Index: trunk/FACT++/pal/.gitignore =================================================================== --- trunk/FACT++/pal/.gitignore (revision 18347) +++ trunk/FACT++/pal/.gitignore (revision 18347) @@ -0,0 +1,54 @@ +*~ +*.trs +.deps +.libs +Makefile +Makefile.in +configure +configure.in +*.o +*.lo +*.la +*.dSYM +palTest +make.log +make.log.err +config.h +config.h.in +config.log +config.status +stamp-h1 +libtool +*.htx +*.aux +*.bbl +*.blg +*.dvi +*.log +*.htx_tar +aclocal.m4 +autom4te.cache/ +componentinfo.dtd +starconf.status +sun267.ps +sun267.pdf +compile +config.guess +config.sub +depcomp +install-sh +ltmain.sh +missing +stamp-h2 +pal-*.tar.gz +pubs/adass2012/P56.pdf +test-driver +*.os +.sconf_temp/ +.sconsign.dblite +libpal.*.dylib +libpal.a +libpal.dylib +sun267.fls +sun267.out +sun267.toc Index: trunk/FACT++/pal/COPYING =================================================================== --- trunk/FACT++/pal/COPYING (revision 18347) +++ trunk/FACT++/pal/COPYING (revision 18347) @@ -0,0 +1,674 @@ + GNU 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. + + Preamble + + The GNU General Public License is a free, copyleft license for +software and other kinds of works. + + The licenses for most software and other practical works are designed +to take away your freedom to share and change the works. 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If your program is a subroutine library, you +may consider it more useful to permit linking proprietary applications with +the library. If this is what you want to do, use the GNU Lesser General +Public License instead of this License. But first, please read +. Index: trunk/FACT++/pal/COPYING.LESSER =================================================================== --- trunk/FACT++/pal/COPYING.LESSER (revision 18347) +++ trunk/FACT++/pal/COPYING.LESSER (revision 18347) @@ -0,0 +1,165 @@ + 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. 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Index: trunk/FACT++/pal/Makefile.am =================================================================== --- trunk/FACT++/pal/Makefile.am (revision 18347) +++ trunk/FACT++/pal/Makefile.am (revision 18347) @@ -0,0 +1,138 @@ +## 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. This is handy for creating +# shareable libraries from the static ones (Java JNI libraries). +if !NOPIC +libpal_la_CFLAGS = $(AM_CFLAGS) -prefer-pic +endif + +# install pal as "star/pal.h" +cincludedir = $(includedir)/star +cinclude_HEADERS = pal.h palmac.h + +noinst_HEADERS = $(PRIVATE_INCLUDES) + +PRIVATE_INCLUDES = pal1.h pal1sofa.h + +PUBLIC_C_FILES = \ +palAddet.c \ +palAirmas.c \ +palAltaz.c \ +palAmp.c \ +palAmpqk.c \ +palAop.c \ +palAoppa.c \ +palAoppat.c \ +palAopqk.c \ +palAtmdsp.c \ +palCaldj.c \ +palDafin.c \ +palDe2h.c \ +palDeuler.c \ +palDfltin.c \ +palDh2e.c \ +palDjcal.c \ +palDmat.c \ +palDs2tp.c \ +palDat.c \ +palDmoon.c \ +palDrange.c \ +palDt.c \ +palDtp2s.c \ +palDtps2c.c \ +palDtt.c \ +palEcleq.c \ +palEcmat.c \ +palEl2ue.c \ +palEpco.c \ +palEpv.c \ +palEtrms.c \ +palEqecl.c \ +palEqgal.c \ +palEvp.c \ +palFk45z.c \ +palFk524.c \ +palFk54z.c \ +palGaleq.c \ +palGalsup.c \ +palGe50.c \ +palGeoc.c \ +palIntin.c \ +palMap.c \ +palMappa.c \ +palMapqk.c \ +palMapqkz.c \ +palNut.c \ +palNutc.c \ +palOap.c \ +palOapqk.c \ +palObs.c \ +palPa.c \ +palPcd.c \ +palPertel.c \ +palPertue.c \ +palPlanel.c \ +palPlanet.c \ +palPlante.c \ +palPlantu.c \ +palPm.c \ +palPolmo.c \ +palPrebn.c \ +palPrec.c \ +palPreces.c \ +palPrenut.c \ +palPv2el.c \ +palPv2ue.c \ +palPvobs.c \ +palRdplan.c \ +palRefco.c \ +palRefro.c \ +palRefv.c \ +palRefz.c \ +palRverot.c \ +palRvgalc.c \ +palRvlg.c \ +palRvlsrd.c \ +palRvlsrk.c \ +palSubet.c \ +palSupgal.c \ +palUe2el.c \ +palUe2pv.c \ +palUnpcd.c \ +palVers.c + +PRIVATE_C_FILES = \ +pal1Atms.c \ +pal1Atmt.c + +stardocs_DATA = @STAR_LATEX_DOCUMENTATION@ + +TESTS = palTest + +check_PROGRAMS = palTest +palTest_SOURCES = palTest.c +palTest_LDADD = libpal.la + +# A target for making the SUN documentation. We do not do this automatically +palsun.tex: $(PUBLIC_C_FILES) + -rm -f palsun.tex all.c + cat $(PUBLIC_C_FILES) > all.c + ${STARCONF_DEFAULT_PREFIX}/bin/sst/prolat in=all.c out=palsun.tex single=no page=no atask=no document=no + -rm all.c Index: trunk/FACT++/pal/README.md =================================================================== --- trunk/FACT++/pal/README.md (revision 18347) +++ trunk/FACT++/pal/README.md (revision 18347) @@ -0,0 +1,76 @@ +PAL - Positional Astronomy Library +================================== + +[![DOI](https://zenodo.org/badge/12517/Starlink/pal.svg)](http://dx.doi.org/10.5281/zenodo.17212) + +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 --without-starlink + 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`. + +`--without-starlink` forces the configure script to forget about any Starlink +configurations. This is the safe option if you run into problems when using +a simple `--prefix` for building outside of Starlink. The configure script +will assume Starlink is not being used by looking to see if +`STARCONF_DEFAULT_PREFIX` environment variable is set. You may run into problems if +`STARCONF_DEFAULT_PREFIX` is set but you use `--without-starlink`. + +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. + Index: trunk/FACT++/pal/SConstruct =================================================================== --- trunk/FACT++/pal/SConstruct (revision 18347) +++ trunk/FACT++/pal/SConstruct (revision 18347) @@ -0,0 +1,208 @@ +# PAL SConstruct file +import os + +version = "0.9.2" + +def CheckStarlink(context): + context.Message( "Checking for Starlink environment...") + if "STARLINK_DIR" in os.environ: + star_root = os.environ["STARCONF_DEFAULT_PREFIX"] + star_lib = os.path.join(star_root, "lib") + star_inc = os.path.join(star_root, "include") + star_share = os.path.join(star_root, "share") + star_bin = os.path.join(star_root, "bin") + context.env.PrependENVPath('PATH', star_bin) + context.Result(star_root) + context.env.Replace(PREFIX = star_root) + context.env.Append(CPPPATH=star_inc, LIBPATH=star_lib) + return { "root": star_root, + "lib": star_lib, + "include": star_inc, + "bin": star_bin, + "share": star_share, } + context.Result("failed") + return None + +# Allow --prefix to be specified. We don't use it in Starlink mode +# though +AddOption('--prefix', + dest='prefix', + type='string', + nargs=1, + action='store', + metavar='DIR', + help='installation prefix') + +env = Environment(PREFIX = "/usr/local" ) # Initialise the environment + +prefix = GetOption("prefix") +if prefix: + env.Replace(PREFIX = prefix) + + +# Basic configure checks: but not if --help or --clean +if not GetOption("help") and not GetOption("clean"): + conf = Configure(env, custom_tests = {"CheckStarlink": CheckStarlink} ) + + if not conf.CheckCC(): + print("!! Your compiler and/or environment is not correctly configured.") + Exit(0) + + if conf.CheckFunc("copysign"): + conf.env.Append(CPPDEFINES={"HAVE_COPYSIGN": 1}) + + if conf.CheckFunc("isblank"): + conf.env.Append(CPPDEFINES={"HAVE_ISBLANK": 1}) + + if conf.CheckFunc("strlcpy"): + conf.env.Append(CPPDEFINES={"HAVE_STRLCPY": 1}) + + # Force -lm if we need it + conf.CheckLib("m","sin") + + # Try to look in current directory + conf.env.Append(LIBPATH=["."]) + conf.env.Append(CPPPATH=["."]) + + # If we are in a Starlink environment we know we have + # ERFA so just set things up for that. This should be done + # using a general SCons "are we starlink" plugin + starlink = conf.CheckStarlink() + if starlink is not None: + conf.env.Append(LIBS=["erfa"]) + conf.env.Append(CPPDEFINES={"HAVE_STAR_UTIL": 1}) + conf.env.Append(LIBS=["starutil"]) + else: + # Allow PREFIX to work + conf.env.Append(CPPPATH=[os.path.join("$PREFIX", "include")]) + conf.env.Append(LIBPATH=[os.path.join("$PREFIX", "lib")]) + + # Maybe starutil will be available + if conf.CheckLib("starutil"): + conf.env.Append(CPPDEFINES={"HAVE_STAR_UTIL": 1}) + + # Need to look for ERFA vs SOFA + if not conf.CheckLib("erfa","eraCal2jd"): + if conf.CheckLib("sofa_c","iauCal2jd"): + conf.env.Append(CPPDEFINES={"HAVE_SOFA_H": 1}) + else: + print("!! Neither ERFA not SOFA library located. Can not continue. !!") + Exit(0) + + env = conf.Finish() + +# PAL source code +libpal_sources = [ + "pal1Atms.c", + "pal1Atmt.c", + "palAddet.c", + "palAirmas.c", + "palAltaz.c", + "palAmp.c", + "palAmpqk.c", + "palAop.c", + "palAoppa.c", + "palAoppat.c", + "palAopqk.c", + "palAtmdsp.c", + "palCaldj.c", + "palDafin.c", + "palDat.c", + "palDe2h.c", + "palDeuler.c", + "palDfltin.c", + "palDh2e.c", + "palDjcal.c", + "palDmat.c", + "palDmoon.c", + "palDrange.c", + "palDs2tp.c", + "palDt.c", + "palDtp2s.c", + "palDtps2c.c", + "palDtt.c", + "palEcmat.c", + "palEl2ue.c", + "palEpco.c", + "palEpv.c", + "palEqecl.c", + "palEqgal.c", + "palEtrms.c", + "palEvp.c", + "palFk45z.c", + "palFk524.c", + "palFk54z.c", + "palGaleq.c", + "palGalsup.c", + "palGe50.c", + "palGeoc.c", + "palIntin.c", + "palMap.c", + "palMappa.c", + "palMapqk.c", + "palMapqkz.c", + "palNut.c", + "palNutc.c", + "palOap.c", + "palOapqk.c", + "palObs.c", + "palOne2One.c", + "palPa.c", + "palPertel.c", + "palPertue.c", + "palPlanel.c", + "palPlanet.c", + "palPlante.c", + "palPlantu.c", + "palPm.c", + "palPolmo.c", + "palPrebn.c", + "palPrec.c", + "palPreces.c", + "palPrenut.c", + "palPv2el.c", + "palPv2ue.c", + "palPvobs.c", + "palRdplan.c", + "palRefco.c", + "palRefro.c", + "palRefv.c", + "palRefz.c", + "palRverot.c", + "palRvgalc.c", + "palRvlg.c", + "palRvlsrd.c", + "palRvlsrk.c", + "palSubet.c", + "palSupgal.c", + "palUe2el.c", + "palUe2pv.c", + ] + +sun267_sources = [ "sun267.tex" ] +sun267_pdf = env.PDF( sun267_sources ) +Default(sun267_pdf) + +# Compiler should look in current directory for header files + +staticpal = env.StaticLibrary(target="pal", source=libpal_sources) +sharedpal = env.SharedLibrary( target="pal", source = libpal_sources, + SHLIBVERSION=version ) + +palTest = env.Program("palTest", "palTest.c", LIBS=["pal"] ) +test_alias = Alias("test", [palTest], palTest[0].abspath) +AlwaysBuild(test_alias) + +installed_sharedlib = env.InstallVersionedLib(os.path.join("$PREFIX","lib"), + [sharedpal], SHLIBVERSION=version ) +installed_staticlib = env.Install("$PREFIX/lib", [staticpal] ) + +# Just build the library by default +Default(sharedpal) +Default(staticpal) + +# install on request +if "install" in COMMAND_LINE_TARGETS: + env.Alias( "install", "$PREFIX" ) + Default(installed_sharedlib, installed_staticlib) + Index: trunk/FACT++/pal/bootstrap =================================================================== --- trunk/FACT++/pal/bootstrap (revision 18347) +++ trunk/FACT++/pal/bootstrap (revision 18347) @@ -0,0 +1,134 @@ +#! /bin/sh - +# original bootstrap file, installed by starconf 1.3, rnum=1003000 +# If you _need_ to change this file, delete `original' in the line above, +# or else starconf may overwrite it with an updated version. +# +# bootstrap.installed. Generated from bootstrap.installed.in by configure. +# +# Bootstrap a checked-out component of the Starlink software tree. +# Run this script in a freshly checked-out directory to bring the +# system to the point where you can just type ./configure;make +# +# Usage: +# ./bootstrap + + +# This script should be installed, by starconf, in all `component +# directories'. A `component directory' is a directory which has a +# component.xml.in file in it. All component directories will have a +# manifest file created and installed in .../manifests; non-component +# directories will not have manifest files. Everything that's +# installed should be installed as part of some component +# or other. +# +# The ./bootstrap scripts will stop recursing when they find a +# component.xml.in file. They'll warn if they find a component.xml.in +# file in any AC_CONFIG_SUBDIRS directory, but ignore it, and exit +# with an error if they do not find a component.xml.in file and there +# are no AC_CONFIG_SUBDIRS directories in which to search further. +# That is, the tree of directories which the top-level bootstrap +# traverses should have component.xml.in files at or above all its +# leaves. + + +# The starconf below might update bootstrap, if a newer version is +# available. Unfortunately, this confuses sh, which appears _not_ to +# keep open the script it's reading, but to reopen it afresh, or reseek +# within the file, for each line (or something like that!?). +# So rewrite this script to a temporary file and exec it. +tempfile="${TMP-/tmp}/$0-$$.tmp" +rm -f $tempfile +echo "trap 'rm -f $tempfile' 0" >$tempfile # remove temporary at exit +sed '1,/^--TRAMPOLINE--/d' $0 >>$tempfile # strip out the trampoline +exec /bin/sh $tempfile # exec the temporary +--TRAMPOLINE-- + + +echo "Bootstrapping `pwd` ..." + +if test ! -f configure.ac; then + echo "bootstrap: No configure.ac in directory `pwd`" >&2 + exit 1 +fi + +subdirs=`autoconf --trace=AC_CONFIG_SUBDIRS:$% configure.ac` + +if test -f component.xml.in; then + + if starconf --show buildsupport >/dev/null 2>&1; then + + # starconf is in the path + echo "...using starconf in " `starconf --show buildsupport` + starconf || exit 1 + + else + + # The temptation here is to use ./starconf.status to find the + # starconf that it came from and invoke that explicitly. Don't do + # this, however: we don't want to be too clever, and it's better + # to be consistent with the way the autotools behave (the first + # one in your path is the one that works, and they don't have this + # sort of `phone home' cleverness in them). + + echo "bootstrap error: The starconf application is not in your path" + + # This doesn't stop us being helpful, however. + if test -f ./starconf.status; then + starconf_home=`./starconf.status --show buildsupport` + echo "This directory was last bootstrapped with $starconf_home/bin/starconf" + fi + + exit 1 + fi + + # Check that there are no component.xml.in files in any subdirectories + if test -n "$subdirs"; then + for d in $subdirs + do + if test -d "$d" && test -f "$d/component.xml.in"; then + echo "bootstrap: warning: ignoring child $d/component.xml.in" >&2 + fi + done + fi + + # If STAR_SUPPRESS_AUTORECONF is true in the environment, then we + # suppress the call of `autoreconf'. This is here _only_ so that + # the top-level bootstrap file can suppress multiple calls of this + # in bootstrap scripts in its children. This mechanism must not + # be used by users, as it is likely to change without warning. + if ${STAR_SUPPRESS_AUTORECONF-false}; then + echo "Suppressing autoreconf in" `pwd` + else + echo autoreconf --install --symlink + autoreconf --install --symlink || exit 1 + fi + +else + + # This is not a component directory, so simply recurse into the children. + + # ...if there are any, that is. + if test -z "$subdirs"; then + echo "bootstrap: error: non-component directory `pwd` has no subdirs" >&2 + exit 1 + fi + + # Bootstrap the child directories mentioned in AC_CONFIG_SUBDIRS. + # These bootstrap files must exist. + for d in $subdirs + do + if test -d "$d"; then + echo "Bootstrapping $d..." + if test -f $d/bootstrap; then + # good... + (cd $d; /bin/sh ./bootstrap) + else + echo "bootstrap: no file $d/bootstrap" >&2 + exit 1 + fi + fi + done + +fi + +exit 0 Index: trunk/FACT++/pal/codemeta.json =================================================================== --- trunk/FACT++/pal/codemeta.json (revision 18347) +++ trunk/FACT++/pal/codemeta.json (revision 18347) @@ -0,0 +1,41 @@ +{ + "@context": "https://raw.githubusercontent.com/mbjones/codemeta/master/codemeta.jsonld", + "@type": "Code", + "author": [ + { + "@id": "http://orcid.org/0000-0001-5982-167X", + "@type": "Person", + "email": "tim.jenness@gmail.com", + "name": "Tim Jenness", + }, + { + "@id": "http://orcid.org/0000-0001-6524-2447", + "@type": "Person", + "email": "d.berry@eaobservatory.org", + "name": "David Berry", + "affiliation": "East Asian Observatory" + }, + { + "@id": "", + "@type": "Person", + "email": "patrick.wallace@stfc.ac.uk", + "name": "Patrick Wallace", + "affiliation": "STFC", + } + ], + "identifier": "http://dx.doi.org/10.5281/zenodo.17212", + "codeRepository": "https://github.com/Starlink/pal", + "dateCreated": "2012-02-08", + "description": "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.", + "keywords": "astronomy, Starlink, astrometry", + "license": "http://opensource.org/licenses/GPL-3.0", + "title": "PAL: Positional Astronomy Library", + "version": "0.9.1", + "uploadedBy": + { + "@id": "http://orcid.org/0000-0001-5982-167X", + "@type": "Person", + "email": "tim.jenness@gmail.com", + "name": "Tim Jenness", + } +} Index: trunk/FACT++/pal/component.xml =================================================================== --- trunk/FACT++/pal/component.xml (revision 18347) +++ trunk/FACT++/pal/component.xml (revision 18347) @@ -0,0 +1,28 @@ + + + + + + 0.9.3 + libext/pal + Positional Astronomy Library +

+ 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. +

+ + erfastarutilerfastarutilstar2html + + + + Tim Jenness + t.jenness@jach.hawaii.edu + + + sun267 + starlink@jiscmail.ac.uk + + Index: trunk/FACT++/pal/component.xml.in =================================================================== --- trunk/FACT++/pal/component.xml.in (revision 18347) +++ trunk/FACT++/pal/component.xml.in (revision 18347) @@ -0,0 +1,28 @@ + + + + + + @PACKAGE_VERSION@ + libext/pal + Positional Astronomy Library +

+ 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. +

