 0 = OK \sstitemlist{ \sstitem 1 = numerical error } } } \sstnotes{ \sstitemlist{ \sstitem The {\tt "}universal{\tt "} elements are those which define the orbit for the purposes of the method of universal variables (see reference 2). They consist of the combined mass of the two bodies, an epoch, and the position and velocity vectors (arbitrary reference frame) at that epoch. The parameter set used here includes also various quantities that can, in fact, be derived from the other information. This approach is taken to avoiding unnecessary computation and loss of accuracy. The supplementary quantities are (i) alpha, which is proportional to the total energy of the orbit, (ii) the heliocentric distance at epoch, (iii) the outwards component of the velocity at the given epoch, (iv) an estimate of psi, the {\tt "}universal eccentric anomaly{\tt "} at a given date and (v) that date. \sstitem The universal elements are with respect to the J2000 equator and equinox. \sstitem The epochs DATE, U(3) and U(12) are all Modified Julian Dates (JD-2400000.5). \sstitem The algorithm is a simplified form of Encke{\tt '}s method. It takes as a basis the unperturbed motion of the body, and numerically integrates the perturbing accelerations from the major planets. The expression used is essentially Sterne{\tt '}s 6.7-2 (reference 1). Everhart and Pitkin (reference 2) suggest rectifying the orbit at each integration step by propagating the new perturbed position and velocity as the new universal variables. In the present routine the orbit is rectified less frequently than this, in order to gain a slight speed advantage. However, the rectification is done directly in terms of position and velocity, as suggested by Everhart and Pitkin, bypassing the use of conventional orbital elements. } The f(q) part of the full Encke method is not used. The purpose of this part is to avoid subtracting two nearly equal quantities when calculating the {\tt "}indirect member{\tt "}, which takes account of the small change in the Sun{\tt '}s attraction due to the slightly displaced position of the perturbed body. A simpler, direct calculation in double precision proves to be faster and not significantly less accurate. Apart from employing a variable timestep, and occasionally {\tt "}rectifying the orbit{\tt "} to keep the indirect member small, the integration is done in a fairly straightforward way. The acceleration estimated for the middle of the timestep is assumed to apply throughout that timestep; it is also used in the extrapolation of the perturbations to the middle of the next timestep, to predict the new disturbed position. There is no iteration within a timestep. Measures are taken to reach a compromise between execution time and accuracy. The starting-point is the goal of achieving arcsecond accuracy for ordinary minor planets over a ten-year timespan. This goal dictates how large the timesteps can be, which in turn dictates how frequently the unperturbed motion has to be recalculated from the osculating elements. Within predetermined limits, the timestep for the numerical integration is varied in length in inverse proportion to the magnitude of the net acceleration on the body from the major planets. The numerical integration requires estimates of the major-planet motions. Approximate positions for the major planets (Pluto alone is omitted) are obtained from the routine palPlanet. Two levels of interpolation are used, to enhance speed without significantly degrading accuracy. At a low frequency, the routine palPlanet is called to generate updated position$+$velocity {\tt "}state vectors{\tt "}. The only task remaining to be carried out at the full frequency (i.e. at each integration step) is to use the state vectors to extrapolate the planetary positions. In place of a strictly linear extrapolation, some allowance is made for the curvature of the orbit by scaling back the radius vector as the linear extrapolation goes off at a tangent. Various other approximations are made. For example, perturbations by Pluto and the minor planets are neglected and relativistic effects are not taken into account. In the interests of simplicity, the background calculations for the major planets are carried out en masse. The mean elements and state vectors for all the planets are refreshed at the same time, without regard for orbit curvature, mass or proximity. The Earth-Moon system is treated as a single body when the body is distant but as separate bodies when closer to the EMB than the parameter RNE, which incurs a time penalty but improves accuracy for near-Earth objects. \sstitemlist{ \sstitem This routine is not intended to be used for major planets. However, if major-planet elements are supplied, sensible results will, in fact, be produced. This happens because the routine checks the separation between the body and each of the planets and interprets a suspiciously small value (0.001 AU) as an attempt to apply the routine to the planet concerned. If this condition is detected, the contribution from that planet is ignored, and the status is set to the planet number (1-10 = Mercury, Venus, EMB, Mars, Jupiter, Saturn, Uranus, Neptune, Earth, Moon) as a warning. } } \sstdiytopic{ See Also }{ \sstitemlist{ \sstitem Sterne, Theodore E., {\tt "}An Introduction to Celestial Mechanics{\tt "}, Interscience Publishers Inc., 1960. Section 6.7, p199. \sstitem Everhart, E. \& Pitkin, E.T., Am.J.Phys. 51, 712, 1983. } } } sun267.htx/section51.tex000644 000765 000024 00000016347 12365763500 015410 0ustar00timjstaff000000 000000 \sstroutine{ palPlanel }{ Transform conventional elements into position and velocity }{ \sstdescription{ Heliocentric position and velocity of a planet, asteroid or comet, starting from orbital elements. } \sstinvocation{ void palPlanel ( double date, int jform, double epoch, double orbinc, double anode, double perih, double aorq, double e, double aorl, double dm, double pv[6], int $*$jstat ); } \sstarguments{ \sstsubsection{ date = double (Given) }{ Epoch (TT MJD) of osculation (Note 1) } \sstsubsection{ jform = int (Given) }{ Element set actually returned (1-3; Note 3) } \sstsubsection{ epoch = double (Given) }{ Epoch of elements (TT MJD) (Note 4) } \sstsubsection{ orbinc = double (Given) }{ inclination (radians) } \sstsubsection{ anode = double (Given) }{ longitude of the ascending node (radians) } \sstsubsection{ perih = double (Given) }{ longitude or argument of perihelion (radians) } \sstsubsection{ aorq = double (Given) }{ mean distance or perihelion distance (AU) } \sstsubsection{ e = double (Given) }{ eccentricity } \sstsubsection{ aorl = double (Given) }{ mean anomaly or longitude (radians, JFORM=1,2 only) } \sstsubsection{ dm = double (Given) }{ daily motion (radians, JFORM=1 only) } \sstsubsection{ u = double [13] (Returned) }{ Universal orbital elements (Note 1) (0) combined mass (M$+$m) (1) total energy of the orbit (alpha) (2) reference (osculating) epoch (t0) (3-5) position at reference epoch (r0) (6-8) velocity at reference epoch (v0) (9) heliocentric distance at reference epoch (10) r0.v0 (11) date (t) (12) universal eccentric anomaly (psi) of date, approx } \sstsubsection{ jstat = int $*$ (Returned) }{ status: 0 = OK \sstitemlist{ \sstitem -1 = illegal JFORM \sstitem -2 = illegal E \sstitem -3 = illegal AORQ \sstitem -4 = illegal DM \sstitem -5 = numerical error } } } \sstnotes{ \sstitemlist{ \sstitem DATE is the instant for which the prediction is required. It is in the TT timescale (formerly Ephemeris Time, ET) and is a Modified Julian Date (JD-2400000.5). \sstitem The elements are with respect to the J2000 ecliptic and equinox. \sstitem A choice of three different element-set options is available: } Option JFORM = 1, suitable for the major planets: EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = longitude of perihelion, curly pi (radians) AORQ = mean distance, a (AU) E = eccentricity, e (range 0 to $<$1) AORL = mean longitude L (radians) DM = daily motion (radians) Option JFORM = 2, suitable for minor planets: EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = mean distance, a (AU) E = eccentricity, e (range 0 to $<$1) AORL = mean anomaly M (radians) Option JFORM = 3, suitable for comets: EPOCH = epoch of elements and perihelion (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = perihelion distance, q (AU) E = eccentricity, e (range 0 to 10) Unused arguments (DM for JFORM=2, AORL and DM for JFORM=3) are not accessed. \sstitemlist{ \sstitem Each of the three element sets defines an unperturbed heliocentric orbit. For a given epoch of observation, the position of the body in its orbit can be predicted from these elements, which are called {\tt "}osculating elements{\tt "}, using standard two-body analytical solutions. However, due to planetary perturbations, a given set of osculating elements remains usable for only as long as the unperturbed orbit that it describes is an adequate approximation to reality. Attached to such a set of elements is a date called the {\tt "}osculating epoch{\tt "}, at which the elements are, momentarily, a perfect representation of the instantaneous position and velocity of the body. } Therefore, for any given problem there are up to three different epochs in play, and it is vital to distinguish clearly between them: . The epoch of observation: the moment in time for which the position of the body is to be predicted. . The epoch defining the position of the body: the moment in time at which, in the absence of purturbations, the specified position (mean longitude, mean anomaly, or perihelion) is reached. . The osculating epoch: the moment in time at which the given elements are correct. For the major-planet and minor-planet cases it is usual to make the epoch that defines the position of the body the same as the epoch of osculation. Thus, only two different epochs are involved: the epoch of the elements and the epoch of observation. For comets, the epoch of perihelion fixes the position in the orbit and in general a different epoch of osculation will be chosen. Thus, all three types of epoch are involved. For the present routine: . The epoch of observation is the argument DATE. . The epoch defining the position of the body is the argument EPOCH. . The osculating epoch is not used and is assumed to be close enough to the epoch of observation to deliver adequate accuracy. If not, a preliminary call to sla\_PERTEL may be used to update the element-set (and its associated osculating epoch) by applying planetary perturbations. \sstitemlist{ \sstitem The reference frame for the result is with respect to the mean equator and equinox of epoch J2000. \sstitem The algorithm was originally adapted from the EPHSLA program of D.H.P.Jones (private communication, 1996). The method is based on Stumpff{\tt '}s Universal Variables. } } \sstdiytopic{ See Also }{ Everhart, E. \& Pitkin, E.T., Am.J.Phys. 51, 712, 1983. } } sun267.htx/section52.tex000644 000765 000024 00000002766 12365763500 015411 0ustar00timjstaff000000 000000 \sstroutine{ palPlanet }{ Approximate heliocentric position and velocity of major planet }{ \sstdescription{ Calculates the approximate heliocentric position and velocity of the specified major planet. } \sstinvocation{ void palPlanet ( double date, int np, double pv[6], int $*$j ); } \sstarguments{ \sstsubsection{ date = double (Given) }{ TDB Modified Julian Date (JD-2400000.5). } \sstsubsection{ np = int (Given) }{ planet (1=Mercury, 2=Venus, 3=EMB, 4=Mars, 5=Jupiter, 6=Saturn, 7=Uranus, 8=Neptune) } \sstsubsection{ pv = double [6] (Returned) }{ heliocentric x,y,z,xdot,ydot,zdot, J2000, equatorial triad in units AU and AU/s. } \sstsubsection{ j = int $*$ (Returned) }{ \sstitemlist{ \sstitem -2 = solution didn{\tt '}t converge. \sstitem -1 = illegal np (1-8) \sstitem 0 = OK \sstitem $+$1 = warning: year outside 1000-3000 } } } \sstnotes{ \sstitemlist{ \sstitem See SOFA iauPlan94 for details \sstitem Note that Pluto is supported in SLA/F but not in this routine \sstitem Status -2 is equivalent to iauPlan94 status $+$2. \sstitem Note that velocity units here match the SLA/F documentation. } } } sun267.htx/section53.tex000644 000765 000024 00000022231 12365763500 015377 0ustar00timjstaff000000 000000 \sstroutine{ palPlante }{ Topocentric RA,Dec of a Solar-System object from heliocentric orbital elements }{ \sstdescription{ Topocentric apparent RA,Dec of a Solar-System object whose heliocentric orbital elements are known. } \sstinvocation{ void palPlante ( double date, double elong, double phi, int jform, double epoch, double orbinc, double anode, double perih, double aorq, double e, double aorl, double dm, double $*$ra, double $*$dec, double $*$r, int $*$jstat ); } \sstarguments{ \sstsubsection{ date = double (Given) }{ TT MJD of observation (JD-2400000.5) } \sstsubsection{ elong = double (Given) }{ Observer{\tt '}s east longitude (radians) } \sstsubsection{ phi = double (Given) }{ Observer{\tt '}s geodetic latitude (radians) } \sstsubsection{ jform = int (Given) }{ Element set actually returned (1-3; Note 6) } \sstsubsection{ epoch = double (Given) }{ Epoch of elements (TT MJD) } \sstsubsection{ orbinc = double (Given) }{ inclination (radians) } \sstsubsection{ anode = double (Given) }{ longitude of the ascending node (radians) } \sstsubsection{ perih = double (Given) }{ longitude or argument of perihelion (radians) } \sstsubsection{ aorq = double (Given) }{ mean distance or perihelion distance (AU) } \sstsubsection{ e = double (Given) }{ eccentricity } \sstsubsection{ aorl = double (Given) }{ mean anomaly or longitude (radians, JFORM=1,2 only) } \sstsubsection{ dm = double (Given) }{ daily motion (radians, JFORM=1 only) } \sstsubsection{ ra = double $*$ (Returned) }{ Topocentric apparent RA (radians) } \sstsubsection{ dec = double $*$ (Returned) }{ Topocentric apparent Dec (radians) } \sstsubsection{ r = double $*$ (Returned) }{ Distance from observer (AU) } \sstsubsection{ jstat = int $*$ (Returned) }{ status: 0 = OK \sstitemlist{ \sstitem -1 = illegal jform \sstitem -2 = illegal e \sstitem -3 = illegal aorq \sstitem -4 = illegal dm \sstitem -5 = numerical error } } } \sstnotes{ \sstitemlist{ \sstitem DATE is the instant for which the prediction is required. It is in the TT timescale (formerly Ephemeris Time, ET) and is a Modified Julian Date (JD-2400000.5). \sstitem The longitude and latitude allow correction for geocentric parallax. This is usually a small effect, but can become important for near-Earth asteroids. Geocentric positions can be generated by appropriate use of routines palEpv (or palEvp) and palUe2pv. \sstitem The elements are with respect to the J2000 ecliptic and equinox. \sstitem A choice of three different element-set options is available: } Option JFORM = 1, suitable for the major planets: EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = longitude of perihelion, curly pi (radians) AORQ = mean distance, a (AU) E = eccentricity, e (range 0 to $<$1) AORL = mean longitude L (radians) DM = daily motion (radians) Option JFORM = 2, suitable for minor planets: EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = mean distance, a (AU) E = eccentricity, e (range 0 to $<$1) AORL = mean anomaly M (radians) Option JFORM = 3, suitable for comets: EPOCH = epoch of elements and perihelion (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = perihelion distance, q (AU) E = eccentricity, e (range 0 to 10) Unused arguments (DM for JFORM=2, AORL and DM for JFORM=3) are not accessed. \sstitemlist{ \sstitem Each of the three element sets defines an unperturbed heliocentric orbit. For a given epoch of observation, the position of the body in its orbit can be predicted from these elements, which are called {\tt "}osculating elements{\tt "}, using standard two-body analytical solutions. However, due to planetary perturbations, a given set of osculating elements remains usable for only as long as the unperturbed orbit that it describes is an adequate approximation to reality. Attached to such a set of elements is a date called the {\tt "}osculating epoch{\tt "}, at which the elements are, momentarily, a perfect representation of the instantaneous position and velocity of the body. } Therefore, for any given problem there are up to three different epochs in play, and it is vital to distinguish clearly between them: . The epoch of observation: the moment in time for which the position of the body is to be predicted. . The epoch defining the position of the body: the moment in time at which, in the absence of purturbations, the specified position (mean longitude, mean anomaly, or perihelion) is reached. . The osculating epoch: the moment in time at which the given elements are correct. For the major-planet and minor-planet cases it is usual to make the epoch that defines the position of the body the same as the epoch of osculation. Thus, only two different epochs are involved: the epoch of the elements and the epoch of observation. For comets, the epoch of perihelion fixes the position in the orbit and in general a different epoch of osculation will be chosen. Thus, all three types of epoch are involved. For the present routine: . The epoch of observation is the argument DATE. . The epoch defining the position of the body is the argument EPOCH. . The osculating epoch is not used and is assumed to be close enough to the epoch of observation to deliver adequate accuracy. If not, a preliminary call to sla\_PERTEL may be used to update the element-set (and its associated osculating epoch) by applying planetary perturbations. \sstitemlist{ \sstitem Two important sources for orbital elements are Horizons, operated by the Jet Propulsion Laboratory, Pasadena, and the Minor Planet Center, operated by the Center for Astrophysics, Harvard. } The JPL Horizons elements (heliocentric, J2000 ecliptic and equinox) correspond to SLALIB arguments as follows. Major planets: JFORM = 1 EPOCH = JDCT-2400000.5 ORBINC = IN (in radians) ANODE = OM (in radians) PERIH = OM$+$W (in radians) AORQ = A E = EC AORL = MA$+$OM$+$W (in radians) DM = N (in radians) Epoch of osculation = JDCT-2400000.5 Minor planets: JFORM = 2 EPOCH = JDCT-2400000.5 ORBINC = IN (in radians) ANODE = OM (in radians) PERIH = W (in radians) AORQ = A E = EC AORL = MA (in radians) Epoch of osculation = JDCT-2400000.5 Comets: JFORM = 3 EPOCH = Tp-2400000.5 ORBINC = IN (in radians) ANODE = OM (in radians) PERIH = W (in radians) AORQ = QR E = EC Epoch of osculation = JDCT-2400000.5 The MPC elements correspond to SLALIB arguments as follows. Minor planets: JFORM = 2 EPOCH = Epoch-2400000.5 ORBINC = Incl. (in radians) ANODE = Node (in radians) PERIH = Perih. (in radians) AORQ = a E = e AORL = M (in radians) Epoch of osculation = Epoch-2400000.5 Comets: JFORM = 3 EPOCH = T-2400000.5 ORBINC = Incl. (in radians) ANODE = Node. (in radians) PERIH = Perih. (in radians) AORQ = q E = e Epoch of osculation = Epoch-2400000.5 } } sun267.htx/section54.tex000644 000765 000024 00000010145 12365763500 015401 0ustar00timjstaff000000 000000 \sstroutine{ palPlantu }{ Topocentric RA,Dec of a Solar-System object from universal elements }{ \sstdescription{ Topocentric apparent RA,Dec of a Solar-System object whose heliocentric universal elements are known. } \sstinvocation{ void palPlantu ( double date, double elong, double phi, const double u[13], double $*$ra, double $*$dec, double $*$r, int $*$jstat ) \{ } \sstarguments{ \sstsubsection{ date = double (Given) }{ TT MJD of observation (JD-2400000.5) } \sstsubsection{ elong = double (Given) }{ Observer{\tt '}s east longitude (radians) } \sstsubsection{ phi = double (Given) }{ Observer{\tt '}s geodetic latitude (radians) } \sstsubsection{ u = const double [13] (Given) }{ Universal orbital elements \sstitemlist{ \sstitem (0) combined mass (M$+$m) \sstitem (1) total energy of the orbit (alpha) \sstitem (2) reference (osculating) epoch (t0) \sstitem (3-5) position at reference epoch (r0) \sstitem (6-8) velocity at reference epoch (v0) \sstitem (9) heliocentric distance at reference epoch \sstitem (10) r0.v0 \sstitem (11) date (t) \sstitem (12) universal eccentric anomaly (psi) of date, approx } } \sstsubsection{ ra = double $*$ (Returned) }{ Topocentric apparent RA (radians) } \sstsubsection{ dec = double $*$ (Returned) }{ Topocentric apparent Dec (radians) } \sstsubsection{ r = double $*$ (Returned) }{ Distance from observer (AU) } \sstsubsection{ jstat = int $*$ (Returned) }{ status: 0 = OK \sstitemlist{ \sstitem -1 = radius vector zero \sstitem -2 = failed to converge } } } \sstnotes{ \sstitemlist{ \sstitem DATE is the instant for which the prediction is required. It is in the TT timescale (formerly Ephemeris Time, ET) and is a Modified Julian Date (JD-2400000.5). \sstitem The longitude and latitude allow correction for geocentric parallax. This is usually a small effect, but can become important for near-Earth asteroids. Geocentric positions can be generated by appropriate use of routines palEpv (or palEvp) and palUe2pv. \sstitem The {\tt "}universal{\tt "} elements are those which define the orbit for the purposes of the method of universal variables (see reference 2). They consist of the combined mass of the two bodies, an epoch, and the position and velocity vectors (arbitrary reference frame) at that epoch. The parameter set used here includes also various quantities that can, in fact, be derived from the other information. This approach is taken to avoiding unnecessary computation and loss of accuracy. The supplementary quantities are (i) alpha, which is proportional to the total energy of the orbit, (ii) the heliocentric distance at epoch, (iii) the outwards component of the velocity at the given epoch, (iv) an estimate of psi, the {\tt "}universal eccentric anomaly{\tt "} at a given date and (v) that date. \sstitem The universal elements are with respect to the J2000 equator and equinox. } } \sstdiytopic{ See Also }{ \sstitemlist{ \sstitem Sterne, Theodore E., {\tt "}An Introduction to Celestial Mechanics{\tt "}, Interscience Publishers Inc., 1960. Section 6.7, p199. \sstitem Everhart, E. \& Pitkin, E.T., Am.J.Phys. 51, 712, 1983. } } } sun267.htx/section55.tex000644 000765 000024 00000003553 12365763500 015407 0ustar00timjstaff000000 000000 \sstroutine{ palPm }{ Apply corrections for proper motion a star RA,Dec }{ \sstdescription{ Apply corrections for proper motion to a star RA,Dec using the SOFA routine iauStarpm. } \sstinvocation{ void palPm ( double r0, double d0, double pr, double pd, double px, double rv, double ep0, double ep1, double $*$r1, double $*$d1 ); } \sstarguments{ \sstsubsection{ r0 = double (Given) }{ RA at epoch ep0 (radians) } \sstsubsection{ d0 = double (Given) }{ Dec at epoch ep0 (radians) } \sstsubsection{ pr = double (Given) }{ RA proper motion in radians per year. } \sstsubsection{ pd = double (Given) }{ Dec proper motion in radians per year. } \sstsubsection{ px = double (Given) }{ Parallax (arcsec) } \sstsubsection{ rv = double (Given) }{ Radial velocity (km/sec $+$ve if receding) } \sstsubsection{ ep0 = double (Given) }{ Start epoch in years, assumed to be Julian. } \sstsubsection{ ep1 = double (Given) }{ End epoch in years, assumed to be Julian. } \sstsubsection{ r1 = double $*$ (Returned) }{ RA at epoch ep1 (radians) } \sstsubsection{ d1 = double $*$ (Returned) }{ Dec at epoch ep1 (radians) } } \sstnotes{ \sstitemlist{ \sstitem Uses iauStarpm but ignores the status returns from that routine. In particular note that parallax should not be zero when the proper motions are non-zero. SLA/F allows parallax to be zero. \sstitem Assumes all epochs are Julian epochs. } } } sun267.htx/section56.tex000644 000765 000024 00000001722 12365763500 015404 0ustar00timjstaff000000 000000 \sstroutine{ palPrebn }{ Generate the matrix of precession between two objects (old) }{ \sstdescription{ Generate the matrix of precession between two epochs, using the old, pre-IAU1976, Bessel-Newcomb model, using Kinoshita{\tt '}s formulation } \sstinvocation{ void palPrebn ( double bep0, double bep1, double rmatp[3][3] ); } \sstarguments{ \sstsubsection{ bep0 = double (Given) }{ Beginning Besselian epoch. } \sstsubsection{ bep1 = double (Given) }{ Ending Besselian epoch } \sstsubsection{ rmatp = double[3][3] (Returned) }{ precession matrix in the sense V(BEP1) = RMATP $*$ V(BEP0) } } \sstdiytopic{ See Also }{ Kinoshita, H. (1975) {\tt '}Formulas for precession{\tt '}, SAO Special Report No. 364, Smithsonian Institution Astrophysical Observatory, Cambridge, Massachusetts. } } sun267.htx/section57.tex000644 000765 000024 00000001655 12365763500 015412 0ustar00timjstaff000000 000000 \sstroutine{ palPrec }{ Form the matrix of precession between two epochs (IAU 2006) }{ \sstdescription{ The IAU 2006 precession matrix from ep0 to ep1 is found and returned. The matrix is in the sense V(EP1) = RMATP $*$ V(EP0). The epochs are TDB (loosely TT) Julian epochs. Though the matrix method itself is rigorous, the precession angles are expressed through canonical polynomials which are valid only for a limited time span of a few hundred years around the current epoch. } \sstinvocation{ palPrec( double ep0, double ep1, double rmatp[3][3] ) } \sstarguments{ \sstsubsection{ ep0 = double (Given) }{ Beginning epoch } \sstsubsection{ ep1 = double (Given) }{ Ending epoch } \sstsubsection{ rmatp = double[3][3] (Returned) }{ Precession matrix } } } sun267.htx/section58.tex000644 000765 000024 00000003571 12365763500 015412 0ustar00timjstaff000000 000000 \sstroutine{ palPreces }{ Precession - either FK4 or FK5 as required }{ \sstdescription{ Precess coordinates using the appropriate system and epochs. } \sstinvocation{ void palPreces ( const char sys[3], double ep0, double ep1, double $*$ra, double $*$dc ); } \sstarguments{ \sstsubsection{ sys = const char [3] (Given) }{ Precession to be applied: FK4 or FK5. Case insensitive. } \sstsubsection{ ep0 = double (Given) }{ Starting epoch. } \sstsubsection{ ep1 = double (Given) }{ Ending epoch } \sstsubsection{ ra = double $*$ (Given \& Returned) }{ On input the RA mean equator \& equinox at epoch