+ + @STAR_DEPENDENCIES_CHILDREN@ + + + + Tim Jenness + t.jenness@jach.hawaii.edu + + + @STAR_DOCUMENTATION@ + @PACKAGE_BUGREPORT@ + + Index: trunk/FACT++/pal/configure.ac =================================================================== --- trunk/FACT++/pal/configure.ac (revision 18347) +++ trunk/FACT++/pal/configure.ac (revision 18347) @@ -0,0 +1,137 @@ +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],[0.9.3],[starlink@jiscmail.ac.uk]) +AC_CONFIG_AUX_DIR([build-aux]) + +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 Would like the version number as an integer +AC_DEFINE_UNQUOTED([PACKAGE_VERSION_INTEGER], $PACKAGE_VERSION_INTEGER, + [Integer version number, in the form major*1e6+minor*1e3+release]) + +dnl Find required versions of the programs we need for configuration +AC_PROG_CC +LT_INIT + +# If --with-pic=no is set we should honour that. +AM_CONDITIONAL(NOPIC, test x$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]) +AS_IF([test "x$ac_cv_search_strlcpy" = "x-lbsd"], [AC_CHECK_HEADERS([bsd/string.h])]) +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 $STARLINK will be unset but to play safe we also check STARCONF_DEFAULT_PREFIX +dnl If we do not have Starlink we can do the test anyhow just in case + +if test -n "$STARCONF_DEFAULT_PREFIX" -a -n "$STARLINK" +then + AC_MSG_NOTICE([Assuming a Starlink environment]) + AC_SUBST( STARUTIL_LIBADD, "${libdir}/libstarutil.la" ) + AC_SUBST( ERFA_LIBADD, "${libdir}/liberfa.la" ) + AC_SUBST( ERFA_LDFLAGS, "" ) + AC_DEFINE( [HAVE_STAR_UTIL_H], [1], [Define to 1 if you have the header file]) +else + + # Allow ERFA/SOFA location to be specified using --with-erfa=$ERFA_DIR + # Assumes that the value supplied here is the root and lib and include directories + # are below it. --with-erfa=no or --without-erfa will result in ERFA being + # located in $PREFIX tree. This option is only effective if Starlink is not + # active. + AC_ARG_WITH(erfa, + AS_HELP_STRING([--with-erfa], + [Location of ERFA/SOFA tree]), + [if test -z "$withval" -o "$withval" = yes; then + unset ERFA_DIR + elif test "X$withval" = Xno; then + unset ERFA_DIR + elif test -d "$withval"; then + ERFA_DIR="$withval" + else + unset ERFA_DIR + AC_MSG_WARN([--with-erfa given nonexistent directory; ignored: using default instead]) + fi]) + if test -n "$ERFA_DIR"; then + AC_MSG_NOTICE([ERFA/SOFA tree located at $ERFA_DIR]) + erfa_includedir="${ERFA_DIR}/include" + erfa_libdir="${ERFA_DIR}/lib" + else + ERFA_DIR=${prefix} + erfa_includedir=${includedir} + erfa_libdir=${libdir} + AC_MSG_NOTICE([Looking for ERFA/SOFA in default location of $ERFA_DIR]) + fi + + dnl AC_CHECK_HEADERS does not search $includedir + save_CPPFLAGS="$CPPFLAGS" + eval CPPFLAGS=\"$CPPFLAGS -I${includedir} -I${erfa_includedir}\" + eval CPPFLAGS=\"$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} -L${erfa_libdir}\" + eval LDFLAGS=\"$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 $prefix values and the ERFA values + AC_SUBST( ERFA_LDFLAGS, "-L${libdir} -L${erfa_libdir}" ) + AC_SUBST( ERFA_CPPFLAGS, "-I${includedir} -I${erfa_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, [erfa starutil]) +STAR_DECLARE_DEPENDENCIES(link, [erfa 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 Index: trunk/FACT++/pal/pal.h =================================================================== --- trunk/FACT++/pal/pal.h (revision 18347) +++ trunk/FACT++/pal/pal.h (revision 18347) @@ -0,0 +1,551 @@ +#ifndef PALHDEF +#define PALHDEF + +/* +*+ +* Name: +* pal.h + +* Purpose: +* Function prototypes for PAL routines. + +* Language: +* Starlink ANSI C + +* Type of Module: +* Include file + +* Description: +* Function prototypes for PAL routines. + +* Authors: +* TIMJ: Tim Jenness (JAC, Hawaii) +* {enter_new_authors_here} + +* Notes: +* + +* History: +* 2012-02-08 (TIMJ): +* Initial version. 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 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} +*- +*/ + +#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] ); + +int palVers ( char * verstring, size_t verlen ); + +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 Index: trunk/FACT++/pal/pal.news =================================================================== --- trunk/FACT++/pal/pal.news (revision 18347) +++ trunk/FACT++/pal/pal.news (revision 18347) @@ -0,0 +1,134 @@ +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. + +V0.9.3 + +- Fix value of small in palFk524. Typo in port from Fortran + had removed the "e" in the number. Thanks to @danielsf. + +- Add test for palFk524 + +V0.9.2 + +Thanks to Github user @nega0 for some BSD build fixes. + +More STARCONF_DEFAULT_PREFIX fixes for Scons file and for +document building. + +New configure option: --with-erfa to allow the ERFA +root location to be specified. + +V0.9.1 + +Now checks for STARCONF_DEFAULT_PREFIX environment variable +when deciding whether a Starlink environment is present. This +was more reliable than checking for STARLINK_DIR. + +V0.9.0 + +Add palPcd and palUnpcd + +V0.8.0 + +Add palEcleq + +V0.7.0 + +Add palPolmo. + +V0.6.0 + +New function, palVers, provides API access to the PAL +version number as a string or integer. + +V0.5.1 + +The configure script was getting confused if run outside of +Starlink without using --without-starlink. This was because +$STARLINK is set in the script if it is not set and the +configure script was assuming $STARLINK would be unset +outside of a Starlink environment. The configure script +now keys off $STARLINK_DIR but that may interact badly +if STARLINK_DIR is set and --without-starlink is used. + +An experimental SConstruct build script is now available +for users of scons. + +SUN/267 has been synced up with the associated source files. + +palIntin now respects the isblank configure check (as it +should have done all along). + +Minor clean ups of some source prologues. + +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. Index: trunk/FACT++/pal/pal1.h =================================================================== --- trunk/FACT++/pal/pal1.h (revision 18347) +++ trunk/FACT++/pal/pal1.h (revision 18347) @@ -0,0 +1,68 @@ +/* +*+ +* 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 Index: trunk/FACT++/pal/pal1Atms.c =================================================================== --- trunk/FACT++/pal/pal1Atms.c (revision 18347) +++ trunk/FACT++/pal/pal1Atms.c (revision 18347) @@ -0,0 +1,95 @@ +/* +*+ +* 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; + +} + Index: trunk/FACT++/pal/pal1Atmt.c =================================================================== --- trunk/FACT++/pal/pal1Atmt.c (revision 18347) +++ trunk/FACT++/pal/pal1Atmt.c (revision 18347) @@ -0,0 +1,119 @@ +/* +*+ +* 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 ); + +} Index: trunk/FACT++/pal/pal1sofa.h =================================================================== --- trunk/FACT++/pal/pal1sofa.h (revision 18347) +++ trunk/FACT++/pal/pal1sofa.h (revision 18347) @@ -0,0 +1,142 @@ +/* +*+ +* Name: +* pal1sofa.h + +* Purpose: +* Mappings of ERFA names to SOFA names + +* Language: +* Starlink ANSI C + +* Type of Module: +* Include file + +* Invocation: +* #include "pal1sofa.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 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} +*- +*/ + +#ifndef PAL1SOFAHDEF +#define PAL1SOFAHDEF + +#if HAVE_CONFIG_H +# include +#endif + +# 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 Index: trunk/FACT++/pal/palAddet.c =================================================================== --- trunk/FACT++/pal/palAddet.c (revision 18347) +++ trunk/FACT++/pal/palAddet.c (revision 18347) @@ -0,0 +1,112 @@ +/* +*+ +* 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 ); + +} Index: trunk/FACT++/pal/palAirmas.c =================================================================== --- trunk/FACT++/pal/palAirmas.c (revision 18347) +++ trunk/FACT++/pal/palAirmas.c (revision 18347) @@ -0,0 +1,99 @@ +/* +*+ +* 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; +} Index: trunk/FACT++/pal/palAltaz.c =================================================================== --- trunk/FACT++/pal/palAltaz.c (revision 18347) +++ trunk/FACT++/pal/palAltaz.c (revision 18347) @@ -0,0 +1,200 @@ +/* +*+ +* Name: +* palAltaz + +* Purpose: +* Positions, velocities and accelerations for an altazimuth telescope mount + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* 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 ); + +* Arguments: +* ha = double (Given) +* Hour angle (radians) +* dec = double (Given) +* Declination (radians) +* phi = double (Given) +* Observatory latitude (radians) +* az = double * (Returned) +* Azimuth (radians) +* azd = double * (Returned) +* Azimuth velocity (radians per radian of HA) +* azdd = double * (Returned) +* Azimuth acceleration (radians per radian of HA squared) +* el = double * (Returned) +* Elevation (radians) +* eld = double * (Returned) +* Elevation velocity (radians per radian of HA) +* eldd = double * (Returned) +* Elevation acceleration (radians per radian of HA squared) +* pa = double * (Returned) +* Parallactic angle (radians) +* pad = double * (Returned) +* Parallactic angle velocity (radians per radian of HA) +* padd = double * (Returned) +* Parallactic angle acceleration (radians per radian of HA squared) + + +* Description: +* Positions, velocities and accelerations for an altazimuth +* telescope mount. + +* Authors: +* PTW: P. T. Wallace +* TIMJ: Tim Jenness (Cornell) +* {enter_new_authors_here} + +* Notes: +* - Natural units are used throughout. HA, DEC, PHI, AZ, EL +* and ZD are in radians. The velocities and accelerations +* assume constant declination and constant rate of change of +* hour angle (as for tracking a star); the units of AZD, ELD +* and PAD are radians per radian of HA, while the units of AZDD, +* ELDD and PADD are radians per radian of HA squared. To +* convert into practical degree- and second-based units: +* +* angles * 360/2pi -> degrees +* velocities * (2pi/86400)*(360/2pi) -> degree/sec +* accelerations * ((2pi/86400)**2)*(360/2pi) -> degree/sec/sec +* +* Note that the seconds here are sidereal rather than SI. One +* sidereal second is about 0.99727 SI seconds. +* +* The velocity and acceleration factors assume the sidereal +* tracking case. Their respective numerical values are (exactly) +* 1/240 and (approximately) 1/3300236.9. +* +* - Azimuth is returned in the range 0-2pi; north is zero, +* and east is +pi/2. Elevation and parallactic angle are +* returned in the range +/-pi. Parallactic angle is +ve for +* a star west of the meridian and is the angle NP-star-zenith. +* +* - The latitude is geodetic as opposed to geocentric. The +* hour angle and declination are topocentric. Refraction and +* deficiencies in the telescope mounting are ignored. The +* purpose of the routine is to give the general form of the +* quantities. The details of a real telescope could profoundly +* change the results, especially close to the zenith. +* +* - 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: +* 2014-09-30 (TIMJ): +* Initial version. Ported from Fortran SLA +* {enter_further_changes_here} + +* Copyright: +* Copyright (C) 2004 P.T. Wallace +* 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, see . + +* Bugs: +* {note_any_bugs_here} +*- +*/ + +#include + +#include "pal.h" +#include "palmac.h" + +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 ) { + + const double TINY = 1E-30; + + double sh,ch,sd,cd,sp,cp,chcd,sdcp,x,y,z,rsq,r,a,e,c,s, + q,qd,ad,ed,edr,add,edd,qdd; + + + /* Useful functions */ + sh=sin(ha); + ch=cos(ha); + sd=sin(dec); + cd=cos(dec); + sp=sin(phi); + cp=cos(phi); + chcd=ch*cd; + sdcp=sd*cp; + x=-chcd*sp+sdcp; + y=-sh*cd; + z=chcd*cp+sd*sp; + rsq=x*x+y*y; + r=sqrt(rsq); + + /* Azimuth and elevation */ + if (rsq == 0.0) { + a=0.0; + } else { + a=atan2(y,x); + } + if (a < 0.0) a += PAL__D2PI; + e=atan2(z,r); + + /* Parallactic angle */ + c=cd*sp-ch*sdcp; + s=sh*cp; + if (c*c+s*s > 0) { + q=atan2(s,c); + } else { + q= PAL__DPI - ha; + } + + /* Velocities and accelerations (clamped at zenith/nadir) */ + if (rsq < TINY) { + rsq=TINY; + r=sqrt(rsq); + } + qd=-x*cp/rsq; + ad=sp+z*qd; + ed=cp*y/r; + edr=ed/r; + add=edr*(z*sp+(2.0-rsq)*qd); + edd=-r*qd*ad; + qdd=edr*(sp+2.0*z*qd); + + /* Results */ + *az=a; + *azd=ad; + *azdd=add; + *el=e; + *eld=ed; + *eldd=edd; + *pa=q; + *pad=qd; + *padd=qdd; + +} Index: trunk/FACT++/pal/palAmp.c =================================================================== --- trunk/FACT++/pal/palAmp.c (revision 18347) +++ trunk/FACT++/pal/palAmp.c (revision 18347) @@ -0,0 +1,84 @@ +/* +*+ +* 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 ); +} Index: trunk/FACT++/pal/palAmpqk.c =================================================================== --- trunk/FACT++/pal/palAmpqk.c (revision 18347) +++ trunk/FACT++/pal/palAmpqk.c (revision 18347) @@ -0,0 +1,128 @@ +/* +*+ +* 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 ); +} Index: trunk/FACT++/pal/palAop.c =================================================================== --- trunk/FACT++/pal/palAop.c (revision 18347) +++ trunk/FACT++/pal/palAop.c (revision 18347) @@ -0,0 +1,238 @@ +/* +*+ +* 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); + +} Index: trunk/FACT++/pal/palAoppa.c =================================================================== --- trunk/FACT++/pal/palAoppa.c (revision 18347) +++ trunk/FACT++/pal/palAoppa.c (revision 18347) @@ -0,0 +1,963 @@ +/* +*+ +* 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 pal_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 */ + pal_eqeqx=dpsi*cos(eps0)+PAL__DAS2R*(0.00264*sin(om)+ + 0.000063*sin(om+om)); + + return pal_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 , 0 , 0 , 0 }, + { 2 , 0 , 0 , 2 , 0 , 0 , 0 , 0 , 0 }, + { 1 , 1 , 2 , 0 , 1 , 0 , 0 , 0 , 0 }, + { -1 , 0 , 0 , 2 , 2 , 0 , 0 , 0 , 0 }, + { 1 , 0 , -2 , 2 , 0 , 0 , 0 , 0 , 0 }, + { 0 , -1 , 0 , 2 , -1 , 0 , 0 , 0 , 0 }, + { -1 , 0 , 1 , 0 , 2 , 0 , 0 , 0 , 0 }, + { 0 , 1 , 0 , 1 , 0 , 0 , 0 , 0 , 0 }, + { 1 , 0 , -2 , 2 , -2 , 0 , 0 , 0 , 0 }, + { 0 , 0 , 0 , 1 , -1 , 0 , 0 , 0 , 0 }, + { 1 , -1 , 0 , 0 , -1 , 0 , 0 , 0 , 0 }, + { 0 , 0 , 0 , 4 , 0 , 0 , 0 , 0 , 0 }, + { 1 , -1 , 0 , 2 , 0 , 0 , 0 , 0 , 0 }, + { 1 , 0 , 2 , 1 , 2 , 0 , 0 , 0 , 0 }, + { 1 , 0 , 2 , -1 , 2 , 0 , 0 , 0 , 0 }, + { -1 , 0 , 0 , 2 , -2 , 0 , 0 , 0 , 0 }, + { 0 , 0 , 2 , 1 , 1 , 0 , 0 , 0 , 0 }, + { -1 , 0 , 2 , 0 , -1 , 0 , 0 , 0 , 0 }, + { -1 , 0 , 2 , 4 , 1 , 0 , 0 , 0 , 0 }, + { 0 , 0 , 2 , 2 , 0 , 0 , 0 , 0 , 0 }, + { 1 , 1 , 2 , -2 , 1 , 0 , 0 , 0 , 0 }, + { 0 , 0 , 1 , 0 , 1 , 0 , 0 , 0 , 0 }, + { -1 , 0 , 2 , -1 , 1 , 0 , 0 , 0 , 0 }, + { -2 , 0 , 2 , 2 , 1 , 0 , 0 , 0 , 0 }, + { 2 , -1 , 0 , 0 , 0 , 0 , 0 , 0 , 0 }, + { 4 , 0 , 2 , 0 , 2 , 0 , 0 , 0 , 0 }, + { 2 , 1 , 2 , -2 , 2 , 0 , 0 , 0 , 0 }, + { 0 , 1 , 2 , 1 , 2 , 0 , 0 , 0 , 0 }, + { 1 , 0 , 4 , -2 , 2 , 0 , 0 , 0 , 0 }, + { 1 , 1 , 0 , 0 , -1 , 0 , 0 , 0 , 0 }, + { -2 , 0 , 2 , 4 , 1 , 0 , 0 , 0 , 0 }, + { 2 , 0 , 2 , 0 , 0 , 0 , 0 , 0 , 0 }, + { -1 , 0 , 1 , 0 , 0 , 0 , 0 , 0 , 0 }, + { 1 , 0 , 0 , 1 , 0 , 0 , 0 , 0 , 0 }, + { 0 , 1 , 0 , 2 , 1 , 0 , 0 , 0 , 0 }, + { -1 , 0 , 4 , 0 , 1 , 0 , 0 , 0 , 0 }, + { -1 , 0 , 0 , 4 , 1 , 0 , 0 , 0 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0.29999999999999999 }, + { -3.7999999999999998 , 0.40000000000000002 , 0.0000000000000000 , -0.20000000000000001 }, + { 12.600000000000000 , 3.2000000000000002 , 0.50000000000000000 , -1.5000000000000000 }, + { 0.10000000000000001 , 0.0000000000000000 , 0.0000000000000000 , 0.0000000000000000 }, + { -13.600000000000000 , 2.3999999999999999 , -0.10000000000000001 , 0.0000000000000000 }, + { 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; + +} Index: trunk/FACT++/pal/palAoppat.c =================================================================== --- trunk/FACT++/pal/palAoppat.c (revision 18347) +++ trunk/FACT++/pal/palAoppat.c (revision 18347) @@ -0,0 +1,103 @@ +/* +*+ +* 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/ERFA 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; +} Index: trunk/FACT++/pal/palAopqk.c =================================================================== --- trunk/FACT++/pal/palAopqk.c (revision 18347) +++ trunk/FACT++/pal/palAopqk.c (revision 18347) @@ -0,0 +1,288 @@ +/* +*+ +* 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 (fabs(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; + +} Index: trunk/FACT++/pal/palAtmdsp.c =================================================================== --- trunk/FACT++/pal/palAtmdsp.c (revision 18347) +++ trunk/FACT++/pal/palAtmdsp.c (revision 18347) @@ -0,0 +1,180 @@ +/* +*+ +* 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; + } + } + +} Index: trunk/FACT++/pal/palCaldj.c =================================================================== --- trunk/FACT++/pal/palCaldj.c (revision 18347) +++ trunk/FACT++/pal/palCaldj.c (revision 18347) @@ -0,0 +1,99 @@ +/* +*+ +* 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/ERFA 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 ); +} Index: trunk/FACT++/pal/palDafin.c =================================================================== --- trunk/FACT++/pal/palDafin.c (revision 18347) +++ trunk/FACT++/pal/palDafin.c (revision 18347) @@ -0,0 +1,194 @@ +/* +*+ +* 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; + +} Index: trunk/FACT++/pal/palDat.c =================================================================== --- trunk/FACT++/pal/palDat.c (revision 18347) +++ trunk/FACT++/pal/palDat.c (revision 18347) @@ -0,0 +1,95 @@ +/* +*+ +* Name: +* palDat + +* Purpose: +* Return offset between UTC and TAI + +* 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/ERFA eraDat function. +* - This routine matches the slaDat interface which differs from the eraDat +* interface. Consider coding directly to the SOFA/ERFA 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; +} Index: trunk/FACT++/pal/palDe2h.c =================================================================== --- trunk/FACT++/pal/palDe2h.c (revision 18347) +++ trunk/FACT++/pal/palDe2h.c (revision 18347) @@ -0,0 +1,142 @@ +/* +*+ +* 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; +} Index: trunk/FACT++/pal/palDeuler.c =================================================================== --- trunk/FACT++/pal/palDeuler.c (revision 18347) +++ trunk/FACT++/pal/palDeuler.c (revision 18347) @@ -0,0 +1,141 @@ +/* +*+ +* 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; +} Index: trunk/FACT++/pal/palDfltin.c =================================================================== --- trunk/FACT++/pal/palDfltin.c (revision 18347) +++ trunk/FACT++/pal/palDfltin.c (revision 18347) @@ -0,0 +1,258 @@ +/* +*+ +* 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 + +#ifdef HAVE_BSD_STRING_H +#include +#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; + +} Index: trunk/FACT++/pal/palDh2e.c =================================================================== --- trunk/FACT++/pal/palDh2e.c (revision 18347) +++ trunk/FACT++/pal/palDh2e.c (revision 18347) @@ -0,0 +1,133 @@ +/* +*+ +* 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; +} Index: trunk/FACT++/pal/palDjcal.c =================================================================== --- trunk/FACT++/pal/palDjcal.c (revision 18347) +++ trunk/FACT++/pal/palDjcal.c (revision 18347) @@ -0,0 +1,97 @@ +/* +*+ +* 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); + +} Index: trunk/FACT++/pal/palDmat.c =================================================================== --- trunk/FACT++/pal/palDmat.c (revision 18347) +++ trunk/FACT++/pal/palDmat.c (revision 18347) @@ -0,0 +1,182 @@ +/* +*+ +* 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; + +} Index: trunk/FACT++/pal/palDrange.c =================================================================== --- trunk/FACT++/pal/palDrange.c (revision 18347) +++ trunk/FACT++/pal/palDrange.c (revision 18347) @@ -0,0 +1,77 @@ +/* +*+ +* 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; +} + Index: trunk/FACT++/pal/palDs2tp.c =================================================================== --- trunk/FACT++/pal/palDs2tp.c (revision 18347) +++ trunk/FACT++/pal/palDs2tp.c (revision 18347) @@ -0,0 +1,127 @@ +/* +*+ +* 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; +} Index: trunk/FACT++/pal/palDt.c =================================================================== --- trunk/FACT++/pal/palDt.c (revision 18347) +++ trunk/FACT++/pal/palDt.c (revision 18347) @@ -0,0 +1,125 @@ +/* +*+ +* 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; + +} Index: trunk/FACT++/pal/palDtp2s.c =================================================================== --- trunk/FACT++/pal/palDtp2s.c (revision 18347) +++ trunk/FACT++/pal/palDtp2s.c (revision 18347) @@ -0,0 +1,95 @@ +/* +*+ +* 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; +} Index: trunk/FACT++/pal/palDtps2c.c =================================================================== --- trunk/FACT++/pal/palDtps2c.c (revision 18347) +++ trunk/FACT++/pal/palDtps2c.c (revision 18347) @@ -0,0 +1,151 @@ +/* +*+ +* 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; +} Index: trunk/FACT++/pal/palDtt.c =================================================================== --- trunk/FACT++/pal/palDtt.c (revision 18347) +++ trunk/FACT++/pal/palDtt.c (revision 18347) @@ -0,0 +1,77 @@ +/* +*+ +* 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.iausofa.