ep0. On exit the RA mean equator \& equinox of epoch ep1. } \sstsubsection{ dec = double $*$ (Given \& Returned) }{ On input the dec mean equator \& equinox at epoch ep0. On exit the dec mean equator \& equinox of epoch ep1. } } \sstnotes{ \sstitemlist{ \sstitem Uses palPrec for FK5 data and palPrebn for FK4 data. \sstitem The epochs are Besselian if SYSTEM={\tt '}FK4{\tt '} and Julian if {\tt '}FK5{\tt '}. For example, to precess coordinates in the old system from equinox 1900.0 to 1950.0 the call would be: palPreces( {\tt "}FK4{\tt "}, 1900.0, 1950.0, \&ra, \&dc ); \sstitem This routine will NOT correctly convert between the old and the new systems - for example conversion from B1950 to J2000. For these purposes see palFk425, palFk524, palFk45z and palFk54z. \sstitem If an invalid SYSTEM is supplied, values of -99D0,-99D0 will be returned for both RA and DC. } } } sun267.htx/section59.tex000644 000765 000024 00000001453 12365763500 015410 0ustar00timjstaff000000 000000 \sstroutine{ palPrenut }{ Form the matrix of bias-precession-nutation (IAU 2006/2000A) }{ \sstdescription{ Form the matrix of bias-precession-nutation (IAU 2006/2000A). The epoch and date are TT (but TDB is usually close enough). The matrix is in the sense v(true) = rmatpn $*$ v(mean). } \sstinvocation{ void palPrenut( double epoch, double date, double rmatpn[3][3] ) } \sstarguments{ \sstsubsection{ epoch = double (Returned) }{ Julian epoch for mean coordinates. } \sstsubsection{ date = double (Returned) }{ Modified Julian Date (JD-2400000.5) for true coordinates. } \sstsubsection{ rmatpn = double[3][3] (Returned) }{ combined NPB matrix } } } sun267.htx/section6.tex000644 000765 000024 00000003233 12365763500 015316 0ustar00timjstaff000000 000000 \sstroutine{ palAirmas }{ Air mass at given zenith distance }{ \sstdescription{ Calculates the airmass at the observed zenith distance. } \sstinvocation{ double palAirmas( double zd ); } \sstarguments{ \sstsubsection{ zd = double (Given) }{ Observed zenith distance (radians) } } \sstnotes{ \sstitemlist{ \sstitem The {\tt "}observed{\tt "} zenith distance referred to above means {\tt "}as affected by refraction{\tt "}. \sstitem Uses Hardie{\tt '}s (1962) polynomial fit to Bemporad{\tt '}s data for the relative air mass, X, in units of thickness at the zenith as tabulated by Schoenberg (1929). This is adequate for all normal needs as it is accurate to better than 0.1\% up to X = 6.8 and better than 1\% up to X = 10. Bemporad{\tt '}s tabulated values are unlikely to be trustworthy to such accuracy because of variations in density, pressure and other conditions in the atmosphere from those assumed in his work. \sstitem The sign of the ZD is ignored. \sstitem At zenith distances greater than about ZD = 87 degrees the air mass is held constant to avoid arithmetic overflows. } } \sstdiytopic{ See Also }{ \sstitemlist{ \sstitem Hardie, R.H., 1962, in {\tt "}Astronomical Techniques{\tt "} ed. W.A. Hiltner, University of Chicago Press, p180. \sstitem Schoenberg, E., 1929, Hdb. d. Ap., Berlin, Julius Springer, 2, 268. } } } sun267.htx/section60.tex000644 000765 000024 00000016275 12365763500 015410 0ustar00timjstaff000000 000000 \sstroutine{ palPv2el }{ Position velocity to heliocentirc osculating elements }{ \sstdescription{ Heliocentric osculating elements obtained from instantaneous position and velocity. } \sstinvocation{ void palPv2el ( const double pv[6], double date, double pmass, int jformr, int $*$jform, double $*$epoch, double $*$orbinc, double $*$anode, double $*$perih, double $*$aorq, double $*$e, double $*$aorl, double $*$dm, int $*$jstat ); } \sstarguments{ \sstsubsection{ pv = const double [6] (Given) }{ Heliocentric x,y,z,xdot,ydot,zdot of date, J2000 equatorial triad (AU,AU/s; Note 1) } \sstsubsection{ date = double (Given) }{ Date (TT Modified Julian Date = JD-2400000.5) } \sstsubsection{ pmass = double (Given) }{ Mass of the planet (Sun=1; Note 2) } \sstsubsection{ jformr = int (Given) }{ Requested element set (1-3; Note 3) } \sstsubsection{ jform = int $*$ (Returned) }{ Element set actually returned (1-3; Note 4) } \sstsubsection{ epoch = double $*$ (Returned) }{ Epoch of elements (TT MJD) } \sstsubsection{ orbinc = double $*$ (Returned) }{ inclination (radians) } \sstsubsection{ anode = double $*$ (Returned) }{ longitude of the ascending node (radians) } \sstsubsection{ perih = double $*$ (Returned) }{ longitude or argument of perihelion (radians) } \sstsubsection{ aorq = double $*$ (Returned) }{ mean distance or perihelion distance (AU) } \sstsubsection{ e = double $*$ (Returned) }{ eccentricity } \sstsubsection{ aorl = double $*$ (Returned) }{ mean anomaly or longitude (radians, JFORM=1,2 only) } \sstsubsection{ dm = double $*$ (Returned) }{ daily motion (radians, JFORM=1 only) } \sstsubsection{ jstat = int $*$ (Returned) }{ status: 0 = OK \sstitemlist{ \sstitem -1 = illegal PMASS \sstitem -2 = illegal JFORMR \sstitem -3 = position/velocity out of range } } } \sstnotes{ \sstitemlist{ \sstitem The PV 6-vector is with respect to the mean equator and equinox of epoch J2000. The orbital elements produced are with respect to the J2000 ecliptic and mean equinox. \sstitem The mass, PMASS, is important only for the larger planets. For most purposes (e.g. asteroids) use 0D0. Values less than zero are illegal. \sstitem Three different element-format options are supported: } Option JFORM=1, suitable for the major planets: EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = longitude of perihelion, curly pi (radians) AORQ = mean distance, a (AU) E = eccentricity, e AORL = mean longitude L (radians) DM = daily motion (radians) Option JFORM=2, suitable for minor planets: EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = mean distance, a (AU) E = eccentricity, e AORL = mean anomaly M (radians) Option JFORM=3, suitable for comets: EPOCH = epoch of perihelion (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = perihelion distance, q (AU) E = eccentricity, e \sstitemlist{ \sstitem It may not be possible to generate elements in the form requested through JFORMR. The caller is notified of the form of elements actually returned by means of the JFORM argument: } JFORMR JFORM meaning 1 1 OK - elements are in the requested format 1 2 never happens 1 3 orbit not elliptical 2 1 never happens 2 2 OK - elements are in the requested format 2 3 orbit not elliptical 3 1 never happens 3 2 never happens 3 3 OK - elements are in the requested format \sstitemlist{ \sstitem The arguments returned for each value of JFORM (cf Note 5: JFORM may not be the same as JFORMR) are as follows: } JFORM 1 2 3 EPOCH t0 t0 T ORBINC i i i ANODE Omega Omega Omega PERIH curly pi omega omega AORQ a a q E e e e AORL L M - DM n - - where: t0 is the epoch of the elements (MJD, TT) T {\tt "} epoch of perihelion (MJD, TT) i {\tt "} inclination (radians) Omega {\tt "} longitude of the ascending node (radians) curly pi {\tt "} longitude of perihelion (radians) omega {\tt "} argument of perihelion (radians) a {\tt "} mean distance (AU) q {\tt "} perihelion distance (AU) e {\tt "} eccentricity L {\tt "} longitude (radians, 0-2pi) M {\tt "} mean anomaly (radians, 0-2pi) n {\tt "} daily motion (radians) \sstitemlist{ \sstitem means no value is set \sstitem At very small inclinations, the longitude of the ascending node ANODE becomes indeterminate and under some circumstances may be set arbitrarily to zero. Similarly, if the orbit is close to circular, the true anomaly becomes indeterminate and under some circumstances may be set arbitrarily to zero. In such cases, the other elements are automatically adjusted to compensate, and so the elements remain a valid description of the orbit. \sstitem The osculating epoch for the returned elements is the argument DATE. \sstitem Reference: Sterne, Theodore E., {\tt "}An Introduction to Celestial Mechanics{\tt "}, Interscience Publishers, 1960 } } } sun267.htx/section61.tex000644 000765 000024 00000006534 12365763500 015406 0ustar00timjstaff000000 000000 \sstroutine{ palPv2ue }{ Universal elements to position and velocity }{ \sstdescription{ Construct a universal element set based on an instantaneous position and velocity. } \sstinvocation{ void palPv2ue( const double pv[6], double date, double pmass, double u[13], int $*$ jstat ); } \sstarguments{ \sstsubsection{ pv = double [6] (Given) }{ Heliocentric x,y,z,xdot,ydot,zdot of date, (AU,AU/s; Note 1) } \sstsubsection{ date = double (Given) }{ Date (TT modified Julian Date = JD-2400000.5) } \sstsubsection{ pmass = double (Given) }{ Mass of the planet (Sun=1; note 2) } \sstsubsection{ u = double [13] (Returned) }{ Universal orbital elements (Note 3) \sstitemlist{ \sstitem (0) combined mass (M$+$m) \sstitem (1) total energy of the orbit (alpha) \sstitem (2) reference (osculating) epoch (t0) \sstitem (3-5) position at reference epoch (r0) \sstitem (6-8) velocity at reference epoch (v0) \sstitem (9) heliocentric distance at reference epoch \sstitem (10) r0.v0 \sstitem (11) date (t) \sstitem (12) universal eccentric anomaly (psi) of date, approx } } \sstsubsection{ jstat = int $*$ (Returned) }{ status: 0 = OK \sstitemlist{ \sstitem -1 = illegal PMASS \sstitem -2 = too close to Sun \sstitem -3 = too slow } } } \sstnotes{ \sstitemlist{ \sstitem The PV 6-vector can be with respect to any chosen inertial frame, and the resulting universal-element set will be with respect to the same frame. A common choice will be mean equator and ecliptic of epoch J2000. \sstitem The mass, PMASS, is important only for the larger planets. For most purposes (e.g. asteroids) use 0D0. Values less than zero are illegal. \sstitem The {\tt "}universal{\tt "} elements are those which define the orbit for the purposes of the method of universal variables (see reference). They consist of the combined mass of the two bodies, an epoch, and the position and velocity vectors (arbitrary reference frame) at that epoch. The parameter set used here includes also various quantities that can, in fact, be derived from the other information. This approach is taken to avoiding unnecessary computation and loss of accuracy. The supplementary quantities are (i) alpha, which is proportional to the total energy of the orbit, (ii) the heliocentric distance at epoch, (iii) the outwards component of the velocity at the given epoch, (iv) an estimate of psi, the {\tt "}universal eccentric anomaly{\tt "} at a given date and (v) that date. \sstitem Reference: Everhart, E. \& Pitkin, E.T., Am.J.Phys. 51, 712, 1983. } } } sun267.htx/section62.tex000644 000765 000024 00000001657 12365763500 015410 0ustar00timjstaff000000 000000 \sstroutine{ palPvobs }{ Position and velocity of an observing station }{ \sstdescription{ Returns the position and velocity of an observing station. } \sstinvocation{ palPvobs( double p, double h, double stl, double pv[6] ) } \sstarguments{ \sstsubsection{ p = double (Given) }{ Latitude (geodetic, radians). } \sstsubsection{ h = double (Given) }{ Height above reference spheroid (geodetic, metres). } \sstsubsection{ stl = double (Given) }{ Local apparent sidereal time (radians). } \sstsubsection{ pv = double[ 6 ] (Returned) }{ position/velocity 6-vector (AU, AU/s, true equator and equinox of date). } } \sstnotes{ \sstitemlist{ \sstitem The WGS84 reference ellipsoid is used. } } } sun267.htx/section63.tex000644 000765 000024 00000004117 12365763500 015403 0ustar00timjstaff000000 000000 \sstroutine{ palRdplan }{ Approximate topocentric apparent RA,Dec of a planet }{ \sstdescription{ Approximate topocentric apparent RA,Dec of a planet, and its angular diameter. } \sstinvocation{ void palRdplan( double date, int np, double elong, double phi, double $*$ ra, double $*$ dec, double $*$ diam ); } \sstarguments{ \sstsubsection{ date = double (Given) }{ MJD of observation (JD-2400000.5) in TDB. For all practical purposes TT can be used instead of TDB, and for many applications UT will do (except for the Moon). } \sstsubsection{ np = int (Given) }{ Planet: 1 = Mercury 2 = Venus 3 = Moon 4 = Mars 5 = Jupiter 6 = Saturn 7 = Uranus 8 = Neptune else = Sun } \sstsubsection{ elong = double (Given) }{ Observer{\tt '}s east longitude (radians) } \sstsubsection{ phi = double (Given) }{ Observer{\tt '}s geodetic latitude (radians) } \sstsubsection{ ra = double $*$ (Returned) }{ RA (topocentric apparent, radians) } \sstsubsection{ dec = double $*$ (Returned) }{ Dec (topocentric apparent, radians) } \sstsubsection{ diam = double $*$ (Returned) }{ Angular diameter (equatorial, radians) } } \sstnotes{ \sstitemlist{ \sstitem Unlike with slaRdplan, Pluto is not supported. \sstitem The longitude and latitude allow correction for geocentric parallax. This is a major effect for the Moon, but in the context of the limited accuracy of the present routine its effect on planetary positions is small (negligible for the outer planets). Geocentric positions can be generated by appropriate use of the routines palDmoon and iauPlan94. } } } sun267.htx/section64.tex000644 000765 000024 00000002365 12365763500 015407 0ustar00timjstaff000000 000000 \sstroutine{ palRverot }{ Velocity component in a given direction due to Earth rotation }{ \sstdescription{ Calculate the velocity component in a given direction due to Earth rotation. The simple algorithm used assumes a spherical Earth, of a radius chosen to give results accurate to about 0.0005 km/s for observing stations at typical latitudes and heights. For applications requiring greater precision, use the routine palPvobs. } \sstinvocation{ double palRverot ( double phi, double ra, double da, double st ); } \sstarguments{ \sstsubsection{ phi = double (Given) }{ latitude of observing station (geodetic) (radians) } \sstsubsection{ ra = double (Given) }{ apparent RA (radians) } \sstsubsection{ da = double (Given) }{ apparent Dec (radians) } \sstsubsection{ st = double (Given) }{ } } \sstreturnedvalue{ \sstsubsection{ palRverot = double }{ Component of Earth rotation in direction RA,DA (km/s). The result is $+$ve when the observatory is receding from the given point on the sky. } } } sun267.htx/section65.tex000644 000765 000024 00000002644 12365763500 015410 0ustar00timjstaff000000 000000 \sstroutine{ palRvgalc }{ Velocity component in a given direction due to the rotation of the Galaxy }{ \sstdescription{ This function returns the Component of dynamical LSR motion in the direction of R2000,D2000. The result is $+$ve when the dynamical LSR is receding from the given point on the sky. } \sstinvocation{ double palRvgalc( double r2000, double d2000 ) } \sstarguments{ \sstsubsection{ r2000 = double (Given) }{ J2000.0 mean RA (radians) } \sstsubsection{ d2000 = double (Given) }{ J2000.0 mean Dec (radians) } } \sstreturnedvalue{ \sstsubsection{ Component of dynamical LSR motion in direction R2000,D2000 (km/s). }{ } } \sstnotes{ \sstitemlist{ \sstitem The Local Standard of Rest used here is a point in the vicinity of the Sun which is in a circular orbit around the Galactic centre. Sometimes called the {\tt "}dynamical{\tt "} LSR, it is not to be confused with a {\tt "}kinematical{\tt "} LSR, which is the mean standard of rest of star catalogues or stellar populations. } } \sstdiytopic{ Reference }{ \sstitemlist{ \sstitem The orbital speed of 220 km/s used here comes from Kerr \& Lynden-Bell (1986), MNRAS, 221, p1023. } } } sun267.htx/section66.tex000644 000765 000024 00000002012 12365763500 015376 0ustar00timjstaff000000 000000 \sstroutine{ palRvlg }{ Velocity component in a given direction due to Galactic rotation and motion of the local group }{ \sstdescription{ This function returns the velocity component in a given direction due to the combination of the rotation of the Galaxy and the motion of the Galaxy relative to the mean motion of the local group. The result is $+$ve when the Sun is receding from the given point on the sky. } \sstinvocation{ double palRvlg( double r2000, double d2000 ) } \sstarguments{ \sstsubsection{ r2000 = double (Given) }{ J2000.0 mean RA (radians) } \sstsubsection{ d2000 = double (Given) }{ J2000.0 mean Dec (radians) } } \sstreturnedvalue{ \sstsubsection{ Component of SOLAR motion in direction R2000,D2000 (km/s). }{ } } \sstdiytopic{ Reference }{ \sstitemlist{ \sstitem IAU Trans 1976, 168, p201. } } } sun267.htx/section67.tex000644 000765 000024 00000003721 12365763500 015407 0ustar00timjstaff000000 000000 \sstroutine{ palRvlsrd }{ Velocity component in a given direction due to the Sun{\tt '}s motion with respect to the dynamical Local Standard of Rest }{ \sstdescription{ This function returns the velocity component in a given direction due to the Sun{\tt '}s motion with respect to the dynamical Local Standard of Rest. The result is $+$ve when the Sun is receding from the given point on the sky. } \sstinvocation{ double palRvlsrd( double r2000, double d2000 ) } \sstarguments{ \sstsubsection{ r2000 = double (Given) }{ J2000.0 mean RA (radians) } \sstsubsection{ d2000 = double (Given) }{ J2000.0 mean Dec (radians) } } \sstreturnedvalue{ \sstsubsection{ Component of {\tt "}peculiar{\tt "} solar motion in direction R2000,D2000 (km/s). }{ } } \sstnotes{ \sstitemlist{ \sstitem The Local Standard of Rest used here is the {\tt "}dynamical{\tt "} LSR, a point in the vicinity of the Sun which is in a circular orbit around the Galactic centre. The Sun{\tt '}s motion with respect to the dynamical LSR is called the {\tt "}peculiar{\tt "} solar motion. \sstitem There is another type of LSR, called a {\tt "}kinematical{\tt "} LSR. A kinematical LSR is the mean standard of rest of specified star catalogues or stellar populations, and several slightly different kinematical LSRs are in use. The Sun{\tt '}s motion with respect to an agreed kinematical LSR is known as the {\tt "}standard{\tt "} solar motion. To obtain a radial velocity correction with respect to an adopted kinematical LSR use the routine sla\_RVLSRK. } } \sstdiytopic{ Reference }{ \sstitemlist{ \sstitem Delhaye (1965), in {\tt "}Stars and Stellar Systems{\tt "}, vol 5, p73. } } } sun267.htx/section68.tex000644 000765 000024 00000003661 12365763500 015413 0ustar00timjstaff000000 000000 \sstroutine{ palRvlsrk }{ Velocity component in a given direction due to the Sun{\tt '}s motion with respect to an adopted kinematic Local Standard of Rest }{ \sstdescription{ This function returns the velocity component in a given direction due to the Sun{\tt '}s motion with respect to an adopted kinematic Local Standard of Rest. The result is $+$ve when the Sun is receding from the given point on the sky. } \sstinvocation{ double palRvlsrk( double r2000, double d2000 ) } \sstarguments{ \sstsubsection{ r2000 = double (Given) }{ J2000.0 mean RA (radians) } \sstsubsection{ d2000 = double (Given) }{ J2000.0 mean Dec (radians) } } \sstreturnedvalue{ \sstsubsection{ Component of {\tt "}standard{\tt "} solar motion in direction R2000,D2000 (km/s). }{ } } \sstnotes{ \sstitemlist{ \sstitem The Local Standard of Rest used here is one of several {\tt "}kinematical{\tt "} LSRs in common use. A kinematical LSR is the mean standard of rest of specified star catalogues or stellar populations. The Sun{\tt '}s motion with respect to a kinematical LSR is known as the {\tt "}standard{\tt "} solar motion. \sstitem There is another sort of LSR, the {\tt "}dynamical{\tt "} LSR, which is a point in the vicinity of the Sun which is in a circular orbit around the Galactic centre. The Sun{\tt '}s motion with respect to the dynamical LSR is called the {\tt "}peculiar{\tt "} solar motion. To obtain a radial velocity correction with respect to the dynamical LSR use the routine sla\_RVLSRD. } } \sstdiytopic{ Reference }{ \sstitemlist{ \sstitem Delhaye (1965), in {\tt "}Stars and Stellar Systems{\tt "}, vol 5, p73. } } } sun267.htx/section69.tex000644 000765 000024 00000002573 12365763500 015415 0ustar00timjstaff000000 000000 \sstroutine{ palSubet }{ Remove the E-terms from a pre IAU 1976 catalogue RA,Dec }{ \sstdescription{ Remove the E-terms (elliptic component of annual aberration) from a pre IAU 1976 catalogue RA,Dec to give a mean place. } \sstinvocation{ void palSubet ( double rc, double dc, double eq, double $*$rm, double $*$dm ); } \sstarguments{ \sstsubsection{ rc = double (Given) }{ RA with E-terms included (radians) } \sstsubsection{ dc = double (Given) }{ Dec with E-terms included (radians) } \sstsubsection{ eq = double (Given) }{ Besselian epoch of mean equator and equinox } \sstsubsection{ rm = double $*$ (Returned) }{ RA without E-terms (radians) } \sstsubsection{ dm = double $*$ (Returned) }{ Dec without E-terms (radians) } } \sstnotes{ Most star positions from pre-1984 optical catalogues (or derived from astrometry using such stars) embody the E-terms. This routine converts such a position to a formal mean place (allowing, for example, comparison with a pulsar timing position). } \sstdiytopic{ See Also }{ Explanatory Supplement to the Astronomical Ephemeris, section 2D, page 48. } } sun267.htx/section7.tex000644 000765 000024 00000002227 12365763500 015321 0ustar00timjstaff000000 000000 \sstroutine{ palAmp }{ Convert star RA,Dec from geocentric apparaent to mean place }{ \sstdescription{ Convert star RA,Dec from geocentric apparent to mean place. The mean coordinate system is close to ICRS. See palAmpqk for details. } \sstinvocation{ void palAmp ( double ra, double da, double date, double eq, double $*$rm, double $*$dm ); } \sstarguments{ \sstsubsection{ ra = double (Given) }{ Apparent RA (radians) } \sstsubsection{ dec = double (Given) }{ Apparent Dec (radians) } \sstsubsection{ date = double (Given) }{ TDB for apparent place (JD-2400000.5) } \sstsubsection{ eq = double (Given) }{ Equinox: Julian epoch of mean place. } \sstsubsection{ rm = double $*$ (Returned) }{ Mean RA (radians) } \sstsubsection{ dm = double $*$ (Returned) }{ Mean Dec (radians) } } \sstnotes{ \sstitemlist{ \sstitem See palMappa and palAmpqk for details. } } } sun267.htx/section70.tex000644 000765 000024 00000002460 12365763500 015400 0ustar00timjstaff000000 000000 \sstroutine{ palSupgal }{ Convert from supergalactic to galactic coordinates }{ \sstdescription{ Transformation from de Vaucouleurs supergalactic coordinates to IAU 1958 galactic coordinates } \sstinvocation{ void palSupgal ( double dsl, double dsb, double $*$dl, double $*$db ); } \sstarguments{ \sstsubsection{ dsl = double (Given) }{ Supergalactic longitude. } \sstsubsection{ dsb = double (Given) }{ Supergalactic latitude. } \sstsubsection{ dl = double $*$ (Returned) }{ Galactic longitude. } \sstsubsection{ db = double $*$ (Returned) }{ Galactic latitude. } } \sstdiytopic{ See Also }{ \sstitemlist{ \sstitem de Vaucouleurs, de Vaucouleurs, \& Corwin, Second Reference Catalogue of Bright Galaxies, U. Texas, page 8. \sstitem Systems \& Applied Sciences Corp., Documentation for the machine-readable version of the above catalogue, Contract NAS 5-26490. } (These two references give different values for the galactic longitude of the supergalactic origin. Both are wrong; the correct value is L2=137.37.) } } sun267.htx/section71.tex000644 000765 000024 00000020422 12365763500 015377 0ustar00timjstaff000000 000000 \sstroutine{ palUe2el }{ Universal elements to heliocentric osculating elements }{ \sstdescription{ Transform universal elements into conventional heliocentric osculating elements. } \sstinvocation{ void palUe2el ( const double u[13], int jformr, int $*$jform, double $*$epoch, double $*$orbinc, double $*$anode, double $*$perih, double $*$aorq, double $*$e, double $*$aorl, double $*$dm, int $*$jstat ); } \sstarguments{ \sstsubsection{ u = const double [13] (Given) }{ Universal orbital elements (Note 1) (0) combined mass (M$+$m) (1) total energy of the orbit (alpha) (2) reference (osculating) epoch (t0) (3-5) position at reference epoch (r0) (6-8) velocity at reference epoch (v0) (9) heliocentric distance at reference epoch (10) r0.v0 (11) date (t) (12) universal eccentric anomaly (psi) of date, approx } \sstsubsection{ jformr = int (Given) }{ Requested element set (1-3; Note 3) } \sstsubsection{ jform = int $*$ (Returned) }{ Element set actually returned (1-3; Note 4) } \sstsubsection{ epoch = double $*$ (Returned) }{ Epoch of elements (TT MJD) } \sstsubsection{ orbinc = double $*$ (Returned) }{ inclination (radians) } \sstsubsection{ anode = double $*$ (Returned) }{ longitude of the ascending node (radians) } \sstsubsection{ perih = double $*$ (Returned) }{ longitude or argument of perihelion (radians) } \sstsubsection{ aorq = double $*$ (Returned) }{ mean distance or perihelion distance (AU) } \sstsubsection{ e = double $*$ (Returned) }{ eccentricity } \sstsubsection{ aorl = double $*$ (Returned) }{ mean anomaly or longitude (radians, JFORM=1,2 only) } \sstsubsection{ dm = double $*$ (Returned) }{ daily motion (radians, JFORM=1 only) } \sstsubsection{ jstat = int $*$ (Returned) }{ status: 0 = OK \sstitemlist{ \sstitem 1 = illegal combined mass \sstitem 2 = illegal JFORMR \sstitem 3 = position/velocity out of range } } } \sstnotes{ \sstitemlist{ \sstitem The {\tt "}universal{\tt "} elements are those which define the orbit for the purposes of the method of universal variables (see reference 2). They consist of the combined mass of the two bodies, an epoch, and the position and velocity vectors (arbitrary reference frame) at that epoch. The parameter set used here includes also various quantities that can, in fact, be derived from the other information. This approach is taken to avoiding unnecessary computation and loss of accuracy. The supplementary quantities are (i) alpha, which is proportional to the total energy of the orbit, (ii) the heliocentric distance at epoch, (iii) the outwards component of the velocity at the given epoch, (iv) an estimate of psi, the {\tt "}universal eccentric anomaly{\tt "} at a given date and (v) that date. \sstitem The universal elements are with respect to the mean equator and equinox of epoch J2000. The orbital elements produced are with respect to the J2000 ecliptic and mean equinox. \sstitem Three different element-format options are supported: } Option JFORM=1, suitable for the major planets: EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = longitude of perihelion, curly pi (radians) AORQ = mean distance, a (AU) E = eccentricity, e AORL = mean longitude L (radians) DM = daily motion (radians) Option JFORM=2, suitable for minor planets: EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = mean distance, a (AU) E = eccentricity, e AORL = mean anomaly M (radians) Option JFORM=3, suitable for comets: EPOCH = epoch of perihelion (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = perihelion distance, q (AU) E = eccentricity, e \sstitemlist{ \sstitem It may not be possible to generate elements in the form requested through JFORMR. The caller is notified of the form of elements actually returned by means of the JFORM argument: } JFORMR JFORM meaning 1 1 OK - elements are in the requested format 1 2 never happens 1 3 orbit not elliptical 2 1 never happens 2 2 OK - elements are in the requested format 2 3 orbit not elliptical 3 1 never happens 3 2 never happens 3 3 OK - elements are in the requested format \sstitemlist{ \sstitem The arguments returned for each value of JFORM (cf Note 6: JFORM may not be the same as JFORMR) are as follows: } JFORM 1 2 3 EPOCH t0 t0 T ORBINC i i i ANODE Omega Omega Omega PERIH curly pi omega omega AORQ a a q E e e e AORL L M - DM n - - where: t0 is the epoch of the elements (MJD, TT) T {\tt "} epoch of perihelion (MJD, TT) i {\tt "} inclination (radians) Omega {\tt "} longitude of the ascending node (radians) curly pi {\tt "} longitude of perihelion (radians) omega {\tt "} argument of perihelion (radians) a {\tt "} mean distance (AU) q {\tt "} perihelion distance (AU) e {\tt "} eccentricity L {\tt "} longitude (radians, 0-2pi) M {\tt "} mean anomaly (radians, 0-2pi) n {\tt "} daily motion (radians) \sstitemlist{ \sstitem means no value is set \sstitem At very small inclinations, the longitude of the ascending node ANODE becomes indeterminate and under some circumstances may be set arbitrarily to zero. Similarly, if the orbit is close to circular, the true anomaly becomes indeterminate and under some circumstances may be set arbitrarily to zero. In such cases, the other elements are automatically adjusted to compensate, and so the elements remain a valid description of the orbit. } See Also: \sstitemlist{ \sstitem Sterne, Theodore E., {\tt "}An Introduction to Celestial Mechanics{\tt "}, Interscience Publishers Inc., 1960. Section 6.7, p199. \sstitem Everhart, E. \& Pitkin, E.T., Am.J.Phys. 51, 712, 1983. } } } sun267.htx/section72.tex000644 000765 000024 00000010007 12365763500 015376 0ustar00timjstaff000000 000000 \sstroutine{ palUe2pv }{ Heliocentric position and velocity of a planet, asteroid or comet, from universal elements }{ \sstdescription{ Heliocentric position and velocity of a planet, asteroid or comet, starting from orbital elements in the {\tt "}universal variables{\tt "} form. } \sstinvocation{ void palUe2pv( double date, double u[13], double pv[6], int $*$jstat ); } \sstarguments{ \sstsubsection{ date = double (Given) }{ TT Modified Julian date (JD-2400000.5). } \sstsubsection{ u = double [13] (Given \& Returned) }{ Universal orbital elements (updated, see note 1) given (0) combined mass (M$+$m) {\tt "} (1) total energy of the orbit (alpha) {\tt "} (2) reference (osculating) epoch (t0) {\tt "} (3-5) position at reference epoch (r0) {\tt "} (6-8) velocity at reference epoch (v0) {\tt "} (9) heliocentric distance at reference epoch {\tt "} (10) r0.v0 returned (11) date (t) {\tt "} (12) universal eccentric anomaly (psi) of date } \sstsubsection{ jstat = int $*$ (Returned) }{ status: 0 = OK \sstitemlist{ \sstitem 1 = radius vector zero \sstitem 2 = failed to converge } } } \sstnotes{ \sstitemlist{ \sstitem The {\tt "}universal{\tt "} elements are those which define the orbit for the purposes of the method of universal variables (see reference). They consist of the combined mass of the two bodies, an epoch, and the position and velocity vectors (arbitrary reference frame) at that epoch. The parameter set used here includes also various quantities that can, in fact, be derived from the other information. This approach is taken to avoiding unnecessary computation and loss of accuracy. The supplementary quantities are (i) alpha, which is proportional to the total energy of the orbit, (ii) the heliocentric distance at epoch, (iii) the outwards component of the velocity at the given epoch, (iv) an estimate of psi, the {\tt "}universal eccentric anomaly{\tt "} at a given date and (v) that date. \sstitem The companion routine is palEl2ue. This takes the conventional orbital elements and transforms them into the set of numbers needed by the present routine. A single prediction requires one one call to palEl2ue followed by one call to the present routine; for convenience, the two calls are packaged as the routine sla\_PLANEL. Multiple predictions may be made by again calling palEl2ue once, but then calling the present routine multiple times, which is faster than multiple calls to palPlanel. \sstitem It is not obligatory to use palEl2ue to obtain the parameters. However, it should be noted that because palEl2ue performs its own validation, no checks on the contents of the array U are made by the present routine. in the TT timescale (formerly Ephemeris Time, ET) and is a Modified Julian Date (JD-2400000.5). units (solar masses, AU and canonical days). The position and velocity are not sensitive to the choice of reference frame. The palEl2ue routine in fact produces coordinates with respect to the J2000 equator and equinox. \sstitem The algorithm was originally adapted from the EPHSLA program of D.H.P.Jones (private communication, 1996). The method is based on Stumpff{\tt '}s Universal Variables. \sstitem Reference: Everhart, E. \& Pitkin, E.T., Am.J.Phys. 51, 712, 1983. } } } % ? End of main text \end{document} sun267.htx/section8.tex000644 000765 000024 00000003035 12365763500 015320 0ustar00timjstaff000000 000000 \sstroutine{ palAmpqk }{ Convert star RA,Dec from geocentric apparent to mean place }{ \sstdescription{ Convert star RA,Dec from geocentric apparent to mean place. The {\tt "}mean{\tt "} coordinate system is in fact close to ICRS. Use of this function is appropriate when efficiency is important and where many star positions are all to be transformed for one epoch and equinox. The star-independent parameters can be obtained by calling the palMappa function. } \sstinvocation{ void palAmpqk ( double ra, double da, double amprms[21], double $*$rm, double $*$dm ) } \sstarguments{ \sstsubsection{ ra = double (Given) }{ Apparent RA (radians). } \sstsubsection{ da = double (Given) }{ Apparent Dec (radians). } \sstsubsection{ amprms = double[21] (Given) }{ Star-independent mean-to-apparent parameters (see palMappa): (0) time interval for proper motion (Julian years) (1-3) barycentric position of the Earth (AU) (4-6) not used (7) not used (8-10) abv: barycentric Earth velocity in units of c (11) sqrt(1-v$*$v) where v=modulus(abv) (12-20) precession/nutation (3,3) matrix } \sstsubsection{ rm = double (Returned) }{ Mean RA (radians). } \sstsubsection{ dm = double (Returned) }{ Mean Dec (radians). } } } sun267.htx/section9.tex000644 000765 000024 00000003034 12365763500 015320 0ustar00timjstaff000000 000000 \sstroutine{ palCaldj }{ Gregorian Calendar to Modified Julian Date }{ \sstdescription{ Modified Julian Date to Gregorian Calendar with special behaviour for 2-digit years relating to 1950 to 2049. } \sstinvocation{ void palCaldj ( int iy, int im, int id, double $*$djm, int $*$j ); } \sstarguments{ \sstsubsection{ iy = int (Given) }{ Year in the Gregorian calendar } \sstsubsection{ im = int (Given) }{ Month in the Gergorian calendar } \sstsubsection{ id = int (Given) }{ Day in the Gregorian calendar } \sstsubsection{ djm = double $*$ (Returned) }{ Modified Julian Date (JD-2400000.5) for 0 hrs } \sstsubsection{ j = status (Returned) }{ 0 = OK. See iauCal2jd for other values. } } \sstnotes{ \sstitemlist{ \sstitem Uses iauCal2jd \sstitem Unlike iauCal2jd this routine treats the years 0-100 as referring to the end of the 20th Century and beginning of the 21st Century. If this behaviour is not acceptable use the SOFA routine directly or palCldj. Acceptable years are 00-49, interpreted as 2000-2049, 50-99, {\tt "} {\tt "} 1950-1999, all others, interpreted literally. \sstitem Unlike SLA this routine will work with negative years. } } } sun267.htx/source.gif000644 000765 000024 00000000301 12365763733 015032 0ustar00timjstaff000000 000000 GIF89a　€½½½¿¿¿ÀÀÀÁÁÁÂÂÂøüøÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿÿ,vÉI«½8çÀ»ÿ`0‰š&bQ€jëªÂ)¥+ŽoŒ"*9#\K÷ëE¡œ È«ÙlÁá’†ô<£"Óx­Þ²Ó¦—s‰j©•1îÊì°öÆ‹BŸí¾Í‡Ìms‚`rƒsg1Š‹ŒSŽŽ>”u%—˜™;sun267.htx/star2html.perl000644 000765 000024 00000002323 12365763500 015645 0ustar00timjstaff000000 000000 package main; # The base name for all document cross reference roots. # For local documents this would be: # $DOCBASE = '/star/docs/'; # And for remote documents at RAL: $DOCBASE = 'http://www.starlink.ac.uk/cgi-bin/htxserver/'; sub do_cmd_xref{ my $arg = shift; my ($text, $docname, $label); $arg =~ s/$next_pair_pr_rx/$text = $2; ''/eo; $arg =~ s/$next_pair_pr_rx/$docname = $2; ''/eo; $arg =~ s/$next_pair_pr_rx/$label = $2; ''/eo; # Default for local documents would be: #join('','',$text,'',$arg); # And for remote ones (notice?). join('','',$text,'',$arg); } sub do_cmd_xlabel{ local($_) = @_; my $label; s/$next_pair_pr_rx/$label = $2; ''/eo; $label =~ s/\n//g; $label =~ s/ //g; $label =~ s/\t//g; $label = 'xref_' . $label; &anchor_label( $label, $CURRENT_FILE, $_); } sub do_env_quote { join('',"
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"); } 1;# This must be the last line sun267.htx/star2html.sty000644 000765 000024 00000000000 12365763500 015510 0ustar00timjstaff000000 000000 sun267.htx/sun267.css000644 000765 000024 00000001573 12365763733 014635 0ustar00timjstaff000000 000000 /* Century Schoolbook font is very similar to Computer Modern Math: cmmi */ .MATH { font-family: "Century Schoolbook", serif; } .MATH I { font-family: "Century Schoolbook", serif; font-style: italic } .BOLDMATH { font-family: "Century Schoolbook", serif; font-weight: bold } /* implement both fixed-size and relative sizes */ SMALL.XTINY { font-size : xx-small } SMALL.TINY { font-size : x-small } SMALL.SCRIPTSIZE { font-size : smaller } SMALL.FOOTNOTESIZE { font-size : small } SMALL.SMALL { } BIG.LARGE { } BIG.XLARGE { font-size : large } BIG.XXLARGE { font-size : x-large } BIG.HUGE { font-size : larger } BIG.XHUGE { font-size : xx-large } /* heading styles */ H1 { } H2 { } H3 { } H4 { } H5 { } /* mathematics styles */ DIV.displaymath { } /* math displays */ TD.eqno { } /* equation-number cells */ /* document-specific styles come next */ sun267.htx/sun267.html000644 000765 000024 00000026727 12365763733 015021 0ustar00timjstaff000000 000000 PAL -- Positional Astronomy Library
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PAL -- Positional Astronomy Library
0.1.0
Programmer's Manual

Starlink User Note 267.1
Tim Jenness
2012 March 23

Joint Astronomy Centre
Science & Technology Facilities Council

Starlink Project

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PAL --- Positional Astronomy Library
Starlink User Note 267
Tim Jenness
2012 March 23
E-mail:starlink@jiscmail.ac.uk

Copyright © 2012 Science and Technology Facilities Council
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Specify used packages % \usepackage{graphicx} % Use this one for final production. % \usepackage[draft]{graphicx} % Use this one for drafting. % ? End of specify used packages \pagestyle{myheadings} % ----------------------------------------------------------------------------- % ? Document identification % Fixed part \newcommand{\stardoccategory} {Starlink User Note} \newcommand{\stardocinitials} {SUN} \newcommand{\stardocsource} {sun\stardocnumber} \newcommand{\stardoccopyright} {Copyright \copyright\ 2012 Science and Technology Facilities Council} % Variable part - replace [xxx] as appropriate. \newcommand{\stardocnumber} {267.1} \newcommand{\stardocauthors} {Tim Jenness} \newcommand{\stardocdate} {2012 March 23} \newcommand{\stardoctitle} {PAL --- Positional Astronomy Library} \newcommand{\stardocversion} {0.1.0} \newcommand{\stardocmanual} {Programmer's Manual} \newcommand{\stardocabstract} { PAL provides a subset of the Fortran SLALIB library but written in C using the SLALIB C API. Where possible the PAL routines are implemented using the C SOFA library. It is provided with a GPL license. } % ? End of document identification % ----------------------------------------------------------------------------- % + % Name: % sun.tex % % Purpose: % Template for Starlink User Note (SUN) documents. % Refer to SUN/199 % % Authors: % AJC: A.J.Chipperfield (Starlink, RAL) % BLY: M.J.Bly (Starlink, RAL) % PWD: Peter W. Draper (Starlink, Durham University) % % History: % 17-JAN-1996 (AJC): % Original with hypertext macros, based on MDL plain originals. % 16-JUN-1997 (BLY): % Adapted for LaTeX2e. % Added picture commands. % 13-AUG-1998 (PWD): % Converted for use with LaTeX2HTML version 98.2 and % Star2HTML version 1.3. % 1-FEB-2000 (AJC): % Add Copyright statement in LaTeX % {Add further history here} % % - \newcommand{\stardocname}{\stardocinitials /\stardocnumber} \markboth{\stardocname}{\stardocname} \setlength{\textwidth}{160mm} \setlength{\textheight}{230mm} \setlength{\topmargin}{-2mm} \setlength{\oddsidemargin}{0mm} \setlength{\evensidemargin}{0mm} \setlength{\parindent}{0mm} \setlength{\parskip}{\medskipamount} \setlength{\unitlength}{1mm} % ----------------------------------------------------------------------------- % Hypertext definitions. % ====================== % These are used by the LaTeX2HTML translator in conjunction with star2html. % Comment.sty: version 2.0, 19 June 1992 % Selectively in/exclude pieces of text. % % Author % Victor Eijkhout % Department of Computer Science % University Tennessee at Knoxville % 104 Ayres Hall % Knoxville, TN 37996 % USA % Do not remove the %begin{latexonly} and %end{latexonly} lines (used by % LaTeX2HTML to signify text it shouldn't process). %begin{latexonly} \makeatletter \def\makeinnocent#1{\catcode`#1=12 } \def\csarg#1#2{\expandafter#1\csname#2\endcsname} \def\ThrowAwayComment#1{\begingroup \def\CurrentComment{#1}% \let\do\makeinnocent \dospecials \makeinnocent\^^L% and whatever other special cases \endlinechar`\^^M \catcode`\^^M=12 \xComment} {\catcode`\^^M=12 \endlinechar=-1 % \gdef\xComment#1^^M{\def\test{#1} \csarg\ifx{PlainEnd\CurrentComment Test}\test \let\html@next\endgroup \else \csarg\ifx{LaLaEnd\CurrentComment Test}\test \edef\html@next{\endgroup\noexpand\end{\CurrentComment}} \else \let\html@next\xComment \fi \fi \html@next} } \makeatother \def\includecomment #1{\expandafter\def\csname#1\endcsname{}% \expandafter\def\csname end#1\endcsname{}} \def\excludecomment #1{\expandafter\def\csname#1\endcsname{\ThrowAwayComment{#1}}% {\escapechar=-1\relax \csarg\xdef{PlainEnd#1Test}{\string\\end#1}% \csarg\xdef{LaLaEnd#1Test}{\string\\end\string\{#1\string\}}% }} % Define environments that ignore their contents. \excludecomment{comment} \excludecomment{rawhtml} \excludecomment{htmlonly} % Hypertext commands etc. This is a condensed version of the html.sty % file supplied with LaTeX2HTML by: Nikos Drakos & % Jelle van Zeijl . The LaTeX2HTML documentation % should be consulted about all commands (and the environments defined above) % except \xref and \xlabel which are Starlink specific. \newcommand{\htmladdnormallinkfoot}[2]{#1\footnote{#2}} \newcommand{\htmladdnormallink}[2]{#1} \newcommand{\htmladdimg}[1]{} \newcommand{\hyperref}[4]{#2\ref{#4}#3} \newcommand{\htmlref}[2]{#1} \newcommand{\htmlimage}[1]{} \newcommand{\htmladdtonavigation}[1]{} \newenvironment{latexonly}{}{} \newcommand{\latex}[1]{#1} \newcommand{\html}[1]{} \newcommand{\latexhtml}[2]{#1} \newcommand{\HTMLcode}[2][]{} % Starlink cross-references and labels. \newcommand{\xref}[3]{#1} \newcommand{\xlabel}[1]{} % LaTeX2HTML symbol. \newcommand{\latextohtml}{\LaTeX2\texttt{HTML}} % Define command to re-centre underscore for Latex and leave as normal % for HTML (severe problems with \_ in tabbing environments and \_\_ % generally otherwise). \renewcommand{\_}{\texttt{\symbol{95}}} % ----------------------------------------------------------------------------- % Debugging. % ========= % Remove % on the following to debug links in the HTML version using Latex. % \newcommand{\hotlink}[2]{\fbox{\begin{tabular}[t]{@{}c@{}}#1\\\hline{\footnotesize #2}\end{tabular}}} % \renewcommand{\htmladdnormallinkfoot}[2]{\hotlink{#1}{#2}} % \renewcommand{\htmladdnormallink}[2]{\hotlink{#1}{#2}} % \renewcommand{\hyperref}[4]{\hotlink{#1}{\S\ref{#4}}} % \renewcommand{\htmlref}[2]{\hotlink{#1}{\S\ref{#2}}} % \renewcommand{\xref}[3]{\hotlink{#1}{#2 -- #3}} %end{latexonly} % ----------------------------------------------------------------------------- % ? Document specific \newcommand or \newenvironment commands. %+ % Name: % SST.TEX % Purpose: % Define LaTeX commands for laying out Starlink routine descriptions. % Language: % LaTeX % Type of Module: % LaTeX data file. % Description: % This file defines LaTeX commands which allow routine documentation % produced by the SST application PROLAT to be processed by LaTeX and % by LaTeX2html. The contents of this file should be included in the % source prior to any statements that make of the sst commnds. % Notes: % The commands defined in the style file html.sty provided with LaTeX2html % are used. These should either be made available by using the appropriate % sun.tex (with hypertext extensions) or by putting the file html.sty % on your TEXINPUTS path (and including the name as part of the % documentstyle declaration). % Authors: % RFWS: R.F. Warren-Smith (STARLINK) % PDRAPER: P.W. Draper (Starlink - Durham University) % MJC: Malcolm J. Currie (STARLINK) % DSB: David Berry (STARLINK) % TIMJ: Tim Jenness (JAC) % History: % 10-SEP-1990 (RFWS): % Original version. % 10-SEP-1990 (RFWS): % Added the implementation status section. % 12-SEP-1990 (RFWS): % Added support for the usage section and adjusted various spacings. % 8-DEC-1994 (PDRAPER): % Added support for simplified formatting using LaTeX2html. % 1995 October 4 (MJC): % Added goodbreaks and pagebreak[3] in various places to improve % pages breaking before headings, not immediately after. % Corrected banner width. % 1996 March 7 (MJC): % Mark document name on both sides of an sstroutine. % 2-DEC-1998 (DSB): % Added sstattributetype (copied from sun210.tex). % 2004 August 6 (MJC): % Added sstattribute. % 21-JUL-2009 (TIMJ): % Added \sstdiylist{}{} as used when a Parameters section is located that % is not "ADAM Parameters". % {enter_further_changes_here} % Bugs: % {note_any_bugs_here} %- % Define length variables. \newlength{\sstbannerlength} \newlength{\sstcaptionlength} \newlength{\sstexampleslength} \newlength{\sstexampleswidth} % Define a \tt font of the required size. \latex{\newfont{\ssttt}{cmtt10 scaled 1095}} \html{\newcommand{\ssttt}{\tt}} % Define a command to produce a routine header, including its name, % a purpose description and the rest of the routine's documentation. \newcommand{\sstroutine}[3]{ \goodbreak \markboth{{\stardocname}~ --- #1}{{\stardocname}~ --- #1} \rule{\textwidth}{0.5mm} \vspace{-7ex} \newline \settowidth{\sstbannerlength}{{\Large {\bf #1}}} \setlength{\sstcaptionlength}{\textwidth} \setlength{\sstexampleslength}{\textwidth} \addtolength{\sstbannerlength}{0.5em} \addtolength{\sstcaptionlength}{-2.0\sstbannerlength} \addtolength{\sstcaptionlength}{-5.0pt} \settowidth{\sstexampleswidth}{{\bf Examples:}} \addtolength{\sstexampleslength}{-\sstexampleswidth} \parbox[t]{\sstbannerlength}{\flushleft{\Large {\bf #1}}} \parbox[t]{\sstcaptionlength}{\center{\Large #2}} \parbox[t]{\sstbannerlength}{\flushright{\Large {\bf #1}}} \begin{description} #3 \end{description} } % Frame attributes fount. Need to find a way for these to stand out. % San serif doesn't work by default. Also without the \rm the % san serif continues after \sstatt hyperlinks. Extra braces % failed to prevent \sstattribute from using roman fount for its % headings. The current lash up appears to work, but needs further % investigation or a TeX wizard. \newcommand{\sstatt}[1]{\sf #1} \begin{htmlonly} \newcommand{\sstatt}[1]{\large{\tt #1}} \end{htmlonly} % Define a command to produce an attribute header, including its name, % a purpose description and the rest of the routine's documentation. \newcommand{\sstattribute}[3]{ \goodbreak \markboth{{\stardocname}~ --- #1}{{\stardocname}~ --- #1} \rule{\textwidth}{0.5mm} \vspace{-7ex} \newline \settowidth{\sstbannerlength}{{\Large {\sstatt #1}}} \setlength{\sstcaptionlength}{\textwidth} \setlength{\sstexampleslength}{\textwidth} \addtolength{\sstbannerlength}{0.5em} \addtolength{\sstcaptionlength}{-2.0\sstbannerlength} \addtolength{\sstcaptionlength}{-4.9pt} \settowidth{\sstexampleswidth}{{\bf Examples:}} \addtolength{\sstexampleslength}{-\sstexampleswidth} \parbox[t]{\sstbannerlength}{\flushleft{\Large {\sstatt #1}}} \parbox[t]{\sstcaptionlength}{\center{\Large #2}} \parbox[t]{\sstbannerlength}{\flushright{\Large {\sstatt #1}}} \begin{description} #3 \end{description} } % Format the description section. \newcommand{\sstdescription}[1]{\item[Description:] #1} % Format the usage section. \newcommand{\sstusage}[1]{\goodbreak \item[Usage:] \mbox{} \\[1.3ex]{\raggedright \ssttt #1}} % Format the invocation section. \newcommand{\sstinvocation}[1]{\item[Invocation:]\hspace{0.4em}{\tt #1}} % Format the attribute data type section. \newcommand{\sstattributetype}[1]{ \item[Type:] \mbox{} \\ #1 } % Format the arguments section. \newcommand{\sstarguments}[1]{ \item[Arguments:] \mbox{} \\ \vspace{-3.5ex} \begin{description} #1 \end{description} } % Format the returned value section (for a function). \newcommand{\sstreturnedvalue}[1]{ \item[Returned Value:] \mbox{} \\ \vspace{-3.5ex} \begin{description} #1 \end{description} } % Format the parameters section (for an application). \newcommand{\sstparameters}[1]{ \goodbreak \item[Parameters:] \mbox{} \\ \vspace{-3.5ex} \begin{description} #1 \end{description} } % Format the applicability section. \newcommand{\sstapplicability}[1]{ \item[Class Applicability:] \mbox{} \\ \vspace{-3.5ex} \begin{description} #1 \end{description} } % Format the examples section. \newcommand{\sstexamples}[1]{ \goodbreak \item[Examples:] \mbox{} \\ \vspace{-3.5ex} \begin{description} #1 \end{description} } % Define the format of a subsection in a normal section. \newcommand{\sstsubsection}[1]{ \item[{#1}] \mbox{} \\} % Define the format of a subsection in the examples section. \newcommand{\sstexamplesubsection}[2]{\sloppy \item[\parbox{\sstexampleslength}{\ssttt #1}] \mbox{} \vspace{1.0ex} \\ #2 } % Format the notes section. \newcommand{\sstnotes}[1]{\goodbreak \item[Notes:] \mbox{} \\[1.3ex] #1} % Provide a general-purpose format for additional (DIY) sections. \newcommand{\sstdiytopic}[2]{\item[{\hspace{-0.35em}#1\hspace{-0.35em}:}] \mbox{} \\[1.3ex] #2} % Format the a generic section as a list \newcommand{\sstdiylist}[2]{ \item[#1:] \mbox{} \\ \vspace{-3.5ex} \begin{description} #2 \end{description} } % Format the implementation status section. \newcommand{\sstimplementationstatus}[1]{ \item[{Implementation Status:}] \mbox{} \\[1.3ex] #1} % Format the bugs section. \newcommand{\sstbugs}[1]{\item[Bugs:] #1} % Format a list of items while in paragraph mode. \newcommand{\sstitemlist}[1]{ \mbox{} \\ \vspace{-3.5ex} \begin{itemize} #1 \end{itemize} } % Define the format of an item. \newcommand{\sstitem}{\item} % Now define html equivalents of those already set. These are used by % latex2html and are defined in the html.sty files. \begin{htmlonly} % sstroutine. \newcommand{\sstroutine}[3]{ \subsection{#1\xlabel{#1}-\label{#1}#2} \begin{description} #3 \end{description} } % sstattribute. Note the further level of subsectioning. \newcommand{\sstattribute}[3]{ \subsubsection{#1\xlabel{#1}-\label{#1}#2} \begin{description} #3 \end{description} \\ } % sstdescription \newcommand{\sstdescription}[1]{\item[Description:] \begin{description} #1 \end{description} \\ } % sstusage \newcommand{\sstusage}[1]{\item[Usage:] \begin{description} {\ssttt #1} \end{description} \\ } % sstinvocation \newcommand{\sstinvocation}[1]{\item[Invocation:] \begin{description} {\ssttt #1} \end{description} \\ } % sstarguments \newcommand{\sstarguments}[1]{ \item[Arguments:] \\ \begin{description} #1 \end{description} \\ } % sstreturnedvalue \newcommand{\sstreturnedvalue}[1]{ \item[Returned Value:] \\ \begin{description} #1 \end{description} \\ } % sstparameters \newcommand{\sstparameters}[1]{ \item[Parameters:] \\ \begin{description} #1 \end{description} \\ } % sstapplicability \newcommand{\sstapplicability}[1]{% \item[Class Applicability:] \begin{description} #1 \end{description} \\ } % sstexamples \newcommand{\sstexamples}[1]{ \item[Examples:] \\ \begin{description} #1 \end{description} \\ } % sstsubsection \newcommand{\sstsubsection}[1]{\item[{#1}]} % sstexamplesubsection \newcommand{\sstexamplesubsection}[2]{\item[{\ssttt #1}] #2\\} % sstnotes \newcommand{\sstnotes}[1]{\item[Notes:] #1 } % sstdiytopic \newcommand{\sstdiytopic}[2]{\item[{#1}] #2 } % sstimplementationstatus \newcommand{\sstimplementationstatus}[1]{ \item[Implementation Status:] #1 } % sstitemlist \newcommand{\sstitemlist}[1]{ \begin{itemize} #1 \end{itemize} \\ } % sstitem \newcommand{\sstitem}{\item} \end{htmlonly} % End of sst.tex layout definitions. %. % ? End of document specific commands % ----------------------------------------------------------------------------- % Title Page. % =========== \renewcommand{\thepage}{\roman{page}} \begin{document} \thispagestyle{empty} % Latex document header. % ====================== \begin{latexonly} \textsc{Joint Astronomy Centre} \hfill \textbf{\stardocname}\\ {\large Science \& Technology Facilities Council}\\ {\large Starlink Project\\} {\large \stardoccategory\ \stardocnumber} \begin{flushright} \stardocauthors\\ \stardocdate \end{flushright} \vspace{-4mm} \rule{\textwidth}{0.5mm} \vspace{5mm} \begin{center} {\Huge\textbf{\stardoctitle \\ [2.5ex]}} {\LARGE\textbf{\stardocversion \\ [4ex]}} {\Huge\textbf{\stardocmanual}} \end{center} \vspace{5mm} % ? Add picture here if required for the LaTeX version. % e.g. \includegraphics[scale=0.3]{filename.ps} % ? End of picture % ? Heading for abstract if used. \vspace{10mm} \begin{center} {\Large\textbf{Abstract}} \end{center} % ? End of heading for abstract. \end{latexonly} % HTML documentation header. % ========================== \begin{htmlonly} \xlabel{} \begin{rawhtml}