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 ); +} Index: trunk/FACT++/pal/palEcleq.c =================================================================== --- trunk/FACT++/pal/palEcleq.c (revision 18347) +++ trunk/FACT++/pal/palEcleq.c (revision 18347) @@ -0,0 +1,97 @@ +/* +*+ +* Name: +* palEcleq + +* Purpose: +* Transform from ecliptic coordinates to J2000.0 equatorial coordinates + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* void palEcleq ( double dl, double db, double date, +* double *dr, double *dd ); + +* Arguments: +* dl = double (Given) +* Ecliptic longitude (mean of date, IAU 1980 theory, radians) +* db = double (Given) +* Ecliptic latitude (mean of date, IAU 1980 theory, 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). +* dr = double * (Returned) +* J2000.0 mean RA (radians) +* dd = double * (Returned) +* J2000.0 mean Dec (Radians) + +* Description: +* Transform from ecliptic coordinate to J2000.0 equatorial coordinates. + +* Authors: +* PTW: Patrick T. Wallace +* TIMJ: Tim Jenness (Cornell University) +* {enter_new_authors_here} + +* History: +* 2014-11-18 (TIMJ): +* Initial version +* Adapted with permission from the Fortran SLALIB library. +* {enter_further_changes_here} + +* Copyright: +* Copyright (C) 1995 Rutherford Appleton Laboratory +* 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} +*- +*/ + +#include "pal.h" +#include "pal1sofa.h" + +void palEcleq ( double dl, double db, double date, double *dr, double *dd ) { + double v1[3], v2[3]; + double rmat[3][3]; + + /* Spherical to Cartesian */ + eraS2c( dl, db, v1 ); + + /* Ecliptic to equatorial */ + palEcmat( date, rmat ); + eraTrxp( rmat, v1, v2 ); + + /* Mean of date to J2000 */ + palPrec( 2000.0, palEpj(date), rmat ); + eraTrxp( rmat, v2, v1 ); + + /* Cartesian to spherical */ + eraC2s( v1, dr, dd ); + + /* Express in conventional range */ + *dr = eraAnp( *dr ); + *dd = palDrange( *dd ); +} Index: trunk/FACT++/pal/palEcmat.c =================================================================== --- trunk/FACT++/pal/palEcmat.c (revision 18347) +++ trunk/FACT++/pal/palEcmat.c (revision 18347) @@ -0,0 +1,82 @@ +/* +*+ +* 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 ); + +} Index: trunk/FACT++/pal/palEl2ue.c =================================================================== --- trunk/FACT++/pal/palEl2ue.c (revision 18347) +++ trunk/FACT++/pal/palEl2ue.c (revision 18347) @@ -0,0 +1,351 @@ +/* +*+ +* 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; + +} Index: trunk/FACT++/pal/palEpco.c =================================================================== --- trunk/FACT++/pal/palEpco.c (revision 18347) +++ trunk/FACT++/pal/palEpco.c (revision 18347) @@ -0,0 +1,102 @@ +/* +*+ +* 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; +} Index: trunk/FACT++/pal/palEpv.c =================================================================== --- trunk/FACT++/pal/palEpv.c (revision 18347) +++ trunk/FACT++/pal/palEpv.c (revision 18347) @@ -0,0 +1,96 @@ +/* +*+ +* 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]; + } + +} Index: trunk/FACT++/pal/palEqecl.c =================================================================== --- trunk/FACT++/pal/palEqecl.c (revision 18347) +++ trunk/FACT++/pal/palEqecl.c (revision 18347) @@ -0,0 +1,97 @@ +/* +*+ +* 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 ); + + /* Express in conventional range */ + *dl = eraAnp( *dl ); + *db = palDrange( *db ); +} Index: trunk/FACT++/pal/palEqgal.c =================================================================== --- trunk/FACT++/pal/palEqgal.c (revision 18347) +++ trunk/FACT++/pal/palEqgal.c (revision 18347) @@ -0,0 +1,118 @@ +/* +*+ +* 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 ); + +} Index: trunk/FACT++/pal/palEtrms.c =================================================================== --- trunk/FACT++/pal/palEtrms.c (revision 18347) +++ trunk/FACT++/pal/palEtrms.c (revision 18347) @@ -0,0 +1,106 @@ +/* +*+ +* 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); + +} Index: trunk/FACT++/pal/palEvp.c =================================================================== --- trunk/FACT++/pal/palEvp.c (revision 18347) +++ trunk/FACT++/pal/palEvp.c (revision 18347) @@ -0,0 +1,110 @@ +/* +*+ +* 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]; + } +} Index: trunk/FACT++/pal/palFk45z.c =================================================================== --- trunk/FACT++/pal/palFk45z.c (revision 18347) +++ trunk/FACT++/pal/palFk45z.c (revision 18347) @@ -0,0 +1,186 @@ +/* +*+ +* 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 ); +} + + Index: trunk/FACT++/pal/palFk524.c =================================================================== --- trunk/FACT++/pal/palFk524.c (revision 18347) +++ trunk/FACT++/pal/palFk524.c (revision 18347) @@ -0,0 +1,259 @@ +/* +*+ +* 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 = 1.0E-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; +} Index: trunk/FACT++/pal/palFk54z.c =================================================================== --- trunk/FACT++/pal/palFk54z.c (revision 18347) +++ trunk/FACT++/pal/palFk54z.c (revision 18347) @@ -0,0 +1,113 @@ +/* +*+ +* 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; + +} + Index: trunk/FACT++/pal/palGaleq.c =================================================================== --- trunk/FACT++/pal/palGaleq.c (revision 18347) +++ trunk/FACT++/pal/palGaleq.c (revision 18347) @@ -0,0 +1,118 @@ +/* +*+ +* 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 ); + +} Index: trunk/FACT++/pal/palGalsup.c =================================================================== --- trunk/FACT++/pal/palGalsup.c (revision 18347) +++ trunk/FACT++/pal/palGalsup.c (revision 18347) @@ -0,0 +1,116 @@ +/* +*+ +* 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 ); + +} Index: trunk/FACT++/pal/palGe50.c =================================================================== --- trunk/FACT++/pal/palGe50.c (revision 18347) +++ trunk/FACT++/pal/palGe50.c (revision 18347) @@ -0,0 +1,128 @@ +/* +*+ +* 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 ); + +} Index: trunk/FACT++/pal/palGeoc.c =================================================================== --- trunk/FACT++/pal/palGeoc.c (revision 18347) +++ trunk/FACT++/pal/palGeoc.c (revision 18347) @@ -0,0 +1,83 @@ +/* +*+ +* 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; +} Index: trunk/FACT++/pal/palIntin.c =================================================================== --- trunk/FACT++/pal/palIntin.c (revision 18347) +++ trunk/FACT++/pal/palIntin.c (revision 18347) @@ -0,0 +1,185 @@ +/* +*+ +* 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. +* 2014-08-07 (TIMJ): +* Check for isblank availability. +* {enter_further_changes_here} + +* Copyright: +* Copyright (C) 2012,2014 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} +*- +*/ + +#if HAVE_CONFIG_H +# include +#endif + +#include +#include + +/* isblank() is a C99 feature so we just reimplement it if it is missing */ +#if HAVE_ISBLANK +#ifndef _ISOC99_SOURCE +#define _ISOC99_SOURCE +#endif +#include +# define ISBLANK isblank +#else + +static int ISBLANK( int c ) { + return ( c == ' ' || c == '\t' ); +} + +#endif + +/* Still need ctype for isalpha and isdigit */ +#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; + +} Index: trunk/FACT++/pal/palMap.c =================================================================== --- trunk/FACT++/pal/palMap.c (revision 18347) +++ trunk/FACT++/pal/palMap.c (revision 18347) @@ -0,0 +1,128 @@ +/* +*+ +* 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 ); + +} Index: trunk/FACT++/pal/palMappa.c =================================================================== --- trunk/FACT++/pal/palMappa.c (revision 18347) +++ trunk/FACT++/pal/palMappa.c (revision 18347) @@ -0,0 +1,129 @@ +/* +*+ +* 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 ] ); +} Index: trunk/FACT++/pal/palMapqk.c =================================================================== --- trunk/FACT++/pal/palMapqk.c (revision 18347) +++ trunk/FACT++/pal/palMapqk.c (revision 18347) @@ -0,0 +1,159 @@ +/* +*+ +* 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 ); + +} Index: trunk/FACT++/pal/palMapqkz.c =================================================================== --- trunk/FACT++/pal/palMapqkz.c (revision 18347) +++ trunk/FACT++/pal/palMapqkz.c (revision 18347) @@ -0,0 +1,127 @@ +/* +*+ +* Name: +* palMapqkz + +* Purpose: +* Quick mean to apparent place (no proper motion or parallax). + +* 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 ); +} Index: trunk/FACT++/pal/palNut.c =================================================================== --- trunk/FACT++/pal/palNut.c (revision 18347) +++ trunk/FACT++/pal/palNut.c (revision 18347) @@ -0,0 +1,85 @@ +/* +*+ +* 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 "pal.h" + +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 ); + +} Index: trunk/FACT++/pal/palNutc.c =================================================================== --- trunk/FACT++/pal/palNutc.c (revision 18347) +++ trunk/FACT++/pal/palNutc.c (revision 18347) @@ -0,0 +1,80 @@ +/* +*+ +* 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/ERFA 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 ); +} Index: trunk/FACT++/pal/palOap.c =================================================================== --- trunk/FACT++/pal/palOap.c (revision 18347) +++ trunk/FACT++/pal/palOap.c (revision 18347) @@ -0,0 +1,234 @@ +/* +*+ +* 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); + +} Index: trunk/FACT++/pal/palOapqk.c =================================================================== --- trunk/FACT++/pal/palOapqk.c (revision 18347) +++ trunk/FACT++/pal/palOapqk.c (revision 18347) @@ -0,0 +1,266 @@ +/* +*+ +* 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 palRefco 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); + +} Index: trunk/FACT++/pal/palObs.c =================================================================== --- trunk/FACT++/pal/palObs.c (revision 18347) +++ trunk/FACT++/pal/palObs.c (revision 18347) @@ -0,0 +1,928 @@ +/* +*+ +* 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 palOBS (and 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 + +#ifdef HAVE_BSD_STRING_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" + +/* +*+ +* Name: +* palCldj + +* Purpose: +* Gregorian Calendar to Modified Julian Date + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* palCldj( int iy, int im, int id, double *djm, int *j ); + +* Arguments: +* iy = int (Given) +* Year in Gregorian calendar +* im = int (Given) +* Month in Gregorian calendar +* id = int (Given) +* Day in Gregorian calendar +* djm = double * (Returned) +* Modified Julian Date (JD-2400000.5) for 0 hrs +* j = int * (Returned) +* status: 0 = OK, 1 = bad year (MJD not computed), +* 2 = bad month (MJD not computed), 3 = bad day (MJD computed). + +* Description: +* Gregorian calendar to Modified Julian Date. + +* Notes: +* - Uses eraCal2jd(). See SOFA/ERFA documentation for details. + +*- +*/ + +void palCldj ( int iy, int im, int id, double *djm, int *j ) { + double djm0; + *j = eraCal2jd( iy, im, id, &djm0, djm ); +} + +/* +*+ +* Name: +* palDbear + +* Purpose: +* Bearing (position angle) of one point on a sphere relative to another + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* pa = palDbear( double a1, double b1, double a2, double b2 ); + +* Arguments: +* a1 = double (Given) +* Longitude of point A (e.g. RA) in radians. +* a2 = double (Given) +* Latitude of point A (e.g. Dec) in radians. +* b1 = double (Given) +* Longitude of point B in radians. +* b2 = double (Given) +* Latitude of point B in radians. + +* Returned Value: +* The result is the bearing (position angle), in radians, of point +* A2,B2 as seen from point A1,B1. It is in the range +/- pi. If +* A2,B2 is due east of A1,B1 the bearing is +pi/2. Zero is returned +* if the two points are coincident. + +* Description: +* Bearing (position angle) of one point in a sphere relative to another. + +* Notes: +* - Uses eraPas(). See SOFA/ERFA documentation for details. + +*- +*/ + +double palDbear ( double a1, double b1, double a2, double b2 ) { + return eraPas( a1, b1, a2, b2 ); +} + +/* +*+ +* Name: +* palDaf2r + +* Purpose: +* Convert degrees, arcminutes, arcseconds to radians + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* palDaf2r( int ideg, int iamin, double asec, double *rad, int *j ); + +* Arguments: +* ideg = int (Given) +* Degrees. +* iamin = int (Given) +* Arcminutes. +* iasec = double (Given) +* Arcseconds. +* rad = double * (Returned) +* Angle in radians. +* j = int * (Returned) +* Status: 0 = OK, 1 = "ideg" out of range 0-359, +* 2 = "iamin" outside of range 0-59, +* 2 = "asec" outside range 0-59.99999 + +* Description: +* Convert degrees, arcminutes, arcseconds to radians. + +* Notes: +* - Uses eraAf2a(). See SOFA/ERFA documentation for details. + +*- +*/ + +/* 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 ); +} + +/* +*+ +* Name: +* palDav2m + +* Purpose: +* Form the rotation matrix corresponding to a given axial vector. + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* palDav2m( double axvec[3], double rmat[3][3] ); + +* Arguments: +* axvec = double [3] (Given) +* Axial vector (radians) +* rmat = double [3][3] (Returned) +* Rotation matrix. + +* Description: +* A rotation matrix describes a rotation about some arbitrary axis, +* called the Euler axis. The "axial vector" supplied to this routine +* has the same direction as the Euler axis, and its magnitude is the +* amount of rotation in radians. + +* Notes: +* - Uses eraRv2m(). See SOFA/ERFA documentation for details. + +*- +*/ + +void palDav2m ( double axvec[3], double rmat[3][3] ) { + eraRv2m( axvec, rmat ); +} + +/* +*+ +* Name: +* palDcc2s + +* Purpose: +* Cartesian to spherical coordinates + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* palDcc2s( double v[3], double *a, double *b ); + +* Arguments: +* v = double [3] (Given) +* x, y, z vector. +* a = double * (Returned) +* Spherical coordinate (radians) +* b = double * (Returned) +* Spherical coordinate (radians) + +* Description: +* The spherical coordinates are longitude (+ve anticlockwise looking +* from the +ve latitude pole) and latitude. The Cartesian coordinates +* are right handed, with the x axis at zero longitude and latitude, and +* the z axis at the +ve latitude pole. + +* Notes: +* - Uses eraC2s(). See SOFA/ERFA documentation for details. + +*- +*/ + +void palDcc2s ( double v[3], double *a, double *b ) { + eraC2s( v, a, b ); +} + +/* +*+ +* Name: +* palDcs2c + +* Purpose: +* Spherical coordinates to direction cosines + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* palDcs2c( double a, double b, double v[3] ); + +* Arguments: +* a = double (Given) +* Spherical coordinate in radians (ra, long etc). +* b = double (Given) +* Spherical coordinate in radians (dec, lat etc). +* v = double [3] (Returned) +* x, y, z vector + +* Description: +* The spherical coordinates are longitude (+ve anticlockwise looking +* from the +ve latitude pole) and latitude. The Cartesian coordinates +* are right handed, with the x axis at zero longitude and latitude, and +* the z axis at the +ve latitude pole. + +* Notes: +* - Uses eraS2c(). See SOFA/ERFA documentation for details. + +*- +*/ + +void palDcs2c ( double a, double b, double v[3] ) { + eraS2c( a, b, v ); +} + +/* +*+ +* Name: +* palDd2tf + +* Purpose: +* Convert an interval in days into hours, minutes, seconds + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* palDd2tf( int ndp, double days, char *sign, int ihmsf[4] ); + +* Arguments: +* ndp = int (Given) +* Number of decimal places of seconds +* days = double (Given) +* Interval in days +* sign = char * (Returned) +* '+' or '-' (single character, not string) +* ihmsf = int [4] (Returned) +* Hours, minutes, seconds, fraction + +* Description: +* Convert and interval in days into hours, minutes, seconds. + +* Notes: +* - Uses eraD2tf(). See SOFA/ERFA documentation for details. + +*- +*/ + +void palDd2tf ( int ndp, double days, char *sign, int ihmsf[4] ) { + eraD2tf( ndp, days, sign, ihmsf ); +} + +/* +*+ +* Name: +* palDimxv + +* Purpose: +* Perform the 3-D backward unitary transformation + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* palDimxv( double dm[3][3], double va[3], double vb[3] ); + +* Arguments: +* dm = double [3][3] (Given) +* Matrix +* va = double [3] (Given) +* vector +* vb = double [3] (Returned) +* Result vector + +* Description: +* Perform the 3-D backward unitary transformation. + +* Notes: +* - Uses eraTrxp(). See SOFA/ERFA documentation for details. + +*- +*/ + +void palDimxv ( double dm[3][3], double va[3], double vb[3] ) { + eraTrxp( dm, va, vb ); +} + +/* +*+ +* Name: +* palDm2av + +* Purpose: +* From a rotation matrix, determine the corresponding axial vector + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* palDm2av( double rmat[3][3], double axvec[3] ); + +* Arguments: +* rmat = double [3][3] (Given) +* Rotation matrix +* axvec = double [3] (Returned) +* Axial vector (radians) + +* Description: +* A rotation matrix describes a rotation about some arbitrary axis, +* called the Euler axis. The "axial vector" returned by this routine +* has the same direction as the Euler axis, and its magnitude is the +* amount of rotation in radians. (The magnitude and direction can be +* separated by means of the routine palDvn.) + +* Notes: +* - Uses eraRm2v(). See SOFA/ERFA documentation for details. + +*- +*/ + +void palDm2av ( double rmat[3][3], double axvec[3] ) { + eraRm2v( rmat, axvec ); +} + +/* +*+ +* Name: +* palDjcl + +* Purpose: +* Modified Julian Date to Gregorian year, month, day and fraction of day + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* palDjcl( double djm, int *iy, int *im, int *id, double *fd, int *j ); + +* Arguments: +* djm = double (Given) +* modified Julian Date (JD-2400000.5) +* iy = int * (Returned) +* year +* im = int * (Returned) +* month +* id = int * (Returned) +* day +* fd = double * (Returned) +* Fraction of day. + +* Description: +* Modified Julian Date to Gregorian year, month, day and fraction of day. + +* Notes: +* - Uses eraJd2cal(). See SOFA/ERFA documentation for details. + +*- +*/ + +/* 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 ); +} + +/* +*+ +* Name: +* palDmxm + +* Purpose: +* Product of two 3x3 matrices + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* palDmxm( double a[3][3], double b[3][3], double c[3][3] ); + +* Arguments: +* a = double [3][3] (Given) +* Matrix +* b = double [3][3] (Given) +* Matrix +* c = double [3][3] (Returned) +* Matrix result + +* Description: +* Product of two 3x3 matrices. + +* Notes: +* - Uses eraRxr(). See SOFA/ERFA documentation for details. + +*- +*/ + +void palDmxm ( double a[3][3], double b[3][3], double c[3][3] ) { + eraRxr( a, b, c ); +} + +/* +*+ +* Name: +* palDmxv + +* Purpose: +* Performs the 3-D forward unitary transformation + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* palDmxv( double dm[3][3], double va[3], double vb[3] ); + +* Arguments: +* dm = double [3][3] (Given) +* matrix +* va = double [3] (Given) +* vector +* dp = double [3] (Returned) +* result vector + +* Description: +* Performs the 3-D forward unitary transformation. + +* Notes: +* - Uses eraRxp(). See SOFA/ERFA documentation for details. + +*- +*/ + +void palDmxv ( double dm[3][3], double va[3], double vb[3] ) { + eraRxp( dm, va, vb ); +} + +/* +*+ +* Name: +* palDpav + +* Purpose: +* Position angle of one celestial direction with respect to another + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* pa = palDpav( double v1[3], double v2[3] ); + +* Arguments: +* v1 = double [3] (Given) +* direction cosines of one point. +* v2 = double [3] (Given) +* direction cosines of the other point. + +* Returned Value: +* The result is the bearing (position angle), in radians, of point +* V2 with respect to point V1. It is in the range +/- pi. The +* sense is such that if V2 is a small distance east of V1, the +* bearing is about +pi/2. Zero is returned if the two points +* are coincident. + +* Description: +* Position angle of one celestial direction with respect to another. + +* Notes: +* - The coordinate frames correspond to RA,Dec, Long,Lat etc. +* - Uses eraPap(). See SOFA/ERFA documentation for details. + +*- +*/ + +double palDpav ( double v1[3], double v2[3] ) { + return eraPap( v1, v2 ); +} + +/* +*+ +* Name: +* palDr2af + +* Purpose: +* Convert an angle in radians to degrees, arcminutes, arcseconds + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* palDr2af( int ndp, double angle, char *sign, int idmsf[4] ); + +* Arguments: +* ndp = int (Given) +* number of decimal places of arcseconds +* angle = double (Given) +* angle in radians +* sign = char * (Returned) +* '+' or '-' (single character) +* idmsf = int [4] (Returned) +* Degrees, arcminutes, arcseconds, fraction + +* Description: +* Convert an angle in radians to degrees, arcminutes, arcseconds. + +* Notes: +* - Uses eraA2af(). See SOFA/ERFA documentation for details. + +*- +*/ + +void palDr2af ( int ndp, double angle, char *sign, int idmsf[4] ) { + eraA2af( ndp, angle, sign, idmsf ); +} + +/* +*+ +* Name: +* palDr2tf + +* Purpose: +* Convert an angle in radians to hours, minutes, seconds + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* palDr2tf ( int ndp, double angle, char *sign, int ihmsf[4] ); + +* Arguments: +* ndp = int (Given) +* number of decimal places of arcseconds +* angle = double (Given) +* angle in radians +* sign = char * (Returned) +* '+' or '-' (single character) +* idmsf = int [4] (Returned) +* Hours, minutes, seconds, fraction + +* Description: +* Convert an angle in radians to hours, minutes, seconds. + +* Notes: +* - Uses eraA2tf(). See SOFA/ERFA documentation for details. + +*- +*/ + +void palDr2tf( int ndp, double