\end{rawhtml} \stardoctitle\\ \stardocversion\\ \stardocmanual \begin{rawhtml}

\end{rawhtml} % ? Add picture here if required for the hypertext version. % e.g. \includegraphics[scale=0.7]{filename.ps} % ? End of picture \begin{rawhtml}

\end{rawhtml} \stardoccategory\ \stardocnumber \\ \stardocauthors \\ \stardocdate \begin{rawhtml}

\end{rawhtml} \htmladdnormallink{Joint Astronomy Centre} {http://www.jach.hawaii.edu} \\ \htmladdnormallink{Science \& Technology Facilities Council} {http://www.scitech.ac.uk} \\ \begin{rawhtml}

\end{rawhtml} \htmladdnormallink{Starlink Project}{http://www.starlink.ac.uk/} \begin{rawhtml}

\end{rawhtml} \htmladdnormallink{\htmladdimg{source.gif} Retrieve hardcopy} {http://www.starlink.ac.uk/cgi-bin/hcserver?\stardocsource}\\ % HTML document table of contents. % ================================ % Add table of contents header and a navigation button to return to this % point in the document (this should always go before the abstract \section). \label{stardoccontents} \begin{rawhtml}

Contents

\end{rawhtml} \htmladdtonavigation{\htmlref{\htmladdimg{contents_motif.gif}} {stardoccontents}} % ? New section for abstract if used. \section{\xlabel{abstract}Abstract} % ? End of new section for abstract \end{htmlonly} % ----------------------------------------------------------------------------- % ? Document Abstract. (if used) % ================== \stardocabstract % ? End of document abstract % ----------------------------------------------------------------------------- % ? Latex Copyright Statement % ========================= \begin{latexonly} \newpage \vspace*{\fill} \stardoccopyright \end{latexonly} % ? End of Latex copyright statement % ----------------------------------------------------------------------------- % ? Latex document Table of Contents (if used). % =========================================== % \newpage % \begin{latexonly} % \setlength{\parskip}{0mm} % \tableofcontents % \setlength{\parskip}{\medskipamount} % \markboth{\stardocname}{\stardocname} %\end{latexonly} % ? End of Latex document table of contents % ----------------------------------------------------------------------------- \cleardoublepage \renewcommand{\thepage}{\arabic{page}} \setcounter{page}{1} % ? Main text \section{Introduction} This library provides a C library designed as a API-compatible replacement for the C SLALIB library (SUN/67) and uses a GPL licence so is freely redistributable. Where possible the functions call equivalent SOFA routines (Hohenkerk, C., 2011, Scholarpedia, \textbf{6}, \emph{11404}) and use current IAU 2006 standards. This means that any functions that rely on nutation or precession will return slightly different answers to the SLA functions. \section{Citing PAL} If you use PAL in your work please consider citing it. The description paper for PAL is: \emph{PAL: A Positional Astronomy Library}, Jenness, T. \& Berry, D. S., in \emph{Astronomoical Data Anaysis Software and Systems XXII}, Friedel, D. N. (ed), ASP Conf.\ Ser. \textbf{475}, p307. \clearpage \appendix \section{\label{APP:SPEC}Function Descriptions} \subsection{SOFA Mappings} The following table lists PAL/SLA functions that have direct replacements in SOFA. Whilst these routines are implemented in the PAL library using SOFA new code should probably call SOFA directly. \begin{tabular}{ll} SLA/PAL & SOFA \\ \texttt{palCldj} & \texttt{iauCal2jd} \\ \texttt{palDbear} & \texttt{iauPas} \\ \texttt{palDaf2r} & \texttt{iauAf2a} \\ \texttt{palDav2m} & \texttt{iauRv2m} \\ \texttt{palDcc2s} & \texttt{iauC2s} \\ \texttt{palDcs2c} & \texttt{iauS2c} \\ \texttt{palDd2tf} & \texttt{iauD2tf}\\ \texttt{palDimxv} & \texttt{iauTrxp}\\ \texttt{palDm2av} & \texttt{iauRm2v}\\ \texttt{palDjcl} & \texttt{iauJd2cal}\\ \texttt{palDmxm} & \texttt{iauRxr}\\ \texttt{palDmxv} & \texttt{iauRxp}\\ \texttt{palDpav} & \texttt{iauPap}\\ \texttt{palDr2af} & \texttt{iauA2af}\\ \texttt{palDr2tf} & \texttt{iauA2tf}\\ \texttt{palDranrm} & \texttt{iauAnp}\\ \texttt{palDsep} & \texttt{iauSeps}\\ \texttt{palDsepv} & \texttt{iauSepp}\\ \texttt{palDtf2d} & \texttt{iauTf2d}\\ \texttt{palDtf2r} & \texttt{iauTf2a}\\ \texttt{palDvdv} & \texttt{iauPdp}\\ \texttt{palDvn} & \texttt{iauPn}\\ \texttt{palDvxv} & \texttt{iauPxp}\\ \texttt{palEpb} & \texttt{iauEpb}\\ \texttt{palEpb2d} & \texttt{iauEpb2d}\\ \texttt{palEpj} & \texttt{iauEpj}\\ \texttt{palEpj2d} & \texttt{iauEpj2jd}\\ \texttt{palEqeqx} & \texttt{iauEe06a}\\ \texttt{palFk5hz} & \texttt{iauFk5hz} \textit{also calls iauEpj2jd}\\ \texttt{palGmst} & \texttt{iauGmst06}\\ \texttt{palGmsta} & \texttt{iauGmst06}\\ \texttt{palHfk5z} & \texttt{iauHfk5z} \textit{also calls iauEpj2jd}\\ \end{tabular} \subsection{More complex functions} These functions do not have a simple equivalent in SOFA so are reimplemented either completely standalone or using multiple SOFA functions. %% Regenerate everything after this from the prologues using SST by %% running "make palsun.tex". We do not build this automatically as %% there is no particular need for an SST dependency. %% Some manual tweaking is required after creating the SST tex. \sstroutine{ palAddet }{ Add the E-terms to a pre IAU 1976 mean place }{ \sstdescription{ Add the E-terms (elliptic component of annual aberration) to a pre IAU 1976 mean place to conform to the old catalogue convention. } \sstinvocation{ void palAddet ( double rm, double dm, double eq, double $*$rc, double $*$dc ); } \sstarguments{ \sstsubsection{ rm = double (Given) }{ RA without E-terms (radians) } \sstsubsection{ dm = double (Given) }{ Dec without E-terms (radians) } \sstsubsection{ eq = double (Given) }{ Besselian epoch of mean equator and equinox } \sstsubsection{ rc = double $*$ (Returned) }{ RA with E-terms included (radians) } \sstsubsection{ dc = double $*$ (Returned) }{ Dec with E-terms included (radians) } } \sstnotes{ Most star positions from pre-1984 optical catalogues (or derived from astrometry using such stars) embody the E-terms. If it is necessary to convert a formal mean place (for example a pulsar timing position) to one consistent with such a star catalogue, then the RA,Dec should be adjusted using this routine. } \sstdiytopic{ See Also }{ Explanatory Supplement to the Astronomical Ephemeris, section 2D, page 48. } } \sstroutine{ palAirmas }{ Air mass at given zenith distance }{ \sstdescription{ Calculates the airmass at the observed zenith distance. } \sstinvocation{ double palAirmas( double zd ); } \sstarguments{ \sstsubsection{ zd = double (Given) }{ Observed zenith distance (radians) } } \sstnotes{ \sstitemlist{ \sstitem The {\tt "}observed{\tt "} zenith distance referred to above means {\tt "}as affected by refraction{\tt "}. \sstitem Uses Hardie{\tt '}s (1962) polynomial fit to Bemporad{\tt '}s data for the relative air mass, X, in units of thickness at the zenith as tabulated by Schoenberg (1929). This is adequate for all normal needs as it is accurate to better than 0.1\% up to X = 6.8 and better than 1\% up to X = 10. Bemporad{\tt '}s tabulated values are unlikely to be trustworthy to such accuracy because of variations in density, pressure and other conditions in the atmosphere from those assumed in his work. \sstitem The sign of the ZD is ignored. \sstitem At zenith distances greater than about ZD = 87 degrees the air mass is held constant to avoid arithmetic overflows. } } \sstdiytopic{ See Also }{ \sstitemlist{ \sstitem Hardie, R.H., 1962, in {\tt "}Astronomical Techniques{\tt "} ed. W.A. Hiltner, University of Chicago Press, p180. \sstitem Schoenberg, E., 1929, Hdb. d. Ap., Berlin, Julius Springer, 2, 268. } } } \sstroutine{ palAmp }{ Convert star RA,Dec from geocentric apparaent to mean place }{ \sstdescription{ Convert star RA,Dec from geocentric apparent to mean place. The mean coordinate system is close to ICRS. See palAmpqk for details. } \sstinvocation{ void palAmp ( double ra, double da, double date, double eq, double $*$rm, double $*$dm ); } \sstarguments{ \sstsubsection{ ra = double (Given) }{ Apparent RA (radians) } \sstsubsection{ dec = double (Given) }{ Apparent Dec (radians) } \sstsubsection{ date = double (Given) }{ TDB for apparent place (JD-2400000.5) } \sstsubsection{ eq = double (Given) }{ Equinox: Julian epoch of mean place. } \sstsubsection{ rm = double $*$ (Returned) }{ Mean RA (radians) } \sstsubsection{ dm = double $*$ (Returned) }{ Mean Dec (radians) } } \sstnotes{ \sstitemlist{ \sstitem See palMappa and palAmpqk for details. } } } \sstroutine{ palAmpqk }{ Convert star RA,Dec from geocentric apparent to mean place }{ \sstdescription{ Convert star RA,Dec from geocentric apparent to mean place. The {\tt "}mean{\tt "} coordinate system is in fact close to ICRS. Use of this function is appropriate when efficiency is important and where many star positions are all to be transformed for one epoch and equinox. The star-independent parameters can be obtained by calling the palMappa function. } \sstinvocation{ void palAmpqk ( double ra, double da, double amprms[21], double $*$rm, double $*$dm ) } \sstarguments{ \sstsubsection{ ra = double (Given) }{ Apparent RA (radians). } \sstsubsection{ da = double (Given) }{ Apparent Dec (radians). } \sstsubsection{ amprms = double[21] (Given) }{ Star-independent mean-to-apparent parameters (see palMappa): (0) time interval for proper motion (Julian years) (1-3) barycentric position of the Earth (AU) (4-6) not used (7) not used (8-10) abv: barycentric Earth velocity in units of c (11) sqrt(1-v$*$v) where v=modulus(abv) (12-20) precession/nutation (3,3) matrix } \sstsubsection{ rm = double (Returned) }{ Mean RA (radians). } \sstsubsection{ dm = double (Returned) }{ Mean Dec (radians). } } } \sstroutine{ palCaldj }{ Gregorian Calendar to Modified Julian Date }{ \sstdescription{ Modified Julian Date to Gregorian Calendar with special behaviour for 2-digit years relating to 1950 to 2049. } \sstinvocation{ void palCaldj ( int iy, int im, int id, double $*$djm, int $*$j ); } \sstarguments{ \sstsubsection{ iy = int (Given) }{ Year in the Gregorian calendar } \sstsubsection{ im = int (Given) }{ Month in the Gergorian calendar } \sstsubsection{ id = int (Given) }{ Day in the Gregorian calendar } \sstsubsection{ djm = double $*$ (Returned) }{ Modified Julian Date (JD-2400000.5) for 0 hrs } \sstsubsection{ j = status (Returned) }{ 0 = OK. See iauCal2jd for other values. } } \sstnotes{ \sstitemlist{ \sstitem Uses iauCal2jd \sstitem Unlike iauCal2jd this routine treats the years 0-100 as referring to the end of the 20th Century and beginning of the 21st Century. If this behaviour is not acceptable use the SOFA routine directly or palCldj. Acceptable years are 00-49, interpreted as 2000-2049, 50-99, {\tt "} {\tt "} 1950-1999, all others, interpreted literally. \sstitem Unlike SLA this routine will work with negative years. } } } \sstroutine{ palDafin }{ Sexagesimal character string to angle }{ \sstdescription{ Extracts an angle from a sexagesimal string with degrees, arcmin, arcsec fields using space or comma delimiters. } \sstinvocation{ void palDafin ( const char $*$string, int $*$ipos, double $*$a, int $*$j ); } \sstarguments{ \sstsubsection{ string = const char $*$ (Given) }{ String containing deg, arcmin, arcsec fields } \sstsubsection{ ipos = int $*$ (Given \& Returned) }{ Position to start decoding {\tt "}string{\tt "}. First character is position 1 for compatibility with SLA. After calling this routine {\tt "}iptr{\tt "} will be positioned after the sexagesimal string. } \sstsubsection{ a = double $*$ (Returned) }{ Angle in radians. } \sstsubsection{ j = int $*$ (Returned) }{ status: 0 = OK $+$1 = default, A unchanged \sstitemlist{ \sstitem 1 = bad degrees ) \sstitem 2 = bad arcminutes ) (note 3) \sstitem 3 = bad arcseconds ) } } } \sstnotes{ \sstitemlist{ \sstitem The first three {\tt "}fields{\tt "} in STRING are degrees, arcminutes, arcseconds, separated by spaces or commas. The degrees field may be signed, but not the others. The decoding is carried out by the palDfltin routine and is free-format. \sstitem Successive fields may be absent, defaulting to zero. For zero status, the only combinations allowed are degrees alone, degrees and arcminutes, and all three fields present. If all three fields are omitted, a status of $+$1 is returned and A is unchanged. In all other cases A is changed. \sstitem Range checking: } The degrees field is not range checked. However, it is expected to be integral unless the other two fields are absent. The arcminutes field is expected to be 0-59, and integral if the arcseconds field is present. If the arcseconds field is absent, the arcminutes is expected to be 0-59.9999... The arcseconds field is expected to be 0-59.9999... \sstitemlist{ \sstitem Decoding continues even when a check has failed. Under these circumstances the field takes the supplied value, defaulting to zero, and the result A is computed and returned. \sstitem Further fields after the three expected ones are not treated as an error. The pointer IPOS is left in the correct state for further decoding with the present routine or with palDfltin etc. See the example, above. \sstitem If STRING contains hours, minutes, seconds instead of degrees etc, or if the required units are turns (or days) instead of radians, the result A should be multiplied as follows: } for to obtain multiply STRING A in A by d {\tt '} {\tt "} radians 1 = 1.0 d {\tt '} {\tt "} turns 1/2pi = 0.1591549430918953358 h m s radians 15 = 15.0 h m s days 15/2pi = 2.3873241463784300365 } \sstdiytopic{ Example }{ argument before after STRING {\tt '}-57 17 44.806 12 34 56.7{\tt '} unchanged IPTR 1 16 (points to 12...) A ? -1.00000D0 J ? 0 } } \sstroutine{ palDe2h }{ Equatorial to horizon coordinates: HA,Dec to Az,E }{ \sstdescription{ Convert equatorial to horizon coordinates. } \sstinvocation{ palDe2h( double ha, double dec, double phi, double $*$ az, double $*$ el ); } \sstarguments{ \sstsubsection{ ha = double $*$ (Given) }{ Hour angle (radians) } \sstsubsection{ dec = double $*$ (Given) }{ Declination (radians) } \sstsubsection{ phi = double (Given) }{ Observatory latitude (radians) } \sstsubsection{ az = double $*$ (Returned) }{ Azimuth (radians) } \sstsubsection{ el = double $*$ (Returned) }{ Elevation (radians) } } \sstnotes{ \sstitemlist{ \sstitem All the arguments are angles in radians. \sstitem Azimuth is returned in the range 0-2pi; north is zero, and east is $+$pi/2. Elevation is returned in the range $+$/-pi/2. \sstitem The latitude must be geodetic. In critical applications, corrections for polar motion should be applied. \sstitem In some applications it will be important to specify the correct type of hour angle and declination in order to produce the required type of azimuth and elevation. In particular, it may be important to distinguish between elevation as affected by refraction, which would require the {\tt "}observed{\tt "} HA,Dec, and the elevation in vacuo, which would require the {\tt "}topocentric{\tt "} HA,Dec. If the effects of diurnal aberration can be neglected, the {\tt "}apparent{\tt "} HA,Dec may be used instead of the topocentric HA,Dec. \sstitem No range checking of arguments is carried out. \sstitem In applications which involve many such calculations, rather than calling the present routine it will be more efficient to use inline code, having previously computed fixed terms such as sine and cosine of latitude, and (for tracking a star) sine and cosine of declination. } } } \sstroutine{ palDeuler }{ Form a rotation matrix from the Euler angles }{ \sstdescription{ A rotation is positive when the reference frame rotates anticlockwise as seen looking towards the origin from the positive region of the specified axis. The characters of ORDER define which axes the three successive rotations are about. A typical value is {\tt '}ZXZ{\tt '}, indicating that RMAT is to become the direction cosine matrix corresponding to rotations of the reference frame through PHI radians about the old Z-axis, followed by THETA radians about the resulting X-axis, then PSI radians about the resulting Z-axis. The axis names can be any of the following, in any order or combination: X, Y, Z, uppercase or lowercase, 1, 2, 3. Normal axis labelling/numbering conventions apply; the xyz (=123) triad is right-handed. Thus, the {\tt '}ZXZ{\tt '} example given above could be written {\tt '}zxz{\tt '} or {\tt '}313{\tt '} (or even {\tt '}ZxZ{\tt '} or {\tt '}3xZ{\tt '}). ORDER is terminated by length or by the first unrecognized character. Fewer than three rotations are acceptable, in which case the later angle arguments are ignored. If all rotations are zero, the identity matrix is produced. } \sstinvocation{ void palDeuler ( const char $*$order, double phi, double theta, double psi, double rmat[3][3] ); } \sstarguments{ \sstsubsection{ order = const char[] (Given) }{ Specifies about which axes the rotation occurs } \sstsubsection{ phi = double (Given) }{ 1st rotation (radians) } \sstsubsection{ theta = double (Given) }{ 2nd rotation (radians) } \sstsubsection{ psi = double (Given) }{ 3rd rotation (radians) } \sstsubsection{ rmat = double[3][3] (Given \& Returned) }{ Rotation matrix } } } \sstroutine{ palDfltin }{ Convert free-format input into double precision floating point }{ \sstdescription{ Extracts a number from an input string starting at the specified index. } \sstinvocation{ void palDfltin( const char $*$ string, int $*$nstrt, double $*$dreslt, int $*$jflag ); } \sstarguments{ \sstsubsection{ string = const char $*$ (Given) }{ String containing number to be decoded. } \sstsubsection{ nstrt = int $*$ (Given and Returned) }{ Character number indicating where decoding should start. On output its value is updated to be the location of the possible next value. For compatibility with SLA the first character is index 1. } \sstsubsection{ dreslt = double $*$ (Returned) }{ Result. Not updated when jflag=1. } \sstsubsection{ jflag = int $*$ (Returned) }{ status: -1 = -OK, 0 = $+$OK, 1 = null, 2 = error } } \sstnotes{ \sstitemlist{ \sstitem Uses the strtod() system call to do the parsing. This may lead to subtle differences when compared to the SLA/F parsing. \sstitem All {\tt "}D{\tt "} characters are converted to {\tt "}E{\tt "} to handle fortran exponents. \sstitem Commas are recognized as a special case and are skipped if one happens to be the next character when updating nstrt. Additionally the output nstrt position will skip past any trailing space. \sstitem If no number can be found flag will be set to 1. \sstitem If the number overflows or underflows jflag will be set to 2. For overflow the returned result will have the value HUGE\_VAL, for underflow it will have the value 0.0. \sstitem For compatiblity with SLA/F -0 will be returned as {\tt "}0{\tt "} with jflag == -1. \sstitem Unlike slaDfltin a standalone {\tt "}E{\tt "} will return status 1 (could not find a number) rather than 2 (bad number). } } } \sstroutine{ palDh2e }{ Horizon to equatorial coordinates: Az,El to HA,Dec }{ \sstdescription{ Convert horizon to equatorial coordinates. } \sstinvocation{ palDh2e( double az, double el, double phi, double $*$ ha, double $*$ dec ); } \sstarguments{ \sstsubsection{ az = double (Given) }{ Azimuth (radians) } \sstsubsection{ el = double (Given) }{ Elevation (radians) } \sstsubsection{ phi = double (Given) }{ Observatory latitude (radians) } \sstsubsection{ ha = double $*$ (Returned) }{ Hour angle (radians) } \sstsubsection{ dec = double $*$ (Returned) }{ Declination (radians) } } \sstnotes{ \sstitemlist{ \sstitem All the arguments are angles in radians. \sstitem The sign convention for azimuth is north zero, east $+$pi/2. \sstitem HA is returned in the range $+$/-pi. Declination is returned in the range $+$/-pi/2. \sstitem The latitude is (in principle) geodetic. In critical applications, corrections for polar motion should be applied. \sstitem In some applications it will be important to specify the correct type of elevation in order to produce the required type of HA,Dec. In particular, it may be important to distinguish between the elevation as affected by refraction, which will yield the {\tt "}observed{\tt "} HA,Dec, and the elevation in vacuo, which will yield the {\tt "}topocentric{\tt "} HA,Dec. If the effects of diurnal aberration can be neglected, the topocentric HA,Dec may be used as an approximation to the {\tt "}apparent{\tt "} HA,Dec. \sstitem No range checking of arguments is done. \sstitem In applications which involve many such calculations, rather than calling the present routine it will be more efficient to use inline code, having previously computed fixed terms such as sine and cosine of latitude. } } } \sstroutine{ palDjcal }{ Modified Julian Date to Gregorian Calendar }{ \sstdescription{ Modified Julian Date to Gregorian Calendar, expressed in a form convenient for formatting messages (namely rounded to a specified precision, and with the fields stored in a single array) } \sstinvocation{ void palDjcal ( int ndp, double djm, int iymdf[4], int $*$j ); } \sstarguments{ \sstsubsection{ ndp = int (Given) }{ Number of decimal places of days in fraction. } \sstsubsection{ djm = double (Given) }{ Modified Julian Date (JD-2400000.5) } \sstsubsection{ iymdf[4] = int[] (Returned) }{ Year, month, day, fraction in Gregorian calendar. } \sstsubsection{ j = status (Returned) }{ 0 = OK. See iauJd2cal for other values. } } \sstnotes{ \sstitemlist{ \sstitem Uses iauJd2cal } } } \sstroutine{ palDmat }{ Matrix inversion \& solution of simultaneous equations }{ \sstdescription{ Matrix inversion \& solution of simultaneous equations For the set of n simultaneous equations in n unknowns: A.Y = X this routine calculates the inverse of A, the determinant of matrix A and the vector of N unknowns. } \sstinvocation{ void palDmat( int n, double $*$a, double $*$y, double $*$d, int $*$jf, int $*$iw ); } \sstarguments{ \sstsubsection{ n = int (Given) }{ Number of simultaneous equations and number of unknowns. } \sstsubsection{ a = double[] (Given \& Returned) }{ A non-singular NxN matrix (implemented as a contiguous block of memory). After calling this routine {\tt "}a{\tt "} contains the inverse of the matrix. } \sstsubsection{ y = double[] (Given \& Returned) }{ The vector of N unknowns. On exit this vector contains the N solutions. } \sstsubsection{ d = double $*$ (Returned) }{ The determinant. } \sstsubsection{ jf = int $*$ (Returned) }{ The singularity flag. If the matrix is non-singular, jf=0 is returned. If the matrix is singular, jf=-1 \& d=0.0 are returned. In the latter case, the contents of array {\tt "}a{\tt "} on return are undefined. } } \sstnotes{ \sstitemlist{ \sstitem Implemented using Gaussian elimination with partial pivoting. \sstitem Optimized for speed rather than accuracy with errors 1 to 4 times those of routines optimized for accuracy. } } } \sstroutine{ palDs2tp }{ Spherical to tangent plane projection }{ \sstdescription{ Projection of spherical coordinates onto tangent plane: {\tt "}gnomonic{\tt "} projection - {\tt "}standard coordinates{\tt "} } \sstinvocation{ palDs2tp( double ra, double dec, double raz, double decz, double $*$xi, double $*$eta, int $*$j ); } \sstarguments{ \sstsubsection{ ra = double (Given) }{ RA spherical coordinate of point to be projected (radians) } \sstsubsection{ dec = double (Given) }{ Dec spherical coordinate of point to be projected (radians) } \sstsubsection{ raz = double (Given) }{ RA spherical coordinate of tangent point (radians) } \sstsubsection{ decz = double (Given) }{ Dec spherical coordinate of tangent point (radians) } \sstsubsection{ xi = double $*$ (Returned) }{ First rectangular coordinate on tangent plane (radians) } \sstsubsection{ eta = double $*$ (Returned) }{ Second rectangular coordinate on tangent plane (radians) } \sstsubsection{ j = int $*$ (Returned) }{ status: 0 = OK, star on tangent plane 1 = error, star too far from axis 2 = error, antistar on tangent plane 3 = error, antistar too far from axis } } } \sstroutine{ palDtt }{ Return offset between UTC and TT }{ \sstdescription{ Increment to be applied to Coordinated Universal Time UTC to give International Atomic Time (TAI). } \sstinvocation{ dat = palDat( double utc ); } \sstarguments{ \sstsubsection{ utc = double (Given) }{ UTC date as a modified JD (JD-2400000.5) } } \sstreturnedvalue{ \sstsubsection{ dat = double }{ TAI-UTC in seconds } } \sstnotes{ \sstitemlist{ \sstitem This routine converts the MJD argument to calendar date before calling the SOFA iauDat function. \sstitem This routine matches the slaDat interface which differs from the iauDat interface. Consider coding directly to the SOFA interface. \sstitem See iauDat for a description of error conditions when calling this function with a time outside of the UTC range. \sstitem The status argument from iauDat is ignored. This is reasonable since the error codes are mainly related to incorrect calendar dates when calculating the JD internally. } } } \sstroutine{ palDmoon }{ Approximate geocentric position and velocity of the Moon }{ \sstdescription{ Calculate the approximate geocentric position of the Moon using a full implementation of the algorithm published by Meeus (l{\tt '}Astronomie, June 1984, p348). } \sstinvocation{ void palDmoon( double date, double pv[6] ); } \sstarguments{ \sstsubsection{ date = double (Given) }{ TDB as a Modified Julian Date (JD-2400000.5) } \sstsubsection{ pv = double [6] (Returned) }{ Moon x,y,z,xdot,ydot,zdot, mean equator and equinox of date (AU, AU/s) } } \sstnotes{ \sstitemlist{ \sstitem Meeus quotes accuracies of 10 arcsec in longitude, 3 arcsec in latitude and 0.2 arcsec in HP (equivalent to about 20 km in distance). Comparison with JPL DE200 over the interval 1960-2025 gives RMS errors of 3.7 arcsec and 83 mas/hour in longitude, 2.3 arcsec and 48 mas/hour in latitude, 11 km and 81 mm/s in distance. The maximum errors over the same interval are 18 arcsec and 0.50 arcsec/hour in longitude, 11 arcsec and 0.24 arcsec/hour in latitude, 40 km and 0.29 m/s in distance. \sstitem The original algorithm is expressed in terms of the obsolete timescale Ephemeris Time. Either TDB or TT can be used, but not UT without incurring significant errors (30 arcsec at the present time) due to the Moon{\tt '}s 0.5 arcsec/sec movement. \sstitem The algorithm is based on pre IAU 1976 standards. However, the result has been moved onto the new (FK5) equinox, an adjustment which is in any case much smaller than the intrinsic accuracy of the procedure. \sstitem Velocity is obtained by a complete analytical differentiation of the Meeus model. } } } \sstroutine{ palDrange }{ Normalize angle into range $+$/- pi }{ \sstdescription{ The result is {\tt "}angle{\tt "} expressed in the range $+$/- pi. If the supplied value for {\tt "}angle{\tt "} is equal to $+$/- pi, it is returned unchanged. } \sstinvocation{ palDrange( double angle ) } \sstarguments{ \sstsubsection{ angle = double (Given) }{ The angle in radians. } } } \sstroutine{ palDt }{ Estimate the offset between dynamical time and UT }{ \sstdescription{ Estimate the offset between dynamical time and Universal Time for a given historical epoch. } \sstinvocation{ double palDt( double epoch ); } \sstarguments{ \sstsubsection{ epoch = double (Given) }{ Julian epoch (e.g. 1850.0) } } \sstreturnedvalue{ \sstsubsection{ palDt = double }{ Rough estimate of ET-UT (after 1984, TT-UT) at the given epoch, in seconds. } } \sstnotes{ \sstitemlist{ \sstitem Depending on the epoch, one of three parabolic approximations is used: } before 979 Stephenson \& Morrison{\tt '}s 390 BC to AD 948 model 979 to 1708 Stephenson \& Morrison{\tt '}s 948 to 1600 model after 1708 McCarthy \& Babcock{\tt '}s post-1650 model The breakpoints are chosen to ensure continuity: they occur at places where the adjacent models give the same answer as each other. \sstitemlist{ \sstitem The accuracy is modest, with errors of up to 20 sec during the interval since 1650, rising to perhaps 30 min by 1000 BC. Comparatively accurate values from AD 1600 are tabulated in the Astronomical Almanac (see section K8 of the 1995 AA). \sstitem The use of double-precision for both argument and result is purely for compatibility with other SLALIB time routines. \sstitem The models used are based on a lunar tidal acceleration value of -26.00 arcsec per century. } } \sstdiytopic{ See Also }{ Explanatory Supplement to the Astronomical Almanac, ed P.K.Seidelmann, University Science Books (1992), section 2.553, p83. This contains references to the Stephenson \& Morrison and McCarthy \& Babcock papers. } } \sstroutine{ palDtp2s }{ Tangent plane to spherical coordinates }{ \sstdescription{ Transform tangent plane coordinates into spherical. } \sstinvocation{ palDtp2s( double xi, double eta, double raz, double decz, double $*$ra, double $*$dec); } \sstarguments{ \sstsubsection{ xi = double (Given) }{ First rectangular coordinate on tangent plane (radians) } \sstsubsection{ eta = double (Given) }{ Second rectangular coordinate on tangent plane (radians) } \sstsubsection{ raz = double (Given) }{ RA spherical coordinate of tangent point (radians) } \sstsubsection{ decz = double (Given) }{ Dec spherical coordinate of tangent point (radians) } \sstsubsection{ ra = double $*$ (Returned) }{ RA spherical coordinate of point to be projected (radians) } \sstsubsection{ dec = double $*$ (Returned) }{ Dec spherical coordinate of point to be projected (radians) } } } \sstroutine{ palDtps2c }{ Determine RA,Dec of tangent point from coordinates }{ \sstdescription{ From the tangent plane coordinates of a star of known RA,Dec, determine the RA,Dec of the tangent point. } \sstinvocation{ palDtps2c( double xi, double eta, double ra, double dec, double $*$ raz1, double decz1, double $*$ raz2, double decz2, int $*$n); } \sstarguments{ \sstsubsection{ xi = double (Given) }{ First rectangular coordinate on tangent plane (radians) } \sstsubsection{ eta = double (Given) }{ Second rectangular coordinate on tangent plane (radians) } \sstsubsection{ ra = double (Given) }{ RA spherical coordinate of star (radians) } \sstsubsection{ dec = double (Given) }{ Dec spherical coordinate of star (radians) } \sstsubsection{ raz1 = double $*$ (Returned) }{ RA spherical coordinate of tangent point, solution 1 (radians) } \sstsubsection{ decz1 = double $*$ (Returned) }{ Dec spherical coordinate of tangent point, solution 1 (radians) } \sstsubsection{ raz2 = double $*$ (Returned) }{ RA spherical coordinate of tangent point, solution 2 (radians) } \sstsubsection{ decz2 = double $*$ (Returned) }{ Dec spherical coordinate of tangent point, solution 2 (radians) } \sstsubsection{ n = int $*$ (Returned) }{ number of solutions: 0 = no solutions returned (note 2) 1 = only the first solution is useful (note 3) 2 = both solutions are useful (note 3) } } \sstnotes{ \sstitemlist{ \sstitem The RAZ1 and RAZ2 values are returned in the range 0-2pi. \sstitem Cases where there is no solution can only arise near the poles. For example, it is clearly impossible for a star at the pole itself to have a non-zero XI value, and hence it is meaningless to ask where the tangent point would have to be to bring about this combination of XI and DEC. \sstitem Also near the poles, cases can arise where there are two useful solutions. The argument N indicates whether the second of the two solutions returned is useful. N=1 indicates only one useful solution, the usual case; under these circumstances, the second solution corresponds to the {\tt "}over-the-pole{\tt "} case, and this is reflected in the values of RAZ2 and DECZ2 which are returned. \sstitem The DECZ1 and DECZ2 values are returned in the range $+$/-pi, but in the usual, non-pole-crossing, case, the range is $+$/-pi/2. \sstitem This routine is the spherical equivalent of the routine sla\_DTPV2C. } } } \sstroutine{ palDtt }{ Return offset between UTC and TT }{ \sstdescription{ Increment to be applied to Coordinated Universal Time UTC to give Terrestrial Time TT (formerly Ephemeris Time ET) } \sstinvocation{ dtt = palDtt( double utc ); } \sstarguments{ \sstsubsection{ utc = double (Given) }{ UTC date as a modified JD (JD-2400000.5) } } \sstreturnedvalue{ \sstsubsection{ dtt = double }{ TT-UTC in seconds } } \sstnotes{ \sstitemlist{ \sstitem Consider a comprehensive upgrade to use the time transformations in SOFA{\tt '}s time cookbook: http://www.iausofa.org/sofa\_ts\_c.pdf. \sstitem See iauDat for a description of error conditions when calling this function with a time outside of the UTC range. This behaviour differs from slaDtt. } } } \sstroutine{ palEcmat }{ Form the equatorial to ecliptic rotation matrix - IAU 2006 precession model }{ \sstdescription{ The equatorial to ecliptic rotation matrix is found and returned. The matrix is in the sense V(ecl) = RMAT $*$ V(equ); the equator, equinox and ecliptic are mean of date. } \sstinvocation{ palEcmat( double date, double rmat[3][3] ) } \sstarguments{ \sstsubsection{ date = double (Given) }{ TT as Modified Julian Date (JD-2400000.5). The difference between TT and TDB is of the order of a millisecond or two (i.e. about 0.02 arc-seconds). } \sstsubsection{ rmat = double[3][3] (Returned) }{ Rotation matrix } } } \sstroutine{ palEl2ue }{ Transform conventional elements into {\tt "}universal{\tt "} form }{ \sstdescription{ Transform conventional osculating elements into {\tt "}universal{\tt "} form. } \sstinvocation{ void palEl2ue ( double date, int jform, double epoch, double orbinc, double anode, double perih, double aorq, double e, double aorl, double dm, double u[13], int $*$jstat ); } \sstarguments{ \sstsubsection{ date = double (Given) }{ Epoch (TT MJD) of osculation (Note 3) } \sstsubsection{ jform = int (Given) }{ Element set actually returned (1-3; Note 6) } \sstsubsection{ epoch = double (Given) }{ Epoch of elements (TT MJD) } \sstsubsection{ orbinc = double (Given) }{ inclination (radians) } \sstsubsection{ anode = double (Given) }{ longitude of the ascending node (radians) } \sstsubsection{ perih = double (Given) }{ longitude or argument of perihelion (radians) } \sstsubsection{ aorq = double (Given) }{ mean distance or perihelion distance (AU) } \sstsubsection{ e = double (Given) }{ eccentricity } \sstsubsection{ aorl = double (Given) }{ mean anomaly or longitude (radians, JFORM=1,2 only) } \sstsubsection{ dm = double (Given) }{ daily motion (radians, JFORM=1 only) } \sstsubsection{ u = double [13] (Returned) }{ Universal orbital elements (Note 1) (0) combined mass (M$+$m) (1) total energy of the orbit (alpha) (2) reference (osculating) epoch (t0) (3-5) position at reference epoch (r0) (6-8) velocity at reference epoch (v0) (9) heliocentric distance at reference epoch (10) r0.v0 (11) date (t) (12) universal eccentric anomaly (psi) of date, approx } \sstsubsection{ jstat = int $*$ (Returned) }{ status: 0 = OK \sstitemlist{ \sstitem 1 = illegal JFORM \sstitem 2 = illegal E \sstitem 3 = illegal AORQ \sstitem 4 = illegal DM \sstitem 5 = numerical error } } } \sstnotes{ \sstitemlist{ \sstitem The {\tt "}universal{\tt "} elements are those which define the orbit for the purposes of the method of universal variables (see reference). They consist of the combined mass of the two bodies, an epoch, and the position and velocity vectors (arbitrary reference frame) at that epoch. The parameter set used here includes also various quantities that can, in fact, be derived from the other information. This approach is taken to avoiding unnecessary computation and loss of accuracy. The supplementary quantities are (i) alpha, which is proportional to the total energy of the orbit, (ii) the heliocentric distance at epoch, (iii) the outwards component of the velocity at the given epoch, (iv) an estimate of psi, the {\tt "}universal eccentric anomaly{\tt "} at a given date and (v) that date. \sstitem The companion routine is palUe2pv. This takes the set of numbers that the present routine outputs and uses them to derive the object{\tt '}s position and velocity. A single prediction requires one call to the present routine followed by one call to palUe2pv; for convenience, the two calls are packaged as the routine palPlanel. Multiple predictions may be made by again calling the present routine once, but then calling palUe2pv multiple times, which is faster than multiple calls to palPlanel. \sstitem DATE is the epoch of osculation. It is in the TT timescale (formerly Ephemeris Time, ET) and is a Modified Julian Date (JD-2400000.5). \sstitem The supplied orbital elements are with respect to the J2000 ecliptic and equinox. The position and velocity parameters returned in the array U are with respect to the mean equator and equinox of epoch J2000, and are for the perihelion prior to the specified epoch. \sstitem The universal elements returned in the array U are in canonical units (solar masses, AU and canonical days). \sstitem Three different element-format options are available: } Option JFORM=1, suitable for the major planets: EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = longitude of perihelion, curly pi (radians) AORQ = mean distance, a (AU) E = eccentricity, e (range 0 to $<$1) AORL = mean longitude L (radians) DM = daily motion (radians) Option JFORM=2, suitable for minor planets: EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = mean distance, a (AU) E = eccentricity, e (range 0 to $<$1) AORL = mean anomaly M (radians) Option JFORM=3, suitable for comets: EPOCH = epoch of perihelion (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = perihelion distance, q (AU) E = eccentricity, e (range 0 to 10) \sstitemlist{ \sstitem Unused elements (DM for JFORM=2, AORL and DM for JFORM=3) are not accessed. \sstitem The algorithm was originally adapted from the EPHSLA program of D.H.P.Jones (private communication, 1996). The method is based on Stumpff{\tt '}s Universal Variables. } } \sstdiytopic{ See Also }{ Everhart \& Pitkin, Am.J.Phys. 51, 712 (1983). } } \sstroutine{ palEpco }{ Convert an epoch into the appropriate form - {\tt '}B{\tt '} or {\tt '}J{\tt '} }{ \sstdescription{ Converts a Besselian or Julian epoch to a Julian or Besselian epoch. } \sstinvocation{ double palEpco( char k0, char k, double e ); } \sstarguments{ \sstsubsection{ k0 = char (Given) }{ Form of result: {\tt '}B{\tt '}=Besselian, {\tt '}J{\tt '}=Julian } \sstsubsection{ k = char (Given) }{ Form of given epoch: {\tt '}B{\tt '} or {\tt '}J{\tt '}. } } \sstnotes{ \sstitemlist{ \sstitem The result is always either equal to or very close to the given epoch E. The routine is required only in applications where punctilious treatment of heterogeneous mixtures of star positions is necessary. \sstitem k and k0 are case insensitive. This differes slightly from the Fortran SLA implementation. \sstitem k and k0 are not validated. They are interpreted as follows: o If k0 and k are the same the result is e o If k0 is {\tt '}b{\tt '} or {\tt '}B{\tt '} and k isn{\tt '}t the conversion is J to B. o In all other cases, the conversion is B to J. } } } \sstroutine{ palEpv }{ Earth position and velocity with respect to the BCRS }{ \sstdescription{ Earth position and velocity, heliocentric and barycentric, with respect to the Barycentric Celestial Reference System. } \sstinvocation{ void palEpv( double date, double ph[3], double vh[3], double pb[3], double vb[3] ); } \sstarguments{ \sstsubsection{ date = double (Given) }{ Date, TDB Modified Julian Date (JD-2400000.5) } \sstsubsection{ ph = double [3] (Returned) }{ Heliocentric Earth position (AU) } \sstsubsection{ vh = double [3] (Returned) }{ Heliocentric Earth velocity (AU/day) } \sstsubsection{ pb = double [3] (Returned) }{ Barycentric Earth position (AU) } \sstsubsection{ vb = double [3] (Returned) }{ Barycentric Earth velocity (AU/day) } } \sstnotes{ \sstitemlist{ \sstitem See iauEpv00 for details on accuracy \sstitem Note that the status argument from iauEpv00 is ignored } } } \sstroutine{ palEtrms }{ Compute the E-terms vector }{ \sstdescription{ Computes the E-terms (elliptic component of annual aberration) vector. Note the use of the J2000 aberration constant (20.49552 arcsec). This is a reflection of the fact that the E-terms embodied in existing star catalogues were computed from a variety of aberration constants. Rather than adopting one of the old constants the latest value is used here. } \sstinvocation{ void palEtrms ( double ep, double ev[3] ); } \sstarguments{ \sstsubsection{ ep = double (Given) }{ Besselian epoch } \sstsubsection{ ev = double [3] (Returned) }{ E-terms as (dx,dy,dz) } } \sstdiytopic{ See also }{ \sstitemlist{ \sstitem Smith, C.A. et al., 1989. Astr.J. 97, 265. \sstitem Yallop, B.D. et al., 1989. Astr.J. 97, 274. } } } \sstroutine{ palEqecl }{ Transform from J2000.0 equatorial coordinates to ecliptic coordinates }{ \sstdescription{ Transform from J2000.0 equatorial coordinates to ecliptic coordinates. } \sstinvocation{ void palEqecl( double dr, double dd, double date, double $*$dl, double $*$db); } \sstarguments{ \sstsubsection{ dr = double (Given) }{ J2000.0 mean RA (radians) } \sstsubsection{ dd = double (Given) }{ J2000.0 mean Dec (Radians) } \sstsubsection{ date = double (Given) }{ TT as Modified Julian Date (JD-2400000.5). The difference between TT and TDB is of the order of a millisecond or two (i.e. about 0.02 arc-seconds). } \sstsubsection{ dl = double $*$ (Returned) }{ Ecliptic longitude (mean of date, IAU 1980 theory, radians) } \sstsubsection{ db = double $*$ (Returned) }{ Ecliptic latitude (mean of date, IAU 1980 theory, radians) } } } \sstroutine{ palEqgal }{ Convert from J2000.0 equatorial coordinates to Galactic }{ \sstdescription{ Transformation from J2000.0 equatorial coordinates to IAU 1958 galactic coordinates. } \sstinvocation{ void palEqgal ( double dr, double dd, double $*$dl, double $*$db ); } \sstarguments{ \sstsubsection{ dr = double (Given) }{ J2000.0 RA (radians) } \sstsubsection{ dd = double (Given) }{ J2000.0 Dec (radians } \sstsubsection{ dl = double $*$ (Returned) }{ Galactic longitude (radians). } \sstsubsection{ db = double $*$ (Returned) }{ Galactic latitude (radians). } } \sstnotes{ The equatorial coordinates are J2000.0. Use the routine palGe50 if conversion to B1950.0 {\tt '}FK4{\tt '} coordinates is required. } \sstdiytopic{ See Also }{ Blaauw et al, Mon.Not.R.Astron.Soc.,121,123 (1960) } } \sstroutine{ palEvp }{ Returns the barycentric and heliocentric velocity and position of the Earth }{ \sstdescription{ Returns the barycentric and heliocentric velocity and position of the Earth at a given epoch, given with respect to a specified equinox. For information about accuracy, see the function iauEpv00. } \sstinvocation{ void palEvp( double date, double deqx, double dvb[3], double dpb[3], double dvh[3], double dph[3] ) } \sstarguments{ \sstsubsection{ date = double (Given) }{ TDB (loosely ET) as a Modified Julian Date (JD-2400000.5) } \sstsubsection{ deqx = double (Given) }{ Julian epoch (e.g. 2000.0) of mean equator and equinox of the vectors returned. If deqx $<$= 0.0, all vectors are referred to the mean equator and equinox (FK5) of epoch date. } \sstsubsection{ dvb = double[3] (Returned) }{ Barycentric velocity (AU/s, AU) } \sstsubsection{ dpb = double[3] (Returned) }{ Barycentric position (AU/s, AU) } \sstsubsection{ dvh = double[3] (Returned) }{ heliocentric velocity (AU/s, AU) } \sstsubsection{ dph = double[3] (Returned) }{ Heliocentric position (AU/s, AU) } } } \sstroutine{ palFk45z }{ Convert B1950.0 FK4 star data to J2000.0 FK5 assuming zero proper motion in the FK5 frame }{ \sstdescription{ Convert B1950.0 FK4 star data to J2000.0 FK5 assuming zero proper motion in the FK5 frame (double precision) This function converts stars from the Bessel-Newcomb, FK4 system to the IAU 1976, FK5, Fricke system, in such a way that the FK5 proper motion is zero. Because such a star has, in general, a non-zero proper motion in the FK4 system, the routine requires the epoch at which the position in the FK4 system was determined. The method is from Appendix 2 of Ref 1, but using the constants of Ref 4. } \sstinvocation{ palFk45z( double r1950, double d1950, double bepoch, double $*$r2000, double $*$d2000 ) } \sstarguments{ \sstsubsection{ r1950 = double (Given) }{ B1950.0 FK4 RA at epoch (radians). } \sstsubsection{ d1950 = double (Given) }{ B1950.0 FK4 Dec at epoch (radians). } \sstsubsection{ bepoch = double (Given) }{ Besselian epoch (e.g. 1979.3) } \sstsubsection{ r2000 = double (Returned) }{ J2000.0 FK5 RA (Radians). } \sstsubsection{ d2000 = double (Returned) }{ J2000.0 FK5 Dec(Radians). } } \sstnotes{ \sstitemlist{ \sstitem The epoch BEPOCH is strictly speaking Besselian, but if a Julian epoch is supplied the result will be affected only to a negligible extent. \sstitem Conversion from Besselian epoch 1950.0 to Julian epoch 2000.0 only is provided for. Conversions involving other epochs will require use of the appropriate precession, proper motion, and E-terms routines before and/or after palFk45z is called. \sstitem In the FK4 catalogue the proper motions of stars within 10 degrees of the poles do not embody the differential E-term effect and should, strictly speaking, be handled in a different manner from stars outside these regions. However, given the general lack of homogeneity of the star data available for routine astrometry, the difficulties of handling positions that may have been determined from astrometric fields spanning the polar and non-polar regions, the likelihood that the differential E-terms effect was not taken into account when allowing for proper motion in past astrometry, and the undesirability of a discontinuity in the algorithm, the decision has been made in this routine to include the effect of differential E-terms on the proper motions for all stars, whether polar or not. At epoch 2000, and measuring on the sky rather than in terms of dRA, the errors resulting from this simplification are less than 1 milliarcsecond in position and 1 milliarcsecond per century in proper motion. } } \sstdiytopic{ References }{ \sstitemlist{ \sstitem Aoki,S., et al, 1983. Astron.Astrophys., 128, 263. \sstitem Smith, C.A. et al, 1989. {\tt "}The transformation of astrometric catalog systems to the equinox J2000.0{\tt "}. Astron.J. 97, 265. \sstitem Yallop, B.D. et al, 1989. {\tt "}Transformation of mean star places from FK4 B1950.0 to FK5 J2000.0 using matrices in 6-space{\tt "}. Astron.J. 97, 274. \sstitem Seidelmann, P.K. (ed), 1992. {\tt "}Explanatory Supplement to the Astronomical Almanac{\tt "}, ISBN 0-935702-68-7. } } } \sstroutine{ palFk524 }{ Convert J2000.0 FK5 star data to B1950.0 FK4 }{ \sstdescription{ This function converts stars from the IAU 1976, FK5, Fricke system, to the Bessel-Newcomb, FK4 system. The precepts of Smith et al (Ref 1) are followed, using the implementation by Yallop et al (Ref 2) of a matrix method due to Standish. Kinoshita{\tt '}s development of Andoyer{\tt '}s post-Newcomb precession is used. The numerical constants from Seidelmann et al (Ref 3) are used canonically. } \sstinvocation{ palFk524( double r2000, double d2000, double dr2000, double dd2000, double p2000, double v2000, double $*$r1950, double $*$d1950, double $*$dr1950, double $*$dd1950, double $*$p1950, double $*$v1950 ) } \sstarguments{ \sstsubsection{ r2000 = double (Given) }{ J2000.0 FK5 RA (radians). } \sstsubsection{ d2000 = double (Given) }{ J2000.0 FK5 Dec (radians). } \sstsubsection{ dr2000 = double (Given) }{ J2000.0 FK5 RA proper motion (rad/Jul.yr) } \sstsubsection{ dd2000 = double (Given) }{ J2000.0 FK5 Dec proper motion (rad/Jul.yr) } \sstsubsection{ p2000 = double (Given) }{ J2000.0 FK5 parallax (arcsec) } \sstsubsection{ v2000 = double (Given) }{ J2000.0 FK5 radial velocity (km/s, $+$ve = moving away) } \sstsubsection{ r1950 = double $*$ (Returned) }{ B1950.0 FK4 RA (radians). } \sstsubsection{ d1950 = double $*$ (Returned) }{ B1950.0 FK4 Dec (radians). } \sstsubsection{ dr1950 = double $*$ (Returned) }{ B1950.0 FK4 RA proper motion (rad/Jul.yr) } \sstsubsection{ dd1950 = double $*$ (Returned) }{ B1950.0 FK4 Dec proper motion (rad/Jul.yr) } \sstsubsection{ p1950 = double $*$ (Returned) }{ B1950.0 FK4 parallax (arcsec) } \sstsubsection{ v1950 = double $*$ (Returned) }{ B1950.0 FK4 radial velocity (km/s, $+$ve = moving away) } } \sstnotes{ \sstitemlist{ \sstitem The proper motions in RA are dRA/dt rather than cos(Dec)$*$dRA/dt, and are per year rather than per century. \sstitem Note that conversion from Julian epoch 2000.0 to Besselian epoch 1950.0 only is provided for. Conversions involving other epochs will require use of the appropriate precession, proper motion, and E-terms routines before and/or after FK524 is called. \sstitem In the FK4 catalogue the proper motions of stars within 10 degrees of the poles do not embody the differential E-term effect and should, strictly speaking, be handled in a different manner from stars outside these regions. However, given the general lack of homogeneity of the star data available for routine astrometry, the difficulties of handling positions that may have been determined from astrometric fields spanning the polar and non-polar regions, the likelihood that the differential E-terms effect was not taken into account when allowing for proper motion in past astrometry, and the undesirability of a discontinuity in the algorithm, the decision has been made in this routine to include the effect of differential E-terms on the proper motions for all stars, whether polar or not. At epoch 2000, and measuring on the sky rather than in terms of dRA, the errors resulting from this simplification are less than 1 milliarcsecond in position and 1 milliarcsecond per century in proper motion. } } \sstdiytopic{ References }{ \sstitemlist{ \sstitem Smith, C.A. et al, 1989. {\tt "}The transformation of astrometric catalog systems to the equinox J2000.0{\tt "}. Astron.J. 97, 265. \sstitem Yallop, B.D. et al, 1989. {\tt "}Transformation of mean star places from FK4 B1950.0 to FK5 J2000.0 using matrices in 6-space{\tt "}. Astron.J. 97, 274. \sstitem Seidelmann, P.K. (ed), 1992. {\tt "}Explanatory Supplement to the Astronomical Almanac{\tt "}, ISBN 0-935702-68-7. } } } \sstroutine{ palFk54z }{ Convert a J2000.0 FK5 star position to B1950.0 FK4 assuming zero proper motion and parallax }{ \sstdescription{ This function converts star positions from the IAU 1976, FK5, Fricke system to the Bessel-Newcomb, FK4 system. } \sstinvocation{ palFk54z( double r2000, double d2000, double bepoch, double $*$r1950, double $*$d1950, double $*$dr1950, double $*$dd1950 ) } \sstarguments{ \sstsubsection{ r2000 = double (Given) }{ J2000.0 FK5 RA (radians). } \sstsubsection{ d2000 = double (Given) }{ J2000.0 FK5 Dec (radians). } \sstsubsection{ bepoch = double (Given) }{ Besselian epoch (e.g. 1950.0). } \sstsubsection{ r1950 = double $*$ (Returned) }{ B1950 FK4 RA (radians) at epoch {\tt "}bepoch{\tt "}. } \sstsubsection{ d1950 = double $*$ (Returned) }{ B1950 FK4 Dec (radians) at epoch {\tt "}bepoch{\tt "}. } \sstsubsection{ dr1950 = double $*$ (Returned) }{ B1950 FK4 proper motion (RA) (radians/trop.yr)). } \sstsubsection{ dr1950 = double $*$ (Returned) }{ B1950 FK4 proper motion (Dec) (radians/trop.yr)). } } \sstnotes{ \sstitemlist{ \sstitem The proper motion in RA is dRA/dt rather than cos(Dec)$*$dRA/dt. \sstitem Conversion from Julian epoch 2000.0 to Besselian epoch 1950.0 only is provided for. Conversions involving other epochs will require use of the appropriate precession functions before and after this function is called. \sstitem The FK5 proper motions, the parallax and the radial velocity are presumed