angle, char *sign, int ihmsf[4] ) { + eraA2tf( ndp, angle, sign, ihmsf ); +} + +/* +*+ +* Name: +* palDranrm + +* Purpose: +* Normalize angle into range 0-2 pi + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* norm = palDranrm( double angle ); + +* Arguments: +* angle = double (Given) +* angle in radians + +* Returned Value: +* Angle expressed in the range 0-2 pi + +* Description: +* Normalize angle into range 0-2 pi. + +* Notes: +* - Uses eraAnp(). See SOFA/ERFA documentation for details. + +*- +*/ + +double palDranrm ( double angle ) { + return eraAnp( angle ); +} + +/* +*+ +* Name: +* palDsep + +* Purpose: +* Angle between two points on a sphere + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* ang = palDsep( double a1, double b1, double a2, double b2 ); + +* Arguments: +* a1 = double (Given) +* Spherical coordinate of one point (radians) +* b1 = double (Given) +* Spherical coordinate of one point (radians) +* a2 = double (Given) +* Spherical coordinate of other point (radians) +* b2 = double (Given) +* Spherical coordinate of other point (radians) + +* Returned Value: +* Angle, in radians, between the two points. Always positive. + +* Description: +* Angle between two points on a sphere. + +* Notes: +* - The spherical coordinates are [RA,Dec], [Long,Lat] etc, in radians. +* - Uses eraSeps(). See SOFA/ERFA documentation for details. + +*- +*/ + +double palDsep ( double a1, double b1, double a2, double b2 ) { + return eraSeps( a1, b1, a2, b2 ); +} + +/* +*+ +* Name: +* palDsepv + +* Purpose: +* Angle between two vectors + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* ang = palDsepv( double v1[3], double v2[3] ); + +* Arguments: +* v1 = double [3] (Given) +* First vector +* v2 = double [3] (Given) +* Second vector + +* Returned Value: +* Angle, in radians, between the two points. Always positive. + +* Description: +* Angle between two vectors. + +* Notes: +* - Uses eraSepp(). See SOFA/ERFA documentation for details. + +*- +*/ + +double palDsepv ( double v1[3], double v2[3] ) { + return eraSepp( v1, v2 ); +} + +/* +*+ +* Name: +* palDtf2d + +* Purpose: +* Convert hours, minutes, seconds to days + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* palDtf2d( int ihour, int imin, double sec, double *days, int *j ); + +* Arguments: +* ihour = int (Given) +* Hours +* imin = int (Given) +* Minutes +* sec = double (Given) +* Seconds +* days = double * (Returned) +* Interval in days +* j = int * (Returned) +* status: 0 = ok, 1 = ihour outside range 0-23, +* 2 = imin outside range 0-59, 3 = sec outside range 0-59.999... + +* Description: +* Convert hours, minutes, seconds to days. + +* Notes: +* - Uses eraTf2d(). See SOFA/ERFA documentation for details. + +*- +*/ + +/* 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 ); +} + +/* +*+ +* Name: +* palDtf2r + +* Purpose: +* Convert hours, minutes, seconds to radians + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* palDtf2r( int ihour, int imin, double sec, double *rad, int *j ); + +* Arguments: +* ihour = int (Given) +* Hours +* imin = int (Given) +* Minutes +* sec = double (Given) +* Seconds +* days = double * (Returned) +* Angle in radians +* j = int * (Returned) +* status: 0 = ok, 1 = ihour outside range 0-23, +* 2 = imin outside range 0-59, 3 = sec outside range 0-59.999... + +* Description: +* Convert hours, minutes, seconds to radians. + +* Notes: +* - Uses eraTf2a(). See SOFA/ERFA documentation for details. + +*- +*/ + +/* 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 ); +} + +/* +*+ +* Name: +* palDvdv + +* Purpose: +* Scalar product of two 3-vectors + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* prod = palDvdv ( double va[3], double vb[3] ); + +* Arguments: +* va = double [3] (Given) +* First vector +* vb = double [3] (Given) +* Second vector + +* Returned Value: +* Scalar product va.vb + +* Description: +* Scalar product of two 3-vectors. + +* Notes: +* - Uses eraPdp(). See SOFA/ERFA documentation for details. + +*- +*/ + +double palDvdv ( double va[3], double vb[3] ) { + return eraPdp( va, vb ); +} + +/* +*+ +* Name: +* palDvn + +* Purpose: +* Normalizes a 3-vector also giving the modulus + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* palDvn( double v[3], double uv[3], double *vm ); + +* Arguments: +* v = double [3] (Given) +* vector +* uv = double [3] (Returned) +* unit vector in direction of "v" +* vm = double * (Returned) +* modulus of "v" + +* Description: +* Normalizes a 3-vector also giving the modulus. + +* Notes: +* - Uses eraPn(). See SOFA/ERFA documentation for details. + +*- +*/ + +/* Note that the arguments are flipped */ +void palDvn ( double v[3], double uv[3], double *vm ) { + eraPn( v, vm, uv ); +} + +/* +*+ +* Name: +* palDvxv + +* Purpose: +* Vector product of two 3-vectors + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* palDvxv( double va[3], double vb[3], double vc[3] ); + +* Arguments: +* va = double [3] (Given) +* First vector +* vb = double [3] (Given) +* Second vector +* vc = double [3] (Returned) +* Result vector + +* Description: +* Vector product of two 3-vectors. + +* Notes: +* - Uses eraPxp(). See SOFA/ERFA documentation for details. + +*- +*/ + +void palDvxv ( double va[3], double vb[3], double vc[3] ) { + eraPxp( va, vb, vc ); +} + +/* +*+ +* Name: +* palEpb + +* Purpose: +* Conversion of modified Julian Data to Besselian Epoch + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* epb = palEpb ( double date ); + +* Arguments: +* date = double (Given) +* Modified Julian Date (JD - 2400000.5) + +* Returned Value: +* Besselian epoch. + +* Description: +* Conversion of modified Julian Data to Besselian Epoch. + +* Notes: +* - Uses eraEpb(). See SOFA/ERFA documentation for details. + +*- +*/ + +/* Requires additional SLA MJD reference date */ +double palEpb ( double date ) { + return eraEpb( PAL__MJD0, date ); +} + +/* +*+ +* Name: +* palEpb2d + +* Purpose: +* Conversion of Besselian Epoch to Modified Julian Date + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* mjd = palEpb2d ( double epb ); + +* Arguments: +* epb = double (Given) +* Besselian Epoch + +* Returned Value: +* Modified Julian Date (JD - 2400000.5) + +* Description: +* Conversion of Besselian Epoch to Modified Julian Date. + +* Notes: +* - Uses eraEpb2jd(). See SOFA/ERFA documentation for details. + +*- +*/ + + +double palEpb2d ( double epb ) { + double djm0, djm; + eraEpb2jd( epb, &djm0, &djm ); + return djm; +} + +/* +*+ +* Name: +* palEpj + +* Purpose: +* Conversion of Modified Julian Date to Julian Epoch + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* epj = palEpj ( double date ); + +* Arguments: +* date = double (Given) +* Modified Julian Date (JD - 2400000.5) + +* Returned Value: +* The Julian Epoch. + +* Description: +* Conversion of Modified Julian Date to Julian Epoch. + +* Notes: +* - Uses eraEpj(). See SOFA/ERFA documentation for details. + +*- +*/ + +/* Requires additional SLA MJD reference date */ +double palEpj ( double date ) { + return eraEpj( PAL__MJD0, date ); +} + +/* +*+ +* Name: +* palEpj2d + +* Purpose: +* Conversion of Julian Epoch to Modified Julian Date + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* mjd = palEpj2d ( double epj ); + +* Arguments: +* epj = double (Given) +* Julian Epoch. + +* Returned Value: +* Modified Julian Date (JD - 2400000.5) + +* Description: +* Conversion of Julian Epoch to Modified Julian Date. + +* Notes: +* - Uses eraEpj2d(). See SOFA/ERFA documentation for details. + +*- +*/ +double palEpj2d ( double epj ) { + double djm0, djm; + eraEpj2jd( epj, &djm0, &djm ); + return djm; +} + +/* +*+ +* Name: +* palEqeqx + +* Purpose: +* Equation of the equinoxes (IAU 2000/2006) + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* palEqeqx( double date ); + +* Arguments: +* date = double (Given) +* TT as Modified Julian Date (JD-400000.5) + +* Description: +* Equation of the equinoxes (IAU 2000/2006). + +* Notes: +* - Uses eraEe06a(). See SOFA/ERFA documentation for details. + +*- +*/ + +/* Requires additional SLA MJD reference date */ +double palEqeqx ( double date ) { + return eraEe06a( PAL__MJD0, date ); +} + +/* +*+ +* Name: +* palFk5hz + +* Purpose: +* Transform an FK5 (J2000) star position into the frame of the +* Hipparcos catalogue. + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* palFk5hz ( double r5, double d5, double epoch, +* double *rh, double *dh ); + +* Arguments: +* r5 = double (Given) +* FK5 RA (radians), equinox J2000, epoch "epoch" +* d5 = double (Given) +* FK5 dec (radians), equinox J2000, epoch "epoch" +* epoch = double (Given) +* Julian epoch +* rh = double * (Returned) +* RA (radians) +* dh = double * (Returned) +* Dec (radians) + +* Description: +* Transform an FK5 (J2000) star position into the frame of the +* Hipparcos catalogue. + +* Notes: +* - Assumes zero Hipparcos proper motion. +* - Uses eraEpj2jd() and eraFk5hz. +* See SOFA/ERFA documentation for details. + +*- +*/ + +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 ); +} + +/* +*+ +* Name: +* palGmst + +* Purpose: +* Greenwich mean sidereal time (consistent with IAU 2006 precession). + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* mst = palGmst ( double ut1 ); + +* Arguments: +* ut1 = double (Given) +* Universal time (UT1) expressed as modified Julian Date (JD-2400000.5) + +* Returned Value: +* Greenwich mean sidereal time + +* Description: +* Greenwich mean sidereal time (consistent with IAU 2006 precession). + +* Notes: +* - Uses eraGmst06(). See SOFA/ERFA documentation for details. + +*- +*/ + +/* Note that SOFA/ERFA has more accurate time arguments + and we use the 2006 precession model */ +double palGmst ( double ut1 ) { + return eraGmst06( PAL__MJD0, ut1, PAL__MJD0, ut1 ); +} + +/* +*+ +* Name: +* palGmsta + +* Purpose: +* Greenwich mean sidereal time (consistent with IAU 2006 precession). + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* mst = palGmsta ( double date, double ut1 ); + +* Arguments: +* date = double (Given) +* UT1 date (MJD: integer part of JD-2400000.5) +* ut1 = double (Given) +* UT1 time (fraction of a day) + +* Returned Value: +* Greenwich mean sidereal time (in range 0 to 2 pi) + +* Description: +* Greenwich mean sidereal time (consistent with IAU 2006 precession). + +* Notes: +* - For best accuracy use eraGmst06() directly. +* - Uses eraGmst06(). See SOFA/ERFA documentation for details. + +*- +*/ + +/* Slightly better but still not as accurate as SOFA/ERFA */ + +double palGmsta( double date, double ut ) { + date += PAL__MJD0; + return eraGmst06( date, ut, date, ut ); +} + +/* +*+ +* Name: +* palHfk5z + +* Purpose: +* Hipparcos star position to FK5 J2000 + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* palHfk5z( double rh, double dh, double epoch, +* double *r5, double *d5, double *dr5, double *dd5 ); + +* Arguments: +* rh = double (Given) +* Hipparcos RA (radians) +* dh = double (Given) +* Hipparcos Dec (radians) +* epoch = double (Given) +* Julian epoch (TDB) +* r5 = double * (Returned) +* RA (radians, FK5, equinox J2000, epoch "epoch") +* d5 = double * (Returned) +* Dec (radians, FK5, equinox J2000, epoch "epoch") + +* Description: +* Transform a Hipparcos star position into FK5 J2000, assuming +* zero Hipparcos proper motion. + +* Notes: +* - Uses eraEpj2jd and eraHfk5z(). See SOFA/ERFA documentation for details. + +*- +*/ + +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 ); +} + +/* +*+ +* Name: +* palRefcoq + +* Purpose: +* Determine the constants A and B in the atmospheric refraction model + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* palRefcoq( double tdk, double pmb, double rh, double wl, +* double *refa, double *refb ); + +* Arguments: +* 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). +* Radio refraction is chosen by specifying wl > 100 micrometres. +* 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. This is a fast alternative +* to the palRefco routine. +* +* 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. + +* Notes: +* - Uses eraRefco(). See SOFA/ERFA documentation for details. +* - Note that the SOFA/ERFA routine uses different order of +* of arguments and uses deg C rather than K. + +*- +*/ + +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/ERFA uses deg C */ + eraRefco( pmb, tdk - 273.15, rh, wl, refa, refb ); +} Index: trunk/FACT++/pal/palPa.c =================================================================== --- trunk/FACT++/pal/palPa.c (revision 18347) +++ trunk/FACT++/pal/palPa.c (revision 18347) @@ -0,0 +1,91 @@ +/* +*+ +* 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 ); +} Index: trunk/FACT++/pal/palPcd.c =================================================================== --- trunk/FACT++/pal/palPcd.c (revision 18347) +++ trunk/FACT++/pal/palPcd.c (revision 18347) @@ -0,0 +1,105 @@ +/* +*+ +* Name: +* palPcd + +* Purpose: +* Apply pincushion/barrel distortion to a tangent-plane [x,y] + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* palPcd( double disco, double * x, double * y ); + +* Arguments: +* disco = double (Given) +* Pincushion/barrel distortion coefficient. +* x = double * (Given & Returned) +* On input the tangent-plane X coordinate, on output +* the distorted X coordinate. +* y = double * (Given & Returned) +* On input the tangent-plane Y coordinate, on output +* the distorted Y coordinate. + +* Description: +* Applies pincushion and barrel distortion to a tangent +* plane coordinate. + +* Authors: +* PTW: Pat Wallace (RAL) +* TIMJ: Tim Jenness +* {enter_new_authors_here} + +* Notes: +* - The distortion is of the form RP = R*(1 + C*R**2), where R is +* the radial distance from the tangent point, C is the DISCO +* argument, and RP is the radial distance in the presence of +* the distortion. +* +* - For pincushion distortion, C is +ve; for barrel distortion, +* C is -ve. +* +* - For X,Y in units of one projection radius (in the case of +* a photographic plate, the focal length), the following +* DISCO values apply: +* +* Geometry DISCO +* +* astrograph 0.0 +* Schmidt -0.3333 +* AAT PF doublet +147.069 +* AAT PF triplet +178.585 +* AAT f/8 +21.20 +* JKT f/8 +13.32 +* +* See Also: +* - There is a companion routine, palUnpcd, which performs the +* inverse operation. + +* History: +* 2000-09-03 (PTW): +* SLALIB implementation. +* 2015-01-01 (TIMJ): +* Initial version. Ported from Fortran. +* {enter_further_changes_here} + +* Copyright: +* Copyright (C) 2000 Rutherford Appleton Laboratory. +* Copyright (C) 2015 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 (see SLA_CONDITIONS); 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 palPcd( double disco, double *x, double *y ) { + double f; + + f = 1.0 + disco * ( (*x) * (*x) + (*y) * (*y) ); + *x *= f; + *y *= f; +} + Index: trunk/FACT++/pal/palPertel.c =================================================================== --- trunk/FACT++/pal/palPertel.c (revision 18347) +++ trunk/FACT++/pal/palPertel.c (revision 18347) @@ -0,0 +1,212 @@ +/* +*+ +* 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 palPertue 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; +} Index: trunk/FACT++/pal/palPertue.c =================================================================== --- trunk/FACT++/pal/palPertue.c (revision 18347) +++ trunk/FACT++/pal/palPertue.c (revision 18347) @@ -0,0 +1,655 @@ +/* +*+ +* 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; +} Index: trunk/FACT++/pal/palPlanel.c =================================================================== --- trunk/FACT++/pal/palPlanel.c (revision 18347) +++ trunk/FACT++/pal/palPlanel.c (revision 18347) @@ -0,0 +1,220 @@ +/* +*+ +* 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 palPertel 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; + +} Index: trunk/FACT++/pal/palPlanet.c =================================================================== --- trunk/FACT++/pal/palPlanet.c (revision 18347) +++ trunk/FACT++/pal/palPlanet.c (revision 18347) @@ -0,0 +1,99 @@ +/* +*+ +* 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/ERFA 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; + +} Index: trunk/FACT++/pal/palPlante.c =================================================================== --- trunk/FACT++/pal/palPlante.c (revision 18347) +++ trunk/FACT++/pal/palPlante.c (revision 18347) @@ -0,0 +1,286 @@ +/* +*+ +* 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 palPertel 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 PAL/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 ); + +} + + + Index: trunk/FACT++/pal/palPlantu.c =================================================================== --- trunk/FACT++/pal/palPlantu.c (revision 18347) +++ trunk/FACT++/pal/palPlantu.c (revision 18347) @@ -0,0 +1,189 @@ +/* +*+ +* 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; +} + Index: trunk/FACT++/pal/palPm.c =================================================================== --- trunk/FACT++/pal/palPm.c (revision 18347) +++ trunk/FACT++/pal/palPm.c (revision 18347) @@ -0,0 +1,108 @@ +/* +*+ +* 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/ERFA 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/ERFA 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 ); + +} Index: trunk/FACT++/pal/palPolmo.c =================================================================== --- trunk/FACT++/pal/palPolmo.c (revision 18347) +++ trunk/FACT++/pal/palPolmo.c (revision 18347) @@ -0,0 +1,190 @@ +/* +*+ +* Name: +* palPolmo + +* Purpose: +* Correct for polar motion + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* palPolmo ( double elongm, double phim, double xp, double yp, +* double *elong, double *phi, double *daz ); + +* Arguments: +* elongm = double (Given) +* Mean logitude of the observer (radians, east +ve) +* phim = double (Given) +* Mean geodetic latitude of the observer (radians) +* xp = double (Given) +* Polar motion x-coordinate (radians) +* yp = double (Given) +* Polar motion y-coordinate (radians) +* elong = double * (Returned) +* True longitude of the observer (radians, east +ve) +* phi = double * (Returned) +* True geodetic latitude of the observer (radians) +* daz = double * (Returned) +* Azimuth correction (terrestrial-celestial, radians) + +* Description: +* Polar motion: correct site longitude and latitude for polar +* motion and calculate azimuth difference between celestial and +* terrestrial poles. + +* Authors: +* PTW: Patrick Wallace (STFC) +* TIMJ: Tim Jenness (Cornell) +* {enter_new_authors_here} + +* Notes: +* - "Mean" longitude and latitude are the (fixed) values for the +* site's location with respect to the IERS terrestrial reference +* frame; the latitude is geodetic. TAKE CARE WITH THE LONGITUDE +* SIGN CONVENTION. The longitudes used by the present routine +* are east-positive, in accordance with geographical convention +* (and right-handed). In particular, note that the longitudes +* returned by the sla_OBS routine are west-positive, following +* astronomical usage, and must be reversed in sign before use in +* the present routine. +* +* - XP and YP are the (changing) coordinates of the Celestial +* Ephemeris Pole with respect to the IERS Reference Pole. +* XP is positive along the meridian at longitude 0 degrees, +* and YP is positive along the meridian at longitude +* 270 degrees (i.e. 90 degrees west). Values for XP,YP can +* be obtained from IERS circulars and equivalent publications; +* the maximum amplitude observed so far is about 0.3 arcseconds. +* +* - "True" longitude and latitude are the (moving) values for +* the site's location with respect to the celestial ephemeris +* pole and the meridian which corresponds to the Greenwich +* apparent sidereal time. The true longitude and latitude +* link the terrestrial coordinates with the standard celestial +* models (for precession, nutation, sidereal time etc). +* +* - The azimuths produced by sla_AOP and sla_AOPQK are with +* respect to due north as defined by the Celestial Ephemeris +* Pole, and can therefore be called "celestial azimuths". +* However, a telescope fixed to the Earth measures azimuth +* essentially with respect to due north as defined by the +* IERS Reference Pole, and can therefore be called "terrestrial +* azimuth". Uncorrected, this would manifest itself as a +* changing "azimuth zero-point error". The value DAZ is the +* correction to be added to a celestial azimuth to produce +* a terrestrial azimuth. +* +* - The present routine is rigorous. For most practical +* purposes, the following simplified formulae provide an +* adequate approximation: +* +* elong = elongm+xp*cos(elongm)-yp*sin(elongm) +* phi = phim+(xp*sin(elongm)+yp*cos(elongm))*tan(phim) +* daz = -sqrt(xp*xp+yp*yp)*cos(elongm-atan2(xp,yp))/cos(phim) +* +* An alternative formulation for DAZ is: +* +* x = cos(elongm)*cos(phim) +* y = sin(elongm)*cos(phim) +* daz = atan2(-x*yp-y*xp,x*x+y*y) +* +* - Reference: Seidelmann, P.K. (ed), 1992. "Explanatory Supplement +* to the Astronomical Almanac", ISBN 0-935702-68-7, +* sections 3.27, 4.25, 4.52. + +* History: +* 2000-11-30 (PTW): +* SLALIB implementation. +* 2014-10-18 (TIMJ): +* Initial version in C. +* {enter_further_changes_here} + +* Copyright: +* Copyright (C) 2000 Rutherford Appleton Laboratory. +* 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, see . + +* Bugs: +* {note_any_bugs_here} +*- +*/ + +#include + +#include "pal.h" + +void palPolmo ( double elongm, double phim, double xp, double yp, + double *elong, double *phi, double *daz ) { + + double sel,cel,sph,cph,xm,ym,zm,xnm,ynm,znm, + sxp,cxp,syp,cyp,zw,xt,yt,zt,xnt,ynt; + + /* Site mean longitude and mean geodetic latitude as a Cartesian vector */ + sel=sin(elongm); + cel=cos(elongm); + sph=sin(phim); + cph=cos(phim); + + xm=cel*cph; + ym=sel*cph; + zm=sph; + + /* Rotate site vector by polar motion, Y-component then X-component */ + sxp=sin(xp); + cxp=cos(xp); + syp=sin(yp); + cyp=cos(yp); + + zw=(-ym*syp+zm*cyp); + + xt=xm*cxp-zw*sxp; + yt=ym*cyp+zm*syp; + zt=xm*sxp+zw*cxp; + + /* Rotate also the geocentric direction of the terrestrial pole (0,0,1) */ + xnm=-sxp*cyp; + ynm=syp; + znm=cxp*cyp; + + cph=sqrt(xt*xt+yt*yt); + if (cph == 0.0) xt=1.0; + sel=yt/cph; + cel=xt/cph; + + /* Return true longitude and true geodetic latitude of site */ + if (xt != 0.0 || yt != 0.0) { + *elong=atan2(yt,xt); + } else { + *elong=0.0; + } + *phi=atan2(zt,cph); + + /* Return current azimuth of terrestrial pole seen from site position */ + xnt=(xnm*cel+ynm*sel)*zt-znm*cph; + ynt=-xnm*sel+ynm*cel; + if (xnt != 0.0 || ynt != 0.0) { + *daz=atan2(-ynt,-xnt); + } else { + *daz=0.0; + } + +} Index: trunk/FACT++/pal/palPrebn.c =================================================================== --- trunk/FACT++/pal/palPrebn.c (revision 18347) +++ trunk/FACT++/pal/palPrebn.c (revision 18347) @@ -0,0 +1,98 @@ +/* +*+ +* 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); + +} Index: trunk/FACT++/pal/palPrec.c =================================================================== --- trunk/FACT++/pal/palPrec.c (revision 18347) +++ trunk/FACT++/pal/palPrec.c (revision 18347) @@ -0,0 +1,107 @@ +/* +*+ +* 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 ); + } + +} Index: trunk/FACT++/pal/palPreces.c =================================================================== --- trunk/FACT++/pal/palPreces.c (revision 18347) +++ trunk/FACT++/pal/palPreces.c (revision 18347) @@ -0,0 +1,118 @@ +/* +*+ +* 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 ); +} Index: trunk/FACT++/pal/palPrenut.c =================================================================== --- trunk/FACT++/pal/palPrenut.c (revision 18347) +++ trunk/FACT++/pal/palPrenut.c (revision 18347) @@ -0,0 +1,111 @@ +/* +*+ +* 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 ); +} Index: trunk/FACT++/pal/palPv2el.c =================================================================== --- trunk/FACT++/pal/palPv2el.c (revision 18347) +++ trunk/FACT++/pal/palPv2el.c (revision 18347) @@ -0,0 +1,405 @@ +/* +*+ +* 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; + +} Index: trunk/FACT++/pal/palPv2ue.c =================================================================== --- trunk/FACT++/pal/palPv2ue.c (revision 18347) +++ trunk/FACT++/pal/palPv2ue.c (revision 18347) @@ -0,0 +1,182 @@ +/* +*+ +* 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; +} Index: trunk/FACT++/pal/palPvobs.c =================================================================== --- trunk/FACT++/pal/palPvobs.c (revision 18347) +++ trunk/FACT++/pal/palPvobs.c (revision 18347) @@ -0,0 +1,108 @@ +/* +*+ +* 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; + +} + + Index: trunk/FACT++/pal/palRdplan.c =================================================================== --- trunk/FACT++/pal/palRdplan.c (revision 18347) +++ trunk/FACT++/pal/palRdplan.c (revision 18347) @@ -0,0 +1,224 @@ +/* +*+ +* 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 ) ); + +} Index: trunk/FACT++/pal/palRefco.c =================================================================== --- trunk/FACT++/pal/palRefco.c (revision 18347) +++ trunk/FACT++/pal/palRefco.c (revision 18347) @@ -0,0 +1,120 @@ +/* +*+ +* 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; + +} Index: trunk/FACT++/pal/palRefro.c =================================================================== --- trunk/FACT++/pal/palRefro.c (revision 18347) +++ trunk/FACT++/pal/palRefro.c (revision 18347) @@ -0,0 +1,437 @@ +/* +*+ +* 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); + +} Index: trunk/FACT++/pal/palRefv.c =================================================================== --- trunk/FACT++/pal/palRefv.c (revision 18347) +++ trunk/FACT++/pal/palRefv.c (revision 18347) @@ -0,0 +1,155 @@ +/* +*+ +* 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 palRefco +* 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); +} Index: trunk/FACT++/pal/palRefz.c =================================================================== --- trunk/FACT++/pal/palRefz.c (revision 18347) +++ trunk/FACT++/pal/palRefz.c (revision 18347) @@ -0,0 +1,191 @@ +/* +*+ +* 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; + +} Index: trunk/FACT++/pal/palRverot.c =================================================================== --- trunk/FACT++/pal/palRverot.c (revision 18347) +++ trunk/FACT++/pal/palRverot.c (revision 18347) @@ -0,0 +1,91 @@ +/* +*+ +* 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) +* 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); +} Index: trunk/FACT++/pal/palRvgalc.c =================================================================== --- trunk/FACT++/pal/palRvgalc.c (revision 18347) +++ trunk/FACT++/pal/palRvgalc.c (revision 18347) @@ -0,0 +1,111 @@ +/* +*+ +* 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 ); +} Index: trunk/FACT++/pal/palRvlg.c =================================================================== --- trunk/FACT++/pal/palRvlg.c (revision 18347) +++ trunk/FACT++/pal/palRvlg.c (revision 18347) @@ -0,0 +1,106 @@ +/* +*+ +* 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 ); +} Index: trunk/FACT++/pal/palRvlsrd.c =================================================================== --- trunk/FACT++/pal/palRvlsrd.c (revision 18347) +++ trunk/FACT++/pal/palRvlsrd.c (revision 18347) @@ -0,0 +1,116 @@ +/* +*+ +* 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 palRvlsrk. + +* 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 ); +} Index: trunk/FACT++/pal/palRvlsrk.c =================================================================== --- trunk/FACT++/pal/palRvlsrk.c (revision 18347) +++ trunk/FACT++/pal/palRvlsrk.c (revision 18347) @@ -0,0 +1,116 @@ +/* +*+ +* 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 palRvlsrd. + +* 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 ); +} Index: trunk/FACT++/pal/palSubet.c =================================================================== --- trunk/FACT++/pal/palSubet.c (revision 18347) +++ trunk/FACT++/pal/palSubet.c (revision 18347) @@ -0,0 +1,112 @@ +/* +*+ +* 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 ); + +} Index: trunk/FACT++/pal/palSupgal.c =================================================================== --- trunk/FACT++/pal/palSupgal.c (revision 18347) +++ trunk/FACT++/pal/palSupgal.c (revision 18347) @@ -0,0 +1,116 @@ +/* +*+ +* 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 ); + +} Index: trunk/FACT++/pal/palTest.c =================================================================== --- trunk/FACT++/pal/palTest.c (revision 18347) +++ trunk/FACT++/pal/palTest.c (revision 18347) @@ -0,0 +1,2057 @@ +/* +*+ +* 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/ERFA 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 ); +} + +/* Altaz */ + +static void t_altaz( int *status ) { + double az, azd, azdd, el, eld, eldd, pa, pad, padd; + palAltaz( 0.7, -0.7, -0.65, + &az, &azd, &azdd, &el, &eld, &eldd, &pa, &pad, &padd ); + + vvd ( az, 4.400560746660174, 1e-12, "palAltaz", + "AZ", status ); + vvd ( azd, -0.2015438937145421, 1e-13, "palAltaz", + "AZD", status ); + vvd ( azdd, -0.4381266949668748, 1e-13, "palAltaz", + "AZDD", status ); + vvd ( el, 1.026646506651396, 1e-12, "palAltaz", + "EL", status ); + vvd ( eld, -0.7576920683826450, 1e-13, "palAltaz", + "ELD", status ); + vvd ( eldd, 0.04922465406857453, 1e-14, "palAltaz", + "ELDD", status ); + vvd ( pa, 1.707639969653937, 1e-12, "palAltaz", + "PA", status ); + vvd ( pad, 0.4717832355365627, 1e-13, "palAltaz", + "PAD", status ); + vvd ( padd, -0.2957914128185515, 1e-13, "palAltaz", + "PADD", 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/ERFA 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/ERFA */ + 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/ERFA 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/ERFA 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_ecleq( int *status ) { + double dr; + double dd; + palEcleq( 1.234, -0.123, 43210.0, &dr, &dd ); + vvd( dr, 1.229910118208851, 1e-5, "palEcleq", + "RA", status ); + vvd( dd, 0.2638461400411088, 1e-5, "palEcleq", + "Dec", 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/ERFA. 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_fk524( int *status ) { + double r1950, d1950, dr1950, dd1950, p1950, v1950; + palFk524(4.567, -1.23, -3e-5, 8e-6, 0.29, + -35.0, &r1950, &d1950, &dr1950, &dd1950, &p1950, &v1950); + vvd(r1950, 4.543778603272084, 1e-12, "palFk524", "r", status); + vvd(d1950, -1.229642790187574, 1e-12, "palFk524", "d", status); + vvd(dr1950, -2.957873121769244e-5, 1e-17, "palFk524", "dr", status); + vvd(dd1950, 8.117725309659079e-6, 1e-17, "palFk524", "dd", status); + vvd(p1950, 0.2898494999992917, 1e-12, "palFk524", "p", status); + vvd(v1950, -35.026862824252680, 1e-11, "palFk524", "v", 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_pcd( int *status ) { + double disco, x, y; + disco = 178.585; + x = 0.0123; + y = -0.00987; + + palPcd ( disco, &x, &y ); + vvd ( x, 0.01284630845735895, 1e-14, "palPcd", "x", status ); + vvd ( y, -0.01030837922553926, 1e-14, "palPcd", "y", status ); + + palUnpcd ( disco, &x, &y ); + vvd ( x, 0.0123, 1e-14, "palUnpcd", "x", status ); + vvd ( y, -0.00987, 1e-14, "palUnpcd", "y,", status ); + + /* Now negative disco round trip */ + disco = -0.3333333; + x = 0.0123; + y = -0.00987; + palPcd ( disco, &x, &y ); + palUnpcd ( disco, &x, &y ); + vvd ( x, 0.0123, 1e-14, "palUnpcd", "x", status ); + vvd ( y, -0.00987, 1e-14, "palUnpcd", "y,", 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., + 0. + }; + 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/ERFA 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_polmo( int *status ) { + double elong, phi, daz; + + palPolmo( 0.7, -0.5, 1.0e-6, -2.0e-6, &elong, &phi, &daz ); + vvd(elong, 0.7000004837322044, 1.0e-12, "palPolmo", "elong", status ); + vvd(phi, -0.4999979467222241, 1.0e-12, "palPolmo", "phi", status ); + vvd(daz, 1.008982781275728e-6, 1.0e-12, "palPolmo", "daz", 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 ); + + + +} + +static void t_vers( int *status ) { + char verstring[32]; + + int ver = palVers( verstring, sizeof(verstring)); + printf("PAL Version %s (%d)\n", verstring, ver); + if ( ver < 6000 ) { + *status = 1; /* palVers introduced at v0.6.0 */ + } +} + +/**********************************************************************/ + +int main (void) { + + /* Use the SLA and SOFA/ERFA conventions */ + int status = 0; /* Unix and SAE convention */ + + t_addet(&status); + t_afin(&status); + t_altaz(&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_fk524(&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_ecleq(&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_pcd(&status); + t_planet(&status); + t_pm(&status); + t_polmo(&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); + t_vers(&status); + return status; +} + Index: trunk/FACT++/pal/palUe2el.c =================================================================== --- trunk/FACT++/pal/palUe2el.c (revision 18347) +++ trunk/FACT++/pal/palUe2el.c (revision 18347) @@ -0,0 +1,234 @@ +/* +*+ +* 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 ); +} Index: trunk/FACT++/pal/palUe2pv.c =================================================================== --- trunk/FACT++/pal/palUe2pv.c (revision 18347) +++ trunk/FACT++/pal/palUe2pv.c (revision 18347) @@ -0,0 +1,263 @@ +/* +*+ +* 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 +* pv = double [6] (Returned) +* Position (AU) and velocity (AU/s) +* 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 +* palPlanel. 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; +} Index: trunk/FACT++/pal/palUnpcd.c =================================================================== --- trunk/FACT++/pal/palUnpcd.c (revision 18347) +++ trunk/FACT++/pal/palUnpcd.c (revision 18347) @@ -0,0 +1,176 @@ +/* +*+ +* Name: +* palUnpcd + +* Purpose: +* Remove pincushion/barrel distortion + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* palUnpcd( double disco, double * x, double * y ); + +* Arguments: +* disco = double (Given) +* Pincushion/barrel distortion coefficient. +* x = double * (Given & Returned) +* On input the distorted X coordinate, on output +* the tangent-plane X coordinate. +* y = double * (Given & Returned) +* On input the distorted Y coordinate, on output +* the tangent-plane Y coordinate. + +* Description: +* Remove pincushion/barrel distortion from a distorted [x,y] to give +* tangent-plane [x,y]. + +* Authors: +* PTW: Pat Wallace (RAL) +* TIMJ: Tim Jenness +* {enter_new_authors_here} + +* Notes: +* - The distortion is of the form RP = R*(1+C*R^2), where R is +* the radial distance from the tangent point, C is the DISCO +* argument, and RP is the radial distance in the presence of +* the distortion. +* +* - For pincushion distortion, C is +ve; for barrel distortion, +* C is -ve. +* +* - For X,Y in "radians" - units of one projection radius, +* which in the case of a photograph is the focal length of +* the camera - the following DISCO values apply: +* +* Geometry DISCO +* +* astrograph 0.0 +* Schmidt -0.3333 +* AAT PF doublet +147.069 +* AAT PF triplet +178.585 +* AAT f/8 +21.20 +* JKT f/8 +13.32 +* +* - The present routine is a rigorous inverse of the companion +* routine palPcd. The expression for RP in Note 1 is rewritten +* in the form x^3+a*x+b=0 and solved by standard techniques. +* +* - Cases where the cubic has multiple real roots can sometimes +* occur, corresponding to extreme instances of barrel distortion +* where up to three different undistorted [X,Y]s all produce the +* same distorted [X,Y]. However, only one solution is returned, +* the one that produces the smallest change in [X,Y]. + +* See Also: +* palPcd + +* History: +* 2000-09-03 (PTW): +* SLALIB implementation. +* 2015-01-01 (TIMJ): +* Initial version +* {enter_further_changes_here} + +* Copyright: +* Copyright (C) 2000 Rutherford Appleton Laboratory. +* Copyright (C) 2015 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, see . + +* Bugs: +* {note_any_bugs_here} +*- +*/ + +#if HAVE_CONFIG_H +#include +#endif + +#include + +#include "pal.h" +#include "palmac.h" + +/* copysign is C99 */ +#if HAVE_COPYSIGN +# define COPYSIGN copysign +#else +# define COPYSIGN(a,b) DSIGN(a,b) +#endif + +void palUnpcd( double disco, double * x, double *y ) { + + const double THIRD = 1.0/3.0; + + double rp,q,r,d,w,s,t,f,c,t3,f1,f2,f3,w1,w2,w3; + double c2; + + /* Distance of the point from the origin. */ + rp = sqrt( (*x)*(*x)+(*y)*(*y)); + + /* If zero, or if no distortion, no action is necessary. */ + if (rp != 0.0 && disco != 0.0) { + + /* Begin algebraic solution. */ + q = 1.0/(3.0*disco); + r = rp/(2.0*disco); + w = q*q*q+r*r; + + /* Continue if one real root, or three of which only one is positive. */ + if (w > 0.0) { + + d = sqrt(w); + w = r+d; + s = COPYSIGN(pow(fabs(w),THIRD),w); + w = r-d; + t = COPYSIGN(pow(fabs(w),THIRD),w); + f = s+t; + + } else { + /* Three different real roots: use geometrical method instead. */ + w = 2.0/sqrt(-3.0*disco); + c = 4.0*rp/(disco*w*w*w); + c2 = c*c; + s = sqrt(1.0-DMIN(c2,1.0)); + t3 = atan2(s,c); + + /* The three solutions. */ + f1 = w*cos((PAL__D2PI-t3)/3.0); + f2 = w*cos((t3)/3.0); + f3 = w*cos((PAL__D2PI+t3)/3.0); + + /* Pick the one that moves [X,Y] least. */ + w1 = fabs(f1-rp); + w2 = fabs(f2-rp); + w3 = fabs(f3-rp); + if (w1 < w2) { + f = ( w1 < w3 ? f1 : f3 ); + } else { + f = ( w2 < w3 ? f2 : f3 ); + } + } + + /* Remove the distortion. */ + f = f/rp; + *x *= f; + *y *= f; + } +} Index: trunk/FACT++/pal/palVers.c =================================================================== --- trunk/FACT++/pal/palVers.c (revision 18347) +++ trunk/FACT++/pal/palVers.c (revision 18347) @@ -0,0 +1,92 @@ +/* +*+ +* Name: +* palVers + +* Purpose: +* Obtain PAL version number + +* Language: +* Starlink ANSI C + +* Type of Module: +* Library routine + +* Invocation: +* int palVers( char *verstring, size_t verlen ); + +* Arguments: +* verstring = char * (Returned) +* Buffer to receive version string of the form "A.B.C". Can be NULL. +* verlen = size_t (Given) +* Allocated size of "verstring" including nul. Version string +* will be truncated if it does not fit in buffer. + +* Returned Value: +* vernum = int (Returned) +* Version number as an integer. + +* Description: +* Retrieve the PAL version number as a string in the form "A.B.C" +* and as an integer (major*1e6+minor*1e3+release). + +* Authors: +* TIMJ: Tim Jenness (Cornell) +* {enter_new_authors_here} + +* Notes: +* - Note that this API does not match the slaVers API. + +* History: +* 2014-08-27 (TIMJ): +* Initial version +* {enter_further_changes_here} + +* Copyright: +* 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, see . + +* Bugs: +* {note_any_bugs_here} +*- +*/ + +#if HAVE_CONFIG_H +# include +#endif + +#ifdef HAVE_BSD_STRING_H +#include +#endif + +#include + +/* This version is just a straight copy without putting ellipsis on the end. */ +static void my__strlcpy( 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 +} + +int +palVers( char *verstring, size_t verlen ) { + if (verstring) my__strlcpy( verstring, PACKAGE_VERSION, verlen ); + return PACKAGE_VERSION_INTEGER; +} Index: trunk/FACT++/pal/palmac.h =================================================================== --- trunk/FACT++/pal/palmac.h (revision 18347) +++ trunk/FACT++/pal/palmac.h (revision 18347) @@ -0,0 +1,136 @@ +#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 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} +*- +*/ + +/* 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; + +/* DINT(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 Index: trunk/FACT++/pal/sofa-porting-guide.txt =================================================================== --- trunk/FACT++/pal/sofa-porting-guide.txt (revision 18347) +++ trunk/FACT++/pal/sofa-porting-guide.txt (revision 18347) @@ -0,0 +1,42 @@ +Some SLA routines migrate directly to SOFA. Simple PAL wrappers are +made available using the SLA name but new code should use the SOFA +variant directly. The PAL routines should not be called internally +by other PAL routines. + +Daf2r => Af2a +Dav2m => Rv2m +Dcc2s => C2s +Dcs2c => S2c +Dd2tf => D2tf +Dimxv => Trxp +Djcl => Jd2cal +Dmxm => Rxr +Dmxv => Rxp +Dm2av => Rm2v +Dranrm => Anp +Drange => Anpm +Dsep => Seps +Dsepv => Sepp +Dtf2d => Tf2d +Dtf2r => Tf2a +Dvdv => Pdp +Dvn => Pn +Dvxv => Pxp +Epb => Epb +Epb2d => Epb2jd +Epj => Epj +Epj2d => Epj2jd +Eqeqx => Ee06a +Fk5hz => Fk5hz +Gmst => Gmst06 +Hfk5z => Hfk5z + + +Some SLA routines are close to the same but have different arguments +so a PAL routine is provided although it is probably best to port software +to the SOFA variant: + +slaDat =>palDat => iauDat + +slaGeoc has different arguments and uses the WGS84 model. The code is not +quite one-to-one. Index: trunk/FACT++/pal/sun267.tex =================================================================== --- trunk/FACT++/pal/sun267.tex (revision 18347) +++ trunk/FACT++/pal/sun267.tex (revision 18347) @@ -0,0 +1,8810 @@ +\documentclass[twoside,11pt,nolof]{starlink} + +% ? Specify used packages +% ? End of specify used packages + +% ----------------------------------------------------------------------------- +% ? Document identification +% Fixed part +\stardoccategory {Starlink User Note} +\stardocinitials {SUN} +\stardocsource {sun\stardocnumber} +\stardoccopyright{% +Copyright \copyright\ 2012 Science and Technology Facilities + Council.\\ Copyright \copyright\ 2014 Cornell University.\\ +Copyright \copyright\ 2015 Tim Jenness} + +% Variable part - replace [xxx] as appropriate. +\stardocnumber {267.3} +\stardocauthors {Tim Jenness} +\stardocdate {2015 January 1} +\stardoctitle {PAL --- Positional Astronomy Library} +\stardocversion {0.9.0} +\stardocmanual {Programmer's Manual} +\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/ERFA library. It is provided with a GPLv3 license. +} +% ? End of document identification +% ----------------------------------------------------------------------------- + +\begin{document} +\scfrontmatter + +% ? 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})\footnote{or equivalent ERFA routines.} +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{Astronomical Data Anaysis Software and Systems XXII}, Friedel, D. N. (ed), +ASP Conf.\ Ser. \textbf{475}, p307. + +\clearpage +\appendix +\section{\label{APP:SPEC}Function Descriptions} + +By default PAL is set up to use the ERFA variant of SOFA. ERFA is an +approved redistribution of the SOFA code using a BSD-license and +renamed function calls. Whereas SOFA routines have a \texttt{iau} prefix +the ERFA equivalents have a \texttt{era} prefix. The PAL build script +will try to detect which of ERFA and SOFA is available. Wherever SOFA +is mentioned in this document the ERFA equivalent can be substituted. + +ERFA can be obtained from \htmladdnormallink{https://github.com/liberfa/erfa}. + +\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{tabbing} +\hspace*{2cm}\=\hspace*{3cm}\= \kill +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}\\ +\texttt{palRefcoq} \> \texttt{iauRefco}\\ +\end{tabbing} + +\sstroutine{ + palCldj +}{ + Gregorian Calendar to Modified Julian Date +}{ + \sstdescription{ + Gregorian calendar to Modified Julian Date. + } + \sstinvocation{ + palCldj( int iy, int im, int id, double $*$djm, int $*$j ); + } + \sstarguments{ + \sstsubsection{ + iy = int (Given) + }{ + Year in Gregorian calendar + } + \sstsubsection{ + im = int (Given) + }{ + Month in Gregorian calendar + } + \sstsubsection{ + id = int (Given) + }{ + Day in Gregorian calendar + } + \sstsubsection{ + djm = double $*$ (Returned) + }{ + Modified Julian Date (JD-2400000.5) for 0 hrs + } + \sstsubsection{ + j = int $*$ (Returned) + }{ + status: 0 = OK, 1 = bad year (MJD not computed), + 2 = bad month (MJD not computed), 3 = bad day (MJD computed). + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraCal2jd(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palDbear +}{ + Bearing (position angle) of one point on a sphere relative to another +}{ + \sstdescription{ + Bearing (position angle) of one point in a sphere relative to another. + } + \sstinvocation{ + pa = palDbear( double a1, double b1, double a2, double b2 ); + } + \sstarguments{ + \sstsubsection{ + a1 = double (Given) + }{ + Longitude of point A (e.g. RA) in radians. + } + \sstsubsection{ + a2 = double (Given) + }{ + Latitude of point A (e.g. Dec) in radians. + } + \sstsubsection{ + b1 = double (Given) + }{ + Longitude of point B in radians. + } + \sstsubsection{ + b2 = double (Given) + }{ + Latitude of point B in radians. + } + } + \sstreturnedvalue{ + \sstsubsection{ + The result is the bearing (position angle), in radians, of point + }{ + } + \sstsubsection{ + A2,B2 as seen from point A1,B1. It is in the range $+$/- pi. If + }{ + } + \sstsubsection{ + A2,B2 is due east of A1,B1 the bearing is $+$pi/2. Zero is returned + }{ + } + \sstsubsection{ + if the two points are coincident. + }{ + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraPas(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palDaf2r +}{ + Convert degrees, arcminutes, arcseconds to radians +}{ + \sstdescription{ + Convert degrees, arcminutes, arcseconds to radians. + } + \sstinvocation{ + palDaf2r( int ideg, int iamin, double asec, double $*$rad, int $*$j ); + } + \sstarguments{ + \sstsubsection{ + ideg = int (Given) + }{ + Degrees. + } + \sstsubsection{ + iamin = int (Given) + }{ + Arcminutes. + } + \sstsubsection{ + iasec = double (Given) + }{ + Arcseconds. + } + \sstsubsection{ + rad = double $*$ (Returned) + }{ + Angle in radians. + } + \sstsubsection{ + j = int $*$ (Returned) + }{ + Status: 0 = OK, 1 = {\tt "}ideg{\tt "} out of range 0-359, + 2 = {\tt "}iamin{\tt "} outside of range 0-59, + 2 = {\tt "}asec{\tt "} outside range 0-59.99999 + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraAf2a(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palDav2m +}{ + Form the rotation matrix corresponding to a given axial vector +}{ + \sstdescription{ + A rotation matrix describes a rotation about some arbitrary axis, + called the Euler axis. The {\tt "}axial vector{\tt "} supplied to this routine + has the same direction as the Euler axis, and its magnitude is the + amount of rotation in radians. + } + \sstinvocation{ + palDav2m( double axvec[3], double rmat[3][3] ); + } + \sstarguments{ + \sstsubsection{ + axvec = double [3] (Given) + }{ + Axial vector (radians) + } + \sstsubsection{ + rmat = double [3][3] (Returned) + }{ + Rotation matrix. + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraRv2m(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palDcc2s +}{ + Cartesian to spherical coordinates +}{ + \sstdescription{ + The spherical coordinates are longitude ($+$ve anticlockwise looking + from the $+$ve latitude pole) and latitude. The Cartesian coordinates + are right handed, with the x axis at zero longitude and latitude, and + the z axis at the $+$ve latitude pole. + } + \sstinvocation{ + palDcc2s( double v[3], double $*$a, double $*$b ); + } + \sstarguments{ + \sstsubsection{ + v = double [3] (Given) + }{ + x, y, z vector. + } + \sstsubsection{ + a = double $*$ (Returned) + }{ + Spherical coordinate (radians) + } + \sstsubsection{ + b = double $*$ (Returned) + }{ + Spherical coordinate (radians) + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraC2s(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palDcs2c +}{ + Spherical coordinates to direction cosines +}{ + \sstdescription{ + The spherical coordinates are longitude ($+$ve anticlockwise looking + from the $+$ve latitude pole) and latitude. The Cartesian coordinates + are right handed, with the x axis at zero longitude and latitude, and + the z axis at the $+$ve latitude pole. + } + \sstinvocation{ + palDcs2c( double a, double b, double v[3] ); + } + \sstarguments{ + \sstsubsection{ + a = double (Given) + }{ + Spherical coordinate in radians (ra, long etc). + } + \sstsubsection{ + b = double (Given) + }{ + Spherical coordinate in radians (dec, lat etc). + } + \sstsubsection{ + v = double [3] (Returned) + }{ + x, y, z vector + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraS2c(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palDd2tf +}{ + Convert an interval in days into hours, minutes, seconds +}{ + \sstdescription{ + Convert and interval in days into hours, minutes, seconds. + } + \sstinvocation{ + palDd2tf( int ndp, double days, char $*$sign, int ihmsf[4] ); + } + \sstarguments{ + \sstsubsection{ + ndp = int (Given) + }{ + Number of decimal places of seconds + } + \sstsubsection{ + days = double (Given) + }{ + Interval in days + } + \sstsubsection{ + sign = char $*$ (Returned) + }{ + {\tt '}$+${\tt '} or {\tt '}-{\tt '} (single character, not string) + } + \sstsubsection{ + ihmsf = int [4] (Returned) + }{ + Hours, minutes, seconds, fraction + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraD2tf(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palDimxv +}{ + Perform the 3-D backward unitary transformation +}{ + \sstdescription{ + Perform the 3-D backward unitary transformation. + } + \sstinvocation{ + palDimxv( double dm[3][3], double va[3], double vb[3] ); + } + \sstarguments{ + \sstsubsection{ + dm = double [3][3] (Given) + }{ + Matrix + } + \sstsubsection{ + va = double [3] (Given) + }{ + vector + } + \sstsubsection{ + vb = double [3] (Returned) + }{ + Result vector + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraTrxp(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palDm2av +}{ + From a rotation matrix, determine the corresponding axial vector +}{ + \sstdescription{ + A rotation matrix describes a rotation about some arbitrary axis, + called the Euler axis. The {\tt "}axial vector{\tt "} returned by this routine + has the same direction as the Euler axis, and its magnitude is the + amount of rotation in radians. (The magnitude and direction can be + separated by means of the routine palDvn.) + } + \sstinvocation{ + palDm2av( double rmat[3][3], double axvec[3] ); + } + \sstarguments{ + \sstsubsection{ + rmat = double [3][3] (Given) + }{ + Rotation matrix + } + \sstsubsection{ + axvec = double [3] (Returned) + }{ + Axial vector (radians) + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraRm2v(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palDjcl +}{ + Modified Julian Date to Gregorian year, month, day and fraction of day +}{ + \sstdescription{ + Modified Julian Date to Gregorian year, month, day and fraction of day. + } + \sstinvocation{ + palDjcl( double djm, int $*$iy, int $*$im, int $*$id, double $*$fd, int $*$j ); + } + \sstarguments{ + \sstsubsection{ + djm = double (Given) + }{ + modified Julian Date (JD-2400000.5) + } + \sstsubsection{ + iy = int $*$ (Returned) + }{ + year + } + \sstsubsection{ + im = int $*$ (Returned) + }{ + month + } + \sstsubsection{ + id = int $*$ (Returned) + }{ + day + } + \sstsubsection{ + fd = double $*$ (Returned) + }{ + Fraction of day. + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraJd2cal(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palDmxm +}{ + Product of two 3x3 matrices +}{ + \sstdescription{ + Product of two 3x3 matrices. + } + \sstinvocation{ + palDmxm( double a[3][3], double b[3][3], double c[3][3] ); + } + \sstarguments{ + \sstsubsection{ + a = double [3][3] (Given) + }{ + Matrix + } + \sstsubsection{ + b = double [3][3] (Given) + }{ + Matrix + } + \sstsubsection{ + c = double [3][3] (Returned) + }{ + Matrix result + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraRxr(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palDmxv +}{ + Performs the 3-D forward unitary transformation +}{ + \sstdescription{ + Performs the 3-D forward unitary transformation. + } + \sstinvocation{ + palDmxv( double dm[3][3], double va[3], double vb[3] ); + } + \sstarguments{ + \sstsubsection{ + dm = double [3][3] (Given) + }{ + matrix + } + \sstsubsection{ + va = double [3] (Given) + }{ + vector + } + \sstsubsection{ + dp = double [3] (Returned) + }{ + result vector + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraRxp(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palDpav +}{ + Position angle of one celestial direction with respect to another +}{ + \sstdescription{ + Position angle of one celestial direction with respect to another. + } + \sstinvocation{ + pa = palDpav( double v1[3], double v2[3] ); + } + \sstarguments{ + \sstsubsection{ + v1 = double [3] (Given) + }{ + direction cosines of one point. + } + \sstsubsection{ + v2 = double [3] (Given) + }{ + direction cosines of the other point. + } + } + \sstreturnedvalue{ + \sstsubsection{ + The result is the bearing (position angle), in radians, of point + }{ + } + \sstsubsection{ + V2 with respect to point V1. It is in the range $+$/- pi. The + }{ + } + \sstsubsection{ + sense is such that if V2 is a small distance east of V1, the + }{ + } + \sstsubsection{ + bearing is about $+$pi/2. Zero is returned if the two points + }{ + } + \sstsubsection{ + are coincident. + }{ + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + The coordinate frames correspond to RA,Dec, Long,Lat etc. + + \sstitem + Uses eraPap(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palDr2af +}{ + Convert an angle in radians to degrees, arcminutes, arcseconds +}{ + \sstdescription{ + Convert an angle in radians to degrees, arcminutes, arcseconds. + } + \sstinvocation{ + palDr2af( int ndp, double angle, char $*$sign, int idmsf[4] ); + } + \sstarguments{ + \sstsubsection{ + ndp = int (Given) + }{ + number of decimal places of arcseconds + } + \sstsubsection{ + angle = double (Given) + }{ + angle in radians + } + \sstsubsection{ + sign = char $*$ (Returned) + }{ + {\tt '}$+${\tt '} or {\tt '}-{\tt '} (single character) + } + \sstsubsection{ + idmsf = int [4] (Returned) + }{ + Degrees, arcminutes, arcseconds, fraction + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraA2af(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palDr2tf +}{ + Convert an angle in radians to hours, minutes, seconds +}{ + \sstdescription{ + Convert an angle in radians to hours, minutes, seconds. + } + \sstinvocation{ + palDr2tf ( int ndp, double angle, char $*$sign, int ihmsf[4] ); + } + \sstarguments{ + \sstsubsection{ + ndp = int (Given) + }{ + number of decimal places of arcseconds + } + \sstsubsection{ + angle = double (Given) + }{ + angle in radians + } + \sstsubsection{ + sign = char $*$ (Returned) + }{ + {\tt '}$+${\tt '} or {\tt '}-{\tt '} (single character) + } + \sstsubsection{ + idmsf = int [4] (Returned) + }{ + Hours, minutes, seconds, fraction + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraA2tf(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palDranrm +}{ + Normalize angle into range 0-2 pi +}{ + \sstdescription{ + Normalize angle into range 0-2 pi. + } + \sstinvocation{ + norm = palDranrm( double angle ); + } + \sstarguments{ + \sstsubsection{ + angle = double (Given) + }{ + angle in radians + } + } + \sstreturnedvalue{ + \sstsubsection{ + Angle expressed in the range 0-2 pi + }{ + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraAnp(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palDsep +}{ + Angle between two points on a sphere +}{ + \sstdescription{ + Angle between two points on a sphere. + } + \sstinvocation{ + ang = palDsep( double a1, double b1, double a2, double b2 ); + } + \sstarguments{ + \sstsubsection{ + a1 = double (Given) + }{ + Spherical coordinate of one point (radians) + } + \sstsubsection{ + b1 = double (Given) + }{ + Spherical coordinate of one point (radians) + } + \sstsubsection{ + a2 = double (Given) + }{ + Spherical coordinate of other point (radians) + } + \sstsubsection{ + b2 = double (Given) + }{ + Spherical coordinate of other point (radians) + } + } + \sstreturnedvalue{ + \sstsubsection{ + Angle, in radians, between the two points. Always positive. + }{ + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + The spherical coordinates are [RA,Dec], [Long,Lat] etc, in radians. + + \sstitem + Uses eraSeps(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palDsepv +}{ + Angle between two vectors +}{ + \sstdescription{ + Angle between two vectors. + } + \sstinvocation{ + ang = palDsepv( double v1[3], double v2[3] ); + } + \sstarguments{ + \sstsubsection{ + v1 = double [3] (Given) + }{ + First vector + } + \sstsubsection{ + v2 = double [3] (Given) + }{ + Second vector + } + } + \sstreturnedvalue{ + \sstsubsection{ + Angle, in radians, between the two points. Always positive. + }{ + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraSepp(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palDtf2d +}{ + Convert hours, minutes, seconds to days +}{ + \sstdescription{ + Convert hours, minutes, seconds to days. + } + \sstinvocation{ + palDtf2d( int ihour, int imin, double sec, double $*$days, int $*$j ); + } + \sstarguments{ + \sstsubsection{ + ihour = int (Given) + }{ + Hours + } + \sstsubsection{ + imin = int (Given) + }{ + Minutes + } + \sstsubsection{ + sec = double (Given) + }{ + Seconds + } + \sstsubsection{ + days = double $*$ (Returned) + }{ + Interval in days + } + \sstsubsection{ + j = int $*$ (Returned) + }{ + status: 0 = ok, 1 = ihour outside range 0-23, + 2 = imin outside range 0-59, 3 = sec outside range 0-59.999... + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraTf2d(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palDtf2r +}{ + Convert hours, minutes, seconds to radians +}{ + \sstdescription{ + Convert hours, minutes, seconds to radians. + } + \sstinvocation{ + palDtf2r( int ihour, int imin, double sec, double $*$rad, int $*$j ); + } + \sstarguments{ + \sstsubsection{ + ihour = int (Given) + }{ + Hours + } + \sstsubsection{ + imin = int (Given) + }{ + Minutes + } + \sstsubsection{ + sec = double (Given) + }{ + Seconds + } + \sstsubsection{ + days = double $*$ (Returned) + }{ + Angle in radians + } + \sstsubsection{ + j = int $*$ (Returned) + }{ + status: 0 = ok, 1 = ihour outside range 0-23, + 2 = imin outside range 0-59, 3 = sec outside range 0-59.999... + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraTf2a(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palDvdv +}{ + Scalar product of two 3-vectors +}{ + \sstdescription{ + Scalar product of two 3-vectors. + } + \sstinvocation{ + prod = palDvdv ( double va[3], double vb[3] ); + } + \sstarguments{ + \sstsubsection{ + va = double [3] (Given) + }{ + First vector + } + \sstsubsection{ + vb = double [3] (Given) + }{ + Second vector + } + } + \sstreturnedvalue{ + \sstsubsection{ + Scalar product va.vb + }{ + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraPdp(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palDvn +}{ + Normalizes a 3-vector also giving the modulus +}{ + \sstdescription{ + Normalizes a 3-vector also giving the modulus. + } + \sstinvocation{ + palDvn( double v[3], double uv[3], double $*$vm ); + } + \sstarguments{ + \sstsubsection{ + v = double [3] (Given) + }{ + vector + } + \sstsubsection{ + uv = double [3] (Returned) + }{ + unit vector in direction of {\tt "}v{\tt "} + } + \sstsubsection{ + vm = double $*$ (Returned) + }{ + modulus of {\tt "}v{\tt "} + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraPn(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palDvxv +}{ + Vector product of two 3-vectors +}{ + \sstdescription{ + Vector product of two 3-vectors. + } + \sstinvocation{ + palDvxv( double va[3], double vb[3], double vc[3] ); + } + \sstarguments{ + \sstsubsection{ + va = double [3] (Given) + }{ + First vector + } + \sstsubsection{ + vb = double [3] (Given) + }{ + Second vector + } + \sstsubsection{ + vc = double [3] (Returned) + }{ + Result vector + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraPxp(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palEpb +}{ + Conversion of modified Julian Data to Besselian Epoch +}{ + \sstdescription{ + Conversion of modified Julian Data to Besselian Epoch. + } + \sstinvocation{ + epb = palEpb ( double date ); + } + \sstarguments{ + \sstsubsection{ + date = double (Given) + }{ + Modified Julian Date (JD - 2400000.5) + } + } + \sstreturnedvalue{ + \sstsubsection{ + Besselian epoch. + }{ + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraEpb(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palEpb2d +}{ + Conversion of Besselian Epoch to Modified Julian Date +}{ + \sstdescription{ + Conversion of Besselian Epoch to Modified Julian Date. + } + \sstinvocation{ + mjd = palEpb2d ( double epb ); + } + \sstarguments{ + \sstsubsection{ + epb = double (Given) + }{ + Besselian Epoch + } + } + \sstreturnedvalue{ + \sstsubsection{ + Modified Julian Date (JD - 2400000.5) + }{ + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraEpb2jd(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palEpj +}{ + Conversion of Modified Julian Date to Julian Epoch +}{ + \sstdescription{ + Conversion of Modified Julian Date to Julian Epoch. + } + \sstinvocation{ + epj = palEpj ( double date ); + } + \sstarguments{ + \sstsubsection{ + date = double (Given) + }{ + Modified Julian Date (JD - 2400000.5) + } + } + \sstreturnedvalue{ + \sstsubsection{ + The Julian Epoch. + }{ + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraEpj(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palEpj2d +}{ + Conversion of Julian Epoch to Modified Julian Date +}{ + \sstdescription{ + Conversion of Julian Epoch to Modified Julian Date. + } + \sstinvocation{ + mjd = palEpj2d ( double epj ); + } + \sstarguments{ + \sstsubsection{ + epj = double (Given) + }{ + Julian Epoch. + } + } + \sstreturnedvalue{ + \sstsubsection{ + Modified Julian Date (JD - 2400000.5) + }{ + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraEpj2d(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palEqeqx +}{ + Equation of the equinoxes (IAU 2000/2006) +}{ + \sstdescription{ + Equation of the equinoxes (IAU 2000/2006). + } + \sstinvocation{ + palEqeqx( double date ); + } + \sstarguments{ + \sstsubsection{ + date = double (Given) + }{ + TT as Modified Julian Date (JD-400000.5) + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraEe06a(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palFk5hz +}{ + Transform an FK5 (J2000) star position into the frame of the + Hipparcos catalogue +}{ + \sstdescription{ + Transform an FK5 (J2000) star position into the frame of the + Hipparcos catalogue. + } + \sstinvocation{ + palFk5hz ( double r5, double d5, double epoch, + double $*$rh, double $*$dh ); + } + \sstarguments{ + \sstsubsection{ + r5 = double (Given) + }{ + FK5 RA (radians), equinox J2000, epoch {\tt "}epoch{\tt "} + } + \sstsubsection{ + d5 = double (Given) + }{ + FK5 dec (radians), equinox J2000, epoch {\tt "}epoch{\tt "} + } + \sstsubsection{ + epoch = double (Given) + }{ + Julian epoch + } + \sstsubsection{ + rh = double $*$ (Returned) + }{ + RA (radians) + } + \sstsubsection{ + dh = double $*$ (Returned) + }{ + Dec (radians) + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Assumes zero Hipparcos proper motion. + + \sstitem + Uses eraEpj2jd() and eraFk5hz. + See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palGmst +}{ + Greenwich mean sidereal time (consistent with IAU 2006 precession) +}{ + \sstdescription{ + Greenwich mean sidereal time (consistent with IAU 2006 precession). + } + \sstinvocation{ + mst = palGmst ( double ut1 ); + } + \sstarguments{ + \sstsubsection{ + ut1 = double (Given) + }{ + Universal time (UT1) expressed as modified Julian Date (JD-2400000.5) + } + } + \sstreturnedvalue{ + \sstsubsection{ + Greenwich mean sidereal time + }{ + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraGmst06(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palGmsta +}{ + Greenwich mean sidereal time (consistent with IAU 2006 precession) +}{ + \sstdescription{ + Greenwich mean sidereal time (consistent with IAU 2006 precession). + } + \sstinvocation{ + mst = palGmsta ( double date, double ut1 ); + } + \sstarguments{ + \sstsubsection{ + date = double (Given) + }{ + UT1 date (MJD: integer part of JD-2400000.5) + } + \sstsubsection{ + ut1 = double (Given) + }{ + UT1 time (fraction of a day) + } + } + \sstreturnedvalue{ + \sstsubsection{ + Greenwich mean sidereal time (in range 0 to 2 pi) + }{ + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + For best accuracy use eraGmst06() directly. + + \sstitem + Uses eraGmst06(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palHfk5z +}{ + Hipparcos star position to FK5 J2000 +}{ + \sstdescription{ + Transform a Hipparcos star position into FK5 J2000, assuming + zero Hipparcos proper motion. + } + \sstinvocation{ + palHfk5z( double rh, double dh, double epoch, + double $*$r5, double $*$d5, double $*$dr5, double $*$dd5 ); + } + \sstarguments{ + \sstsubsection{ + rh = double (Given) + }{ + Hipparcos RA (radians) + } + \sstsubsection{ + dh = double (Given) + }{ + Hipparcos Dec (radians) + } + \sstsubsection{ + epoch = double (Given) + }{ + Julian epoch (TDB) + } + \sstsubsection{ + r5 = double $*$ (Returned) + }{ + RA (radians, FK5, equinox J2000, epoch {\tt "}epoch{\tt "}) + } + \sstsubsection{ + d5 = double $*$ (Returned) + }{ + Dec (radians, FK5, equinox J2000, epoch {\tt "}epoch{\tt "}) + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraEpj2jd and eraHfk5z(). See SOFA/ERFA documentation for details. + } + } +} +\sstroutine{ + palRefcoq +}{ + Determine the constants A and B in the atmospheric refraction model +}{ + \sstdescription{ + Determine the constants A and B in the atmospheric refraction + model dZ = A tan Z $+$ B tan$*$$*$3 Z. This is a fast alternative + to the palRefco routine. + + Z is the {\tt "}observed{\tt "} zenith distance (i.e. affected by refraction) + and dZ is what to add to Z to give the {\tt "}topocentric{\tt "} (i.e. in vacuo) + zenith distance. + } + \sstinvocation{ + palRefcoq( double tdk, double pmb, double rh, double wl, + double $*$refa, double $*$refb ); + } + \sstarguments{ + \sstsubsection{ + tdk = double (Given) + }{ + Ambient temperature at the observer (K) + } + \sstsubsection{ + pmb = double (Given) + }{ + Pressure at the observer (millibar) + } + \sstsubsection{ + rh = double (Given) + }{ + Relative humidity at the observer (range 0-1) + } + \sstsubsection{ + wl = double (Given) + }{ + Effective wavelength of the source (micrometre). + Radio refraction is chosen by specifying wl $>$ 100 micrometres. + } + \sstsubsection{ + refa = double $*$ (Returned) + }{ + tan Z coefficient (radian) + } + \sstsubsection{ + refb = double $*$ (Returned) + }{ + tan$*$$*$3 Z coefficient (radian) + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraRefco(). See SOFA/ERFA documentation for details. + + \sstitem + Note that the SOFA/ERFA routine uses different order of + of arguments and uses deg C rather than K. + } + } +} + + +\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{ + palAop +}{ + Apparent to observed place +}{ + \sstdescription{ + Apparent to observed place for sources distant from the solar system. + } + \sstinvocation{ + 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 ); + } + \sstarguments{ + \sstsubsection{ + rap = double (Given) + }{ + Geocentric apparent right ascension + } + \sstsubsection{ + dap = double (Given) + }{ + Geocentirc apparent declination + } + \sstsubsection{ + date = double (Given) + }{ + UTC date/time (Modified Julian Date, JD-2400000.5) + } + \sstsubsection{ + dut = double (Given) + }{ + delta UT: UT1-UTC (UTC seconds) + } + \sstsubsection{ + elongm = double (Given) + }{ + Mean longitude of the observer (radians, east $+$ve) + } + \sstsubsection{ + phim = double (Given) + }{ + Mean geodetic latitude of the observer (radians) + } + \sstsubsection{ + hm = double (Given) + }{ + Observer{\tt '}s height above sea level (metres) + } + \sstsubsection{ + xp = double (Given) + }{ + Polar motion x-coordinates (radians) + } + \sstsubsection{ + yp = double (Given) + }{ + Polar motion y-coordinates (radians) + } + \sstsubsection{ + tdk = double (Given) + }{ + Local ambient temperature (K; std=273.15) + } + \sstsubsection{ + pmb = double (Given) + }{ + Local atmospheric pressure (mb; std=1013.25) + } + \sstsubsection{ + rh = double (Given) + }{ + Local relative humidity (in the range 0.0-1.0) + } + \sstsubsection{ + wl = double (Given) + }{ + Effective wavelength (micron, e.g. 0.55) + } + \sstsubsection{ + tlr = double (Given) + }{ + Tropospheric laps rate (K/metre, e.g. 0.0065) + } + \sstsubsection{ + aob = double $*$ (Returned) + }{ + Observed azimuth (radians: N=0; E=90) + } + \sstsubsection{ + zob = double $*$ (Returned) + }{ + Observed zenith distance (radians) + } + \sstsubsection{ + hob = double $*$ (Returned) + }{ + Observed Hour Angle (radians) + } + \sstsubsection{ + dob = double $*$ (Returned) + }{ + Observed Declination (radians) + } + \sstsubsection{ + rob = double $*$ (Returned) + }{ + Observed Right Ascension (radians) + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + This routine returns zenith distance rather than elevation + in order to reflect the fact that no allowance is made for + depression of the horizon. + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + {\tt "}Apparent{\tt "} 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{\tt '}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. + + \sstitem + {\tt "}Observed{\tt "} 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{\tt '}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. + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + 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 $\sim$ -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 $\sim$ 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. + + \sstitemlist{ + + \sstitem + 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. + } + } +} +\sstroutine{ + palAoppa +}{ + Precompute apparent to observed place parameters +}{ + \sstdescription{ + Precompute apparent to observed place parameters required by palAopqk + and palOapqk. + } + \sstinvocation{ + 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] ); + } + \sstarguments{ + \sstsubsection{ + date = double (Given) + }{ + UTC date/time (modified Julian Date, JD-2400000.5) + } + \sstsubsection{ + dut = double (Given) + }{ + delta UT: UT1-UTC (UTC seconds) + } + \sstsubsection{ + elongm = double (Given) + }{ + mean longitude of the observer (radians, east $+$ve) + } + \sstsubsection{ + phim = double (Given) + }{ + mean geodetic latitude of the observer (radians) + } + \sstsubsection{ + hm = double (Given) + }{ + observer{\tt '}s height above sea level (metres) + } + \sstsubsection{ + xp = double (Given) + }{ + polar motion x-coordinate (radians) + } + \sstsubsection{ + yp = double (Given) + }{ + polar motion y-coordinate (radians) + } + \sstsubsection{ + tdk = double (Given) + }{ + local ambient temperature (K; std=273.15) + } + \sstsubsection{ + pmb = double (Given) + }{ + local atmospheric pressure (mb; std=1013.25) + } + \sstsubsection{ + rh = double (Given) + }{ + local relative humidity (in the range 0.0-1.0) + } + \sstsubsection{ + wl = double (Given) + }{ + effective wavelength (micron, e.g. 0.55) + } + \sstsubsection{ + tlr = double (Given) + }{ + tropospheric lapse rate (K/metre, e.g. 0.0065) + } + \sstsubsection{ + 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) + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + 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 $\sim$ -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 $\sim$ 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. + + \sstitemlist{ + + \sstitem + 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. + } + } +} +\sstroutine{ + palAoppat +}{ + Recompute sidereal time to support apparent to observed place +}{ + \sstdescription{ + This routine recomputes the sidereal time in the apparent to + observed place star-independent parameter block. + } + \sstinvocation{ + void palAoppat( double date, double aoprms[14] ); + } + \sstarguments{ + \sstsubsection{ + date = double (Given) + }{ + UTC date/time (modified Julian Date, JD-2400000.5) + (see palAoppa description for comments on leap seconds) + } + \sstsubsection{ + 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). + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + See palAoppa for more information. + + \sstitem + The star-independent parameters are not treated as an opaque + struct in order to retain compatibility with SLA. + } + } +} +\sstroutine{ + palAopqk +}{ + Quick apparent to observed place +}{ + \sstdescription{ + Quick apparent to observed place. + } + \sstinvocation{ + void palAopqk ( double rap, double dap, const double aoprms[14], + double $*$aob, double $*$zob, double $*$hob, + double $*$dob, double $*$rob ); + } + \sstarguments{ + \sstsubsection{ + rap = double (Given) + }{ + Geocentric apparent right ascension + } + \sstsubsection{ + dap = double (Given) + }{ + Geocentric apparent declination + } + \sstsubsection{ + 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) + } + \sstsubsection{ + aob = double $*$ (Returned) + }{ + Observed azimuth (radians: N=0,E=90) + } + \sstsubsection{ + zob = double $*$ (Returned) + }{ + Observed zenith distance (radians) + } + \sstsubsection{ + hob = double $*$ (Returned) + }{ + Observed Hour Angle (radians) + } + \sstsubsection{ + dob = double $*$ (Returned) + }{ + Observed Declination (radians) + } + \sstsubsection{ + rob = double $*$ (Returned) + }{ + Observed Right Ascension (radians) + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + This routine returns zenith distance rather than elevation + in order to reflect the fact that no allowance is made for + depression of the horizon. + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + {\tt "}Apparent{\tt "} 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{\tt '}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. + + \sstitem + {\tt "}Observed{\tt "} 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{\tt '}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. + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + 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. + } + } +} +\sstroutine{ + palAtmdsp +}{ + Apply atmospheric-dispersion adjustments to refraction coefficients +}{ + \sstdescription{ + Apply atmospheric-dispersion adjustments to refraction coefficients. + } + \sstinvocation{ + void palAtmdsp( double tdk, double pmb, double rh, double wl1, + double a1, double b1, double wl2, double $*$a2, double $*$b2 ); + } + \sstarguments{ + \sstsubsection{ + tdk = double (Given) + }{ + Ambient temperature, K + } + \sstsubsection{ + pmb = double (Given) + }{ + Ambient pressure, millibars + } + \sstsubsection{ + rh = double (Given) + }{ + Ambient relative humidity, 0-1 + } + \sstsubsection{ + wl1 = double (Given) + }{ + Reference wavelength, micrometre (0.4 recommended) + } + \sstsubsection{ + a1 = double (Given) + }{ + Refraction coefficient A for wavelength wl1 (radians) + } + \sstsubsection{ + b1 = double (Given) + }{ + Refraction coefficient B for wavelength wl1 (radians) + } + \sstsubsection{ + wl2 = double (Given) + }{ + Wavelength for which adjusted A,B required + } + \sstsubsection{ + a2 = double $*$ (Returned) + }{ + Refraction coefficient A for wavelength WL2 (radians) + } + \sstsubsection{ + b2 = double $*$ (Returned) + }{ + Refraction coefficient B for wavelength WL2 (radians) + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + 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. + + \sstitemlist{ + + \sstitem + 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. + + \sstitem + 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, + {\tt "}Spherical Astronomy{\tt "}, Cambridge University Press, 1985). + } + } +} +\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 eraCal2jd for other values. + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraCal2jd + + \sstitem + 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/ERFA 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). + } + } + \sstimplementationstatus{ + \sstitemlist{ + + \sstitem + 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. + } + } +} +\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 eraJd2cal for other values. + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Uses eraJd2cal + } + } +} +\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) + }{ + On input the vector of N knowns. 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. + } + \sstsubsection{ + iw = int[] (Given) + }{ + Integer workspace of size N. + } + } + \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{ + palDat +}{ + Return offset between UTC and TAI +}{ + \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/ERFA eraDat function. + + \sstitem + This routine matches the slaDat interface which differs from the eraDat + interface. Consider coding directly to the SOFA/ERFA interface. + + \sstitem + See eraDat for a description of error conditions when calling this function + with a time outside of the UTC range. + + \sstitem + 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. + } + } +} +\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 eraDat for a description of error conditions when calling this function + with a time outside of the UTC range. This behaviour differs from slaDtt. + } + } +} +\sstroutine{ + palEcleq +}{ + Transform from ecliptic coordinates to J2000.0 equatorial coordinates +}{ + \sstdescription{ + Transform from ecliptic coordinate to J2000.0 equatorial coordinates. + } + \sstinvocation{ + void palEcleq ( double dl, double db, double date, + double $*$dr, double $*$dd ); + } + \sstarguments{ + \sstsubsection{ + dl = double (Given) + }{ + Ecliptic longitude (mean of date, IAU 1980 theory, radians) + } + \sstsubsection{ + db = double (Given) + }{ + Ecliptic latitude (mean of date, IAU 1980 theory, 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{ + dr = double $*$ (Returned) + }{ + J2000.0 mean RA (radians) + } + \sstsubsection{ + dd = double $*$ (Returned) + }{ + J2000.0 mean Dec (Radians) + } + } +} +\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) + \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 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 eraEpv00 for details on accuracy + + \sstitem + Note that the status argument from eraEpv00 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 eraEpv00. + } + \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 eraGd2gc + } + } +} +\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. + + \sstitem + 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. + + \sstitem + The distinction between the required TDB and TT is always + negligible. Moreover, for all but the most critical + applications UTC is adequate. + + \sstitem + The proper motions in RA are dRA/dt rather than cos(Dec)$*$dRA/dt. + + \sstitem + 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). + + \sstitem + The accuracy is sub-milliarcsecond, limited by the + precession-nutation model (see palPrenut for details). + + \sstitem + 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. + } + } +} +\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 eraNut06a 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/ERFA 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 eraObl06 and eraNut06a 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{ + palOap +}{ + Observed to apparent place +}{ + \sstdescription{ + Observed to apparent place. + } + \sstinvocation{ + 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 ); + } + \sstarguments{ + \sstsubsection{ + type = const char $*$ (Given) + }{ + Type of coordinates - {\tt '}R{\tt '}, {\tt '}H{\tt '} or {\tt '}A{\tt '} (see below) + } + \sstsubsection{ + ob1 = double (Given) + }{ + Observed Az, HA or RA (radians; Az is N=0;E=90) + } + \sstsubsection{ + ob2 = double (Given) + }{ + Observed ZD or Dec (radians) + } + \sstsubsection{ + date = double (Given) + }{ + UTC date/time (Modified Julian Date, JD-2400000.5) + } + \sstsubsection{ + dut = double (Given) + }{ + delta UT: UT1-UTC (UTC seconds) + } + \sstsubsection{ + elongm = double (Given) + }{ + Mean longitude of the observer (radians, east $+$ve) + } + \sstsubsection{ + phim = double (Given) + }{ + Mean geodetic latitude of the observer (radians) + } + \sstsubsection{ + hm = double (Given) + }{ + Observer{\tt '}s height above sea level (metres) + } + \sstsubsection{ + xp = double (Given) + }{ + Polar motion x-coordinates (radians) + } + \sstsubsection{ + yp = double (Given) + }{ + Polar motion y-coordinates (radians) + } + \sstsubsection{ + tdk = double (Given) + }{ + Local ambient temperature (K; std=273.15) + } + \sstsubsection{ + pmb = double (Given) + }{ + Local atmospheric pressure (mb; std=1013.25) + } + \sstsubsection{ + rh = double (Given) + }{ + Local relative humidity (in the range 0.0-1.0) + } + \sstsubsection{ + wl = double (Given) + }{ + Effective wavelength (micron, e.g. 0.55) + } + \sstsubsection{ + tlr = double (Given) + }{ + Tropospheric laps rate (K/metre, e.g. 0.0065) + } + \sstsubsection{ + rap = double $*$ (Given) + }{ + Geocentric apparent right ascension + } + \sstsubsection{ + dap = double $*$ (Given) + }{ + Geocentric apparent declination + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Only the first character of the TYPE argument is significant. + {\tt '}R{\tt '} or {\tt '}r{\tt '} indicates that OBS1 and OBS2 are the observed right + ascension and declination; {\tt '}H{\tt '} or {\tt '}h{\tt '} indicates that they are + hour angle (west $+$ve) and declination; anything else ({\tt '}A{\tt '} or + {\tt '}a{\tt '} 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.) + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + {\tt "}Observed{\tt "} 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. {\tt "}Observed{\tt "} 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{\tt '}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. + + \sstitem + 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 {\tt "}FK5{\tt "} (J2000) mean place, by + allowing for the Sun{\tt '}s gravitational lens effect, annual + aberration, nutation and precession. Should {\tt "}FK4{\tt "} (1950) + coordinates be needed, the routines palFk524 etc will also + need to be applied. + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + 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 $\sim$ -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 $\sim$ 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. + + \sstitemlist{ + + \sstitem + 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. + } + } +} +\sstroutine{ + palOapqk +}{ + Quick observed to apparent place +}{ + \sstdescription{ + type = const char $*$ (Given) + Type of coordinates - {\tt '}R{\tt '}, {\tt '}H{\tt '} or {\tt '}A{\tt '} (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 + } + \sstinvocation{ + void palOapqk ( const char $*$type, double ob1, double ob2, + const double aoprms[14], double $*$rap, double $*$dap ); + } + \sstarguments{ + \sstsubsection{ + Quick observed to apparent place. + }{ + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Only the first character of the TYPE argument is significant. + {\tt '}R{\tt '} or {\tt '}r{\tt '} indicates that OBS1 and OBS2 are the observed right + ascension and declination; {\tt '}H{\tt '} or {\tt '}h{\tt '} indicates that they are + hour angle (west $+$ve) and declination; anything else ({\tt '}A{\tt '} or + {\tt '}a{\tt '} 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.) + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + {\tt "}Observed{\tt "} 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. {\tt "}Observed{\tt "} 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{\tt '}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. + + \sstitem + 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 {\tt "}FK5{\tt "} (J2000) mean place, by + allowing for the Sun{\tt '}s gravitational lens effect, annual + aberration, nutation and precession. Should {\tt "}FK4{\tt "} (1950) + coordinates be needed, the routines palFk524 etc will also + need to be applied. + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + 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. + } + } +} +\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{ + palPcd +}{ + Apply pincushion/barrel distortion to a tangent-plane [x,y] +}{ + \sstdescription{ + Applies pincushion and barrel distortion to a tangent + plane coordinate. + } + \sstinvocation{ + palPcd( double disco, double $*$ x, double $*$ y ); + } + \sstarguments{ + \sstsubsection{ + disco = double (Given) + }{ + Pincushion/barrel distortion coefficient. + } + \sstsubsection{ + x = double $*$ (Given \& Returned) + }{ + On input the tangent-plane X coordinate, on output + the distorted X coordinate. + } + \sstsubsection{ + y = double $*$ (Given \& Returned) + }{ + On input the tangent-plane Y coordinate, on output + the distorted Y coordinate. + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + The distortion is of the form RP = R$*$(1 $+$ C$*$R$*$$*$2), where R is + the radial distance from the tangent point, C is the DISCO + argument, and RP is the radial distance in the presence of + the distortion. + + \sstitem + For pincushion distortion, C is $+$ve; for barrel distortion, + C is -ve. + + \sstitem + For X,Y in units of one projection radius (in the case of + a photographic plate, the focal length), the following + DISCO values apply: + +\begin{center} +\begin{tabular}{ll} + Geometry &DISCO \\ +\hline + astrograph & 0.0 \\ + Schmidt &-0.3333 \\ + AAT PF doublet &$+$147.069 \\ + AAT PF triplet &$+$178.585 \\ + AAT f/8 &$+$21.20 \\ + JKT f/8 &$+$13.32 \\ +\end{tabular} +\end{center} + } + } + \sstdiytopic{ + See Also + }{ + \sstitemlist{ + + \sstitem + There is a companion routine, palUnpcd, which performs the + inverse operation. + } + } +} + +\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/ERFA eraPlan94 for details + + \sstitem + Note that Pluto is supported in SLA/F but not in this routine + + \sstitem + Status -2 is equivalent to eraPlan94 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/ERFA routine eraStarpm. + } + \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 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. + + \sstitem + Assumes all epochs are Julian epochs. + } + } +} +\sstroutine{ + palPolmo +}{ + Correct for polar motion +}{ + \sstdescription{ + Polar motion: correct site longitude and latitude for polar + motion and calculate azimuth difference between celestial and + terrestrial poles. + } + \sstinvocation{ + palPolmo ( double elongm, double phim, double xp, double yp, + double $*$elong, double $*$phi, double $*$daz ); + } + \sstarguments{ + \sstsubsection{ + elongm = double (Given) + }{ + Mean logitude of the observer (radians, east $+$ve) + } + \sstsubsection{ + phim = double (Given) + }{ + Mean geodetic latitude of the observer (radians) + } + \sstsubsection{ + xp = double (Given) + }{ + Polar motion x-coordinate (radians) + } + \sstsubsection{ + yp = double (Given) + }{ + Polar motion y-coordinate (radians) + } + \sstsubsection{ + elong = double $*$ (Returned) + }{ + True longitude of the observer (radians, east $+$ve) + } + \sstsubsection{ + phi = double $*$ (Returned) + }{ + True geodetic latitude of the observer (radians) + } + \sstsubsection{ + daz = double $*$ (Returned) + }{ + Azimuth correction (terrestrial-celestial, radians) + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + {\tt "}Mean{\tt "} longitude and latitude are the (fixed) values for the + site{\tt '}s location with respect to the IERS terrestrial reference + frame; the latitude is geodetic. TAKE CARE WITH THE LONGITUDE + SIGN CONVENTION. The longitudes used by the present routine + are east-positive, in accordance with geographical convention + (and right-handed). In particular, note that the longitudes + returned by the sla\_OBS routine are west-positive, following + astronomical usage, and must be reversed in sign before use in + the present routine. + + \sstitem + XP and YP are the (changing) coordinates of the Celestial + Ephemeris Pole with respect to the IERS Reference Pole. + XP is positive along the meridian at longitude 0 degrees, + and YP is positive along the meridian at longitude + 270 degrees (i.e. 90 degrees west). Values for XP,YP can + be obtained from IERS circulars and equivalent publications; + the maximum amplitude observed so far is about 0.3 arcseconds. + + \sstitem + {\tt "}True{\tt "} longitude and latitude are the (moving) values for + the site{\tt '}s location with respect to the celestial ephemeris + pole and the meridian which corresponds to the Greenwich + apparent sidereal time. The true longitude and latitude + link the terrestrial coordinates with the standard celestial + models (for precession, nutation, sidereal time etc). + + \sstitem + The azimuths produced by sla\_AOP and sla\_AOPQK are with + respect to due north as defined by the Celestial Ephemeris + Pole, and can therefore be called {\tt "}celestial azimuths{\tt "}. + However, a telescope fixed to the Earth measures azimuth + essentially with respect to due north as defined by the + IERS Reference Pole, and can therefore be called {\tt "}terrestrial + azimuth{\tt "}. Uncorrected, this would manifest itself as a + changing {\tt "}azimuth zero-point error{\tt "}. The value DAZ is the + correction to be added to a celestial azimuth to produce + a terrestrial azimuth. + + \sstitem + The present routine is rigorous. For most practical + purposes, the following simplified formulae provide an + adequate approximation: + + } + elong = elongm$+$xp$*$cos(elongm)-yp$*$sin(elongm) + phi = phim$+$(xp$*$sin(elongm)$+$yp$*$cos(elongm))$*$tan(phim) + daz = -sqrt(xp$*$xp$+$yp$*$yp)$*$cos(elongm-atan2(xp,yp))/cos(phim) + + An alternative formulation for DAZ is: + + x = cos(elongm)$*$cos(phim) + y = sin(elongm)$*$cos(phim) + daz = atan2(-x$*$yp-y$*$xp,x$*$x$+$y$*$y) + + \sstitemlist{ + + \sstitem + Reference: Seidelmann, P.K. (ed), 1992. {\tt "}Explanatory Supplement + to the Astronomical Almanac{\tt "}, ISBN 0-935702-68-7, + sections 3.27, 4.25, 4.52. + } + } +} + +\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 eraPlan94. + } + } +} +\sstroutine{ + palRefco +}{ + Determine constants in atmospheric refraction model +}{ + \sstdescription{ + Determine the constants A and B in the atmospheric refraction + model dZ = A tan Z $+$ B tan$*$$*$3 Z. + + Z is the {\tt "}observed{\tt "} zenith distance (i.e. affected by refraction) + and dZ is what to add to Z to give the {\tt "}topocentric{\tt "} (i.e. in vacuo) + zenith distance. + } + \sstinvocation{ + void palRefco ( double hm, double tdk, double pmb, double rh, + double wl, double phi, double tlr, double eps, + double $*$refa, double $*$refb ); + } + \sstarguments{ + \sstsubsection{ + hm = double (Given) + }{ + Height of the observer above sea level (metre) + } + \sstsubsection{ + tdk = double (Given) + }{ + Ambient temperature at the observer (K) + } + \sstsubsection{ + pmb = double (Given) + }{ + Pressure at the observer (millibar) + } + \sstsubsection{ + rh = double (Given) + }{ + Relative humidity at the observer (range 0-1) + } + \sstsubsection{ + wl = double (Given) + }{ + Effective wavelength of the source (micrometre) + } + \sstsubsection{ + phi = double (Given) + }{ + Latitude of the observer (radian, astronomical) + } + \sstsubsection{ + tlr = double (Given) + }{ + Temperature lapse rate in the troposphere (K/metre) + } + \sstsubsection{ + eps = double (Given) + }{ + Precision required to terminate iteration (radian) + } + \sstsubsection{ + refa = double $*$ (Returned) + }{ + tan Z coefficient (radian) + } + \sstsubsection{ + refb = double $*$ (Returned) + }{ + tan$*$$*$3 Z coefficient (radian) + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + Typical values for the TLR and EPS arguments might be 0.0065 and + 1E-10 respectively. + + \sstitem + The radio refraction is chosen by specifying WL $>$ 100 micrometres. + + \sstitem + 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. + } + } +} +\sstroutine{ + palRefro +}{ + Atmospheric refraction for radio and optical/IR wavelengths +}{ + \sstdescription{ + Calculates the atmospheric refraction for radio and optical/IR + wavelengths. + } + \sstinvocation{ + void palRefro( double zobs, double hm, double tdk, double pmb, + } + \sstarguments{ + \sstsubsection{ + zobs = double (Given) + }{ + Observed zenith distance of the source (radian) + } + \sstsubsection{ + hm = double (Given) + }{ + Height of the observer above sea level (metre) + } + \sstsubsection{ + tdk = double (Given) + }{ + Ambient temperature at the observer (K) + } + \sstsubsection{ + pmb = double (Given) + }{ + Pressure at the observer (millibar) + } + \sstsubsection{ + rh = double (Given) + }{ + Relative humidity at the observer (range 0-1) + } + \sstsubsection{ + wl = double (Given) + }{ + Effective wavelength of the source (micrometre) + } + \sstsubsection{ + phi = double (Given) + }{ + Latitude of the observer (radian, astronomical) + } + \sstsubsection{ + tlr = double (Given) + }{ + Temperature lapse rate in the troposphere (K/metre) + } + \sstsubsection{ + eps = double (Given) + }{ + Precision required to terminate iteration (radian) + } + \sstsubsection{ + ref = double $*$ (Returned) + }{ + Refraction: in vacuao ZD minus observed ZD (radian) + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + 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). + + \sstitem + 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{\tt '}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, {\tt "}Refractive Index Formulae for + Electronic Distance Measurement with Radio and Millimetre + Waves{\tt "}, 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. + + \sstitemlist{ + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + 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. + + \sstitem + It should be noted that the relative humidity RH is formally + defined in terms of {\tt "}mixing ratio{\tt "} 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). + + \sstitem + 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. + } + } +} +\sstroutine{ + palRefv +}{ + Adjust an unrefracted Cartesian vector to include the effect of atmospheric refraction +}{ + \sstdescription{ + Adjust an unrefracted Cartesian vector to include the effect of + atmospheric refraction, using the simple A tan Z $+$ B tan$*$$*$3 Z + model. + } + \sstinvocation{ + void palRefv ( double vu[3], double refa, double refb, double vr[3] ); + } + \sstarguments{ + \sstsubsection{ + vu[3] = double (Given) + }{ + Unrefracted position of the source (Az/El 3-vector) + } + \sstsubsection{ + refa = double (Given) + }{ + tan Z coefficient (radian) + } + \sstsubsection{ + refb = double (Given) + }{ + tan$*$$*$3 Z coefficient (radian) + } + \sstsubsection{ + vr[3] = double (Returned) + }{ + Refracted position of the source (Az/El 3-vector) + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + This routine applies the adjustment for refraction in the + opposite sense to the usual one - it takes an unrefracted + (in vacuo) position and produces an observed (refracted) + position, whereas the A tan Z $+$ B tan$*$$*$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. + + \sstitem + Though optimized for speed rather than precision, the present + routine achieves consistency with the refracted-to-unrefracted + A tan Z $+$ B tan$*$$*$3 Z model at better than 1 microarcsecond within + 30 degrees of the zenith and remains within 1 milliarcsecond to + beyond ZD 70 degrees. The inherent accuracy of the model is, of + course, far worse than this - see the documentation for sla\_REFCO + for more information. + + \sstitem + At low elevations (below about 3 degrees) the refraction + correction is held back to prevent arithmetic problems and + wildly wrong results. For optical/IR wavelengths, over a wide + range of observer heights and corresponding temperatures and + pressures, the following levels of accuracy (arcsec, worst case) + are achieved, relative to numerical integration through a model + atmosphere: + + } + ZD error + + 80 0.7 + 81 1.3 + 82 2.5 + 83 5 + 84 10 + 85 20 + 86 55 + 87 160 + 88 360 + 89 640 + 90 1100 + 91 1700 \} relevant only to + 92 2600 \} high-elevation sites + + The results for radio are slightly worse over most of the range, + becoming significantly worse below ZD=88 and unusable beyond + ZD=90. + + \sstitemlist{ + + \sstitem + See also the routine palRefz, which performs the adjustment to + the zenith distance rather than in Cartesian Az/El coordinates. + The present routine is faster than palRefz and, except very low down, + is equally accurate for all practical purposes. However, beyond + about ZD 84 degrees palRefz should be used, and for the utmost + accuracy iterative use of palRefro should be considered. + } + } +} +\sstroutine{ + palRefz +}{ + Adjust unrefracted zenith distance +}{ + \sstdescription{ + Adjust an unrefracted zenith distance to include the effect of + atmospheric refraction, using the simple A tan Z $+$ B tan$*$$*$3 Z + model (plus special handling for large ZDs). + } + \sstinvocation{ + void palRefz ( double zu, double refa, double refb, double $*$zr ); + } + \sstarguments{ + \sstsubsection{ + zu = double (Given) + }{ + Unrefracted zenith distance of the source (radians) + } + \sstsubsection{ + refa = double (Given) + }{ + tan Z coefficient (radians) + } + \sstsubsection{ + refb = double (Given) + }{ + tan$*$$*$3 Z coefficient (radian) + } + \sstsubsection{ + zr = double $*$ (Returned) + }{ + Refracted zenith distance (radians) + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + This routine applies the adjustment for refraction in the + opposite sense to the usual one - it takes an unrefracted + (in vacuo) position and produces an observed (refracted) + position, whereas the A tan Z $+$ B tan$*$$*$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. + + \sstitem + At ZD 83 degrees, the rapidly-worsening A tan Z $+$ B tan$\wedge$3 Z + model is abandoned and an empirical formula takes over. For + optical/IR wavelengths, over a wide range of observer heights and + corresponding temperatures and pressures, the following levels of + accuracy (arcsec, worst case) are achieved, relative to numerical + integration through a model atmosphere: + + } + ZR error + + 80 0.7 + 81 1.3 + 82 2.4 + 83 4.7 + 84 6.2 + 85 6.4 + 86 8 + 87 10 + 88 15 + 89 30 + 90 60 + 91 150 \} relevant only to + 92 400 \} high-elevation sites + + For radio wavelengths the errors are typically 50\% larger than + the optical figures and by ZD 85 deg are twice as bad, worsening + rapidly below that. To maintain 1 arcsec accuracy down to ZD=85 + at the Green Bank site, Condon (2004) has suggested amplifying + the amount of refraction predicted by palRefz below 10.8 deg + elevation by the factor (1$+$0.00195$*$(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. + + \sstitemlist{ + + \sstitem + Beyond 93 deg zenith distance, the refraction is held at its + 93 deg value. + + \sstitem + See also the routine palRefv, which performs the adjustment in + Cartesian Az/El coordinates, and with the emphasis on speed + rather than numerical accuracy. + } + } + \sstdiytopic{ + References + }{ + Condon,J.J., Refraction Corrections for the GBT, PTCS/PN/35.2, + NRAO Green Bank, 2004. + } +} +\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{ + pv = double [6] (Returned) + }{ + Position (AU) and velocity (AU/s) + } + \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. + } + } +} +\sstroutine{ + palUnpcd +}{ + Remove pincushion/barrel distortion +}{ + \sstdescription{ + Remove pincushion/barrel distortion from a distorted [x,y] to give + tangent-plane [x,y]. + } + \sstinvocation{ + palUnpcd( double disco, double $*$ x, double $*$ y ); + } + \sstarguments{ + \sstsubsection{ + disco = double (Given) + }{ + Pincushion/barrel distortion coefficient. + } + \sstsubsection{ + x = double $*$ (Given \& Returned) + }{ + On input the distorted X coordinate, on output + the tangent-plane X coordinate. + } + \sstsubsection{ + y = double $*$ (Given \& Returned) + }{ + On input the distorted Y coordinate, on output + the tangent-plane Y coordinate. + } + } + \sstnotes{ + \sstitemlist{ + + \sstitem + The distortion is of the form RP = R$*$(1$+$C$*$R$\wedge$2), where R is + the radial distance from the tangent point, C is the DISCO + argument, and RP is the radial distance in the presence of + the distortion. + + \sstitem + For pincushion distortion, C is $+$ve; for barrel distortion, + C is -ve. + + \sstitem + For X,Y in \texttt{"} radians\texttt{"} - units of one projection radius, + which in the case of a photograph is the focal length of + the camera - the following DISCO values apply: + +\begin{center} +\begin{tabular}{ll} + Geometry &DISCO \\ +\hline + astrograph & 0.0 \\ + Schmidt &-0.3333 \\ + AAT PF doublet &$+$147.069 \\ + AAT PF triplet &$+$178.585 \\ + AAT f/8 &$+$21.20 \\ + JKT f/8 &$+$13.32 \\ +\end{tabular} +\end{center} + + } + \sstitemlist{ + + \sstitem + The present routine is a rigorous inverse of the companion + routine palPcd. The expression for RP in Note 1 is rewritten + in the form x$\wedge$3$+$a$*$x$+$b=0 and solved by standard techniques. + + \sstitem + Cases where the cubic has multiple real roots can sometimes + occur, corresponding to extreme instances of barrel distortion + where up to three different undistorted [X,Y]s all produce the + same distorted [X,Y]. However, only one solution is returned, + the one that produces the smallest change in [X,Y]. + } + } + \sstdiytopic{ + See Also + }{ + palPcd + } +} + + + +% ? End of main text +\end{document}