zero. \sstitem It is the intention that FK5 should be a close approximation to an inertial frame, so that distant objects have zero proper motion; such objects have (in general) non-zero proper motion in FK4, and this function returns those fictitious proper motions. \sstitem The position returned by this function is in the B1950 reference frame but at Besselian epoch BEPOCH. For comparison with catalogues the {\tt "}bepoch{\tt "} argument will frequently be 1950.0. } } } \sstroutine{ palGaleq }{ Convert from galactic to J2000.0 equatorial coordinates }{ \sstdescription{ Transformation from IAU 1958 galactic coordinates to J2000.0 equatorial coordinates. } \sstinvocation{ void palGaleq ( double dl, double db, double $*$dr, double $*$dd ); } \sstarguments{ \sstsubsection{ dl = double (Given) }{ Galactic longitude (radians). } \sstsubsection{ db = double (Given) }{ Galactic latitude (radians). } \sstsubsection{ dr = double $*$ (Returned) }{ J2000.0 RA (radians) } \sstsubsection{ dd = double $*$ (Returned) }{ J2000.0 Dec (radians) } } \sstnotes{ The equatorial coordinates are J2000.0. Use the routine palGe50 if conversion to B1950.0 {\tt '}FK4{\tt '} coordinates is required. } \sstdiytopic{ See Also }{ Blaauw et al, Mon.Not.R.Astron.Soc.,121,123 (1960) } } \sstroutine{ palGalsup }{ Convert from galactic to supergalactic coordinates }{ \sstdescription{ Transformation from IAU 1958 galactic coordinates to de Vaucouleurs supergalactic coordinates. } \sstinvocation{ void palGalsup ( double dl, double db, double $*$dsl, double $*$dsb ); } \sstarguments{ \sstsubsection{ dl = double (Given) }{ Galactic longitude. } \sstsubsection{ db = double (Given) }{ Galactic latitude. } \sstsubsection{ dsl = double $*$ (Returned) }{ Supergalactic longitude. } \sstsubsection{ dsb = double $*$ (Returned) }{ Supergalactic latitude. } } \sstdiytopic{ See Also }{ \sstitemlist{ \sstitem de Vaucouleurs, de Vaucouleurs, \& Corwin, Second Reference Catalogue of Bright Galaxies, U. Texas, page 8. \sstitem Systems \& Applied Sciences Corp., Documentation for the machine-readable version of the above catalogue, Contract NAS 5-26490. } (These two references give different values for the galactic longitude of the supergalactic origin. Both are wrong; the correct value is L2=137.37.) } } \sstroutine{ palGe50 }{ Transform Galactic Coordinate to B1950 FK4 }{ \sstdescription{ Transformation from IAU 1958 galactic coordinates to B1950.0 {\tt '}FK4{\tt '} equatorial coordinates. } \sstinvocation{ palGe50( double dl, double db, double $*$dr, double $*$dd ); } \sstarguments{ \sstsubsection{ dl = double (Given) }{ Galactic longitude (radians) } \sstsubsection{ db = double (Given) }{ Galactic latitude (radians) } \sstsubsection{ dr = double $*$ (Returned) }{ B9150.0 FK4 RA. } \sstsubsection{ dd = double $*$ (Returned) }{ B1950.0 FK4 Dec. } } \sstnotes{ \sstitemlist{ \sstitem The equatorial coordinates are B1950.0 {\tt '}FK4{\tt '}. Use the routine palGaleq if conversion to J2000.0 coordinates is required. } } \sstdiytopic{ See Also }{ \sstitemlist{ \sstitem Blaauw et al, Mon.Not.R.Astron.Soc.,121,123 (1960) } } } \sstroutine{ palGeoc }{ Convert geodetic position to geocentric }{ \sstdescription{ Convert geodetic position to geocentric. } \sstinvocation{ void palGeoc( double p, double h, double $*$ r, double $*$z ); } \sstarguments{ \sstsubsection{ p = double (Given) }{ latitude (radians) } \sstsubsection{ h = double (Given) }{ height above reference spheroid (geodetic, metres) } \sstsubsection{ r = double $*$ (Returned) }{ distance from Earth axis (AU) } \sstsubsection{ z = double $*$ (Returned) }{ distance from plane of Earth equator (AU) } } \sstnotes{ \sstitemlist{ \sstitem Geocentric latitude can be obtained by evaluating atan2(z,r) \sstitem Uses WGS84 reference ellipsoid and calls iauGd2gc } } } \sstroutine{ palIntin }{ Convert free-format input into an integer }{ \sstdescription{ Extracts a number from an input string starting at the specified index. } \sstinvocation{ void palIntin( const char $*$ string, int $*$nstrt, long $*$ireslt, int $*$jflag ); } \sstarguments{ \sstsubsection{ string = const char $*$ (Given) }{ String containing number to be decoded. } \sstsubsection{ nstrt = int $*$ (Given and Returned) }{ Character number indicating where decoding should start. On output its value is updated to be the location of the possible next value. For compatibility with SLA the first character is index 1. } \sstsubsection{ ireslt = long $*$ (Returned) }{ Result. Not updated when jflag=1. } \sstsubsection{ jflag = int $*$ (Returned) }{ status: -1 = -OK, 0 = $+$OK, 1 = null, 2 = error } } \sstnotes{ \sstitemlist{ \sstitem Uses the strtol() system call to do the parsing. This may lead to subtle differences when compared to the SLA/F parsing. \sstitem Commas are recognized as a special case and are skipped if one happens to be the next character when updating nstrt. Additionally the output nstrt position will skip past any trailing space. \sstitem If no number can be found flag will be set to 1. \sstitem If the number overflows or underflows jflag will be set to 2. For overflow the returned result will have the value LONG\_MAX, for underflow it will have the value LONG\_MIN. } } } \sstroutine{ palMap }{ Convert star RA,Dec from mean place to geocentric apparent }{ \sstdescription{ Convert star RA,Dec from mean place to geocentric apparent. } \sstinvocation{ void palMap( double rm, double dm, double pr, double pd, double px, double rv, double eq, double date, double $*$ra, double $*$da ); } \sstarguments{ \sstsubsection{ rm = double (Given) }{ Mean RA (radians) } \sstsubsection{ dm = double (Given) }{ Mean declination (radians) } \sstsubsection{ pr = double (Given) }{ RA proper motion, changes per Julian year (radians) } \sstsubsection{ pd = double (Given) }{ Dec proper motion, changes per Julian year (radians) } \sstsubsection{ px = double (Given) }{ Parallax (arcsec) } \sstsubsection{ rv = double (Given) }{ Radial velocity (km/s, $+$ve if receding) } \sstsubsection{ eq = double (Given) }{ Epoch and equinox of star data (Julian) } \sstsubsection{ date = double (Given) }{ TDB for apparent place (JD-2400000.5) } \sstsubsection{ ra = double $*$ (Returned) }{ Apparent RA (radians) } \sstsubsection{ dec = double $*$ (Returned) }{ Apparent dec (radians) } } \sstnotes{ \sstitemlist{ \sstitem Calls palMappa and palMapqk \sstitem The reference systems and timescales used are IAU 2006. } } } \sstroutine{ palMappa }{ Compute parameters needed by palAmpqk and palMapqk }{ \sstdescription{ Compute star-independent parameters in preparation for transformations between mean place and geocentric apparent place. The parameters produced by this function are required in the parallax, aberration, and nutation/bias/precession parts of the mean/apparent transformations. The reference systems and timescales used are IAU 2006. } \sstinvocation{ void palMappa( double eq, double date, double amprms[21] ) } \sstarguments{ \sstsubsection{ eq = double (Given) }{ epoch of mean equinox to be used (Julian) } \sstsubsection{ date = double (Given) }{ TDB (JD-2400000.5) } \sstsubsection{ amprms = double[21] (Returned) }{ star-independent mean-to-apparent parameters: \sstitemlist{ \sstitem (0) time interval for proper motion (Julian years) \sstitem (1-3) barycentric position of the Earth (AU) \sstitem (4-6) heliocentric direction of the Earth (unit vector) \sstitem (7) (grav rad Sun)$*$2/(Sun-Earth distance) \sstitem (8-10) abv: barycentric Earth velocity in units of c \sstitem (11) sqrt(1-v$*$$*$2) where v=modulus(abv) \sstitem (12-20) precession/nutation (3,3) matrix } } } \sstnotes{ \sstitemlist{ \sstitem For date, the distinction between the required TDB and TT is always negligible. Moreover, for all but the most critical applications UTC is adequate. \sstitem The vector amprms(1-3) is referred to the mean equinox and equator of epoch eq. \sstitem The parameters amprms produced by this function are used by palAmpqk, palMapqk and palMapqkz. } } } \sstroutine{ palMapqk }{ Quick mean to apparent place }{ \sstdescription{ Quick mean to apparent place: transform a star RA,Dec from mean place to geocentric apparent place, given the star-independent parameters. Use of this routine is appropriate when efficiency is important and where many star positions, all referred to the same equator and equinox, are to be transformed for one epoch. The star-independent parameters can be obtained by calling the palMappa routine. If the parallax and proper motions are zero the palMapqkz routine can be used instead. } \sstinvocation{ void palMapqk ( double rm, double dm, double pr, double pd, double px, double rv, double amprms[21], double $*$ra, double $*$da ); } \sstarguments{ \sstsubsection{ rm = double (Given) }{ Mean RA (radians) } \sstsubsection{ dm = double (Given) }{ Mean declination (radians) } \sstsubsection{ pr = double (Given) }{ RA proper motion, changes per Julian year (radians) } \sstsubsection{ pd = double (Given) }{ Dec proper motion, changes per Julian year (radians) } \sstsubsection{ px = double (Given) }{ Parallax (arcsec) } \sstsubsection{ rv = double (Given) }{ Radial velocity (km/s, $+$ve if receding) } \sstsubsection{ amprms = double [21] (Given) }{ Star-independent mean-to-apparent parameters (see palMappa). } \sstsubsection{ ra = double $*$ (Returned) }{ Apparent RA (radians) } \sstsubsection{ dec = double $*$ (Returned) }{ Apparent dec (radians) } } \sstnotes{ \sstitemlist{ \sstitem The reference frames and timescales used are post IAU 2006. } } } \sstroutine{ palMapqkz }{ Quick mean to apparent place }{ \sstdescription{ Quick mean to apparent place: transform a star RA,dec from mean place to geocentric apparent place, given the star-independent parameters, and assuming zero parallax and proper motion. Use of this function is appropriate when efficiency is important and where many star positions, all with parallax and proper motion either zero or already allowed for, and all referred to the same equator and equinox, are to be transformed for one epoch. The star-independent parameters can be obtained by calling the palMappa function. The corresponding function for the case of non-zero parallax and proper motion is palMapqk. The reference systems and timescales used are IAU 2006. Strictly speaking, the function is not valid for solar-system sources, though the error will usually be extremely small. } \sstinvocation{ void palMapqkz( double rm, double dm, double amprms[21], double $*$ra, double $*$da ) } \sstarguments{ \sstsubsection{ rm = double (Given) }{ Mean RA (radians). } \sstsubsection{ dm = double (Given) }{ Mean Dec (radians). } \sstsubsection{ amprms = double[21] (Given) }{ Star-independent mean-to-apparent parameters (see palMappa): (0-3) not used (4-6) not used (7) not used (8-10) abv: barycentric Earth velocity in units of c (11) sqrt(1-v$*$$*$2) where v=modulus(abv) (12-20) precession/nutation (3,3) matrix } \sstsubsection{ ra = double $*$ (Returned) }{ Apparent RA (radians). } \sstsubsection{ da = double $*$ (Returned) }{ Apparent Dec (radians). } } } \sstroutine{ palNut }{ Form the matrix of nutation }{ \sstdescription{ Form the matrix of nutation for a given date using the IAU 2006 nutation model and palDeuler. } \sstinvocation{ void palNut( double date, double rmatn[3][3] ); } \sstarguments{ \sstsubsection{ date = double (Given) }{ TT as modified Julian date (JD-2400000.5) } \sstsubsection{ rmatn = double [3][3] (Returned) }{ Nutation matrix in the sense v(true)=rmatn $*$ v(mean) where v(true) is the star vector relative to the true equator and equinox of date and v(mean) is the star vector relative to the mean equator and equinox of date. } } \sstnotes{ \sstitemlist{ \sstitem Uses iauNut06a via palNutc \sstitem The distinction between TDB and TT is negligible. For all but the most critical applications UTC is adequate. } } } \sstroutine{ palNutc }{ Calculate nutation longitude \& obliquoty components }{ \sstdescription{ Calculates the longitude $*$ obliquity components and mean obliquity using the SOFA library. } \sstinvocation{ void palNutc( double date, double $*$ dpsi, double $*$deps, double $*$eps0 ); } \sstarguments{ \sstsubsection{ date = double (Given) }{ TT as modified Julian date (JD-2400000.5) } \sstsubsection{ dpsi = double $*$ (Returned) }{ Nutation in longitude } \sstsubsection{ deps = double $*$ (Returned) }{ Nutation in obliquity } \sstsubsection{ eps0 = double $*$ (Returned) }{ Mean obliquity. } } \sstnotes{ \sstitemlist{ \sstitem Calls iauObl06 and iauNut06a and therefore uses the IAU 206 precession/nutation model. \sstitem Note the change from SLA/F regarding the date. TT is used rather than TDB. } } } \sstroutine{ palObs }{ Parameters of selected ground-based observing stations }{ \sstdescription{ Station numbers, identifiers, names and other details are subject to change and should not be hardwired into application programs. All characters in {\tt "}c{\tt "} up to the first space are checked; thus an abbreviated ID will return the parameters for the first station in the list which matches the abbreviation supplied, and no station in the list will ever contain embedded spaces. {\tt "}c{\tt "} must not have leading spaces. IMPORTANT -- BEWARE OF THE LONGITUDE SIGN CONVENTION. The longitude returned by sla\_OBS is west-positive in accordance with astronomical usage. However, this sign convention is left-handed and is the opposite of the one used by geographers; elsewhere in PAL the preferable east-positive convention is used. In particular, note that for use in palAop, palAoppa and palOap the sign of the longitude must be reversed. Users are urged to inform the author of any improvements they would like to see made. For example: typographical corrections more accurate parameters better station identifiers or names additional stations } \sstinvocation{ int palObs( size\_t n, const char $*$ c, char $*$ ident, size\_t identlen, char $*$ name, size\_t namelen, double $*$ w, double $*$ p, double $*$ h ); } \sstarguments{ \sstsubsection{ n = size\_t (Given) }{ Number specifying the observing station. If 0 the identifier in {\tt "}c{\tt "} is used to determine the observing station to use. } \sstsubsection{ c = const char $*$ (Given) }{ Identifier specifying the observing station for which the parameters should be returned. Only used if n is 0. Can be NULL for n$>$0. Case insensitive. } \sstsubsection{ ident = char $*$ (Returned) }{ Identifier of the observing station selected. Will be identical to {\tt "}c{\tt "} if n==0. Unchanged if {\tt "}n{\tt "} or {\tt "}c{\tt "} do not match an observing station. Should be at least 11 characters (including the trailing nul). } \sstsubsection{ identlen = size\_t (Given) }{ Size of the buffer {\tt "}ident{\tt "} including trailing nul. } \sstsubsection{ name = char $*$ (Returned) }{ Full name of the specified observing station. Contains {\tt "}?{\tt "} if {\tt "}n{\tt "} or {\tt "}c{\tt "} did not correspond to a valid station. Should be at least 41 characters (including the trailing nul). } \sstsubsection{ w = double $*$ (Returned) }{ Longitude (radians, West $+$ve). Unchanged if observing station could not be identified. } \sstsubsection{ p = double $*$ (Returned) }{ Geodetic latitude (radians, North $+$ve). Unchanged if observing station could not be identified. } \sstsubsection{ h = double $*$ (Returned) }{ Height above sea level (metres). Unchanged if observing station could not be identified. } } \sstreturnedvalue{ \sstsubsection{ palObs = int }{ 0 if an observing station was returned. -1 if no match was found. } } \sstnotes{ \sstitemlist{ \sstitem Differs from the SLA interface in that the output short name is not the same variable as the input short name. This simplifies consting. Additionally the size of the output buffers are now specified in the API and a status integer is returned. } } } \sstroutine{ palPa }{ HA, Dec to Parallactic Angle }{ \sstdescription{ Converts HA, Dec to Parallactic Angle. } \sstinvocation{ double palPa( double ha, double dec, double phi ); } \sstarguments{ \sstsubsection{ ha = double (Given) }{ Hour angle in radians (Geocentric apparent) } \sstsubsection{ dec = double (Given) }{ Declination in radians (Geocentric apparent) } \sstsubsection{ phi = double (Given) }{ Observatory latitude in radians (geodetic) } } \sstreturnedvalue{ \sstsubsection{ palPa = double }{ Parallactic angle in the range -pi to $+$pi. } } \sstnotes{ \sstitemlist{ \sstitem The parallactic angle at a point in the sky is the position angle of the vertical, i.e. the angle between the direction to the pole and to the zenith. In precise applications care must be taken only to use geocentric apparent HA,Dec and to consider separately the effects of atmospheric refraction and telescope mount errors. \sstitem At the pole a zero result is returned. } } } \sstroutine{ palPertel }{ Update elements by applying planetary perturbations }{ \sstdescription{ Update the osculating orbital elements of an asteroid or comet by applying planetary perturbations. } \sstinvocation{ void palPertel (int jform, double date0, double date1, double epoch0, double orbi0, double anode0, double perih0, double aorq0, double e0, double am0, double $*$epoch1, double $*$orbi1, double $*$anode1, double $*$perih1, double $*$aorq1, double $*$e1, double $*$am1, int $*$jstat ); } \sstarguments{ \sstsubsection{ jform = int (Given) }{ Element set actually returned (1-3; Note 6) } \sstsubsection{ date0 = double (Given) }{ Date of osculation (TT MJD) for the given elements. } \sstsubsection{ date1 = double (Given) }{ Date of osculation (TT MJD) for the updated elements. } \sstsubsection{ epoch0 = double (Given) }{ Epoch of elements (TT MJD) } \sstsubsection{ orbi0 = double (Given) }{ inclination (radians) } \sstsubsection{ anode0 = double (Given) }{ longitude of the ascending node (radians) } \sstsubsection{ perih0 = double (Given) }{ longitude or argument of perihelion (radians) } \sstsubsection{ aorq0 = double (Given) }{ mean distance or perihelion distance (AU) } \sstsubsection{ e0 = double (Given) }{ eccentricity } \sstsubsection{ am0 = double (Given) }{ mean anomaly (radians, JFORM=2 only) } \sstsubsection{ epoch1 = double $*$ (Returned) }{ Epoch of elements (TT MJD) } \sstsubsection{ orbi1 = double $*$ (Returned) }{ inclination (radians) } \sstsubsection{ anode1 = double $*$ (Returned) }{ longitude of the ascending node (radians) } \sstsubsection{ perih1 = double $*$ (Returned) }{ longitude or argument of perihelion (radians) } \sstsubsection{ aorq1 = double $*$ (Returned) }{ mean distance or perihelion distance (AU) } \sstsubsection{ e1 = double $*$ (Returned) }{ eccentricity } \sstsubsection{ am1 = double $*$ (Returned) }{ mean anomaly (radians, JFORM=2 only) } \sstsubsection{ jstat = int $*$ (Returned) }{ status: \sstitemlist{ \sstitem $+$102 = warning, distant epoch \sstitem $+$101 = warning, large timespan ( $>$ 100 years) \sstitem $+$1 to $+$10 = coincident with planet (Note 6) \sstitem 0 = OK \sstitem -1 = illegal JFORM \sstitem -2 = illegal E0 \sstitem -3 = illegal AORQ0 \sstitem -4 = internal error \sstitem -5 = numerical error } } } \sstnotes{ \sstitemlist{ \sstitem Two different element-format options are available: } Option JFORM=2, suitable for minor planets: EPOCH = epoch of elements (TT MJD) ORBI = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = mean distance, a (AU) E = eccentricity, e AM = mean anomaly M (radians) Option JFORM=3, suitable for comets: EPOCH = epoch of perihelion (TT MJD) ORBI = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = perihelion distance, q (AU) E = eccentricity, e \sstitemlist{ \sstitem DATE0, DATE1, EPOCH0 and EPOCH1 are all instants of time in the TT timescale (formerly Ephemeris Time, ET), expressed as Modified Julian Dates (JD-2400000.5). } DATE0 is the instant at which the given (i.e. unperturbed) osculating elements are correct. DATE1 is the specified instant at which the updated osculating elements are correct. EPOCH0 and EPOCH1 will be the same as DATE0 and DATE1 (respectively) for the JFORM=2 case, normally used for minor planets. For the JFORM=3 case, the two epochs will refer to perihelion passage and so will not, in general, be the same as DATE0 and/or DATE1 though they may be similar to one another. \sstitemlist{ \sstitem The elements are with respect to the J2000 ecliptic and equinox. \sstitem Unused elements (AM0 and AM1 for JFORM=3) are not accessed. \sstitem See the palPertue routine for details of the algorithm used. \sstitem This routine is not intended to be used for major planets, which is why JFORM=1 is not available and why there is no opportunity to specify either the longitude of perihelion or the daily motion. However, if JFORM=2 elements are somehow obtained for a major planet and supplied to the routine, sensible results will, in fact, be produced. This happens because the sla\_PERTUE routine that is called to perform the calculations checks the separation between the body and each of the planets and interprets a suspiciously small value (0.001 AU) as an attempt to apply it to the planet concerned. If this condition is detected, the contribution from that planet is ignored, and the status is set to the planet number (1-10 = Mercury, Venus, EMB, Mars, Jupiter, Saturn, Uranus, Neptune, Earth, Moon) as a warning. } } \sstdiytopic{ See Also }{ \sstitemlist{ \sstitem Sterne, Theodore E., {\tt "}An Introduction to Celestial Mechanics{\tt "}, Interscience Publishers Inc., 1960. Section 6.7, p199. } } } \sstroutine{ palPertue }{ Update the universal elements by applying planetary perturbations }{ \sstdescription{ Update the universal elements of an asteroid or comet by applying planetary perturbations. } \sstinvocation{ void palPertue( double date, double u[13], int $*$jstat ); } \sstarguments{ \sstsubsection{ date = double (Given) }{ Final epoch (TT MJD) for the update elements. } \sstsubsection{ u = const double [13] (Given \& Returned) }{ Universal orbital elements (Note 1) (0) combined mass (M$+$m) (1) total energy of the orbit (alpha) (2) reference (osculating) epoch (t0) (3-5) position at reference epoch (r0) (6-8) velocity at reference epoch (v0) (9) heliocentric distance at reference epoch (10) r0.v0 (11) date (t) (12) universal eccentric anomaly (psi) of date, approx } \sstsubsection{ jstat = int $*$ (Returned) }{ status: $+$102 = warning, distant epoch $+$101 = warning, large timespan ( $>$ 100 years) $+$1 to $+$10 = coincident with major planet (Note 5) 0 = OK \sstitemlist{ \sstitem 1 = numerical error } } } \sstnotes{ \sstitemlist{ \sstitem The {\tt "}universal{\tt "} elements are those which define the orbit for the purposes of the method of universal variables (see reference 2). They consist of the combined mass of the two bodies, an epoch, and the position and velocity vectors (arbitrary reference frame) at that epoch. The parameter set used here includes also various quantities that can, in fact, be derived from the other information. This approach is taken to avoiding unnecessary computation and loss of accuracy. The supplementary quantities are (i) alpha, which is proportional to the total energy of the orbit, (ii) the heliocentric distance at epoch, (iii) the outwards component of the velocity at the given epoch, (iv) an estimate of psi, the {\tt "}universal eccentric anomaly{\tt "} at a given date and (v) that date. \sstitem The universal elements are with respect to the J2000 equator and equinox. \sstitem The epochs DATE, U(3) and U(12) are all Modified Julian Dates (JD-2400000.5). \sstitem The algorithm is a simplified form of Encke{\tt '}s method. It takes as a basis the unperturbed motion of the body, and numerically integrates the perturbing accelerations from the major planets. The expression used is essentially Sterne{\tt '}s 6.7-2 (reference 1). Everhart and Pitkin (reference 2) suggest rectifying the orbit at each integration step by propagating the new perturbed position and velocity as the new universal variables. In the present routine the orbit is rectified less frequently than this, in order to gain a slight speed advantage. However, the rectification is done directly in terms of position and velocity, as suggested by Everhart and Pitkin, bypassing the use of conventional orbital elements. } The f(q) part of the full Encke method is not used. The purpose of this part is to avoid subtracting two nearly equal quantities when calculating the {\tt "}indirect member{\tt "}, which takes account of the small change in the Sun{\tt '}s attraction due to the slightly displaced position of the perturbed body. A simpler, direct calculation in double precision proves to be faster and not significantly less accurate. Apart from employing a variable timestep, and occasionally {\tt "}rectifying the orbit{\tt "} to keep the indirect member small, the integration is done in a fairly straightforward way. The acceleration estimated for the middle of the timestep is assumed to apply throughout that timestep; it is also used in the extrapolation of the perturbations to the middle of the next timestep, to predict the new disturbed position. There is no iteration within a timestep. Measures are taken to reach a compromise between execution time and accuracy. The starting-point is the goal of achieving arcsecond accuracy for ordinary minor planets over a ten-year timespan. This goal dictates how large the timesteps can be, which in turn dictates how frequently the unperturbed motion has to be recalculated from the osculating elements. Within predetermined limits, the timestep for the numerical integration is varied in length in inverse proportion to the magnitude of the net acceleration on the body from the major planets. The numerical integration requires estimates of the major-planet motions. Approximate positions for the major planets (Pluto alone is omitted) are obtained from the routine palPlanet. Two levels of interpolation are used, to enhance speed without significantly degrading accuracy. At a low frequency, the routine palPlanet is called to generate updated position$+$velocity {\tt "}state vectors{\tt "}. The only task remaining to be carried out at the full frequency (i.e. at each integration step) is to use the state vectors to extrapolate the planetary positions. In place of a strictly linear extrapolation, some allowance is made for the curvature of the orbit by scaling back the radius vector as the linear extrapolation goes off at a tangent. Various other approximations are made. For example, perturbations by Pluto and the minor planets are neglected and relativistic effects are not taken into account. In the interests of simplicity, the background calculations for the major planets are carried out en masse. The mean elements and state vectors for all the planets are refreshed at the same time, without regard for orbit curvature, mass or proximity. The Earth-Moon system is treated as a single body when the body is distant but as separate bodies when closer to the EMB than the parameter RNE, which incurs a time penalty but improves accuracy for near-Earth objects. \sstitemlist{ \sstitem This routine is not intended to be used for major planets. However, if major-planet elements are supplied, sensible results will, in fact, be produced. This happens because the routine checks the separation between the body and each of the planets and interprets a suspiciously small value (0.001 AU) as an attempt to apply the routine to the planet concerned. If this condition is detected, the contribution from that planet is ignored, and the status is set to the planet number (1-10 = Mercury, Venus, EMB, Mars, Jupiter, Saturn, Uranus, Neptune, Earth, Moon) as a warning. } } \sstdiytopic{ See Also }{ \sstitemlist{ \sstitem Sterne, Theodore E., {\tt "}An Introduction to Celestial Mechanics{\tt "}, Interscience Publishers Inc., 1960. Section 6.7, p199. \sstitem Everhart, E. \& Pitkin, E.T., Am.J.Phys. 51, 712, 1983. } } } \sstroutine{ palPlanel }{ Transform conventional elements into position and velocity }{ \sstdescription{ Heliocentric position and velocity of a planet, asteroid or comet, starting from orbital elements. } \sstinvocation{ void palPlanel ( double date, int jform, double epoch, double orbinc, double anode, double perih, double aorq, double e, double aorl, double dm, double pv[6], int $*$jstat ); } \sstarguments{ \sstsubsection{ date = double (Given) }{ Epoch (TT MJD) of osculation (Note 1) } \sstsubsection{ jform = int (Given) }{ Element set actually returned (1-3; Note 3) } \sstsubsection{ epoch = double (Given) }{ Epoch of elements (TT MJD) (Note 4) } \sstsubsection{ orbinc = double (Given) }{ inclination (radians) } \sstsubsection{ anode = double (Given) }{ longitude of the ascending node (radians) } \sstsubsection{ perih = double (Given) }{ longitude or argument of perihelion (radians) } \sstsubsection{ aorq = double (Given) }{ mean distance or perihelion distance (AU) } \sstsubsection{ e = double (Given) }{ eccentricity } \sstsubsection{ aorl = double (Given) }{ mean anomaly or longitude (radians, JFORM=1,2 only) } \sstsubsection{ dm = double (Given) }{ daily motion (radians, JFORM=1 only) } \sstsubsection{ u = double [13] (Returned) }{ Universal orbital elements (Note 1) (0) combined mass (M$+$m) (1) total energy of the orbit (alpha) (2) reference (osculating) epoch (t0) (3-5) position at reference epoch (r0) (6-8) velocity at reference epoch (v0) (9) heliocentric distance at reference epoch (10) r0.v0 (11) date (t) (12) universal eccentric anomaly (psi) of date, approx } \sstsubsection{ jstat = int $*$ (Returned) }{ status: 0 = OK \sstitemlist{ \sstitem -1 = illegal JFORM \sstitem -2 = illegal E \sstitem -3 = illegal AORQ \sstitem -4 = illegal DM \sstitem -5 = numerical error } } } \sstnotes{ \sstitemlist{ \sstitem DATE is the instant for which the prediction is required. It is in the TT timescale (formerly Ephemeris Time, ET) and is a Modified Julian Date (JD-2400000.5). \sstitem The elements are with respect to the J2000 ecliptic and equinox. \sstitem A choice of three different element-set options is available: } Option JFORM = 1, suitable for the major planets: EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = longitude of perihelion, curly pi (radians) AORQ = mean distance, a (AU) E = eccentricity, e (range 0 to $<$1) AORL = mean longitude L (radians) DM = daily motion (radians) Option JFORM = 2, suitable for minor planets: EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = mean distance, a (AU) E = eccentricity, e (range 0 to $<$1) AORL = mean anomaly M (radians) Option JFORM = 3, suitable for comets: EPOCH = epoch of elements and perihelion (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = perihelion distance, q (AU) E = eccentricity, e (range 0 to 10) Unused arguments (DM for JFORM=2, AORL and DM for JFORM=3) are not accessed. \sstitemlist{ \sstitem Each of the three element sets defines an unperturbed heliocentric orbit. For a given epoch of observation, the position of the body in its orbit can be predicted from these elements, which are called {\tt "}osculating elements{\tt "}, using standard two-body analytical solutions. However, due to planetary perturbations, a given set of osculating elements remains usable for only as long as the unperturbed orbit that it describes is an adequate approximation to reality. Attached to such a set of elements is a date called the {\tt "}osculating epoch{\tt "}, at which the elements are, momentarily, a perfect representation of the instantaneous position and velocity of the body. } Therefore, for any given problem there are up to three different epochs in play, and it is vital to distinguish clearly between them: . The epoch of observation: the moment in time for which the position of the body is to be predicted. . The epoch defining the position of the body: the moment in time at which, in the absence of purturbations, the specified position (mean longitude, mean anomaly, or perihelion) is reached. . The osculating epoch: the moment in time at which the given elements are correct. For the major-planet and minor-planet cases it is usual to make the epoch that defines the position of the body the same as the epoch of osculation. Thus, only two different epochs are involved: the epoch of the elements and the epoch of observation. For comets, the epoch of perihelion fixes the position in the orbit and in general a different epoch of osculation will be chosen. Thus, all three types of epoch are involved. For the present routine: . The epoch of observation is the argument DATE. . The epoch defining the position of the body is the argument EPOCH. . The osculating epoch is not used and is assumed to be close enough to the epoch of observation to deliver adequate accuracy. If not, a preliminary call to sla\_PERTEL may be used to update the element-set (and its associated osculating epoch) by applying planetary perturbations. \sstitemlist{ \sstitem The reference frame for the result is with respect to the mean equator and equinox of epoch J2000. \sstitem The algorithm was originally adapted from the EPHSLA program of D.H.P.Jones (private communication, 1996). The method is based on Stumpff{\tt '}s Universal Variables. } } \sstdiytopic{ See Also }{ Everhart, E. \& Pitkin, E.T., Am.J.Phys. 51, 712, 1983. } } \sstroutine{ palPlanet }{ Approximate heliocentric position and velocity of major planet }{ \sstdescription{ Calculates the approximate heliocentric position and velocity of the specified major planet. } \sstinvocation{ void palPlanet ( double date, int np, double pv[6], int $*$j ); } \sstarguments{ \sstsubsection{ date = double (Given) }{ TDB Modified Julian Date (JD-2400000.5). } \sstsubsection{ np = int (Given) }{ planet (1=Mercury, 2=Venus, 3=EMB, 4=Mars, 5=Jupiter, 6=Saturn, 7=Uranus, 8=Neptune) } \sstsubsection{ pv = double [6] (Returned) }{ heliocentric x,y,z,xdot,ydot,zdot, J2000, equatorial triad in units AU and AU/s. } \sstsubsection{ j = int $*$ (Returned) }{ \sstitemlist{ \sstitem -2 = solution didn{\tt '}t converge. \sstitem -1 = illegal np (1-8) \sstitem 0 = OK \sstitem $+$1 = warning: year outside 1000-3000 } } } \sstnotes{ \sstitemlist{ \sstitem See SOFA iauPlan94 for details \sstitem Note that Pluto is supported in SLA/F but not in this routine \sstitem Status -2 is equivalent to iauPlan94 status $+$2. \sstitem Note that velocity units here match the SLA/F documentation. } } } \sstroutine{ palPlante }{ Topocentric RA,Dec of a Solar-System object from heliocentric orbital elements }{ \sstdescription{ Topocentric apparent RA,Dec of a Solar-System object whose heliocentric orbital elements are known. } \sstinvocation{ void palPlante ( double date, double elong, double phi, int jform, double epoch, double orbinc, double anode, double perih, double aorq, double e, double aorl, double dm, double $*$ra, double $*$dec, double $*$r, int $*$jstat ); } \sstarguments{ \sstsubsection{ date = double (Given) }{ TT MJD of observation (JD-2400000.5) } \sstsubsection{ elong = double (Given) }{ Observer{\tt '}s east longitude (radians) } \sstsubsection{ phi = double (Given) }{ Observer{\tt '}s geodetic latitude (radians) } \sstsubsection{ jform = int (Given) }{ Element set actually returned (1-3; Note 6) } \sstsubsection{ epoch = double (Given) }{ Epoch of elements (TT MJD) } \sstsubsection{ orbinc = double (Given) }{ inclination (radians) } \sstsubsection{ anode = double (Given) }{ longitude of the ascending node (radians) } \sstsubsection{ perih = double (Given) }{ longitude or argument of perihelion (radians) } \sstsubsection{ aorq = double (Given) }{ mean distance or perihelion distance (AU) } \sstsubsection{ e = double (Given) }{ eccentricity } \sstsubsection{ aorl = double (Given) }{ mean anomaly or longitude (radians, JFORM=1,2 only) } \sstsubsection{ dm = double (Given) }{ daily motion (radians, JFORM=1 only) } \sstsubsection{ ra = double $*$ (Returned) }{ Topocentric apparent RA (radians) } \sstsubsection{ dec = double $*$ (Returned) }{ Topocentric apparent Dec (radians) } \sstsubsection{ r = double $*$ (Returned) }{ Distance from observer (AU) } \sstsubsection{ jstat = int $*$ (Returned) }{ status: 0 = OK \sstitemlist{ \sstitem -1 = illegal jform \sstitem -2 = illegal e \sstitem -3 = illegal aorq \sstitem -4 = illegal dm \sstitem -5 = numerical error } } } \sstnotes{ \sstitemlist{ \sstitem DATE is the instant for which the prediction is required. It is in the TT timescale (formerly Ephemeris Time, ET) and is a Modified Julian Date (JD-2400000.5). \sstitem The longitude and latitude allow correction for geocentric parallax. This is usually a small effect, but can become important for near-Earth asteroids. Geocentric positions can be generated by appropriate use of routines palEpv (or palEvp) and palUe2pv. \sstitem The elements are with respect to the J2000 ecliptic and equinox. \sstitem A choice of three different element-set options is available: } Option JFORM = 1, suitable for the major planets: EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = longitude of perihelion, curly pi (radians) AORQ = mean distance, a (AU) E = eccentricity, e (range 0 to $<$1) AORL = mean longitude L (radians) DM = daily motion (radians) Option JFORM = 2, suitable for minor planets: EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = mean distance, a (AU) E = eccentricity, e (range 0 to $<$1) AORL = mean anomaly M (radians) Option JFORM = 3, suitable for comets: EPOCH = epoch of elements and perihelion (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = perihelion distance, q (AU) E = eccentricity, e (range 0 to 10) Unused arguments (DM for JFORM=2, AORL and DM for JFORM=3) are not accessed. \sstitemlist{ \sstitem Each of the three element sets defines an unperturbed heliocentric orbit. For a given epoch of observation, the position of the body in its orbit can be predicted from these elements, which are called {\tt "}osculating elements{\tt "}, using standard two-body analytical solutions. However, due to planetary perturbations, a given set of osculating elements remains usable for only as long as the unperturbed orbit that it describes is an adequate approximation to reality. Attached to such a set of elements is a date called the {\tt "}osculating epoch{\tt "}, at which the elements are, momentarily, a perfect representation of the instantaneous position and velocity of the body. } Therefore, for any given problem there are up to three different epochs in play, and it is vital to distinguish clearly between them: . The epoch of observation: the moment in time for which the position of the body is to be predicted. . The epoch defining the position of the body: the moment in time at which, in the absence of purturbations, the specified position (mean longitude, mean anomaly, or perihelion) is reached. . The osculating epoch: the moment in time at which the given elements are correct. For the major-planet and minor-planet cases it is usual to make the epoch that defines the position of the body the same as the epoch of osculation. Thus, only two different epochs are involved: the epoch of the elements and the epoch of observation. For comets, the epoch of perihelion fixes the position in the orbit and in general a different epoch of osculation will be chosen. Thus, all three types of epoch are involved. For the present routine: . The epoch of observation is the argument DATE. . The epoch defining the position of the body is the argument EPOCH. . The osculating epoch is not used and is assumed to be close enough to the epoch of observation to deliver adequate accuracy. If not, a preliminary call to sla\_PERTEL may be used to update the element-set (and its associated osculating epoch) by applying planetary perturbations. \sstitemlist{ \sstitem Two important sources for orbital elements are Horizons, operated by the Jet Propulsion Laboratory, Pasadena, and the Minor Planet Center, operated by the Center for Astrophysics, Harvard. } The JPL Horizons elements (heliocentric, J2000 ecliptic and equinox) correspond to SLALIB arguments as follows. Major planets: JFORM = 1 EPOCH = JDCT-2400000.5 ORBINC = IN (in radians) ANODE = OM (in radians) PERIH = OM$+$W (in radians) AORQ = A E = EC AORL = MA$+$OM$+$W (in radians) DM = N (in radians) Epoch of osculation = JDCT-2400000.5 Minor planets: JFORM = 2 EPOCH = JDCT-2400000.5 ORBINC = IN (in radians) ANODE = OM (in radians) PERIH = W (in radians) AORQ = A E = EC AORL = MA (in radians) Epoch of osculation = JDCT-2400000.5 Comets: JFORM = 3 EPOCH = Tp-2400000.5 ORBINC = IN (in radians) ANODE = OM (in radians) PERIH = W (in radians) AORQ = QR E = EC Epoch of osculation = JDCT-2400000.5 The MPC elements correspond to SLALIB arguments as follows. Minor planets: JFORM = 2 EPOCH = Epoch-2400000.5 ORBINC = Incl. (in radians) ANODE = Node (in radians) PERIH = Perih. (in radians) AORQ = a E = e AORL = M (in radians) Epoch of osculation = Epoch-2400000.5 Comets: JFORM = 3 EPOCH = T-2400000.5 ORBINC = Incl. (in radians) ANODE = Node. (in radians) PERIH = Perih. (in radians) AORQ = q E = e Epoch of osculation = Epoch-2400000.5 } } \sstroutine{ palPlantu }{ Topocentric RA,Dec of a Solar-System object from universal elements }{ \sstdescription{ Topocentric apparent RA,Dec of a Solar-System object whose heliocentric universal elements are known. } \sstinvocation{ void palPlantu ( double date, double elong, double phi, const double u[13], double $*$ra, double $*$dec, double $*$r, int $*$jstat ) \{ } \sstarguments{ \sstsubsection{ date = double (Given) }{ TT MJD of observation (JD-2400000.5) } \sstsubsection{ elong = double (Given) }{ Observer{\tt '}s east longitude (radians) } \sstsubsection{ phi = double (Given) }{ Observer{\tt '}s geodetic latitude (radians) } \sstsubsection{ u = const double [13] (Given) }{ Universal orbital elements \sstitemlist{ \sstitem (0) combined mass (M$+$m) \sstitem (1) total energy of the orbit (alpha) \sstitem (2) reference (osculating) epoch (t0) \sstitem (3-5) position at reference epoch (r0) \sstitem (6-8) velocity at reference epoch (v0) \sstitem (9) heliocentric distance at reference epoch \sstitem (10) r0.v0 \sstitem (11) date (t) \sstitem (12) universal eccentric anomaly (psi) of date, approx } } \sstsubsection{ ra = double $*$ (Returned) }{ Topocentric apparent RA (radians) } \sstsubsection{ dec = double $*$ (Returned) }{ Topocentric apparent Dec (radians) } \sstsubsection{ r = double $*$ (Returned) }{ Distance from observer (AU) } \sstsubsection{ jstat = int $*$ (Returned) }{ status: 0 = OK \sstitemlist{ \sstitem -1 = radius vector zero \sstitem -2 = failed to converge } } } \sstnotes{ \sstitemlist{ \sstitem DATE is the instant for which the prediction is required. It is in the TT timescale (formerly Ephemeris Time, ET) and is a Modified Julian Date (JD-2400000.5). \sstitem The longitude and latitude allow correction for geocentric parallax. This is usually a small effect, but can become important for near-Earth asteroids. Geocentric positions can be generated by appropriate use of routines palEpv (or palEvp) and palUe2pv. \sstitem The {\tt "}universal{\tt "} elements are those which define the orbit for the purposes of the method of universal variables (see reference 2). They consist of the combined mass of the two bodies, an epoch, and the position and velocity vectors (arbitrary reference frame) at that epoch. The parameter set used here includes also various quantities that can, in fact, be derived from the other information. This approach is taken to avoiding unnecessary computation and loss of accuracy. The supplementary quantities are (i) alpha, which is proportional to the total energy of the orbit, (ii) the heliocentric distance at epoch, (iii) the outwards component of the velocity at the given epoch, (iv) an estimate of psi, the {\tt "}universal eccentric anomaly{\tt "} at a given date and (v) that date. \sstitem The universal elements are with respect to the J2000 equator and equinox. } } \sstdiytopic{ See Also }{ \sstitemlist{ \sstitem Sterne, Theodore E., {\tt "}An Introduction to Celestial Mechanics{\tt "}, Interscience Publishers Inc., 1960. Section 6.7, p199. \sstitem Everhart, E. \& Pitkin, E.T., Am.J.Phys. 51, 712, 1983. } } } \sstroutine{ palPm }{ Apply corrections for proper motion a star RA,Dec }{ \sstdescription{ Apply corrections for proper motion to a star RA,Dec using the SOFA routine iauStarpm. } \sstinvocation{ void palPm ( double r0, double d0, double pr, double pd, double px, double rv, double ep0, double ep1, double $*$r1, double $*$d1 ); } \sstarguments{ \sstsubsection{ r0 = double (Given) }{ RA at epoch ep0 (radians) } \sstsubsection{ d0 = double (Given) }{ Dec at epoch ep0 (radians) } \sstsubsection{ pr = double (Given) }{ RA proper motion in radians per year. } \sstsubsection{ pd = double (Given) }{ Dec proper motion in radians per year. } \sstsubsection{ px = double (Given) }{ Parallax (arcsec) } \sstsubsection{ rv = double (Given) }{ Radial velocity (km/sec $+$ve if receding) } \sstsubsection{ ep0 = double (Given) }{ Start epoch in years, assumed to be Julian. } \sstsubsection{ ep1 = double (Given) }{ End epoch in years, assumed to be Julian. } \sstsubsection{ r1 = double $*$ (Returned) }{ RA at epoch ep1 (radians) } \sstsubsection{ d1 = double $*$ (Returned) }{ Dec at epoch ep1 (radians) } } \sstnotes{ \sstitemlist{ \sstitem Uses iauStarpm but ignores the status returns from that routine. In particular note that parallax should not be zero when the proper motions are non-zero. SLA/F allows parallax to be zero. \sstitem Assumes all epochs are Julian epochs. } } } \sstroutine{ palPrebn }{ Generate the matrix of precession between two objects (old) }{ \sstdescription{ Generate the matrix of precession between two epochs, using the old, pre-IAU1976, Bessel-Newcomb model, using Kinoshita{\tt '}s formulation } \sstinvocation{ void palPrebn ( double bep0, double bep1, double rmatp[3][3] ); } \sstarguments{ \sstsubsection{ bep0 = double (Given) }{ Beginning Besselian epoch. } \sstsubsection{ bep1 = double (Given) }{ Ending Besselian epoch } \sstsubsection{ rmatp = double[3][3] (Returned) }{ precession matrix in the sense V(BEP1) = RMATP $*$ V(BEP0) } } \sstdiytopic{ See Also }{ Kinoshita, H. (1975) {\tt '}Formulas for precession{\tt '}, SAO Special Report No. 364, Smithsonian Institution Astrophysical Observatory, Cambridge, Massachusetts. } } \sstroutine{ palPrec }{ Form the matrix of precession between two epochs (IAU 2006) }{ \sstdescription{ The IAU 2006 precession matrix from ep0 to ep1 is found and returned. The matrix is in the sense V(EP1) = RMATP $*$ V(EP0). The epochs are TDB (loosely TT) Julian epochs. Though the matrix method itself is rigorous, the precession angles are expressed through canonical polynomials which are valid only for a limited time span of a few hundred years around the current epoch. } \sstinvocation{ palPrec( double ep0, double ep1, double rmatp[3][3] ) } \sstarguments{ \sstsubsection{ ep0 = double (Given) }{ Beginning epoch } \sstsubsection{ ep1 = double (Given) }{ Ending epoch } \sstsubsection{ rmatp = double[3][3] (Returned) }{ Precession matrix } } } \sstroutine{ palPreces }{ Precession - either FK4 or FK5 as required }{ \sstdescription{ Precess coordinates using the appropriate system and epochs. } \sstinvocation{ void palPreces ( const char sys[3], double ep0, double ep1, double $*$ra, double $*$dc ); } \sstarguments{ \sstsubsection{ sys = const char [3] (Given) }{ Precession to be applied: FK4 or FK5. Case insensitive. } \sstsubsection{ ep0 = double (Given) }{ Starting epoch. } \sstsubsection{ ep1 = double (Given) }{ Ending epoch } \sstsubsection{ ra = double $*$ (Given \& Returned) }{ On input the RA mean equator \& equinox at epoch ep0. On exit the RA mean equator \& equinox of epoch ep1. } \sstsubsection{ dec = double $*$ (Given \& Returned) }{ On input the dec mean equator \& equinox at epoch ep0. On exit the dec mean equator \& equinox of epoch ep1. } } \sstnotes{ \sstitemlist{ \sstitem Uses palPrec for FK5 data and palPrebn for FK4 data. \sstitem The epochs are Besselian if SYSTEM={\tt '}FK4{\tt '} and Julian if {\tt '}FK5{\tt '}. For example, to precess coordinates in the old system from equinox 1900.0 to 1950.0 the call would be: palPreces( {\tt "}FK4{\tt "}, 1900.0, 1950.0, \&ra, \&dc ); \sstitem This routine will NOT correctly convert between the old and the new systems - for example conversion from B1950 to J2000. For these purposes see palFk425, palFk524, palFk45z and palFk54z. \sstitem If an invalid SYSTEM is supplied, values of -99D0,-99D0 will be returned for both RA and DC. } } } \sstroutine{ palPrenut }{ Form the matrix of bias-precession-nutation (IAU 2006/2000A) }{ \sstdescription{ Form the matrix of bias-precession-nutation (IAU 2006/2000A). The epoch and date are TT (but TDB is usually close enough). The matrix is in the sense v(true) = rmatpn $*$ v(mean). } \sstinvocation{ void palPrenut( double epoch, double date, double rmatpn[3][3] ) } \sstarguments{ \sstsubsection{ epoch = double (Returned) }{ Julian epoch for mean coordinates. } \sstsubsection{ date = double (Returned) }{ Modified Julian Date (JD-2400000.5) for true coordinates. } \sstsubsection{ rmatpn = double[3][3] (Returned) }{ combined NPB matrix } } } \sstroutine{ palPv2el }{ Position velocity to heliocentirc osculating elements }{ \sstdescription{ Heliocentric osculating elements obtained from instantaneous position and velocity. } \sstinvocation{ void palPv2el ( const double pv[6], double date, double pmass, int jformr, int $*$jform, double $*$epoch, double $*$orbinc, double $*$anode, double $*$perih, double $*$aorq, double $*$e, double $*$aorl, double $*$dm, int $*$jstat ); } \sstarguments{ \sstsubsection{ pv = const double [6] (Given) }{ Heliocentric x,y,z,xdot,ydot,zdot of date, J2000 equatorial triad (AU,AU/s; Note 1) } \sstsubsection{ date = double (Given) }{ Date (TT Modified Julian Date = JD-2400000.5) } \sstsubsection{ pmass = double (Given) }{ Mass of the planet (Sun=1; Note 2) } \sstsubsection{ jformr = int (Given) }{ Requested element set (1-3; Note 3) } \sstsubsection{ jform = int $*$ (Returned) }{ Element set actually returned (1-3; Note 4) } \sstsubsection{ epoch = double $*$ (Returned) }{ Epoch of elements (TT MJD) } \sstsubsection{ orbinc = double $*$ (Returned) }{ inclination (radians) } \sstsubsection{ anode = double $*$ (Returned) }{ longitude of the ascending node (radians) } \sstsubsection{ perih = double $*$ (Returned) }{ longitude or argument of perihelion (radians) } \sstsubsection{ aorq = double $*$ (Returned) }{ mean distance or perihelion distance (AU) } \sstsubsection{ e = double $*$ (Returned) }{ eccentricity } \sstsubsection{ aorl = double $*$ (Returned) }{ mean anomaly or longitude (radians, JFORM=1,2 only) } \sstsubsection{ dm = double $*$ (Returned) }{ daily motion (radians, JFORM=1 only) } \sstsubsection{ jstat = int $*$ (Returned) }{ status: 0 = OK \sstitemlist{ \sstitem -1 = illegal PMASS \sstitem -2 = illegal JFORMR \sstitem -3 = position/velocity out of range } } } \sstnotes{ \sstitemlist{ \sstitem The PV 6-vector is with respect to the mean equator and equinox of epoch J2000. The orbital elements produced are with respect to the J2000 ecliptic and mean equinox. \sstitem The mass, PMASS, is important only for the larger planets. For most purposes (e.g. asteroids) use 0D0. Values less than zero are illegal. \sstitem Three different element-format options are supported: } Option JFORM=1, suitable for the major planets: EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = longitude of perihelion, curly pi (radians) AORQ = mean distance, a (AU) E = eccentricity, e AORL = mean longitude L (radians) DM = daily motion (radians) Option JFORM=2, suitable for minor planets: EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = mean distance, a (AU) E = eccentricity, e AORL = mean anomaly M (radians) Option JFORM=3, suitable for comets: EPOCH = epoch of perihelion (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = perihelion distance, q (AU) E = eccentricity, e \sstitemlist{ \sstitem It may not be possible to generate elements in the form requested through JFORMR. The caller is notified of the form of elements actually returned by means of the JFORM argument: } JFORMR JFORM meaning 1 1 OK - elements are in the requested format 1 2 never happens 1 3 orbit not elliptical 2 1 never happens 2 2 OK - elements are in the requested format 2 3 orbit not elliptical 3 1 never happens 3 2 never happens 3 3 OK - elements are in the requested format \sstitemlist{ \sstitem The arguments returned for each value of JFORM (cf Note 5: JFORM may not be the same as JFORMR) are as follows: } JFORM 1 2 3 EPOCH t0 t0 T ORBINC i i i ANODE Omega Omega Omega PERIH curly pi omega omega AORQ a a q E e e e AORL L M - DM n - - where: t0 is the epoch of the elements (MJD, TT) T {\tt "} epoch of perihelion (MJD, TT) i {\tt "} inclination (radians) Omega {\tt "} longitude of the ascending node (radians) curly pi {\tt "} longitude of perihelion (radians) omega {\tt "} argument of perihelion (radians) a {\tt "} mean distance (AU) q {\tt "} perihelion distance (AU) e {\tt "} eccentricity L {\tt "} longitude (radians, 0-2pi) M {\tt "} mean anomaly (radians, 0-2pi) n {\tt "} daily motion (radians) \sstitemlist{ \sstitem means no value is set \sstitem At very small inclinations, the longitude of the ascending node ANODE becomes indeterminate and under some circumstances may be set arbitrarily to zero. Similarly, if the orbit is close to circular, the true anomaly becomes indeterminate and under some circumstances may be set arbitrarily to zero. In such cases, the other elements are automatically adjusted to compensate, and so the elements remain a valid description of the orbit. \sstitem The osculating epoch for the returned elements is the argument DATE. \sstitem Reference: Sterne, Theodore E., {\tt "}An Introduction to Celestial Mechanics{\tt "}, Interscience Publishers, 1960 } } } \sstroutine{ palPv2ue }{ Universal elements to position and velocity }{ \sstdescription{ Construct a universal element set based on an instantaneous position and velocity. } \sstinvocation{ void palPv2ue( const double pv[6], double date, double pmass, double u[13], int $*$ jstat ); } \sstarguments{ \sstsubsection{ pv = double [6] (Given) }{ Heliocentric x,y,z,xdot,ydot,zdot of date, (AU,AU/s; Note 1) } \sstsubsection{ date = double (Given) }{ Date (TT modified Julian Date = JD-2400000.5) } \sstsubsection{ pmass = double (Given) }{ Mass of the planet (Sun=1; note 2) } \sstsubsection{ u = double [13] (Returned) }{ Universal orbital elements (Note 3) \sstitemlist{ \sstitem (0) combined mass (M$+$m) \sstitem (1) total energy of the orbit (alpha) \sstitem (2) reference (osculating) epoch (t0) \sstitem (3-5) position at reference epoch (r0) \sstitem (6-8) velocity at reference epoch (v0) \sstitem (9) heliocentric distance at reference epoch \sstitem (10) r0.v0 \sstitem (11) date (t) \sstitem (12) universal eccentric anomaly (psi) of date, approx } } \sstsubsection{ jstat = int $*$ (Returned) }{ status: 0 = OK \sstitemlist{ \sstitem -1 = illegal PMASS \sstitem -2 = too close to Sun \sstitem -3 = too slow } } } \sstnotes{ \sstitemlist{ \sstitem The PV 6-vector can be with respect to any chosen inertial frame, and the resulting universal-element set will be with respect to the same frame. A common choice will be mean equator and ecliptic of epoch J2000. \sstitem The mass, PMASS, is important only for the larger planets. For most purposes (e.g. asteroids) use 0D0. Values less than zero are illegal. \sstitem The {\tt "}universal{\tt "} elements are those which define the orbit for the purposes of the method of universal variables (see reference). They consist of the combined mass of the two bodies, an epoch, and the position and velocity vectors (arbitrary reference frame) at that epoch. The parameter set used here includes also various quantities that can, in fact, be derived from the other information. This approach is taken to avoiding unnecessary computation and loss of accuracy. The supplementary quantities are (i) alpha, which is proportional to the total energy of the orbit, (ii) the heliocentric distance at epoch, (iii) the outwards component of the velocity at the given epoch, (iv) an estimate of psi, the {\tt "}universal eccentric anomaly{\tt "} at a given date and (v) that date. \sstitem Reference: Everhart, E. \& Pitkin, E.T., Am.J.Phys. 51, 712, 1983. } } } \sstroutine{ palPvobs }{ Position and velocity of an observing station }{ \sstdescription{ Returns the position and velocity of an observing station. } \sstinvocation{ palPvobs( double p, double h, double stl, double pv[6] ) } \sstarguments{ \sstsubsection{ p = double (Given) }{ Latitude (geodetic, radians). } \sstsubsection{ h = double (Given) }{ Height above reference spheroid (geodetic, metres). } \sstsubsection{ stl = double (Given) }{ Local apparent sidereal time (radians). } \sstsubsection{ pv = double[ 6 ] (Returned) }{ position/velocity 6-vector (AU, AU/s, true equator and equinox of date). } } \sstnotes{ \sstitemlist{ \sstitem The WGS84 reference ellipsoid is used. } } } \sstroutine{ palRdplan }{ Approximate topocentric apparent RA,Dec of a planet }{ \sstdescription{ Approximate topocentric apparent RA,Dec of a planet, and its angular diameter. } \sstinvocation{ void palRdplan( double date, int np, double elong, double phi, double $*$ ra, double $*$ dec, double $*$ diam ); } \sstarguments{ \sstsubsection{ date = double (Given) }{ MJD of observation (JD-2400000.5) in TDB. For all practical purposes TT can be used instead of TDB, and for many applications UT will do (except for the Moon). } \sstsubsection{ np = int (Given) }{ Planet: 1 = Mercury 2 = Venus 3 = Moon 4 = Mars 5 = Jupiter 6 = Saturn 7 = Uranus 8 = Neptune else = Sun } \sstsubsection{ elong = double (Given) }{ Observer{\tt '}s east longitude (radians) } \sstsubsection{ phi = double (Given) }{ Observer{\tt '}s geodetic latitude (radians) } \sstsubsection{ ra = double $*$ (Returned) }{ RA (topocentric apparent, radians) } \sstsubsection{ dec = double $*$ (Returned) }{ Dec (topocentric apparent, radians) } \sstsubsection{ diam = double $*$ (Returned) }{ Angular diameter (equatorial, radians) } } \sstnotes{ \sstitemlist{ \sstitem Unlike with slaRdplan, Pluto is not supported. \sstitem The longitude and latitude allow correction for geocentric parallax. This is a major effect for the Moon, but in the context of the limited accuracy of the present routine its effect on planetary positions is small (negligible for the outer planets). Geocentric positions can be generated by appropriate use of the routines palDmoon and iauPlan94. } } } \sstroutine{ palRverot }{ Velocity component in a given direction due to Earth rotation }{ \sstdescription{ Calculate the velocity component in a given direction due to Earth rotation. The simple algorithm used assumes a spherical Earth, of a radius chosen to give results accurate to about 0.0005 km/s for observing stations at typical latitudes and heights. For applications requiring greater precision, use the routine palPvobs. } \sstinvocation{ double palRverot ( double phi, double ra, double da, double st ); } \sstarguments{ \sstsubsection{ phi = double (Given) }{ latitude of observing station (geodetic) (radians) } \sstsubsection{ ra = double (Given) }{ apparent RA (radians) } \sstsubsection{ da = double (Given) }{ apparent Dec (radians) } \sstsubsection{ st = double (Given) }{ } } \sstreturnedvalue{ \sstsubsection{ palRverot = double }{ Component of Earth rotation in direction RA,DA (km/s). The result is $+$ve when the observatory is receding from the given point on the sky. } } } \sstroutine{ palRvgalc }{ Velocity component in a given direction due to the rotation of the Galaxy }{ \sstdescription{ This function returns the Component of dynamical LSR motion in the direction of R2000,D2000. The result is $+$ve when the dynamical LSR is receding from the given point on the sky. } \sstinvocation{ double palRvgalc( double r2000, double d2000 ) } \sstarguments{ \sstsubsection{ r2000 = double (Given) }{ J2000.0 mean RA (radians) } \sstsubsection{ d2000 = double (Given) }{ J2000.0 mean Dec (radians) } } \sstreturnedvalue{ \sstsubsection{ Component of dynamical LSR motion in direction R2000,D2000 (km/s). }{ } } \sstnotes{ \sstitemlist{ \sstitem The Local Standard of Rest used here is a point in the vicinity of the Sun which is in a circular orbit around the Galactic centre. Sometimes called the {\tt "}dynamical{\tt "} LSR, it is not to be confused with a {\tt "}kinematical{\tt "} LSR, which is the mean standard of rest of star catalogues or stellar populations. } } \sstdiytopic{ Reference }{ \sstitemlist{ \sstitem The orbital speed of 220 km/s used here comes from Kerr \& Lynden-Bell (1986), MNRAS, 221, p1023. } } } \sstroutine{ palRvlg }{ Velocity component in a given direction due to Galactic rotation and motion of the local group }{ \sstdescription{ This function returns the velocity component in a given direction due to the combination of the rotation of the Galaxy and the motion of the Galaxy relative to the mean motion of the local group. The result is $+$ve when the Sun is receding from the given point on the sky. } \sstinvocation{ double palRvlg( double r2000, double d2000 ) } \sstarguments{ \sstsubsection{ r2000 = double (Given) }{ J2000.0 mean RA (radians) } \sstsubsection{ d2000 = double (Given) }{ J2000.0 mean Dec (radians) } } \sstreturnedvalue{ \sstsubsection{ Component of SOLAR motion in direction R2000,D2000 (km/s). }{ } } \sstdiytopic{ Reference }{ \sstitemlist{ \sstitem IAU Trans 1976, 168, p201. } } } \sstroutine{ palRvlsrd }{ Velocity component in a given direction due to the Sun{\tt '}s motion with respect to the dynamical Local Standard of Rest }{ \sstdescription{ This function returns the velocity component in a given direction due to the Sun{\tt '}s motion with respect to the dynamical Local Standard of Rest. The result is $+$ve when the Sun is receding from the given point on the sky. } \sstinvocation{ double palRvlsrd( double r2000, double d2000 ) } \sstarguments{ \sstsubsection{ r2000 = double (Given) }{ J2000.0 mean RA (radians) } \sstsubsection{ d2000 = double (Given) }{ J2000.0 mean Dec (radians) } } \sstreturnedvalue{ \sstsubsection{ Component of {\tt "}peculiar{\tt "} solar motion in direction R2000,D2000 (km/s). }{ } } \sstnotes{ \sstitemlist{ \sstitem The Local Standard of Rest used here is the {\tt "}dynamical{\tt "} LSR, a point in the vicinity of the Sun which is in a circular orbit around the Galactic centre. The Sun{\tt '}s motion with respect to the dynamical LSR is called the {\tt "}peculiar{\tt "} solar motion. \sstitem There is another type of LSR, called a {\tt "}kinematical{\tt "} LSR. A kinematical LSR is the mean standard of rest of specified star catalogues or stellar populations, and several slightly different kinematical LSRs are in use. The Sun{\tt '}s motion with respect to an agreed kinematical LSR is known as the {\tt "}standard{\tt "} solar motion. To obtain a radial velocity correction with respect to an adopted kinematical LSR use the routine sla\_RVLSRK. } } \sstdiytopic{ Reference }{ \sstitemlist{ \sstitem Delhaye (1965), in {\tt "}Stars and Stellar Systems{\tt "}, vol 5, p73. } } } \sstroutine{ palRvlsrk }{ Velocity component in a given direction due to the Sun{\tt '}s motion with respect to an adopted kinematic Local Standard of Rest }{ \sstdescription{ This function returns the velocity component in a given direction due to the Sun{\tt '}s motion with respect to an adopted kinematic Local Standard of Rest. The result is $+$ve when the Sun is receding from the given point on the sky. } \sstinvocation{ double palRvlsrk( double r2000, double d2000 ) } \sstarguments{ \sstsubsection{ r2000 = double (Given) }{ J2000.0 mean RA (radians) } \sstsubsection{ d2000 = double (Given) }{ J2000.0 mean Dec (radians) } } \sstreturnedvalue{ \sstsubsection{ Component of {\tt "}standard{\tt "} solar motion in direction R2000,D2000 (km/s). }{ } } \sstnotes{ \sstitemlist{ \sstitem The Local Standard of Rest used here is one of several {\tt "}kinematical{\tt "} LSRs in common use. A kinematical LSR is the mean standard of rest of specified star catalogues or stellar populations. The Sun{\tt '}s motion with respect to a kinematical LSR is known as the {\tt "}standard{\tt "} solar motion. \sstitem There is another sort of LSR, the {\tt "}dynamical{\tt "} LSR, which is a point in the vicinity of the Sun which is in a circular orbit around the Galactic centre. The Sun{\tt '}s motion with respect to the dynamical LSR is called the {\tt "}peculiar{\tt "} solar motion. To obtain a radial velocity correction with respect to the dynamical LSR use the routine sla\_RVLSRD. } } \sstdiytopic{ Reference }{ \sstitemlist{ \sstitem Delhaye (1965), in {\tt "}Stars and Stellar Systems{\tt "}, vol 5, p73. } } } \sstroutine{ palSubet }{ Remove the E-terms from a pre IAU 1976 catalogue RA,Dec }{ \sstdescription{ Remove the E-terms (elliptic component of annual aberration) from a pre IAU 1976 catalogue RA,Dec to give a mean place. } \sstinvocation{ void palSubet ( double rc, double dc, double eq, double $*$rm, double $*$dm ); } \sstarguments{ \sstsubsection{ rc = double (Given) }{ RA with E-terms included (radians) } \sstsubsection{ dc = double (Given) }{ Dec with E-terms included (radians) } \sstsubsection{ eq = double (Given) }{ Besselian epoch of mean equator and equinox } \sstsubsection{ rm = double $*$ (Returned) }{ RA without E-terms (radians) } \sstsubsection{ dm = double $*$ (Returned) }{ Dec without E-terms (radians) } } \sstnotes{ Most star positions from pre-1984 optical catalogues (or derived from astrometry using such stars) embody the E-terms. This routine converts such a position to a formal mean place (allowing, for example, comparison with a pulsar timing position). } \sstdiytopic{ See Also }{ Explanatory Supplement to the Astronomical Ephemeris, section 2D, page 48. } } \sstroutine{ palSupgal }{ Convert from supergalactic to galactic coordinates }{ \sstdescription{ Transformation from de Vaucouleurs supergalactic coordinates to IAU 1958 galactic coordinates } \sstinvocation{ void palSupgal ( double dsl, double dsb, double $*$dl, double $*$db ); } \sstarguments{ \sstsubsection{ dsl = double (Given) }{ Supergalactic longitude. } \sstsubsection{ dsb = double (Given) }{ Supergalactic latitude. } \sstsubsection{ dl = double $*$ (Returned) }{ Galactic longitude. } \sstsubsection{ db = double $*$ (Returned) }{ Galactic latitude. } } \sstdiytopic{ See Also }{ \sstitemlist{ \sstitem de Vaucouleurs, de Vaucouleurs, \& Corwin, Second Reference Catalogue of Bright Galaxies, U. Texas, page 8. \sstitem Systems \& Applied Sciences Corp., Documentation for the machine-readable version of the above catalogue, Contract NAS 5-26490. } (These two references give different values for the galactic longitude of the supergalactic origin. Both are wrong; the correct value is L2=137.37.) } } \sstroutine{ palUe2el }{ Universal elements to heliocentric osculating elements }{ \sstdescription{ Transform universal elements into conventional heliocentric osculating elements. } \sstinvocation{ void palUe2el ( const double u[13], int jformr, int $*$jform, double $*$epoch, double $*$orbinc, double $*$anode, double $*$perih, double $*$aorq, double $*$e, double $*$aorl, double $*$dm, int $*$jstat ); } \sstarguments{ \sstsubsection{ u = const double [13] (Given) }{ Universal orbital elements (Note 1) (0) combined mass (M$+$m) (1) total energy of the orbit (alpha) (2) reference (osculating) epoch (t0) (3-5) position at reference epoch (r0) (6-8) velocity at reference epoch (v0) (9) heliocentric distance at reference epoch (10) r0.v0 (11) date (t) (12) universal eccentric anomaly (psi) of date, approx } \sstsubsection{ jformr = int (Given) }{ Requested element set (1-3; Note 3) } \sstsubsection{ jform = int $*$ (Returned) }{ Element set actually returned (1-3; Note 4) } \sstsubsection{ epoch = double $*$ (Returned) }{ Epoch of elements (TT MJD) } \sstsubsection{ orbinc = double $*$ (Returned) }{ inclination (radians) } \sstsubsection{ anode = double $*$ (Returned) }{ longitude of the ascending node (radians) } \sstsubsection{ perih = double $*$ (Returned) }{ longitude or argument of perihelion (radians) } \sstsubsection{ aorq = double $*$ (Returned) }{ mean distance or perihelion distance (AU) } \sstsubsection{ e = double $*$ (Returned) }{ eccentricity } \sstsubsection{ aorl = double $*$ (Returned) }{ mean anomaly or longitude (radians, JFORM=1,2 only) } \sstsubsection{ dm = double $*$ (Returned) }{ daily motion (radians, JFORM=1 only) } \sstsubsection{ jstat = int $*$ (Returned) }{ status: 0 = OK \sstitemlist{ \sstitem 1 = illegal combined mass \sstitem 2 = illegal JFORMR \sstitem 3 = position/velocity out of range } } } \sstnotes{ \sstitemlist{ \sstitem The {\tt "}universal{\tt "} elements are those which define the orbit for the purposes of the method of universal variables (see reference 2). They consist of the combined mass of the two bodies, an epoch, and the position and velocity vectors (arbitrary reference frame) at that epoch. The parameter set used here includes also various quantities that can, in fact, be derived from the other information. This approach is taken to avoiding unnecessary computation and loss of accuracy. The supplementary quantities are (i) alpha, which is proportional to the total energy of the orbit, (ii) the heliocentric distance at epoch, (iii) the outwards component of the velocity at the given epoch, (iv) an estimate of psi, the {\tt "}universal eccentric anomaly{\tt "} at a given date and (v) that date. \sstitem The universal elements are with respect to the mean equator and equinox of epoch J2000. The orbital elements produced are with respect to the J2000 ecliptic and mean equinox. \sstitem Three different element-format options are supported: } Option JFORM=1, suitable for the major planets: EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = longitude of perihelion, curly pi (radians) AORQ = mean distance, a (AU) E = eccentricity, e AORL = mean longitude L (radians) DM = daily motion (radians) Option JFORM=2, suitable for minor planets: EPOCH = epoch of elements (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = mean distance, a (AU) E = eccentricity, e AORL = mean anomaly M (radians) Option JFORM=3, suitable for comets: EPOCH = epoch of perihelion (TT MJD) ORBINC = inclination i (radians) ANODE = longitude of the ascending node, big omega (radians) PERIH = argument of perihelion, little omega (radians) AORQ = perihelion distance, q (AU) E = eccentricity, e \sstitemlist{ \sstitem It may not be possible to generate elements in the form requested through JFORMR. The caller is notified of the form of elements actually returned by means of the JFORM argument: } JFORMR JFORM meaning 1 1 OK - elements are in the requested format 1 2 never happens 1 3 orbit not elliptical 2 1 never happens 2 2 OK - elements are in the requested format 2 3 orbit not elliptical 3 1 never happens 3 2 never happens 3 3 OK - elements are in the requested format \sstitemlist{ \sstitem The arguments returned for each value of JFORM (cf Note 6: JFORM may not be the same as JFORMR) are as follows: } JFORM 1 2 3 EPOCH t0 t0 T ORBINC i i i ANODE Omega Omega Omega PERIH curly pi omega omega AORQ a a q E e e e AORL L M - DM n - - where: t0 is the epoch of the elements (MJD, TT) T {\tt "} epoch of perihelion (MJD, TT) i {\tt "} inclination (radians) Omega {\tt "} longitude of the ascending node (radians) curly pi {\tt "} longitude of perihelion (radians) omega {\tt "} argument of perihelion (radians) a {\tt "} mean distance (AU) q {\tt "} perihelion distance (AU) e {\tt "} eccentricity L {\tt "} longitude (radians, 0-2pi) M {\tt "} mean anomaly (radians, 0-2pi) n {\tt "} daily motion (radians) \sstitemlist{ \sstitem means no value is set \sstitem At very small inclinations, the longitude of the ascending node ANODE becomes indeterminate and under some circumstances may be set arbitrarily to zero. Similarly, if the orbit is close to circular, the true anomaly becomes indeterminate and under some circumstances may be set arbitrarily to zero. In such cases, the other elements are automatically adjusted to compensate, and so the elements remain a valid description of the orbit. } See Also: \sstitemlist{ \sstitem Sterne, Theodore E., {\tt "}An Introduction to Celestial Mechanics{\tt "}, Interscience Publishers Inc., 1960. Section 6.7, p199. \sstitem Everhart, E. \& Pitkin, E.T., Am.J.Phys. 51, 712, 1983. } } } \sstroutine{ palUe2pv }{ Heliocentric position and velocity of a planet, asteroid or comet, from universal elements }{ \sstdescription{ Heliocentric position and velocity of a planet, asteroid or comet, starting from orbital elements in the {\tt "}universal variables{\tt "} form. } \sstinvocation{ void palUe2pv( double date, double u[13], double pv[6], int $*$jstat ); } \sstarguments{ \sstsubsection{ date = double (Given) }{ TT Modified Julian date (JD-2400000.5). } \sstsubsection{ u = double [13] (Given \& Returned) }{ Universal orbital elements (updated, see note 1) given (0) combined mass (M$+$m) {\tt "} (1) total energy of the orbit (alpha) {\tt "} (2) reference (osculating) epoch (t0) {\tt "} (3-5) position at reference epoch (r0) {\tt "} (6-8) velocity at reference epoch (v0) {\tt "} (9) heliocentric distance at reference epoch {\tt "} (10) r0.v0 returned (11) date (t) {\tt "} (12) universal eccentric anomaly (psi) of date } \sstsubsection{ jstat = int $*$ (Returned) }{ status: 0 = OK \sstitemlist{ \sstitem 1 = radius vector zero \sstitem 2 = failed to converge } } } \sstnotes{ \sstitemlist{ \sstitem The {\tt "}universal{\tt "} elements are those which define the orbit for the purposes of the method of universal variables (see reference). They consist of the combined mass of the two bodies, an epoch, and the position and velocity vectors (arbitrary reference frame) at that epoch. The parameter set used here includes also various quantities that can, in fact, be derived from the other information. This approach is taken to avoiding unnecessary computation and loss of accuracy. The supplementary quantities are (i) alpha, which is proportional to the total energy of the orbit, (ii) the heliocentric distance at epoch, (iii) the outwards component of the velocity at the given epoch, (iv) an estimate of psi, the {\tt "}universal eccentric anomaly{\tt "} at a given date and (v) that date. \sstitem The companion routine is palEl2ue. This takes the conventional orbital elements and transforms them into the set of numbers needed by the present routine. A single prediction requires one one call to palEl2ue followed by one call to the present routine; for convenience, the two calls are packaged as the routine sla\_PLANEL. Multiple predictions may be made by again calling palEl2ue once, but then calling the present routine multiple times, which is faster than multiple calls to palPlanel. \sstitem It is not obligatory to use palEl2ue to obtain the parameters. However, it should be noted that because palEl2ue performs its own validation, no checks on the contents of the array U are made by the present routine. in the TT timescale (formerly Ephemeris Time, ET) and is a Modified Julian Date (JD-2400000.5). units (solar masses, AU and canonical days). The position and velocity are not sensitive to the choice of reference frame. The palEl2ue routine in fact produces coordinates with respect to the J2000 equator and equinox. \sstitem The algorithm was originally adapted from the EPHSLA program of D.H.P.Jones (private communication, 1996). The method is based on Stumpff{\tt '}s Universal Variables. \sstitem Reference: Everhart, E. \& Pitkin, E.T., Am.J.Phys. 51, 712, 1983. } } } % ? End of main text \end{document} pal-0.5.0/test-driver000755 000765 000024 00000010277 12363621607 014611 0ustar00timjstaff000000 000000 #! /bin/sh # test-driver - basic testsuite driver script. scriptversion=2013-07-13.22; # UTC # Copyright (C) 2011-2013 Free Software Foundation, Inc. # # This program is free software; you can redistribute it and/or modify # it under the terms of the GNU General Public License as published by # the Free Software Foundation; either version 2, or (at your option) # any later version. # # This program is distributed in the hope that it will be useful, # but WITHOUT ANY WARRANTY; without even the implied warranty of # MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the # GNU General Public License for more details. # # You should have received a copy of the GNU General Public License # along with this program. If not, see . # As a special exception to the GNU General Public License, if you # distribute this file as part of a program that contains a # configuration script generated by Autoconf, you may include it under # the same distribution terms that you use for the rest of that program. # This file is maintained in Automake, please report # bugs to or send patches to # . # Make unconditional expansion of undefined variables an error. This # helps a lot in preventing typo-related bugs. set -u usage_error () { echo "$0: $*" >&2 print_usage >&2 exit 2 } print_usage () { cat <$log_file 2>&1 estatus=$? if test $enable_hard_errors = no && test $estatus -eq 99; then estatus=1 fi case $estatus:$expect_failure in 0:yes) col=$red res=XPASS recheck=yes gcopy=yes;; 0:*) col=$grn res=PASS recheck=no gcopy=no;; 77:*) col=$blu res=SKIP recheck=no gcopy=yes;; 99:*) col=$mgn res=ERROR recheck=yes gcopy=yes;; *:yes) col=$lgn res=XFAIL recheck=no gcopy=yes;; *:*) col=$red res=FAIL recheck=yes gcopy=yes;; esac # Report outcome to console. echo "${col}${res}${std}: $test_name" # Register the test result, and other relevant metadata. echo ":test-result: $res" > $trs_file echo ":global-test-result: $res" >> $trs_file echo ":recheck: $recheck" >> $trs_file echo ":copy-in-global-log: $gcopy" >> $trs_file # Local Variables: # mode: shell-script # sh-indentation: 2 # eval: (add-hook 'write-file-hooks 'time-stamp) # time-stamp-start: "scriptversion=" # time-stamp-format: "%:y-%02m-%02d.%02H" # time-stamp-time-zone: "UTC" # time-stamp-end: "; # UTC" # End: