Initial commit

1037 files changed, 146508 insertions, 0 deletions

diff --git a/src/Makefile.Linux.orig b/src/Makefile.Linux.orig
new file mode 100644
index 0000000..1351804
--- /dev/null
+++ b/src/Makefile.Linux.orig
@@ -0,0 +1,138 @@
+
+CALFUSEDIR=	${PWD}/..
+PLATFORM=	ix86_Linux
+SHARED=		-shared
+FITSVER=	2.470
+
+# Symbols for make
+MAKE=		make
+
+#Symbols used for compiling
+CC=		cc
+OPT=		-Wall -g -DCFORTRAN -Dg77Fortran -Df2cFortran
+CFLAGS=		${OPT} -I${CALFUSEDIR}/include
+LIBS=		-lc -lm -lnsl -ldl -lgfortran
+
+all:		lib bin fes jitter
+
+lib:		libcfitsio libsla libfuse
+
+install:	libinstall bininstall analinstall jitinstall # fesinstall
+
+libinstall:	libcfitsioinstall libslainstall libfuseinstall
+
+clean:		binclean fesclean analclean libclean jitclean
+
+distclean:	bindistclean fesdistclean analdistclean libdistclean jitdistclean
+
+libclean:	libcfitsioclean libslaclean libfuseclean
+
+libdistclean:	libcfitsiodistclean libsladistclean libfusedistclean
+
+cfitsio/Makefile:
+		cd cfitsio; CC="${CC}"; export CC; ./configure;
+
+libcfitsio.so:
+		cd cfitsio; /bin/rm -f libcfitsio-${FITSVER}.so
+
+libcfitsio:	cfitsio/Makefile
+		cd cfitsio; ${MAKE} CFLAGS="${OPT}"; \
+		${CC} ${SHARED} -o libcfitsio-${FITSVER}.so *.o ${LIBS}
+
+libsla:		
+		SYSTEM="${PLATFORM}"; export SYSTEM; \
+		FFLAGS="${OPT}"; export FFLAGS; \
+		cd slalib; ./mk build; ${CC} ${SHARED} -o libsla.so *.o ${LIBS}
+
+libfuse:
+		cd libcf; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" FITSVER=${FITSVER} all
+
+bin:
+		cd fuv; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" FITSVER=${FITSVER} all
+
+fes:
+		cd fes; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" FITSVER=${FITSVER} all
+
+analysis:
+		cd analysis; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" FITSVER=${FITSVER} all
+
+jitter:
+		cd cal/jitter; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" FITSVER=${FITSVER} all
+
+libcfitsioinstall: libcfitsio
+		cd cfitsio; cp libcfitsio-${FITSVER}.so ${CALFUSEDIR}/lib
+
+libslainstall:	libsla
+		cd slalib; cp libsla.so ${CALFUSEDIR}/lib
+
+libfuseinstall:	libfuse
+		cd libcf; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" install
+
+bininstall:	bin
+		cd fuv; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" install
+
+fesinstall:	fes
+		cd fes; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" install
+
+analinstall:	analysis
+		cd analysis; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" install
+
+jitinstall:	jitter
+		cd cal/jitter; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" install
+
+libcfitsioclean:
+	-	cd cfitsio; ${MAKE} clean; /bin/rm -f libcfitsio-${FITSVER}.so
+
+libcfitsiodistclean:
+	-	cd cfitsio; ${MAKE} distclean; /bin/rm -f libcfitsio-${FITSVER}.so
+		cd ../lib; /bin/rm -f libcfitsio-${FITSVER}.so
+
+libslaclean:
+	-	SYSTEM="${PLATFORM}"; export SYSTEM; \
+		cd slalib; ./mk clean; /bin/rm -f libsla.a libsla.so
+
+libsladistclean:
+	-	SYSTEM="${PLATFORM}"; export SYSTEM; \
+		cd slalib; ./mk unbuild
+		cd ../lib; /bin/rm -f libsla.so
+
+libfuseclean:
+		cd libcf; ${MAKE} clean
+
+libfusedistclean:
+		cd libcf; ${MAKE} distclean
+
+binclean:
+		cd fuv; ${MAKE} clean
+
+bindistclean:
+		cd fuv; ${MAKE} distclean
+
+fesclean:
+		cd fes; ${MAKE} clean
+
+fesdistclean:
+		cd fes; ${MAKE} distclean
+
+analclean:
+		cd analysis; ${MAKE} clean
+
+analdistclean:
+		cd analysis; ${MAKE} distclean
+
+jitclean:
+		cd cal/jitter; ${MAKE} clean
+
+jitdistclean:
+		cd cal/jitter; ${MAKE} distclean
+
diff --git a/src/Makefile.Linux64.orig b/src/Makefile.Linux64.orig
new file mode 100644
index 0000000..6c498d9
--- /dev/null
+++ b/src/Makefile.Linux64.orig
@@ -0,0 +1,113 @@
+
+CALFUSEDIR=	${PWD}/..
+PLATFORM=	x86_64
+SHARED=		-shared -fPIC
+
+# Symbols for make
+MAKE=		make
+
+#Symbols used for compiling
+CC=		gcc
+OPT=		-Wall -g -DCFORTRAN -Dg77Fortran -Df2cFortran
+CFLAGS=		${OPT} -I${CALFUSEDIR}/include
+LIBS=		-lc -lm -lnsl -ldl -lgfortran -lcfitsio
+
+install:	libinstall bininstall analinstall jitinstall # fesinstall
+
+libinstall:	libslainstall libfuseinstall
+
+clean:		binclean fesclean analclean libclean jitclean
+
+distclean:	bindistclean fesdistclean analdistclean libdistclean jitdistclean
+
+libclean:	libslaclean libfuseclean
+
+libdistclean:	libsladistclean libfusedistclean
+
+libsla:		
+		SYSTEM="${PLATFORM}"; export SYSTEM; \
+		FFLAGS="${OPT}"; export FFLAGS; \
+		cd slalib; ./mk build; ${CC} ${SHARED} -o libsla.so *.o ${LIBS}
+
+libfuse:
+		cd libcf; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT} ${SHARED}" all
+
+bin:
+		cd fuv; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" all
+
+fes:
+		cd fes; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" all
+
+analysis:
+		cd analysis; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" all
+
+jitter:
+		cd cal/jitter; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" all
+
+libslainstall:	libsla
+		cd slalib; cp libsla.so ${CALFUSEDIR}/lib
+
+libfuseinstall:	libfuse
+		cd libcf; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" install
+
+bininstall:	bin
+		cd fuv; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" install
+
+fesinstall:	fes
+		cd fes; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" install
+
+analinstall:	analysis
+		cd analysis; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" install
+
+jitinstall:	jitter
+		cd cal/jitter; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" install
+
+libslaclean:
+	-	SYSTEM="${PLATFORM}"; export SYSTEM; \
+		cd slalib; ./mk clean; /bin/rm -f libsla.a libsla.so
+
+libsladistclean:
+	-	SYSTEM="${PLATFORM}"; export SYSTEM; \
+		cd slalib; ./mk unbuild
+		cd ../lib; /bin/rm -f libsla.so
+
+libfuseclean:
+		cd libcf; ${MAKE} clean
+
+libfusedistclean:
+		cd libcf; ${MAKE} distclean
+
+binclean:
+		cd fuv; ${MAKE} clean
+
+bindistclean:
+		cd fuv; ${MAKE} distclean
+
+fesclean:
+		cd fes; ${MAKE} clean
+
+fesdistclean:
+		cd fes; ${MAKE} distclean
+
+analclean:
+		cd analysis; ${MAKE} clean
+
+analdistclean:
+		cd analysis; ${MAKE} distclean
+
+jitclean:
+		cd cal/jitter; ${MAKE} clean
+
+jitdistclean:
+		cd cal/jitter; ${MAKE} distclean
+
diff --git a/src/Makefile.MacOSX.orig b/src/Makefile.MacOSX.orig
new file mode 100644
index 0000000..6bfae3e
--- /dev/null
+++ b/src/Makefile.MacOSX.orig
@@ -0,0 +1,143 @@
+
+# Master Makefile for Mac OS X Version 10.2 or higher
+# Slalib installation requires the command "make -e install"
+# Leave PLATFORM = ix86_Linux; required by slalib.
+# FITSVER is not used; library is always called libcfitsio.dylib.
+
+CALFUSEDIR=	${PWD}/..
+PLATFORM=       ix86_Linux
+SHARED=         -dynamiclib
+FITSVER=	2.470
+MACOSX_DEPLOYMENT_TARGET=	10.2
+
+# Symbols for make
+MAKE=		make
+
+#Symbols used for compiling
+CC=		cc
+OPT=		-O3 -Wall -DCFORTRAN -Dg77Fortran -Df2cFortran
+CFLAGS=		${OPT} -I${CALFUSEDIR}/include
+LIBS=		-L/sw/lib/ -lgfortran
+
+all:		lib bin fes jitter
+
+lib:		libcfitsio libsla libfuse
+
+install:	libinstall bininstall analinstall jitinstall # fesinstall
+
+libinstall:	libcfitsioinstall libslainstall libfuseinstall
+
+clean:		binclean fesclean analclean libclean jitclean
+
+distclean:	bindistclean fesdistclean analdistclean libdistclean jitdistclean
+
+libclean:	libcfitsioclean libslaclean libfuseclean
+
+libdistclean:	libcfitsiodistclean libsladistclean libfusedistclean
+
+cfitsio/Makefile:
+		cd cfitsio; CC="${CC}"; export CC; ./configure;
+
+libcfitsio:	cfitsio/Makefile
+		cd cfitsio; ${MAKE} shared
+
+libsla:		
+	-	SYSTEM="${PLATFORM}"; export SYSTEM; \
+		cd slalib; ./mk build; \
+		${CC} ${SHARED} -o libsla.dylib *.o ${LIBS}
+
+libfuse:
+		cd libcf; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" FITSVER=${FITSVER} all
+
+bin:
+		MACOSX_DEPLOYMENT_TARGET="${MACOSX_DEPLOYMENT_TARGET}"; \
+		export MACOSX_DEPLOYMENT_TARGET; \
+		cd fuv; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" FITSVER=${FITSVER} all
+
+fes:
+		cd fes; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" FITSVER=${FITSVER} all
+
+analysis:
+		cd analysis; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" FITSVER=${FITSVER} all
+
+jitter:
+		cd cal/jitter; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" FITSVER=${FITSVER} all
+
+libcfitsioinstall: libcfitsio
+		cd cfitsio; cp libcfitsio.dylib ${CALFUSEDIR}/lib
+
+libslainstall:	libsla
+		cd slalib; cp libsla.dylib ${CALFUSEDIR}/lib
+
+libfuseinstall:	libfuse
+		cd libcf; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" install
+
+bininstall:	bin
+		cd fuv; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" install
+
+fesinstall:	fes
+		cd fes; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" install
+
+analinstall:	analysis
+		cd analysis; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" install
+
+jitinstall:	jitter
+		cd cal/jitter; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" install
+
+libcfitsioclean:
+	-	cd cfitsio; ${MAKE} clean; /bin/rm -f libcfitsio.dylib
+
+libcfitsiodistclean:
+	-	cd cfitsio; ${MAKE} distclean; /bin/rm -f libcfitsio.dylib
+		/bin/rm -f ../lib/libcfitsio.dylib
+		# cd ../lib; /bin/rm libcfitsio-${FITSVER}.dylib
+
+libslaclean:
+	-	SYSTEM="${PLATFORM}"; export SYSTEM; \
+		cd slalib; ./mk clean; /bin/rm -f libsla.a libsla.dylib
+
+libsladistclean:
+	-	SYSTEM="${PLATFORM}"; export SYSTEM; \
+		cd slalib; ./mk unbuild
+		cd ../lib; /bin/rm -f libsla.dylib
+
+libfuseclean:
+		cd libcf; ${MAKE} clean
+
+libfusedistclean:
+		cd libcf; ${MAKE} distclean
+
+binclean:
+		cd fuv; ${MAKE} clean
+
+bindistclean:
+		cd fuv; ${MAKE} distclean
+
+fesclean:
+		cd fes; ${MAKE} clean
+
+fesdistclean:
+		cd fes; ${MAKE} distclean
+
+analclean:
+		cd analysis; ${MAKE} clean
+
+analdistclean:
+		cd analysis; ${MAKE} distclean
+
+jitclean:
+		cd cal/jitter; ${MAKE} clean
+
+jitdistclean:
+		cd cal/jitter; ${MAKE} distclean
+
diff --git a/src/Makefile.Solaris.orig b/src/Makefile.Solaris.orig
new file mode 100644
index 0000000..6661a7d
--- /dev/null
+++ b/src/Makefile.Solaris.orig
@@ -0,0 +1,137 @@
+
+CALFUSEDIR=	${PWD}/..
+PLATFORM=	sun4_Solaris
+SHARED=		-G
+FITSVER=	2.470
+
+# Symbols for make
+MAKE=		make
+
+#Symbols used for compiling
+CC=		cc
+OPT=		-O -DCFORTRAN -KPIC -DSOLARIS
+CFLAGS=		${OPT} -I${CALFUSEDIR}/include
+LIBS=		-lc -lm -lnsl -ldl -lsocket -lsunmath -lM77 -lF77
+
+all:		lib bin fes jitter
+
+lib:		libcfitsio libsla libfuse
+
+install:	libinstall bininstall analinstall jitinstall # fesinstall
+
+libinstall:	libcfitsioinstall libslainstall libfuseinstall
+
+clean:		binclean fesclean analclean libclean jitclean
+
+distclean:	bindistclean fesdistclean analdistclean libdistclean jitdistclean
+
+libclean:	libcfitsioclean libslaclean libfuseclean
+
+libdistclean:	libcfitsiodistclean libsladistclean libfusedistclean
+
+cfitsio/Makefile:
+		cd cfitsio; CC="${CC}"; export CC; ./configure;
+
+libcfitsio.so:
+		cd cfitsio; /bin/rm -f libcfitsio-${FITSVER}.so
+
+libcfitsio:	cfitsio/Makefile
+		cd cfitsio; ${MAKE} CFLAGS="${OPT}"; \
+		${CC} ${SHARED} -o libcfitsio-${FITSVER}.so *.o ${LIBS}
+
+libsla:		
+		SYSTEM="${PLATFORM}"; export SYSTEM; \
+		FFLAGS="${OPT}"; export FFLAGS; \
+		cd slalib; ./mk build; ${CC} ${SHARED} -o libsla.so *.o ${LIBS}
+
+libfuse:
+		cd libcf; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" FITSVER=${FITSVER} all
+
+bin:
+		cd fuv; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" FITSVER=${FITSVER} all
+
+fes:
+		cd fes; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" FITSVER=${FITSVER} all
+
+analysis:
+		cd analysis; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" FITSVER=${FITSVER} all
+
+jitter:
+		cd cal/jitter; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" FITSVER=${FITSVER} all
+
+libcfitsioinstall: libcfitsio
+		cd cfitsio; cp libcfitsio-${FITSVER}.so ${CALFUSEDIR}/lib
+
+libslainstall:	libsla
+		cd slalib; cp libsla.so ${CALFUSEDIR}/lib
+
+libfuseinstall:	libfuse
+		cd libcf; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" install
+
+bininstall:	bin
+		cd fuv; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" install
+
+fesinstall:	fes
+		cd fes; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" install
+
+analinstall:	analysis
+		cd analysis; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" install
+
+jitinstall:	jitter
+		cd cal/jitter; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" install
+
+libcfitsioclean:
+	-	cd cfitsio; ${MAKE} clean; /bin/rm -f libcfitsio-${FITSVER}.so
+
+libcfitsiodistclean:
+	-	cd cfitsio; ${MAKE} distclean; /bin/rm -f libcfitsio-${FITSVER}.so
+		cd ../lib; /bin/rm -f libcfitsio-${FITSVER}.so
+
+libslaclean:
+	-	SYSTEM="${PLATFORM}"; export SYSTEM; \
+		cd slalib; ./mk clean; /bin/rm -f libsla.a libsla.so
+
+libsladistclean:
+	-	SYSTEM="${PLATFORM}"; export SYSTEM; \
+		cd slalib; ./mk unbuild
+		cd ../lib; /bin/rm -f libsla.so
+
+libfuseclean:
+		cd libcf; ${MAKE} clean
+
+libfusedistclean:
+		cd libcf; ${MAKE} distclean
+
+binclean:
+		cd fuv; ${MAKE} clean
+
+bindistclean:
+		cd fuv; ${MAKE} distclean
+
+fesclean:
+		cd fes; ${MAKE} clean
+
+fesdistclean:
+		cd fes; ${MAKE} distclean
+
+analclean:
+		cd analysis; ${MAKE} clean
+
+analdistclean:
+		cd analysis; ${MAKE} distclean
+
+jitclean:
+		cd cal/jitter; ${MAKE} clean
+
+jitdistclean:
+		cd cal/jitter; ${MAKE} distclean
diff --git a/src/Makefile.am b/src/Makefile.am
new file mode 100644
index 0000000..7a3bd69
--- /dev/null
+++ b/src/Makefile.am
@@ -0,0 +1 @@
+SUBDIRS = slalib
diff --git a/src/Makefile.in b/src/Makefile.in
new file mode 100644
index 0000000..b58841d
--- /dev/null
+++ b/src/Makefile.in
@@ -0,0 +1,619 @@
+# Makefile.in generated by automake 1.15 from Makefile.am.
+# @configure_input@
+
+# Copyright (C) 1994-2014 Free Software Foundation, Inc.
+
+# This Makefile.in is free software; the Free Software Foundation
+# gives unlimited permission to copy and/or distribute it,
+# with or without modifications, as long as this notice is preserved.
+
+# This program is distributed in the hope that it will be useful,
+# but WITHOUT ANY WARRANTY, to the extent permitted by law; without
+# even the implied warranty of MERCHANTABILITY or FITNESS FOR A
+# PARTICULAR PURPOSE.
+
+@SET_MAKE@
+VPATH = @srcdir@
+am__is_gnu_make = { \
+  if test -z '$(MAKELEVEL)'; then \
+    false; \
+  elif test -n '$(MAKE_HOST)'; then \
+    true; \
+  elif test -n '$(MAKE_VERSION)' && test -n '$(CURDIR)'; then \
+    true; \
+  else \
+    false; \
+  fi; \
+}
+am__make_running_with_option = \
+  case $${target_option-} in \
+      ?) ;; \
+      *) echo "am__make_running_with_option: internal error: invalid" \
+              "target option '$${target_option-}' specified" >&2; \
+         exit 1;; \
+  esac; \
+  has_opt=no; \
+  sane_makeflags=$$MAKEFLAGS; \
+  if $(am__is_gnu_make); then \
+    sane_makeflags=$$MFLAGS; \
+  else \
+    case $$MAKEFLAGS in \
+      *\\[\ \	]*) \
+        bs=\\; \
+        sane_makeflags=`printf '%s\n' "$$MAKEFLAGS" \
+          | sed "s/$$bs$$bs[$$bs $$bs	]*//g"`;; \
+    esac; \
+  fi; \
+  skip_next=no; \
+  strip_trailopt () \
+  { \
+    flg=`printf '%s\n' "$$flg" | sed "s/$$1.*$$//"`; \
+  }; \
+  for flg in $$sane_makeflags; do \
+    test $$skip_next = yes && { skip_next=no; continue; }; \
+    case $$flg in \
+      *=*|--*) continue;; \
+        -*I) strip_trailopt 'I'; skip_next=yes;; \
+      -*I?*) strip_trailopt 'I';; \
+        -*O) strip_trailopt 'O'; skip_next=yes;; \
+      -*O?*) strip_trailopt 'O';; \
+        -*l) strip_trailopt 'l'; skip_next=yes;; \
+      -*l?*) strip_trailopt 'l';; \
+      -[dEDm]) skip_next=yes;; \
+      -[JT]) skip_next=yes;; \
+    esac; \
+    case $$flg in \
+      *$$target_option*) has_opt=yes; break;; \
+    esac; \
+  done; \
+  test $$has_opt = yes
+am__make_dryrun = (target_option=n; $(am__make_running_with_option))
+am__make_keepgoing = (target_option=k; $(am__make_running_with_option))
+pkgdatadir = $(datadir)/@PACKAGE@
+pkgincludedir = $(includedir)/@PACKAGE@
+pkglibdir = $(libdir)/@PACKAGE@
+pkglibexecdir = $(libexecdir)/@PACKAGE@
+am__cd = CDPATH="$${ZSH_VERSION+.}$(PATH_SEPARATOR)" && cd
+install_sh_DATA = $(install_sh) -c -m 644
+install_sh_PROGRAM = $(install_sh) -c
+install_sh_SCRIPT = $(install_sh) -c
+INSTALL_HEADER = $(INSTALL_DATA)
+transform = $(program_transform_name)
+NORMAL_INSTALL = :
+PRE_INSTALL = :
+POST_INSTALL = :
+NORMAL_UNINSTALL = :
+PRE_UNINSTALL = :
+POST_UNINSTALL = :
+build_triplet = @build@
+host_triplet = @host@
+subdir = src
+ACLOCAL_M4 = $(top_srcdir)/aclocal.m4
+am__aclocal_m4_deps = $(top_srcdir)/m4/libtool.m4 \
+	$(top_srcdir)/m4/ltoptions.m4 $(top_srcdir)/m4/ltsugar.m4 \
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diff --git a/src/Makefile.orig.orig b/src/Makefile.orig.orig
new file mode 100644
index 0000000..6661a7d
--- /dev/null
+++ b/src/Makefile.orig.orig
@@ -0,0 +1,137 @@
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+PLATFORM=	sun4_Solaris
+SHARED=		-G
+FITSVER=	2.470
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+# Symbols for make
+MAKE=		make
+
+#Symbols used for compiling
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+lib:		libcfitsio libsla libfuse
+
+install:	libinstall bininstall analinstall jitinstall # fesinstall
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+libinstall:	libcfitsioinstall libslainstall libfuseinstall
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+libdistclean:	libcfitsiodistclean libsladistclean libfusedistclean
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+
+libcfitsio:	cfitsio/Makefile
+		cd cfitsio; ${MAKE} CFLAGS="${OPT}"; \
+		${CC} ${SHARED} -o libcfitsio-${FITSVER}.so *.o ${LIBS}
+
+libsla:		
+		SYSTEM="${PLATFORM}"; export SYSTEM; \
+		FFLAGS="${OPT}"; export FFLAGS; \
+		cd slalib; ./mk build; ${CC} ${SHARED} -o libsla.so *.o ${LIBS}
+
+libfuse:
+		cd libcf; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" FITSVER=${FITSVER} all
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+bin:
+		cd fuv; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" FITSVER=${FITSVER} all
+
+fes:
+		cd fes; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" FITSVER=${FITSVER} all
+
+analysis:
+		cd analysis; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" FITSVER=${FITSVER} all
+
+jitter:
+		cd cal/jitter; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" FITSVER=${FITSVER} all
+
+libcfitsioinstall: libcfitsio
+		cd cfitsio; cp libcfitsio-${FITSVER}.so ${CALFUSEDIR}/lib
+
+libslainstall:	libsla
+		cd slalib; cp libsla.so ${CALFUSEDIR}/lib
+
+libfuseinstall:	libfuse
+		cd libcf; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" install
+
+bininstall:	bin
+		cd fuv; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" install
+
+fesinstall:	fes
+		cd fes; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" install
+
+analinstall:	analysis
+		cd analysis; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" install
+
+jitinstall:	jitter
+		cd cal/jitter; ${MAKE} CALFUSEDIR="${CALFUSEDIR}" \
+		CC="${CC}" OPT="${OPT}" install
+
+libcfitsioclean:
+	-	cd cfitsio; ${MAKE} clean; /bin/rm -f libcfitsio-${FITSVER}.so
+
+libcfitsiodistclean:
+	-	cd cfitsio; ${MAKE} distclean; /bin/rm -f libcfitsio-${FITSVER}.so
+		cd ../lib; /bin/rm -f libcfitsio-${FITSVER}.so
+
+libslaclean:
+	-	SYSTEM="${PLATFORM}"; export SYSTEM; \
+		cd slalib; ./mk clean; /bin/rm -f libsla.a libsla.so
+
+libsladistclean:
+	-	SYSTEM="${PLATFORM}"; export SYSTEM; \
+		cd slalib; ./mk unbuild
+		cd ../lib; /bin/rm -f libsla.so
+
+libfuseclean:
+		cd libcf; ${MAKE} clean
+
+libfusedistclean:
+		cd libcf; ${MAKE} distclean
+
+binclean:
+		cd fuv; ${MAKE} clean
+
+bindistclean:
+		cd fuv; ${MAKE} distclean
+
+fesclean:
+		cd fes; ${MAKE} clean
+
+fesdistclean:
+		cd fes; ${MAKE} distclean
+
+analclean:
+		cd analysis; ${MAKE} clean
+
+analdistclean:
+		cd analysis; ${MAKE} distclean
+
+jitclean:
+		cd cal/jitter; ${MAKE} clean
+
+jitdistclean:
+		cd cal/jitter; ${MAKE} distclean
diff --git a/src/analysis/Makefile.Linux.orig b/src/analysis/Makefile.Linux.orig
new file mode 100644
index 0000000..b1786ef
--- /dev/null
+++ b/src/analysis/Makefile.Linux.orig
@@ -0,0 +1,142 @@
+
+FITSVER=	2.470
+CALFUSEDIR=	${PWD}/../..
+
+# Symbols for include directories
+FUSEINCLDIR=	-I${CALFUSEDIR}/include
+
+# Symbols used for compiling
+CC=		cc
+OPT=		-g -Wall -DCFORTRAN -Dg77Fortran -Df2cFortran
+CFLAGS=		${OPT} ${FUSEINCLDIR}
+
+# Symbols used for creating shared binaries
+FUSEBINDIR=	${CALFUSEDIR}/bin
+FUSELIBDIR=	-L${CALFUSEDIR}/lib
+LIBDIR=		-L/opt/SUNWspro/lib
+FUSELIBS=	-lsla -lcfitsio-${FITSVER} -lcf
+LIBS=		-lc -lm -lnsl -ldl -lgfortran
+LDFLAGS=	-Wl,-R${CALFUSEDIR}/lib
+
+# Binaries to be made
+
+BINS=		cf_ttag_to_hist get_shift mjd2hjd cf_reflux \
+		idf_screen extract_jitter modhead \
+		cf_arith cf_combine cf_nvo cf_pack cf_xcorr \
+		idf_combine bpm_combine ttag_combine \
+		cf_coadd cf_make_all_exp \
+                remove_target_orbital_motion idf_cut \
+		ttag_lightcurve \
+		ttag_lightcurve_channel_sum \
+		ttag_lightcurve_mjd2hmjd \
+		ttag_lightcurve_combine \
+		ttag_lightcurve_periodogram 
+
+all:		${BINS}
+		chmod g+rw ${BINS}
+
+install:	all
+		/bin/cp ${BINS} cf_make_all_obs.csh cf_make_900_obs.csh ${FUSEBINDIR}
+
+clean:
+		/bin/rm -f *.o ${BINS}
+
+distclean:
+		/bin/rm -f *.o ${BINS}
+		cd ../../bin; /bin/rm -f ${BINS}
+
+cf_arith: cf_arith.c cf_wrspec7.c cf_wrspec_cf2.c
+		${CC} ${CFLAGS} -o cf_arith cf_arith.c cf_wrspec7.c cf_wrspec_cf2.c\
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_coadd: cf_coadd.c
+		${CC} ${CFLAGS} -o cf_coadd cf_coadd.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_combine: cf_combine.c cf_wrspec7.c
+		${CC} ${CFLAGS} -o cf_combine cf_combine.c cf_wrspec7.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_make_all_exp:
+		${CC} ${CFLAGS} -o cf_make_all_exp cf_make_all_exp.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_ttag_to_hist:
+		${CC} ${CFLAGS} -o cf_ttag_to_hist cf_ttag_to_hist.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_combine:
+		${CC} ${CFLAGS} -o ttag_combine ttag_combine.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+idf_combine:
+		${CC} ${CFLAGS} -o idf_combine idf_combine.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+bpm_combine:
+		${CC} ${CFLAGS} -o bpm_combine bpm_combine.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+get_shift:
+		${CC} ${CFLAGS} -o get_shift get_shift.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_pack:
+		${CC} ${CFLAGS} -o cf_pack cf_pack.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_nvo:
+		${CC} ${CFLAGS} -o cf_nvo cf_nvo.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_reflux:
+		${CC} ${CFLAGS} -o cf_reflux cf_reflux.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_xcorr:
+		${CC} ${CFLAGS} -o cf_xcorr cf_xcorr.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+modhead:
+		${CC} ${CFLAGS} -o modhead modhead.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_lightcurve:
+		${CC} ${CFLAGS} -o ttag_lightcurve ttag_lightcurve.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_lightcurve_periodogram:
+		${CC} ${CFLAGS} -o ttag_lightcurve_periodogram ttag_lightcurve_periodogram.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+mjd2hjd: mjd2hjd.c gethmjd.c
+		${CC} ${CFLAGS} -o mjd2hjd mjd2hjd.c gethmjd.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_lightcurve_channel_sum:
+		${CC} ${CFLAGS} -o ttag_lightcurve_channel_sum ttag_lightcurve_channel_sum.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_lightcurve_mjd2hmjd : ttag_lightcurve_mjd2hmjd.c gethmjd.c
+		${CC} ${CFLAGS} -o ttag_lightcurve_mjd2hmjd ttag_lightcurve_mjd2hmjd.c gethmjd.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_lightcurve_combine:
+		${CC} ${CFLAGS} -o ttag_lightcurve_combine ttag_lightcurve_combine.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+idf_screen:
+		${CC} ${CFLAGS} -o idf_screen idf_screen.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+remove_target_orbital_motion: remove_target_orbital_motion.c gethmjd.c
+		${CC} ${CFLAGS} -o remove_target_orbital_motion remove_target_orbital_motion.c gethmjd.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+idf_cut:
+		${CC} ${CFLAGS} -o idf_cut idf_cut.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+extract_jitter:
+		${CC} ${CFLAGS} -o extract_jitter extract_jitter.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
diff --git a/src/analysis/Makefile.Linux64.orig b/src/analysis/Makefile.Linux64.orig
new file mode 100644
index 0000000..2ef8094
--- /dev/null
+++ b/src/analysis/Makefile.Linux64.orig
@@ -0,0 +1,141 @@
+
+CALFUSEDIR=	${PWD}/../..
+
+# Symbols for include directories
+FUSEINCLDIR=	-I${CALFUSEDIR}/include
+
+# Symbols used for compiling
+CC=		cc
+OPT=		-g -Wall -DCFORTRAN -Dg77Fortran -Df2cFortran
+CFLAGS=		${OPT} ${FUSEINCLDIR}
+
+# Symbols used for creating shared binaries
+FUSEBINDIR=	${CALFUSEDIR}/bin
+FUSELIBDIR=	-L${CALFUSEDIR}/lib
+LIBDIR=		-L/opt/SUNWspro/lib
+FUSELIBS=	-lsla -lcf
+LIBS=		-lc -lm -lnsl -ldl -lgfortran -lcfitsio
+LDFLAGS=	-Wl,-R${CALFUSEDIR}/lib
+
+# Binaries to be made
+
+BINS=		cf_ttag_to_hist get_shift mjd2hjd cf_reflux \
+		idf_screen extract_jitter modhead \
+		cf_arith cf_combine cf_nvo cf_pack cf_xcorr \
+		idf_combine bpm_combine ttag_combine \
+		cf_coadd cf_make_all_exp \
+                remove_target_orbital_motion idf_cut \
+		ttag_lightcurve \
+		ttag_lightcurve_channel_sum \
+		ttag_lightcurve_mjd2hmjd \
+		ttag_lightcurve_combine \
+		ttag_lightcurve_periodogram 
+
+all:		${BINS}
+		chmod g+rw ${BINS}
+
+install:	all
+		/bin/cp ${BINS} cf_make_all_obs.csh cf_make_900_obs.csh ${FUSEBINDIR}
+
+clean:
+		/bin/rm -f *.o ${BINS}
+
+distclean:
+		/bin/rm -f *.o ${BINS}
+		cd ../../bin; /bin/rm -f ${BINS}
+
+cf_arith: cf_arith.c cf_wrspec7.c cf_wrspec_cf2.c
+		${CC} ${CFLAGS} -o cf_arith cf_arith.c cf_wrspec7.c cf_wrspec_cf2.c\
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_coadd: cf_coadd.c
+		${CC} ${CFLAGS} -o cf_coadd cf_coadd.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_combine: cf_combine.c cf_wrspec7.c
+		${CC} ${CFLAGS} -o cf_combine cf_combine.c cf_wrspec7.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_make_all_exp:
+		${CC} ${CFLAGS} -o cf_make_all_exp cf_make_all_exp.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_ttag_to_hist:
+		${CC} ${CFLAGS} -o cf_ttag_to_hist cf_ttag_to_hist.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_combine:
+		${CC} ${CFLAGS} -o ttag_combine ttag_combine.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+idf_combine:
+		${CC} ${CFLAGS} -o idf_combine idf_combine.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+bpm_combine:
+		${CC} ${CFLAGS} -o bpm_combine bpm_combine.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+get_shift:
+		${CC} ${CFLAGS} -o get_shift get_shift.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_pack:
+		${CC} ${CFLAGS} -o cf_pack cf_pack.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_nvo:
+		${CC} ${CFLAGS} -o cf_nvo cf_nvo.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_reflux:
+		${CC} ${CFLAGS} -o cf_reflux cf_reflux.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_xcorr:
+		${CC} ${CFLAGS} -o cf_xcorr cf_xcorr.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+modhead:
+		${CC} ${CFLAGS} -o modhead modhead.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_lightcurve:
+		${CC} ${CFLAGS} -o ttag_lightcurve ttag_lightcurve.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_lightcurve_periodogram:
+		${CC} ${CFLAGS} -o ttag_lightcurve_periodogram ttag_lightcurve_periodogram.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+mjd2hjd: mjd2hjd.c gethmjd.c
+		${CC} ${CFLAGS} -o mjd2hjd mjd2hjd.c gethmjd.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_lightcurve_channel_sum:
+		${CC} ${CFLAGS} -o ttag_lightcurve_channel_sum ttag_lightcurve_channel_sum.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_lightcurve_mjd2hmjd : ttag_lightcurve_mjd2hmjd.c gethmjd.c
+		${CC} ${CFLAGS} -o ttag_lightcurve_mjd2hmjd ttag_lightcurve_mjd2hmjd.c gethmjd.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_lightcurve_combine:
+		${CC} ${CFLAGS} -o ttag_lightcurve_combine ttag_lightcurve_combine.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+idf_screen:
+		${CC} ${CFLAGS} -o idf_screen idf_screen.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+remove_target_orbital_motion: remove_target_orbital_motion.c gethmjd.c
+		${CC} ${CFLAGS} -o remove_target_orbital_motion remove_target_orbital_motion.c gethmjd.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+idf_cut:
+		${CC} ${CFLAGS} -o idf_cut idf_cut.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+extract_jitter:
+		${CC} ${CFLAGS} -o extract_jitter extract_jitter.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
diff --git a/src/analysis/Makefile.MacOSX.orig b/src/analysis/Makefile.MacOSX.orig
new file mode 100644
index 0000000..5e40b35
--- /dev/null
+++ b/src/analysis/Makefile.MacOSX.orig
@@ -0,0 +1,145 @@
+
+FITSVER=	2.470
+CALFUSEDIR=	${PWD}/../..
+MACOSX_DEPLOYMENT_TARGET=	10.2
+
+# Symbols for include directories
+FUSEINCLDIR=	-I${CALFUSEDIR}/include
+
+# Symbols used for compiling
+CC=		cc
+OPT=		-O3 -Wall -DCFORTRAN -Dg77Fortran -Df2cFortran
+CFLAGS=		${OPT} ${FUSEINCLDIR}
+
+# Symbols used for creating shared binaries
+FUSEBINDIR=	${CALFUSEDIR}/bin
+FUSELIBDIR=	-L${CALFUSEDIR}/lib
+# FUSELIBS=	-lsla -lcfitsio-${FITSVER} -lcf
+FUSELIBS=	-lsla -lcfitsio -lcf
+LIBS=		-lc -lm -ldl -L/sw/lib/ -lgfortran
+
+# Binaries to be made
+
+BINS=		cf_ttag_to_hist get_shift mjd2hjd cf_reflux \
+		idf_screen extract_jitter modhead \
+		cf_arith cf_combine cf_nvo cf_pack cf_xcorr \
+		idf_combine bpm_combine ttag_combine \
+		cf_coadd cf_make_all_exp \
+                remove_target_orbital_motion idf_cut \
+		ttag_lightcurve \
+		ttag_lightcurve_channel_sum \
+		ttag_lightcurve_mjd2hmjd \
+		ttag_lightcurve_combine \
+		ttag_lightcurve_periodogram 
+
+all:		${BINS}
+		chmod g+rw ${BINS}
+
+install:
+		MACOSX_DEPLOYMENT_TARGET="${MACOSX_DEPLOYMENT_TARGET}"; \
+		export MACOSX_DEPLOYMENT_TARGET; \
+		make all
+		/bin/cp ${BINS} cf_make_all_obs.csh cf_make_900_obs.csh ${FUSEBINDIR}
+
+clean:
+		/bin/rm -f *.o ${BINS}
+
+distclean:
+		/bin/rm -f *.o ${BINS}
+		cd ../../bin; /bin/rm -f ${BINS}
+
+cf_arith: cf_arith.c cf_wrspec7.c cf_wrspec_cf2.c
+		${CC} ${CFLAGS} -o cf_arith cf_arith.c cf_wrspec7.c cf_wrspec_cf2.c\
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_coadd: cf_coadd.c
+		${CC} ${CFLAGS} -o cf_coadd cf_coadd.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_combine: cf_combine.c cf_wrspec7.c
+		${CC} ${CFLAGS} -o cf_combine cf_combine.c cf_wrspec7.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_make_all_exp:
+		${CC} ${CFLAGS} -o cf_make_all_exp cf_make_all_exp.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_ttag_to_hist:
+		${CC} ${CFLAGS} -o cf_ttag_to_hist cf_ttag_to_hist.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_combine:
+		${CC} ${CFLAGS} -o ttag_combine ttag_combine.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+idf_combine:
+		${CC} ${CFLAGS} -o idf_combine idf_combine.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+bpm_combine:
+		${CC} ${CFLAGS} -o bpm_combine bpm_combine.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+get_shift:
+		${CC} ${CFLAGS} -o get_shift get_shift.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_pack:
+		${CC} ${CFLAGS} -o cf_pack cf_pack.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_nvo:
+		${CC} ${CFLAGS} -o cf_nvo cf_nvo.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_reflux:
+		${CC} ${CFLAGS} -o cf_reflux cf_reflux.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_xcorr:
+		${CC} ${CFLAGS} -o cf_xcorr cf_xcorr.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+modhead:
+		${CC} ${CFLAGS} -o modhead modhead.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_lightcurve:
+		${CC} ${CFLAGS} -o ttag_lightcurve ttag_lightcurve.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_lightcurve_periodogram:
+		${CC} ${CFLAGS} -o ttag_lightcurve_periodogram ttag_lightcurve_periodogram.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+mjd2hjd: mjd2hjd.c gethmjd.c
+		${CC} ${CFLAGS} -o mjd2hjd mjd2hjd.c gethmjd.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_lightcurve_channel_sum:
+		${CC} ${CFLAGS} -o ttag_lightcurve_channel_sum ttag_lightcurve_channel_sum.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_lightcurve_mjd2hmjd : ttag_lightcurve_mjd2hmjd.c gethmjd.c
+		${CC} ${CFLAGS} -o ttag_lightcurve_mjd2hmjd ttag_lightcurve_mjd2hmjd.c gethmjd.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_lightcurve_combine:
+		${CC} ${CFLAGS} -o ttag_lightcurve_combine ttag_lightcurve_combine.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+idf_screen:
+		${CC} ${CFLAGS} -o idf_screen idf_screen.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+remove_target_orbital_motion: remove_target_orbital_motion.c gethmjd.c
+		${CC} ${CFLAGS} -o remove_target_orbital_motion remove_target_orbital_motion.c gethmjd.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+idf_cut:
+		${CC} ${CFLAGS} -o idf_cut idf_cut.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+extract_jitter:
+		${CC} ${CFLAGS} -o extract_jitter extract_jitter.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
diff --git a/src/analysis/Makefile.Solaris.orig b/src/analysis/Makefile.Solaris.orig
new file mode 100644
index 0000000..52fb31b
--- /dev/null
+++ b/src/analysis/Makefile.Solaris.orig
@@ -0,0 +1,147 @@
+
+FITSVER=	2.470
+CALFUSEDIR=	${PWD}/../..
+
+# Symbols for include directories
+FUSEINCLDIR=	-I${CALFUSEDIR}/include
+
+# Symbols used for compiling
+CC=		cc
+#  Romelfanger's optimizations
+# OPT=		-fast -xO5 -xtarget=ultra2 -xarch=v8plusa
+#
+#  SunWorld's optimizations
+# OPT=		-p -v -xO2 -xdepend -xchip=ultra -xarch=generic
+OPT=		-O -DCFORTRAN -KPIC -DSOLARIS
+CFLAGS=		${OPT} ${FUSEINCLDIR}
+
+# Symbols used for creating shared binaries
+FUSEBINDIR=	${CALFUSEDIR}/bin
+FUSELIBDIR=	-L${CALFUSEDIR}/lib
+LIBDIR=		-L/opt/SUNWspro/lib
+FUSELIBS=	-lsla -lcfitsio-${FITSVER} -lcf
+LIBS=		-lc -lm -lnsl -ldl -lsocket -lsunmath -lM77 -lF77
+LDFLAGS=	-Wl,-R${CALFUSEDIR}/lib
+
+# Binaries to be made
+
+BINS=		cf_ttag_to_hist get_shift mjd2hjd cf_reflux \
+		idf_screen extract_jitter modhead \
+		cf_arith cf_combine cf_nvo cf_pack cf_xcorr \
+		idf_combine bpm_combine ttag_combine \
+		cf_coadd cf_make_all_exp \
+                remove_target_orbital_motion idf_cut \
+		ttag_lightcurve \
+		ttag_lightcurve_channel_sum \
+		ttag_lightcurve_mjd2hmjd \
+		ttag_lightcurve_combine \
+		ttag_lightcurve_periodogram 
+
+all:		${BINS}
+		chmod g+rw ${BINS}
+
+install:	all
+		/bin/cp ${BINS} cf_make_all_obs.csh cf_make_900_obs.csh ${FUSEBINDIR}
+
+clean:
+		/bin/rm -f *.o ${BINS}
+
+distclean:
+		/bin/rm -f *.o ${BINS}
+		cd ../../bin; /bin/rm -f ${BINS}
+
+cf_arith: cf_arith.c cf_wrspec7.c cf_wrspec_cf2.c
+		${CC} ${CFLAGS} -o cf_arith cf_arith.c cf_wrspec7.c cf_wrspec_cf2.c\
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_coadd: cf_coadd.c
+		${CC} ${CFLAGS} -o cf_coadd cf_coadd.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_combine: cf_combine.c cf_wrspec7.c
+		${CC} ${CFLAGS} -o cf_combine cf_combine.c cf_wrspec7.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_make_all_exp:
+		${CC} ${CFLAGS} -o cf_make_all_exp cf_make_all_exp.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_ttag_to_hist:
+		${CC} ${CFLAGS} -o cf_ttag_to_hist cf_ttag_to_hist.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_combine:
+		${CC} ${CFLAGS} -o ttag_combine ttag_combine.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+idf_combine:
+		${CC} ${CFLAGS} -o idf_combine idf_combine.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+bpm_combine:
+		${CC} ${CFLAGS} -o bpm_combine bpm_combine.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+get_shift:
+		${CC} ${CFLAGS} -o get_shift get_shift.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_pack:
+		${CC} ${CFLAGS} -o cf_pack cf_pack.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_nvo:
+		${CC} ${CFLAGS} -o cf_nvo cf_nvo.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_reflux:
+		${CC} ${CFLAGS} -o cf_reflux cf_reflux.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_xcorr:
+		${CC} ${CFLAGS} -o cf_xcorr cf_xcorr.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+modhead:
+		${CC} ${CFLAGS} -o modhead modhead.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_lightcurve:
+		${CC} ${CFLAGS} -o ttag_lightcurve ttag_lightcurve.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_lightcurve_periodogram:
+		${CC} ${CFLAGS} -o ttag_lightcurve_periodogram ttag_lightcurve_periodogram.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+mjd2hjd: mjd2hjd.c gethmjd.c
+		${CC} ${CFLAGS} -o mjd2hjd mjd2hjd.c gethmjd.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_lightcurve_channel_sum:
+		${CC} ${CFLAGS} -o ttag_lightcurve_channel_sum ttag_lightcurve_channel_sum.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_lightcurve_mjd2hmjd : ttag_lightcurve_mjd2hmjd.c gethmjd.c
+		${CC} ${CFLAGS} -o ttag_lightcurve_mjd2hmjd ttag_lightcurve_mjd2hmjd.c gethmjd.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_lightcurve_combine:
+		${CC} ${CFLAGS} -o ttag_lightcurve_combine ttag_lightcurve_combine.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+idf_screen:
+		${CC} ${CFLAGS} -o idf_screen idf_screen.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+remove_target_orbital_motion: remove_target_orbital_motion.c gethmjd.c
+		${CC} ${CFLAGS} -o remove_target_orbital_motion remove_target_orbital_motion.c gethmjd.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+idf_cut:
+		${CC} ${CFLAGS} -o idf_cut idf_cut.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+extract_jitter:
+		${CC} ${CFLAGS} -o extract_jitter extract_jitter.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
diff --git a/src/analysis/Makefile.orig.orig b/src/analysis/Makefile.orig.orig
new file mode 100644
index 0000000..52fb31b
--- /dev/null
+++ b/src/analysis/Makefile.orig.orig
@@ -0,0 +1,147 @@
+
+FITSVER=	2.470
+CALFUSEDIR=	${PWD}/../..
+
+# Symbols for include directories
+FUSEINCLDIR=	-I${CALFUSEDIR}/include
+
+# Symbols used for compiling
+CC=		cc
+#  Romelfanger's optimizations
+# OPT=		-fast -xO5 -xtarget=ultra2 -xarch=v8plusa
+#
+#  SunWorld's optimizations
+# OPT=		-p -v -xO2 -xdepend -xchip=ultra -xarch=generic
+OPT=		-O -DCFORTRAN -KPIC -DSOLARIS
+CFLAGS=		${OPT} ${FUSEINCLDIR}
+
+# Symbols used for creating shared binaries
+FUSEBINDIR=	${CALFUSEDIR}/bin
+FUSELIBDIR=	-L${CALFUSEDIR}/lib
+LIBDIR=		-L/opt/SUNWspro/lib
+FUSELIBS=	-lsla -lcfitsio-${FITSVER} -lcf
+LIBS=		-lc -lm -lnsl -ldl -lsocket -lsunmath -lM77 -lF77
+LDFLAGS=	-Wl,-R${CALFUSEDIR}/lib
+
+# Binaries to be made
+
+BINS=		cf_ttag_to_hist get_shift mjd2hjd cf_reflux \
+		idf_screen extract_jitter modhead \
+		cf_arith cf_combine cf_nvo cf_pack cf_xcorr \
+		idf_combine bpm_combine ttag_combine \
+		cf_coadd cf_make_all_exp \
+                remove_target_orbital_motion idf_cut \
+		ttag_lightcurve \
+		ttag_lightcurve_channel_sum \
+		ttag_lightcurve_mjd2hmjd \
+		ttag_lightcurve_combine \
+		ttag_lightcurve_periodogram 
+
+all:		${BINS}
+		chmod g+rw ${BINS}
+
+install:	all
+		/bin/cp ${BINS} cf_make_all_obs.csh cf_make_900_obs.csh ${FUSEBINDIR}
+
+clean:
+		/bin/rm -f *.o ${BINS}
+
+distclean:
+		/bin/rm -f *.o ${BINS}
+		cd ../../bin; /bin/rm -f ${BINS}
+
+cf_arith: cf_arith.c cf_wrspec7.c cf_wrspec_cf2.c
+		${CC} ${CFLAGS} -o cf_arith cf_arith.c cf_wrspec7.c cf_wrspec_cf2.c\
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_coadd: cf_coadd.c
+		${CC} ${CFLAGS} -o cf_coadd cf_coadd.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_combine: cf_combine.c cf_wrspec7.c
+		${CC} ${CFLAGS} -o cf_combine cf_combine.c cf_wrspec7.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_make_all_exp:
+		${CC} ${CFLAGS} -o cf_make_all_exp cf_make_all_exp.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_ttag_to_hist:
+		${CC} ${CFLAGS} -o cf_ttag_to_hist cf_ttag_to_hist.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_combine:
+		${CC} ${CFLAGS} -o ttag_combine ttag_combine.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+idf_combine:
+		${CC} ${CFLAGS} -o idf_combine idf_combine.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+bpm_combine:
+		${CC} ${CFLAGS} -o bpm_combine bpm_combine.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+get_shift:
+		${CC} ${CFLAGS} -o get_shift get_shift.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_pack:
+		${CC} ${CFLAGS} -o cf_pack cf_pack.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_nvo:
+		${CC} ${CFLAGS} -o cf_nvo cf_nvo.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_reflux:
+		${CC} ${CFLAGS} -o cf_reflux cf_reflux.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_xcorr:
+		${CC} ${CFLAGS} -o cf_xcorr cf_xcorr.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+modhead:
+		${CC} ${CFLAGS} -o modhead modhead.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_lightcurve:
+		${CC} ${CFLAGS} -o ttag_lightcurve ttag_lightcurve.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_lightcurve_periodogram:
+		${CC} ${CFLAGS} -o ttag_lightcurve_periodogram ttag_lightcurve_periodogram.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+mjd2hjd: mjd2hjd.c gethmjd.c
+		${CC} ${CFLAGS} -o mjd2hjd mjd2hjd.c gethmjd.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_lightcurve_channel_sum:
+		${CC} ${CFLAGS} -o ttag_lightcurve_channel_sum ttag_lightcurve_channel_sum.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_lightcurve_mjd2hmjd : ttag_lightcurve_mjd2hmjd.c gethmjd.c
+		${CC} ${CFLAGS} -o ttag_lightcurve_mjd2hmjd ttag_lightcurve_mjd2hmjd.c gethmjd.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+ttag_lightcurve_combine:
+		${CC} ${CFLAGS} -o ttag_lightcurve_combine ttag_lightcurve_combine.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+idf_screen:
+		${CC} ${CFLAGS} -o idf_screen idf_screen.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+remove_target_orbital_motion: remove_target_orbital_motion.c gethmjd.c
+		${CC} ${CFLAGS} -o remove_target_orbital_motion remove_target_orbital_motion.c gethmjd.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+idf_cut:
+		${CC} ${CFLAGS} -o idf_cut idf_cut.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+extract_jitter:
+		${CC} ${CFLAGS} -o extract_jitter extract_jitter.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
diff --git a/src/analysis/bpm_combine.c b/src/analysis/bpm_combine.c
new file mode 100644
index 0000000..86ec7d0
--- /dev/null
+++ b/src/analysis/bpm_combine.c
@@ -0,0 +1,548 @@
+
+/*****************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSEbpm_combine
+ *****************************************************************************
+ *
+ * Synopsis:	bpm_combine output_bpm_file combined_idf_file
+ *		
+ *
+ * Description: Creates a bpm file associated with a combined idf file
+ *              It gets the names of the idf files from the combined idf 
+ *		file header. It gets the name of the bpm files from the idf 
+ *		files header. These bpm files are then combined using the   
+ *		offset information provided in the combined idf file header.  
+ *		The BPM_CAL keyword is updated in the combined idf file 
+ *		header.
+ *
+ * 		WARNING: all the single exposure IDF files (who took part in 
+ *		the creation of the idf_file) and their associated BPM files
+ *		must be in the working directory.
+ *		
+ *
+ * History:	12/03/03	bjg	v1.0	Begin work.
+ *              12/05/03        bjg             First version that compiles
+ *              
+ *		12/10/03 	bjg 	        Accept now only idf as parameter
+ *                                              Updated NSPEC keyword and 
+ *						SPECxxx, WOFFLxxx, WOFFSxxx
+ *						keywords
+ *						Removed paths in filenames 
+ *						written into header.
+ *              04/05/04        bjg             Remove unused variables
+ *                                              Change formats to match arg
+ *                                              types in printf
+ *              05/25/04        bjg             Skip when BPM_CAL unpopulated 
+ *                                              or not present.
+ *              04/13/05	wvd	v2.0	combined_idf_file may be
+ *						replaced by a file containing
+ *						a list of BPM files.  The first
+ *						line of this file must contain
+ *						the number of entries that 
+ *						follow.
+ *
+ ****************************************************************************/
+
+
+
+#include <stdlib.h>
+#include <stdio.h>
+#include <string.h>
+#include <time.h>
+#include "calfuse.h"
+
+typedef char filename[FLEN_CARD];
+
+
+
+static char CF_PRGM_ID[]= "bpm_combine";
+static char CF_VER_NUM[]= "2.0";
+
+int main(int argc,char *argv[]){
+
+  char  date[FLEN_CARD]={'\0'};      
+  char     rootname[FLEN_CARD];
+  char *corrected_filename;
+  char *string_pointer;
+
+  int      felem_hdu2;
+
+  char     stime[FLEN_CARD],keyword[FLEN_CARD];
+
+ 
+
+  time_t   vtime;
+
+  fitsfile *infits,*outfits,*idffits;
+  char     *has_bpm_list;
+  filename *filelist;
+  double   *expstartlist;
+  double   *expendlist;
+  long     *neventslist;
+  double   *sicshiftlist;
+  double   *lifshiftlist;
+  double   *exptimelist;
+  
+  double delta_t;
+  
+  filename tempstring,tempstring2;
+  double   tempdouble;
+  long     templong;
+  float    tempfloat;
+  char     tempchar;
+  
+  double   minexpstart;
+  int      minindex;
+  
+  int      nfiles;
+
+  int      intnull=0,anynull;
+  int      ncol;
+  
+  int      status=0;
+  int      hdutype=0;
+  int      tref = 0;
+
+  long     nevents=0;
+  long     n_real_events=0;	
+  long     i,j,istart;
+
+  
+  float   * xfield,*yfield,*weightfield,*lambdafield;
+  char   *channelfield;
+  
+  char     fmt_byte[FLEN_CARD],fmt_float[FLEN_CARD],fmt_short[FLEN_CARD];  
+  
+  double   totalexptime=0, rawtime=0;
+  long     neventscreened=0, neventscreenedpha=0;
+  float    timescreened=0, timesaa=0, timelowlimbangle=0, timeburst=0, timejitter=0,timenight=0;
+
+  
+
+  int  hdu2_tfields=5;
+  
+  char hdu2_extname[]="POTHOLE_DATA";   /* Name of this extension */
+  
+  char *hdu2_ttype[]={"X", "Y", "CHANNEL", "WEIGHT", "LAMBDA"};
+
+  char *hdu2_tform[5];  /* We'll assign values when we know 
+			    the number of elements in the data set. */
+
+
+  char *hdu2_tunit[]={"PIXELS", "PIXELS", "UNITLESS", "UNITLESS", "ANGSTROMS"};
+
+  
+  FILE *fp=NULL;
+  char line[FLEN_FILENAME];
+  int  maxline=FLEN_FILENAME;
+
+  
+  if (argc != 3) {
+    printf("Incorrect number of arguments.\n");
+    printf("Calling sequence:bpm_combine bpm_file combined_idf_file\n");
+    printf("Final argument may be the name of a file containing a list of BPM files.\n");
+    printf("First line must be number of BPM files in list.\n");
+    exit(1);
+  }
+  
+  /* Initialize error checking. */
+  cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Started execution.");
+  
+  /* get and display time */
+  vtime = time(NULL) ;
+  strcpy(stime,ctime(&vtime));
+  
+  fits_open_file(&idffits,argv[2],READONLY,&status);
+  if (status) {
+	status = 0;
+	if ((fp = fopen(argv[2], "r")) == NULL) {
+	    printf("Can't open file %s\n", argv[2]);
+	    return 1;
+	}
+	if ((fgets(line, maxline, fp)) == NULL) {
+	    printf("Error reading file %s\n", argv[2]);
+	    return 1;
+	}
+        sscanf(line,"%d",&nfiles);
+  }
+  else FITS_read_key(idffits,TINT,"NSPEC",&nfiles,NULL,&status);
+  
+  filelist     = (filename *)malloc(nfiles*sizeof(filename));
+  neventslist  = (long *)malloc(nfiles*sizeof(long));     
+  sicshiftlist  = (double *)calloc((size_t)nfiles,sizeof(double)); 
+  lifshiftlist  = (double *)calloc((size_t)nfiles,sizeof(double)); 
+  expstartlist = (double *)malloc(nfiles*sizeof(double));
+  expendlist   = (double *)malloc(nfiles*sizeof(double));
+  exptimelist   = (double *)malloc(nfiles*sizeof(double));
+  has_bpm_list     = (char *)malloc(nfiles*sizeof(char));
+
+  for (i=0; i<nfiles;i++) {
+
+    has_bpm_list[i]=1;
+    
+    if (fp != NULL) {
+	if((fgets(line, maxline, fp)) == NULL) {
+	   printf("Error reading %s\n", argv[2]);
+           return 1;
+	}
+        sscanf(line, "%s", filelist[i]);
+    }
+    else {
+	/* Read name of individual IDF file from combined file header. */
+      sprintf(tempstring, "SPEC%.3ld", i+1);
+      FITS_read_key(idffits,TSTRING,tempstring,tempstring2,NULL,&status);
+	/* Open individual IDF file and read name of associated BPM file. */
+      FITS_open_file(&infits,tempstring2,READONLY,&status);
+      fits_read_key(infits,TSTRING,"BPM_CAL",filelist[i],NULL,&status);
+      if (status) {
+        status=0;
+        FITS_close_file(infits,&status);
+        printf("BPM_CAL keyword not found in IDF %s; skipping.\n",tempstring2);
+        has_bpm_list[i]=0;
+        filelist[i][0]='\0';
+        continue;
+      }
+	/* Close individual IDF file. */
+      FITS_close_file(infits,&status);
+
+	/* These keywords don't apply to a user-provided list of BPM files. */
+      sprintf(tempstring, "WOFFL%.3ld", i+1);
+      FITS_read_key(idffits,TDOUBLE,tempstring,&lifshiftlist[i],NULL,&status);
+    
+      sprintf(tempstring, "WOFFS%.3ld", i+1);
+      FITS_read_key(idffits,TDOUBLE,tempstring,&sicshiftlist[i],NULL,&status);
+    }
+
+    /* Open individual BPM file. */
+    fits_open_file(&infits,filelist[i],READONLY,&status);
+    if (status) {
+      status=0;
+      printf("Could not open BPM %s for IDF %s; BPM_CAL keyword may be incorrectly populated; skipping.\n",filelist[i],tempstring2);
+      has_bpm_list[i]=0;
+      filelist[i][0]='\0';
+      continue;
+    }
+
+    FITS_read_key(infits,TDOUBLE,"EXPSTART",&(expstartlist[i]),NULL,&status);
+    FITS_read_key(infits,TDOUBLE,"EXPEND",&(expendlist[i]),NULL,&status);
+   
+    FITS_read_key(infits,TDOUBLE,"EXPTIME",&(exptimelist[i]),NULL,&status); 
+    totalexptime+=exptimelist[i];
+
+    FITS_read_key(infits,TDOUBLE,"RAWTIME",&(tempdouble),NULL,&status);
+    rawtime+=tempdouble;
+    
+    FITS_read_key(infits,TLONG,"NBADEVNT",&templong,NULL,&status);
+    neventscreened+=templong;
+    FITS_read_key(infits,TLONG,"NBADPHA",&templong,NULL,&status);
+    neventscreenedpha+=templong;
+    
+    FITS_read_key(infits,TFLOAT,"EXP_BAD",&tempfloat,NULL,&status);
+    timescreened+=tempfloat;
+    FITS_read_key(infits,TFLOAT,"EXP_SAA",&tempfloat,NULL,&status);
+    timesaa+=tempfloat;
+    FITS_read_key(infits,TFLOAT,"EXP_LIM",&tempfloat,NULL,&status);
+    timelowlimbangle+=tempfloat;
+    FITS_read_key(infits,TFLOAT,"EXP_BRST",&tempfloat,NULL,&status);
+    timeburst+=tempfloat;
+    FITS_read_key(infits,TFLOAT,"EXP_JITR",&tempfloat,NULL,&status);
+    timejitter+=tempfloat;
+    FITS_read_key(infits,TFLOAT,"EXPNIGHT",&tempfloat,NULL,&status);
+    timenight+=tempfloat;
+    
+    FITS_read_key(infits,TFLOAT,"NEVENTS",&templong,NULL,&status);
+    n_real_events+=templong;
+
+    
+    FITS_movabs_hdu(infits,2,&hdutype,&status);
+    
+    FITS_read_key(infits,TSTRING,"TFORM1",&tempstring,NULL,&status);
+    sscanf(tempstring,"%ld%c",&neventslist[i],&tempchar);
+    nevents+=neventslist[i];
+    
+    FITS_close_file(infits,&status);
+    
+  }
+  
+  if (fp != NULL) fclose(fp);
+  else FITS_close_file(idffits,&status); 
+  
+  
+  
+  
+
+  
+  printf("---SORTING INPUT FILES IN TIME ORDER---\n") ;
+  
+  for (i=0; i<nfiles-1;i++) {
+    if (!(has_bpm_list[i])) continue;
+    minexpstart=expstartlist[i];
+    minindex=i;
+    for (j=i+1; j<nfiles;j++) {
+      if (!(has_bpm_list[j])) continue;
+      if (expstartlist[j]<minexpstart){
+	minexpstart=expstartlist[j];
+	minindex=j;
+      }
+    }
+    
+    strcpy(tempstring,filelist[minindex]);
+    strcpy(filelist[minindex],filelist[i]);
+    strcpy(filelist[i],tempstring);
+    
+    tempdouble=expstartlist[minindex];
+    expstartlist[minindex]=expstartlist[i];
+    expstartlist[i]=tempdouble;
+    
+    tempdouble=expendlist[minindex];
+    expendlist[minindex]=expendlist[i];
+    expendlist[i]=tempdouble;
+
+    tempdouble=exptimelist[minindex];
+    exptimelist[minindex]=exptimelist[i];
+    exptimelist[i]=tempdouble;
+    
+    templong=neventslist[minindex];
+    neventslist[minindex]=neventslist[i];
+    neventslist[i]=templong;
+		    
+    tempdouble=lifshiftlist[minindex];
+    lifshiftlist[minindex]=lifshiftlist[i];
+    lifshiftlist[i]=tempdouble;
+    
+    tempdouble=sicshiftlist[minindex];
+    sicshiftlist[minindex]=sicshiftlist[i];
+    sicshiftlist[i]=tempdouble;
+    
+  }
+
+  istart=-1;
+
+  for (i=0; i<nfiles;i++) {
+    if (!(has_bpm_list[i])) continue; 
+      printf("%s %7.1f %7.1f %4ld %f %f\n",filelist[i],expstartlist[i],expendlist[i],neventslist[i],lifshiftlist[i],sicshiftlist[i]);
+      if (istart==-1) istart=i;
+  }
+  printf("\n");
+
+  if (istart==-1) {
+    printf("No BPM files found. Exiting\n");
+    exit(0);
+  }
+ 
+ 
+  
+  
+  printf("--------CREATING OUTPUT FILE-----\n");
+  
+  FITS_open_file(&infits,filelist[istart],READONLY,&status);
+  FITS_create_file(&outfits,argv[1],&status);
+	
+  
+	
+	
+  printf("--------WRITING MAIN HEADER-----\n");
+  
+  FITS_copy_hdu(infits,outfits,0,&status);
+	
+  FITS_read_key(infits,TSTRING,"ROOTNAME",rootname,NULL,&status);
+	
+  rootname[8]='9';
+  rootname[9]='9';
+  rootname[10]='9';
+	
+  FITS_update_key(outfits,TSTRING,"ROOTNAME",rootname,NULL,&status);
+
+  string_pointer=strrchr(argv[1],'/');
+  if (string_pointer==NULL) corrected_filename=argv[1];
+    else corrected_filename=&(string_pointer[1]); 
+	
+  FITS_update_key(outfits,TSTRING,"FILENAME",corrected_filename,NULL,&status);
+	
+  FITS_update_key(outfits,TSTRING,"EXP_ID","999",NULL,&status);
+	
+  string_pointer=strrchr(argv[2],'/');
+  if (string_pointer==NULL) corrected_filename=argv[2];
+    else corrected_filename=&(string_pointer[1]); 
+	
+
+  if (fp == NULL) 
+  FITS_update_key(outfits,TSTRING,"IDF_FILE",corrected_filename,NULL,&status);
+
+
+
+
+  fits_get_system_time(date, &tref, &status);
+	
+  FITS_update_key(outfits,TSTRING,"DATE",date,NULL,&status);
+	
+  FITS_update_key(outfits,TDOUBLE,"EXPEND",&expendlist[nfiles-1],NULL,&status);	
+  FITS_update_key(outfits,TDOUBLE,"EXPTIME",&totalexptime,NULL,&status);
+  FITS_update_key(outfits,TDOUBLE,"RAWTIME",&rawtime,NULL,&status);	
+  FITS_update_key(outfits,TLONG,"NEVENTS",&n_real_events,NULL,&status);	
+  FITS_update_key(outfits,TLONG,"NBADEVNT",&neventscreened,NULL,&status);
+  FITS_update_key(outfits,TLONG,"NBADPHA",&neventscreenedpha,NULL,&status);
+  FITS_update_key(outfits,TFLOAT,"EXP_BAD",&(timescreened),NULL,&status);
+  FITS_update_key(outfits,TFLOAT,"EXP_SAA",&(timesaa),NULL,&status);
+  FITS_update_key(outfits,TFLOAT,"EXP_LIM",&(timelowlimbangle),NULL,&status);
+  FITS_update_key(outfits,TFLOAT,"EXP_BRST",&(timeburst),NULL,&status);		
+  FITS_update_key(outfits,TFLOAT,"EXP_JITR",&(timejitter),NULL,&status);
+  FITS_update_key(outfits,TFLOAT,"EXPNIGHT",&(timenight),NULL,&status);
+
+    fits_write_history(outfits," COMBINED WITH BPM_COMBINE ",&status);
+    
+  FITS_update_key(outfits,TINT,"NSPEC",&nfiles,NULL,&status);
+  
+  for (i=0;i<nfiles;i++){
+
+    if (!(has_bpm_list[i])) continue; 
+    
+    string_pointer=strrchr(filelist[i],'/');
+    if (string_pointer==NULL) corrected_filename=filelist[i];
+    else corrected_filename=&(string_pointer[1]); 
+    
+    sprintf(keyword, "SPEC%.3ld", i+1);
+    FITS_update_key(outfits,TSTRING,keyword,corrected_filename,NULL,&status);
+    sprintf(keyword, "WOFFL%.3ld", i+1);
+    FITS_update_key(outfits,TFLOAT,keyword,&lifshiftlist[i],NULL,&status);
+    sprintf(keyword, "WOFFS%.3ld", i+1);
+    FITS_update_key(outfits,TFLOAT,keyword,&sicshiftlist[i],NULL,&status);
+  
+      
+
+  }
+
+
+
+  
+  FITS_close_file(infits,&status);
+  
+  printf("--------PREPARING EVENTS LIST HDU-----\n");
+  
+  /* Generate the tform array */
+  sprintf(fmt_byte,  "%ldB", nevents);
+  sprintf(fmt_float, "%ldE", nevents);
+  sprintf(fmt_short, "%ldI", nevents);
+  
+  hdu2_tform[0] = fmt_float;
+  hdu2_tform[1] = fmt_float;
+  hdu2_tform[2] = fmt_byte;
+  hdu2_tform[3] = fmt_float;
+  hdu2_tform[4] = fmt_float;
+  
+  
+
+  /* Append a new empty binary table to the output file */
+  FITS_create_tbl(outfits, BINARY_TBL, 1, hdu2_tfields, hdu2_ttype, hdu2_tform,
+		  hdu2_tunit, hdu2_extname, &status);
+  
+ 
+  
+  
+  
+ 
+  
+  printf("--------COMBINING HDU-----\n");
+  felem_hdu2=1;
+  for (i=0;i<nfiles;i++){
+    if (!(has_bpm_list[i])) continue;
+    
+    
+    delta_t=(expstartlist[i]-expstartlist[0])*3600*24;
+    
+    FITS_open_file(&infits,filelist[i],READONLY,&status);
+
+   
+    FITS_movabs_hdu(infits, 2, &hdutype, &status);
+    FITS_movabs_hdu(outfits, 2, &hdutype, &status);
+    printf("Processing file %s\n",filelist[i]);
+    
+    xfield=(float *)malloc(neventslist[i]*sizeof(float));
+    yfield=(float *)malloc(neventslist[i]*sizeof(float));
+    channelfield=(char *)malloc(neventslist[i]*sizeof(char));
+    weightfield=(float *)malloc(neventslist[i]*sizeof(float));
+    lambdafield=(float *)malloc(neventslist[i]*sizeof(float));
+    
+    
+    FITS_get_colnum(infits, TRUE, "X", &ncol, &status);
+    FITS_read_col(infits, TFLOAT, ncol, 1, 1, neventslist[i], &intnull,
+		  xfield, &anynull, &status);
+    
+    
+    FITS_get_colnum(infits, TRUE, "Y", &ncol, &status);
+    FITS_read_col(infits, TFLOAT, ncol, 1, 1, neventslist[i], &intnull,
+		  yfield, &anynull, &status);
+   
+
+    FITS_get_colnum(infits, TRUE, "CHANNEL", &ncol, &status);
+    FITS_read_col(infits, TBYTE, ncol, 1, 1, neventslist[i], &intnull,
+		  channelfield, &anynull, &status);
+    
+
+    FITS_get_colnum(infits, TRUE, "WEIGHT", &ncol, &status);
+    FITS_read_col(infits, TFLOAT, ncol, 1, 1, neventslist[i], &intnull,
+		  weightfield, &anynull, &status);
+   
+		
+    FITS_get_colnum(infits, TRUE, "LAMBDA", &ncol, &status);
+    FITS_read_col(infits, TFLOAT, ncol, 1, 1, neventslist[i], &intnull,
+		  lambdafield, &anynull, &status);
+    
+    
+
+    
+    for (j=0;j<neventslist[i];j++){
+	if (channelfield[j]<5) lambdafield[j]=lambdafield[j]+lifshiftlist[i];  
+        if (channelfield[j]>4) lambdafield[j]=lambdafield[j]+sicshiftlist[i]; 
+	weightfield[j]=weightfield[j]*exptimelist[i]/totalexptime;
+    }
+
+
+    
+    FITS_write_col(outfits, TFLOAT, 1, 1, felem_hdu2, neventslist[i], xfield, &status);
+    FITS_write_col(outfits, TFLOAT, 2, 1, felem_hdu2, neventslist[i], yfield, &status);
+    FITS_write_col(outfits, TBYTE, 3, 1, felem_hdu2, neventslist[i], channelfield, &status);
+    FITS_write_col(outfits, TFLOAT, 4, 1, felem_hdu2, neventslist[i], weightfield, &status);
+    FITS_write_col(outfits, TFLOAT, 5, 1, felem_hdu2, neventslist[i], lambdafield, &status);
+    
+    
+    free(xfield);
+    free(yfield);
+    free(channelfield);
+    free(weightfield);
+    free(lambdafield);
+    
+    felem_hdu2+=neventslist[i];
+    
+    FITS_close_file(infits,&status);
+    
+    
+  }
+  
+  printf("--------CLOSING OUTPUT FILE-----\n");
+
+  
+  FITS_close_file(outfits,&status);
+  
+  
+  if (fp == NULL) {
+    FITS_open_file(&idffits,argv[2],READWRITE,&status);
+
+    string_pointer=strrchr(argv[1],'/');
+    if (string_pointer==NULL) corrected_filename=argv[1];
+    else corrected_filename=&(string_pointer[1]);  
+
+    FITS_update_key(idffits,TSTRING,"BPM_CAL",corrected_filename,NULL,&status);
+    FITS_close_file(idffits,&status);
+  }
+  
+
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished execution.");
+  return EXIT_SUCCESS;
+  
+}
+
+
diff --git a/src/analysis/cf_arith.c b/src/analysis/cf_arith.c
new file mode 100644
index 0000000..94e40e9
--- /dev/null
+++ b/src/analysis/cf_arith.c
@@ -0,0 +1,2154 @@
+/*****************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *****************************************************************************
+ *
+ * Synopsis:	cf_arith infile1 op infile2 outfile
+ *
+ * Description: This is a generic utility program that performs arithmetic 
+ *		operations on two FUSE FITS files.  The files must
+ *		contain extracted FUSE spectra.
+ *		Input files are assumed to have 6 columns in a binary
+ *		table in the first extension (wavelength, flux, error, quality,
+ *		counts, counts_error).  Files with 4 columns (no counts or
+ *		counts_error) are also handled for compatibility with
+ *		pipeline output written prior to 12/1/99.
+ *
+ *		(The next paragraph is included for completeness, but is
+ *		not expected to be applicable to most users).
+ *		If infile1 and infile2 have the same number of extensions,
+ *		the specified operation is performed for each extension
+ *		(outfile_ext_i = infile1_ext_i op infile2_ext_i).
+ *		If infile2 has a single extension, the operation is performed
+ *		for each extension in infile1 with the extension in infile2
+ *		(outfile_ext_i = infile1_ext_i op infile2_ext_1).
+ *
+ *		infile1 and infile2 must have the same number of elements 
+ *		in each binary table (ie. binned by the same factor).
+ *		infile2 may be a numeric string instead of a file.
+ *		The header in outfile will be the same as for infile1,
+ *		plus some HISTORY lines.
+ *		No check is performed that the wavelengths in infile2 match
+ *		those in infile1.
+ *		It is assumed that error arrays contain errors, not variances.
+ *
+ *		If infile2 is the string "EXPTIME" (without the quotes)
+ *		operand 2 is set to the exposure time in the header of infile1.
+ *
+ *		valid choices for the operation "op" are:
+ *		+, -, *, /, avg_t, avg_s, repl_d, repl_e, boxcar, delta, 
+ *		min, max, shift, bin, deriv, addnoise
+ *
+ *		avg_t = average weighted by exposure time
+ *		avg_s = average weighted by sigma (errors)
+ *		  avg_t, avg_s valid only if infile2 is a fits file.
+ *		repl_d  = replace data in operand1 with data from operand2
+ *		repl_e  = replace errors in operand1 with errors from operand2
+ *		boxcar  = smooth data in operand1 with moving boxcar
+ *			 of width operand2.  If operand2 is a FITS file,
+ *			 the "FLUX" column is used as the width.  This
+ *			 permits application of variable smoothing.
+ *		delta = adds delta functions to operand 1 every 100 pixels;
+ *			height is equal to operand 2 (must be a scalar).
+ *			Used only for creating test spectra.
+ *		shift = shift data by the specified number of pixels.  Operand2
+ *			must be an integer.  A positive shift moves the data 
+ *			to higher pixel numbers.
+ *		bin   = bin data by the specified number of pixels.  Operand2
+ *			must be an integer.  The flux column is averaged, the
+ *			counts column is summed.
+ *		deriv = take derivative of input: out[i] = in[i+1] - in[i]
+ *			operand 2 is ignored for this!
+ *		addnoise = a uniformly distributed random number in the range
+ *			+/-operand2 is added pixel-by-pixel to the flux 
+ *			Used only for creating test spectra.
+ *
+ *		If op = "+" and the second operand is a file (not a scalar), 
+ *			or if op = "avg_t" or if op = "avg_s", the exposure
+ *			time in the output is the sum of the exposure times
+ *			in the input files.
+ *
+ *		For op1 min op2 out:  op1 is replaced by op2 if op1 < op2.
+ *		  (op2 sets a min value for the flux)
+ *		For op1 max op2 out:  op1 is replaced by op2 if op1 > op2.
+ *		  (op2 sets a max value for the flux)
+ *
+ *		The same operations are performed on the counts/countserr
+ *		columns as on the flux/fluxerr columns.  In most cases this
+ *		leads to reasonable results.  However, in a few cases, such
+ *		as addition or subtraction of a scalar, the result is likely
+ *		to be meaningless for either the flux or counts columns.
+ *		Exceptions:  MIN, MAX, REPL_D, REPL_E, DELTA, only affect
+ *		the flux and fluxerr columns.  The counts and countserror
+ *		columns are unaffected.
+ *
+ *		Note that avg_t and avg_s also average the counts; in some
+ *		cases the user may have really wanted the counts to be summed!
+ *
+ *		NOTE:  Must enclose * in quotes (ie. "*") or the shell
+ *			will expand it into filenames in the pwd!
+ *
+ *
+ * History:     08/15/99        jwk     started work
+ *		10/25/99 v1.1	jwk	avg_t,_s sum exp times in output
+ *		11/30/99	jwk	handle either 4 or 6-column files
+ *		01/06/00 v1.2	jwk	add bin option
+ *		05/01/00 v1.3	jwk	handle byte or short quality flags
+ *		09/20/00 v1.4   jwk	add derivative operation
+ *		10/11/00 v1.5   jwk     update FILENAME keyword in output file
+ *		12/11/00 v1.6   jwk	improve numeric accuracy of error prop.
+ *		01/23/01 v1.7	jwk	smooth quality rather than sum when
+ *					doing BOXCAR, to avoid overflow of
+ *					short datasize.
+ *		10/10/01 v1.8	jwk	add handling of eff area files
+ *              05/30/03 v1.9   jwk     change timeval from long to time_t; put
+ *                                      ifdef SOLARIS/endif around ieee_retro
+ *                                      spec field width for final timestamp
+ *                                      (make consistent with calfuse version)
+ *		02/04/04 v2.0   jwk     implement addnoise option
+ *		02/25/04 v2.1   jwk     check for zero errors in avg_s code
+ *		03/06/04 v3.0   jwk     add support for calfuse 3.0 files
+ *              04/05/04 v3.1   bjg     Declarations for cf_wrspec7 and
+ *                                      cf_wrspec_cf2
+ *                                      Include ctype.h
+ *                                      Correct formats to match argument
+ *                                      types in printf
+ *                                      Remove unused variable long npix
+ *                                      Casting to char * arg of setstate
+ *                                      Remove local definitions of
+ *                                      initstate() and setstate()
+ *                                      Correct use of cf_wrspec7
+ *              08/26/05 v3.2   wvd     Change name from cf_arith3 to cf_arith.
+ *					If no arguments, don't return error.
+ *					Just print message and exit.\
+ *              08/27/07 v3.3   bot 	Added L to long l.399 and 537
+ *
+ ****************************************************************************/
+
+#include <time.h>
+#include <math.h>
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include <math.h>
+#include "calfuse.h"
+#include <ctype.h>
+
+#define	PLUS	1
+#define	MINUS	2
+#define	MULT	3
+#define	DIV	4
+#define	AVG_T	5
+#define	AVG_S	6
+#define REPL_D	7
+#define REPL_E	8
+#define	BOXCAR	9
+#define DELTA	10
+#define MIN	11
+#define	MAX	12
+#define SHIFT	13
+#define BIN	14
+#define DERIV	15
+#define ADDNOISE 16
+
+/* arbitrary value for error when no data is present */
+#define DEF_ERROR 1.e-3
+
+#define MAX_RAND 0x7fffffff
+
+static char CF_PRGM_ID[] = "cf_arith";
+static char CF_VER_NUM[] = "3.3";
+
+
+void cf_wrspec7(fitsfile *outfits, long npts, float *wave, float *flux, 
+		       float *error, long *counts, float *weights, 
+		       float *bkgd,short *pothole);
+void cf_wrspec_cf2(fitsfile *outfits, int npts, float *wave,
+			  float *spec, float *errs, short *qual,
+			  float *counts, float *cntserr, int ncol, 
+			  int areaflag);
+
+
+
+
+int main(int argc, char *argv[])
+{
+    char  *timestr;
+    time_t  timeval;
+    char  infile1[80], infile2[80], outfile[80];
+    char  comment[FLEN_CARD];
+    char  expt_comment[FLEN_CARD];
+    char  errstr[80];
+    char  datatype[20];
+    int   areaflag;
+    int	  nbin;
+    int   next_1, next_2;
+    int   status=0, anynull=0, intnull=0;
+    int	  hdutype_1, hdutype_2, hdutype_o;
+    int	  hdunum_1, hdunum_2, hdunum_o;
+    long  npix_1, npix_2, npix_o;
+    long  naxis2_1, naxis2_2;
+    int   fluxcol, wavecol, errorcol, qualcol, cntscol, cntserrcol;
+    int   bkgdcol, wgtscol;
+    int	  tfields_1, tfields_2;
+    int	  opcode;
+    int   cf_version;
+    long  i, j, k, k1, k2;
+    int   arg2_scalar;
+    int	  p_shift;
+    float arg2_val;
+    float swave, sflux, sferr, scnts, scerr, spix;
+    float sbkgd, swgts;
+    long   lqual, slcts;
+    short  squal;
+    short  *qual1, *qual2, *qual_o;
+    float *wave1, *flux1, *flxerr1, *cnts1, *cntserr1;
+    float *flux2, *flxerr2, *cnts2, *cntserr2;
+    float *flux_o, *flxerr_o, *cnts_o, *cntserr_o;
+    float *wave_o;
+    float *wgts1, *wgts2, *wgts_o;
+    float *bkgd1, *bkgd2, *bkgd_o;
+    long  *lcts1, *lcts2, *lcts_o;
+    char  tformstr[FLEN_CARD];
+    char  key_str[FLEN_CARD];
+    char  qual_lbl[FLEN_CARD];
+    float f1, f2, fn;
+    float tmp1, tmp2, tmp3, tmp4;
+    float exptime_1, exptime_2, exptime_o;
+    fitsfile *infits_1, *infits_2, *outfits;
+    int	  chkop();
+    int   check_num();
+    void  padstr();
+    /* following items used by random number generator */
+    clock_t    clock();        /* system clock function */
+    int     ns;             /* used by random # generator */
+    unsigned long   seed;   /* random # generator seed */
+ /*   char    *initstate(), *setstate(); */
+    double  rand1();
+
+/* Initialize random number generator state array. */
+    static unsigned long state1[32]  =  {       3,       0x9a319039,
+          0x32d9c024,  0x9b663182,  0x5da1f342,       0x7449e56b,
+          0xbeb1dbb0,  0xab5c5918,  0x946554fd,       0x8c2e680f,
+          0xeb3d799f,  0xb11ee0b7,  0x2d436b86,       0xda672e2a,
+          0x1588ca88,  0xe369735d,  0x904f35f7,       0xd7158fd6,
+          0x6fa6f051,  0x616e6b96,  0xac94efdc,       0xde3b81e0,
+          0xdf0a6fb5,  0xf103bc02,  0x48f340fb,       0x36413f93,
+          0xc622c298,  0xf5a42ab8,  0x8a88d77b,       0xf5ad9d0e,
+          0x8999220b, 0x27fb47b9      };
+
+
+    /* perform an initial call to clock() - clock() returns the elapsed time
+     * since the first call, so in order to use it for a random # generator
+     * seed later we have to get it started here.  Subsequent calls follow
+     * opening of the first file, so that should provide some run-to-run
+     * variations.
+     */
+    seed = clock();
+
+    /* Enter a timestamp into the log. */
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    /* Initialize error checking */
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+
+    /* check command line */
+    if (argc != 5) {
+	printf("Usage: cf_arith infile1 op infile2 outfile\n");
+	return 1;
+    }
+
+    strcpy (infile1, argv[1]);
+    strcpy (infile2, argv[3]);
+    strcpy (outfile, argv[4]);
+
+    if ((opcode = chkop (argv[2])) == 0)
+	{
+	sprintf (comment,"Undefined operation: %s\n", argv[2]);
+	cf_if_error (comment);
+	}
+
+   /* Open input file(s) */
+
+   FITS_open_file(&infits_1, infile1, READONLY, &status);
+
+   /* get number of extensions in operand1 */
+   FITS_get_num_hdus (infits_1, &next_1, &status);
+   next_1--;
+
+   /* get exposure time in case we need it later. */
+   ffgky(infits_1, TFLOAT, "EXPTIME", &exptime_1, expt_comment, &status);
+   if (status)
+	{
+	fprintf (stderr, "Keyword EXPTIME not found; set exptime_1=1.0\n");
+	exptime_1 = 1.0;
+	status = 0;
+	}
+   exptime_o = exptime_1;
+
+   /* check nature of second operand:  is it a number? */
+   /* can have leading sign, and may contain E,e,D,d and additional sign */
+   arg2_scalar = check_num (argv[3]);
+   if (arg2_scalar)
+	arg2_val = atof (argv[3]);
+
+   /* Also allow the possibility of having argv[3] = "EXPTIME": */
+   if (!strcmp (argv[3], "EXPTIME"))
+	{
+	arg2_scalar = TRUE;
+	arg2_val = exptime_1;
+	}
+
+   /* check for valid operand if operation is SHIFT: */
+   p_shift = 0;
+   if (opcode == SHIFT) 
+	{
+	if (!arg2_scalar)
+	   cf_if_error ("SHIFT requires scalar argument!\n");
+
+	/* convert argument to an integer */
+	p_shift = (int) strtol (argv[3], (char **)NULL, 10);
+	}
+
+   /* check for valid operand if operation is BIN: */
+   nbin = 1;
+   if (opcode == BIN) 
+	{
+	if (!arg2_scalar)
+	   cf_if_error ("BIN requires scalar argument!\n");
+
+	/* convert argument to an integer */
+	nbin = (int) strtol (argv[3], (char **)NULL, 10);
+	if (nbin < 1)
+	   {
+	   sprintf (errstr, "bin factor = %d; must be >0!\n", nbin);
+	   cf_if_error (errstr);
+	   }
+	}
+
+   /* Check for valid operand if operation is ADDNOISE: 
+    * I suppose we could relax this and take a pixel-by-pixel amplitude
+    * from a spectrum, but let's keep it simple for now.
+    * Also initialize random number generator.
+    */
+   if (opcode == ADDNOISE) 
+	{
+	if (!arg2_scalar)
+	   cf_if_error ("ADDNOISE requires scalar argument!\n");
+
+	/* initialize random number generator */
+	/* the local clock function doesn't change rapidly enough to be
+	 * useful, even though it is nominally at microsecond resolution */
+        /* seed  =  2 * (clock() & 0x0ffff) + 1; */
+	time (&timeval);
+	seed = 2 * timeval + 1;
+	
+        ns  =  128;
+        initstate (seed, (char *) state1, ns);
+        setstate ((char *)state1);
+	}
+
+   /* bypass operand2 if op= derivative; we ignore op2 in this case*/
+   if (opcode == DERIV)
+	arg2_scalar = TRUE;
+
+   if (!arg2_scalar)
+	{
+	FITS_open_file (&infits_2, infile2, READONLY, &status);
+	FITS_get_num_hdus (infits_2, &next_2, &status);
+	next_2--;
+
+	if ((next_2 != next_1) && (next_2 != 1))
+	   {
+	   fprintf (stderr, "file %s has %d extensions.\n", infile1, next_1);
+	   fprintf (stderr, "file %s has %d extensions.\n", infile2, next_2);
+	   cf_if_error ("Illegal combination, aborting!\n");
+	   }
+	ffgky(infits_2, TFLOAT, "EXPTIME", &exptime_2, expt_comment, &status);
+	if (status)
+	  {
+	  fprintf (stderr, "Keyword EXPTIME not found; set exptime_2=1.0\n");
+	  exptime_2 = 1.0;
+	  status = 0;
+	  }
+	}
+
+   /* open output file */
+
+   remove(outfile);	/*In case the old file name exists*/
+   FITS_create_file (&outfits, outfile, &status);
+
+   /* Copy header from first operand.  The output file will have the same
+    * number of extensions as operand1.
+    */
+   /* cf_cp_hdr(infits_1, 1, outfits, 1);  */
+   FITS_copy_header (infits_1, outfits, &status);
+
+    /* Loop over extensions */
+    for ( i = 1; i <= next_1; i++ ) 
+	{
+	hdunum_1=i+1;
+
+	FITS_movabs_hdu(infits_1, hdunum_1, &hdutype_1, &status);
+	/* for Calfuse 2 and before, array length is specified by NAXIS2.
+	 * For Calfuse 3, need to get it from TFORM1.
+	 */
+	FITS_read_key(infits_1, TLONG, "NAXIS2", &naxis2_1, NULL, &status);
+	if (naxis2_1 > 1L)
+	   npix_1 = naxis2_1;
+	else
+	   {
+	   FITS_read_key(infits_1, TSTRING, "TFORM1", tformstr, NULL, &status);
+	   sscanf (tformstr, "%ldE", &npix_1);
+	   }
+
+
+	/* need to figure out what kind of data we have.
+	 * tfields=4 implies very old calfuse files, or effective area files;
+	 * tfields=6 implies calfuse 1.8 or 2.x
+	 * tfields=7 implies calfuse 3.x
+	 * Each has different types of data columns.
+	 */
+	FITS_read_key(infits_1, TINT, "TFIELDS", &tfields_1, NULL, &status);
+
+	if ((tfields_1 == 4) || (tfields_1 == 6))
+	   cf_version = 2;
+	else if (tfields_1 == 7)
+	   cf_version = 3;
+	else
+	   {
+	   sprintf (errstr, "Expecting 4,6 or 7 cols, found %d\n", tfields_1);
+	   cf_if_error (errstr);
+	   }
+
+        /* Allocate data arrays */
+	wave1 = (float *) cf_malloc(sizeof(float) * npix_1);
+	flux1 = (float *) cf_malloc(sizeof(float) * npix_1);
+	flxerr1 = (float *) cf_malloc(sizeof(float) * npix_1);
+	qual1 = (short *) cf_malloc(sizeof(short) * npix_1);
+
+	if (cf_version == 2)
+	   {
+	   cnts1 = (float *) cf_malloc(sizeof(float) * npix_1);
+	   cntserr1 = (float *) cf_malloc(sizeof(float) * npix_1);
+	   }
+	else
+	   {
+	   lcts1 = (long *) cf_malloc(sizeof(long) * npix_1);
+	   bkgd1 = (float *) cf_malloc(sizeof(float) * npix_1);
+	   wgts1 = (float *) cf_malloc(sizeof(float) * npix_1);
+	   }
+
+	/* Get the column numbers from file 1 */
+	FITS_read_key(infits_1, TSTRING, "TTYPE2", datatype, NULL, &status);
+	if (!strcmp(datatype, "FLUX"))
+	   {
+	   areaflag = FALSE;
+	   FITS_get_colnum(infits_1, TRUE, "FLUX", &fluxcol, &status);
+	   }
+	else 
+	   {
+	   areaflag = TRUE;
+	   FITS_get_colnum(infits_1, TRUE, "AREA", &fluxcol, &status);
+	   }
+
+	FITS_get_colnum(infits_1, TRUE, "WAVE", &wavecol, &status);
+	FITS_get_colnum(infits_1, TRUE, "ERROR", &errorcol, &status);
+
+	/* don't know at present if calfuse 3.x will use "QUALITY" or
+	 * "POTHOLE", so check both.
+	 */
+	if (cf_version == 2)
+	   FITS_get_colnum(infits_1, TRUE, "QUALITY", &qualcol, &status);
+	else
+	   {
+	   qualcol = 0;
+	   for (j=1; j<=tfields_1; j++)
+	      {
+	      sprintf (key_str, "TTYPE%1ld", j);
+	      FITS_read_key(infits_1, TSTRING, key_str,datatype, NULL, &status);
+	      if (!strcmp (datatype, "QUALITY") || !strcmp(datatype,"POTHOLE"))
+		{
+		strcpy (qual_lbl, datatype);
+		qualcol = j;
+		}
+	      }
+	   if (qualcol == 0)
+	      cf_if_error ("QUALITY column not found!");
+	   }
+
+	if (tfields_1 == 6)
+	   {
+	   FITS_get_colnum(infits_1, TRUE, "COUNTS", &cntscol, &status);
+	   FITS_get_colnum(infits_1, TRUE, "CNTSERR", &cntserrcol, &status);
+	   }
+
+	if (tfields_1 == 7)
+	   {
+	   FITS_get_colnum(infits_1, TRUE, "COUNTS", &cntscol, &status);
+	   FITS_get_colnum(infits_1, TRUE, "WEIGHTS", &wgtscol, &status);
+	   FITS_get_colnum(infits_1, TRUE, "BKGD", &bkgdcol, &status);
+	   }
+
+	FITS_read_col(infits_1, TFLOAT, fluxcol, 1L, 1L, npix_1,
+		&intnull, flux1, &anynull, &status);
+	FITS_read_col(infits_1, TFLOAT, wavecol, 1L, 1L, npix_1,
+		&intnull, wave1, &anynull, &status);
+	FITS_read_col(infits_1, TFLOAT, errorcol, 1L, 1L, npix_1,
+		&intnull, flxerr1, &anynull, &status);
+	FITS_read_col(infits_1, TSHORT, qualcol, 1L, 1L, npix_1,
+		&intnull, qual1, &anynull, &status);
+
+	if (tfields_1 == 6)
+	   {
+	   FITS_read_col(infits_1, TFLOAT, cntscol, 1L, 1L, npix_1,
+		&intnull, cnts1, &anynull, &status);
+	   FITS_read_col(infits_1, TFLOAT, cntserrcol, 1L, 1L, npix_1,
+		&intnull, cntserr1, &anynull, &status);
+	   }
+	else if (tfields_1 == 7)
+	   {
+	   FITS_read_col(infits_1, TLONG, cntscol, 1L, 1L, npix_1,
+		&intnull, lcts1, &anynull, &status);
+	   FITS_read_col(infits_1, TFLOAT, wgtscol, 1L, 1L, npix_1,
+		&intnull, wgts1, &anynull, &status);
+	   FITS_read_col(infits_1, TFLOAT, bkgdcol, 1L, 1L, npix_1,
+		&intnull, bkgd1, &anynull, &status);
+	   }
+	else
+	   {
+	   for (j=0; j<npix_1; j++)
+		{
+		cnts1[j] = 0.;
+		cntserr1[j] = 0.001;
+		}
+	   }
+
+	if (!arg2_scalar)
+	   {
+	   /* for file2, stop at first extension if that is all there is */
+	   if (i <= next_2)
+		{
+		hdunum_2 = i + 1;
+		FITS_movabs_hdu(infits_2, hdunum_2, &hdutype_2, &status);
+		FITS_read_key(infits_2, TLONG,"NAXIS2",&naxis2_2,NULL,&status);
+		if (naxis2_2 > 1L)
+		   npix_2 = naxis2_2;
+		else
+		   {
+		   FITS_read_key(infits_2, TSTRING, "TFORM1", tformstr, NULL, 
+			&status);
+		   sscanf (tformstr, "%ldE", &npix_2);
+		   }
+
+		FITS_read_key(infits_2, TINT, "TFIELDS", &tfields_2, NULL, 
+				&status);
+
+		if (tfields_2 != tfields_1)
+		   {
+		   sprintf (errstr, "File1 has %d cols; File 2 has %d cols!\n", 
+			tfields_1, tfields_2);
+		   cf_if_error (errstr);
+		   }
+
+		if (npix_2 != npix_1)
+		  {
+		  fprintf (stderr, "npix1 = %ld, npix2 = %ld\n", npix_1, npix_2);
+		  cf_if_error ("Aborting");
+		  }
+
+        	/* Allocate data arrays */
+		flux2 = (float *) cf_malloc(sizeof(float) * npix_2);
+		flxerr2 = (float *) cf_malloc(sizeof(float) * npix_2);
+		qual2 = (short *) cf_malloc(sizeof(short) * npix_2);
+		if (cf_version == 2)
+		  {
+		  cnts2 = (float *) cf_malloc(sizeof(float) * npix_2);
+		  cntserr2 = (float *) cf_malloc(sizeof(float) * npix_2);
+		  }
+		else
+		  {
+		  lcts2 = (long *) cf_malloc(sizeof(long) * npix_2);
+		  wgts2 = (float *) cf_malloc(sizeof(float) * npix_2);
+		  bkgd2 = (float *) cf_malloc(sizeof(float) * npix_2);
+		  }
+
+		/* Read the data from file 2 */
+
+		if (areaflag)
+		   FITS_get_colnum(infits_2, TRUE, "AREA", &fluxcol, &status);
+		else
+		   FITS_get_colnum(infits_2, TRUE, "FLUX", &fluxcol, &status);
+
+		FITS_get_colnum(infits_2, TRUE, "ERROR", &errorcol, &status);
+
+		/* don't know at present if calfuse 3.x will use "QUALITY" or
+		 * "POTHOLE", so check both.
+		 * (there may also be a mix of files present!)
+		 */
+		if (cf_version == 2)
+		   FITS_get_colnum(infits_2, TRUE, "QUALITY", &qualcol,&status);
+		else
+		   {
+		   qualcol = 0;
+		   for (j=1; j<=tfields_2; j++)
+		      {
+		      sprintf (key_str, "TTYPE%1ld", j);
+		      FITS_read_key(infits_2, TSTRING, key_str,datatype, NULL, 
+				&status);
+		      if (!strcmp (datatype, "QUALITY") || 
+			  !strcmp(datatype,"POTHOLE"))
+			{
+			strcpy (qual_lbl, datatype);
+			qualcol = j;
+			}
+		      }
+		   if (qualcol == 0)
+		      cf_if_error ("QUALITY column not found!");
+		   }
+
+		if (tfields_2 == 6)
+		   {
+		   FITS_get_colnum(infits_2, TRUE, "COUNTS", &cntscol, &status);
+		   FITS_get_colnum(infits_2, TRUE, "CNTSERR", &cntserrcol, 
+				&status);
+		   }
+
+		if (tfields_2 == 7)
+		   {
+		   FITS_get_colnum(infits_2,TRUE, "COUNTS", &cntscol, &status);
+		   FITS_get_colnum(infits_2,TRUE, "WEIGHTS", &wgtscol, &status);
+		   FITS_get_colnum(infits_2,TRUE, "BKGD", &bkgdcol, &status);
+		   }
+
+		FITS_read_col(infits_2, TFLOAT, fluxcol, 1L, 1L, npix_2,
+			&intnull, flux2, &anynull, &status);
+		FITS_read_col(infits_2, TFLOAT, errorcol, 1L, 1L, npix_2,
+			&intnull, flxerr2, &anynull, &status);
+	 	FITS_read_col(infits_2, TSHORT, qualcol, 1L, 1L, npix_2,
+			&intnull, qual2, &anynull, &status);
+
+		if (tfields_2 == 6)
+		   {
+		   FITS_read_col(infits_2, TFLOAT, cntscol, 1L, 1L, npix_2,
+			&intnull, cnts2, &anynull, &status);
+		   FITS_read_col(infits_2, TFLOAT, cntserrcol, 1L, 1L, npix_2,
+			&intnull, cntserr2, &anynull, &status);
+		   }
+		else if (tfields_1 == 7)
+		   {
+		   FITS_read_col(infits_2, TLONG, cntscol, 1L, 1L, npix_2,
+			&intnull, lcts2, &anynull, &status);
+		   FITS_read_col(infits_2, TFLOAT, wgtscol, 1L, 1L, npix_2,
+			&intnull, wgts2, &anynull, &status);
+		   FITS_read_col(infits_2, TFLOAT, bkgdcol, 1L, 1L, npix_2,
+			&intnull, bkgd2, &anynull, &status);
+		   }
+		else
+		   {
+		   for (j=0; j<npix_2; j++)
+			{
+			cnts2[j] = 0.;
+			cntserr2[j] = 0.001;
+			}
+		   }
+
+		} /* end of if (i<=next_2) */
+	   } /* end of if(!arg2_scalar) */
+
+	if ((opcode == BIN) && (nbin > 1))
+	   {
+	   if (nbin > npix_1)
+	      {
+	      sprintf (errstr, "bin factor = %d; must be < npix!\n", nbin);
+	      cf_if_error (errstr);
+	      }
+	   npix_o = npix_1 / nbin;
+	   }
+	else
+	   npix_o = npix_1;
+
+	/* make space for output arrays */
+	flux_o = (float *) cf_malloc(sizeof(float) * npix_o);
+	flxerr_o = (float *) cf_malloc(sizeof(float) * npix_o);
+	qual_o = (short *) cf_malloc(sizeof(short) * npix_o);
+
+	if (cf_version == 2)
+	  {
+	  cnts_o = (float *) cf_malloc(sizeof(float) * npix_o);
+	  cntserr_o = (float *) cf_malloc(sizeof(float) * npix_o);
+	  }
+	else
+	  {
+	  lcts_o = (long *) cf_malloc(sizeof(long) * npix_o);
+	  wgts_o = (float *) cf_malloc(sizeof(float) * npix_o);
+	  bkgd_o = (float *) cf_malloc(sizeof(float) * npix_o);
+	  }
+
+	if (opcode == BIN)
+	   wave_o =  (float *) cf_malloc(sizeof(float) * npix_o);
+	else
+	   wave_o = wave1;
+
+	/********* perform arithmetic operations here *********/
+	switch (opcode)
+	   {
+	   case PLUS:
+	     if (arg2_scalar)
+		{
+		if (cf_version == 2)
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = flux1[j] + arg2_val;
+		   flxerr_o[j] = flxerr1[j];
+		   cnts_o[j] = cnts1[j]; 
+		   cntserr_o[j] = cntserr1[j];
+		   qual_o[j] = qual1[j];
+		   }
+		  }
+		else
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = flux1[j] + arg2_val;
+		   flxerr_o[j] = flxerr1[j];
+		   lcts_o[j] = lcts1[j]; 
+		   qual_o[j] = qual1[j];
+		   bkgd_o[j] = bkgd1[j];
+		   wgts_o[j] = wgts1[j];
+		   }
+		  }
+		} /* end if(arg2_scalar) */
+	     else
+		{
+		exptime_o = exptime_1 + exptime_2;
+		if (cf_version == 2)
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = flux1[j] + flux2[j];
+		   tmp1 = flxerr1[j]*flxerr1[j];
+		   tmp2 = flxerr2[j]*flxerr2[j];
+		   flxerr_o[j] = sqrt (tmp1 + tmp2);
+		   cnts_o[j] = cnts1[j] + cnts2[j];
+		   tmp1 = cntserr1[j]*cntserr1[j];
+		   tmp2 = cntserr2[j]*cntserr2[j];
+		   cntserr_o[j] = sqrt (tmp1 + tmp2);
+		   if ((qual1[j] == 0) || (qual2[j] == 0))
+			qual_o[j] = 0;
+		   else
+			qual_o[j] = qual1[j];
+		   }
+		  }
+		else
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = flux1[j] + flux2[j];
+		   tmp1 = flxerr1[j]*flxerr1[j];
+		   tmp2 = flxerr2[j]*flxerr2[j];
+		   flxerr_o[j] = sqrt (tmp1 + tmp2);
+		   lcts_o[j] = lcts1[j] + lcts2[j];
+		   if ((qual1[j] == 0) || (qual2[j] == 0))
+			qual_o[j] = 0;
+		   else
+			qual_o[j] = (qual1[j] + qual2[j])/2;
+		   bkgd_o[j] = bkgd1[j] + bkgd2[j];
+		   wgts_o[j] = wgts1[j] + wgts2[j];
+		   }
+		  }
+		}
+	     break;
+
+	   case MINUS:
+	      if (arg2_scalar)
+		{
+		if (cf_version == 2)
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = flux1[j] - arg2_val;
+		   flxerr_o[j] = flxerr1[j];
+		   cnts_o[j] = cnts1[j];
+		   cntserr_o[j] = cntserr1[j];
+		   qual_o[j] = qual1[j];
+		   }
+		  }
+		else
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = flux1[j] - arg2_val;
+		   flxerr_o[j] = flxerr1[j];
+		   lcts_o[j] = lcts1[j];
+		   qual_o[j] = qual1[j];
+		   bkgd_o[j] = bkgd1[j];
+		   wgts_o[j] = wgts1[j];
+		   }
+		  }
+		}
+	      else
+		{
+		if (cf_version == 2)
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = flux1[j] - flux2[j];
+		   tmp1 = flxerr1[j]*flxerr1[j];
+		   tmp2 = flxerr2[j]*flxerr2[j];
+		   flxerr_o[j] = sqrt (tmp1 + tmp2);
+		   cnts_o[j] = cnts1[j] - cnts2[j];
+		   tmp1 = cntserr1[j]*cntserr1[j];
+		   tmp2 = cntserr2[j]*cntserr2[j];
+		   cntserr_o[j] = sqrt (tmp1 + tmp2);
+		   if ((qual1[j] == 0) || (qual2[j] == 0))
+			qual_o[j] = 0;
+		   else
+			qual_o[j] = qual1[j];
+		   }
+		  }
+		else
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = flux1[j] - flux2[j];
+		   tmp1 = flxerr1[j]*flxerr1[j];
+		   tmp2 = flxerr2[j]*flxerr2[j];
+		   flxerr_o[j] = sqrt (tmp1 + tmp2);
+		   lcts_o[j] = lcts1[j] - lcts2[j];
+		   if ((qual1[j] == 0) || (qual2[j] == 0))
+			qual_o[j] = 0;
+		   else
+			qual_o[j] = (qual1[j] + qual2[j])/2;
+		   bkgd_o[j] = bkgd1[j] - bkgd2[j];
+		   wgts_o[j] = wgts1[j] - wgts2[j];
+		   }
+		  }
+		}
+		break;
+
+	   case MULT:
+	      if (arg2_scalar)
+		{
+		if (cf_version == 2)
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = flux1[j] * arg2_val;
+		   flxerr_o[j] = flxerr1[j] * arg2_val;
+		   cnts_o[j] = cnts1[j];
+		   cntserr_o[j] = cntserr1[j];
+		   qual_o[j] = qual1[j];
+		   }
+		  }
+		else
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = flux1[j] * arg2_val;
+		   flxerr_o[j] = flxerr1[j] * arg2_val;
+		   lcts_o[j] = lcts1[j];
+		   qual_o[j] = qual1[j];
+		   bkgd_o[j] = bkgd1[j];
+		   wgts_o[j] = wgts1[j];
+		   }
+		  } /* end cf_version == 3 */
+		} /* end if arg2_scalar */
+	      else
+		{
+		if (cf_version == 2)
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = flux1[j] * flux2[j];
+		   if (flux1[j] == 0.)
+			{
+			flxerr_o[j] = fabs (flux2[j] * flxerr1[j]);
+			}
+		   else if (flux2[j] == 0.)
+			{
+			flxerr_o[j] = fabs (flux1[j] * flxerr2[j]);
+			}
+		   else
+			{
+			tmp1 = flxerr1[j] / flux1[j];
+			tmp2 = flxerr2[j] / flux2[j];
+			tmp3 = tmp1 * tmp1 + tmp2 * tmp2;
+			flxerr_o[j] = fabs (flux_o[j]) * sqrt (tmp3);
+			}
+		   cnts_o[j] = cnts1[j] * cnts2[j];
+		   tmp1 = cnts2[j] * cnts2[j] * cntserr1[j]*cntserr1[j];
+		   tmp2 = cnts1[j] * cnts1[j] * cntserr2[j]*cntserr2[j];
+		   cntserr_o[j] = sqrt (tmp1 + tmp2);
+		   if ((qual1[j] == 0) || (qual2[j] == 0))
+			qual_o[j] = 0;
+		   else
+			qual_o[j] = qual1[j];
+		   }  /* end loop over j */
+		  }   /* end cf_version == 2 */
+		else
+		  {   /* start cf_version == 3 */
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = flux1[j] * flux2[j];
+		   if (flux1[j] == 0.)
+			{
+			flxerr_o[j] = fabs (flux2[j] * flxerr1[j]);
+			}
+		   else if (flux2[j] == 0.)
+			{
+			flxerr_o[j] = fabs (flux1[j] * flxerr2[j]);
+			}
+		   else
+			{
+			tmp1 = flxerr1[j] / flux1[j];
+			tmp2 = flxerr2[j] / flux2[j];
+			tmp3 = tmp1 * tmp1 + tmp2 * tmp2;
+			flxerr_o[j] = fabs (flux_o[j]) * sqrt (tmp3);
+			}
+		   lcts_o[j] = lcts1[j] * lcts2[j];
+		   wgts_o[j] = wgts1[j] * wgts2[j];
+		   bkgd_o[j] = bkgd1[j] * bkgd2[j];
+		   if ((qual1[j] == 0) || (qual2[j] == 0))
+			qual_o[j] = 0;
+		   else
+			qual_o[j] = (qual1[j] + qual2[j])/2;
+		   }  /* end loop over j */
+		  }  /* end cf_version == 3 */
+		} /* end !arg2_scalar */
+		break;
+
+	   case DIV:
+	      if (arg2_scalar)
+		{
+		if (arg2_val == 0.)
+		   cf_if_error ("Commanded division by 0!");
+		if (cf_version == 2)
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = flux1[j] / arg2_val;
+		   flxerr_o[j] = flxerr1[j] / arg2_val;
+		   cnts_o[j] = cnts1[j];
+		   cntserr_o[j] = cntserr1[j];
+		   qual_o[j] = qual1[j];
+		   }
+		  }
+		else
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = flux1[j] / arg2_val;
+		   flxerr_o[j] = flxerr1[j] / arg2_val;
+		   lcts_o[j] = lcts1[j];
+		   qual_o[j] = qual1[j];
+		   bkgd_o[j] = bkgd1[j];
+		   wgts_o[j] = wgts1[j];
+		   }
+		  }
+		}
+	      else
+		{
+		if (cf_version == 2)
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   if (flux2[j] !=0.)
+			{
+			flux_o[j] = flux1[j] / flux2[j];
+			if (flux1[j] != 0.)
+			   {
+			   tmp1 = flxerr1[j] / flux1[j];
+			   tmp2 = flxerr2[j] / flux2[j];
+			   tmp3 = tmp1 * tmp1;
+			   tmp4 = tmp2 * tmp2;
+			   flxerr_o[j] = fabs (flux_o[j]) * sqrt (tmp3 + tmp4);
+			   }
+			else
+			   flxerr_o[j] = flxerr1[j] / flux2[j];
+			if ((qual1[j] == 0) || (qual2[j] == 0))
+			   qual_o[j] = 0;
+			else
+			   qual_o[j] = qual1[j];
+			}
+		   else
+			{
+			flux_o[j] = 0.;
+			flxerr_o[j] = flxerr1[j];
+			qual_o[j] = 0;
+			}
+		   if (cnts2[j] != 0.)
+			{
+			cnts_o[j] = cnts1[j] / cnts2[j];
+			if (cnts1[j] != 0.)
+			   tmp1 = cntserr1[j] / cnts1[j];
+			else
+			   tmp1 = 0.;
+			tmp2 = cntserr2[j] / cnts2[j];
+			tmp3 = tmp1 * tmp1;
+			tmp4 = tmp2 * tmp2;
+			cntserr_o[j] = fabs (cnts_o[j]) * sqrt (tmp3 + tmp4);
+			}
+		   else
+			{
+			cnts_o[j] = 0.;
+			cntserr_o[j] = cntserr1[j];
+			}
+		   } /* end loop over j */
+		  } /* end cf_version == 2 */
+		else
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   if (flux2[j] !=0.)
+			{
+			flux_o[j] = flux1[j] / flux2[j];
+			if (flux1[j] != 0.)
+			   {
+			   tmp1 = flxerr1[j] / flux1[j];
+			   tmp2 = flxerr2[j] / flux2[j];
+			   tmp3 = tmp1 * tmp1;
+			   tmp4 = tmp2 * tmp2;
+			   flxerr_o[j] = fabs (flux_o[j]) * sqrt (tmp3 + tmp4);
+			   }
+			else
+			   flxerr_o[j] = flxerr1[j] / flux2[j];
+			if ((qual1[j] == 0) || (qual2[j] == 0))
+			   qual_o[j] = 0;
+			else
+			   qual_o[j] = (qual1[j] + qual2[j])/2;
+			}
+		   else
+			{
+			flux_o[j] = 0.;
+			flxerr_o[j] = flxerr1[j];
+			qual_o[j] = 0;
+			}
+
+		   if (lcts2[j] != 0.)
+			lcts_o[j] = lcts1[j] / lcts2[j];
+		   else
+			lcts_o[j] = 0.;
+
+		   if (wgts2[j] != 0.)
+			wgts_o[j] = wgts1[j] / wgts2[j];
+		   else
+			wgts_o[j] = 0.;
+
+		   if (bkgd2[j] != 0.)
+			bkgd_o[j] = bkgd1[j] / bkgd2[j];
+		   else
+			bkgd_o[j] = 0.;
+
+		   } /* end loop over j */
+		  } /* end cf_version == 3 */
+		} /* end !arg2_scalar */
+		break;
+
+	   case AVG_T:
+	      if (arg2_scalar)
+		{
+		cf_if_error ("Illegal operation with scalar operand!");
+		}
+	      else
+		{
+		if (cf_version == 2)
+		  {
+		f1 = exptime_1 / (exptime_1 + exptime_2);
+		f2 = exptime_2 / (exptime_1 + exptime_2);
+		exptime_o = exptime_1 + exptime_2;
+		for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = f1 * flux1[j] + f2 * flux2[j];
+		   tmp1 = f1 * f1 * flxerr1[j]*flxerr1[j];
+		   tmp2 = f2 * f2 * flxerr2[j]*flxerr2[j];
+		   flxerr_o[j] = sqrt (tmp1 + tmp2);
+		   cnts_o[j] = f1 * cnts1[j] + f2 * cnts2[j];
+		   tmp1 = f1 * f1 * cntserr1[j]*cntserr1[j];
+		   tmp2 = f2 * f2 * cntserr2[j]*cntserr2[j];
+		   cntserr_o[j] = sqrt (tmp1 + tmp2);
+		   if ((qual1[j] == 0) || (qual2[j] == 0))
+			qual_o[j] = 0;
+		   else
+			qual_o[j] = qual1[j];
+		   }
+		  }
+		else
+		  {
+		  f1 = exptime_1 / (exptime_1 + exptime_2);
+		  f2 = exptime_2 / (exptime_1 + exptime_2);
+		  exptime_o = exptime_1 + exptime_2;
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = f1 * flux1[j] + f2 * flux2[j];
+		   tmp1 = f1 * f1 * flxerr1[j]*flxerr1[j];
+		   tmp2 = f2 * f2 * flxerr2[j]*flxerr2[j];
+		   flxerr_o[j] = sqrt (tmp1 + tmp2);
+		   lcts_o[j] = lcts1[j] + lcts2[j];
+		   wgts_o[j] = wgts1[j] + wgts2[j];
+		   bkgd_o[j] = bkgd1[j] + bkgd2[j];
+		   if ((qual1[j] == 0) || (qual2[j] == 0))
+			qual_o[j] = 0;
+		   else
+			qual_o[j] = (qual1[j] + qual2[j])/2;
+		   }
+		  }
+		}
+		break;
+
+	   case AVG_S:
+	      if (arg2_scalar)
+		{
+		cf_if_error ("Illegal operation with scalar operand!");
+		}
+	      else
+		{
+		exptime_o = exptime_1 + exptime_2;
+		if (cf_version == 2)
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   if ((flxerr1[j] > 0.) && (flxerr2[j] > 0.))
+		      {
+		      f1 = 1. / (flxerr1[j] * flxerr1[j]);
+		      f2 = 1. / (flxerr2[j] * flxerr2[j]);
+		      }
+		   else
+		      f1 = f2 = 1.;
+		   fn = f1 + f2;
+		   flux_o[j] = (f1 * flux1[j] + f2 * flux2[j]) / fn;
+		   flxerr_o[j] = sqrt (1./fn);
+		   if ((cntserr1[j] > 0.) && (cntserr2[j] > 0.))
+		      {
+		      f1 = 1. / (cntserr1[j] * cntserr1[j]);
+		      f2 = 1. / (cntserr2[j] * cntserr2[j]);
+		      }
+		   else
+		      f1 = f2 = 1.;
+		   fn = f1 + f2;
+		   cnts_o[j] = (f1 * cnts1[j] + f2 * cnts2[j]) / fn;
+		   cntserr_o[j] = sqrt (1./fn);
+		   if ((qual1[j] == 0) || (qual2[j] == 0))
+			qual_o[j] = 0;
+		   else
+			qual_o[j] = qual1[j];
+		   }
+		  }  /* end if cf_version == 2 */
+		else
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   if ((flxerr1[j] > 0.) && (flxerr2[j] > 0.))
+		      {
+		      f1 = 1. / (flxerr1[j] * flxerr1[j]);
+		      f2 = 1. / (flxerr2[j] * flxerr2[j]);
+		      }
+		   else
+		      f1 = f2 = 1.;
+		   fn = f1 + f2;
+		   flux_o[j] = (f1 * flux1[j] + f2 * flux2[j]) / fn;
+		   flxerr_o[j] = sqrt (1./fn);
+		   lcts_o[j] = (f1 * lcts1[j] + f2 * lcts2[j]) / fn;
+		   wgts_o[j] = (f1 * wgts1[j] + f2 * wgts2[j]) / fn;
+		   bkgd_o[j] = (f1 * bkgd1[j] + f2 * bkgd2[j]) / fn;
+		   if ((qual1[j] == 0) || (qual2[j] == 0))
+			qual_o[j] = 0;
+		   else
+			qual_o[j] = (f1*qual1[j] + f2*qual2[j]) / fn;
+		   }
+		  }
+		}
+		break;
+
+	   case REPL_D:
+	      if (arg2_scalar)
+		{
+		if (cf_version == 2)
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = arg2_val;
+		   flxerr_o[j] = flxerr1[j];
+		   cnts_o[j] = cnts1[j];
+		   cntserr_o[j] = cntserr1[j];
+		   qual_o[j] = qual1[j];
+		   }
+		  }
+		else
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = arg2_val;
+		   flxerr_o[j] = flxerr1[j];
+		   lcts_o[j] = lcts1[j];
+		   qual_o[j] = qual1[j];
+		   wgts_o[j] = wgts1[j];
+		   bkgd_o[j] = bkgd1[j];
+		   }
+		  }
+		}
+	      else
+		{
+		if (cf_version == 2)
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = flux2[j];
+		   flxerr_o[j] = flxerr1[j];
+		   cnts_o[j] = cnts1[j];
+		   cntserr_o[j] = cntserr1[j];
+		   if ((qual1[j] == 0) || (qual2[j] == 0))
+			qual_o[j] = 0;
+		   else
+			qual_o[j] = qual1[j];
+		   }
+		  }
+		else
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = flux2[j];
+		   flxerr_o[j] = flxerr1[j];
+		   lcts_o[j] = lcts1[j];
+		   wgts_o[j] = wgts1[j];
+		   bkgd_o[j] = bkgd1[j];
+		   if ((qual1[j] == 0) || (qual2[j] == 0))
+			qual_o[j] = 0;
+		   else
+			qual_o[j] = qual1[j];
+		   }
+		  }
+		}
+		break;
+
+	   case REPL_E:
+	      if (arg2_scalar)
+		{
+		if (cf_version == 2)
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = flux1[j];
+		   flxerr_o[j] = arg2_val;
+		   cnts_o[j] = cnts1[j];
+		   cntserr_o[j] = cntserr1[j];
+		   qual_o[j] = qual1[j];
+		   }
+		  }
+		else
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = flux1[j];
+		   flxerr_o[j] = arg2_val;
+		   lcts_o[j] = lcts1[j];
+		   qual_o[j] = qual1[j];
+		   wgts_o[j] = wgts1[j];
+		   bkgd_o[j] = bkgd1[j];
+		   }
+		  }
+		}
+	      else
+		{
+		if (cf_version == 2)
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = flux1[j];
+		   flxerr_o[j] = flxerr2[j];
+		   cnts_o[j] = cnts1[j];
+		   cntserr_o[j] = cntserr1[j];
+		   if ((qual1[j] == 0) || (qual2[j] == 0))
+			qual_o[j] = 0;
+		   else
+			qual_o[j] = qual1[j];
+		   }
+		  }
+		else
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = flux1[j];
+		   flxerr_o[j] = flxerr2[j];
+		   lcts_o[j] = lcts1[j];
+		   wgts_o[j] = wgts1[j];
+		   bkgd_o[j] = bkgd1[j];
+		   if ((qual1[j] == 0) || (qual2[j] == 0))
+			qual_o[j] = 0;
+		   else
+			qual_o[j] = qual1[j];
+		   }
+		  }
+		}
+		break;
+
+	   case DELTA:
+	      /* start by copying input file to output */
+		if (cf_version == 2)
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = flux1[j];
+		   flxerr_o[j] = flxerr1[j];
+		   cnts_o[j] = cnts1[j];
+		   cntserr_o[j] = cntserr1[j];
+		   qual_o[j] = qual1[j];
+		   }
+		  }
+		else
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = flux1[j];
+		   flxerr_o[j] = flxerr1[j];
+		   lcts_o[j] = lcts1[j];
+		   qual_o[j] = qual1[j];
+		   wgts_o[j] = wgts1[j];
+		   bkgd_o[j] = bkgd1[j];
+		   }
+		  }
+	      if (arg2_scalar)
+		{
+		for (j=100; j<npix_1; j+=100)
+		   {
+		   flux_o[j] += arg2_val;
+		   if (flux1[j] != 0) 
+			{
+			flxerr_o[j] *= fabs (flux_o[j] / flux1[j]);
+			}
+		   else
+			{
+			flxerr_o[j] += 0.1 * fabs (flux_o[j]);
+			}
+		   }
+		}
+	      else
+		{
+		for (j=100; j<npix_1; j+=100)
+		   {
+		   flux_o[j] += flux2[j];
+		   if (flux1[j] != 0) 
+			{
+			flxerr_o[j] *= fabs (flux_o[j] / flux1[j]);
+			}
+		   else
+			{
+			flxerr_o[j] += 0.1 * fabs (flux_o[j]);
+			}
+		   }
+		}
+		break;
+
+	   case BOXCAR:
+	      if (arg2_scalar)
+		{
+		/* if width is <= 1, just copy input to output */
+		if (arg2_val <= 1.)
+		  {
+		  if (cf_version == 2)
+		    {
+		    for (j=0; j<npix_1; j++)
+		     {
+		     flux_o[j] = flux1[j];;
+		     flxerr_o[j] = flxerr1[j];
+		     cnts_o[j] = cnts1[j];
+		     cntserr_o[j] = cntserr1[j];
+		     qual_o[j] = qual1[j];
+		     }
+		    } /* end if_cf_version == 2 */
+		  else
+		    {  /* cf_version == 3 */
+		    for (j=0; j<npix_1; j++)
+		     {
+		     flux_o[j] = flux1[j];;
+		     flxerr_o[j] = flxerr1[j];
+		     lcts_o[j] = lcts1[j];
+		     qual_o[j] = qual1[j];
+		     wgts_o[j] = wgts1[j];
+		     bkgd_o[j] = bkgd1[j];
+		     }
+		    } /* end if cf_version == 3 */
+		  } /* end if arg2_val <=1 */
+		else
+		  {
+		  if (cf_version == 2)
+		   {
+		   for (j=0; j<npix_1; j++)
+		     {
+		     k1 = j - arg2_val / 2. + 0.5;
+		     k2 = j + arg2_val / 2. + 0.5;
+		     if (k1 < 0)
+			k1 = 0;
+		     if (k2 > npix_1-1)
+			k2 = npix_1-1;
+		     sflux = 0.;
+		     sferr = 0.;
+		     scnts = 0.;
+		     scerr = 0.;
+		     lqual = 0;
+		     for (k=k1; k<=k2; k++)
+			{
+			sflux += flux1[k];
+			sferr += flxerr1[k] * flxerr1[k];
+			scnts += cnts1[k];
+			scerr += cntserr1[k] * cntserr1[k];
+			lqual += (long) qual1[k];
+			}
+		     spix = (float)(k2 - k1 + 1);
+		     flux_o[j] = sflux / spix;
+		     flxerr_o[j] = sqrt (sferr) / spix;
+		     cnts_o[j] = scnts / spix;
+		     cntserr_o[j] = sqrt (scerr) / spix;
+		     qual_o[j] = (short) (lqual / spix);
+		     } /* end of for j... */
+		   } /* end if cf_version == 2 */
+		  else
+		   { /* start cf_version == 3 for scalar smoothing > 1 */
+		   for (j=0; j<npix_1; j++)
+		     {
+		     k1 = j - arg2_val / 2. + 0.5;
+		     k2 = j + arg2_val / 2. + 0.5;
+		     if (k1 < 0)
+			k1 = 0;
+		     if (k2 > npix_1-1)
+			k2 = npix_1-1;
+		     sflux = 0.;
+		     sferr = 0.;
+		     slcts = 0;
+		     sbkgd = 0.;
+		     swgts = 0.;
+		     lqual = 0;
+		     for (k=k1; k<=k2; k++)
+			{
+			sflux += flux1[k];
+			sferr += flxerr1[k] * flxerr1[k];
+			slcts += lcts1[k];
+			swgts += wgts1[k];
+			sbkgd += bkgd1[k];
+			lqual += (long) qual1[k];
+			}
+		     spix = (float)(k2 - k1 + 1);
+		     flux_o[j] = sflux / spix;
+		     flxerr_o[j] = sqrt (sferr) / spix;
+		     lcts_o[j] = slcts / spix;
+		     bkgd_o[j] = sbkgd / spix;
+		     wgts_o[j] = swgts / spix;
+		     qual_o[j] = (short) (lqual / spix);
+		     } /* end of for j... */
+		   } /* end cf_version == 3 */
+		  } /* end of arg2_scalar > 1 */
+		} /* end of if (arg2_scalar) */
+	      else
+		{
+		/* allow the smoothing width to vary pixel-by-pixel */
+		if (cf_version == 2)
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   arg2_val = flux2[j];
+		   if (arg2_val < 1.)
+		     {
+		     flux_o[j] = flux1[j];
+		     flxerr_o[j] = flxerr1[j];
+		     cnts_o[j] = cnts1[j];
+		     cntserr_o[j] = cntserr1[j];
+		     qual_o[j] = qual1[j];
+		     }
+		   else
+		     {
+		     k1 = j - arg2_val / 2. + 0.5;
+		     k2 = j + arg2_val / 2. + 0.5;
+		     if (k1 < 0)
+			k1 = 0;
+		     if (k2 > npix_1-1)
+			k2 = npix_1-1;
+		     sflux = 0.;
+		     sferr = 0.;
+		     scnts = 0.;
+		     scerr = 0.;
+		     lqual = 0;
+		     for (k=k1; k<=k2; k++)
+			{
+			sflux += flux1[k];
+			sferr += flxerr1[k] * flxerr1[k];
+			scnts += cnts1[k];
+			scerr += cntserr1[k] * cntserr1[k];
+			lqual += (long) qual1[k];
+			}
+		     spix = (float)(k2 - k1 + 1);
+		     flux_o[j] = sflux / spix;
+		     flxerr_o[j] = sqrt (sferr) / spix;
+		     cnts_o[j] = scnts / spix;
+		     cntserr_o[j] = sqrt (scerr) / spix;
+		     qual_o[j] = (short) (lqual / spix);
+		     } /* end of arg2_val > 1 */
+		   } /* end of for j... */
+		  } /* end if cf_version == 2 */
+		else
+		  { /* cf_version == 3 */
+		  for (j=0; j<npix_1; j++)
+		   {
+		   arg2_val = flux2[j];
+		   if (arg2_val < 1.)
+		     {
+		     flux_o[j] = flux1[j];
+		     flxerr_o[j] = flxerr1[j];
+		     lcts_o[j] = lcts1[j];
+		     wgts_o[j] = wgts1[j];
+		     bkgd_o[j] = bkgd1[j];
+		     qual_o[j] = qual1[j];
+		     }
+		   else
+		     {
+		     k1 = j - arg2_val / 2. + 0.5;
+		     k2 = j + arg2_val / 2. + 0.5;
+		     if (k1 < 0)
+			k1 = 0;
+		     if (k2 > npix_1-1)
+			k2 = npix_1-1;
+		     sflux = 0.;
+		     sferr = 0.;
+		     slcts = 0;
+		     sbkgd = 0.;
+		     swgts = 0.;
+		     lqual = 0;
+		     for (k=k1; k<=k2; k++)
+			{
+			sflux += flux1[k];
+			sferr += flxerr1[k] * flxerr1[k];
+			slcts += lcts1[k];
+			swgts += wgts1[k];
+			sbkgd += bkgd1[k];
+			lqual += (long) qual1[k];
+			}
+		     spix = (float)(k2 - k1 + 1);
+		     flux_o[j] = sflux / spix;
+		     flxerr_o[j] = sqrt (sferr) / spix;
+		     lcts_o[j] = slcts / spix;
+		     wgts_o[j] = swgts / spix;
+		     bkgd_o[j] = sbkgd / spix;
+		     qual_o[j] = (short) (lqual / spix);
+		     } /* end of arg2_val > 1 */
+		   } /* end of for j... */
+		  } /* end if cf_version == 3 */
+		} /* end of if (!arg2_scalar) */
+		break; /* end of case BOXCAR */
+
+	   case MIN:
+	      if (arg2_scalar)
+		{
+		if (cf_version == 2)
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   if (flux1[j] < arg2_val)
+			flux_o[j] = arg2_val;
+		   else
+			flux_o[j] = flux1[j];
+		   flxerr_o[j] = flxerr1[j];
+		   cnts_o[j] = cnts1[j];
+		   cntserr_o[j] = cntserr1[j];
+		   qual_o[j] = qual1[j];
+		   }
+		  }
+		else
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   if (flux1[j] < arg2_val)
+			flux_o[j] = arg2_val;
+		   else
+			flux_o[j] = flux1[j];
+		   flxerr_o[j] = flxerr1[j];
+		   lcts_o[j] = lcts1[j];
+		   wgts_o[j] = wgts1[j];
+		   bkgd_o[j] = bkgd1[j];
+		   qual_o[j] = qual1[j];
+		   }
+		  }
+		}
+	      else
+		{
+		for (j=0; j<npix_1; j++)
+		   {
+		   if (flux1[j] < flux2[j])
+			{
+			flux_o[j] = flux2[j];
+			flxerr_o[j] = flxerr2[j];
+			}
+		   else
+			{
+			flux_o[j] = flux1[j];
+			flxerr_o[j] = flxerr1[j];
+			}
+		   if ((qual1[j] == 0) || (qual2[j] == 0))
+			qual_o[j] = 0;
+		   else
+			qual_o[j] = qual1[j];
+		   }
+		if (cf_version == 2)
+		  {
+		  for (j=0; j<npix_1; j++)
+		    {
+		    cnts_o[j] = cnts1[j];
+		    cntserr_o[j] = cntserr1[j];
+		    }
+		  }
+		else
+		  {
+		  for (j=0; j<npix_1; j++)
+		    {
+		    lcts_o[j] = lcts1[j];
+		    wgts_o[j] = wgts1[j];
+		    bkgd_o[j] = bkgd1[j];
+		    }
+		  }
+		}
+		break;
+
+	   case MAX:
+	      if (arg2_scalar)
+		{
+		if (cf_version == 2)
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   if (flux1[j] > arg2_val)
+			flux_o[j] = arg2_val;
+		   else
+			flux_o[j] = flux1[j];
+		   flxerr_o[j] = flxerr1[j];
+		   cnts_o[j] = cnts1[j];
+		   cntserr_o[j] = cntserr1[j];
+		   qual_o[j] = qual1[j];
+		   }
+		  }
+		else
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   if (flux1[j] > arg2_val)
+			flux_o[j] = arg2_val;
+		   else
+			flux_o[j] = flux1[j];
+		   flxerr_o[j] = flxerr1[j];
+		   lcts_o[j] = lcts1[j];
+		   wgts_o[j] = wgts1[j];
+		   bkgd_o[j] = bkgd1[j];
+		   qual_o[j] = qual1[j];
+		   }
+		  }
+		}
+	      else
+		{
+		for (j=0; j<npix_1; j++)
+		   {
+		   if (flux1[j] > flux2[j])
+			{
+			flux_o[j] = flux2[j];
+			flxerr_o[j] = flxerr2[j];
+			}
+		   else
+			{
+			flux_o[j] = flux1[j];
+			flxerr_o[j] = flxerr1[j];
+			}
+		   if ((qual1[j] == 0) || (qual2[j] == 0))
+			qual_o[j] = 0;
+		   else
+			qual_o[j] = qual1[j];
+		   }
+		if (cf_version == 2)
+		  {
+		  for (j=0; j<npix_1; j++)
+		    {
+		    cnts_o[j] = cnts1[j];
+		    cntserr_o[j] = cntserr1[j];
+		    }
+		  }
+		else
+		  {
+		  for (j=0; j<npix_1; j++)
+		    {
+		    lcts_o[j] = lcts1[j];
+		    wgts_o[j] = wgts1[j];
+		    bkgd_o[j] = bkgd1[j];
+		    }
+		  }
+		}
+		break;
+
+	   case SHIFT:
+		if (cf_version == 2)
+		  {
+	          if (p_shift > 0)
+		    {
+		    for (j=0; j<p_shift; j++)
+		       {
+		       flux_o[j] = 0.;
+		       flxerr_o[j] = DEF_ERROR;
+		       cnts_o[j] = 0.;
+		       cntserr_o[j] = DEF_ERROR;
+		       qual_o[j] = 0;
+		       }
+		    for (j=p_shift; j<npix_1; j++)
+		       {
+		       k = j - p_shift;
+		       flux_o[j] = flux1[k];
+		       flxerr_o[j] = flxerr1[k];
+		       cnts_o[j] = cnts1[k];
+		       cntserr_o[j] = cntserr1[k];
+		       qual_o[j] = qual1[k];
+		       }
+		    }
+	          if (p_shift <= 0)
+		    {
+		    for (j=npix_1+p_shift; j<npix_1; j++)
+		       {
+		       flux_o[j] = 0.;
+		       flxerr_o[j] = DEF_ERROR;
+		       cnts_o[j] = 0.;
+		       cntserr_o[j] = DEF_ERROR;
+		       qual_o[j] = 0;
+		       }
+		    for (j=0; j<npix_1+p_shift; j++)
+		       {
+		       k = j - p_shift;
+		       flux_o[j] = flux1[k];
+		       flxerr_o[j] = flxerr1[k];
+		       cnts_o[j] = cnts1[k];
+		       cntserr_o[j] = cntserr1[k];
+		       qual_o[j] = qual1[k];
+		       }
+		    }
+		  } /* end if cf_version == 2 */
+		else
+		  {
+	          if (p_shift > 0)
+		    {
+		    for (j=0; j<p_shift; j++)
+		       {
+		       flux_o[j] = 0.;
+		       flxerr_o[j] = DEF_ERROR;
+		       lcts_o[j] = 0;
+		       qual_o[j] = 0;
+		       wgts_o[j] = 0.;
+		       bkgd_o[j] = 0.;
+		       }
+		    for (j=p_shift; j<npix_1; j++)
+		       {
+		       k = j - p_shift;
+		       flux_o[j] = flux1[k];
+		       flxerr_o[j] = flxerr1[k];
+		       lcts_o[j] = lcts1[k];
+		       wgts_o[j] = wgts1[k];
+		       bkgd_o[j] = bkgd1[k];
+		       qual_o[j] = qual1[k];
+		       }
+		    }
+	          if (p_shift <= 0)
+		    {
+		    for (j=npix_1+p_shift; j<npix_1; j++)
+		       {
+		       flux_o[j] = 0.;
+		       flxerr_o[j] = DEF_ERROR;
+		       lcts_o[j] = 0;
+		       wgts_o[j] = 0.;
+		       bkgd_o[j] = 0.;
+		       qual_o[j] = 0;
+		       }
+		    for (j=0; j<npix_1+p_shift; j++)
+		       {
+		       k = j - p_shift;
+		       flux_o[j] = flux1[k];
+		       flxerr_o[j] = flxerr1[k];
+		       lcts_o[j] = lcts1[k];
+		       wgts_o[j] = wgts1[k];
+		       bkgd_o[j] = bkgd1[k];
+		       qual_o[j] = qual1[k];
+		       }
+		    }
+		  }
+		break;
+
+	   case BIN:
+		/* if nbin = 1, just copy input to output */
+		if (nbin == 1)
+		   {
+		   if (cf_version == 2)
+		     {
+		      for (j=0; j<npix_o; j++)
+		        {
+		        wave_o[j] = wave1[j];
+		        flux_o[j] = flux1[j];;
+		        flxerr_o[j] = flxerr1[j];
+		        cnts_o[j] = cnts1[j];
+		        cntserr_o[j] = cntserr1[j];
+		        qual_o[j] = qual1[j];
+		        }
+		     }
+		   else
+		     {
+		      for (j=0; j<npix_o; j++)
+		        {
+		        wave_o[j] = wave1[j];
+		        flux_o[j] = flux1[j];;
+		        flxerr_o[j] = flxerr1[j];
+		        lcts_o[j] = lcts1[j];
+		        wgts_o[j] = wgts1[j];
+		        bkgd_o[j] = bkgd1[j];
+		        qual_o[j] = qual1[j];
+		        }
+		     } /* end cf_version == 3 */
+		   } /* end nbin == 1 */
+		else
+		   {
+		   if (cf_version == 2)
+		     {
+		      for (j=0; j<npix_o; j++)
+		        {
+		        k1 = j * nbin;
+		        k2 = k1 + nbin;
+		        if (k2 > npix_1)
+			   k2 = npix_1;
+		        swave = 0.;
+		        sflux = 0.;
+		        sferr = 0.;
+		        scnts = 0.;
+		        scerr = 0.;
+		        squal = 0;
+		        spix = 0;
+		        for (k=k1; k<k2; k++)
+			   {
+			   swave += wave1[k];
+			   if (qual1[k] > 0)
+			      {
+			      sflux += flux1[k];
+			      sferr += flxerr1[k] * flxerr1[k];
+			      scnts += cnts1[k];
+			      scerr += cntserr1[k] * cntserr1[k];
+			      squal += qual1[k];
+			      spix++;
+			      }
+			   }
+		        if (spix == 0)
+			   spix = 1;
+		        wave_o[j] = swave / (float)(k2 - k1);
+		        flux_o[j] = sflux / spix;
+		        flxerr_o[j] = sqrt (sferr) / spix;
+		        cnts_o[j] = scnts;
+		        cntserr_o[j] = sqrt (scerr);
+		        qual_o[j] = squal;
+		        } /* end of for j... */
+		     } /* end cf_version == 2 */
+		   else
+		     {
+		      for (j=0; j<npix_o; j++)
+		        {
+		        k1 = j * nbin;
+		        k2 = k1 + nbin;
+		        if (k2 > npix_1)
+			   k2 = npix_1;
+		        swave = 0.;
+		        sflux = 0.;
+		        sferr = 0.;
+		        slcts = 0;
+		        swgts = 0.;
+		        sbkgd = 0.;
+		        squal = 0;
+		        spix = 0;
+		        for (k=k1; k<k2; k++)
+			   {
+			   swave += wave1[k];
+			   if (qual1[k] > 0)
+			      {
+			      sflux += flux1[k];
+			      sferr += flxerr1[k] * flxerr1[k];
+			      slcts += lcts1[k];
+			      swgts += wgts1[k];
+			      sbkgd += bkgd1[k];
+			      squal += qual1[k];
+			      spix++;
+			      }
+			   }
+		        if (spix == 0)
+			   spix = 1;
+		        wave_o[j] = swave / (float)(k2 - k1);
+		        flux_o[j] = sflux / spix;
+		        flxerr_o[j] = sqrt (sferr) / spix;
+		        lcts_o[j] = slcts;
+		        qual_o[j] = squal / spix;
+		        wgts_o[j] = swgts / spix;
+		        bkgd_o[j] = sbkgd;
+		        } /* end of for j... */
+		     } /* end cf_version == 3 */
+		   } /* end of nbin > 1 */
+		break;
+
+	   case DERIV:
+		if (cf_version == 2)
+		  {
+		  for (j=0; j<npix_1-1; j++)
+		   {
+		   flux_o[j] = flux1[j+1] - flux1[j];
+		   tmp1 = flxerr1[j+1]*flxerr1[j+1];
+		   tmp2 = flxerr1[j]*flxerr1[j];
+		   flxerr_o[j] = sqrt (tmp1 + tmp2);
+		   tmp1 = cntserr1[j+1]*cntserr1[j+1];
+		   tmp2 = cntserr1[j]*cntserr1[j];
+		   cnts_o[j] = cnts1[j+1] - cnts1[j];
+		   cntserr_o[j] = sqrt (tmp1 + tmp2);
+		   qual_o[j] = qual1[j];
+		   }
+		  flux_o[npix_1-1] = flux_o[npix_1-2];
+		  flxerr_o[npix_1-1] = flxerr_o[npix_1-2];
+		  cnts_o[npix_1-1] = cnts_o[npix_1-2];
+		  cntserr_o[npix_1-1] = cntserr_o[npix_1-2];
+		  } /* end cf_version == 2 */
+		else
+		  {
+		  for (j=0; j<npix_1-1; j++)
+		   {
+		   flux_o[j] = flux1[j+1] - flux1[j];
+		   tmp1 = flxerr1[j+1]*flxerr1[j+1];
+		   tmp2 = flxerr1[j]*flxerr1[j];
+		   flxerr_o[j] = sqrt (tmp1 + tmp2);
+		   lcts_o[j] = lcts1[j+1] - lcts1[j];
+		   qual_o[j] = qual1[j];
+		   wgts_o[j] = wgts1[j];
+		   bkgd_o[j] = bkgd1[j];
+		   }
+		  flux_o[npix_1-1] = flux_o[npix_1-2];
+		  flxerr_o[npix_1-1] = flxerr_o[npix_1-2];
+		  lcts_o[npix_1-1] = lcts_o[npix_1-2];
+		  } /* end cf_version == 3 */
+		break;
+
+	   case ADDNOISE:
+		if (cf_version == 2)
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = flux1[j] + arg2_val * rand1();
+		   flxerr_o[j] = flxerr1[j];
+		   cnts_o[j] = cnts1[j];
+		   cntserr_o[j] = cntserr1[j];
+		   qual_o[j] = qual1[j];
+		   }
+		  }
+		else
+		  {
+		  for (j=0; j<npix_1; j++)
+		   {
+		   flux_o[j] = flux1[j] + arg2_val * rand1();
+		   flxerr_o[j] = flxerr1[j];
+		   lcts_o[j] = lcts1[j];
+		   wgts_o[j] = wgts1[j];
+		   bkgd_o[j] = bkgd1[j];
+		   qual_o[j] = qual1[j];
+		   }
+		  }
+		break;
+
+	   default:
+		cf_if_error ("Illegal opcode; should never get here!");
+		break;
+
+	   } /* end switch (opcode) */
+ 
+	/* write the extension containing the results as a binary table */
+	hdunum_o=i+1;
+
+	/* cf_write_spec creates the new extension and sets the pointer
+	 * to it.
+	 */
+	if (tfields_1 < 7)
+	   cf_wrspec_cf2 (outfits, npix_o, wave_o, flux_o, flxerr_o, qual_o,
+		cnts_o, cntserr_o, tfields_1, areaflag);
+	else
+	   cf_wrspec7 (outfits, npix_o, wave_o, flux_o, flxerr_o,
+		lcts_o, wgts_o, bkgd_o, qual_o);
+
+ 
+	if (wave_o != wave1)
+	  free(wave_o);
+	free(wave1);
+	free(flux1);
+	free(flxerr1);
+	free(qual1);
+	free(flux_o);
+	free(flxerr_o);
+	free(qual_o);
+	if (cf_version == 2)
+	   {
+	   free(cnts1);
+	   free(cntserr1);
+	   free(cnts_o);
+	   free(cntserr_o);
+	   }
+	else
+	   {
+	   free(lcts1);
+	   free(bkgd1);
+	   free(wgts1);
+	   free(lcts_o);
+	   free(bkgd_o);
+	   free(wgts_o);
+	   }
+
+	/* is there only 1 extension in operand 2, so that we need to keep
+	 * the data we've read in, or do we need to make space to read the
+	 * next extension?
+	 */
+	if (!arg2_scalar && (i < next_2))
+	   {
+	   free(flux2);
+	   free(flxerr2);
+	   free(qual2);
+	   if (cf_version == 2)
+		{
+		free(cnts2);
+		free(cntserr2);
+		}
+	   else
+		{
+		free(lcts2);
+		free(wgts2);
+		free(bkgd2);
+		}
+	   }
+
+	} /* end of loop over next_1 */
+
+   /* add HISTORY lines to output file */
+   hdunum_o = 1;
+   FITS_movabs_hdu (outfits, hdunum_o, &hdutype_o, &status);
+
+   sprintf (comment, "cf_arith:  operation = %s", argv[2]);
+   FITS_write_history (outfits, comment, &status);
+   sprintf (comment, "cf_arith:  operand1 = %s", infile1);
+   FITS_write_history (outfits, comment, &status);
+   sprintf (comment, "cf_arith:  operand2 = %s", infile2);
+   FITS_write_history (outfits, comment, &status);
+
+   /* update exposure time in output header if necessary */
+   if (exptime_o != exptime_1)
+	{
+	FITS_update_key (outfits, TFLOAT, "EXPTIME", &exptime_o, expt_comment,
+			&status);
+	sprintf (comment, "cf_arith: EXPTIME = EXPTIME1 + EXPTIME2");
+	FITS_write_history (outfits, comment, &status);
+	}
+
+   /* update FILENAME keyword in output file */
+   FITS_update_key (outfits, TSTRING, "FILENAME", outfile, NULL, &status);
+
+   time (&timeval);
+   timestr = ctime (&timeval);
+   sprintf (comment, "cf_arith:  completed at %.24s", timestr);
+   /* over-write the trailing \n in timestr */
+/* following not needed when field width is specified as 24 above 
+   comment[strlen(comment)-1] = '\0';
+   padstr (comment, FLEN_CARD);
+*/
+   FITS_write_history (outfits, comment, &status);
+
+   /* Close the files. */
+
+    FITS_close_file(infits_1, &status);
+    if (!arg2_scalar)
+	FITS_close_file(infits_2, &status);
+    FITS_close_file(outfits, &status);
+
+    /* Enter a timestamp into the log. */
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+#ifdef SOLARIS
+    ieee_retrospective(stdout);
+#endif
+    return 0;
+}
+
+int	chkop (opstr)
+char	*opstr;
+{
+	if (!strcmp (opstr, "+"))
+	   return (PLUS);
+	else if (!strcmp (opstr, "-"))
+	   return (MINUS);
+	else if (!strcmp (opstr, "*"))
+	   return (MULT);
+	else if (!strcmp (opstr, "/"))
+	   return (DIV);
+	else if (!strcmp (opstr, "avg_t"))
+	   return (AVG_T);
+	else if (!strcmp (opstr, "avg_s"))
+	   return (AVG_S);
+	else if (!strcmp (opstr, "repl_d"))
+	   return (REPL_D);
+	else if (!strcmp (opstr, "repl_e"))
+	   return (REPL_E);
+	else if (!strcmp (opstr, "boxcar"))
+	   return (BOXCAR);
+	else if (!strcmp (opstr, "delta"))
+	   return (DELTA);
+	else if (!strcmp (opstr, "min"))
+	   return (MIN);
+	else if (!strcmp (opstr, "max"))
+	   return (MAX);
+	else if (!strcmp (opstr, "shift"))
+	   return (SHIFT);
+	else if (!strcmp (opstr, "bin"))
+	   return (BIN);
+	else if (!strcmp (opstr, "deriv"))
+	   return (DERIV);
+	else if (!strcmp (opstr, "addnoise"))
+	   return (ADDNOISE);
+	else
+	   return (0);
+}
+
+/* check_num (in_str) returns TRUE if in_str is a string representation of
+ * a valid number, FALSE otherwise.
+ * This is a simple-minded check:  just see if first char is +,-,digit.
+ */
+int	check_num (in_str)
+char	*in_str;
+{
+	if ((in_str[0] == '+') || (in_str[0] == '-'))
+	   {
+	   if (isdigit (in_str[1]))
+		return (TRUE);
+	   else
+		return (FALSE);
+	   }
+	if (isdigit (in_str[0]))
+	   return (TRUE);
+
+	return (FALSE);
+}
+
+void	padstr (pstr, len)
+char	*pstr;
+int	len;
+{
+	int	i, slen;
+
+	slen = strlen (pstr);
+	for (i=slen; i<len; i++)
+	   *(pstr + i) = ' ';
+
+	return;
+}
+/*      return a random number in range -1 -> 1 */
+double  rand1 ()
+{
+        long    random();
+        double  r;
+
+        r =  2. * (double) random() / (double)MAX_RAND - 1.;
+        return (r);
+}
+
diff --git a/src/analysis/cf_coadd.c b/src/analysis/cf_coadd.c
new file mode 100644
index 0000000..eaa5fe2
--- /dev/null
+++ b/src/analysis/cf_coadd.c
@@ -0,0 +1,192 @@
+/******************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ ******************************************************************************
+ *
+ * Synopsis:  cf_coadd root_name
+ *
+ *	      This program calls the routines that produce the exposure-level
+ *	      all files and the observation-level all, ano, and nvo files.
+ *
+ *            03/29/04  v0.1  bjg Begin work.
+ *            04/05/04  v0.2  bjg Remove unused variables
+ *                                Include unistd.h
+ *            06/07/04  v0.3  bjg Updated some keywords
+ *            08/12/04  v0.4  bjg Keywords QIK_COR and COMB_COR                      
+ *                                now set to COMPLETE.
+ *            08/26/04  v0.5  bjg Handle case aperture=RFPT 
+ *            03/17/05  v0.6  tc  Rename EXPTIME to OBSTIME in all extensions
+ *            08/22/05  v1.0  wvd Completely re-write for CalFUSE v3.1.7.
+ *				  Calls cf_make_all_exp for each exposure and
+ *				  cf_make_all_obs.csh only once.
+ *            08/27/07  v1.1  bot Changed i from int to long to match n
+ *				  Added L to corresponding values
+ *
+ *****************************************************************************/
+
+
+
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include <unistd.h>
+#include "calfuse.h"
+
+static char CF_PRGM_ID[] = "cf_coadd";
+static char CF_VER_NUM[] = "1.1";
+
+
+/*********************************************************************/
+
+int main(int argc, char *argv[])
+{
+
+  char asnf_file[120], filename[120], instmode[100], aper_string[100], aper_num[100];
+  fitsfile   *asnf_fits_ptr, *infits;
+  long n;
+  int status = 0;
+  long i;
+  int anynull;
+  FILE * ffile;
+  
+
+  char command0[256];
+
+
+  char    memname[120], *memname_ptr;
+  char    memtype[120], *memtype_ptr;
+  char ** memname_ptr2;
+  char ** memtype_ptr2;
+
+  char NULL_STR[] = {'\0'};
+
+  char file_present;
+  char expo_num_string[10];
+  int expo_num;
+
+  char know=0;
+
+  /* Enter a timestamp into the log. */
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+  cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+
+  memname_ptr=memname;
+  memtype_ptr=memtype;
+
+  memname_ptr2=&memname_ptr;
+  memtype_ptr2=&memtype_ptr;
+
+  
+  /* Input Parameters */
+  if (argc != 2)
+    cf_if_error("Usage: cf_coadd rootname");
+  
+  /*Open association file*/
+  
+  strcpy(asnf_file, argv[1]);
+  strcat(asnf_file, "asnf.fit");
+  FITS_open_file(&asnf_fits_ptr, asnf_file, READONLY, &status);
+  FITS_movabs_hdu(asnf_fits_ptr, 2, NULL, &status);
+  
+  
+  FITS_read_key(asnf_fits_ptr, TLONG, "NAXIS2", &n, NULL, &status);
+
+  
+  for (i=0L;i<n;i++){
+    
+    cf_if_fits_error(fits_read_col_str(asnf_fits_ptr, 1, i+1L, 1,1, NULL_STR,
+				       memname_ptr2, &anynull, &status));
+ 
+    cf_if_fits_error(fits_read_col_str(asnf_fits_ptr, 2, i+1L, 1,1, NULL_STR,
+				       memtype_ptr2, &anynull, &status));
+
+    cf_if_fits_error(fits_read_col_log(asnf_fits_ptr, 3, i+1L, 1, 1, 0,
+				       &file_present, &anynull, &status));
+    
+    if (file_present == FALSE) continue;
+    if (strncasecmp(memtype,"EXPOSURE",8)) continue;
+
+    strncpy(expo_num_string,&memname[8],3);
+    expo_num=atoi(expo_num_string);
+
+    if (expo_num==701) continue;
+        
+    strcpy(filename,memname);
+    strcat(filename,"1ahistfraw.fit");
+    strcpy(instmode,"hist");
+    ffile=fopen(filename,"r");
+    if (ffile == NULL) {
+      strcpy(instmode,"ttag");
+      strcpy(filename,memname);
+      strcat(filename,"1attagfraw.fit");
+      ffile=fopen(filename,"r");
+      if (ffile == NULL) {
+	printf("Warning: Expo %s not present\n",expo_num_string);
+	continue;
+      }
+      fclose(ffile);
+    }
+    else {
+      fclose(ffile);
+    }
+    
+    
+    if (!know) {
+
+      FITS_open_file(&infits, filename, READONLY, &status);
+      FITS_read_key(infits, TSTRING, "APERTURE", aper_string, NULL, &status);
+
+      if (!strncasecmp(aper_string,"LWRS",4)) strcpy(aper_num,"4");
+      if (!strncasecmp(aper_string,"MDRS",4)) strcpy(aper_num,"2");
+      if (!strncasecmp(aper_string,"HIRS",4)) strcpy(aper_num,"3");
+      if (!strncasecmp(aper_string,"PINH",4)) strcpy(aper_num,"1");
+      if (!strncasecmp(aper_string,"RFPT",4)) strcpy(aper_num,"4");
+
+      FITS_close_file(infits, &status);
+      know=1;
+    }
+
+
+    strcpy(command0,"cf_make_all_exp ");
+    strcat(command0,memname);
+    strcat(command0,"00all");
+    strcat(command0,aper_num);
+    strcat(command0,instmode);
+    strcat(command0,"fcal.fit ");
+    strcat(command0,memname);
+    strcat(command0,"1alif");
+    strcat(command0,aper_num);
+    strcat(command0,instmode);
+    strcat(command0,"fcal.fit ");
+    strcat(command0,memname);
+    strcat(command0,"1blif");
+    strcat(command0,aper_num);
+    strcat(command0,instmode);
+    strcat(command0,"fcal.fit ");
+    strcat(command0,memname);
+    strcat(command0,"2alif");
+    strcat(command0,aper_num);
+    strcat(command0,instmode);
+    strcat(command0,"fcal.fit ");
+    strcat(command0,memname);
+    strcat(command0,"2blif");
+    strcat(command0,aper_num);
+    strcat(command0,instmode);
+    strcat(command0,"fcal.fit ");
+
+    system(command0);
+
+  }
+
+  FITS_close_file(asnf_fits_ptr,&status);
+
+  sprintf(command0,"cf_make_all_obs.csh %s", asnf_file);
+  system(command0);
+
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done Processing");
+
+  return(EXIT_SUCCESS);
+
+}
diff --git a/src/analysis/cf_combine.c b/src/analysis/cf_combine.c
new file mode 100644
index 0000000..0b91009
--- /dev/null
+++ b/src/analysis/cf_combine.c
@@ -0,0 +1,544 @@
+/*******************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *****************************************************************************
+ *
+ * Synopsis:	cf_combine [-ahk] [-v level] file_list output_idf_file
+ *
+ * Description: This is a utility program that combines a series of
+ *		FUSE spectra in the form of FITS binary tables as produced
+ *		by the CalFUSE pipeline.  The files are combined by taking
+ *		the exposure-weighted mean of the fluxes and flux errors
+ *		and summing the counts.
+ *		It is assumed that the error arrays contain standard
+ *		deviations, not variances.
+ *
+ *
+ * History:     01/04/00        jwk     started work
+ *	        05/01/00 v1.2	jwk	handle SHORT qual arrays
+ *	        09/11/00 v1.3	jwk	remove include <sunmath.h>
+ *	        10/11/00 v1.4   jwk	update FILENAME keyword in output file
+ *              10/27/00 v1.5   peb     #ifdef ieee_retrospective
+ *              04/18/01 v1.6   wvd     Change declaration of timeval from
+ *                                      long to time_t
+ *              10/29/02 v1.7   wvd     Correct error in history line.
+ *	        05/19/03 v1.8	wvd	Two updates from jwk:
+ *					Close each input file in initial loop;
+ *                                      without this cfitsio crashes upon
+ *                                      opening the 60th file.
+ *	                                Weight each pixel by exposure time
+ *                                      after excluding 'bad' pixels.
+ *              12/15/03 v1.9	bjg	Changed to work on CalFUSE 3 spectrum
+ *                                      data format
+ *	        01/12/04 v1.10	bjg	npix_1 is now correct
+ *                                      copy header of 1st file instead of 2nd
+ *                                      Updated the name of some FITS cols that
+ *                                      were still using 2.4 format
+ *              03/09/04 v1.11	wvd     Change POTHOLE to QUALITY throughout.
+ *              04/05/04   -    bjg     Declarations for cf_wrspec7 and 
+ *                                      cf_wrspec_cf2
+ *                                      Remove unused variables
+ *              06/07/04 v1.12  bjg     Update some keywords (plantime,     
+ *                                      rawtime, exp_saa, nbadevnt ...)
+ *              04/07/05 v1.13  tc      Read 1D|2D spectrum format. Clean unused
+ *                                      variables. Allows one to shift a 2D
+ *                                      spectrum (2nd column in the filelist).
+ *                                      Use calloc rather than malloc. The
+ *                                      quality value is now the nearest short.
+ *                                      Update ROOTNAME keyword. Change EXP to
+ *                                      OBS if "-k" (optional). Proper use of
+ *                                      fclose() and rewind()
+ *              04/16/05 v1.14  tc      Use cf_read_col()
+ *              05/02/05 v1.15  wvd	Write NSPEC, SPEC###, WOFF### to 
+ *					output file header (primary HDU).
+ *              06/03/05 v1.16  wvd	Delete unused variables.
+ *              07/06/05 v1.17  wvd	Use fgets to read input file.
+ *					Change pix_shift to type int.
+ *              07/21/05 v1.18  wvd	Adopt the sign convention for spectral
+ *					shifts used by FUSE_REGISTER.
+ *              08/26/05 v1.19  wvd	Without arguments, don't return an
+ *					error.  Just print help and exit.
+ *              08/29/05 v1.20  wvd	If input list contains only file 
+ *					names, assume shifts are zero.
+ *              01/31/06 v1.21  wvd	Revise creation date of output file.
+ *              05/19/06 v1.22  wvd	Use same options as idf_combine.
+ *					Ignore spectra with EXP_STAT != 0.
+ *					Override with -a option.
+ *              05/22/06 v1.23  wvd	Rewrite program using a single while
+ *					loop.
+ *              05/23/06 v1.24  wvd	Properly normalize quality array.
+ *              05/26/06 v1.25  wvd	Include unistd.h
+ *              07/12/06 v1.26  wvd	Clean up i/o.
+ *              08/14/06 v1.27  wvd	Count SPEC### and WAVE### using ngood,
+ *					not nfiles.
+ *              05/04/07 v1.28  wvd	If the input file list contains a
+ *					blank line, skip to the next line.
+ *              08/27/07 v1.29  bot	Changed TINT to TLONG l.412
+ *					Added L to long l.125 to 136, 351, 378
+ *              04/04/08 v1.30  wvd	If -a flag is set, include files with
+ *					positive values of EXP_STAT, but not
+ *					those with negative values.
+ *		07/25/08 v1.31  wvd	Set output EXP_STAT keyword to lowest
+ *					non-negative value among input files.
+ *
+ ****************************************************************************/
+
+#include <time.h>
+#include <math.h>
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include <unistd.h>
+#include "calfuse.h"
+
+void cf_wrspec7(fitsfile *outfits, long npts, float *wave, float *flux, 
+		       float *error, long *counts, float *weights, 
+		       float *bkgd,short *quality);
+void cf_wrspec_cf2(fitsfile *outfits, int npts, float *wave,
+			  float *spec, float *errs, short *qual,
+			  float *counts, float *cntserr, int ncol, 
+			  int areaflag);
+
+static char CF_PRGM_ID[] = "cf_combine";
+static char CF_VER_NUM[] = "1.31";
+
+int main(int argc, char *argv[])
+{
+    char  *timestr;
+    time_t  timeval;
+    char  flist[80], infile[80], line[FLEN_CARD], outfile[80], string0[100];
+    char  comment[FLEN_CARD];
+    char  errstr[80];
+    int	  nargs, nfiles, ngood;
+    int   status=0;
+    int	  hdutype_1, hdutype_o;
+    int	  hdunum_1, hdunum_o;
+    long  npix_1;
+    int	  tfields_1, delta = 0;
+    long  j;
+    short *quality1;
+    float *wave1, *flux1, *error1, *weights1, *bkgd1;
+    
+    double *flux_o, *error_o, *quality_o;
+    float *weights_o, *bkgd_o;
+    long *counts_o, *counts1;
+    float *exptime_p;
+    float f1, shift, wpc;
+    
+    float exptime_1,  exptime_o = 0.;
+    float rawtime_1,  rawtime_o = 0.;
+    long plantime_1,  plantime_o = 0L;
+    long nbadevnt_1,  nbadevnt_o = 0L;
+    long nbadpha_1 ,  nbadpha_o = 0L;
+    long exp_bad_1 ,  exp_bad_o = 0L;
+    long exp_brst_1,  exp_brst_o = 0L;
+    long exp_hv_1,    exp_hv_o = 0L;
+    long exp_jitr_1,  exp_jitr_o = 0L;
+    long exp_lim_1 ,  exp_lim_o = 0L;
+    long exp_saa_1 ,  exp_saa_o = 0L;
+    long expnight_1,  expnight_o = 0L;
+
+    long nevents_1, nevents_o = 0L;
+    long exp_stat, exp_stat_out=999;
+
+    double	mjd_start, mjd_end;
+    double	mjd_start_o = 99999., mjd_end_o = 0.;
+    fitsfile *infits_1, *outfits;
+    FILE  *ifp;
+    char keyword[FLEN_KEYWORD], root_name[32];
+	int k_flag = 0;
+	
+	float *temp_float;
+	short *temp_short;
+	long *temp_long;
+
+	/* Function prototypes*/
+	void getnshift_float(float*, float*, long, int);
+	void getnshift_short(short*, short*, long, int);
+	void getnshift_long(long*, long*, long, int);	
+
+  int optc;
+  int ignore_exp_stat=TRUE;
+
+  char opts[] = "ahkv:";
+  char usage[] =
+    "Usage:\n"
+    "  cf_combine [-ahk]  [-v level] file_list output_idf_file\n";
+  char option[] =
+    "Options:\n"
+    "  -h:  this help message\n"
+    "  -v:  verbosity level (=1; 0 is silent)\n"
+    "  -a:  ignore EXP_STAT keyword\n"
+    "  -k:  Change EXP keywords to OBS\n";
+
+  verbose_level = 1;
+
+  /* Check number of options and arguments */
+  while ((optc = getopt(argc, argv, opts)) != -1) {
+    switch(optc) {
+
+    case 'h':
+      printf("%s\n%s", usage, option);
+      return 0;
+    case 'a':
+      ignore_exp_stat=FALSE;
+      break;
+    case 'v':
+      verbose_level = atoi(optarg);
+      break;
+    case 'k':
+      k_flag=1;
+      break;
+    }
+  }
+
+    /* Enter a timestamp into the log. */
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    /* Initialize error checking */
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+  if (argc < optind+2) {
+    printf("%s", usage);
+    return 1;
+  }
+
+    strcpy (flist, argv[optind]);
+    strcpy (outfile, argv[optind+1]);
+
+    if ((ifp = fopen (flist, "r")) == NULL)
+	   {
+	   sprintf (errstr, "Unable to open file %s\n", flist);
+	   cf_if_error (errstr);
+	   }
+
+  if (ignore_exp_stat)
+    cf_verbose(1,"Will include only files with EXP_STAT=0") ;
+  else
+    cf_verbose(1,"Will include only files with EXP_STAT >= 0") ;
+
+    nfiles = ngood = 0;
+
+    /* BIG LOOP THROUGH INPUT FILES */
+    while (fgets(line, FLEN_CARD, ifp) != NULL) {
+	nargs = sscanf(line, "%s %d", infile, &delta);
+	if (nargs == EOF) continue;
+	if (nargs == 1) delta = 0;
+	nfiles++;
+	cf_verbose (3, "Input file loop: nfiles = %d, file = %s", nfiles, infile);
+
+	/* Open input file */
+	FITS_open_file(&infits_1, infile, READONLY, &status);
+	FITS_read_key(infits_1, TLONG, "EXP_STAT", &exp_stat, NULL, &status);
+	FITS_read_key(infits_1, TDOUBLE, "EXPSTART", &mjd_start, NULL, &status);
+	FITS_read_key(infits_1, TDOUBLE, "EXPEND"  , &mjd_end  , NULL, &status);
+	FITS_read_key(infits_1, TFLOAT, "EXPTIME" , &exptime_1 , NULL, &status);
+	FITS_read_key(infits_1, TLONG, "NEVENTS", &nevents_1, NULL, &status);
+	FITS_read_key(infits_1, TFLOAT, "RAWTIME" , &rawtime_1 , NULL, &status);
+	FITS_read_key(infits_1, TLONG, "PLANTIME", &plantime_1, NULL, &status);
+	nevents_o += nevents_1;
+	rawtime_o  += rawtime_1;
+	plantime_o += plantime_1;
+
+	if (mjd_start < mjd_start_o) mjd_start_o = mjd_start;
+	if (mjd_end > mjd_end_o) mjd_end_o = mjd_end;
+	
+	/* Create output file, copy the header from the input file */
+	if (nfiles==1)
+	  {
+	    /* open output file */
+	    remove(outfile);	/* In case the old file name exists */    
+	    FITS_create_file (&outfits, outfile, &status);
+	    FITS_copy_header(infits_1, outfits, &status);
+	    FITS_write_date(outfits, &status);
+
+	    FITS_read_key(infits_1, TFLOAT, "WPC" , &wpc , NULL, &status);
+		
+	    /* Now go to the second HDU and figure out how long the arrays are. */
+	    hdunum_1 = 2;
+	    FITS_movabs_hdu(infits_1, hdunum_1, &hdutype_1, &status);
+	    FITS_read_key(infits_1, TINT, "TFIELDS", &tfields_1, NULL, &status);
+
+	    if (tfields_1 != 7)
+	      {
+		sprintf (errstr, "Expecting 7 cols, found %d\n", tfields_1);
+		cf_if_error (errstr);
+	      }
+		
+	    npix_1 = cf_read_col(infits_1, TFLOAT, "WAVE", (void **) &wave1);
+
+	    /* Allocate data arrays (calloc initializes to 0 by default). */
+	    exptime_p = (float *) cf_calloc(npix_1, sizeof(float));
+	    
+	    flux1 = (float *) cf_calloc(npix_1, sizeof(float));
+	    error1 = (float *) cf_calloc(npix_1, sizeof(float));
+	    counts1 = (long *) cf_calloc(npix_1, sizeof(long));
+	    weights1 = (float *) cf_calloc(npix_1, sizeof(float));
+	    bkgd1 = (float *) cf_calloc(npix_1, sizeof(float));
+	    quality1 = (short *) cf_calloc(npix_1, sizeof(short));
+		
+	    flux_o = (double *) cf_calloc(npix_1, sizeof(double));
+	    error_o = (double *) cf_calloc(npix_1, sizeof(double));
+	    counts_o = (long *) cf_calloc(npix_1, sizeof(long));
+	    weights_o = (float *) cf_calloc(npix_1, sizeof(float));
+	    bkgd_o = (float *) cf_calloc(npix_1, sizeof(float));
+	    quality_o = (double *) cf_calloc(npix_1, sizeof(double));
+		
+            hdunum_1 = 1;
+            FITS_movabs_hdu(infits_1, hdunum_1, &hdutype_1, &status);
+
+	  }  /* end of if(nfiles==1) */
+	
+	/* Set EXP_STAT to lowest non-negative value in input files. */
+	if (exp_stat_out > exp_stat && exp_stat >= 0) exp_stat_out = exp_stat;
+
+	/* Skip files with EXP_TIME = 0 or EXP_STAT != 0. */
+	if (ignore_exp_stat && exp_stat != 0) {
+	    cf_if_warning("File %s rejected. EXP_STAT not equal to zero. Use -a flag to override.",
+		infile) ;
+	    FITS_close_file(infits_1,&status);
+	    continue;
+	}
+
+	/* Never include files with negative values of EXP_STAT. */
+	else if (exp_stat < 0) {
+	    cf_if_warning("File %s rejected. EXP_STAT less than zero.", infile) ;
+	    FITS_close_file(infits_1,&status);
+	    continue;
+	}
+
+	if (exptime_1 < 1.) {
+	    cf_verbose (3, "Rejecting file %s: EXPTIME = %f", infile, exptime_1);
+	    FITS_close_file(infits_1,&status);
+	    continue;
+	}
+	ngood++;
+	
+	FITS_read_key(infits_1, TLONG, "NBADEVNT", &nbadevnt_1, NULL, &status);
+	FITS_read_key(infits_1, TLONG, "NBADPHA" , &nbadpha_1 , NULL, &status);
+	FITS_read_key(infits_1, TLONG, "EXP_BAD" , &exp_bad_1 , NULL, &status);
+	FITS_read_key(infits_1, TLONG, "EXP_BRST", &exp_brst_1, NULL, &status);
+	FITS_read_key(infits_1, TLONG, "EXP_HV",   &exp_hv_1,   NULL, &status);
+	FITS_read_key(infits_1, TLONG, "EXP_JITR", &exp_jitr_1, NULL, &status);
+	FITS_read_key(infits_1, TLONG, "EXP_LIM" , &exp_lim_1 , NULL, &status);
+	FITS_read_key(infits_1, TLONG, "EXP_SAA" , &exp_saa_1 , NULL, &status);
+	FITS_read_key(infits_1, TLONG, "EXPNIGHT", &expnight_1, NULL, &status);
+
+	exptime_o  += exptime_1;
+	nbadevnt_o += nbadevnt_1;
+	nbadpha_o  += nbadpha_1; 
+	exp_bad_o  += exp_bad_1;
+	exp_saa_o  += exp_saa_1;
+	exp_lim_o  += exp_lim_1;
+	exp_brst_o += exp_brst_1;
+	exp_hv_o   += exp_hv_1;
+	exp_jitr_o += exp_jitr_1;
+	expnight_o += expnight_1;
+
+	/* Read the data from input file (HDU 2) */
+	hdunum_1 = 2;
+	FITS_movabs_hdu(infits_1, hdunum_1, &hdutype_1, &status);
+	
+	(void) cf_read_col(infits_1, TFLOAT, "FLUX", (void **) &temp_float);
+	getnshift_float(flux1, temp_float, npix_1, delta);
+	free(temp_float);
+	
+	(void) cf_read_col(infits_1, TFLOAT, "ERROR", (void **) &temp_float);
+	getnshift_float(error1, temp_float, npix_1, delta);
+	free(temp_float);
+	
+	(void) cf_read_col(infits_1, TSHORT, "QUALITY", (void **) &temp_short);
+	getnshift_short(quality1, temp_short, npix_1, delta);
+	free(temp_short);
+			
+	(void) cf_read_col(infits_1, TLONG, "COUNTS", (void **) &temp_long);
+	getnshift_long(counts1, temp_long, npix_1, delta);
+	free(temp_long);
+			
+	(void) cf_read_col(infits_1, TFLOAT, "WEIGHTS", (void **) &temp_float);
+	getnshift_float(weights1, temp_float, npix_1, delta);
+	free(temp_float);
+			
+	(void) cf_read_col(infits_1, TFLOAT, "BKGD", (void **) &temp_float);
+	getnshift_float(bkgd1, temp_float, npix_1, delta);
+	free(temp_float);
+
+        /* Average fluxes, weighting by exposure time; add counts. */
+        /* Include only pixels with non-zero quality flags. */
+        for (j=0L; j<npix_1; j++) {
+	    if (quality1[j] > 0) {
+	       f1 = exptime_1;
+	       exptime_p[j] += f1;
+	       flux_o[j]    += f1 * flux1[j];
+	       error_o[j]   += f1 * f1 * (double) error1[j]*error1[j];
+	       counts_o[j]  += counts1[j];
+	       weights_o[j] += weights1[j];
+	       bkgd_o[j]    += bkgd1[j];
+	       quality_o[j] += f1 * (double) quality1[j];
+	    }
+	}
+	
+	FITS_close_file(infits_1, &status);
+
+	/* Write input file name and spectral shift to output file header. */
+	sprintf(keyword, "SPEC%03d", ngood);
+	FITS_update_key(outfits, TSTRING, keyword, infile, NULL, &status);
+	sprintf(keyword, "WOFF%03d", ngood);
+	shift = delta * wpc;
+	FITS_update_key(outfits, TFLOAT, keyword, &shift, "[A]", &status);
+
+
+      }  /* end of loop over input files */
+
+    /* Convert variances back to sigma. Normalize flux, error, and quality by EXPTIME. 
+	Convert from doubles to floats. */
+    for (j=0L; j<npix_1; j++) if (exptime_p[j] > 0.) {
+	flux1[j] = flux_o[j] / exptime_p[j];
+	error1[j] = sqrt(error_o[j]) / exptime_p[j];
+	quality1[j] = cf_nint(quality_o[j] / exptime_p[j]);
+    }
+    else {
+	flux1[j] = error1[j] = 0.;
+	quality1[j] = 0;
+    }
+    
+	/* Write the output file (in multi-row format). */
+    cf_wrspec7 (outfits, npix_1, wave1, flux1, error1, counts_o, weights_o, bkgd_o, quality1);
+    
+    free(exptime_p);
+    free(wave1);
+    free(flux1);
+    free(error1);
+    free(bkgd1);
+    free(counts1);
+    free(weights1);
+    free(quality1);
+    free(flux_o);
+    free(error_o);
+    free(quality_o);
+    free(bkgd_o);
+    free(counts_o);
+    free(weights_o);
+    
+    hdunum_o = 1;
+    FITS_movabs_hdu (outfits, hdunum_o, &hdutype_o, &status);
+
+	    /* update output header keywords*/
+
+	    FITS_update_key(outfits, TLONG, "EXP_STAT",  &exp_stat_out, NULL, &status);
+	    FITS_update_key(outfits, TDOUBLE, "EXPSTART", &mjd_start_o, NULL, &status);
+	    FITS_update_key(outfits, TDOUBLE, "EXPEND", &mjd_end_o  , NULL, &status);
+	    FITS_update_key(outfits, TFLOAT, "EXPTIME", &exptime_o , NULL, &status);
+	    FITS_update_key(outfits, TLONG, "NEVENTS",  &nevents_o, NULL, &status);
+	    FITS_update_key(outfits, TFLOAT, "RAWTIME", &rawtime_o , NULL, &status);
+	    FITS_update_key(outfits, TLONG, "PLANTIME", &plantime_o, NULL, &status);
+	    FITS_update_key(outfits, TLONG, "NBADEVNT", &nbadevnt_o, NULL, &status);
+	    FITS_update_key(outfits, TLONG, "NBADPHA" , &nbadpha_o , NULL, &status);
+	    FITS_update_key(outfits, TLONG, "EXP_BAD" , &exp_bad_o , NULL, &status);
+	    FITS_update_key(outfits, TLONG, "EXP_BRST", &exp_brst_o, NULL, &status);
+	    FITS_update_key(outfits, TLONG, "EXP_HV",   &exp_hv_o, NULL, &status);
+	    FITS_update_key(outfits, TLONG, "EXP_JITR", &exp_jitr_o, NULL, &status);
+	    FITS_update_key(outfits, TLONG, "EXP_LIM" , &exp_lim_o , NULL, &status);
+	    FITS_update_key(outfits, TLONG, "EXP_SAA" , &exp_saa_o , NULL, &status);
+	    FITS_update_key(outfits, TLONG, "EXPNIGHT", &expnight_o, NULL, &status);
+
+	    /* update FILENAME keyword in output file */
+	    FITS_update_key(outfits, TSTRING, "FILENAME", outfile, NULL, &status);
+	    
+	    strcpy(string0, "COMBINED SPECTRA");
+	    FITS_update_key(outfits, TSTRING, "FILETYPE", string0, NULL, &status);
+
+	    sprintf(string0, "000");
+	    FITS_update_key(outfits, TSTRING, "EXP_ID", string0, NULL, &status);
+		
+	    FITS_read_key(outfits, TSTRING, "ROOTNAME", root_name, NULL, &status);
+	    sprintf(string0, "%.8s000", root_name);
+	    FITS_update_key(outfits, TSTRING, "ROOTNAME", string0, NULL, &status);
+
+	    FITS_update_key(outfits, TINT, "NSPEC", &ngood,
+		"Number of combined spectral files", &status);
+
+	if (k_flag)
+	{
+	    cf_if_fits_error(fits_modify_name(outfits, "EXP_STAT", "OBS_STAT", &status));
+	    cf_if_fits_error(fits_modify_name(outfits, "EXPSTART", "OBSSTART", &status));
+	    cf_if_fits_error(fits_modify_name(outfits, "EXPEND", "OBSEND", &status));
+	    cf_if_fits_error(fits_modify_name(outfits, "EXPTIME", "OBSTIME", &status));
+	    cf_if_fits_error(fits_modify_name(outfits, "EXPNIGHT", "OBSNIGHT", &status));
+	}
+	else {
+	    /* Add HISTORY lines to output file */
+	    if (ignore_exp_stat) {
+	    sprintf (comment, "cf_combine:  Including only files with EXP_STAT=0");
+	    FITS_write_history (outfits, comment, &status);
+	    }
+
+	    else {
+	    sprintf (comment, "cf_combine:  Including only files with EXP_STAT >= 0");
+	    FITS_write_history (outfits, comment, &status);
+	    }
+
+	    sprintf (comment, "cf_combine:  File list = %s", flist);
+	    FITS_write_history (outfits, comment, &status);
+    
+	    time (&timeval);
+	    timestr = ctime (&timeval);
+	    sprintf (comment, "cf_combine:  Completed on %.24s", timestr);
+	    FITS_write_history (outfits, comment, &status);
+	}
+	
+    /* Close the files. */
+	fclose(ifp);
+    FITS_close_file(outfits, &status);
+    
+    /* Enter a timestamp into the log. */
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+#ifdef SOLARIS
+    ieee_retrospective(stdout);
+#endif
+    return 0;
+}
+
+
+void getnshift_float (float *out_vect, float *in_vect, long n, int delta)
+{
+	long k, ind;
+	
+	for (k = 0; k < n; k++)	
+	{
+		ind = k - delta;
+		if((ind >= 0) && (ind < n))
+			out_vect[k] = in_vect[ind];
+		else
+			out_vect[k] = 0;
+	}
+}
+
+void getnshift_short (short *out_vect, short *in_vect, long n, int delta)
+{
+	long k, ind;
+	
+	for (k = 0; k < n; k++)	
+	{
+		ind = k - delta;
+		if((ind >= 0) && (ind < n))
+			out_vect[k] = in_vect[ind];
+		else
+			out_vect[k] = 0;
+	}
+}
+
+void getnshift_long (long *out_vect, long *in_vect, long n, int delta)
+{
+	long k, ind;
+	
+	for (k = 0; k < n; k++)	
+	{
+		ind = k - delta;
+		if((ind >= 0) && (ind < n))
+			out_vect[k] = in_vect[ind];
+		else
+			out_vect[k] = 0;
+	}
+}
diff --git a/src/analysis/cf_make_900_obs.csh b/src/analysis/cf_make_900_obs.csh
new file mode 100755
index 0000000..9edbc70
--- /dev/null
+++ b/src/analysis/cf_make_900_obs.csh
@@ -0,0 +1,193 @@
+#!/usr/local/bin/tcsh -f
+
+#******************************************************************************
+#*              Johns Hopkins University 
+#*              Center For Astrophysical Sciences
+#*              FUSE
+#******************************************************************************
+#*
+#* Synopsis:    cf_make_900_obs.csh association_file
+#*
+#* Description: This routine is derived from cf_make_all_obs.csh, but modified
+#*		to consider only 900+ (airglow) files.  Output is a single
+#*		quick-look image of the airglow spactrum.
+#*
+#*  		Extracted spectra are combined, not IDF files.
+#*
+#*              When an expected data set is missing, the script stops, cleans
+#*              the directory, and returns 1.
+#*
+#* History:     08/08/08   1.00	 wvd   Create separate quick-look image
+#*					for 900+ (airglow) exposures.
+#*					Always combine extracted spectra.  If
+#*					cf_xcorr fails, combine with no shift.
+#* 		08/08/08   1.01	 wvd   Rename airglow quick-look file to
+#*					M112580100000airgttagf.gif
+#*
+#*****************************************************************************/
+
+# Delete files after processing?  (Default is no.)
+#set DELETE_IDF                 # Delete intermediate data files
+set DELETE_BPM                 # Delete bad-pixel map files
+
+# Set program path
+set rm = "/bin/rm -f"
+
+set cf_xcorr = cf_xcorr
+set cf_combine = cf_combine
+set cf_pack = cf_pack
+set cf_nvo = cf_nvo
+set idl_obsplot = idl_obsplot.pl
+set modhead = modhead
+
+# Init var list
+set detector = (1a 2b)
+set channel = (lif sic)
+set resolution = (2 3 4)
+set obsmod = (hist ttag)
+
+# Determine the root name and the program ID
+set asnf = $1
+set rn = ${asnf:s/000asnf.fit//}
+set pid = `echo $rn | awk '{print substr($1, 1, 4)}'`
+
+# Determine the object class
+set tmp_file = `ls ${rn}*fcal.fit | awk '{if (NR == 1) print}'`
+set tmp_buf = `$modhead $tmp_file OBJCLASS`
+set objclass = $tmp_buf[2]
+
+# Clean tmp files that the script will create (safe)
+$rm tmp_xcorr.res tmp_combine.lis 
+$rm tmp_good_exp.lis tmp_exp.lis tmp_seg_dn.lis 
+$rm DN_${rn}*.fit
+
+foreach om ($obsmod)
+    foreach res ($resolution)    
+        foreach chan ($channel)    
+            foreach det ($detector)
+            	
+		set ignore_exp_stat = ''
+		if ($om == hist) set ignore_exp_stat = -a
+		if ($pid == S100) set ignore_exp_stat = -a
+		if ($pid == M106) set ignore_exp_stat = -a
+		
+		# Find exposures that match the current segment
+                set seg = $det$chan$res$om
+                set readfiles = 0
+                ls ${rn}9[0-9][0-9]${seg}fcal.fit |& grep -v 000${seg} > tmp_exp.lis  # Keep only "9xx" exposures
+                if ($? == 0) then 
+                	set readfiles = 2
+			set ignore_exp_stat = -a
+                endif
+                
+                if ($readfiles >= 1) then  # There are one or more exposures
+                
+                    echo " "
+                    echo "*** Processing: $seg ***"
+                    # [1a][lif] -> [1b][lif], [2b][lif] -> [2a][lif] etc...
+                    if ($det == 1a) set det2 = 1b
+                    if ($det == 2b) set det2 = 2a
+                    set seg2 = $det2$chan$res$om
+                
+                    echo "----- cf_xcorr input   -----"
+                    cat tmp_exp.lis
+                    echo "----------------------------"
+                    $cf_xcorr tmp_exp.lis tmp_xcorr.res  # Compute shift and sigma_shift
+                    echo "----- cf_xcorr results -----"
+                    cat tmp_xcorr.res
+                    echo "----------------------------"
+
+                    awk '{if ($3 >= 0) {print $6, $2} else {print $6}}' tmp_xcorr.res > tmp_good_exp.lis
+                    
+                        #
+                        # --- Path 1: Optimize resolution ---
+                        #
+                    
+                        echo "Optimize resolution..."
+                        set n_good = `cat tmp_good_exp.lis | wc -l`
+                    
+                        # Extract [Day + Night] spectra
+                        set s = DN_${rn}900${seg}fcal.fit
+                        awk '{print "'$rn'"$1"'$seg'fcal.fit",$2}' tmp_good_exp.lis > tmp_combine.lis  # Combine $seg [dn]
+			# echo "----- Combining Files ----- "
+			# cat tmp_combine.lis
+			# echo "Output: " $s
+                        $cf_combine -k $ignore_exp_stat tmp_combine.lis $s
+                        # $modhead "${s}[1]" NUM_EXP $n_good
+                        $modhead "${s}[1]" COMBMETH XCORR
+                        echo $s >> tmp_seg_dn.lis
+                    
+                        set s = DN_${rn}900${seg2}fcal.fit
+                        awk '{print "'$rn'"$1"'$seg2'fcal.fit",$2}' tmp_good_exp.lis > tmp_combine.lis  # Combine $seg2 [dn]
+			# echo "----- Combining Files ----- "
+			# cat tmp_combine.lis
+			# echo "Output: " $s
+                        $cf_combine -k $ignore_exp_stat tmp_combine.lis $s
+                        # $modhead "${s}[1]" NUM_EXP $n_good
+                        $modhead "${s}[1]" COMBMETH XCORR
+                        echo $s >> tmp_seg_dn.lis
+                
+                endif
+            end
+            
+            $rm tmp_xcorr.res tmp_combine.lis
+            $rm tmp_good_exp.lis tmp_exp.lis 
+            
+        end
+        
+        # Pack the 8 [detector][channel] pairs together
+        if (-e tmp_seg_dn.lis) then
+    
+            set fcal_all = ${rn}00900all$res${om}fcal.fit  # Final output name
+            $rm $fcal_all  # Clean (safe)
+            set n_segs = `cat tmp_seg_dn.lis | wc -l`
+    
+            if (!($n_segs == 8)) then
+    
+                @ mseg = 8 - $n_segs
+                echo "ERROR: $mseg (day + night) segments are missing"
+                $rm tmp_seg_dn.lis
+                goto crash
+
+            else
+    
+                $cf_pack tmp_seg_dn.lis $fcal_all
+                $rm tmp_seg_dn.lis
+    
+                # Plot figures, delete unwanted files
+                $idl_obsplot {$rn} airglow
+		mv ${rn}00900spec${om}f.gif ${rn}00000airg${om}f.gif
+		$rm ${rn}00900lif*.gif ${rn}00900sic*.gif
+		$rm $fcal_all
+        
+            endif
+        endif
+    end
+end
+
+# Clean [dn] files. 
+$rm DN_${rn}*.fit
+
+# Delete IDF files
+if $?DELETE_IDF then
+    echo "NOTE: Deleting intermediate data files."
+    $rm ${rn}*idf.fit
+endif
+
+# Delete bad-pixel-map (bpm) files
+if $?DELETE_BPM then
+    echo "NOTE: Deleting bad pixel map (bpm) files."
+    $rm ${rn}*bpm.fit
+endif
+
+exit(0)
+
+crash:  # Procedure when script crashes
+
+# Clean directory
+$rm tmp_xcorr.res tmp_combine.lis 
+$rm tmp_good_exp.lis tmp_exp.lis tmp_seg_dn.lis 
+$rm DN_*.fit
+
+# Return 1
+exit(1)
diff --git a/src/analysis/cf_make_all_exp.c b/src/analysis/cf_make_all_exp.c
new file mode 100644
index 0000000..926ac2c
--- /dev/null
+++ b/src/analysis/cf_make_all_exp.c
@@ -0,0 +1,91 @@
+/*****************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *****************************************************************************
+ *
+ * Synopsis: cf_make_all_exp output_filename input1 input2 input3 input4
+ *
+ * Description: For a single exposure, copies header of channel with largest	
+ *              value of EXPTIME into an otherwise empty "all" file.
+ *		Input files should represent each of the four FUSE channels.
+ *
+ *
+ * History:	08/11/05	wvd	v1.0	Based on cf_quicklook.
+ *
+ ****************************************************************************/
+
+#include <stdlib.h>
+#include <stdio.h>
+#include <string.h>
+#include "calfuse.h"
+
+static char CF_PRGM_ID[]= "cf_make_all_exp";
+static char CF_VER_NUM[]= "1.0";
+
+int main(int argc,char *argv[]){
+  
+	char	*corrected_filename, *string_pointer;
+	char	comment[FLEN_CARD], datestr[FLEN_CARD];
+	int	i, nextend=0, ref_file=2, timeref;
+	int	status=0;
+	float	exptime, max_exptime;
+
+	fitsfile *infits,*outfits; 
+
+	if (argc != 6) {
+		printf("Incorrect number of arguments.\n");
+		printf("Calling sequence:  cf_make_all_exp output_filename "
+			"input1 input2 input3 input4\n");
+		exit(1);
+	}
+
+	/* Initialize error checking. */
+	cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+	cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Started execution.");
+
+	/* Determine the channel with the longest exposure time */
+
+	max_exptime = 0;
+	for (i = 0; i < 4; i++) {
+		FITS_open_file(&infits, argv[2+i], READONLY, &status);
+		FITS_read_key(infits, TFLOAT, "EXPTIME", &exptime, NULL, &status);
+		if (exptime >= max_exptime) {
+        		ref_file = 2 + i;
+    			max_exptime = exptime;
+		}
+		FITS_close_file(infits, &status);
+	}
+
+	/* Copy header from the reference file to the exposure-level "all" file. */
+
+	FITS_open_file(&infits, argv[ref_file], READONLY, &status);
+	FITS_create_file(&outfits, argv[1], &status);
+	FITS_copy_hdu(infits, outfits, 0, &status);
+
+	/* Modify a few header keywords. */
+	string_pointer = strrchr(argv[1],'/');
+	if (string_pointer == NULL) corrected_filename = argv[1];
+	else corrected_filename = &(string_pointer[1]);
+	FITS_update_key(outfits, TINT, "NEXTEND", &nextend, NULL, &status);
+	FITS_write_date(outfits, &status);
+	FITS_update_key(outfits, TSTRING, "FILENAME", corrected_filename, NULL, &status);
+	FITS_update_key(outfits, TSTRING, "FILETYPE", "EXPOSURE-LEVEL STATUS FILE", NULL, &status);
+
+	/* Add a note warning that this file contains no data. */
+        FITS_write_comment(outfits, "  ", &status);
+        FITS_write_comment(outfits,
+                "This file contains no data.", &status);
+        FITS_write_comment(outfits,
+                "Its header keywords are used by the DADS cataloging software.", &status);
+        fits_get_system_time(datestr, &timeref, &status);
+        sprintf(comment, "CalFUSE v%s   %.10s", CALFUSE_VERSION, datestr);
+        FITS_write_comment(outfits, comment, &status);
+        FITS_write_comment(outfits, "  ", &status);
+
+
+	FITS_close_file(infits, &status);
+	FITS_close_file(outfits,&status);
+
+	return EXIT_SUCCESS;
+}
diff --git a/src/analysis/cf_make_all_obs.csh b/src/analysis/cf_make_all_obs.csh
new file mode 100755
index 0000000..2a97247
--- /dev/null
+++ b/src/analysis/cf_make_all_obs.csh
@@ -0,0 +1,555 @@
+#!/usr/local/bin/tcsh -f
+
+#******************************************************************************
+#*              Johns Hopkins University 
+#*              Center For Astrophysical Sciences
+#*              FUSE
+#******************************************************************************
+#*
+#* Synopsis:    cf_make_all_obs.csh association_file
+#*
+#* Description: Creates 3 files from Calfuse output (properly run):
+#*
+#*                1) An "all" file containing 1 extension per detector (= 8).
+#*                   Each extension contains a combined spectrum from the set
+#*                   of exposures, using "Xcorr" or "Background" method.
+#*                2) In the case of TTAG data, creates an "ano" file. Same as
+#*                   the "all" file but considering "night only" exposure time.
+#*                3) A National Virtual Observatory "nvo" file. One extension
+#*                   containing wavelengths that span the whole FUSE range.
+#*
+#*              The Xcorr method consists of co-adding spectra, the latter
+#*              being corrected for a possible shift. The Background method
+#*              consists of combining all the IDF files.
+#*
+#*              The Xcorr test is performed on 4 (detector, channel) pairs, the
+#*              method of other pairs are given by them:
+#*                LiF 1a -> Lif 1b
+#*                LiF 2b -> LiF 2a
+#*                SiC 1a -> Sic 1b
+#*                Sic 2b -> Sic 2a
+#*              In the script, the left segments are referred as to $seg (or 
+#*              $det) and the right segments are referred as to $seg2 (or
+#*              $det2).
+#*  
+#*              When an expected data set is missing, the script stops, cleans
+#*              the directory, and returns 1.
+#*
+#* History:     04/15/05   1.0   tc    First release
+#*		08/22/05   1.1   wvd   Argument is name of association file.
+#*		10/20/05   1.2   wvd   Use idl_obsplot.pl to call cf_obsplot.
+#*		10/25/05   1.3   wvd   Add option to delete BPM or IDF files.
+#*		03/21/06   1.4   wvd   If there's only one exposure, always
+#*					follow the cross-correlation path.
+#*				       Don't check the number of night-only
+#*				      	spectra before calling cf_pack.
+#*		03/28/06   1.5   wvd   If there's no good time in any exposure,
+#*					follow the cross-correlation path.
+#*		04/27/06   1.6   wvd   Be smarter when discarding 000 files.
+#*					Always use cross-corr for HIST data.
+#*		05/23/06   1.7   wvd   Move -k to proper spot after cf_combine.
+#*		06/02/06   1.8   wvd   If OBJCLASS = 7 (Sky Background)
+#*					always combine IDF files.
+#*		06/22/06   1.9   wvd   Call idf_combine with -z flag.
+#*		05/24/07   1.10  bot   If only 900+ spectra are available,
+#*					use them.
+#*		04/04/08   1.11	 bot   Ignore EXP_STAT in cf_combine for HIST
+#*					data.
+#*		07/25/08   1.12	 wvd   Ignore EXP_STAT in cf_combine and
+#*					idf_combine for BR-EARTH observations
+#*					(S100, M106, and 900+ exposures).
+#*		08/08/08   1.13	 wvd   Don't ignore EXP_STAT for 900+ exposures.
+#*		08/15/08   1.14	 wvd   Call cf_make_900_obs.csh
+#*					to make quick-look airglow plot.
+#*
+#*****************************************************************************/
+
+# Delete files after processing?  (Default is no.)
+#set DELETE_IDF                 # Delete intermediate data files
+#set DELETE_BPM                 # Delete bad-pixel map files
+
+# Set program path
+set rm = "/bin/rm -f"
+
+set cf_xcorr = cf_xcorr
+set cf_combine = cf_combine
+set cf_pack = cf_pack
+set cf_nvo = cf_nvo
+set idl_obsplot = idl_obsplot.pl
+set modhead = modhead
+
+#set cf_xcorr = /home/vela/civeit/Work/CalFuse/Xcorr/New/cf_xcorr
+#set cf_combine = /home/vela/civeit/Work/CalFuse/Shiftexp/cf_combine
+#set cf_pack = /home/vela/civeit/Work/CalFuse/Pack/cf_pack
+#set cf_nvo = /home/vela/civeit/Work/CalFuse/Nvo/cf_nvo
+#set modhead = /home/vela/civeit/local/bin/modhead
+
+#set cf_obsplot = /data1/fuse/calfuse/v3.1/idl/cf_obsplot.pro
+
+# Init var list
+set detector = (1a 2b)
+set channel = (lif sic)
+set resolution = (2 3 4)
+set obsmod = (hist ttag)
+
+# Determine the root name and the program ID
+set asnf = $1
+set rn = ${asnf:s/000asnf.fit//}
+set pid = `echo $rn | awk '{print substr($1, 1, 4)}'`
+
+# Determine the object class
+set tmp_file = `ls ${rn}*fcal.fit | awk '{if (NR == 1) print}'`
+set tmp_buf = `$modhead $tmp_file OBJCLASS`
+set objclass = $tmp_buf[2]
+
+# Clean tmp files that the script will create (safe)
+$rm tmp_xcorr.res tmp_bpm1.lis tmp_bpm2.lis tmp_combine.lis tmp_night_exp.lis
+$rm tmp_all_night_exp.lis tmp_good_exp.lis tmp_exp.lis tmp_seg_dn.lis tmp_seg_no.lis
+$rm DN_${rn}*.fit NO_${rn}*.fit
+
+foreach om ($obsmod)
+    foreach res ($resolution)    
+        foreach chan ($channel)    
+            foreach det ($detector)
+            	
+		set ignore_exp_stat = ''
+		if ($om == hist) set ignore_exp_stat = -a
+		if ($pid == S100) set ignore_exp_stat = -a
+		if ($pid == M106) set ignore_exp_stat = -a
+		
+		# Find exposures that match the current segment
+                set seg = $det$chan$res$om
+                set readfiles = 0
+                ls ${rn}[0-8][0-9][0-9]${seg}fcal.fit |& grep -v 000${seg} > tmp_exp.lis  # Reject EXP "9xx" and "000"
+                
+                if ($? == 0) then 
+                	set readfiles = 1
+                else
+                	ls ${rn}9[0-9][0-9]${seg}fcal.fit |& grep -v 000${seg} > tmp_exp.lis  # Keep only "9xx" exposures
+                	if ($? == 0) set readfiles = 2
+                endif
+                
+                if ($readfiles >= 1) then  # There are one or more exposures
+                
+                    echo " "
+                    echo "*** Processing: $seg ***"
+                    # [1a][lif] -> [1b][lif], [2b][lif] -> [2a][lif] etc...
+                    if ($det == 1a) set det2 = 1b
+                    if ($det == 2b) set det2 = 2a
+                    set seg2 = $det2$chan$res$om
+                
+                    echo "----- cf_xcorr input   -----"
+                    cat tmp_exp.lis
+                    echo "----------------------------"
+                    $cf_xcorr tmp_exp.lis tmp_xcorr.res  # Compute shift and sigma_shift
+                    echo "----- cf_xcorr results -----"
+                    cat tmp_xcorr.res
+                    echo "----------------------------"
+
+                    awk '{if ($5 > 0) print $6, $4, $5}' tmp_xcorr.res > tmp_all_night_exp.lis
+                    awk '{if ($3 >= 0) print $6, $2}' tmp_xcorr.res > tmp_good_exp.lis
+                    awk '{if (($3 >= 0) && ($5 > 0)) print $6, $2, $4, $5}' tmp_xcorr.res > tmp_night_exp.lis
+                    set time_good = `awk 'BEGIN{$t = 0} {if ($3 >= 0) $t = $t + $4} END{print $t}' tmp_xcorr.res`
+                    set time_bad  = `awk 'BEGIN{$t = 0} {if ($3 < 0)  $t = $t + $4} END{print $t}' tmp_xcorr.res`
+                    echo "Xcorr time: $time_good  -  Background time: $time_bad"
+                    set n_exp = `cat tmp_xcorr.res | wc -l`
+                
+                    if (($time_good > 2 * $time_bad && $objclass != 7) || ($time_good == 0 && $time_bad == 0) || $n_exp == 1 || $om == hist) then
+                    
+                        #
+                        # --- Path 1: Optimize resolution ---
+                        #
+                    
+                        echo "Optimize resolution..."
+                        set n_good = `cat tmp_good_exp.lis | wc -l`
+                    
+                        # Extract [Day + Night] spectra
+                        set s = DN_${rn}000${seg}fcal.fit
+                        awk '{print "'$rn'"$1"'$seg'fcal.fit",$2}' tmp_good_exp.lis > tmp_combine.lis  # Combine $seg [dn]
+			# echo "----- Combining Files ----- "
+			# cat tmp_combine.lis
+			# echo "Output: " $s
+                        $cf_combine -k $ignore_exp_stat tmp_combine.lis $s
+                        # $modhead "${s}[1]" NUM_EXP $n_good
+                        $modhead "${s}[1]" COMBMETH XCORR
+                        echo $s >> tmp_seg_dn.lis
+                    
+                        set s = DN_${rn}000${seg2}fcal.fit
+                        awk '{print "'$rn'"$1"'$seg2'fcal.fit",$2}' tmp_good_exp.lis > tmp_combine.lis  # Combine $seg2 [dn]
+			# echo "----- Combining Files ----- "
+			# cat tmp_combine.lis
+			# echo "Output: " $s
+                        $cf_combine -k $ignore_exp_stat tmp_combine.lis $s
+                        # $modhead "${s}[1]" NUM_EXP $n_good
+                        $modhead "${s}[1]" COMBMETH XCORR
+                        echo $s >> tmp_seg_dn.lis
+                
+                        set n_night = `cat tmp_night_exp.lis | wc -l`
+                        if ($om == ttag && $n_night > 0) then  # Create and combine night only files
+                        
+                            echo "*** Creating night only files ***"                                            
+                            set exp_nums = `awk '{print $1}' tmp_night_exp.lis`
+                        
+                            foreach exp ($exp_nums)
+                            
+                                # Create night-only BPM and FCAL files if they do not already exist.
+                                set bno1 = NO_$rn$exp$det${om}fbpm.fit        # Bad-pixel maps
+                                set bno2 = NO_$rn$exp$det2${om}fbpm.fit
+                                set cno1 = NO_$rn$exp${seg}fcal.fit        # Extracted spectra
+                                set cno2 = NO_$rn$exp${seg2}fcal.fit
+
+                                set etime = `egrep "^$exp" tmp_night_exp.lis | awk '{print $3}'`
+                                set ntime = `egrep "^$exp" tmp_night_exp.lis | awk '{print $4}'`
+                                set ratio = `egrep "^$exp" tmp_night_exp.lis | awk '{printf "%.0f", 0.5+$4/$3*10.}'`
+
+                                if (!(-e $cno1)) then
+                                    if ($etime == $ntime) then
+                                    echo "$cno1 is a symbolic link to $rn$exp${seg}fcal.fit"
+                                    ln -s $rn$exp${seg}fcal.fit $cno1
+                                    else
+
+                                set idf_file = $rn$exp$det${om}fidf.fit
+                                if (!(-e $bno1)) then
+                                    if ($ratio > 9) then 
+                                    echo "$bno1 is a symbolic link to $rn$exp$det${om}fbpm.fit"
+                                    ln -s $rn$exp$det${om}fbpm.fit $bno1
+                                    else
+                                    echo "Creating BPM: $bno1 ..."
+                                    cf_bad_pixels -n $bno1 $idf_file
+                                    endif
+                                endif
+                            
+                                    echo "Creating (LiF + SiC) FCAL: $cno1 ..."
+                                    cf_extract_spectra -n $bno1 -r NO_$rn$exp $idf_file  # Existence of $bno1 is not required
+                                    endif
+                                endif
+
+                                if (!(-e $cno2)) then 
+                                    if ($etime == $ntime) then
+                                    echo "Using a symbolic link to $cno2"
+                                    ln -s $rn$exp${seg2}fcal.fit NO_$rn$exp${seg2}fcal.fit
+                                    else
+
+                                set idf_file = $rn$exp$det2${om}fidf.fit
+                                if (!(-e $bno2)) then 
+                                    if ($ratio > 9) then 
+                                    echo "Using a symbolic link to $bno2"
+                                    ln -s $rn$exp$det2${om}fbpm.fit NO_$rn$exp$det2${om}fbpm.fit
+                                    else
+                                    echo "Creating BPM: $bno2 ..."
+                                    cf_bad_pixels -n $bno2 $idf_file
+                                    endif
+                                endif
+                            
+                                    echo "Creating (LiF + SiC) FCAL: $cno2 ..."
+                                    cf_extract_spectra -n $bno2 -r NO_$rn$exp $idf_file  # Existence of $bno2 is not required
+                                    endif
+                                endif
+                            
+                            end
+                        
+                            # Combine exposures into a single spectrum.
+                            set s = NO_${rn}000${seg}fcal.fit
+                            awk '{print "NO_'$rn'"$1"'$seg'fcal.fit",$2}' tmp_night_exp.lis > tmp_combine.lis  # Combine $seg [no]
+                            $cf_combine -k $ignore_exp_stat tmp_combine.lis $s
+                            # $modhead "${s}[1]" NUM_EXP $n_night
+                            $modhead "${s}[0]" DAYNIGHT NIGHT
+                            $modhead "${s}[1]" COMBMETH XCORR
+                            echo $s >> tmp_seg_no.lis
+                        
+                            set s = NO_${rn}000${seg2}fcal.fit
+                            awk '{print "NO_'$rn'"$1"'$seg2'fcal.fit",$2}' tmp_night_exp.lis > tmp_combine.lis  # Combine $seg2 [no]
+                            $cf_combine -k $ignore_exp_stat tmp_combine.lis $s
+                            # $modhead "${s}[1]" NUM_EXP $n_night
+                            $modhead "${s}[0]" DAYNIGHT NIGHT
+                            $modhead "${s}[1]" COMBMETH XCORR
+                            echo $s >> tmp_seg_no.lis
+                        
+                        endif
+                
+                    else
+                
+                        #
+                        # --- Path 2: Optimize background ---
+                        #
+                    
+                        echo "Optimize background..."
+                    
+                        # Combine IDF files
+                        set idf1_all = DN_${rn}000$det${om}fidf.fit  # Same for [dn] and [no]
+                        set idf2_all = DN_${rn}000$det2${om}fidf.fit
+                                        
+                        if (!(-e $idf1_all)) then
+                            echo "Creating IDF: $idf1_all ..."
+                            if ($readfiles == 1) then 
+                            	ls ${rn}[0-8][0-9][0-9]$det${om}fidf.fit |& grep -v 000${det} > tmp_idf.lis  # Reject EXP "9xx" and "000"
+                            else
+                            	ls ${rn}9[0-9][0-9]$det${om}fidf.fit |& grep -v 000${det} > tmp_idf.lis  # Consider only airglow
+                            endif
+                            if ($? == 0) then  # IDF files exist
+                            
+                                set idf_lis = `awk '{printf "%s ",$1}' tmp_idf.lis`
+				# echo "Combining IDF files: " $idf_lis
+                                idf_combine -cz $ignore_exp_stat $idf1_all $idf_lis  # Create combined IDF file for $seg
+                                $rm tmp_idf.lis
+                                
+                            else
+                            
+                                echo "ERROR: IDF files are missing"
+                                $rm tmp_idf.lis
+                                goto crash
+                            
+                            endif
+                        endif
+
+                        if (!(-e $idf2_all)) then
+                            echo "Creating IDF: $idf2_all ..."
+                            if ($readfiles == 1) then 
+                            	ls ${rn}[0-8][0-9][0-9]$det2${om}fidf.fit |& grep -v 000${det2} > tmp_idf.lis  # Reject EXP "9xx" and "000"
+                            else
+                            	ls ${rn}9[0-9][0-9]$det2${om}fidf.fit |& grep -v 000${det2} > tmp_idf.lis  # Consider only airglow
+                            endif
+                            if ($? == 0) then  # IDF files exist
+                            
+                                set idf_lis = `awk '{printf "%s ",$1}' tmp_idf.lis`
+				# echo "Combining IDF files: " $idf_lis
+                                idf_combine -cz $ignore_exp_stat $idf2_all $idf_lis  # Create combined IDF file for $seg2
+                                $rm tmp_idf.lis
+                                
+                            else
+                            
+                                echo "ERROR: IDF files are missing"
+                                $rm tmp_idf.lis
+                                goto crash
+                            
+                            endif
+                        endif
+                    
+                        # Get the number of (valid) combined IDF files
+                        set tmp_buf = `$modhead $idf1_all NSPEC`
+                        set n_comb1 = $tmp_buf[3]
+                        set tmp_buf = `$modhead $idf1_all SPEC001`
+                        set idf1_1  = $tmp_buf[3]
+                        set tmp_buf = `$modhead $idf2_all NSPEC`
+                        set n_comb2 = $tmp_buf[3]
+                        set tmp_buf = `$modhead $idf2_all SPEC001`
+                        set idf2_1  = $tmp_buf[3]
+                    
+                        # Combine BPM files
+                        set bpm1_all = DN_${rn}000$det${om}fbpm.fit
+                        set bpm2_all = DN_${rn}000$det2${om}fbpm.fit
+                    
+                        if (!(-e $bpm1_all)) then 
+                            echo "Combine all BPM (from IDF): $bpm1_all ..."
+                            bpm_combine $bpm1_all $idf1_all  # Create combined BPM file [dn] for $seg
+                        endif
+                    
+                        if (!(-e $bpm2_all)) then 
+                            echo "Combine all BPM (from IDF): $bpm2_all ..."
+                            bpm_combine $bpm2_all $idf2_all  # Idem for $seg2
+                        endif
+                    
+                        # Extract [Day + Night] spectra
+                        set s = DN_${rn}000${seg}fcal.fit
+                        set xxx = DN_${rn}xxx${seg}fcal.fit
+                        if (!(-e $xxx)) cf_extract_spectra -r DN_${rn}xxx $idf1_all  # Avoid overwrite LiF | SiC
+                        echo $xxx > tmp_combine.lis
+                        $cf_combine -k $ignore_exp_stat tmp_combine.lis $s
+                        $modhead "${s}[0]" NSPEC $n_comb1
+                        $modhead "${s}[0]" SPEC001 $idf1_1
+                        $modhead "${s}[1]" COMBMETH BACKGRND
+                        echo $s >> tmp_seg_dn.lis
+                    
+                        set s = DN_${rn}000${seg2}fcal.fit
+                        set xxx = DN_${rn}xxx${seg2}fcal.fit
+                        if (!(-e $xxx)) cf_extract_spectra -r DN_${rn}xxx $idf2_all  # Avoid overwrite LiF | SiC
+                        echo $xxx > tmp_combine.lis
+                        $cf_combine -k $ignore_exp_stat tmp_combine.lis $s
+                        $modhead "${s}[0]" NSPEC $n_comb2
+                        $modhead "${s}[0]" SPEC001 $idf2_1
+                        $modhead "${s}[1]" COMBMETH BACKGRND
+                        echo $s >> tmp_seg_dn.lis
+                    
+                        set n_night = `cat tmp_all_night_exp.lis | wc -l`
+                        if ($om == ttag && $n_night > 0) then  # Create and combine night only files
+                        
+                            echo "*** Creating night only files ***"    
+                            set exp_nums = `awk '{print $1}' tmp_all_night_exp.lis`
+                            $rm tmp_bpm1.lis tmp_bpm2.lis
+                            
+                            foreach exp ($exp_nums)
+                            
+                                # Create bpm night only files (if they do not exist yet)
+                                set bno1 = NO_$rn$exp$det${om}fbpm.fit
+                                set bno2 = NO_$rn$exp$det2${om}fbpm.fit
+                            
+                                set idf_file = $rn$exp$det${om}fidf.fit
+                                if (!(-e $bno1)) then
+                                    echo "Creating BPM: $bno1 ..."
+                                    cf_bad_pixels -n $bno1 $idf_file
+                                endif
+                                if (-e $bno1) echo $bno1 >> tmp_bpm1.lis  # If valid, add in $seg list
+
+                                set idf_file = $rn$exp$det2${om}fidf.fit
+                                if (!(-e $bno2)) then 
+                                    echo "Creating BPM: $bno2 ..."
+                                    cf_bad_pixels -n $bno2 $idf_file
+                                endif
+                                if (-e $bno2) echo $bno2 >> tmp_bpm2.lis  # If valid, add in $seg2 list
+    
+                            end
+
+                        
+                            # Combine BPM for $seg and extract spectra
+                            
+                            set bpm1_all = NO_${rn}000$det${om}fbpm.fit
+                            set n_bpm = `cat tmp_bpm1.lis | wc -l`
+                            echo "Number of valid BPM files: $n_bpm"
+                        
+                            if ($n_bpm > 0) then
+                        
+                                echo $n_bpm > tmp_bpm.lis
+                                cat tmp_bpm1.lis >> tmp_bpm.lis
+                            
+                                if (!(-e $bpm1_all)) then
+                                    echo "Combine all BPM (from list): $bpm1_all ..."
+                                    bpm_combine $bpm1_all tmp_bpm.lis  # Create combined BPM file [no] for $seg
+                                endif
+                                $rm tmp_bpm.lis
+                            
+                            endif
+                        
+                            # Extract [Night only] spectra. The existence of $bpm1_all is not required
+                            set s = NO_${rn}000${seg}fcal.fit
+                            set xxx = NO_${rn}xxx${seg}fcal.fit
+                            if (!(-e $xxx)) cf_extract_spectra -n $bpm1_all -r NO_${rn}xxx $idf1_all  # Avoid overwrite LiF | SiC
+                            echo $xxx > tmp_combine.lis
+                            $cf_combine -k $ignore_exp_stat tmp_combine.lis $s
+                            $modhead "${s}[0]" NSPEC $n_comb1
+                            $modhead "${s}[0]" SPEC001 $idf1_1
+                            $modhead "${s}[1]" COMBMETH BACKGRND
+                            echo $s >> tmp_seg_no.lis
+
+    
+                            # Combine BPM for $seg2 and extract spectra
+                        
+                            set bpm2_all = NO_${rn}000$det2${om}fbpm.fit
+                            set n_bpm = `cat tmp_bpm2.lis | wc -l`
+                            echo "Number of valid BPM files: $n_bpm"
+                        
+                            if ($n_bpm > 0) then
+                        
+                                echo $n_bpm > tmp_bpm.lis
+                                cat tmp_bpm2.lis >> tmp_bpm.lis
+                            
+                                if (!(-e $bpm2_all)) then 
+                                    echo "Combine all BPM (from list): $bpm2_all ..."
+                                    bpm_combine $bpm2_all tmp_bpm.lis  # Create combined BPM file [no] for $seg2
+                                endif
+                                $rm tmp_bpm.lis
+                            
+                            endif
+                        
+                            # Extract [Night only] spectra. The existence of $bpm2_all is not required
+                            set s = NO_${rn}000${seg2}fcal.fit
+                            set xxx = NO_${rn}xxx${seg2}fcal.fit
+                            if (!(-e $xxx)) cf_extract_spectra -n $bpm2_all -r NO_${rn}xxx $idf2_all  # Avoid overwrite LiF | SiC
+                            echo $xxx > tmp_combine.lis
+                            $cf_combine -k $ignore_exp_stat tmp_combine.lis $s
+                            $modhead "${s}[0]" NSPEC $n_comb2
+                            $modhead "${s}[0]" SPEC001 $idf2_1
+                            $modhead "${s}[1]" COMBMETH BACKGRND
+                            echo $s >> tmp_seg_no.lis
+
+                        endif
+                    endif
+                endif
+            end
+            
+            $rm tmp_xcorr.res tmp_bpm1.lis tmp_bpm2.lis tmp_combine.lis
+            $rm tmp_all_night_exp.lis tmp_good_exp.lis tmp_exp.lis tmp_night_exp.lis
+            
+        end
+        
+        # Pack the 8 [detector][channel] pairs together ([dn] and [no] for ttag)
+        if (-e tmp_seg_dn.lis) then
+    
+            set fcal_all = ${rn}00000all$res${om}fcal.fit  # Final output name
+            $rm $fcal_all  # Clean (safe)
+            set n_segs = `cat tmp_seg_dn.lis | wc -l`
+    
+            if (!($n_segs == 8)) then
+    
+                @ mseg = 8 - $n_segs
+                echo "ERROR: $mseg (day + night) segments are missing"
+                $rm tmp_seg_dn.lis
+                goto crash
+
+            else
+    
+                $cf_pack tmp_seg_dn.lis $fcal_all
+                $rm tmp_seg_dn.lis
+    
+                # Plot figures
+                $idl_obsplot {$rn}
+        
+                # Create National Virtual Observatory file
+                set nvo_file = ${rn}00000nvo$res${om}fcal.fit
+                $rm $nvo_file  # Clean (safe)
+                $cf_nvo $fcal_all $nvo_file  # Create file
+                
+                if (-e tmp_seg_no.lis) then
+                
+                    set fcal_all = ${rn}00000ano$res${om}fcal.fit  # Final output name
+                    $rm $fcal_all  # Clean (safe)
+                    set n_segs = `cat tmp_seg_no.lis | wc -l`
+    
+                    # if (!($n_segs == 8)) then
+                    #
+                    #    @ mseg = 8 - $n_segs
+                    #    echo "ERROR: $mseg (night only) segments are missing"
+                    #    $rm tmp_seg_no.lis
+                    #    # goto crash
+                    #    
+                    # else
+                    
+                        $cf_pack tmp_seg_no.lis $fcal_all
+                        $rm tmp_seg_no.lis
+                
+                    # endif
+                    
+                endif
+            endif
+        endif
+    end
+end
+
+# Clean [dn] and [no] files. Just keep all, (ano) and nvo
+$rm DN_${rn}*.fit NO_${rn}*.fit
+
+# Delete IDF files
+if $?DELETE_IDF then
+    echo "NOTE: Deleting intermediate data files."
+    $rm ${rn}*idf.fit
+endif
+
+# Delete bad-pixel-map (bpm) files
+if $?DELETE_BPM then
+    echo "NOTE: Deleting bad pixel map (bpm) files."
+    $rm ${rn}*bpm.fit
+endif
+
+# Call routine to make quick-look airglow plot.
+cf_make_900_obs.csh $1
+
+exit(0)
+
+crash:  # Procedure when script crashes
+
+# Clean directory
+$rm tmp_xcorr.res tmp_bpm1.lis tmp_bpm2.lis tmp_combine.lis tmp_night_exp.lis
+$rm tmp_all_night_exp.lis tmp_good_exp.lis tmp_exp.lis tmp_seg_dn.lis tmp_seg_no.lis
+$rm DN_*.fit NO_*.fit
+
+# Return 1
+exit(1)
diff --git a/src/analysis/cf_nvo.c b/src/analysis/cf_nvo.c
new file mode 100644
index 0000000..4dd9771
--- /dev/null
+++ b/src/analysis/cf_nvo.c
@@ -0,0 +1,497 @@
+/*******************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *******************************************************************************
+ *
+ * Usage:    cf_nvo all_segments.fit nvo_file.fit
+ *
+ * Description: Write a National Virtual Observatory (nvo) file. The program
+ *              uses the file created by cf_pack, which contains one spectrum
+ *              per extension, each corresponding to a detector channel.
+ *
+ * History:     04/11/05        tc      v1.0    First release
+ *		05/16/2005	wvd	v1.1	Check mean flux of each segment.
+ *						If preferred channel is missing,
+ *						replace it with another.
+ *		05/19/2005	wvd	v1.2	Shift each channel to match
+ *						LiF1A between 1045 and 1070 A.
+ *		05/20/2005	wvd	v1.3	For emission-line sources, 
+ *						cross-correlate on O VI lines.
+ *		05/23/2005	wvd	v1.4	Don't assume that sides A and B
+ *						have the same shift.
+ *		06/01/2005	wvd	v1.5	Do assume that sides A and B
+ *						have the same shift.
+ *		06/03/2005	wvd	v1.6	Delete unused variables.
+ *		06/08/2005	wvd	v1.7	Define MAXFLOAT if needed.
+ *		06/16/2005	wvd	v1.8	Include values.h
+ *		07/06/2005	wvd	v1.9	If FESCENT = FES B, use LiF 2B
+ *						as wavelength standard.
+ *		07/12/2005	wvd	v1.10	Give up on use of MAXFLOAT.
+ *		08/11/2005	wvd	v1.11	Set keyword NEXTEND = 1.
+ *		03/22/2006	wvd	v1.12	Allow use of SiC data for 
+ *						1000-1100 A region.
+ *						Don't cross-correlate segments
+ *						with OBSTIME = 0.
+ *		05/16/2006	wvd	v1.13	Use Lyman beta to align
+ *                                              background exposures.
+ *                                              Use O VI and C II to align WD's.
+ *		05/19/2006	wvd	v1.14	In copy_spec(), test index to 
+ *						prevent extending past the edge.
+ *						For BKGD targets, omit flux
+ *						comparison when deciding which
+ *						regions to use.
+ *						Delete index to the file 
+ *						extensions from the primary HDU.
+ *						Compute mean flux over same
+ *						wavelength region for each band.
+ *		05/24/2006	wvd	v1.16	For PC targets, don't include
+ *						O VI in calculation of mean flux
+ *		12/19/2006	wvd	v1.17	Reject segments with 
+ *						OBSTIME < 10 seconds when full
+ *						exposure is longer than 100 s.
+ *		02/19/2008	bot	v1.18	Fixed indexing problem in
+ *						copy_spec due to shift and n_copy
+ *
+ ******************************************************************************/
+ 
+#include <math.h>
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include "calfuse.h"
+
+#define MAXSHIFT	30
+#define N_SHIFT		61
+#define NVO_MIN 	900
+#define NVO_MAX 	1190
+
+static char CF_PRGM_ID[] = "cf_nvo";
+static char CF_VER_NUM[] = "1.18";
+
+static int
+compute_shift(fitsfile *pt_fits, int hdu_ref, int hdu, float wmin, float wdelta,
+	float wpc, int *shift, int *quality)
+{
+	char	comb[FLEN_VALUE], ref_comb[FLEN_VALUE];
+        int     hdutype, status = 0;
+	int	ind_chi2_min, nchi;
+        long    i, k, n_rows, ref_start, start, n_pix;
+        float   *error, *flux, *wave, *ref_error, *ref_flux, *ref_wave;
+	float	chi_square[N_SHIFT], chi_square_min, chi_square_max;
+	float	ref_obstime, obstime;
+	double	scale, sum, var1, var2;
+
+        /* Don't need to shift reference spectrum. */
+        if (hdu_ref == hdu) {
+                *shift = 0;
+                *quality = TRUE;
+                return(0);
+        }
+
+	/* Read data for reference and data channels. */
+        FITS_movabs_hdu(pt_fits, hdu_ref, &hdutype, &status);
+        FITS_read_key(pt_fits, TSTRING, "COMBMETH", &ref_comb, NULL, &status);
+        FITS_read_key(pt_fits, TFLOAT, "OBSTIME", &ref_obstime, NULL, &status);
+        n_rows = cf_read_col(pt_fits, TFLOAT, "WAVE", (void **) &ref_wave);
+        n_rows = cf_read_col(pt_fits, TFLOAT, "FLUX", (void **) &ref_flux);
+        n_rows = cf_read_col(pt_fits, TFLOAT, "ERROR", (void **) &ref_error);
+
+        FITS_movabs_hdu(pt_fits, hdu, &hdutype, &status);
+        FITS_read_key(pt_fits, TSTRING, "COMBMETH", &comb, NULL, &status);
+        FITS_read_key(pt_fits, TFLOAT, "OBSTIME", &obstime, NULL, &status);
+        n_rows = cf_read_col(pt_fits, TFLOAT, "WAVE", (void **) &wave);
+        n_rows = cf_read_col(pt_fits, TFLOAT, "FLUX", (void **) &flux);
+        n_rows = cf_read_col(pt_fits, TFLOAT, "ERROR", (void **) &error);
+
+	/* If either channel was not constructed using cross-correlation, 
+	 * return a shift of 0. */
+	if (strncmp(ref_comb,"X",1) || strncmp(comb,"X",1)) {
+		*shift = 0;
+                *quality = FALSE;
+		printf("hdu = %d, hdu_ref = %d, COMBMETH != XCORR\n",
+			hdu, hdu_ref);
+		return(0);
+	}
+
+	/* If either channel has OBSTIME = 0, return a shift of 0. */
+	if (ref_obstime < 1 || obstime < 1) {
+		*shift = 0;
+                *quality = FALSE;
+		if (ref_obstime < 1)
+			printf("hdu_ref = %d, OBSTIME = %f\n", hdu_ref, ref_obstime);
+		if (obstime < 1) printf("hdu = %d, OBSTIME = %f\n", hdu, obstime);
+		return(0);
+	}
+
+	/* Compute chi-squared for shifts between +/- MAXSHIFT pixels. */
+        ref_start = cf_nlong((wmin - ref_wave[0]) / wpc) + MAXSHIFT;
+        start = cf_nlong((wmin - wave[0]) / wpc);
+        n_pix = cf_nlong(wdelta / wpc) - (N_SHIFT - 1);
+
+	for (k = 0; k < N_SHIFT; k++) {
+	    nchi = 0;
+	    sum = 0;
+	    for (i = 0; i < n_pix; i++) {
+		var1 = ref_error[ref_start + i] * ref_error[ref_start + i];
+		var2 = error[start + i + k] * error[start + i + k];
+		if ((var1 + var2) > 0.) {
+		    sum += (ref_flux[ref_start + i] - flux[start + i + k]) *
+		           (ref_flux[ref_start + i] - flux[start + i + k]) /
+			   (var1 + var2);
+		    nchi++;
+		}
+	    }
+	    scale = (double) nchi / n_pix;
+	    chi_square[k] = sum / scale;
+	}
+
+	/* If chi-squared changes by less than 20% over range of shifts, abort.
+	 * Otherwise, return shift corresponding to lowest value of chi-square.
+	 */
+	ind_chi2_min = 0;
+        chi_square_min = 1E5;
+        chi_square_max = -1E5;
+        for (k = 0; k < N_SHIFT; k++) {
+                if (chi_square[k] < chi_square_min)
+                {
+                        chi_square_min = chi_square[k];
+                        ind_chi2_min = k;
+                }
+                else if (chi_square[k] > chi_square_max)
+                        chi_square_max = chi_square[k];
+        }
+
+        if (chi_square_max / chi_square_min < 1.2) {
+                *shift = 0;
+                *quality = FALSE;
+		printf("hdu = %d, hdu_ref = %d.  Chi-square dist is flat.\n",
+		hdu, hdu_ref);
+	}
+        else {
+                *shift = ind_chi2_min - MAXSHIFT;
+                *quality = TRUE;
+	}
+
+        free(ref_error);
+        free(ref_flux);
+        free(ref_wave);
+        free(error);
+        free(flux);
+        free(wave);
+
+	return(0);
+}
+
+
+static int
+copy_spec(fitsfile *pt_fits, int hdu, float w_min, float w_max, float wpc,
+	int shift, float *flux_nvo, float *error_nvo, long n_nvo)
+{
+	int	hdutype, status = 0;
+	long	i, i0, n_rows, nvo_start, start, n_copy, n_copy0;
+	float	*error, *flux, w0;
+
+	FITS_movabs_hdu(pt_fits, hdu, &hdutype, &status);
+	FITS_read_key(pt_fits, TFLOAT, "W0", &w0, NULL, &status);
+	n_rows = cf_read_col(pt_fits, TFLOAT, "FLUX", (void **) &flux);
+	n_rows = cf_read_col(pt_fits, TFLOAT, "ERROR", (void **) &error);
+
+	nvo_start = cf_nlong(((double) w_min - NVO_MIN) / wpc);
+	start = cf_nlong(((double) w_min - w0) / wpc);
+	n_copy = cf_nlong(((double) w_max - w_min) / wpc) + 1;
+	if (nvo_start + n_copy > n_nvo) {
+	    printf ("HDU = %d, w_min = %.1f, w_max = %.1f, wpc = %5.3f\n",
+		hdu, w_min, w_max, wpc);
+	    printf ("n_nvo = %ld, nvo_start = %ld, start = %ld, n_copy = %ld\n",
+		n_nvo, nvo_start, start, n_copy);
+	    cf_if_error("Can't create NVO array.");
+	}
+	 
+	n_copy0 = n_copy;   
+	if (start + shift + n_copy > n_rows) {
+	    n_copy = n_rows - (start + shift);
+	    if (hdu == 3) for (i = n_copy; i < n_copy0; i++) {
+		flux_nvo[i+nvo_start]  = 0.0;
+		error_nvo[i+nvo_start] = 0.0;
+	    }
+	}
+
+	i0 = 0;
+	if (start + shift < 0) {
+	    i0 = -(start + shift);
+	    for (i = 0; i < i0; i++) {
+		flux_nvo[i+nvo_start]  = 0.0;
+		error_nvo[i+nvo_start] = 0.0;
+	    }
+	}
+
+	for (i = i0; i < n_copy; i++) {
+	    flux_nvo[i+nvo_start]  = flux[i+start+shift];
+	    error_nvo[i+nvo_start] = error[i+start+shift];
+	}
+ 	   
+	free(error);
+	free(flux);
+	return(0);
+}
+
+
+int main(int argc, char *argv[])
+{
+	/* Variables */
+        char program[FLEN_VALUE];
+	double mean_flux[8], sum_flux;
+	float *wave, *flux, w0, wpc, hdu_wpc;
+	float *wave_nvo, *flux_nvo, *error_nvo;
+	float max_obstime, wmin, wdelta;
+	long n_rows, n_nvo;
+	int ref, i, nextend=1, n_hdus, shift[8], quality[8];
+	int bkgd_obs=FALSE, objclass;
+	int nkeys, morekeys=0;
+	long k, n_elem;
+	
+	char *ttype[] = { "WAVE", "FLUX", "ERROR" };
+	char *tform[] = { "1E", "1E", "1E" };
+	char *tunit[] = { "ANGSTROMS", "ERG/CM2/S/A", "ERG/CM2/S/A" };
+	
+	/* HDU numbers must be consistent with output of cf_pack. */
+	char *extname[] = { "1ASIC", "2BSIC", "1ALIF", "2BLIF", "1BSIC", "2ASIC", "1BLIF", "2ALIF" };
+	int hdu[]       = { 6,       8,       2,       4,       7,       9,       3      , 5       };
+	float w_min[]   = {  997,    1010,    990,     990,     904,     917.5,   1094   , 1090    };
+	float w_max[]   = { 1090,    1104,    1080,    1074,    992,     998,     1190   , 1180    };
+
+	/* Regions to use when computing mean flux. */
+	float *region;
+	float region_array[8][6] = {
+		{0, 0, 1030, 1039, 1045, 1070},			/* 1ASIC */
+	        {0, 0, 1030, 1039, 1045, 1070},			/* 2BSIC */
+	        {0, 0, 1030, 1039, 1045, 1070},			/* 1ALIF */
+	        {0, 0, 1030, 1039, 1045, 1070},			/* 2BLIF */
+	        {912, 935, 955, 970, 980, 985},			/* 1BSIC */
+	        {912, 935, 955, 970, 980, 985},			/* 2ASIC */
+	        {1095, 1130, 1140, 1165, 1170, 1180},		/* 1BLIF */
+	        {1095, 1130, 1140, 1165, 1170, 1180}		/* 2ALIF */
+	};
+
+	char in_name[80], out_name[80];
+	char extname_key[80], src_type[FLEN_VALUE], sp_type[FLEN_VALUE], fescent[FLEN_VALUE];
+	fitsfile *pt_fits, *pt_fits_out;
+	int status = 0, hdutype;
+
+	    
+	/***********************************
+	** Enter a timestamp into the log **
+	***********************************/
+	cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+	cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+
+	/***********************************************************	
+	** Check for proper command-line usage and read arguments **
+	***********************************************************/
+	if (argc != 3)
+		cf_if_error("Usage: cf_nvo all_segments.fit nvo_file.fit");
+	
+	strcpy(in_name, argv[1]);
+	strcpy(out_name, "!");
+	strcat(out_name, argv[2]); /* Force overwrite */
+	
+	/*******************************************	
+	** Open input file, read header keywords. **
+	*******************************************/
+	FITS_open_file(&pt_fits, in_name, READONLY, &status);
+        FITS_read_key(pt_fits, TSTRING, "PRGRM_ID", &program,  NULL, &status);
+        FITS_read_key(pt_fits, TINT,    "OBJCLASS", &objclass, NULL, &status);
+        FITS_read_key(pt_fits, TSTRING, "SP_TYPE",  &sp_type,  NULL, &status);
+        FITS_read_key(pt_fits, TSTRING, "SRC_TYPE", &src_type, NULL, &status);
+	FITS_read_key(pt_fits, TFLOAT,  "OBSTIME",  &max_obstime, NULL, &status);
+	FITS_read_key(pt_fits, TFLOAT,  "WPC",      &wpc,      NULL, &status);
+        FITS_read_key(pt_fits, TSTRING, "FESCENT",  &fescent,  NULL, &status);
+	ref = 2;					/* LiF 1A */
+	if (!strncmp(fescent, "FES B", 5)) ref = 3;	/* LiF 2B */
+
+	/****************************************************************	
+	** If SRC_TYPE = PC, exclude O VI in calculation of mean flux. **
+	****************************************************************/
+	if (!strncmp(src_type, "PC", 2))
+	    for (i = 0; i < 4; i++)
+		region_array[i][2] = region_array[i][3] = 0;
+
+	/***************************************	
+	** Compute mean flux in each channel. **
+	***************************************/
+	FITS_get_num_hdus(pt_fits, &n_hdus, &status);
+	if (n_hdus != 9)
+		cf_if_error("Input file must have 9 extensions (%d found)", n_hdus);
+	
+	for (i = 0; i < 8; i++) {
+		float obstime;
+		FITS_movabs_hdu(pt_fits, hdu[i], &hdutype, &status);
+		FITS_read_key(pt_fits, TSTRING, "EXTNAME", extname_key, NULL, &status);
+		if (strcmp(extname_key, extname[i]))
+			cf_if_error("Extension %d's name does not match (%s)",
+			hdu[i], extname[i]);
+		FITS_read_key(pt_fits, TFLOAT, "WPC", &hdu_wpc, NULL, &status);
+		if (hdu_wpc != wpc) 
+			cf_if_error("Extension %d's WPC does not match primary HDU",
+			hdu[i]);
+        	FITS_read_key(pt_fits, TFLOAT, "OBSTIME", &obstime, NULL, &status);
+		if (obstime < 1. || (obstime < 10 && max_obstime > 100))
+			mean_flux[i] = -1;
+		else {
+		   n_rows = cf_read_col(pt_fits, TFLOAT, "WAVE", (void **) &wave);
+		   n_rows = cf_read_col(pt_fits, TFLOAT, "FLUX", (void **) &flux);
+
+		   sum_flux = n_elem = 0;
+		   region = region_array[i];
+		   for (k = 0; k < n_rows; k++)
+		   {
+			if ((wave[k] > region[0] && wave[k] < region[1]) ||
+			    (wave[k] > region[2] && wave[k] < region[3]) ||
+			    (wave[k] > region[4] && wave[k] < region[5])) {
+				sum_flux += flux[k];
+				n_elem ++;
+			}
+		   }
+		
+		   mean_flux[i] = sum_flux / n_elem;
+		   free(wave);
+		   free(flux);
+		}
+
+		printf("%s\tmean_flux = %g\n", extname_key, mean_flux[i]);
+	}
+	
+	/*******************************************************************
+	 * If FESCENT = FES A, compute shifts relative to LiF 1A. 
+	 * If FESCENT = FES B, use LiF 2B.
+	 * For background targets, compare Lyman beta lines.
+	 * For other emission-line targets, compare O VI lines.
+	 * For white dwarfs, use O VI and C II.
+	 * For other continuum sources, use the region between 1045 and 1070 A
+	 * for the four 1000-1100 A channels.
+	 ******************************************************************/
+
+	if (src_type[1] == 'E') {	/* Emission-line source */
+                        /* Use Lyman beta to align background observations. */
+            if (objclass == 7 || (program[0] == 'S' && program[2] == '0' && program[3] == '5')) {
+	    	printf("Assuming background observation.\n");
+                wmin = 1024.;
+                wdelta = 6.;
+            } else {    /* Use O VI emission for everything else. */
+	    	printf("SRC_TYPE = %s.  Emission-line target.\n", src_type);
+                wmin = 1030.;
+                wdelta = 9.;
+            }
+	}
+					/* Continuum source */
+        else if (objclass == 17 || objclass == 29 || objclass == 37) {
+                        /* Use O VI and C II to align white dwarf spectra. */
+            printf("OBJCLASS = %d.  Assuming nearby white dwarf.\n", objclass);
+            wmin = 1030.;
+            wdelta = 9.;
+        }
+        else {  /* Use 1045-1070 A region for all other continuum sources. */
+            printf("SRC_TYPE = %s.  Continuum target.\n", src_type);
+            wmin = 1045.;
+            wdelta = 25.;
+        }
+
+	for (i = 0; i < 4; i++) {
+	    if (mean_flux[i] > -1) 
+		compute_shift(pt_fits, hdu[ref], hdu[i], wmin, wdelta, wpc, shift+i, quality+i);
+	    else
+		shift[i] = 0;
+	    shift[i+4] = shift[i];
+	    printf("hdu = %d, hdu_ref = %d, shift = %d\n", hdu[i], hdu[ref], shift[i]);
+	}
+
+	/**************************
+	** Set up output arrays. **
+	**************************/
+	n_nvo = cf_nlong((double) (NVO_MAX - NVO_MIN) / wpc) + 1;
+	wave_nvo = (float *) cf_calloc(n_nvo, sizeof(float));
+	for (i = 0; i < n_nvo; i++) wave_nvo[i] = NVO_MIN + (double) wpc * i;
+	flux_nvo = (float *) cf_calloc(n_nvo, sizeof(float));
+	error_nvo = (float *) cf_calloc(n_nvo, sizeof(float));
+	
+	for (i = 0; i < n_nvo; i++) {
+		flux_nvo[i]  = 0.0;
+		error_nvo[i] = 0.0;
+	}
+	
+	/**************************************************************
+	** In each wave band, copy best data set into output arrays. **
+	**************************************************************/
+	/* For BKGD targets, omit flux comparison when selecting which
+	   regions to use. */
+	if (objclass == 7 || !strncmp(sp_type, "BKGD", 4)) bkgd_obs = TRUE;
+
+	/* First fill in the 1010-1104 A region with SiC 2B. */
+	copy_spec(pt_fits, hdu[1], w_min[1], w_max[1], wpc, shift[1], flux_nvo, error_nvo, n_nvo);
+
+	/* Replace with SiC 1A if possible.  It has a higher S/N, but extends only to 1090 A. */
+	if ((bkgd_obs && mean_flux[0] > -1) || (mean_flux[0] > 0.9 * mean_flux[1])) 
+	    copy_spec(pt_fits, hdu[0], w_min[0], w_max[0], wpc, shift[0], flux_nvo, error_nvo, n_nvo);
+
+	/* Next overlay the region between 990 and 1080 A with LiF 1A or LiF 2B, if available. */
+	if ((bkgd_obs && mean_flux[2] > -1) || ((mean_flux[2] > 0.9 * mean_flux[3]) &&
+	    (mean_flux[2] > 0.7 * mean_flux[0]) && (mean_flux[2] > 0.7 * mean_flux[1])))
+	    copy_spec(pt_fits, hdu[2], w_min[2], w_max[2], wpc, shift[2], flux_nvo, error_nvo, n_nvo);
+	else if ((bkgd_obs && mean_flux[3] > -1) ||
+	    ((mean_flux[3] > 0.7 * mean_flux[0]) && (mean_flux[3] > 0.7 * mean_flux[1])))
+	    copy_spec(pt_fits, hdu[3], w_min[3], w_max[3], wpc, shift[3], flux_nvo, error_nvo, n_nvo);
+	else 
+	    w_max[5] = 1010, w_min[6] = w_min[7] = 1104;
+		/* If no LiF data, adopt limits of SiC spectra. */
+
+	/* Use SiC 1B to populate the shortest wavelengths. */
+	copy_spec(pt_fits, hdu[4], w_min[4], w_max[4], wpc, shift[4], flux_nvo, error_nvo, n_nvo);
+
+	/* If SiC 2A is good, use it for the main part of 900 - 1000 A. */
+	if ((bkgd_obs && mean_flux[5] > -1) || (mean_flux[5] > 0.9 * mean_flux[4]))
+	    copy_spec(pt_fits, hdu[5], w_min[5], w_max[5], wpc, shift[5], flux_nvo, error_nvo, n_nvo);
+	
+	/* Use LiF 1B to populate the longest wavelengths. */
+	copy_spec(pt_fits, hdu[6], w_min[6], w_max[6], wpc, shift[6], flux_nvo, error_nvo, n_nvo);
+
+	/* If LiF 2A is good, use it for the main part of 1100 - 1180 A. */
+	if ((bkgd_obs && mean_flux[7] > -1) || (mean_flux[7] > 0.9 * mean_flux[6]))
+	    copy_spec(pt_fits, hdu[7], w_min[7], w_max[7], wpc, shift[7], flux_nvo, error_nvo, n_nvo);
+	
+	
+	for (i = 0; i < n_nvo; i++) {
+	    if (flux_nvo[i] >= 1 || error_nvo[i] >= 1) cf_if_error("Bad values in NVO array.");
+	}
+	
+	/*********************
+	** Create NVO file. **
+	*********************/
+	FITS_create_file(&pt_fits_out, out_name, &status);
+	FITS_movabs_hdu(pt_fits, 1, &hdutype, &status);
+	FITS_copy_header(pt_fits, pt_fits_out, &status);
+	FITS_update_key(pt_fits_out, TINT, "NEXTEND", &nextend, NULL, &status);
+	FITS_update_key(pt_fits_out, TSTRING, "FILENAME", (out_name + 1), NULL, &status);
+	FITS_update_key(pt_fits_out, TSTRING, "FILETYPE", "NVO SPECTRUM", NULL, &status);
+	w0 = NVO_MIN;
+	FITS_update_key(pt_fits_out, TFLOAT, "W0", &w0, NULL, &status);
+
+	/* Delete index to file extensions from the primary HDU. */
+	fits_get_hdrspace(pt_fits_out, &nkeys, &morekeys, &status);
+	for (i = nkeys; i > nkeys-12; i--) fits_delete_record(pt_fits_out, i, &status);
+	
+	FITS_create_tbl(pt_fits_out, BINARY_TBL, n_nvo, 3, ttype, tform, tunit, "FUSE_SPECTRUM", &status);
+	FITS_write_col(pt_fits_out, TFLOAT, 1, 1L, 1L, n_nvo, wave_nvo,  &status);
+	FITS_write_col(pt_fits_out, TFLOAT, 2, 1L, 1L, n_nvo, flux_nvo,  &status);
+	FITS_write_col(pt_fits_out, TFLOAT, 3, 1L, 1L, n_nvo, error_nvo, &status);
+	
+	free(wave_nvo);
+	free(flux_nvo);
+	free(error_nvo);
+	
+	FITS_close_file(pt_fits_out, &status);
+	FITS_close_file(pt_fits, &status);
+	
+	return(0);
+}
diff --git a/src/analysis/cf_pack.c b/src/analysis/cf_pack.c
new file mode 100644
index 0000000..a823c22
--- /dev/null
+++ b/src/analysis/cf_pack.c
@@ -0,0 +1,270 @@
+/*******************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *******************************************************************************
+ *
+ * Usage:    cf_pack combined_exposure_list out_file_name.fit
+ *
+ * Description: Write the 8 segments (1alif, 1blif etc...) into a single fits
+ *              file with 8 extensions (in addition to the primary array).
+ *
+ * History:     04/08/05        tc      v1.0	First release
+ *		05/02/05	wvd	v1.1	Copy SPEC and WOFF keywords to
+ *						output file.
+ *		06/03/05	wvd	v1.2	Delete unused variables.
+ *		06/29/05	wvd	v1.3	Set keyword COMB_COR = COMPLETE.
+ *		09/30/05	wvd	v1.4	Update archive search keywords.
+ *		03/23/06	wvd	v1.5	If a segment is missing, write
+ *						an empty image extension.
+ *		05/19/06	wvd	v1.6	Write an index to the file
+ *						extensions to the primary HDU.
+ *		05/24/06	wvd	v1.7	Remove SPEC* keywords from 
+ *						primary HDU.
+ *		05/29/06	wvd	v1.8	Use while construction to 
+ *						delete WOFF* keywords.
+ *		06/22/06	wvd	v1.9	Truncate APER_ACT from (for
+ *						example) MDRS_LIF to MDRS.
+ *		08/14/06	wvd	v1.10	Tinker with code to copy SPEC
+ *						keywords to new file header.
+ *		04/07/07	wvd	v1.11	Clean up compiler warnings.
+ *		08/27/07	bot	v1.12	Changed TINT to TLONG l.163,214,
+ *						and 215 ; added L to every number
+ * 						occurence related to i and j ;
+ * 						Changed i to k l.123 to 131 to
+ * 						keep an int in this case
+ *
+ ******************************************************************************/
+ 
+#include <math.h>
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include "calfuse.h"
+
+/* Calfuse variables */
+static char CF_PRGM_ID[] = "cf_pack";
+static char CF_VER_NUM[] = "1.12";
+
+int main(int argc, char *argv[])
+{
+	/* Variables */
+	float obstime, obstime_max, woffset;
+	float w0, wpc;
+	int wave_cnum, flux_cnum, error_cnum;
+	int n_spec, n_best_spec;
+	long i, j, num_exp, n_rows;
+	int k;
+	
+	char *ttype[] = { "WAVE", "FLUX", "ERROR" };
+	char *tform[] = { "1E", "1E", "1E" };
+	char *tunit[] = { "ANGSTROMS", "ERG/CM2/S/A", "ERG/CM2/S/A" };
+	char *extname[] = { "1ALIF", "1BLIF", "2BLIF", "2ALIF", "1ASIC", "1BSIC", "2BSIC", "2ASIC" };
+	char spec_list[][80] = { "NULL", "NULL", "NULL", "NULL", "NULL", "NULL", "NULL", "NULL" };
+
+	/* New values for archive search keywords */
+	float bandwid = 285.;
+	float centrwv = 1046.;
+	float wavemin = 904.;
+	float wavemax = 1189.;
+	
+	FILE *pt_file;
+	char comment[FLEN_COMMENT], spec_lis[80], out_name[80], spec_name[80];
+	char aper_act[80], detector[80], segment[80];
+	char err_str[80], aper_key[8], combmeth_key[9];
+	char keyname[FLEN_KEYWORD], keyvalue[FLEN_VALUE];
+	fitsfile *pt_fits, *pt_fits_out;
+	int status = 0, hdutype = 0;
+	int nextend_key = 8;
+	float obstime_key = 0;
+
+	    
+	/***********************************
+	** Enter a timestamp into the log **
+	***********************************/
+	cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+	cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+
+	/***********************************************************	
+	** Check for proper command-line usage and read arguments **
+	***********************************************************/
+	if (argc != 3)
+		cf_if_error("Usage: cf_pack combined_exposure_list out_file_name.fit\n");
+	
+	strcpy(spec_lis, argv[1]);
+	strcpy(out_name, "!");
+	strcat(out_name, argv[2]); /* Force overwrite */
+	
+	/********************	
+	** Open input list **
+	********************/
+	if ((pt_file = fopen(spec_lis, "r")) == NULL)
+	{
+		sprintf(err_str, "Unable to open file %s\n", spec_lis);
+		cf_if_error(err_str);
+	}
+	
+	/* ***********************************************
+	** Determine which spectrum has maximum OBSTIME **
+	** Write input file list to spec_list array.	**
+	*************************************************/
+	n_best_spec = -1;
+	n_spec = 0;
+	obstime_max = -1;
+    
+	while (fscanf(pt_file, "%80s", spec_name) != EOF)
+	{
+		FITS_open_file(&pt_fits, spec_name, READONLY, &status);
+		FITS_read_key(pt_fits, TFLOAT, "OBSTIME" , &obstime, NULL, &status);
+		FITS_read_key(pt_fits, TSTRING, "DETECTOR" , &detector, NULL, &status);
+		FITS_read_key(pt_fits, TSTRING, "APER_ACT" , &aper_act, NULL, &status);
+		FITS_close_file(pt_fits, &status);
+
+		sprintf(segment, "%2s%3s", detector, aper_act+5);
+		for (k=0; k<8; k++)
+			if (!strcmp(segment, extname[k])) {
+				strcpy(spec_list[k], spec_name); 
+				break;
+			}
+        	if (obstime_max < obstime) {
+			n_best_spec = k;
+			obstime_max = obstime;
+		}
+		n_spec++;
+	}
+	fclose(pt_file);
+	if (n_spec == 0) cf_if_error("No valid segments provided");
+	if (n_spec != 8) cf_if_warning("Combining fewer than 8 segments");
+
+	/* ***************************************************
+	** Copy header of reference spectrum to output file **
+	** Update a few header keywords.	 	    **
+	*****************************************************/
+
+	FITS_open_file(&pt_fits, spec_list[n_best_spec], READONLY, &status);
+	FITS_create_file(&pt_fits_out, out_name, &status);
+	FITS_copy_header(pt_fits, pt_fits_out, &status);
+	FITS_close_file(pt_fits, &status);
+
+	FITS_update_key(pt_fits_out, TSTRING, "FILENAME", (out_name + 1), NULL, &status);
+	FITS_update_key(pt_fits_out, TSTRING, "DETECTOR", "ALL", NULL, &status);
+	FITS_update_key(pt_fits_out, TSTRING, "COMB_COR", "COMPLETE", NULL, &status);
+	
+	sprintf(aper_key, "%4s", aper_act);
+	FITS_update_key(pt_fits_out, TSTRING, "APER_ACT", aper_key, NULL, &status);
+	FITS_update_key(pt_fits_out, TINT, "NEXTEND", &nextend_key, NULL, &status);
+
+	FITS_update_key(pt_fits_out, TFLOAT, "BANDWID", &bandwid, NULL, &status);
+	FITS_update_key(pt_fits_out, TFLOAT, "CENTRWV", &centrwv, NULL, &status);
+	FITS_update_key(pt_fits_out, TFLOAT, "WAVEMIN", &wavemin, NULL, &status);
+	FITS_update_key(pt_fits_out, TFLOAT, "WAVEMAX", &wavemax, NULL, &status);
+
+	FITS_read_key(pt_fits_out, TLONG, "NSPEC", &num_exp, NULL, &status);
+	FITS_delete_key(pt_fits_out, "NSPEC", &status);
+	for (i = 0L; i < num_exp; i++) {
+	    sprintf(keyname, "SPEC%03ld", i+1L);
+	    FITS_delete_key(pt_fits_out, keyname, &status);
+            sprintf(keyname, "WOFF*%03ld", i+1L);
+	    FITS_delete_key(pt_fits_out, keyname, &status);
+	    fits_delete_key(pt_fits_out, keyname, &status);
+	    if (status != 0) status = 0;
+	}
+
+
+	/* ***************************************************
+	** Step through detector segments.  
+	** Copy spectra into extensions of output file.
+	*****************************************************/
+	for (i = 0L; i < 8L; i++) {
+
+	    if (!strncmp(spec_list[i], "NULL", 4)) {
+		n_rows = 0L;
+		FITS_create_tbl(pt_fits_out, BINARY_TBL, n_rows, 3, ttype, tform,
+		tunit, extname[i], &status);
+		FITS_write_comment(pt_fits_out, "Extension is empty.  No data available.", &status);
+	    }
+	    else {
+		FITS_open_file(&pt_fits, spec_list[i], READONLY, &status);
+
+		FITS_movabs_hdu(pt_fits, 2, &hdutype, &status);
+        	FITS_get_colnum(pt_fits, TRUE, "WAVE", &wave_cnum, &status);
+		FITS_get_colnum(pt_fits, TRUE, "FLUX", &flux_cnum, &status);
+		FITS_get_colnum(pt_fits, TRUE, "ERROR", &error_cnum, &status);
+		FITS_get_num_rows(pt_fits, &n_rows, &status);
+		
+		FITS_create_tbl(pt_fits_out, BINARY_TBL, n_rows, 3, ttype, tform,
+			tunit, extname[i], &status);
+		
+		FITS_copy_col(pt_fits, pt_fits_out, wave_cnum, 1, FALSE, &status);
+		FITS_copy_col(pt_fits, pt_fits_out, flux_cnum, 2, FALSE, &status);
+		FITS_copy_col(pt_fits, pt_fits_out, error_cnum, 3, FALSE, &status);
+		
+		/* Copy various header keywords */
+		FITS_read_key(pt_fits, TSTRING, "COMBMETH", combmeth_key, NULL, &status);
+		FITS_update_key(pt_fits_out, TSTRING, "COMBMETH", combmeth_key, NULL, &status);
+
+		FITS_movabs_hdu(pt_fits, 1, &hdutype, &status);
+		FITS_read_key(pt_fits, TFLOAT, "W0", &w0, NULL, &status);
+		FITS_update_key(pt_fits_out, TFLOAT, "W0", &w0, NULL, &status);
+		FITS_read_key(pt_fits, TFLOAT, "WPC", &wpc, NULL, &status);
+		FITS_update_key(pt_fits_out, TFLOAT, "WPC", &wpc, NULL, &status);
+		FITS_read_key(pt_fits, TFLOAT, "OBSTIME", &obstime_key, NULL, &status);
+		FITS_update_key(pt_fits_out, TFLOAT, "OBSTIME", &obstime_key, NULL, &status);
+		FITS_read_key(pt_fits, TLONG, "NSPEC", &num_exp, NULL, &status);
+		FITS_update_key(pt_fits_out, TLONG, "NSPEC", &num_exp, NULL, &status);
+
+		for (j = 0L; j < num_exp; j++) {
+		    sprintf(keyname, "SPEC%03ld", j+1L);
+		    FITS_read_key(pt_fits, TSTRING, keyname, keyvalue, NULL, &status);
+		    FITS_update_key(pt_fits_out, TSTRING, keyname, keyvalue, NULL, &status);
+		    sprintf(keyname, "WOFF%03ld", j+1L);
+		    fits_read_key(pt_fits, TFLOAT, keyname, &woffset, comment, &status);
+		    if (status) {
+			status = 0;
+			woffset = 0.;
+			sprintf(comment, "[A]");
+		    }
+		    FITS_update_key(pt_fits_out, TFLOAT, keyname, &woffset, comment, &status);
+		}
+	        FITS_close_file(pt_fits, &status);
+	    }
+	}
+	if (n_spec != 8) {
+		char datestr[FLEN_CARD];
+		int timeref;
+		FITS_movabs_hdu(pt_fits_out, 1, &hdutype, &status);
+		FITS_write_comment(pt_fits_out, "  ", &status);
+		sprintf(comment, "Segments");
+		for (i=0L; i<8L; i++) if (!strncmp(spec_list[i], "NULL", 4))
+			sprintf(comment, "%s %s", comment, extname[i]);
+		sprintf(comment, "%s are missing.", comment);
+		FITS_write_comment(pt_fits_out, comment, &status);
+		sprintf(comment, "Extensions");
+		for (i=0L; i<8L; i++) if (!strncmp(spec_list[i], "NULL", 4))
+			sprintf(comment, "%s %ld", comment, i+1L);
+		sprintf(comment, "%s of this file contain no data.", comment);
+		FITS_write_comment(pt_fits_out, comment, &status);
+		fits_get_system_time(datestr, &timeref, &status);
+		sprintf(comment, "CalFUSE v%s   %.10s", CALFUSE_VERSION, datestr);
+		FITS_write_comment(pt_fits_out, comment, &status);
+		FITS_write_comment(pt_fits_out, "  ", &status);
+ 	}
+
+	/* Add an index to the file extensions. */
+	FITS_movabs_hdu(pt_fits_out, 1, &hdutype, &status);
+        FITS_write_comment(pt_fits_out, "  ", &status);
+        sprintf(comment, "Index to file extensions:");
+        FITS_write_comment(pt_fits_out, comment, &status);
+        sprintf(comment, "Extension 0   This Header");
+        FITS_write_comment(pt_fits_out, comment, &status);
+        for (i=0L; i<8L; i++) {
+                sprintf(comment, "Extension %ld   %s", i+1L, extname[i]);
+        	FITS_write_comment(pt_fits_out, comment, &status);
+	}
+        FITS_write_comment(pt_fits_out, "  ", &status);
+
+	FITS_close_file(pt_fits_out, &status);
+	
+	return(0);
+}
diff --git a/src/analysis/cf_reflux.c b/src/analysis/cf_reflux.c
new file mode 100644
index 0000000..1a2511f
--- /dev/null
+++ b/src/analysis/cf_reflux.c
@@ -0,0 +1,148 @@
+/*****************************************************************************
+ *		Johns Hopkins University
+ *		Center For Astrophysical Sciences
+ *		FUSE
+ *
+ * Synopsis:	cf_reflux input_file output_file aeff_cal1 [aeff_cal2]
+ *
+ * Description: Program applies a new flux calibration to an extracted
+ *		spectral file.  If two effective-area files are given,
+ *		program interpolates between them based on the MDJ
+ *		of the exposure.
+ *		Program writes a history line to output file header.
+ *
+ * Arguments:	input_file	FUSE extracted spectral file (fcal.fit)
+ *		output_file	Copy of input file with modified flux cal.
+ *		aeff_cal1	Effective-area curve
+ *		aeff_cal2	Optional effective-area curve, needed only
+ *				if you wish to interpolate.
+ *
+ * Returns:     none
+ *
+ * History:     06/02/05 1.1    wvd	Based on programs cf_uninterp and
+ *					cf_extract_spectra.
+ *
+ ****************************************************************************/
+
+#include <math.h>
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include "calfuse.h"
+
+static char CF_PRGM_ID[] = "cf_reflux";
+static char CF_VER_NUM[] = "1.1";
+
+int main(int argc, char *argv[])
+{
+    char  aper_act[FLEN_VALUE], datestr[FLEN_VALUE];
+    int   status=0, hdutype;
+    int   aperture, timeref;
+    long  i, frow=1, felement=1, nout;
+    float exptime, wpc;
+    float *wave, *flux, *error, *weights, *bkgd;
+    unsigned char *channel;
+    fitsfile *infits, *outfits;
+
+    /* Enter a timestamp into the log. */
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    /* Initialize error checking */
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+    if (argc < 4) {
+	printf("Usage: cf_reflux input_file output_file aeff_cal1 [aeff_cal2]\n");
+	return 0;
+    }
+
+    /* Copy input spectral file to output.  Close input file. */
+    FITS_open_file(&infits, argv[1], READONLY, &status);
+    FITS_create_file(&outfits, argv[2], &status);
+    FITS_copy_hdu(infits, outfits, 0, &status);
+    FITS_movrel_hdu(infits, 1, &hdutype, &status);
+    FITS_copy_hdu(infits, outfits, 0, &status);
+    FITS_close_file(infits, &status);
+
+    /* Modify output file keywords. */
+    FITS_movabs_hdu(outfits, 1, &hdutype, &status);
+    FITS_update_key(outfits, TSTRING, "FILENAME", argv[2], NULL, &status);
+    FITS_update_key(outfits, TSTRING, "AEFF1CAL", argv[3], NULL, &status);
+    if (argc == 5)
+	FITS_update_key(outfits, TSTRING, "AEFF2CAL", argv[4], NULL, &status);
+    else
+	FITS_update_key(outfits, TSTRING, "AEFF2CAL", argv[3], NULL, &status);
+
+    /* Add HISTORY lines to the output file */
+    fits_get_system_time(datestr, &timeref, &status);
+    strcat(datestr, "   File recalibrated using cf_reflux");
+    FITS_write_history(outfits, datestr, &status);
+
+    /* Through which aperture was this spectrum obtained? */
+    FITS_read_key(outfits, TSTRING, "APER_ACT", aper_act, NULL, &status);
+         if (!strcmp(aper_act, "HIRS_LIF")) aperture = 1;
+    else if (!strcmp(aper_act, "MDRS_LIF")) aperture = 2;
+    else if (!strcmp(aper_act, "LWRS_LIF")) aperture = 3;
+    else if (!strcmp(aper_act, "HIRS_SIC")) aperture = 5;
+    else if (!strcmp(aper_act, "MDRS_SIC")) aperture = 6;
+    else if (!strcmp(aper_act, "LWRS_SIC")) aperture = 7;
+    else {
+	printf("Unable to interpret header keyword APER_ACT = %s\n", aper_act);
+        FITS_close_file(outfits, &status);
+	return 0;
+    }
+
+    /* Read WAVE, FLUX, ERROR, WEIGHTS, and BKGD arrays */
+    FITS_movabs_hdu(outfits, 2, &hdutype, &status);
+    nout = cf_read_col(outfits, TFLOAT, "WAVE", (void **) &wave);
+    nout = cf_read_col(outfits, TFLOAT, "FLUX", (void **) &flux);
+    nout = cf_read_col(outfits, TFLOAT, "ERROR", (void **) &error);
+    nout = cf_read_col(outfits, TFLOAT, "WEIGHTS", (void **) &weights);
+    nout = cf_read_col(outfits, TFLOAT, "BKGD", (void **) &bkgd);
+    channel = (unsigned char *) cf_malloc(sizeof(unsigned char) * nout);
+
+    /* Compute inputs to flux-calibration routine */
+    for (i = 0; i < nout; i++) {
+	channel[i] = (unsigned char) aperture;
+	if (flux[i] != 0.) error[i] /= flux[i];		/* Relative error */
+	flux[i] = weights[i] - bkgd[i];			/* Units are counts */
+    }
+    
+    /* Apply flux calibration */
+    FITS_movabs_hdu(outfits, 1, &hdutype, &status);
+    FITS_update_key(outfits, TSTRING, "FLUX_COR", "PERFORM", NULL, &status) ;
+    cf_convert_to_ergs(outfits, nout, flux, flux, channel, wave);
+
+    /* Convert flux and error arrays to units of erg/cm2/s/A. */
+    FITS_movabs_hdu(outfits, 1, &hdutype, &status);
+    FITS_read_key(outfits, TFLOAT, "EXPTIME", &exptime, NULL, &status);
+    FITS_read_key(outfits, TFLOAT, "WPC", &wpc, NULL, &status);
+    if (exptime < 1) {
+	printf ("EXPTIME = %g.  Exiting.\n", exptime);
+        FITS_close_file(outfits, &status);
+	return 0;
+    }
+    for (i = 0; i < nout; i++) {
+        flux[i]  /= exptime * wpc;
+        error[i] *= flux[i];
+    }
+ 
+    /* Write new flux and error arrays to the output file. */
+    FITS_movabs_hdu(outfits, 2, &hdutype, &status);
+    FITS_write_col(outfits, TFLOAT, 2, frow, felement, nout, flux, &status);
+    FITS_write_col(outfits, TFLOAT, 3, frow, felement, nout, error, &status);
+ 
+    /* Close output file. */
+    FITS_close_file(outfits, &status);
+
+    /* Free memory. */
+    free(wave);
+    free(flux);
+    free(error);
+    free(weights);
+    free(bkgd);
+    free(channel);
+
+    /* Enter a timestamp into the log. */
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return 0;
+}
diff --git a/src/analysis/cf_ttag_to_hist.c b/src/analysis/cf_ttag_to_hist.c
new file mode 100644
index 0000000..070a1a6
--- /dev/null
+++ b/src/analysis/cf_ttag_to_hist.c
@@ -0,0 +1,463 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:   cf_ttag_to_hist input_file output_file
+ *
+ * Description: Creates a FITS 2D image from a time-tagged data file (FITS 
+ *              binary table of photon address data).  The 2D SIA table is
+ *              written to the first extension (HDU=1) and the other four
+ *              extensions contain the two apertures and stim-lamp pulses.
+ *
+ * 
+ * Arguments:   input_file      Input raw time-tagged FITS file name
+ *              output_file     Output raw histogram FITS file name
+ *
+ * Returns:     none
+ *
+ * History:     03/28/00 1.01   peb     Begin work
+ *              12/21/00 1.03   peb     Fixed type mismatched in cfitsio
+ *                                      calls
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include "calfuse.h"
+
+#define  STIMX 2048
+
+static char CF_PRGM_ID[] = "cf_ttag_to_hist";
+static char CF_VER_NUM[] = "1.03";
+
+int main(int argc, char *argv[])
+{
+    fitsfile *infits, *outfits;
+    char   buffer[FLEN_CARD], *siabuf;
+    int    status = 0, intnull, anynull, hdutype, fcol, begkey=5, endkey;
+    int    j, k1, kx1, ky1, k2, kx2, ky2, k3, kx3, ky3, k4, kx4, ky4;
+    int    naxis, naxis1, naxis2, naxis3, naxis4;
+    int    *posx, *posy, npixel, fpixel=1, frow, felem, nrow;
+    int    begx1, begy1, begx2, begy2, begx3, begy3, begx4, begy4;
+    int    rcnt1, rcnt2, rcnt3, rcnt4, min1, min2, min3, min4;
+    int    max1, max2, max3, max4, binx, biny;
+    int    keynum, nextend=4, extver=0, bzero=32768, bscale=1;
+    short  *outbuf1, *outbuf2, *outbuf3, *outbuf4;
+    long   naxes[2], naxes1[2], naxes2[2], naxes3[2], naxes4[2];
+    float  fzero=0.0;
+    double ra_targ, dec_targ, pa_aper, equinox;
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    /*
+     *  Open input ttag data file and create output file.
+     */
+    FITS_open_file(&infits, argv[1], READONLY, &status);
+    FITS_create_file(&outfits, argv[2], &status);
+    /*
+     *  Create primary image header
+     */
+    naxis = 2; naxes[0] = 8; naxes[1] = 64;
+    FITS_create_img(outfits, BYTE_IMG, naxis, naxes, &status);
+    /*
+     *  Copy header from primary HDU of the input file to the output file,
+     *  but leave the primary HDU data array empty.
+     */
+    FITS_read_key(infits, TINT, "SPECBINX", &binx, buffer, &status);
+    FITS_read_key(infits, TINT, "SPECBINY", &biny, buffer, &status);
+    FITS_get_hdrpos(infits, &endkey, &keynum, &status);
+    for (j = begkey; j <= endkey; j++) {
+	FITS_read_record(infits, j, buffer, &status);
+	FITS_write_record(outfits, buffer, &status);
+    }
+    FITS_update_key(outfits, TINT, "NEXTEND", &nextend, NULL, &status);
+    FITS_update_key(outfits, TSTRING, "FILETYPE", "RAW HISTOGRAM",
+		    NULL, &status);
+    FITS_update_key(outfits, TSTRING, "INSTMODE", "HIST", NULL, &status);
+    /*
+     *  Populate primary data or SIA table.
+     */
+    npixel = naxes[0]*naxes[1];
+    siabuf = cf_malloc(npixel);
+    memset(siabuf, 1, npixel);
+    FITS_write_img(outfits, TBYTE, fpixel, npixel, siabuf, &status);
+    free(siabuf);
+    /*
+     *  Move to the 1st HDU of the input file and read the binary table.
+     */
+    FITS_movabs_hdu(infits, 2, &hdutype, &status);
+    if(hdutype != BINARY_TBL) {
+	cf_if_error("Error: This HDU is not a binary table!");
+    }
+    FITS_read_key(infits, TINT,    "NAXIS2",  &nrow, buffer, &status);
+    FITS_read_key(infits, TDOUBLE, "RA_TARG", &ra_targ, buffer, &status);
+    FITS_read_key(infits, TDOUBLE, "DEC_TARG", &dec_targ, buffer, &status);
+    FITS_read_key(infits, TDOUBLE, "PA_APER", &pa_aper, buffer, &status);
+    FITS_read_key(infits, TDOUBLE, "EQUINOX", &equinox, buffer, &status);
+    /*
+     *  Allocate memory for X, Y photon event arrays
+     */
+    posx = cf_malloc(sizeof(int) * nrow);
+    posy = cf_malloc(sizeof(int) * nrow);
+    /*
+     *  Read X and Y from table
+     */
+    frow = felem = 1; intnull = anynull = 0;
+    
+    FITS_get_colnum(infits, TRUE, "X", &fcol, &status);
+    FITS_read_col(infits, TINT, fcol, frow, felem, nrow, &intnull,
+		  posx, &anynull, &status);
+    FITS_get_colnum(infits, TRUE, "Y", &fcol, &status);
+    FITS_read_col(infits, TINT, fcol, frow, felem, nrow, &intnull,
+		  posy, &anynull, &status);
+    /*
+     *  Create buffers (outbufn) to hold binned images, and
+     *  initialize them.
+     */
+    naxis1 = 2; naxes1[0] = NXMAX; naxes1[1] = 20;
+    begx1 = 0; begy1 = 48; rcnt1 = 56; min1 = max1 = 0;
+    outbuf1 = cf_calloc(naxes1[0]*naxes1[1], sizeof(short));
+
+    naxis2 = 2; naxes2[0] = NXMAX; naxes2[1] = 20;
+    begx2 = 0; begy2 = 76; rcnt2 = 57; min2 = max2 = 0;
+    outbuf2 = cf_calloc(naxes2[0]*naxes2[1], sizeof(short));
+
+    naxis3 = 2; naxes3[0] = STIMX; naxes3[1] = 2;
+    begx3 = 0; begy3 = 76; rcnt3 = 1; min3 = max3 = 0;
+    outbuf3 = cf_calloc(naxes3[0]*naxes3[1], sizeof(short));
+
+    naxis4 = 2; naxes4[0] = STIMX; naxes4[1] = 2;
+    begx4 = 14336; begy4 = 78; rcnt4 = 1; min4 = max4 = 0;
+    outbuf4 = cf_calloc(naxes4[0]*naxes4[1], sizeof(short));
+    
+    for(j = 0; j < nrow; j++) {
+	kx1 = posx[j]/binx-begx1;
+	ky1 = posy[j]/biny-begy1;
+	if (kx1 >= 0 && kx1 < naxes1[0] && ky1 >= 0 && ky1 < naxes1[1]) {
+	    k1 = naxes1[0]*ky1 + kx1;
+	    outbuf1[k1] += 1;
+	    if (outbuf1[k1] < min1)
+		min1 = outbuf1[k1];
+	    if (outbuf1[k1] > max1)
+		max1 = outbuf1[k1];
+	}
+	kx2 = posx[j]/binx-begx2;
+	ky2 = posy[j]/biny-begy2;
+	if (kx2 >= 0 && kx2 < naxes2[0] && ky2 >= 0 && ky2 < naxes2[1]) {
+	    k2 = naxes2[0]*ky2 + kx2;
+	    outbuf2[k2] += 1;
+	    if (outbuf2[k2] < min2)
+		min2 = outbuf2[k2];
+	    if (outbuf2[k2] > max2)
+		max2 = outbuf2[k2];
+	}
+	kx3 = posx[j]/binx-begx3;
+	ky3 = posy[j]/biny-begy3;
+	if (kx3 >= 0 && kx3 < naxes3[0] && ky3 >= 0 && ky3 < naxes3[1]) {
+	    k3 = naxes3[0]*ky3 + kx3;
+	    outbuf3[k3] += 1;
+	    if (outbuf3[k3] < min3)
+		min3 = outbuf3[k3];
+	    if (outbuf3[k3] > max3)
+		max3 = outbuf3[k3];
+	}
+	kx4 = posx[j]/binx-begx4;
+	ky4 = posy[j]/biny-begy4;
+	if (kx4 >= 0 && kx4 < naxes4[0] && ky4 >= 0 && ky4 < naxes4[1]) {
+	    k4 = naxes4[0]*ky4 + kx4;
+	    outbuf4[k4] += 1;
+	    if (outbuf4[k4] < min4)
+		min4 = outbuf4[k4];
+	    if (outbuf4[k4] > max4)
+		max4 = outbuf4[k4];
+	}
+    }
+    /*
+     *  Extension 1
+     */
+    FITS_create_img(outfits, SHORT_IMG, naxis1, naxes1, &status);
+    extver = 1;
+    
+    FITS_write_key(outfits, TSTRING, "EXTNAME", "HISTOGRAM",
+		   "name of this extension", &status);
+    FITS_write_key(outfits, TINT, "EXTVER" , &extver,
+		   "extension version number", &status);
+    FITS_write_key(outfits, TINT, "BZERO"  , &bzero,
+		   "image brightness offset", &status);
+    FITS_write_key(outfits, TINT, "BSCALE" , &bscale,
+		   "image brightness scale", &status);
+    
+    FITS_write_comment(outfits, "        ", &status);
+    FITS_write_comment(outfits, "        ", &status);
+    FITS_write_comment(outfits,
+		       "    World Coordinate System and Related Parameters",
+		       &status);
+    FITS_write_comment(outfits, "        ", &status);
+    
+    FITS_write_key(outfits, TFLOAT,  "CRPIX1",  &fzero,
+		   "x-coordinate of reference pixel", &status);
+    FITS_write_key(outfits, TFLOAT,  "CRPIX2",  &fzero, 
+		   "y-coordinate of reference pixel", &status);
+    FITS_write_key(outfits, TFLOAT,  "CRVAL1",  &fzero, 
+		   "first axis value at reference pixel", &status);
+    FITS_write_key(outfits, TFLOAT,  "CRVAL2",  &fzero,
+		   "second axis value at reference pixel", &status);
+    FITS_write_key(outfits, TSTRING, "CTYPE1", "LAMBDA", 
+		   "the coordinate type for the first axis", &status);
+    FITS_write_key(outfits, TSTRING, "CYTPE2", "ANGLE", 
+		   "the coordinate type for the second axis", &status);
+    FITS_write_key(outfits, TFLOAT,  "CD1_1",   &fzero,
+		   "partial of first axis coordinate w.r.t. x", &status);
+    FITS_write_key(outfits, TFLOAT,  "CD1_2",   &fzero,
+		   "partial of first axis coordinate w.r.t. y", &status);
+    FITS_write_key(outfits, TFLOAT,  "CD2_1",   &fzero,
+		   "partial of second axis coordinate w.r.t. x", &status);
+    FITS_write_key(outfits, TFLOAT,  "CD2_2",   &fzero,
+		   "partial of second axis coordinate w.r.t. y", &status);
+    FITS_write_key(outfits, TDOUBLE,  "RA_TARG", &ra_targ,
+		   "RA of reference aperture center", &status);
+    FITS_write_key(outfits, TDOUBLE,  "DEC_TARG", &dec_targ,
+		   "Declination of reference aperture center", &status);
+    FITS_write_key(outfits, TDOUBLE,  "PA_APER", &pa_aper,
+		   "Position Angle of reference aperture center", &status);
+    FITS_write_key(outfits, TDOUBLE,  "EQUINOX", &equinox,
+		   "equinox of celestial coord. system", &status);
+    
+    FITS_write_comment(outfits, "        ", &status);
+    FITS_write_comment(outfits, "    HISTOGRAM REGION PARAMETERS", &status);
+    FITS_write_comment(outfits, "        ", &status);
+    
+    FITS_write_key(outfits, TINT, "XORIGIN", &begx1,
+		   "offset of this region in the x dimension", &status);
+    FITS_write_key(outfits, TINT, "YORIGIN", &begy1,
+		   "offset of this region in the y dimension", &status);
+    FITS_write_key(outfits, TINT, "RCOUNT",  &rcnt1,
+		   "count of rectangles in this region", &status);
+    FITS_write_key(outfits, TINT, "MINVAL",  &min1,
+		   "minimum value within rectangles", &status);
+    FITS_write_key(outfits, TINT, "MAXVAL",  &max1,
+		   "maximum value within rectangles", &status);
+
+    FITS_write_img(outfits, TSHORT, fpixel, naxes1[0]*naxes1[1],
+		   outbuf1, &status);
+    /*
+     *  Extension 2
+     */
+    FITS_create_img(outfits, SHORT_IMG, naxis2, naxes2, &status);
+    extver = 2;
+    
+    FITS_write_key(outfits, TSTRING, "EXTNAME", "HISTOGRAM",
+		   "name of this extension", &status);
+    FITS_write_key(outfits, TINT, "EXTVER" , &extver,
+		   "extension version number", &status);
+    FITS_write_key(outfits, TINT, "BZERO"  , &bzero,
+		   "image brightness offset", &status);
+    FITS_write_key(outfits, TINT, "BSCALE" , &bscale,
+		   "image brightness scale", &status);
+    
+    FITS_write_comment(outfits, "        ", &status);
+    FITS_write_comment(outfits, "        ", &status);
+    FITS_write_comment(outfits,
+		       "    World Coordinate System and Related Parameters",
+		       &status);
+    FITS_write_comment(outfits, "        ", &status);
+    
+    FITS_write_key(outfits, TFLOAT,  "CRPIX1",  &fzero,
+		   "x-coordinate of reference pixel", &status);
+    FITS_write_key(outfits, TFLOAT,  "CRPIX2",  &fzero, 
+		   "y-coordinate of reference pixel", &status);
+    FITS_write_key(outfits, TFLOAT,  "CRVAL1",  &fzero, 
+		   "first axis value at reference pixel", &status);
+    FITS_write_key(outfits, TFLOAT,  "CRVAL2",  &fzero,
+		   "second axis value at reference pixel", &status);
+    FITS_write_key(outfits, TSTRING, "CTYPE1", "LAMBDA", 
+		   "the coordinate type for the first axis", &status);
+    FITS_write_key(outfits, TSTRING, "CYTPE2", "ANGLE", 
+		   "the coordinate type for the second axis", &status);
+    FITS_write_key(outfits, TFLOAT,  "CD1_1",   &fzero,
+		   "partial of first axis coordinate w.r.t. x", &status);
+    FITS_write_key(outfits, TFLOAT,  "CD1_2",   &fzero,
+		   "partial of first axis coordinate w.r.t. y", &status);
+    FITS_write_key(outfits, TFLOAT,  "CD2_1",   &fzero,
+		   "partial of second axis coordinate w.r.t. x", &status);
+    FITS_write_key(outfits, TFLOAT,  "CD2_2",   &fzero,
+		   "partial of second axis coordinate w.r.t. y", &status);
+    FITS_write_key(outfits, TDOUBLE,  "RA_TARG", &ra_targ,
+		   "RA of reference aperture center", &status);
+    FITS_write_key(outfits, TDOUBLE,  "DEC_TARG", &dec_targ,
+		   "Declination of reference aperture center", &status);
+    FITS_write_key(outfits, TDOUBLE,  "PA_APER", &pa_aper,
+		   "Position Angle of reference aperture center", &status);
+    FITS_write_key(outfits, TDOUBLE,  "EQUINOX", &equinox,
+		   "equinox of celestial coord. system", &status);
+    
+    FITS_write_comment(outfits, "        ", &status);
+    FITS_write_comment(outfits, "    HISTOGRAM REGION PARAMETERS", &status);
+    FITS_write_comment(outfits, "        ", &status);
+    
+    FITS_write_key(outfits, TINT, "XORIGIN", &begx2,
+		   "offset of this region in the x dimension", &status);
+    FITS_write_key(outfits, TINT, "YORIGIN", &begy2,
+		   "offset of this region in the y dimension", &status);
+    FITS_write_key(outfits, TINT, "RCOUNT",  &rcnt2,
+		   "count of rectangles in this region", &status);
+    FITS_write_key(outfits, TINT, "MINVAL",  &min2,
+		   "minimum value within rectangles", &status);
+    FITS_write_key(outfits, TINT, "MAXVAL",  &max2,
+		   "maximum value within rectangles", &status);
+
+    FITS_write_img(outfits, TSHORT, fpixel, naxes2[0]*naxes2[1],
+		   outbuf2, &status);
+    /*
+     *  Extension 3
+     */
+    FITS_create_img(outfits, SHORT_IMG, naxis3, naxes3, &status);
+    extver = 3;
+    
+    FITS_write_key(outfits, TSTRING, "EXTNAME", "HISTOGRAM",
+		   "name of this extension", &status);
+    FITS_write_key(outfits, TINT, "EXTVER" , &extver,
+		   "extension version number", &status);
+    FITS_write_key(outfits, TINT, "BZERO"  , &bzero,
+		   "image brightness offset", &status);
+    FITS_write_key(outfits, TINT, "BSCALE" , &bscale,
+		   "image brightness scale", &status);
+    
+    FITS_write_comment(outfits, "        ", &status);
+    FITS_write_comment(outfits, "        ", &status);
+    FITS_write_comment(outfits,
+		       "    World Coordinate System and Related Parameters",
+		       &status);
+    FITS_write_comment(outfits, "        ", &status);
+    
+    FITS_write_key(outfits, TFLOAT,  "CRPIX1",  &fzero,
+		   "x-coordinate of reference pixel", &status);
+    FITS_write_key(outfits, TFLOAT,  "CRPIX2",  &fzero, 
+		   "y-coordinate of reference pixel", &status);
+    FITS_write_key(outfits, TFLOAT,  "CRVAL1",  &fzero, 
+		   "first axis value at reference pixel", &status);
+    FITS_write_key(outfits, TFLOAT,  "CRVAL2",  &fzero,
+		   "second axis value at reference pixel", &status);
+    FITS_write_key(outfits, TSTRING, "CTYPE1", "LAMBDA", 
+		   "the coordinate type for the first axis", &status);
+    FITS_write_key(outfits, TSTRING, "CYTPE2", "ANGLE", 
+		   "the coordinate type for the second axis", &status);
+    FITS_write_key(outfits, TFLOAT,  "CD1_1",   &fzero,
+		   "partial of first axis coordinate w.r.t. x", &status);
+    FITS_write_key(outfits, TFLOAT,  "CD1_2",   &fzero,
+		   "partial of first axis coordinate w.r.t. y", &status);
+    FITS_write_key(outfits, TFLOAT,  "CD2_1",   &fzero,
+		   "partial of second axis coordinate w.r.t. x", &status);
+    FITS_write_key(outfits, TFLOAT,  "CD2_2",   &fzero,
+		   "partial of second axis coordinate w.r.t. y", &status);
+    FITS_write_key(outfits, TDOUBLE,  "RA_TARG", &ra_targ,
+		   "RA of reference aperture center", &status);
+    FITS_write_key(outfits, TDOUBLE,  "DEC_TARG", &dec_targ,
+		   "Declination of reference aperture center", &status);
+    FITS_write_key(outfits, TDOUBLE,  "PA_APER", &pa_aper,
+		   "Position Angle of reference aperture center", &status);
+    FITS_write_key(outfits, TDOUBLE,  "EQUINOX", &equinox,
+		   "equinox of celestial coord. system", &status);
+    
+    FITS_write_comment(outfits, "        ", &status);
+    FITS_write_comment(outfits, "    HISTOGRAM REGION PARAMETERS", &status);
+    FITS_write_comment(outfits, "        ", &status);
+    
+    FITS_write_key(outfits, TINT, "XORIGIN", &begx3,
+		   "offset of this region in the x dimension", &status);
+    FITS_write_key(outfits, TINT, "YORIGIN", &begy3,
+		   "offset of this region in the y dimension", &status);
+    FITS_write_key(outfits, TINT, "RCOUNT",  &rcnt3,
+		   "count of rectangles in this region", &status);
+    FITS_write_key(outfits, TINT, "MINVAL",  &min3,
+		   "minimum value within rectangles", &status);
+    FITS_write_key(outfits, TINT, "MAXVAL",  &max3,
+		   "maximum value within rectangles", &status);
+
+    FITS_write_img(outfits, TSHORT, fpixel, naxes3[0]*naxes3[1],
+		   outbuf3, &status);
+    /*
+     *  Extension 4
+     */
+    FITS_create_img(outfits, SHORT_IMG, naxis4, naxes4, &status);
+    extver = 4;
+    
+    FITS_write_key(outfits, TSTRING, "EXTNAME", "HISTOGRAM",
+		   "name of this extension", &status);
+    FITS_write_key(outfits, TINT, "EXTVER" , &extver,
+		   "extension version number", &status);
+    FITS_write_key(outfits, TINT, "BZERO"  , &bzero,
+		   "image brightness offset", &status);
+    FITS_write_key(outfits, TINT, "BSCALE" , &bscale,
+		   "image brightness scale", &status);
+    
+    FITS_write_comment(outfits, "        ", &status);
+    FITS_write_comment(outfits, "        ", &status);
+    FITS_write_comment(outfits,
+		       "    World Coordinate System and Related Parameters",
+		       &status);
+    FITS_write_comment(outfits, "        ", &status);
+    
+    FITS_write_key(outfits, TFLOAT,  "CRPIX1",  &fzero,
+		   "x-coordinate of reference pixel", &status);
+    FITS_write_key(outfits, TFLOAT,  "CRPIX2",  &fzero, 
+		   "y-coordinate of reference pixel", &status);
+    FITS_write_key(outfits, TFLOAT,  "CRVAL1",  &fzero, 
+		   "first axis value at reference pixel", &status);
+    FITS_write_key(outfits, TFLOAT,  "CRVAL2",  &fzero,
+		   "second axis value at reference pixel", &status);
+    FITS_write_key(outfits, TSTRING, "CTYPE1", "LAMBDA", 
+		   "the coordinate type for the first axis", &status);
+    FITS_write_key(outfits, TSTRING, "CYTPE2", "ANGLE", 
+		   "the coordinate type for the second axis", &status);
+    FITS_write_key(outfits, TFLOAT,  "CD1_1",   &fzero,
+		   "partial of first axis coordinate w.r.t. x", &status);
+    FITS_write_key(outfits, TFLOAT,  "CD1_2",   &fzero,
+		   "partial of first axis coordinate w.r.t. y", &status);
+    FITS_write_key(outfits, TFLOAT,  "CD2_1",   &fzero,
+		   "partial of second axis coordinate w.r.t. x", &status);
+    FITS_write_key(outfits, TFLOAT,  "CD2_2",   &fzero,
+		   "partial of second axis coordinate w.r.t. y", &status);
+    FITS_write_key(outfits, TDOUBLE,  "RA_TARG", &ra_targ,
+		   "RA of reference aperture center", &status);
+    FITS_write_key(outfits, TDOUBLE,  "DEC_TARG", &dec_targ,
+		   "Declination of reference aperture center", &status);
+    FITS_write_key(outfits, TDOUBLE,  "PA_APER", &pa_aper,
+		   "Position Angle of reference aperture center", &status);
+    FITS_write_key(outfits, TDOUBLE,  "EQUINOX", &equinox,
+		   "equinox of celestial coord. system", &status);
+    
+    FITS_write_comment(outfits, "        ", &status);
+    FITS_write_comment(outfits, "    HISTOGRAM REGION PARAMETERS", &status);
+    FITS_write_comment(outfits, "        ", &status);
+    
+    FITS_write_key(outfits, TINT, "XORIGIN", &begx4,
+		   "offset of this region in the x dimension", &status);
+    FITS_write_key(outfits, TINT, "YORIGIN", &begy4,
+		   "offset of this region in the y dimension", &status);
+    FITS_write_key(outfits, TINT, "RCOUNT",  &rcnt4,
+		   "count of rectangles in this region", &status);
+    FITS_write_key(outfits, TINT, "MINVAL",  &min4,
+		   "minimum value within rectangles", &status);
+    FITS_write_key(outfits, TINT, "MAXVAL",  &max4,
+		   "maximum value within rectangles", &status);
+
+    FITS_write_img(outfits, TSHORT, fpixel, naxes4[0]*naxes4[1],
+		   outbuf4, &status);
+    /*
+     *  Free memory and close the input and output files
+     */
+    free(outbuf1);
+    free(outbuf2);
+    free(outbuf3);
+    free(outbuf4);
+    free(posx);
+    free(posy);
+    
+    FITS_close_file(outfits, &status);
+    FITS_close_file(infits, &status);
+
+    return 0;
+}
diff --git a/src/analysis/cf_wrspec7.c b/src/analysis/cf_wrspec7.c
new file mode 100644
index 0000000..979046b
--- /dev/null
+++ b/src/analysis/cf_wrspec7.c
@@ -0,0 +1,58 @@
+/*******************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *******************************************************************************
+ *
+ * Synopsis:    cf_wrspec7(fitsfile *outfits, long npts, float *wave, float *flux,
+ *		           float *error, long *counts, float *weights,
+ *                         float *bkgd,short *pothole)
+ *
+ * Description: Write a file containing a FUSE 2D spectrum.
+ *
+ * Arguments:   fitsfile *fname		Output FITS file structure
+ *
+ * Returns:     none
+ *
+ * History:     12/15/03        bjg     Begin work from cf_wrspec4.
+ *              01/12/04        bjg     Call to fits_create_tbl with nrow=1
+ *                                      instead of npts
+ *              03/22/04        bjg     Change POTHOLE to QUALITY
+ *              03/25/04        bjg     Moved time stamp writing to beginning 
+ *                                      of routine
+ *              04/07/05  v1.1  tc      Create a multi-rows table rather than
+ *                                      a unique vector in a cell
+ *
+ ******************************************************************************/
+
+#include <stdio.h>
+#include <stdlib.h>
+#include "calfuse.h"
+
+static char CF_PRGM_ID[] = "cf_wrspec7";
+static char CF_VER_NUM[] = "1.1";
+
+void cf_wrspec7(fitsfile *outfits, long npts, float *wave, float *flux,
+		float *error, long *counts, float *weights,float *bkgd,short *pothole)
+{
+	char	*ttype[] = {"WAVE", "FLUX", "ERROR", "COUNTS", "WEIGHTS", "BKGD", "QUALITY" };
+	char	*tform[] = {"1E", "1E", "1E", "1J", "1E", "1E", "1I"};
+	char	*tunit[] = {"ANGSTROMS", "ERG/CM2/S/A", "ERG/CM2/S/A", "COUNTS", "COUNTS", "COUNTS", "UNITLESS"};
+	char	extname[] = "FUSE 2D Spectrum";
+	int	tfields = 7, status = 0;
+
+	/* Write time stamp to log file. */
+	cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "");
+		
+	fits_create_tbl(outfits, BINARY_TBL, 1, tfields, ttype,	tform, tunit, extname, &status);
+     
+	/* Write out the data. */
+	FITS_write_col(outfits, TFLOAT, 1, 1L, 1L, npts, wave, &status);
+	FITS_write_col(outfits, TFLOAT, 2, 1L, 1L, npts, flux, &status);
+	FITS_write_col(outfits, TFLOAT, 3, 1L, 1L, npts, error, &status );
+	FITS_write_col(outfits, TLONG, 4, 1L, 1L, npts, counts, &status);
+	FITS_write_col(outfits, TFLOAT, 5, 1L, 1L, npts, weights, &status);
+	FITS_write_col(outfits, TFLOAT, 6, 1L, 1L, npts, bkgd, &status);
+	FITS_write_col(outfits, TSHORT, 7, 1L, 1L, npts, pothole, &status);
+	
+}
diff --git a/src/analysis/cf_wrspec_cf2.c b/src/analysis/cf_wrspec_cf2.c
new file mode 100644
index 0000000..883c3d5
--- /dev/null
+++ b/src/analysis/cf_wrspec_cf2.c
@@ -0,0 +1,120 @@
+/*******************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *******************************************************************************
+ *
+ * Synopsis:    cf_wrspec_cf2(fitsfile *outfits, int npts, float *wave,
+ *				float *spec, float *errs, short *qual,
+ *                              float *counts, float *cntserr, int ncol,
+ *				int areaflag);
+ *
+ * Description: Write a file containing a FUSE 1D spectrum, in a format
+ *		compatible with Calfuse 2.4 and earlier.
+ *
+ * Arguments:   char    *fname		Output file name
+ *		float	*wave		wavelengths
+ *		float	*spec		spectrum
+ *		float	*errs		associated 1-sigma error bars
+ *		short	*qual		associated quality flags
+ *		float	*counts		total counts in column
+ *		float	*cntserr	1-sigma error bar on total counts
+ *		int	ncol		specifies 4 or 6 column format
+ *		int	areaflag	0 if spectrum column is FLUX
+ *					1 if spectrum column is AREA
+ *
+ * Returns:     none
+ *
+ * History:     05/04/98        gak     Begin work.
+ *              04/20/99        emm     Added FITS_ error checking routines,
+ *                                      converted qual flags to BYTE.
+ *              06/07/99 1.2    peb     Added reporting of version number.
+ *              10/22/99 1.3    emm     Added total counts column.
+ *              10/22/99 1.4    emm     Added total counts errors column.
+ *              10/22/99 1.5    emm     totcnts and errors are just duplicates
+ *                                      of flux and error for now
+ *              10/29/99 1.6    emm     counts and cntserr are now read in
+ *                                      from calling program.
+ *              12/21/99 1.7    emm     Quality flags now short (1I) instead
+ *                                      of byte char (1B).
+ *              11/30/01 1.8    wvd     Don't write timestamp to log file.
+ *		03/08/04 1.9    jwk     allow tfields=4 or 6, and option to
+ *					change "FLUX" col to "AREA"; for use
+ *					with cf_arith
+ *              04/05/04        bjg     Include string.h
+ *                                      Write timestamp
+ *
+ ******************************************************************************/
+
+#include <stdio.h>
+#include <stdlib.h>
+#include <string.h>
+#include "calfuse.h"
+
+static char CF_PRGM_ID[] = "cf_wrspec_cf2";
+static char CF_VER_NUM[] = "1.9";
+
+void cf_wrspec_cf2(fitsfile *outfits, int npts, float *wave, float *spec,
+		float *errs, short *qual, float *counts, float *cntserr,
+		int ncol, int areaflag)
+{
+	char	*ttype[] = {"WAVE", "FLUX", "ERROR", "QUALITY", "COUNTS","CNTSERR"};
+	char	*tform[] = {"1E", "1E", "1E", "1I", "1E", "1E"};
+	char	*tunit[] = {"ANGSTROMS", "ERG/CM2/S/A", "ERG/CM2/S/A", " ","COUNTS","COUNTS"};
+	char	extname[] = "FUSE 1D Spectrum";
+	int	tfields = 6,
+		status = 0;
+	long	felem = 1,
+		frow = 1;	
+
+/* Write time stamp to log file. */
+	cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "");
+
+
+/* Create the extension for the data in the output file.
+   Columns will be
+	WAVE	1E
+	FLUX	1E
+	ERROR	1E
+	QUALITY	1B
+	TOTAL COUNTS 1E      Same as FLUX column for now
+	COUNTS ERRORS 1E     Same as ERROR column for now
+*/
+
+    if (ncol == 4)
+	{
+	tfields = 4;
+	if (areaflag)
+	   {
+	   strcpy(ttype[1], "AREA");
+	   strcpy(tunit[1], "CM^2");
+	   strcpy(tunit[2], "CM^2");
+	   }
+	}
+
+	fits_create_tbl (outfits, BINARY_TBL, (long)npts, tfields, ttype,
+	     tform, tunit, extname, &status);
+
+/* Write out the data. */
+	FITS_write_col(outfits, TFLOAT, 1, frow, felem, (long)npts, 
+		       wave, &status);
+
+	FITS_write_col(outfits, TFLOAT, 2, frow, felem, (long)npts,
+		       spec, &status);
+
+	FITS_write_col(outfits, TFLOAT, 3, frow, felem, (long)npts,
+		       errs, &status );
+
+	FITS_write_col(outfits,  TSHORT, 4, frow, felem, (long)npts,
+		       qual, &status);
+
+	if (tfields == 6)
+	  {
+	  FITS_write_col(outfits, TFLOAT, 5, frow, felem, (long)npts,
+		       counts, &status);
+
+	  FITS_write_col(outfits, TFLOAT, 6, frow, felem, (long)npts,
+		       cntserr, &status);
+	  }
+
+}
diff --git a/src/analysis/cf_xcorr.c b/src/analysis/cf_xcorr.c
new file mode 100644
index 0000000..383f281
--- /dev/null
+++ b/src/analysis/cf_xcorr.c
@@ -0,0 +1,303 @@
+/*******************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *******************************************************************************
+ *
+ * Usage:    cf_xcorr exposure_list exp_shift_list
+ *
+ * Description: Determine pixel shifts between exposures. The
+ *              reference spectrum is the one having the longest exposure
+ *              time. The input list (ASCII) is the set of exposures to process,
+ *              the output list (ASCII) has 3 columns: exposure name, shift and
+ *              sigma_shift. Sigma_shift = -1 corresponds to non-detected shift.
+ *		Sigma_shift = 1 indicates a valid shift value.
+ *              The reference exposure always has shift and sigma_shift of 0.
+ *
+ * History:     04/07/05        tc      v1.0    First release
+ *              04/15/05        tc      v1.1    Use cf_read_col
+ *              04/27/05       wvd      v1.2    Use variance arrays properly.
+ *						Use QUALITY array to identify
+ *						   bad data.
+ *						Change spec array to type INT.
+ *						Use chi2, not reduced chi2,
+ *						   to set error bars.
+ *              05/20/05       wvd      v1.3    For continuum spectra, use
+ *						single region between 1045 and
+ *						1070 A.  For emission-line
+ *						targets, use O VI lines.
+ *              06/03/05       wvd      v1.4    Delete unused variables.
+ *              07/21/05       wvd      v1.5    Adopt the sign convention for 
+ *						spectral shifts used by
+ *						FUSE_REGISTER.
+ *              08/01/05       wvd      v1.6    Store EXPNIGHT of reference
+ *						spectrum in ref_expnight.
+ *              09/13/05       wvd      v1.7    If called with no arguments,
+ *						return calling info, not error.
+ *              04/27/06       wvd      v1.8    Scale each spectrum to match
+ *						mean of reference spectrum.
+ *              05/16/06       wvd      v1.9    Use Lyman beta to align 
+ *						background exposures.
+ *						Use O VI and C II to align WD's.
+ *              03/28/08       wvd      v1.10   Write value of NORM to output.
+ *						For HIST data only: if XCORRR
+ *						fails, but NORM > 0.5, then
+ *						set shift and sigma to 0.
+ *              08/15/08       wvd      v1.11   If EXP_STAT = 2, treat as
+ *						background observation.
+ *
+ ******************************************************************************/
+ 
+#include <math.h>
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include "calfuse.h"
+
+/* Calfuse variables */
+static char CF_PRGM_ID[] = "cf_xcorr";
+static char CF_VER_NUM[] = "1.11";
+
+/* Parameters */
+#define MAXSHIFT     20
+#define N_SHIFT	     41
+
+int main(int argc, char *argv[])
+{
+	/* Variables */
+	char *spec_lis, *out_name, src_type[FLEN_VALUE];
+	char spec_name[FLEN_FILENAME], ref_spec_name[FLEN_FILENAME];
+	char program[FLEN_VALUE]; 
+	char instmode[FLEN_CARD] ;
+	double *ref_flux, *ref_error, *flux, *error;
+	double scale, sum, variance, norm, ref_tot, total;
+	float chi_square[N_SHIFT], chi_square_min, chi_square_max;
+	float exptime, exptime_max;
+	float *wave, w0, wpc, wmin, wdelta;
+	int ly_beta=FALSE, exp_stat, objclass, shift, sigma;
+	int ind_chi2_min, N, N_tmp, nchi, n_spec, ind_ref_spec=0;
+	long expnight, ref_expnight, i, k, n_pix, ref_start, start;
+    
+	FILE *pt_file, *pt_file_out;
+	fitsfile *in_fits;
+	int status = 0, hdutype = 0;
+	
+	/***********************************
+	** Enter a timestamp into the log **
+	***********************************/
+	cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+	cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+
+	/***********************************************************	
+	** Check for proper command-line usage and read arguments **
+	***********************************************************/
+	if (argc != 3) {
+		printf("Usage: cf_xcorr exposure_list exp_shift_list\n");
+		return(0);
+	}
+
+	spec_lis = argv[1];
+	out_name = argv[2];
+	
+	/********************************************	
+	** Open input list and create output file  **
+	********************************************/
+	if ((pt_file = fopen(spec_lis, "r")) == NULL)
+	{
+		cf_if_error("Unable to open file %s", spec_lis);
+	}
+	pt_file_out = fopen(out_name, "w");
+
+	/********************************************************************
+	** Set the reference spectrum to the one which has maximum EXPTIME **
+	********************************************************************/
+	n_spec = 0;
+	exptime_max = -1;
+    
+	while (fscanf(pt_file, "%80s", spec_name) != EOF)
+	{
+		FITS_open_file(&in_fits, spec_name, READONLY, &status);
+		FITS_read_key(in_fits, TFLOAT, "EXPTIME", &exptime, NULL, &status);
+		FITS_read_key(in_fits, TLONG, "EXPNIGHT", &expnight, NULL, &status);
+		FITS_close_file(in_fits, &status);
+        	if (exptime > exptime_max)
+		{
+			exptime_max = exptime;
+			ind_ref_spec = n_spec;
+			strcpy(ref_spec_name, spec_name);
+		}
+		n_spec++;
+	}
+	
+	if (n_spec == 0) cf_if_error("At least one spectrum is required");
+	
+	if (n_spec == 1)
+	{
+		fprintf(pt_file_out, "%s %2d %2d %5.0f %5ld %c%c%c 1.0\n", ref_spec_name, 0, 0,
+			exptime_max, expnight, ref_spec_name[8], ref_spec_name[9], ref_spec_name[10]);
+		fclose(pt_file_out);
+		return(0);
+	}
+	printf("n_spec: %d, max exptime: %g, ind_ref: %d, ref_name: %s\n",
+		n_spec, exptime_max, ind_ref_spec, ref_spec_name);
+		
+        /* Read source type and set XCORR limits accordingly. */
+	FITS_open_file(&in_fits, ref_spec_name, READONLY, &status);
+        FITS_read_key(in_fits, TINT, "EXP_STAT", &exp_stat, NULL, &status);
+        FITS_read_key(in_fits, TSTRING, "PRGRM_ID", &program, NULL, &status);
+        FITS_read_key(in_fits, TINT, "OBJCLASS", &objclass, NULL, &status);
+        FITS_read_key(in_fits, TSTRING, "SRC_TYPE", &src_type, NULL, &status);
+	FITS_read_key(in_fits, TSTRING, "INSTMODE", instmode, NULL, &status) ;
+	FITS_read_key(in_fits, TFLOAT, "W0", &w0, NULL, &status);
+	FITS_read_key(in_fits, TFLOAT, "WPC", &wpc, NULL, &status);
+        if (src_type[1] == 'E') {       /* Emission-line source */
+			/* Use Lyman beta to align background observations. */
+	    if (exp_stat == (int) TEMPORAL_LIMB || 
+		objclass == 1 || objclass == 7 || objclass == 90) {
+                printf("Assuming background observation.\n");
+            	wmin = 1024.;
+            	wdelta = 6.;
+		ly_beta = TRUE;
+	    } else {	/* Use O VI emission for everything else. */
+                printf("SRC_TYPE = %s.  Emission-line target.\n", src_type);
+            	wmin = 1030.;
+            	wdelta = 9.;
+	    }
+        }
+	else if (objclass == 17 || objclass == 29 || objclass == 37) {
+			/* Use O VI and C II to align white dwarf spectra. */
+            printf("OBJCLASS = %d.  Assuming nearby white dwarf.\n", objclass);
+            wmin = 1030.;
+            wdelta = 9.;
+        }
+        else {  /* Use 1045-1070 A region for all other continuum sources. */
+            printf("SRC_TYPE = %s.  Assuming continuum target.\n", src_type);
+            wmin = 1045.;
+            wdelta = 25.;
+        }
+        start = cf_nlong((wmin - w0) / wpc);
+        ref_start = start + MAXSHIFT;
+        n_pix = cf_nlong(wdelta / wpc) - (N_SHIFT - 1);
+
+	/* Read wave, flux, and error arrays from reference exposure. */	
+	FITS_read_key(in_fits, TLONG, "EXPNIGHT" , &ref_expnight, NULL, &status);
+	FITS_movabs_hdu(in_fits, 2, &hdutype, &status);
+	if (hdutype != BINARY_TBL) cf_if_error("FITS files must contain BINARY TABLE in HDU #2");
+	N = cf_read_col(in_fits, TFLOAT, "WAVE", (void **) &wave);
+	N = cf_read_col(in_fits, TDOUBLE, "FLUX", (void **) &ref_flux);
+	N = cf_read_col(in_fits, TDOUBLE, "ERROR", (void **) &ref_error);
+	FITS_close_file(in_fits, &status);
+
+	/* Compute total flux of reference spectrum in region of interest. */
+	ref_tot = 0.;
+	for (i = 0; i < n_pix; i++) ref_tot += ref_flux[start+i];
+	
+	/*****************************************************************
+	** Compute the shift of each spectrum relative to the reference **
+	******************************************************************/
+	n_spec = 0;
+	rewind(pt_file);
+	
+	while (fscanf(pt_file, "%80s", spec_name) != EOF)
+	{
+		/* Do nothing if the current spectrum is the reference. */
+		if (n_spec++ == ind_ref_spec) {
+			fprintf(pt_file_out, "%s %3d %2d %5.0f %5ld %c%c%c 1.0\n",
+				ref_spec_name, 0, 0, exptime_max, ref_expnight,
+				ref_spec_name[8], ref_spec_name[9], ref_spec_name[10]);
+			continue;
+		}
+
+		/* Read the next spectrum */
+		FITS_open_file(&in_fits, spec_name, READONLY, &status);
+		FITS_read_key(in_fits, TFLOAT, "EXPTIME", &exptime, NULL, &status);
+		FITS_read_key(in_fits, TLONG, "EXPNIGHT", &expnight, NULL, &status);
+		FITS_movabs_hdu(in_fits, 2, &hdutype, &status);
+		if (hdutype != BINARY_TBL) cf_if_error("FITS files must contain BINARY TABLE in HDU #2");
+		N_tmp = cf_read_col(in_fits, TDOUBLE, "FLUX", (void **) &flux);
+		N_tmp = cf_read_col(in_fits, TDOUBLE, "ERROR", (void **) &error);
+		if (N_tmp != N) cf_if_error("Tables must have the same number of elements");
+		FITS_close_file(in_fits, &status);
+
+		/* If EXPTIME < 1, move on to the next data file. */
+		if (exptime < 1) {
+		    fprintf(pt_file_out, "%s %3d %2d %5.0f %5ld %c%c%c 0.0\n",
+			spec_name, 0, -1, exptime, expnight,
+			spec_name[8], spec_name[9], spec_name[10]);
+		    continue;
+		}
+
+		/* Compute total flux of data spectrum in region of interest. */
+		norm = 1.;
+		if (!ly_beta) {		/* Don't rescale if aligning on airglow. */
+		    total = 0.;
+		    for (i = 0; i < n_pix; i++) total += flux[start+i];
+		    norm = ref_tot / total;
+		}
+	
+        	/* Compute chi-squared for shifts between +/- MAXSHIFT pixels. */
+        	for (k = 0; k < N_SHIFT; k++) {
+		    nchi = 0;
+            	    sum = 0;
+            	    for (i = 0; i < n_pix; i++) {
+                	variance = ref_error[ref_start + i] * ref_error[ref_start + i] +
+                           norm * norm * error[start + i + k] * error[start + i + k];
+                        if (variance > 0) {
+                            sum += (ref_flux[ref_start + i] - norm * flux[start + i + k]) *
+                               (ref_flux[ref_start + i] - norm * flux[start + i + k]) / variance;
+                            nchi++;
+                        }
+                    }
+                    scale = (double) nchi / n_pix;
+                    chi_square[k] = sum / scale;
+                }
+
+		/* Compute min and max values of chi-squared. */
+        	ind_chi2_min = 0;
+        	chi_square_min = 1E5;
+        	chi_square_max = -1E5;
+        	for (k = 0; k < N_SHIFT; k++) {
+                	if (chi_square[k] < chi_square_min)
+                	{
+                        	chi_square_min = chi_square[k];
+                        	ind_chi2_min = k;
+                	}
+                	else if (chi_square[k] > chi_square_max)
+                        	chi_square_max = chi_square[k];
+        	}
+                shift = MAXSHIFT - ind_chi2_min;
+
+        	/* If chi-squared changes by less than 20% over range of shifts, bail out.
+        	 * Otherwise, return shift corresponding to lowest value of chi-square. */
+        	if (chi_square_max / chi_square_min < 1.2) 
+			sigma = -1;
+        	else 
+			sigma = 1;
+
+
+		/* If we're in HIST mode and sigma = -1 and NORM < 2,
+		 * then set shift = sigma = 0. */
+		if (!(strncasecmp(instmode, "HIST", 4)) && sigma == -1 && norm < 2.0) 
+			shift = sigma = 0;
+
+		/* printf ("shift = %d\tchi_square_max / chi_square_min = %g\n", 
+			ind_chi2_min - MAXSHIFT, chi_square_max / chi_square_min); */
+		
+		fprintf(pt_file_out, "%s %3d %2d %5.0f %5ld %c%c%c %f\n",
+			spec_name, shift, sigma, exptime, expnight,
+			spec_name[8], spec_name[9], spec_name[10], norm);
+
+		free(flux);
+		free(error);
+	}
+	
+	free(wave);
+	free(ref_flux);
+	free(ref_error);
+	
+	fclose(pt_file);
+	fclose(pt_file_out);
+
+	return(0);
+}
diff --git a/src/analysis/extract_jitter.c b/src/analysis/extract_jitter.c
new file mode 100644
index 0000000..a4ceb4d
--- /dev/null
+++ b/src/analysis/extract_jitter.c
@@ -0,0 +1,198 @@
+
+/*************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *************************************************************************
+ *
+ *
+ * Usage:
+ *     extract_jitter [-h] [-v level] input_file
+ *                                    
+ * 
+ *
+ * Arguments:
+ *   input_file     : jitter file                                                    
+ *
+ *
+ *
+ *
+ *
+ *
+ * Options:
+ *     -h:  this help message
+ *     -v:  verbosity level (=1; 0 is silent)
+ *          
+ *
+ *
+ *
+ * History:  	11/04/2004  v1.0 bjg    
+ *		06/03/2005  v1.1 wvd	Fix bug that set expstart=expend.
+ *					Delete unused variables.
+ *   
+ ***************************************************************************/
+
+
+#include <stdlib.h>
+#include <stdio.h>
+#include <string.h>
+#include <time.h>
+#include <unistd.h>
+#include <math.h>
+
+#include "calfuse.h"
+
+
+static char CF_PRGM_ID[]= "extract_jitter";
+static char CF_VER_NUM[]= "1.0";
+
+
+int main(int argc,char *argv[]){
+  
+ 
+  
+  char       input_filename[FLEN_CARD];
+  char       output_filename_x[FLEN_CARD]; 
+  char       output_filename_y[FLEN_CARD];
+  
+  FILE     * output_file_x;
+  FILE     * output_file_y;
+
+  fitsfile * infits;
+
+ 
+
+  int        intnull=0,anynull;
+  int        status=0;
+  int        hdutype=0;
+
+  long       i, N;
+  int        ncol;
+
+  double *   hdu2_time;
+  double *   hdu2_dx;
+  double *   hdu2_dy;
+  int    *   hdu2_trkflg;
+  
+ 
+
+  double mjd,dx,dy;
+
+  int trkflg;
+
+  double expstart, expend;
+
+  int optc;
+  
+  char opts[] = "hfv:";
+  char usage[] = 
+    "Usage:\n"
+    "  extract_jitter [-h] [-v level] input_file\n\n"
+    "Arguments:\n"
+    "  input_file     : jitter file (FITS)\n\n";
+  char option[] =
+    "Options:\n"
+    "  -h:  this help message                 \n"
+    "  -v:  verbosity level (=1; 0 is silent) \n";
+
+  verbose_level = 1;
+  
+  
+  /* Check number of options and arguments */
+  while ((optc = getopt(argc, argv, opts)) != -1) {
+    switch(optc) {    
+    case 'h':
+      printf("%s\n%s", usage, option);
+      return EXIT_SUCCESS;
+    case 'v':
+      verbose_level = atoi(optarg);
+      break;
+    }
+  }
+
+  /* Initialize error checking. */
+  cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+  if (argc != optind+1)
+    cf_if_error("%s\nIncorrect number of program arguments", usage);
+  
+  
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Started execution.");
+  
+  strcpy(input_filename,argv[optind]); 
+  
+
+
+  strcpy(output_filename_x,input_filename);
+  strcpy(output_filename_y,input_filename);
+  strcat(output_filename_x,".jtx");
+  strcat(output_filename_y,".jty");
+  
+
+  /* Create the output file */
+  output_file_x = fopen(output_filename_x,"w");
+  output_file_y = fopen(output_filename_y,"w");
+  
+
+
+  FITS_open_file(&infits,input_filename,READONLY,&status);
+
+  FITS_read_key(infits,TDOUBLE,"EXPSTART",&expstart,NULL,&status);
+  FITS_read_key(infits,TDOUBLE,"EXPEND",&expend,NULL,&status);
+
+  FITS_movabs_hdu(infits,2,&hdutype,&status);
+
+  FITS_read_key(infits,TLONG,"NAXIS2",&N,NULL,&status);
+ 
+  hdu2_time=(double *)malloc(N*sizeof(double));
+  hdu2_dx=(double *)malloc(N*sizeof(double));
+  hdu2_dy=(double *)malloc(N*sizeof(double));
+  hdu2_trkflg=(int *)malloc(N*sizeof(int));
+ 
+  FITS_get_colnum(infits, TRUE, "TIME", &ncol, &status);
+  FITS_read_col(infits, TDOUBLE, ncol, 1, 1, N, &intnull,
+		hdu2_time, &anynull, &status);
+ 
+  FITS_get_colnum(infits, TRUE, "DX", &ncol, &status);
+  FITS_read_col(infits, TDOUBLE, ncol, 1, 1, N, &intnull,
+		hdu2_dx, &anynull, &status);
+
+  FITS_get_colnum(infits, TRUE, "DY", &ncol, &status);
+  FITS_read_col(infits, TDOUBLE, ncol, 1, 1, N, &intnull,
+		hdu2_dy, &anynull, &status);
+  
+  FITS_get_colnum(infits, TRUE, "TRKFLG", &ncol, &status);
+  FITS_read_col(infits, TINT, ncol, 1, 1, N, &intnull,
+		hdu2_trkflg, &anynull, &status);
+  
+
+  for (i=0;i<N-100;i++){
+    mjd=expstart+(hdu2_time[i])/(3600.0*24.0);
+    dx=hdu2_dx[i];
+    dy=hdu2_dy[i];
+    trkflg=hdu2_trkflg[i];
+
+    if ((mjd>=expstart) && (mjd<=expend) && (trkflg==5)){
+      fprintf(output_file_x,"%15lf %15lf\n",mjd,dx);
+      fprintf(output_file_y,"%15lf %15lf\n",mjd,dy);
+    }
+  }
+
+
+    
+  free(hdu2_time);
+  free(hdu2_dx);
+  free(hdu2_dy);
+  free(hdu2_trkflg);
+ 
+
+       
+  FITS_close_file(infits,&status);
+ 
+  fclose(output_file_x);
+  fclose(output_file_y);
+
+
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished execution.");
+  return EXIT_SUCCESS;
+  
+}
diff --git a/src/analysis/get_shift.c b/src/analysis/get_shift.c
new file mode 100644
index 0000000..a4c2b70
--- /dev/null
+++ b/src/analysis/get_shift.c
@@ -0,0 +1,164 @@
+/*****************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *****************************************************************************
+ *
+ * Synopsis:	getshift spec1 spec2 w1 w2
+ *
+ * Description:  Computes the wavelength shift between the spectra from two
+ *               different exposures spec1 and spec2 using a cross-correlation
+ *               in the wavelength window defined by w1 and w2  
+ *
+ *
+ * History:   01/08/04  bjg  1.0  begin work 
+ *            04/05/04  bjg  1.1  Return EXIT_SUCCESS
+ *                                Correct formats to match
+ *                                argument types in printf
+ *            08/26/05  wvd  1.2  If given no arguments, don't return error.
+ *				  Just print message and exit.
+ *
+ ****************************************************************************/
+
+#include <time.h>
+#include <math.h>
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include "calfuse.h"
+
+
+#define MAXSHIFT 25
+#define SMOOTH_PAR 4
+
+
+static char CF_PRGM_ID[] = "get_shift";
+static char CF_VER_NUM[] = "1.2";
+
+
+int wave_search(float *table, int i, int j, float elmt){
+
+  int k;
+  
+  if (i>=j) return i;
+  if (elmt==table[i]) return i;
+  if (elmt==table[j]) return j;
+  k=(i+j)/2;
+  if (elmt==table[k]) return k;
+  if ((elmt-table[i])*(elmt-table[k])<0) return wave_search(table,i,k,elmt);
+  return wave_search(table,k+1,j,elmt);
+}
+
+int main(int argc, char *argv[])
+{
+   
+  int      status=0;
+  int      hdutype=0;
+
+  long n,n1,n2,laux,i,j,k;
+  
+  float *wave, *flux1, *flux2, *flux1s, *flux2s;
+  
+  float w1,w2;
+  
+  fitsfile *infits1, *infits2;
+  
+  float correl[2*MAXSHIFT+1];
+  
+  
+  /* Enter a timestamp into the log. */
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+  /* Initialize error checking */
+  cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+  
+  
+  /* check command line */
+  if (argc != 5) {
+    printf("Usage: getshift spec1 spec2 w1 w2 \n");
+    return 1;
+  }
+  
+  
+  FITS_open_file(&infits1, argv[1], READONLY, &status);
+  FITS_open_file(&infits2, argv[2], READONLY, &status);
+  
+  sscanf(argv[3],"%f",&w1);
+  sscanf(argv[4],"%f",&w2);
+  
+	
+  FITS_movabs_hdu(infits1, 2, &hdutype, &status);
+  FITS_movabs_hdu(infits2, 2, &hdutype, &status);
+  
+
+  n=cf_read_col(infits1,TFLOAT,"WAVE",(void **) &wave);
+  n=cf_read_col(infits1,TFLOAT,"FLUX",(void **) &flux1);
+  n=cf_read_col(infits2,TFLOAT,"FLUX",(void **) &flux2);
+  
+  
+  flux1s=(float*)malloc(n*sizeof(float));
+  flux2s=(float*)malloc(n*sizeof(float));
+  
+  
+  for (i=0;i<n;i++){
+        flux1s[i]=0;
+        flux2s[i]=0;
+        k=0;
+  	for (j=i-SMOOTH_PAR;j<=i+SMOOTH_PAR;j++){
+  		if ((j>=0)&&(j<n)) {
+  			flux1s[i]+=flux1[j];
+                        flux2s[i]+=flux2[j];
+                        k=k+1;
+  		}
+  	}
+  	flux1s[i]/=k;
+  	flux2s[i]/=k;
+  	
+  	
+  }
+  
+ 
+
+  if ((w1-wave[0])*(w1-wave[n-1])>0) 
+    cf_if_error("Wavelength parameters out of range\n");  
+
+  if ((w2-wave[0])*(w2-wave[n-1])>0) 
+    cf_if_error("Wavelength parameters out of range\n");
+  
+  n1=wave_search(wave,0,n-1,w1);
+  n2=wave_search(wave,0,n-1,w2);
+  
+  
+  if (n1>n2) {
+    laux=n2;
+    n2=n1;
+    n1=laux;
+  }
+  
+  if ((n1-MAXSHIFT<0)||(n2+MAXSHIFT>=n)) 
+    cf_if_error("Wavelength parameters too close to bounds\n");
+  
+  k=0;
+  
+  for (i=0;i<=2*MAXSHIFT;i++){
+    correl[i]=0;
+    for (j=n1;j<=n2;j++){
+      correl[i]=correl[i]+flux1s[j]*flux2s[j+i-MAXSHIFT];
+    }
+    if (correl[i]>correl[k]) k=i;    
+  }
+  
+  
+  
+  FITS_close_file(infits1, &status);
+  FITS_close_file(infits2, &status);
+
+  /* Enter a timestamp into the log. */
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+
+  printf("Shift is %ld steps.\n",k-MAXSHIFT);
+  
+  return EXIT_SUCCESS;
+ 
+
+}
diff --git a/src/analysis/gethmjd.c b/src/analysis/gethmjd.c
new file mode 100644
index 0000000..dcb3cdb
--- /dev/null
+++ b/src/analysis/gethmjd.c
@@ -0,0 +1,98 @@
+
+/*****************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *****************************************************************************
+ *
+ * 
+ * From Modified Julian Day and RA,DEC of target, 
+ * computes Heliocentic Modified Julian Day 
+ *
+ * Uses slalib to compute the light time delay along the target direction.
+ *
+ *
+ * History:	10/06/04	bjg           
+ *
+ ****************************************************************************/
+
+
+
+#include <stdlib.h>
+#include <stdio.h>
+#include <string.h>
+#include <time.h>
+#include <unistd.h>
+#include <math.h>
+
+#ifdef CFORTRAN
+#include "cfortran.h"
+
+PROTOCCALLSFSUB6(SLA_DJCL, sla_djcl, DOUBLE, PINT, PINT, PINT, PDOUBLE, \
+                 PINT)
+#define slaDjcl(DJM, IY, IM, ID, FD, J) \
+     CCALLSFSUB6(SLA_DJCL, sla_djcl, DOUBLE, PINT, PINT, PINT, PDOUBLE, \
+                 PINT, DJM, IY, IM, ID, FD, J)
+
+
+PROTOCCALLSFSUB6(SLA_CALYD, sla_calyd, INT, INT, INT, PINT, PINT, \
+                 PINT)
+#define slaCalyd(IY, IM, ID, NY, ND, J) \
+     CCALLSFSUB6(SLA_CALYD, sla_calyd, INT, INT, INT, PINT, PINT, \
+                 PINT, IY, IM, ID, NY, ND, J)
+
+PROTOCCALLSFSUB7(SLA_ECOR, sla_ecor, FLOAT, FLOAT, INT, INT, FLOAT, PFLOAT, \
+                 PFLOAT)
+#define slaEcor(RM, DM, IY, ID, FD, RV, TL) \
+     CCALLSFSUB7(SLA_ECOR, sla_ecor,  FLOAT, FLOAT, INT, INT, FLOAT, PFLOAT, \
+                 PFLOAT, RM, DM, IY, ID, FD, RV, TL)
+
+#else
+#include "slalib.h"
+#include "slamac.h"
+#endif
+
+
+#include "calfuse.h"
+
+
+#define DEG2RAD (M_PI/180.0f)
+
+double gethmjd(double mjd, int ra_h, int ra_m, float ra_s, int dec_d, int dec_m, float dec_s){
+
+
+  int status;
+
+  int year, month, day;
+  int jyear, jday; 
+  double frac;
+  
+  
+  float ra, dec;
+  float lt, v;
+    
+  ra  = ( ra_h  +  ra_m/60.0 +  ra_s/3600.0 ) * 15.0 * DEG2RAD;
+  dec = ( dec_d + dec_m/60.0 + dec_s/3600.0 ) * DEG2RAD;
+
+  
+#ifdef CFORTRAN
+  slaDjcl(mjd, year, month, day, frac, status);
+#else
+  slaDjcl(mjd, &year, &month, &day, &frac, &status);
+#endif  
+  
+#ifdef CFORTRAN
+  slaCalyd(year, month, day, jyear, jday, status);
+#else
+  slaCalyd(year, month, day, &jyear, &jday, &status);
+#endif
+
+#ifdef CFORTRAN
+  slaEcor(ra, dec, jyear, jday, (float) frac, v, lt);
+#else
+  slaEcor(ra, dec, jyear, jday, (float) frac, &v, &lt);
+#endif
+
+  return (double) (mjd+lt/(3600.0*24.0));
+
+}
diff --git a/src/analysis/idf_combine.c b/src/analysis/idf_combine.c
new file mode 100644
index 0000000..3f1a678
--- /dev/null
+++ b/src/analysis/idf_combine.c
@@ -0,0 +1,945 @@
+
+/*****************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *****************************************************************************
+ *
+ * Synopsis:	idf_combine outfile file1 file2 file3 file4 file5 ...
+ *
+ * Description: Reads multiple contiguous idf files and concatenates them 
+ *              into a single file.
+ *
+ * History:	08/11/03    bjg		Begin work from ttag_combine.c
+ *                                      sort the input files in time order
+ *              08/12/03    bjg	 v1.0	First usable version
+ *              08/13/03    bjg		Some minor changes
+ *              08/14/03    bjg		Fixed some important keywords  
+ *					in the main HDU
+ *		08/20/03    bjg	 v1.1	Changed the way the binary tables
+ *					are read, created and written
+ *					(same as cf_ttag_init)
+ *              09/09/03    bjg  v1.2   Fixed some keywords
+ *              10/29/03    bjg         Changed the scaling format for
+ *                                      output timeline to conform the 
+ *                                      new IDF formatting.
+ *              11/17/03    bjg  v1.3   Now warns users if the Focal
+ *                                      Plane Assembly has moved between 
+ *                                      exposures.
+ *              11/22/03    bjg         Now prints the name of the
+ *                                      included files in the main  
+ *                                      header.
+ *              12/10/03    bjg         Updated NSPEC keyword and 
+ *					SPECxxx, WOFFLxxx, WOFFSxxx keywords
+ *					Removed path in filenames written
+ *					into header.
+ *              02/25/04    bjg         Bug fix 
+ *              03/25/04    bjg         Added TZERO and TSCALE values for 
+ *                                      AIC and FEC countrates
+ *              04/05/04    bjg         Remove unused variables
+ *                                      Change formats to match arg types
+ *                                      in printf
+ *                                      Remove static keyword in struct key 
+ *                                      definition
+ *                                      Add braces in TSCAL and TZERO
+ *                                      definitions
+ *              06/08/04    bjg         Changes to handle EXP_STAT keyword
+ *              08/13/04    bjg  v1.4   Recalculates Y centroid on demand
+ *              10/06/04    bjg  v1.5   Added option -b to store 
+ *                                      ORBITAL_VEL in a float 
+ *              10/26/04    bjg  v1.6   Cosmetic change 
+ *              01/28/2005  bjg  v1.7   Fixed crash within CFITSIO with
+ *                                      with IDF files having empty tables
+ *              02/16/2005  wvd  v1.8   Double TSCALE and TZERO 
+ *                                      for the AIC_CNT_RATE array.
+ *              03/22/2005  wvd  v1.9	Read and write TIME_SUNRISE
+ *                                      and TIME_SUNSET as shorts.
+ *              04/15/2005  tc   v1.10  Update PLANTIME keyword
+ *              06/08/2005  tc   v1.11  Comment out warning if FPA has
+ *					shifted.  Pipeline corrects for this.
+ *              09/19/2005  wvd  v1.12  Don't even read FPA positions.
+ *              05/22/2006  wvd  v1.13  Change most header keyword
+ *					types from float to long.
+ *              06/22/2006  wvd  v1.14  Add -z flag to force creation of
+ *					an output file, even if empty.
+ *              11/10/2006  wvd  v1.15  Add comment fields to WOFFS and
+ *					WOFFL keywords.
+ *              08/27/2007  bot  v1.16  Changed long for int l.138
+ *		07/25/2008  wvd  v1.17  Set output EXP_STAT keyword to lowest
+ *					non-negative value among input files.
+ *              08/22/2008  wvd  v1.18  If -a flag is set, include files with
+ *					positive values of EXP_STAT, but not
+ *					those with negative values.
+ *                                               
+ ****************************************************************************/
+
+
+#include <unistd.h>
+#include <stdlib.h>
+#include <stdio.h>
+#include <string.h>
+#include <time.h>
+#include "calfuse.h"
+
+typedef char filename[FLEN_CARD];
+
+struct key {
+  char keyword[FLEN_KEYWORD];
+  float value;
+};
+
+static char CF_PRGM_ID[]= "idf_combine";
+static char CF_VER_NUM[]= "1.18";
+
+int main(int argc,char *argv[]){
+
+  char     date[FLEN_CARD]={'\0'};      
+  char     rootname[FLEN_CARD];
+  char     comment[FLEN_COMMENT];
+
+  int      felem_hdu2,felem_hdu4,frow_hdu3;
+
+  char     stime[FLEN_CARD],keyword[FLEN_CARD],card[FLEN_CARD];
+
+  char     fmt_byte[FLEN_CARD],fmt_float[FLEN_CARD],fmt_short[FLEN_CARD]; 
+
+  char *corrected_filename;
+  char *string_pointer;
+  char string0[100], string1[100];
+
+  time_t   vtime;
+
+  fitsfile *infits,*outfits;
+	
+  filename *filelist;
+  double   *expstartlist;
+  double   *expendlist;
+  long     *neventslist;
+  long     *nrecordslist;
+  long     *ngtislist;
+  
+  double   delta_t;
+  
+  float    zero=0.0;
+  
+  filename tempstring;
+  double   tempdouble;
+  long     templong;
+  float    tempfloat;
+  char     tempchar;
+  
+  double   minexpstart;
+  int      minindex;
+  
+  int      nfiles;
+
+  int      intnull=0,anynull;
+  int      ncol;
+  
+  int      status=0;
+  int      hdutype=0;
+  int      tref = 0;
+
+  int n2;
+
+  int exp_stat, exp_stat_out=99;
+
+  long     nevents=0, nrecords=0, ngtis=0;
+  long     n_real_events=0;
+  
+  long     i,j;
+  
+  float   *floatlist;
+  short   *shortlist;
+  char    *charlist;
+  double  *doublelist;
+  
+  float    exptime=0, rawtime=0;
+  long     neventscreened=0, neventscreenedpha=0, plantime=0, timehv=0;
+  long     timescreened=0, timesaa=0, timelowlimbangle=0, timeburst=0,
+		timejitter=0,timenight=0;
+
+  /* float    fpasx0, fpasx, fpalx0, fpalx, dfpasx, dfpalx ; */
+  /* int      fpa_split = FALSE; */
+
+  int  hdu2_tfields=14;
+  
+  char hdu2_extname[]="TTAG DATA";   /* Name of this extension */
+  
+  char *hdu2_ttype[]={"TIME", "XRAW", "YRAW", "PHA", "WEIGHT", "XFARF", 
+		      "YFARF",  "X", "Y", "CHANNEL", "TIMEFLGS",
+		      "LOC_FLGS", "LAMBDA", "ERGCM2" };
+
+  char *hdu2_tform[14];  /* We'll assign values when we know 
+			    the number of elements in the data set. */
+
+
+  char *hdu2_tunit[]={"SECONDS", "PIXELS", "PIXELS", "UNITLESS", "UNITLESS",
+		      "PIXELS", "PIXELS", "PIXELS", "PIXELS", "UNITLESS",
+		      "UNITLESS", "UNITLESS", "ANGSTROMS", "ERG CM^-2"};
+
+  struct key hdu2_tscal[] = {{"TSCAL6", 0.25},  {"TSCAL7", 0.1}, 
+			     {"TSCAL8", 0.25},  {"TSCAL9", 0.1}};
+	
+  struct key hdu2_tzero[] = {{"TZERO6", 8192.}, {"TZERO7", 0.}, 
+			     {"TZERO8", 8192.}, {"TZERO9", 0.}};
+  
+  
+
+
+  int  hdu3_tfields=2;
+	
+  char hdu3_extname[]="GTI";   /* Name of this extension */
+  
+  char *hdu3_ttype[]={"START", "STOP" };
+  
+  char *hdu3_tform[2]={"1D", "1D" };  /* We'll assign values when we know 
+					 the number of elements in the data set. */
+
+
+  char *hdu3_tunit[]={"seconds", "seconds"};
+
+  struct key hdu4_tscal[16];
+  struct key hdu4_tzero[16];
+  
+  char hdu4_extname[]="TIMELINE";
+  int hdu4_tfields=16;  /* output table will have 16 columns */
+  char *hdu4_ttype[]={"TIME", "STATUS_FLAGS", "TIME_SUNRISE", "TIME_SUNSET",
+		      "LIMB_ANGLE", "LONGITUDE", "LATITUDE", "ORBITAL_VEL",
+		      "HIGH_VOLTAGE", "LIF_CNT_RATE", "SIC_CNT_RATE",
+		      "FEC_CNT_RATE", "AIC_CNT_RATE", "BKGD_CNT_RATE",
+		      "YCENT_LIF","YCENT_SIC"};
+
+  char *hdu4_tform[16]; /* we will define tform later, when the number
+			   of photons is known */
+  
+  char *hdu4_tunit[]={"seconds", "unitless", "seconds", "seconds", "degrees",
+		      "degrees", "degrees",  "km/s", "unitless", "counts/sec",
+		      "counts/sec", "counts/sec", "counts/sec", "counts/sec",
+		      "pixels","pixels" };
+
+
+  int ignore_exp_stat=0;
+  int do_ycent=0;
+  int big_vel=0;
+  int do_empty=FALSE, empty_output=FALSE;
+
+  float    *x=NULL, *y=NULL, *weight=NULL;
+  unsigned char *channel=NULL, *timeflags=NULL, *locflags=NULL;
+
+  int optc;
+
+  char opts[] = "hacbv:z";
+  char usage[] = 
+    "Usage:\n"
+    "  idf_combine [-ahbcz]  [-v level] output_idf_file input_idf_files\n";
+  char option[] =
+    "Options:\n"
+    "  -h:  this help message\n"
+    "  -v:  verbosity level (=1; 0 is silent)\n"
+    "  -a:  ignore EXP_STAT keyword \n"
+    "  -c:  recalculates Y centroids (use target events) \n"
+    "  -b:  store ORBITAL_VEL in a float \n"
+    "  -z:  if no good data, generate empty output file\n";
+
+  verbose_level = 1;
+
+  /* Check number of options and arguments */
+  while ((optc = getopt(argc, argv, opts)) != -1) {
+    switch(optc) {
+      
+    case 'h':
+      printf("%s\n%s", usage, option);
+      return 0;
+    case 'a':
+      ignore_exp_stat=1;
+      break;
+    case 'v':
+      verbose_level = atoi(optarg);
+      break;
+    case 'c':
+      do_ycent=1;
+      break; 
+    case 'b':
+      big_vel=1;
+      break;
+    case 'z':
+      do_empty=TRUE;
+      break;
+    }
+  }
+
+  cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+  if (argc < optind+2) {
+    printf("%s", usage);
+    return 1;
+  }
+   
+    
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Started execution.");
+  
+  /* get and display time */
+  vtime = time(NULL) ;
+  strcpy(stime,ctime(&vtime));
+  
+      
+  nfiles=argc-optind-1;
+  
+  filelist     = (filename *)cf_calloc(nfiles, sizeof(filename));
+  expstartlist = (double *)cf_calloc(nfiles, sizeof(double));
+  expendlist   = (double *)cf_calloc(nfiles, sizeof(double));
+  neventslist  = (long *)cf_calloc(nfiles, sizeof(long));
+  nrecordslist = (long *)cf_calloc(nfiles, sizeof(long));
+  ngtislist    = (long *)cf_calloc(nfiles, sizeof(long));
+  
+  if (!ignore_exp_stat)
+    cf_verbose(1,"Will include only files with EXP_STAT=0") ;
+  else
+    cf_verbose(1,"Will include only files with EXP_STAT >= 0") ;
+
+  cf_verbose(1,"GETTING INFORMATION ON INPUT FILES") ;
+
+  n2=0;
+
+  for (i=0; i<nfiles;i++) {
+    
+    FITS_open_file(&infits,argv[optind+i+1],READONLY,&status);
+
+    FITS_read_key(infits,TINT,"EXP_STAT",&exp_stat,NULL,&status);
+
+    strcpy(filelist[n2],argv[optind+i+1]);
+    FITS_read_key(infits,TDOUBLE,"EXPSTART",&(expstartlist[n2]),NULL,&status);
+    FITS_read_key(infits,TDOUBLE,"EXPEND",&(expendlist[n2]),NULL,&status);
+    
+    /* Set EXP_STAT to lowest non-negative value in input files. */
+    if (exp_stat_out > exp_stat && exp_stat >= 0) exp_stat_out = exp_stat;
+
+    /* Skip files with bad values of EXP_STAT. */
+    if (!ignore_exp_stat && exp_stat != 0) {
+	cf_if_warning("File %s rejected. EXP_STAT not equal to zero. Use -a flag to override.",
+		argv[optind+i+1]) ;
+	FITS_close_file(infits,&status);
+	continue;
+    }
+    /* Never include files with negative values of EXP_STAT. */
+    else if (exp_stat < 0) {
+	cf_if_warning("File %s rejected. EXP_STAT less than zero.", argv[optind+i+1]) ;
+	FITS_close_file(infits,&status);
+	continue;
+    }
+
+    FITS_read_key(infits,TFLOAT,"EXPTIME",&(tempfloat),NULL,&status);
+    exptime+=tempfloat;
+    FITS_read_key(infits,TLONG,"NEVENTS",&templong,NULL,&status);
+    n_real_events+=templong;
+    FITS_read_key(infits,TFLOAT,"RAWTIME",&(tempfloat),NULL,&status);
+    rawtime+=tempfloat;
+    FITS_read_key(infits,TLONG,"PLANTIME",&(templong),NULL,&status);
+    plantime+=tempfloat;
+		
+    FITS_read_key(infits,TLONG,"NBADEVNT",&templong,NULL,&status);
+    neventscreened+=templong;
+    FITS_read_key(infits,TLONG,"NBADPHA",&templong,NULL,&status);
+    neventscreenedpha+=templong;
+    
+    FITS_read_key(infits,TLONG,"EXP_BAD",&templong,NULL,&status);
+    timescreened+=templong;
+    FITS_read_key(infits,TLONG,"EXP_BRST",&templong,NULL,&status);
+    timeburst+=templong;
+    FITS_read_key(infits,TLONG,"EXP_HV",&templong,NULL,&status);
+    timehv+=templong;
+    FITS_read_key(infits,TLONG,"EXP_JITR",&templong,NULL,&status);
+    timejitter+=templong;
+    FITS_read_key(infits,TLONG,"EXP_LIM",&templong,NULL,&status);
+    timelowlimbangle+=templong;
+    FITS_read_key(infits,TLONG,"EXP_SAA",&templong,NULL,&status);
+    timesaa+=templong;
+    FITS_read_key(infits,TLONG,"EXPNIGHT",&templong,NULL,&status);
+    timenight+=templong;
+    
+    FITS_movabs_hdu(infits,2,&hdutype,&status);
+    FITS_read_key(infits,TSTRING,"TFORM1",&tempstring,NULL,&status);
+    sscanf(tempstring,"%ld%c",&neventslist[n2],&tempchar);
+    nevents+=neventslist[n2];
+    
+    FITS_movabs_hdu(infits,3,&hdutype,&status);
+    FITS_read_key(infits,TLONG,"NAXIS2",&(ngtislist[n2]),NULL,&status);
+    ngtis+=ngtislist[n2];
+    
+    FITS_movabs_hdu(infits,4,&hdutype,&status);
+    FITS_read_key(infits,TSTRING,"TFORM1",&tempstring,NULL,&status);
+    sscanf(tempstring,"%ld%c",&nrecordslist[n2],&tempchar);
+    nrecords+=nrecordslist[n2];
+    
+    FITS_close_file(infits,&status);
+		
+    n2++;
+  }
+
+  nfiles=n2;
+
+  if (nfiles==0){
+    if (do_empty) {
+	cf_verbose(1,"No files to combine. Generating empty output file.");
+	do_ycent = FALSE;
+	empty_output = TRUE;
+	expendlist[0]=expstartlist[0];
+	nfiles = 1;
+    }
+    else {
+	cf_verbose(1,"No files to combine. Exiting.");
+	cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished execution.");
+	exit(0);
+    }
+  }
+  
+  cf_verbose(1,"SORTING INPUT FILES IN TIME ORDER") ;
+  
+  for (i=0; i<nfiles-1;i++) {
+    minexpstart=expstartlist[i];
+    minindex=i;
+    for (j=i+1; j<nfiles;j++) {
+      if (expstartlist[j]<minexpstart){
+	minexpstart=expstartlist[j];
+	minindex=j;
+      }
+    }
+    
+    strcpy(tempstring,filelist[minindex]);
+    strcpy(filelist[minindex],filelist[i]);
+    strcpy(filelist[i],tempstring);
+    
+    tempdouble=expstartlist[minindex];
+    expstartlist[minindex]=expstartlist[i];
+    expstartlist[i]=tempdouble;
+    
+    tempdouble=expendlist[minindex];
+    expendlist[minindex]=expendlist[i];
+    expendlist[i]=tempdouble;
+    
+    templong=neventslist[minindex];
+    neventslist[minindex]=neventslist[i];
+    neventslist[i]=templong;
+		
+    templong=nrecordslist[minindex];
+    nrecordslist[minindex]=nrecordslist[i];
+    nrecordslist[i]=templong;
+    
+    templong=ngtislist[minindex];
+    ngtislist[minindex]=ngtislist[i];
+    ngtislist[i]=templong;
+  }
+
+  cf_verbose(2,
+	"N: Filename                  ExpStart ExpEnd  NEvents NGTIs NSeconds");
+
+  for (i=0; i<nfiles;i++) {
+    cf_verbose(2,"%ld: %s %7.1f  %7.1f %4ld  %2ld    %5ld",i,filelist[i],
+	expstartlist[i],expendlist[i],neventslist[i],ngtislist[i],
+	nrecordslist[i]);
+    
+  }
+  
+  cf_verbose(1,"CREATING OUTPUT FILE");
+  
+  FITS_open_file(&infits,filelist[0],READONLY,&status);
+  FITS_create_file(&outfits,argv[optind],&status);
+	
+	
+  cf_verbose(1,"WRITING MAIN HEADER");
+  
+  FITS_copy_hdu(infits,outfits,0,&status);
+	
+  FITS_read_key(infits,TSTRING,"ROOTNAME",rootname,NULL,&status);
+  	
+  rootname[8]='9';
+  rootname[9]='9';
+  rootname[10]='9';
+  	
+  FITS_update_key(outfits,TSTRING,"ROOTNAME",rootname,NULL,&status);
+
+  string_pointer=strrchr(argv[optind],'/');
+  if (string_pointer==NULL) corrected_filename=argv[optind];
+  else corrected_filename=&(string_pointer[1]); 
+  
+  FITS_update_key(outfits,TINT,"EXP_STAT",&exp_stat_out,NULL,&status);
+
+  FITS_update_key(outfits,TSTRING,"FILENAME",corrected_filename,NULL,&status);
+	
+  FITS_update_key(outfits,TSTRING,"EXP_ID","999",NULL,&status);
+	
+  fits_get_system_time(date, &tref, &status);
+	
+  FITS_update_key(outfits,TSTRING,"DATE",date,NULL,&status);
+  	
+  FITS_update_key(outfits,TDOUBLE,"EXPEND",&expendlist[nfiles-1],NULL,&status);	
+  FITS_update_key(outfits,TFLOAT,"EXPTIME",&exptime,NULL,&status);
+  FITS_update_key(outfits,TLONG,"NEVENTS",&n_real_events,NULL,&status);	
+  FITS_update_key(outfits,TFLOAT,"RAWTIME",&rawtime,NULL,&status);
+  FITS_update_key(outfits,TLONG,"PLANTIME",&plantime,NULL,&status);
+  FITS_update_key(outfits,TLONG,"NBADEVNT",&neventscreened,NULL,&status);
+  FITS_update_key(outfits,TLONG,"NBADPHA",&neventscreenedpha,NULL,&status);
+  FITS_update_key(outfits,TLONG,"EXP_BAD",&(timescreened),NULL,&status);
+  FITS_update_key(outfits,TLONG,"EXP_BRST",&(timeburst),NULL,&status);		
+  FITS_update_key(outfits,TLONG,"EXP_HV",&(timehv),NULL,&status);
+  FITS_update_key(outfits,TLONG,"EXP_JITR",&(timejitter),NULL,&status);
+  FITS_update_key(outfits,TLONG,"EXP_LIM",&(timelowlimbangle),NULL,&status);
+  FITS_update_key(outfits,TLONG,"EXP_SAA",&(timesaa),NULL,&status);
+  FITS_update_key(outfits,TLONG,"EXPNIGHT",&(timenight),NULL,&status);
+  
+  if (do_ycent)   {
+    strcpy(string0,"PERFORM");
+    FITS_update_key(outfits, TSTRING, "YCNT_COR", string0, NULL, &status);
+
+    for (i = 1; i < 8; i++) {
+      if (i == 4) continue;
+      sprintf(string1, "YQUAL%1ld", i);
+      strcpy(string0,"HIGH");
+      FITS_update_key(outfits, TSTRING, string1, string0, NULL, &status);
+    }
+  } 
+
+  /* reset BPM_CAL */
+  fits_read_key(outfits,TSTRING,"BPM_CAL",string0,NULL,&status);
+  if (status!=0) {
+    status = 0;
+  }
+  else {
+    strcpy(string0,"");
+    FITS_update_key(outfits,TSTRING,"BPM_CAL",string0,NULL,&status);
+  }
+
+
+  if (empty_output) {
+     fits_write_history(outfits,"FILE CONTAINS NO DATA.",&status);
+	n2=0;
+     FITS_update_key(outfits,TINT,"NSPEC",&n2,NULL,&status);
+  }
+  else
+     FITS_update_key(outfits,TINT,"NSPEC",&nfiles,NULL,&status);
+  
+  fits_write_history(outfits," COMBINED WITH IDF_COMBINE ",&status);
+    
+  for (i=0;i<nfiles;i++){
+
+    string_pointer=strrchr(filelist[i],'/');
+    if (string_pointer==NULL) corrected_filename=filelist[i];
+    else corrected_filename=&(string_pointer[1]);  
+
+
+    sprintf(keyword, "SPEC%.3ld", i+1);
+    FITS_update_key(outfits,TSTRING,keyword,corrected_filename,NULL,&status);
+    sprintf(keyword, "WOFFL%.3ld", i+1);
+    sprintf(comment, "[Angstroms] Shift applied to LiF spectrum");
+    FITS_update_key(outfits,TFLOAT,keyword,&zero,comment,&status);
+    sprintf(keyword, "WOFFS%.3ld", i+1);
+    sprintf(comment, "[Angstroms] Shift applied to SiC spectrum");
+    FITS_update_key(outfits,TFLOAT,keyword,&zero,comment,&status);
+  }
+  
+  FITS_close_file(infits,&status);
+  
+  cf_verbose(1,"PREPARING EVENTS LIST HDU");
+  
+  /* Generate the tform array */
+  sprintf(fmt_byte,  "%ldB", nevents);
+  sprintf(fmt_float, "%ldE", nevents);
+  sprintf(fmt_short, "%ldI", nevents);
+  
+  hdu2_tform[0] = fmt_float;
+  hdu2_tform[1] = fmt_short;
+  hdu2_tform[2] = fmt_short;
+  hdu2_tform[3] = fmt_byte;
+  hdu2_tform[4] = fmt_float;
+  for (i=5; i<9; i++)
+    hdu2_tform[i] = fmt_short;
+  for ( ; i<12; i++)
+    hdu2_tform[i] = fmt_byte;
+  hdu2_tform[12] = fmt_float;
+  hdu2_tform[13] = fmt_float;
+  
+
+  /* Append a new empty binary table to the output file */
+  FITS_create_tbl(outfits, BINARY_TBL, 1, hdu2_tfields, hdu2_ttype, hdu2_tform,
+		  hdu2_tunit, hdu2_extname, &status);
+  
+  /* Write TSCALE and TZERO entries to header */
+  for (i=0; i<4; i++) {
+    sprintf(keyword, "TUNIT%ld", i+6);
+    if (fits_read_keyword(outfits, keyword, card, NULL, &status))
+      cf_if_fits_error(status);
+    FITS_insert_key_flt(outfits, hdu2_tscal[i].keyword, hdu2_tscal[i].value,
+			-2, NULL, &status);
+    FITS_insert_key_flt(outfits, hdu2_tzero[i].keyword, hdu2_tzero[i].value,
+			-4, NULL, &status);
+  } 
+  
+  
+  
+  cf_verbose(1,"PREPARING GTIs LIST HDU");
+  
+  /* Append a new empty binary table to the output file */
+  FITS_create_tbl(outfits, BINARY_TBL, ngtis, hdu3_tfields, hdu3_ttype, hdu3_tform,
+		  hdu3_tunit, hdu3_extname, &status);
+			
+			
+  cf_verbose(1,"PREPARING TIMELINE HDU");	
+		
+  /* Generate the tform array */
+  sprintf(fmt_byte,  "%ldB", nrecords);
+  sprintf(fmt_float, "%ldE", nrecords);
+  sprintf(fmt_short, "%ldI", nrecords);
+  
+
+  
+  hdu4_tform[0] = fmt_float;
+  hdu4_tform[1] = fmt_byte;
+
+  for (i=2; i<hdu4_tfields; i++) hdu4_tform[i] = fmt_short;
+  
+  /* Set TSCALE and TZERO values */
+  /* Not all of these will be used; see below. */
+  for (i=2; i<hdu4_tfields; i++) {
+    sprintf(hdu4_tscal[i].keyword, "TSCAL%ld", i+1);
+    hdu4_tscal[i].value = 0.1;
+    sprintf(hdu4_tzero[i].keyword, "TZERO%ld", i+1);
+    hdu4_tzero[i].value = 0.;
+  }
+  
+  /* Let's keep three significant figures for vorb. */
+  hdu4_tscal[7].value = 0.01;
+
+    /* FEC_CNT_RATE and AIC_CNT_RATE can get big, so we
+        use TZERO AND TSCALE to compress them. */
+    hdu4_tscal[11].value = 1;                
+    hdu4_tscal[12].value = 2;              
+    hdu4_tzero[11].value = 32768;          
+    hdu4_tzero[12].value = 65536;
+  
+  if (big_vel) hdu4_tform[7]=fmt_float; 
+	
+  /* Append a new empty binary table to the output file */
+  FITS_create_tbl(outfits, BINARY_TBL, 1, hdu4_tfields, hdu4_ttype, hdu4_tform,
+		  hdu4_tunit, hdu4_extname, &status);
+
+	
+  /* Write TSCALE and TZERO entries to header */
+  for (i=2; i<hdu4_tfields; i++) {
+
+    if ((i==7)&&(big_vel)) continue;
+    
+    /* Omit TSCALE and TZERO for these six arrays. */
+    if (i ==  2) continue;	/* TIME_SUNRISE */
+    if (i ==  3) continue;	/* TIME_SUNSET  */
+    if (i ==  8) continue;	/* HIGH_VOLTAGE */
+    if (i ==  9) continue;	/* LIF_CNT_RATE */
+    if (i == 10) continue;	/* SIC_CNT_RATE */
+    if (i == 13) continue;	/* BKGD_CNT_RATE */
+
+    
+    sprintf(keyword, "TUNIT%ld", i+1);
+    if (fits_read_keyword(outfits, keyword, card, NULL, &status))
+      cf_if_fits_error(status);
+    FITS_insert_key_flt(outfits, hdu4_tscal[i].keyword, hdu4_tscal[i].value,
+			-1, NULL, &status);
+    FITS_insert_key_flt(outfits, hdu4_tzero[i].keyword, hdu4_tzero[i].value,
+			-5, NULL, &status);
+    
+  } 
+  
+  
+  
+  
+  
+  
+  felem_hdu2=1; frow_hdu3=1; felem_hdu4=1;
+  
+  
+  cf_verbose(1,"COMBINING HDU");
+  
+  for (i=0;i<nfiles;i++){
+    
+    cf_verbose(2,"PROCESSING FILE %ld EVENTS LIST",i);
+    
+    delta_t=(expstartlist[i]-expstartlist[0])*3600*24;
+    
+    FITS_open_file(&infits,filelist[i],READONLY,&status);
+    
+    FITS_movabs_hdu(infits, 2, &hdutype, &status);
+    FITS_movabs_hdu(outfits, 2, &hdutype, &status);
+
+    if (neventslist[i]>0){
+      floatlist=(float *)malloc(neventslist[i]*sizeof(float));
+      shortlist=(short *)malloc(neventslist[i]*sizeof(short));
+      charlist=(char *)malloc(neventslist[i]*sizeof(char));
+
+      FITS_get_colnum(infits, TRUE, "TIME", &ncol, &status);
+      FITS_read_col(infits, TFLOAT, ncol, 1, 1, neventslist[i], &intnull,
+		    floatlist, &anynull, &status);
+      for (j=0;j<neventslist[i];j++) floatlist[j]+=delta_t;	
+      FITS_write_col(outfits, TFLOAT, 1, 1, felem_hdu2, neventslist[i], floatlist, &status);
+    
+    
+    
+      FITS_get_colnum(infits, TRUE, "XRAW", &ncol, &status);
+      FITS_read_col(infits, TSHORT, ncol, 1, 1, neventslist[i], &intnull,
+		    shortlist, &anynull, &status);
+      FITS_write_col(outfits, TSHORT, 2, 1, felem_hdu2, neventslist[i], shortlist, &status);
+    
+    
+    
+      FITS_get_colnum(infits, TRUE, "YRAW", &ncol, &status);
+      FITS_read_col(infits, TSHORT, ncol, 1, 1, neventslist[i], &intnull,
+		    shortlist, &anynull, &status);
+      FITS_write_col(outfits, TSHORT, 3, 1, felem_hdu2, neventslist[i], shortlist, &status);
+		
+    
+    
+      FITS_get_colnum(infits, TRUE, "PHA", &ncol, &status);
+      FITS_read_col(infits, TBYTE, ncol, 1, 1, neventslist[i], &intnull,
+		    charlist, &anynull, &status);
+      FITS_write_col(outfits, TBYTE, 4, 1, felem_hdu2, neventslist[i], charlist, &status);
+		
+
+    
+      FITS_get_colnum(infits, TRUE, "WEIGHT", &ncol, &status);
+      FITS_read_col(infits, TFLOAT, ncol, 1, 1, neventslist[i], &intnull,
+		    floatlist, &anynull, &status);
+      FITS_write_col(outfits, TFLOAT, 5, 1, felem_hdu2, neventslist[i], floatlist, &status);
+    
+
+    
+      FITS_get_colnum(infits, TRUE, "XFARF", &ncol, &status);
+      FITS_read_col(infits, TFLOAT, ncol, 1, 1, neventslist[i], &intnull,
+		    floatlist, &anynull, &status);
+      FITS_write_col(outfits, TFLOAT, 6, 1, felem_hdu2, neventslist[i], floatlist, &status);
+		
+
+				
+      FITS_get_colnum(infits, TRUE, "YFARF", &ncol, &status);
+      FITS_read_col(infits, TFLOAT, ncol, 1, 1, neventslist[i], &intnull,
+		    floatlist, &anynull, &status);
+      FITS_write_col(outfits, TFLOAT, 7, 1, felem_hdu2, neventslist[i], floatlist, &status);
+    
+    
+    
+      FITS_get_colnum(infits, TRUE, "X", &ncol, &status);
+      FITS_read_col(infits, TFLOAT, ncol, 1, 1, neventslist[i], &intnull,
+		    floatlist, &anynull, &status);
+      FITS_write_col(outfits, TFLOAT, 8, 1, felem_hdu2, neventslist[i], floatlist, &status);
+    
+    
+    
+      FITS_get_colnum(infits, TRUE, "Y", &ncol, &status);
+      FITS_read_col(infits, TFLOAT, ncol, 1, 1, neventslist[i], &intnull,
+		    floatlist, &anynull, &status);
+      FITS_write_col(outfits, TFLOAT, 9, 1, felem_hdu2, neventslist[i], floatlist, &status);
+    
+    
+    
+      FITS_get_colnum(infits, TRUE, "CHANNEL", &ncol, &status);
+      FITS_read_col(infits, TBYTE, ncol, 1, 1, neventslist[i], &intnull,
+		    charlist, &anynull, &status);
+      FITS_write_col(outfits, TBYTE, 10, 1, felem_hdu2, neventslist[i], charlist, &status);
+    
+    
+    
+      FITS_get_colnum(infits, TRUE, "TIMEFLGS", &ncol, &status);
+      FITS_read_col(infits, TBYTE, ncol, 1, 1, neventslist[i], &intnull,
+		    charlist, &anynull, &status);
+      FITS_write_col(outfits, TBYTE, 11, 1, felem_hdu2, neventslist[i], charlist, &status);
+    
+    
+    
+      FITS_get_colnum(infits, TRUE, "LOC_FLGS", &ncol, &status);
+      FITS_read_col(infits, TBYTE, ncol, 1, 1, neventslist[i], &intnull,
+		    charlist, &anynull, &status);
+      FITS_write_col(outfits, TBYTE, 12, 1, felem_hdu2, neventslist[i], charlist, &status);
+    
+    
+    
+      FITS_get_colnum(infits, TRUE, "LAMBDA", &ncol, &status);
+      FITS_read_col(infits, TFLOAT, ncol, 1, 1, neventslist[i], &intnull,
+		    floatlist, &anynull, &status);
+      FITS_write_col(outfits, TFLOAT, 13, 1, felem_hdu2, neventslist[i], floatlist, &status);
+    
+
+    
+      FITS_get_colnum(infits, TRUE, "ERGCM2", &ncol, &status);
+      FITS_read_col(infits, TFLOAT, ncol, 1, 1, neventslist[i], &intnull,
+		    floatlist, &anynull, &status);
+      FITS_write_col(outfits, TFLOAT, 14, 1, felem_hdu2, neventslist[i], floatlist, &status);
+    
+    
+      free(floatlist);
+      free(charlist);
+      free(shortlist);
+    }
+    
+    cf_verbose(2,"PROCESSING FILE %ld GTIs LIST",i);
+    
+    FITS_movabs_hdu(infits, 3, &hdutype, &status);
+    FITS_movabs_hdu(outfits, 3, &hdutype, &status);
+
+    if (ngtislist[i]>0){
+      doublelist=(double *)malloc(ngtislist[i]*sizeof(double));
+    
+      FITS_get_colnum(infits, TRUE, "START", &ncol, &status);
+      FITS_read_col(infits, TDOUBLE, ncol, 1, 1, ngtislist[i], &intnull,
+		    doublelist, &anynull, &status);
+      for (j=0;j<ngtislist[i];j++) doublelist[j]+=delta_t;
+      FITS_write_col(outfits, TDOUBLE, 1, frow_hdu3, 1, ngtislist[i], doublelist, &status);
+    
+      FITS_get_colnum(infits, TRUE, "STOP", &ncol, &status);
+      FITS_read_col(infits, TDOUBLE, ncol, 1, 1, ngtislist[i], &intnull,
+		    doublelist, &anynull, &status);
+      for (j=0;j<ngtislist[i];j++) doublelist[j]+=delta_t;
+      FITS_write_col(outfits, TDOUBLE, 2, frow_hdu3, 1, ngtislist[i], doublelist, &status);
+    
+    
+      free(doublelist);
+    }
+
+    cf_verbose(2,"PROCESSING FILE %ld TIMELINE",i);
+    
+    FITS_movabs_hdu(infits, 4, &hdutype, &status);
+    FITS_movabs_hdu(outfits, 4, &hdutype, &status);
+    
+    if (nrecordslist[i]>0){
+      floatlist=(float *)malloc(nrecordslist[i]*sizeof(float));
+      shortlist=(short *)malloc(nrecordslist[i]*sizeof(short));
+      charlist=(char *)malloc(nrecordslist[i]*sizeof(char));
+    
+    
+      FITS_get_colnum(infits, TRUE, "TIME", &ncol, &status);
+      FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecordslist[i], &intnull,
+		    floatlist, &anynull, &status);
+      for (j=0;j<nrecordslist[i];j++) floatlist[j]+=delta_t;	
+      FITS_write_col(outfits, TFLOAT, 1, 1, felem_hdu4, nrecordslist[i], floatlist, &status);
+    
+      FITS_get_colnum(infits, TRUE, "STATUS_FLAGS", &ncol, &status);
+      FITS_read_col(infits, TBYTE, ncol, 1, 1, nrecordslist[i], &intnull,
+		    charlist, &anynull, &status);
+      FITS_write_col(outfits, TBYTE, 2, 1, felem_hdu4, nrecordslist[i], charlist, &status);
+    
+      FITS_get_colnum(infits, TRUE, "TIME_SUNRISE", &ncol, &status);
+      FITS_read_col(infits, TSHORT, ncol, 1, 1, nrecordslist[i], &intnull,
+		    shortlist, &anynull, &status);
+      FITS_write_col(outfits, TSHORT, 3, 1, felem_hdu4, nrecordslist[i], shortlist, &status);
+    
+      FITS_get_colnum(infits, TRUE, "TIME_SUNSET", &ncol, &status);
+      FITS_read_col(infits, TSHORT, ncol, 1, 1, nrecordslist[i], &intnull,
+		    shortlist, &anynull, &status);
+      FITS_write_col(outfits, TSHORT, 4, 1, felem_hdu4, nrecordslist[i], shortlist, &status);
+    
+      FITS_get_colnum(infits, TRUE, "LIMB_ANGLE", &ncol, &status);
+      FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecordslist[i], &intnull,
+		    floatlist, &anynull, &status);
+      FITS_write_col(outfits, TFLOAT, 5, 1, felem_hdu4, nrecordslist[i], floatlist, &status);
+    
+      FITS_get_colnum(infits, TRUE, "LONGITUDE", &ncol, &status);
+      FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecordslist[i], &intnull,
+		    floatlist, &anynull, &status);
+      FITS_write_col(outfits, TFLOAT, 6, 1, felem_hdu4, nrecordslist[i], floatlist, &status);
+    
+      FITS_get_colnum(infits, TRUE, "LATITUDE", &ncol, &status);
+      FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecordslist[i], &intnull,
+		    floatlist, &anynull, &status);
+      FITS_write_col(outfits, TFLOAT, 7, 1, felem_hdu4, nrecordslist[i], floatlist, &status);
+    
+      FITS_get_colnum(infits, TRUE, "ORBITAL_VEL", &ncol, &status);
+      FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecordslist[i], &intnull,
+		    floatlist, &anynull, &status);
+      FITS_write_col(outfits, TFLOAT, 8, 1, felem_hdu4, nrecordslist[i], floatlist, &status);
+    
+      FITS_get_colnum(infits, TRUE, "HIGH_VOLTAGE", &ncol, &status);
+      FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecordslist[i], &intnull,
+		    floatlist, &anynull, &status);
+      FITS_write_col(outfits, TFLOAT, 9, 1, felem_hdu4, nrecordslist[i], floatlist, &status);
+    
+      FITS_get_colnum(infits, TRUE, "LIF_CNT_RATE", &ncol, &status);
+      FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecordslist[i], &intnull,
+		    floatlist, &anynull, &status);
+      FITS_write_col(outfits, TFLOAT, 10, 1, felem_hdu4, nrecordslist[i], floatlist, &status);
+    
+      FITS_get_colnum(infits, TRUE, "SIC_CNT_RATE", &ncol, &status);
+      FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecordslist[i], &intnull,
+		    floatlist, &anynull, &status);
+      FITS_write_col(outfits, TFLOAT, 11, 1, felem_hdu4, nrecordslist[i], floatlist, &status);
+		
+      FITS_get_colnum(infits, TRUE, "FEC_CNT_RATE", &ncol, &status);
+      FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecordslist[i], &intnull,
+		    floatlist, &anynull, &status);
+      FITS_write_col(outfits, TFLOAT, 12, 1, felem_hdu4, nrecordslist[i], floatlist, &status);
+    
+      FITS_get_colnum(infits, TRUE, "AIC_CNT_RATE", &ncol, &status);
+      FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecordslist[i], &intnull,
+		    floatlist, &anynull, &status);
+      FITS_write_col(outfits, TFLOAT, 13, 1, felem_hdu4, nrecordslist[i], floatlist, &status);
+    
+      FITS_get_colnum(infits, TRUE, "BKGD_CNT_RATE", &ncol, &status);
+      FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecordslist[i], &intnull,
+		    floatlist, &anynull, &status);	      
+      FITS_write_col(outfits, TFLOAT, 14, 1, felem_hdu4, nrecordslist[i], floatlist, &status);
+    
+      FITS_get_colnum(infits, TRUE, "YCENT_LIF", &ncol, &status);
+      FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecordslist[i], &intnull,
+		    floatlist, &anynull, &status);
+      FITS_write_col(outfits, TFLOAT, 15, 1, felem_hdu4, nrecordslist[i], floatlist, &status);
+    
+      FITS_get_colnum(infits, TRUE, "YCENT_SIC", &ncol, &status);
+      FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecordslist[i], &intnull,
+		    floatlist, &anynull, &status);
+      FITS_write_col(outfits, TFLOAT, 16, 1, felem_hdu4, nrecordslist[i], floatlist, &status);
+    
+    
+    
+    
+      free(floatlist);
+      free(charlist);
+      free(shortlist);
+    }
+    
+    
+    felem_hdu2+=neventslist[i];
+    frow_hdu3+=ngtislist[i];
+    felem_hdu4+=nrecordslist[i];
+    FITS_close_file(infits,&status);
+    
+    
+  }
+
+/*
+  if (fpa_split)
+    cf_if_warning("FPA motion detected. Resolution may be compromised.");
+*/
+
+  if (do_ycent){
+    FITS_movabs_hdu(outfits, 2, &hdutype, &status);
+    nevents = cf_read_col(outfits, TFLOAT, "X",  (void **) &x);
+    nevents = cf_read_col(outfits, TFLOAT, "Y",  (void **) &y);
+    nevents = cf_read_col(outfits, TFLOAT, "WEIGHT", (void **) &weight);
+    nevents = cf_read_col(outfits, TBYTE,  "TIMEFLGS", (void **) &timeflags);
+    nevents = cf_read_col(outfits, TBYTE,  "LOC_FLGS", (void **) &locflags);
+    nevents = cf_read_col(outfits, TBYTE,  "CHANNEL", (void **) &channel);
+    
+    FITS_movabs_hdu(outfits, 1, &hdutype, &status);
+    
+    /* Compute centroids. */
+    cf_calculate_y_centroid(outfits, nevents, weight, x, y, channel, 
+			    timeflags, locflags);
+  } 
+  
+  cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+  cf_verbose(1,"CLOSING OUTPUT FILE");
+  
+  FITS_close_file(outfits,&status);
+  
+ 
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished execution.");
+  return EXIT_SUCCESS;
+  
+}
+
+
diff --git a/src/analysis/idf_cut.c b/src/analysis/idf_cut.c
new file mode 100644
index 0000000..b302c60
--- /dev/null
+++ b/src/analysis/idf_cut.c
@@ -0,0 +1,977 @@
+
+/*****************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *****************************************************************************
+ *
+ * Usage:
+ *   idf_cut [-hm]  [-v level] idf_file RefTime Period Nout
+ * Arguments:
+ *   RefTime :  Reference Time in seconds since EXPSTART
+ *   Period  :  Period in seconds
+ *   Nout    :  Number of output files.
+ * Options:
+ *   -m      :  interprets RefTime as MJD
+ *   -h      :  this help message
+ *   -v      :  verbosity level (=1; 0 is silent)
+ *
+ * Description: 
+ *
+ *     Cuts the IDF file into several smaller IDF files, sorting the 
+ *   events according to their phase. The GTIs table and timeline get
+ *   also cut. 
+ *     From the input IDF file, idf_cut generates Nout IDF files named
+ *   {input_idf_filename}.p{X}.fit with X=0..Nout-1. An event in the 
+ *   input file is sorted in output file X if it happens in the interval
+ *   [RefTime+(k+X/Nout)*Period,RefTime+(k+(X+1)/Nout)*Period[     
+ *   with k an integer.
+ *
+ * History:	10/08/04	bjg  v1.0
+ *              10/26/04        bjg  v1.1 Now updates the GTIs table
+ *                                        Fixed EXPNIGHT computation
+ *                                        Added -m switch.
+ *                       		  + some cosmetic changes
+ *              12/01/04        bjg  v1.2 Free allocated memory in the 
+ *                                        subroutines
+ *              12/02/04        bjg  v1.3 Fixed bug in make_gtitab
+ *              06/03/05        wvd  v1.4 Change nevents and nseconds to longs.
+ *              01/18/06        wvd  v1.5 Read arrays with cf_read_col.
+ *
+ ****************************************************************************/
+
+
+#include <unistd.h>
+#include <stdlib.h>
+#include <stdio.h>
+#include <string.h>
+#include <time.h>
+#include <math.h>
+
+#include "calfuse.h"
+
+#define _MIN(a,b) (((a)<(b))?(a):(b))
+
+typedef char filename[FLEN_CARD];
+
+struct key {
+  char keyword[FLEN_KEYWORD];
+  float value;
+};
+
+static char CF_PRGM_ID[]= "idf_cut";
+static char CF_VER_NUM[]= "1.1";
+
+
+static int _isinphase(double t, double RefTime, double Period, double vinf, double vsup){
+  
+  float v;
+
+  v=fmod(t-RefTime,Period);
+  if (v<0) v+=Period; 
+
+  return ((v>=vinf)&&(v<vsup));
+}
+
+static double _getphasenextstart(double t, double RefTime, double Period, double vinf, double vsup){
+
+  float v;
+  
+  v=fmod(t-RefTime,Period);
+  if (v<0) v+=Period; 
+  
+  if (v>vinf) return t-v+vinf+Period; 
+  else return t-v+vinf;
+
+}
+static double _getphasenextstop(double t, double RefTime, double Period, double vinf, double vsup){
+
+  float v;
+  
+  v=fmod(t-RefTime,Period);
+  if (v<0) v+=Period; 
+ 
+  if (v>vsup) return t-v+vsup+Period; 
+  else return t-v+vsup;
+}
+
+struct _gti{
+  double start;
+  double stop;
+  struct _gti *next;
+};
+
+typedef struct{
+  struct _gti * gtilist;
+  long N;
+} _tempgtis;
+
+static void _pushgti(double a, double b, _tempgtis * tempgtis){
+  struct _gti *aux;
+  
+  aux=tempgtis->gtilist;
+  
+  tempgtis->gtilist=malloc(sizeof(struct _gti));
+  tempgtis->N++;
+  tempgtis->gtilist->start=a;
+  tempgtis->gtilist->stop=b;
+  tempgtis->gtilist->next=aux; 
+} 
+
+static void _popgti(double * a, double * b, _tempgtis * tempgtis){
+  struct _gti *aux;
+  
+  *a=tempgtis->gtilist->start;
+  *b=tempgtis->gtilist->stop;
+
+  aux=tempgtis->gtilist;
+  tempgtis->gtilist=tempgtis->gtilist->next;
+  free(aux);
+  tempgtis->N--;
+} 
+
+static _tempgtis * _makegtis(){
+  _tempgtis * tempgtis;
+
+  tempgtis=malloc(sizeof(_tempgtis));
+  tempgtis->gtilist=NULL;
+  tempgtis->N=0;
+  return tempgtis;
+}
+
+static void _deletegtis(_tempgtis * tempgtis){
+  double a,b;
+  while (tempgtis->gtilist!=NULL) _popgti(&a,&b,tempgtis);
+  free(tempgtis);
+  tempgtis=NULL;
+}
+
+static long _ngtis(_tempgtis * tempgtis){
+  return tempgtis->N;
+}
+
+
+/****************************************************************************/
+
+long make_evlist(fitsfile *infits,fitsfile *outfits,
+		 double RefTime,double Period, long Nout, 
+		 long phase,char * daynight,
+		 long * nbadevnt,long * nbadpha){
+ 
+  
+  int status=0;
+
+  char pha;
+  char loc_flgs;
+  char timeflgs;
+  char time_test;
+
+  char     keyword[FLEN_CARD],card[FLEN_CARD];
+
+  char     fmt_byte[FLEN_CARD],fmt_float[FLEN_CARD],fmt_short[FLEN_CARD]; 
+  
+  int  tfields=14;
+  
+  char extname[]="TTAG DATA";   /* Name of this extension */
+  
+  char *ttype[]={"TIME", "XRAW", "YRAW", "PHA", "WEIGHT", "XFARF", 
+		 "YFARF",  "X", "Y", "CHANNEL", "TIMEFLGS",
+		 "LOC_FLGS", "LAMBDA", "ERGCM2" };
+  
+  char *tform[14];  /* We'll assign values when we know 
+		       the number of elements in the data set. */
+  
+  
+  char *tunit[]={"SECONDS", "PIXELS", "PIXELS", "UNITLESS", "UNITLESS",
+		 "PIXELS", "PIXELS", "PIXELS", "PIXELS", "UNITLESS",
+		 "UNITLESS", "UNITLESS", "ANGSTROMS", "ERG CM^-2"};
+  
+  struct key tscal[] = {{"TSCAL6", 0.25},  {"TSCAL7", 0.1}, 
+			{"TSCAL8", 0.25},  {"TSCAL9", 0.1}};
+  
+  struct key tzero[] = {{"TZERO6", 8192.}, {"TZERO7", 0.}, 
+			{"TZERO8", 8192.}, {"TZERO9", 0.}};
+
+  float *i_time;
+  short *i_xraw;
+  short *i_yraw;
+  char *i_pha;
+  float *i_weight;
+  float *i_xfarf;
+  float *i_yfarf;
+  float *i_x;
+  float *i_y;
+  char *i_channel;
+  char *i_timeflgs;
+  char *i_loc_flgs;
+  float *i_lambda;
+  float *i_ergcm2;
+
+
+  float *o_time;
+  short *o_xraw;
+  short *o_yraw;
+  char *o_pha;
+  float *o_weight;
+  float *o_xfarf;
+  float *o_yfarf;
+  float *o_x;
+  float *o_y;
+  char *o_channel;
+  char *o_timeflgs;
+  char *o_loc_flgs;
+  float *o_lambda;
+  float *o_ergcm2;
+
+  long npts;
+
+  long i;
+
+  float vinf,vsup;
+
+  long nevents=0;
+
+  *nbadevnt=0;
+  *nbadpha=0;
+
+
+  npts = cf_read_col(infits, TFLOAT, "TIME", (void **) &i_time);
+  npts = cf_read_col(infits, TSHORT, "XRAW", (void **) &i_xraw);
+  npts = cf_read_col(infits, TSHORT, "YRAW", (void **) &i_yraw);
+  npts = cf_read_col(infits, TBYTE, "PHA", (void **) &i_pha);
+  npts = cf_read_col(infits, TFLOAT, "WEIGHT", (void **) &i_weight);
+  npts = cf_read_col(infits, TFLOAT, "XFARF", (void **) &i_xfarf);
+  npts = cf_read_col(infits, TFLOAT, "YFARF", (void **) &i_yfarf);
+  npts = cf_read_col(infits, TFLOAT, "X", (void **) &i_x);
+  npts = cf_read_col(infits, TFLOAT, "Y", (void **) &i_y); 
+  npts = cf_read_col(infits, TBYTE, "CHANNEL", (void **) &i_channel);
+  npts = cf_read_col(infits, TBYTE, "TIMEFLGS", (void **) &i_timeflgs);
+  npts = cf_read_col(infits, TBYTE, "LOC_FLGS", (void **) &i_loc_flgs);
+  npts = cf_read_col(infits, TFLOAT, "LAMBDA", (void **) &i_lambda);
+  npts = cf_read_col(infits, TFLOAT, "ERGCM2", (void **) &i_ergcm2); 
+
+
+  o_time     = (float *) malloc(npts*sizeof(float));
+  o_xraw     = (short *) malloc(npts*sizeof(short));
+  o_yraw     = (short *) malloc(npts*sizeof(short));
+  o_pha      = (char *)  malloc(npts*sizeof(char));
+  o_weight   = (float *) malloc(npts*sizeof(float));
+  o_xfarf    = (float *) malloc(npts*sizeof(float));
+  o_yfarf    = (float *) malloc(npts*sizeof(float));
+  o_x        = (float *) malloc(npts*sizeof(float));
+  o_y        = (float *) malloc(npts*sizeof(float));
+  o_channel  = (char *)  malloc(npts*sizeof(char));
+  o_timeflgs = (char *)  malloc(npts*sizeof(char));
+  o_loc_flgs = (char *)  malloc(npts*sizeof(char));
+  o_lambda   = (float *) malloc(npts*sizeof(float));
+  o_ergcm2   = (float *) malloc(npts*sizeof(float)); 
+
+  vinf=(phase*Period)/((float)Nout);
+  vsup=((phase+1)*Period)/((float)Nout);
+
+  
+  for (i=0;i<npts;i++){
+ 
+    if (_isinphase(i_time[i], RefTime, Period, vinf, vsup)) {
+      
+      o_time[nevents]     = i_time[i];
+      o_xraw[nevents]     = i_xraw[i];
+      o_yraw[nevents]     = i_yraw[i]; 
+      o_pha[nevents]      = i_pha[i];
+      o_weight[nevents]   = i_weight[i];
+      o_xfarf[nevents]    = i_xfarf[i];
+      o_yfarf[nevents]    = i_yfarf[i];
+      o_x[nevents]        = i_x[i];
+      o_y[nevents]        = i_y[i];
+      o_channel[nevents]  = i_channel[i]; 
+      o_timeflgs[nevents] = i_timeflgs[i]; 
+      o_loc_flgs[nevents] = i_loc_flgs[i];
+      o_lambda[nevents]   = i_lambda[i];
+      o_ergcm2[nevents]   = i_ergcm2[i];  
+
+      pha=i_pha[i];
+      loc_flgs=i_loc_flgs[i];
+      timeflgs=i_timeflgs[i];
+
+      switch(daynight[0]) {
+      case 'D':
+	time_test=timeflgs^TEMPORAL_DAY;
+	break;
+      case 'N':
+	time_test=timeflgs;
+	break;
+      default:
+	time_test=timeflgs&(~TEMPORAL_DAY);
+      }
+
+      if (loc_flgs&LOCATION_PHA){
+	*nbadpha++;
+      } 
+
+      if ((loc_flgs&~LOCATION_AIR) || (time_test)) {
+	*nbadevnt++;
+      }
+
+	
+      nevents++;
+     
+    }
+    
+
+  }
+
+  
+
+
+  /* Generate the tform array */
+  sprintf(fmt_byte,  "%ldB", nevents);
+  sprintf(fmt_float, "%ldE", nevents);
+  sprintf(fmt_short, "%ldI", nevents);
+  
+  tform[0] = fmt_float;
+  tform[1] = fmt_short;
+  tform[2] = fmt_short;
+  tform[3] = fmt_byte;
+  tform[4] = fmt_float;
+  for (i=5; i<9; i++)
+    tform[i] = fmt_short;
+  for ( ; i<12; i++)
+    tform[i] = fmt_byte;
+  tform[12] = fmt_float;
+  tform[13] = fmt_float;
+  
+
+  /* Append a new empty binary table to the output file */
+  FITS_create_tbl(outfits, BINARY_TBL, 1, tfields, ttype, tform,
+		  tunit, extname, &status);
+  
+  /* Write TSCALE and TZERO entries to header */
+  for (i=0; i<4; i++) {
+    sprintf(keyword, "TUNIT%ld", i+6);
+    if (fits_read_keyword(outfits, keyword, card, NULL, &status))
+      cf_if_fits_error(status);
+    FITS_insert_key_flt(outfits, tscal[i].keyword, tscal[i].value,
+			-2, NULL, &status);
+    FITS_insert_key_flt(outfits, tzero[i].keyword, tzero[i].value,
+			-4, NULL, &status);
+  } 
+
+  if (nevents > 0) {
+   
+    FITS_write_col(outfits, TFLOAT,  1, 1, 1, nevents, o_time, &status);
+    FITS_write_col(outfits, TSHORT,  2, 1, 1, nevents, o_xraw, &status);
+    FITS_write_col(outfits, TSHORT,  3, 1, 1, nevents, o_yraw, &status);
+    FITS_write_col(outfits, TBYTE ,  4, 1, 1, nevents, o_pha, &status);
+    FITS_write_col(outfits, TFLOAT,  5, 1, 1, nevents, o_weight, &status);
+    FITS_write_col(outfits, TFLOAT,  6, 1, 1, nevents, o_xfarf, &status);
+    FITS_write_col(outfits, TFLOAT,  7, 1, 1, nevents, o_yfarf, &status);
+    FITS_write_col(outfits, TFLOAT,  8, 1, 1, nevents, o_x, &status);
+    FITS_write_col(outfits, TFLOAT,  9, 1, 1, nevents, o_y, &status);
+    FITS_write_col(outfits, TBYTE , 10, 1, 1, nevents, o_channel, &status);
+    FITS_write_col(outfits, TBYTE , 11, 1, 1, nevents, o_timeflgs, &status);
+    FITS_write_col(outfits, TBYTE , 12, 1, 1, nevents, o_loc_flgs, &status);
+    FITS_write_col(outfits, TFLOAT, 13, 1, 1, nevents, o_lambda, &status);
+    FITS_write_col(outfits, TFLOAT, 14, 1, 1, nevents, o_ergcm2, &status);
+  }
+
+  free(o_time);
+  free(o_xraw );   
+  free(o_yraw);    
+  free(o_pha);     
+  free(o_weight);   
+  free(o_xfarf);    
+  free(o_yfarf);    
+  free(o_x);        
+  free(o_y);        
+  free(o_channel); 
+  free(o_timeflgs);
+  free(o_loc_flgs); 
+  free(o_lambda);   
+  free(o_ergcm2);
+
+  free(i_time);
+  free(i_xraw );   
+  free(i_yraw);    
+  free(i_pha);     
+  free(i_weight);   
+  free(i_xfarf);    
+  free(i_yfarf);    
+  free(i_x);        
+  free(i_y);        
+  free(i_channel); 
+  free(i_timeflgs);
+  free(i_loc_flgs); 
+  free(i_lambda);   
+  free(i_ergcm2); 
+  
+  return nevents;
+}
+
+/****************************************************************************/
+long make_gtitab(fitsfile * infits, fitsfile * outfits, 
+		 double RefTime, double Period, long Nout, 
+		 long phase){
+  
+  
+
+  int status=0;
+  
+  int  tfields=2;
+  char extname[]="GTI";   /* Name of this extension */
+  char *ttype[]={"START", "STOP" };
+  char *tform[2]={"1D", "1D" };  
+  char *tunit[]={"seconds", "seconds"};
+
+  double *i_start;
+  double *i_stop;
+  double *o_start;
+  double *o_stop;
+  
+  _tempgtis * tempgtis;
+
+  long npts=0;
+  long ngtis=0;
+  long i;
+
+  float vinf,vsup;
+  
+  double a,b;
+  double _start, _stop;
+
+  npts = cf_read_col(infits, TDOUBLE, "START", (void **) &i_start);
+  npts = cf_read_col(infits, TDOUBLE, "STOP",  (void **) &i_stop);
+
+  vinf=(phase*Period)/((float)Nout);
+  vsup=((phase+1)*Period)/((float)Nout);
+
+  tempgtis=_makegtis();
+  for (i=0;i<npts;i++){
+    cf_verbose(4,"Input GTI %ld = %lf/%lf",i,i_start[i],i_stop[i]);
+    a=i_start[i];
+    b=i_stop[i];
+    if (_isinphase(a,RefTime, Period, vinf, vsup)) _start=a;
+    else _start=_MIN(b,_getphasenextstart(a,RefTime, Period, vinf, vsup));
+   
+    while (_start<b){
+      _stop=_MIN(b,_getphasenextstop(_start,RefTime, Period, vinf, vsup));
+      _pushgti(_start,_stop,tempgtis);
+      cf_verbose(4,"Output GTI = %lf,%lf",_start,_stop);
+      _start=_getphasenextstart(_stop,RefTime, Period, vinf, vsup);
+    }
+  }
+
+  ngtis=_ngtis(tempgtis);
+
+  o_start=(double *)malloc(ngtis*sizeof(double));
+  o_stop=(double *)malloc(ngtis*sizeof(double)); 
+
+  for (i=ngtis-1;i>=0;i--){
+    _popgti(&o_start[i],&o_stop[i],tempgtis);
+  } 
+  
+  _deletegtis(tempgtis);
+  
+  /* Append a new empty binary table to the output file */
+  FITS_create_tbl(outfits, BINARY_TBL, ngtis, tfields, ttype, tform,
+		  tunit, extname, &status);
+ 
+
+  if (ngtis>0){
+    FITS_write_col(outfits, TDOUBLE, 1, 1, 1, ngtis, o_start, &status);
+    FITS_write_col(outfits, TDOUBLE, 2, 1, 1, ngtis, o_stop, &status);
+  }
+  
+  return ngtis;
+
+}
+/****************************************************************************/
+long make_timeline(fitsfile *infits, fitsfile *outfits, 
+		   double RefTime, double Period, long Nout, long phase, 
+		   char *daynight, 
+		   double *exptime, double *exp_bad, double *exp_brst, double *exp_hv, 
+		   double *exp_jitr, double *exp_lim, double *exp_saa, double *expnight){
+
+  char timeflgs;
+  char time_test;
+  int status=0;
+
+  int bigtime=1;
+  int big_vel=1;
+
+  char     keyword[FLEN_CARD],card[FLEN_CARD];
+
+  char     fmt_byte[FLEN_CARD],fmt_float[FLEN_CARD],fmt_short[FLEN_CARD]; 
+
+  struct key tscal[16];
+  struct key tzero[16];
+  
+  char extname[]="TIMELINE";
+
+  int tfields=16;  /* output table will have 16 columns */
+
+  char *ttype[]={"TIME", "STATUS_FLAGS", "TIME_SUNRISE", "TIME_SUNSET",
+		 "LIMB_ANGLE", "LONGITUDE", "LATITUDE", "ORBITAL_VEL",
+		 "HIGH_VOLTAGE", "LIF_CNT_RATE", "SIC_CNT_RATE",
+		 "FEC_CNT_RATE", "AIC_CNT_RATE", "BKGD_CNT_RATE",
+		 "YCENT_LIF","YCENT_SIC"};
+
+  char *tform[16]; /* we will define tform later, when the number
+		      of photons is known */
+  
+  char *tunit[]={"seconds", "unitless", "seconds", "seconds", "degrees",
+		 "degrees", "degrees",  "km/s", "unitless", "counts/sec",
+		 "counts/sec", "counts/sec", "counts/sec", "counts/sec",
+		 "pixels","pixels" };  
+
+  float *i_time;
+  char  *i_status_flags;
+  float *i_time_sunrise;
+  float *i_time_sunset;
+  float *i_limb_angle;
+  float *i_longitude;
+  float *i_latitude;
+  float *i_orbital_vel;
+  short *i_high_voltage;
+  short *i_lif_cnt_rate;
+  short *i_sic_cnt_rate;
+  short *i_fec_cnt_rate;
+  short *i_aic_cnt_rate;
+  short *i_bkgd_cnt_rate;
+  float *i_ycent_lif;
+  float *i_ycent_sic;
+
+  float *o_time;
+  char  *o_status_flags;
+  float *o_time_sunrise;
+  float *o_time_sunset;
+  float *o_limb_angle;
+  float *o_longitude;
+  float *o_latitude;
+  float *o_orbital_vel;
+  short *o_high_voltage;
+  short *o_lif_cnt_rate;
+  short *o_sic_cnt_rate;
+  short *o_fec_cnt_rate;
+  short *o_aic_cnt_rate;
+  short *o_bkgd_cnt_rate;
+  float *o_ycent_lif;
+  float *o_ycent_sic;
+
+  long npts;
+
+  long i;
+
+  float vinf,vsup;
+
+  long nseconds=0;
+
+  *exptime=0;
+  *expnight=0;
+  *exp_bad=0;
+  *exp_brst=0;
+  *exp_hv=0;
+  *exp_jitr=0;
+  *exp_lim=0;
+  *exp_saa=0;
+  *expnight=0;
+
+
+
+  npts = cf_read_col(infits, TFLOAT, "TIME"          , (void **) &i_time);
+  npts = cf_read_col(infits, TBYTE , "STATUS_FLAGS"  , (void **) &i_status_flags);
+  npts = cf_read_col(infits, TFLOAT, "TIME_SUNRISE"  , (void **) &i_time_sunrise);
+  npts = cf_read_col(infits, TFLOAT, "TIME_SUNSET"   , (void **) &i_time_sunset);
+  npts = cf_read_col(infits, TFLOAT, "LIMB_ANGLE"    , (void **) &i_limb_angle);
+  npts = cf_read_col(infits, TFLOAT, "LONGITUDE"     , (void **) &i_longitude);
+  npts = cf_read_col(infits, TFLOAT, "LATITUDE"      , (void **) &i_latitude);
+  npts = cf_read_col(infits, TFLOAT, "ORBITAL_VEL"   , (void **) &i_orbital_vel);
+  npts = cf_read_col(infits, TSHORT, "HIGH_VOLTAGE"  , (void **) &i_high_voltage); 
+  npts = cf_read_col(infits, TSHORT, "LIF_CNT_RATE"  , (void **) &i_lif_cnt_rate);
+  npts = cf_read_col(infits, TSHORT, "SIC_CNT_RATE"  , (void **) &i_sic_cnt_rate);
+  npts = cf_read_col(infits, TSHORT, "FEC_CNT_RATE"  , (void **) &i_fec_cnt_rate);
+  npts = cf_read_col(infits, TSHORT, "AIC_CNT_RATE"  , (void **) &i_aic_cnt_rate);
+  npts = cf_read_col(infits, TSHORT, "BKGD_CNT_RATE" , (void **) &i_bkgd_cnt_rate); 
+  npts = cf_read_col(infits, TFLOAT, "YCENT_LIF"     , (void **) &i_ycent_lif);
+  npts = cf_read_col(infits, TFLOAT, "YCENT_SIC"     , (void **) &i_ycent_sic);
+
+
+  o_time            = (float *) malloc(npts*sizeof(float));
+  o_status_flags    = (char *)  malloc(npts*sizeof(char));
+  o_time_sunrise    = (float *) malloc(npts*sizeof(float));
+  o_time_sunset     = (float *) malloc(npts*sizeof(float));
+  o_limb_angle      = (float *) malloc(npts*sizeof(float));
+  o_longitude       = (float *) malloc(npts*sizeof(float));
+  o_latitude        = (float *) malloc(npts*sizeof(float));
+  o_orbital_vel     = (float *) malloc(npts*sizeof(float));
+  o_high_voltage    = (short *) malloc(npts*sizeof(short));
+  o_lif_cnt_rate    = (short *) malloc(npts*sizeof(short));
+  o_sic_cnt_rate    = (short *) malloc(npts*sizeof(short));
+  o_fec_cnt_rate    = (short *) malloc(npts*sizeof(short));
+  o_aic_cnt_rate    = (short *) malloc(npts*sizeof(short));
+  o_bkgd_cnt_rate   = (short *) malloc(npts*sizeof(short));
+  o_ycent_lif       = (float *) malloc(npts*sizeof(float));
+  o_ycent_sic       = (float *) malloc(npts*sizeof(float));
+ 
+
+  vinf=(phase*Period)/((float)Nout);
+  vsup=((phase+1)*Period)/((float)Nout);
+
+
+  for (i=0;i<npts;i++){
+    
+    if (_isinphase(i_time[i], RefTime, Period, vinf, vsup)) {
+
+      o_time[nseconds]            = i_time[i];
+      o_status_flags[nseconds]    = i_status_flags[i];
+      o_time_sunrise[nseconds]    = i_time_sunrise[i];
+      o_time_sunset[nseconds]     = i_time_sunset[i];
+      o_limb_angle[nseconds]      = i_limb_angle[i];
+      o_longitude[nseconds]       = i_longitude[i];
+      o_latitude[nseconds]        = i_latitude[i];
+      o_orbital_vel[nseconds]     = i_orbital_vel[i];
+      o_high_voltage[nseconds]    = i_high_voltage[i];
+      o_lif_cnt_rate[nseconds]    = i_lif_cnt_rate[i];
+      o_sic_cnt_rate[nseconds]    = i_sic_cnt_rate[i];
+      o_fec_cnt_rate[nseconds]    = i_fec_cnt_rate[i];
+      o_aic_cnt_rate[nseconds]    = i_aic_cnt_rate[i];
+      o_bkgd_cnt_rate[nseconds]   = i_bkgd_cnt_rate[i];
+      o_ycent_lif[nseconds]       = i_ycent_lif[i];
+      o_ycent_sic[nseconds]       = i_ycent_sic[i];
+
+      timeflgs=i_status_flags[i];
+
+      switch(daynight[0]) {
+      case 'D':
+	time_test=timeflgs^TEMPORAL_DAY;
+	break;
+      case 'N':
+	time_test=timeflgs;
+	break;
+      default:
+	time_test=timeflgs&(~TEMPORAL_DAY);
+      }
+
+    
+      if (time_test==0) {
+
+	*exptime+=1.0;
+
+	if (!(timeflgs & TEMPORAL_DAY))
+	  *expnight+=1.0;
+
+      } else {
+
+	*exp_bad+=1.0;
+	
+	if (timeflgs & TEMPORAL_BRST)
+	  *exp_brst+=1.0;
+
+	if (timeflgs & TEMPORAL_HV)
+	  *exp_hv=+1.0;	
+
+	if (timeflgs & TEMPORAL_JITR)
+	  *exp_jitr=+1.0;
+
+	if (timeflgs & TEMPORAL_LIMB)
+	  *exp_lim=+1.0;
+
+	if (timeflgs & TEMPORAL_SAA)
+	  *exp_saa=+1.0;
+
+      }
+     
+      nseconds++;
+    }
+  }
+    
+  /* Generate the tform array */
+  sprintf(fmt_byte,  "%ldB", nseconds);
+  sprintf(fmt_float, "%ldE", nseconds);
+  sprintf(fmt_short, "%ldI", nseconds);
+
+    
+  tform[0] = fmt_float;
+  tform[1] = fmt_byte;
+
+  for (i=2; i<tfields; i++)	tform[i] = fmt_short;
+  
+  /* Set TSCALE and TZERO values */
+  /* Not all of these will be used; see below. */
+  for (i=2; i<tfields; i++) {
+    sprintf(tscal[i].keyword, "TSCAL%ld", i+1);
+    tscal[i].value = 0.1;
+    sprintf(tzero[i].keyword, "TZERO%ld", i+1);
+    tzero[i].value = 0.;
+  }
+  
+  /* Need TZEROn = 3000. for tsunrise and tsunset. */
+  tzero[2].value = tzero[3].value = 3000.;
+
+  /* Let's keep three significant figures for vorb. */
+  tscal[7].value = 0.01;
+
+  /* FEC_CNT_RATE and AIC_CNT_RATE can get big, so we
+     (essentially) store them as unsigned shorts. */
+  tscal[11].value = 1;
+  tscal[12].value = 1;
+  tzero[11].value = 32768;
+  tzero[12].value = 32768;
+    
+  
+  if (bigtime) { 
+    tform[2]=tform[3]=fmt_float; 
+  }
+
+  if (big_vel) tform[7]=fmt_float; 
+    
+  /* Append a new empty binary table to the output file */
+  FITS_create_tbl(outfits, BINARY_TBL, 1, tfields, ttype, tform,
+		  tunit, extname, &status);
+
+  
+	
+  /* Write TSCALE and TZERO entries to header */
+  for (i=2; i<tfields; i++) {
+
+    /* If bigtime is TRUE, store tsunrise and tsunset as floats.*/
+    if ((i == 2 || i == 3) && bigtime) continue;
+
+    if ((i==7)&&(big_vel)) continue;
+    
+    /* Omit TSCALE and TZERO for these four arrays. */
+    if (i ==  8) continue;	/* HIGH_VOLTAGE */
+    if (i ==  9) continue;	/* LIF_CNT_RATE */
+    if (i == 10) continue;	/* SIC_CNT_RATE */
+    if (i == 13) continue;	/* BKGD_CNT_RATE */
+
+      
+    sprintf(keyword, "TUNIT%ld", i+1);
+    if (fits_read_keyword(outfits, keyword, card, NULL, &status))
+      cf_if_fits_error(status);
+    FITS_insert_key_flt(outfits, tscal[i].keyword, tscal[i].value,
+			-1, NULL, &status);
+    FITS_insert_key_flt(outfits, tzero[i].keyword, tzero[i].value,
+			-5, NULL, &status);
+  } 
+
+  if (nseconds > 0) { 
+
+    FITS_write_col(outfits, TFLOAT,  1, 1, 1, nseconds, o_time          , &status);
+    FITS_write_col(outfits, TBYTE ,  2, 1, 1, nseconds, o_status_flags  , &status);
+    FITS_write_col(outfits, TFLOAT,  3, 1, 1, nseconds, o_time_sunrise  , &status);
+    FITS_write_col(outfits, TFLOAT,  4, 1, 1, nseconds, o_time_sunset   , &status);
+    FITS_write_col(outfits, TFLOAT,  5, 1, 1, nseconds, o_limb_angle    , &status);
+    FITS_write_col(outfits, TFLOAT,  6, 1, 1, nseconds, o_longitude     , &status);
+    FITS_write_col(outfits, TFLOAT,  7, 1, 1, nseconds, o_latitude      , &status);
+    FITS_write_col(outfits, TFLOAT,  8, 1, 1, nseconds, o_orbital_vel   , &status);
+    FITS_write_col(outfits, TSHORT,  9, 1, 1, nseconds, o_high_voltage  , &status);
+    FITS_write_col(outfits, TSHORT, 10, 1, 1, nseconds, o_lif_cnt_rate  , &status);
+    FITS_write_col(outfits, TSHORT, 11, 1, 1, nseconds, o_sic_cnt_rate  , &status);
+    FITS_write_col(outfits, TSHORT, 12, 1, 1, nseconds, o_fec_cnt_rate  , &status);
+    FITS_write_col(outfits, TSHORT, 13, 1, 1, nseconds, o_aic_cnt_rate  , &status);
+    FITS_write_col(outfits, TSHORT, 14, 1, 1, nseconds, o_bkgd_cnt_rate , &status);
+    FITS_write_col(outfits, TFLOAT, 15, 1, 1, nseconds, o_ycent_lif     , &status);
+    FITS_write_col(outfits, TFLOAT, 16, 1, 1, nseconds, o_ycent_sic     , &status);
+
+  } 
+
+  free(o_time);
+  free(o_status_flags);
+  free(o_time_sunrise);  
+  free(o_time_sunset);    
+  free(o_limb_angle);    
+  free(o_longitude);   
+  free(o_latitude); 
+  free(o_orbital_vel);
+  free(o_high_voltage);
+  free(o_lif_cnt_rate);
+  free(o_sic_cnt_rate);
+  free(o_fec_cnt_rate);
+  free(o_aic_cnt_rate);
+  free(o_bkgd_cnt_rate);
+  free(o_ycent_lif);
+  free(o_ycent_sic);
+
+  free(i_time);
+  free(i_status_flags);
+  free(i_time_sunrise);  
+  free(i_time_sunset);    
+  free(i_limb_angle);    
+  free(i_longitude);   
+  free(i_latitude); 
+  free(i_orbital_vel);
+  free(i_high_voltage);
+  free(i_lif_cnt_rate);
+  free(i_sic_cnt_rate);
+  free(i_fec_cnt_rate);
+  free(i_aic_cnt_rate);
+  free(i_bkgd_cnt_rate);
+  free(i_ycent_lif);
+  free(i_ycent_sic);
+
+  return nseconds;
+}
+/****************************************************************************/
+
+
+int main(int argc,char *argv[]){
+  time_t   vtime;
+  char     stime[FLEN_CARD];
+
+  fitsfile * infits;
+  fitsfile * outfits; 
+ 
+  filename input_filename,output_filename, ifname;
+
+  char string0[FLEN_CARD], daynight[FLEN_CARD];
+  
+
+  	
+  long nevents;
+  long nseconds;
+  long ngtis;
+
+  long nbadevnt;
+  long nbadpha;
+ 
+  double exptime;
+  double exp_bad;
+  double exp_brst;
+  double exp_hv;
+  double exp_jitr;
+  double exp_lim;
+  double exp_saa;
+  double expnight;
+ 
+  double RefTime;
+  double Period;
+  long Nout;
+
+  double expstart;
+
+  long i;
+
+  int optc;
+  
+  char opts[] = "hmv:";
+  char usage[] = 
+    "Usage:\n"
+    "  idf_cut [-hm]  [-v level] idf_file RefTime Period Nout\n";
+  char argument[] =
+    "Arguments:\n"
+    "  RefTime :  Reference Time in seconds since EXPSTART\n"
+    "  Period  :  Period in seconds\n"
+    "  Nout    :  Number of output files.\n";
+  char option[] =
+    "Options:\n"
+    "  -m:  interprets RefTime as MJD\n"
+    "  -h:  this help message\n"
+    "  -v:  verbosity level (=1; 0 is silent)\n";
+
+  int hdutype=0;
+  int status=0;
+  int rtime_mjd=0;
+  verbose_level = 1;
+
+  /* Check number of options and arguments */
+  while ((optc = getopt(argc, argv, opts)) != -1) {
+    switch(optc) {
+    case 'h':
+      printf("%s\n%s\n%s", usage, argument, option);
+      return 0;
+    case 'v':
+      verbose_level = atoi(optarg);
+      break;
+    case 'm':
+      rtime_mjd=1;
+      break;
+    }
+  }
+
+  cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+  if (argc != optind+4) {
+    printf("%s", usage);
+    cf_if_error("Incorrect number of arguments");
+  }
+
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Started execution."); 
+
+  /* get and display time */
+  vtime = time(NULL) ;
+  strcpy(stime,ctime(&vtime));
+
+  strcpy(input_filename,argv[optind]);
+
+  sscanf(argv[optind+1],"%lf",&RefTime);
+  sscanf(argv[optind+2],"%lf",&Period);
+  sscanf(argv[optind+3],"%ld",&Nout);
+  
+  FITS_open_file(&infits,input_filename,READONLY,&status);
+  FITS_read_key(infits,TSTRING,"DAYNIGHT",daynight,NULL,&status);
+  FITS_read_key(infits,TSTRING,"FILENAME",ifname,NULL,&status);
+
+  if (rtime_mjd){
+    FITS_read_key(infits,TDOUBLE,"EXPSTART",&expstart,NULL,&status);
+    RefTime=(RefTime-expstart)*3600.0*24.0;
+  }
+
+  for (i=0;i<Nout;i++){
+    FITS_movabs_hdu(infits,1,&hdutype,&status);
+    
+    
+    strcpy(output_filename,ifname);
+    sprintf(string0,".p%ld.fit",i);
+    strcat(output_filename,string0);
+
+    FITS_create_file(&outfits,output_filename,&status);
+    FITS_copy_hdu(infits,outfits,0,&status);
+
+    FITS_update_key(outfits,TSTRING,"FILENAME",output_filename,NULL,&status);
+
+    cf_verbose(1,"Phase: %ld/%ld",i+1,Nout);
+
+    cf_verbose(2,"Creating Events List");
+    /* Create Events List        */
+    FITS_movabs_hdu(infits,2,&hdutype,&status);
+    nevents=make_evlist(infits, outfits, RefTime, Period, Nout, i, daynight,
+			&nbadevnt, &nbadpha);
+    cf_verbose(2,"Number of Events: %ld",nevents);
+
+    cf_verbose(2,"Creating GTI table");
+    /* Create GTIs Table         */
+    FITS_movabs_hdu(infits,3,&hdutype,&status);
+    ngtis=make_gtitab(infits, outfits, RefTime, Period, Nout, i);
+    cf_verbose(2,"Number of GTIs: %ld",ngtis);
+
+    cf_verbose(2,"Creating Timeline");
+    /* Create Timeline */
+    FITS_movabs_hdu(infits,4,&hdutype,&status);
+    nseconds=make_timeline(infits, outfits, RefTime, Period, Nout, i, daynight,
+			   &exptime, &exp_bad, &exp_brst, &exp_hv, &exp_jitr,
+			   &exp_lim, &exp_saa, &expnight);
+    cf_verbose(2,"Number of records in timeline: %ld",nseconds);
+
+
+    /* Update Main Header Keyword */
+    FITS_movabs_hdu(outfits,1,&hdutype,&status);
+
+   
+    FITS_update_key(outfits,TDOUBLE ,"EXPTIME"  ,&exptime   ,NULL,&status);
+    FITS_update_key(outfits,TLONG   ,"RAWTIME"  ,&nseconds  ,NULL,&status);	
+    FITS_update_key(outfits,TLONG   ,"NEVENTS"  ,&nevents   ,NULL,&status);	
+    FITS_update_key(outfits,TLONG   ,"NBADEVNT" ,&nbadevnt  ,NULL,&status);
+    FITS_update_key(outfits,TLONG   ,"NBADPHA"  ,&nbadpha   ,NULL,&status);
+    FITS_update_key(outfits,TDOUBLE ,"EXP_BAD"  ,&exp_bad   ,NULL,&status);
+    FITS_update_key(outfits,TDOUBLE ,"EXP_SAA"  ,&exp_saa   ,NULL,&status);
+    FITS_update_key(outfits,TDOUBLE ,"EXP_LIM"  ,&exp_lim   ,NULL,&status);
+    FITS_update_key(outfits,TDOUBLE ,"EXP_BRST" ,&exp_brst  ,NULL,&status);		
+    FITS_update_key(outfits,TDOUBLE ,"EXP_JITR" ,&exp_jitr  ,NULL,&status);
+    FITS_update_key(outfits,TDOUBLE ,"EXPNIGHT" ,&expnight  ,NULL,&status);
+
+    FITS_close_file(outfits,&status);
+  }
+  FITS_close_file(infits,&status);
+
+  return (status);
+}
diff --git a/src/analysis/idf_screen.c b/src/analysis/idf_screen.c
new file mode 100644
index 0000000..31aa022
--- /dev/null
+++ b/src/analysis/idf_screen.c
@@ -0,0 +1,339 @@
+
+/*****************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *****************************************************************************
+ *
+ * Synopsis:	idf_screen infits outfits timeflag value
+ *
+ * 
+ *
+ * History:	10/05/04	bjg   1.0     	Begin work.
+ *	        10/26/04        bjg   1.1     	Updates important header 
+ *                                              keywords.
+ *
+ ****************************************************************************/
+
+
+#include <unistd.h>
+#include <stdlib.h>
+#include <stdio.h>
+#include <string.h>
+#include <time.h>
+#include "calfuse.h"
+
+
+typedef char filename[FLEN_CARD];
+
+struct key {
+  char keyword[FLEN_KEYWORD];
+  float value;
+};
+
+static char CF_PRGM_ID[]= "idf_screen";
+static char CF_VER_NUM[]= "1.1";
+
+int main(int argc,char *argv[]){
+
+  char       tempstring[FLEN_CARD]; 
+  char       daynight[FLEN_CARD];
+  char *     corrected_filename;
+  char *     string_pointer;
+
+  char time_test;
+  
+  int status=0; 
+  int hdutype=0;
+
+  long i, npts;
+
+  char * tflags, * lflags;
+
+  fitsfile *infits     , *outfits;
+
+  filename input_fname , output_fname;
+
+  char selstr1[FLEN_CARD];
+  char selstr2[FLEN_CARD];
+
+  char sel1;
+  int sel2;
+ 
+  long nbadevnt=0;
+  long nbadpha=0;
+ 
+  double exptime=0.0;
+  double exp_bad=0.0;
+  double exp_brst=0.0;
+  double exp_hv=0.0;
+  double exp_jitr=0.0;
+  double exp_lim=0.0;
+  double exp_saa=0.0;
+  double expnight=0.0;
+
+  int optc;
+
+  char opts[] = "hv:";
+  char usage[] = 
+    "Usage:\n"
+    "  idf_screen [-h]  [-v level] input_idf_file output_idf_file \n"
+    "                              timeflag value\n";
+  char argument[] = 
+    "Arguments :\n"
+    "  timeflag :  USER/JITR/OPUS/BRST/HV/SAA/LIMB/DAY \n"
+    "  value    :  GOOD/BAD/EITHER           \n";
+  char option[] =
+    "Options:\n"
+    "  -h:  this help message\n"
+    "  -v:  verbosity level (=1; 0 is silent)\n";
+
+  verbose_level = 1;
+
+  /* Check number of options and arguments */
+  while ((optc = getopt(argc, argv, opts)) != -1) {
+    switch(optc) { 
+    case 'h':
+      printf("%s\n%s\n%s", usage, argument, option);
+      return 0;
+    case 'v':
+      verbose_level = atoi(optarg);
+      break;
+    }
+  }
+
+ 
+  cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+  if (argc != optind+4) {
+    printf("%s", usage);
+    cf_if_error("Incorrect number of arguments");
+  }
+    
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Started execution.");
+  
+
+  strcpy(input_fname,argv[optind]);
+  strcpy(output_fname,argv[optind+1]);
+  strcpy(selstr1,argv[optind+2]);
+  strcpy(selstr2,argv[optind+3]);  
+
+  
+
+  if (!strcasecmp(selstr2,"GOOD")) {
+    sel2=0;
+  } else if (!strcasecmp(selstr2,"BAD")) {
+    sel2=1;
+  } else if (!strcasecmp(selstr2,"EITHER")) {
+    sel2=2;
+  } else { 
+    printf("%s", usage);
+    cf_if_error("VALUE not recognized.");
+  }
+
+
+  if (!strcasecmp(selstr1,"USER")) {
+    sel1=TEMPORAL_USER;
+  } else if (!strcasecmp(selstr1,"JITR")) {
+    sel1=TEMPORAL_JITR;
+  } else if (!strcasecmp(selstr1,"OPUS")) {
+    sel1=TEMPORAL_OPUS;
+  } else if (!strcasecmp(selstr1,"BRST")) {
+    sel1=TEMPORAL_BRST;
+  } else if (!strcasecmp(selstr1,"HV")) {
+    sel1=TEMPORAL_HV;
+  } else if (!strcasecmp(selstr1,"SAA")) {
+    sel1=TEMPORAL_SAA;
+  } else if (!strcasecmp(selstr1,"LIMB")) {
+    sel1=TEMPORAL_LIMB;
+  } else if (!strcasecmp(selstr1,"DAY")) {
+    sel1=TEMPORAL_DAY;
+  } else { 
+    printf("%s", usage);
+    cf_if_error("TIMEFLAG not recognized.");
+  }
+
+  cf_verbose(1,"Input  Filename : %s",input_fname);
+  cf_verbose(1,"Output Filename : %s",output_fname);
+  cf_verbose(1,"FLAG : %s - %d",selstr1,sel1);
+  cf_verbose(1,"VALUE : %s - %d",selstr2,sel2);
+
+  if ((sel1>1)&&(sel2==0)){
+    cf_verbose(1,"Nothing to do.");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished execution.");
+    return EXIT_SUCCESS;
+  }
+
+  cf_verbose(1,"OPENING INPUT FILE");
+  FITS_open_file(&infits,input_fname,READONLY,&status);
+
+  cf_verbose(1,"CREATING OUTPUT FILE");
+  FITS_create_file(&outfits,output_fname,&status);
+  FITS_copy_hdu(infits,outfits,0,&status);
+
+  string_pointer=strrchr(output_fname,'/');
+  if (string_pointer==NULL) corrected_filename=output_fname;
+  else corrected_filename=&(string_pointer[1]);
+
+  FITS_update_key(outfits,TSTRING,"FILENAME",corrected_filename,NULL,&status);
+
+  strcpy(tempstring,"");
+
+  FITS_update_key(outfits,TSTRING,"BPM_CAL",tempstring,NULL,&status);
+
+  if (sel1 == 1) {
+    switch(sel2) {
+    case 0:
+      strcpy(daynight,"NIGHT");
+      break;
+    case 1:
+      strcpy(daynight,"DAY");      
+      break;
+    case 2:
+      strcpy(daynight,"BOTH");     
+      break;
+    }
+    FITS_update_key(outfits,TSTRING,"DAYNIGHT",daynight,NULL,&status);
+  } else {
+    FITS_read_key(infits,TSTRING,"DAYNIGHT",daynight,NULL,&status);
+  }
+
+
+  FITS_movabs_hdu(infits,2,&hdutype,&status);
+  FITS_create_hdu(outfits,&status);
+  FITS_copy_hdu(infits,outfits,0,&status);
+
+  
+  npts = cf_read_col(outfits, TBYTE, "TIMEFLGS", (void **) &tflags);  
+  npts = cf_read_col(outfits, TBYTE, "LOC_FLGS", (void **) &lflags); 
+  for (i=0;i<npts;i++){
+    if (sel1>1){
+      if (sel2==1){
+	tflags[i]=(tflags[i])^sel1;
+      } else if (sel2==2){
+	tflags[i]=(tflags[i])&(~sel1);
+      }
+    }
+	
+    switch(daynight[0]) {
+    case 'D':
+      time_test=tflags[i]^TEMPORAL_DAY;
+      break;
+    case 'N':
+      time_test=tflags[i];
+      break;
+    default:
+      time_test=tflags[i]&(~TEMPORAL_DAY);
+    }
+      
+    if (lflags[i]&LOCATION_PHA){
+      nbadpha++;
+    } 
+    
+    if ((lflags[i]&~LOCATION_AIR) || (time_test)) {
+      nbadevnt++;
+    }   
+  }
+
+  if ((sel1>1)&&(sel2>0)){
+    cf_write_col(outfits, TBYTE, "TIMEFLGS", (void *) tflags, npts);  
+  }
+
+  free(tflags);
+  free(lflags);
+
+
+  FITS_movabs_hdu(infits,3,&hdutype,&status);
+  FITS_create_hdu(outfits,&status);
+  FITS_copy_hdu(infits,outfits,0,&status);
+  
+
+  FITS_movabs_hdu(infits,4,&hdutype,&status);
+  FITS_create_hdu(outfits,&status);
+  FITS_copy_hdu(infits,outfits,0,&status);
+
+ 
+  npts = cf_read_col(outfits, TBYTE, "STATUS_FLAGS", (void **) &tflags);  
+    
+  for (i=0;i<npts;i++){
+    if (sel1>1){
+      if (sel2==1){
+	tflags[i]=(tflags[i])^sel1;
+      } else if (sel2==2){
+	tflags[i]=(tflags[i])&(~sel1);
+      }
+    }
+
+    switch(daynight[0]) {
+    case 'D':
+      time_test=tflags[i]^TEMPORAL_DAY;
+      break;
+    case 'N':
+      time_test=tflags[i];
+      break;
+    default:
+      time_test=tflags[i]&(~TEMPORAL_DAY);
+    }
+
+    
+    if (time_test==0) {
+      
+      exptime+=1.0;
+      
+      if (!(tflags[i] & TEMPORAL_DAY))
+	expnight+=1.0;
+      
+    } else {
+      
+      exp_bad+=1.0;
+      
+      if (tflags[i] & TEMPORAL_BRST)
+	exp_brst+=1.0;
+      
+      if (tflags[i] & TEMPORAL_HV)
+	exp_hv=+1.0;	
+      
+      if (tflags[i] & TEMPORAL_JITR)
+	exp_jitr=+1.0;
+      
+      if (tflags[i] & TEMPORAL_LIMB)
+	exp_lim=+1.0;
+      
+      if (tflags[i] & TEMPORAL_SAA)
+	exp_saa=+1.0;
+    }
+
+  }
+
+ if ((sel1>1)&&(sel2>0)){
+  cf_write_col(outfits, TBYTE, "STATUS_FLAGS", (void *) tflags, npts);  
+ }
+ 
+ free(tflags);
+  
+ /* Update Main Header Keyword */
+ FITS_movabs_hdu(outfits,1,&hdutype,&status);  
+ 
+ FITS_update_key(outfits,TDOUBLE ,"EXPTIME"  ,&exptime   ,NULL,&status);	
+ FITS_update_key(outfits,TLONG   ,"NBADEVNT" ,&nbadevnt  ,NULL,&status);
+ FITS_update_key(outfits,TLONG   ,"NBADPHA"  ,&nbadpha   ,NULL,&status);
+ FITS_update_key(outfits,TDOUBLE ,"EXP_BAD"  ,&exp_bad   ,NULL,&status);
+ FITS_update_key(outfits,TDOUBLE ,"EXP_SAA"  ,&exp_saa   ,NULL,&status);
+ FITS_update_key(outfits,TDOUBLE ,"EXP_LIM"  ,&exp_lim   ,NULL,&status);
+ FITS_update_key(outfits,TDOUBLE ,"EXP_BRST" ,&exp_brst  ,NULL,&status);		
+ FITS_update_key(outfits,TDOUBLE ,"EXP_JITR" ,&exp_jitr  ,NULL,&status);
+ FITS_update_key(outfits,TDOUBLE ,"EXPNIGHT" ,&expnight  ,NULL,&status);
+
+ cf_verbose(1,"CLOSING INPUT FILE");
+ FITS_close_file(infits,&status);
+ 
+ cf_verbose(1,"CLOSING OUTPUT FILE");
+ FITS_close_file(outfits,&status);
+  
+ 
+ cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished execution.");
+ return EXIT_SUCCESS;
+  
+}
+
+
diff --git a/src/analysis/mjd2hjd.c b/src/analysis/mjd2hjd.c
new file mode 100644
index 0000000..e0ecd18
--- /dev/null
+++ b/src/analysis/mjd2hjd.c
@@ -0,0 +1,129 @@
+
+/*****************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *****************************************************************************
+ *
+ * 
+ *
+ * Usage:
+ *     mjd2hjd [-h] [-v level] mjd ra_h ra_m ra_s dec_d dec_m dec_s
+ *
+ *
+ * Arguments:
+ *       mjd                               :  Modified Julian Day
+ *       ra_h ra_m ra_s dec_d dec_m dec_s  :  RA and DEC of target : hh mm ss.s dd mm ss.s
+ * 
+ *
+ * Options:
+ *     -h:  this help message
+ *     -v:  verbosity level (=1; 0 is silent)
+ *
+ *
+ *
+ *
+ *
+ * History:	10/06/04	bjg	v1.0	      
+ *       	10/26/04	bjg	v1.1    Cosmetic change
+ *
+ ****************************************************************************/
+
+
+
+#include <stdlib.h>
+#include <stdio.h>
+#include <string.h>
+#include <time.h>
+#include <unistd.h>
+#include <math.h>
+
+#include "calfuse.h"
+
+
+
+#define SECONDS_PER_DAY (24.0*3600.0)
+
+static char CF_PRGM_ID[]= "mjd2hjd";
+static char CF_VER_NUM[]= "1.1";
+
+
+double gethmjd(double, int, int, float, int, int, float);
+
+int main(int argc,char *argv[]){
+  
+  int optc;
+
+
+
+  double     lighttime;
+  double     jd, mjd, hjd, hmjd;
+
+  int        rah,ram,decd,decm;
+  float      ras,decs;
+ 
+
+  char opts[] = "hv:";
+  char usage[] = 
+    "Usage:\n"
+    "  mjd2hjd [-h] [-v level] mjd ra_h ra_m ra_s dec_d dec_m dec_s\n";
+  char argument[] =
+    "Arguments:\n"  
+    "    mjd                               :  Modified Julian Day.\n"
+    "    ra_h ra_m ra_s dec_d dec_m dec_s  :  RA and DEC of target.\n";
+  char option[] =
+    "Options:\n"
+    "  -h:  this help message\n"
+    "  -v:  verbosity level (=1; 0 is silent)\n";
+  verbose_level = 1;
+  
+  
+  /* Check number of options and arguments */
+  while ((optc = getopt(argc, argv, opts)) != -1) {
+    switch(optc) {
+      
+    case 'h':
+      printf("%s\n%s\n%s", usage, argument, option);
+      return EXIT_SUCCESS;
+    case 'v':
+      verbose_level = atoi(optarg);
+      break;
+    }
+  }
+
+  /* Initialize error checking. */
+  cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+  if (argc != optind+7)
+    cf_if_error("%s\nIncorrect number of program arguments", usage);
+  
+  
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Started execution.");
+  
+  sscanf(argv[optind],"%lf",&mjd);
+  sscanf(argv[optind+1],"%d",&rah);
+  sscanf(argv[optind+2],"%d",&ram);  
+  sscanf(argv[optind+3],"%f",&ras);
+  sscanf(argv[optind+4],"%d",&decd);
+  sscanf(argv[optind+5],"%d",&decm);
+  sscanf(argv[optind+6],"%f",&decs);
+
+ 
+  hmjd=gethmjd(mjd,rah,ram,ras,decd,decs,decm);
+
+  jd   = mjd  + 2400000.5;
+  hjd  = hmjd + 2400000.5;
+
+  lighttime=(hmjd-mjd)*SECONDS_PER_DAY;
+
+  cf_verbose(1,"Right Ascension of target: %d h %d m %f s",rah,ram,ras);
+  cf_verbose(1,"Declination of target: %d deg %d m %f s",decd,decm,decs);
+  cf_verbose(1,"jd= %lf",jd);
+  cf_verbose(1,"mjd= %lf",mjd);
+  cf_verbose(1,"hjd= %lf",hjd);
+  cf_verbose(1,"hmjd= %lf",hmjd);
+  cf_verbose(1,"heliocentric light time correction = %lf s",lighttime);
+  cf_verbose(1,"---positive when Earth is closer to target than Sun");
+  return EXIT_SUCCESS;
+
+}
+
diff --git a/src/analysis/modhead.c b/src/analysis/modhead.c
new file mode 100644
index 0000000..0ffc40b
--- /dev/null
+++ b/src/analysis/modhead.c
@@ -0,0 +1,114 @@
+/*****************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *****************************************************************************
+ *
+ * Synopsis:	modhead file.fit[ext] KEYWORD NEW_VALUE
+ *
+ * Description: Returns or modifies the value of a header keyword.
+ *		If NEW_VALUE is not specified, current value of KEYWORD is
+ *		returned.  If KEYWORD is not found and NEW_VALUE is given,
+ *		KEYWORD is added to header.  If an extension beyond the
+ *		primary HDU is requested, file name must be given in
+ *		parentheses: "file.fit[3]" or an alternate construction
+ *		used: file.fit+3   Note that the primary HDU is extension 0.
+ *
+ * History:     05/15/05        tc	started work
+ *		08/30/05	wvd	Allow multi-word strings.
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include <stdio.h>
+#include "fitsio.h"
+
+int main(int argc, char *argv[])
+{
+    fitsfile *fptr;         /* FITS file pointer, defined in fitsio.h */
+    char card[FLEN_CARD], newcard[FLEN_CARD];
+    char oldvalue[FLEN_VALUE], comment[FLEN_COMMENT];
+    int status = 0;   /*  CFITSIO status value MUST be initialized to zero!  */
+    int i, iomode, keytype;
+
+    if (argc == 3) 
+      iomode = READONLY;
+    else if (argc >= 4)
+      iomode = READWRITE;
+    else if (argc < 3) {
+      printf("Usage:  modhead filename[ext] keyword new_value\n");
+      printf("\n");
+      printf("Write or modify the value of a header keyword.\n");
+      printf("If 'newvalue' is not specified, then just print \n");
+      printf("the current value. \n");
+      printf("\n");
+      printf("Examples: \n");
+      printf("  modhead file.fits dec      - list the DEC keyword \n");
+      printf("  modhead file.fits dec 30.0 - set DEC = 30.0 \n");
+      printf("\n");
+      printf("  modhead \"file.fits[2]\" OBSTIME  - list OBSTIME from extention 2 \n");
+      printf("  modhead file.fits+2 OBSTIME     - list OBSTIME from extention 2\n");
+      return(0);
+    }
+
+    if (!fits_open_file(&fptr, argv[1], iomode, &status))
+    {
+      if (fits_read_card(fptr,argv[2], card, &status))
+      {
+        printf("Keyword does not exist\n");
+        card[0] = '\0';
+        comment[0] = '\0';
+        status = 0;  /* reset status after error */
+      }
+      else
+        printf("%s\n",card);
+
+      if (argc >= 4)  /* write or overwrite the keyword */
+      {
+          /* check if this is a protected keyword that must not be changed */
+          if (*card && fits_get_keyclass(card) == TYP_STRUC_KEY)
+          {
+            printf("Protected keyword cannot be modified.\n");
+          }
+          else
+          {
+            /* get the comment string */
+            if (*card)fits_parse_value(card, oldvalue, comment, &status);
+
+            /* construct template for new keyword */
+            strcpy(newcard, argv[2]);     /* copy keyword name */
+            strcat(newcard, " = ");       /* '=' value delimiter */
+	    if (argc == 4) strcat(newcard, argv[3]);     /* new value */
+	    else {
+                strcat(newcard, "'");
+	        for (i = 3; i < argc-1; i++) {
+                    strcat(newcard, argv[i]);     /* new value */
+                    strcat(newcard, " ");
+		}
+                strcat(newcard, argv[i]);     /* new value */
+                strcat(newcard, "'");
+	    }
+
+            if (*comment) {
+              strcat(newcard, " / ");  /* comment delimiter */
+              strcat(newcard, comment);     /* append the comment */
+            }
+
+            /* reformat the keyword string to conform to FITS rules */
+            fits_parse_template(newcard, card, &keytype, &status);
+
+            /* overwrite the keyword with the new value */
+            fits_update_card(fptr, argv[2], card, &status);
+
+            printf("Keyword has been changed to:\n");
+            printf("%s\n",card);
+          }
+      }  /* if argc == 4 */
+      fits_close_file(fptr, &status);
+    }    /* open_file */
+
+    /* if error occured, print out error message */
+    if (status) fits_report_error(stderr, status);
+    return(status);
+}
+
diff --git a/src/analysis/remove_target_orbital_motion.c b/src/analysis/remove_target_orbital_motion.c
new file mode 100644
index 0000000..d104b0d
--- /dev/null
+++ b/src/analysis/remove_target_orbital_motion.c
@@ -0,0 +1,503 @@
+
+/*****************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *****************************************************************************
+ *
+ * 
+ *
+ * Usage:
+ *     remove_target_orbital_motion [-hb] [-v level]
+ *                                   input_idf_file output_idf_file
+ *                                   hjd0 period vrmax
+ *                                   [ra_h ra_m ra_s dec_d dec_m dec_s]
+ *
+ * Arguments:
+ *       mjd0                              :  Heliocentric or Geocentric
+ *                                            Julian Day 
+ *                                            of closest approch on orbit.
+ *       period                            :  Period in seconds.
+ *       vrmax                             :  Maximum radial velocity in km/s
+ *       ra_h ra_m ra_s dec_d dec_m dec_s  :  (Optional) RA and DEC of target.
+ *                                            If present mjd0 is interpreted 
+ *                                            as Heliocentric.
+ *
+ * Options:
+ *     -h:  this help message
+ *     -v:  verbosity level (=1; 0 is silent)
+ *     -b:  update timeline doppler information (required for BPM)
+ *
+ *
+ * History:	12/01/03	bjg	v1.0	Begin work.
+ *              12/02/03        bjg             Changed calling 
+ *                                              parameters format.        	
+ *              12/04/03        bjg             Number of elements in HDU2 
+ *                                              is now determined from HDU2 
+ *                                              header instead of HDU1 
+ *                                              header NEVENTS keyword
+ *              12/10/03        bjg		Updated header.
+ *              04/05/04        bjg             Remove unused variables  
+ *              06/10/04        bjg             Some code cleaning    
+ *              10/07/04        bjg     v1.1    Added heliocentric
+ *                                              time correction (optional)
+ *                                              Added timeline doppler
+ *                                              correction information
+ *                                              (optional) for cf_bad_pixels 
+ *              10/26/04        bjg     v1.2    Cosmetic change
+ *
+ ****************************************************************************/
+
+
+
+#include <stdlib.h>
+#include <stdio.h>
+#include <string.h>
+#include <time.h>
+#include <unistd.h>
+#include <math.h>
+
+#include "calfuse.h"
+
+
+
+
+#define LIGHT_SPEED 299792.458 /* speed of light in kilometers per second */
+#define SECONDS_PER_DAY (24.0*3600.0)
+
+static char CF_PRGM_ID[]= "remove_target_orbital_motion";
+static char CF_VER_NUM[]= "1.2";
+
+struct key {
+  char keyword[FLEN_KEYWORD];
+  float value;
+};
+
+
+double gethmjd(double, int, int, float, int, int, float);
+
+int main(int argc,char *argv[]){
+  
+ 
+  char     fmt_byte[FLEN_CARD],fmt_float[FLEN_CARD],fmt_short[FLEN_CARD];  
+  
+  fitsfile * infits;
+  fitsfile * outfits; 
+
+  char       input_filename[FLEN_CARD],output_filename[FLEN_CARD];  
+  char *     corrected_filename;
+  char *     string_pointer;
+
+  int        intnull=0,anynull;
+  int        status=0;
+  int        hdutype=0;
+  int        ncol;
+  char       tempstring[FLEN_CARD]; 
+  char       tempchar;
+  char       keyword[FLEN_CARD],card[FLEN_CARD];
+ 
+
+  struct key hdu4_tscal[16];
+  struct key hdu4_tzero[16];
+  
+  char hdu4_extname[]="TIMELINE";
+  int hdu4_tfields=16;  /* output table will have 16 columns */
+  char *hdu4_ttype[]={"TIME", "STATUS_FLAGS", "TIME_SUNRISE", "TIME_SUNSET",
+		      "LIMB_ANGLE", "LONGITUDE", "LATITUDE", "ORBITAL_VEL",
+		      "HIGH_VOLTAGE", "LIF_CNT_RATE", "SIC_CNT_RATE",
+		      "FEC_CNT_RATE", "AIC_CNT_RATE", "BKGD_CNT_RATE",
+		      "YCENT_LIF","YCENT_SIC"};
+
+  char *hdu4_tform[16]; /* we will define tform later, when the number
+			   of photons is known */
+  
+  char *hdu4_tunit[]={"seconds", "unitless", "seconds", "seconds", "degrees",
+		      "degrees", "degrees",  "km/s", "unitless", "counts/sec",
+		      "counts/sec", "counts/sec", "counts/sec", "counts/sec",
+		      "pixels","pixels" };
+
+
+  long       nevents, nrecords;
+  long       i;
+
+  float *    floatlist;
+  short *    shortlist;
+  char  *    charlist;
+
+  double *    hdu4_time;
+  double *    hdu4_orbvel;
+
+  double *    hdu2_time;
+  double *    hdu2_lambda;
+
+  double      delta_t;
+  double      period, vrmax, mjd0;
+  double      expstart, mjd;
+ 
+  int        rah,ram,decd,decm;
+  float      ras,decs;
+
+  int        optc;
+
+  char opts[] = "hbv:";
+
+  char usage[] = 
+    "Usage:\n"
+    "  remove_target_orbital_motion [-hb] [-v level] \n"
+    "    input_idf_file output_idf_file\n" 
+    "    mjd0 period vrmax\n"
+    "    [ra_h ra_m ra_s dec_d dec_m dec_s]\n";
+  char argument[] =
+    "Arguments:\n"
+    "    mjd0      :  (Geocentric or Heliocentric) Modified Julian Day\n"
+    "                 of closest approch on orbit.\n"
+    "    period    :  Period in seconds.\n"
+    "    vrmax     :  Maximum radial velocity in km/s\n"
+    "    ra_h ra_m ra_s dec_d dec_m dec_s  :  Optional RA and DEC of target.\n" 
+    "                                         If present mjd0 is interpreted\n"
+    "                                         as Heliocentric. \n";
+
+  char option[] =
+    "Options:\n"
+    "  -h:  this help message\n"
+    "  -v:  verbosity level (=1; 0 is silent)\n"
+    "  -b:  update timeline doppler information (required for BPM)\n";
+  
+  
+  
+  int        bigtime=1; /* How to store TSUNRISE and TSUNSET" */
+  int        do_timeline=0;
+  int        helio_corr=0;
+  
+  verbose_level = 1;
+ 
+  
+  /* Check number of options and arguments */
+  while ((optc = getopt(argc, argv, opts)) != -1) {
+    switch(optc) {
+    case 'h':
+      printf("%s\n%s\n%s", usage, argument, option);
+      return EXIT_SUCCESS;
+    case 'v':
+      verbose_level = atoi(optarg);
+      break; 
+    case 'b':
+      do_timeline=1;
+      break;
+    }
+  }
+
+  /* Initialize error checking. */
+  cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+  if ((argc != optind+11)&&(argc != optind+5))
+    cf_if_error("%s\nIncorrect number of program arguments", usage);
+  
+  if (argc==optind+11) helio_corr=1;
+  
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Started execution.");
+  
+  strcpy(input_filename,argv[optind]);
+  strcpy(output_filename,argv[optind+1]);
+
+  sscanf(argv[optind+2],"%lf",&mjd0);
+  sscanf(argv[optind+3],"%lf",&period);
+  sscanf(argv[optind+4],"%lf",&vrmax);  
+  
+  cf_verbose(1,"Target Orbital Motion Doppler Correction");
+  cf_verbose(1,"Processing file %s",input_filename);
+  
+  if (helio_corr) {
+    sscanf(argv[optind+5],"%d",&rah);
+    sscanf(argv[optind+6],"%d",&ram);  
+    sscanf(argv[optind+7],"%f",&ras);
+    sscanf(argv[optind+8],"%d",&decd);
+    sscanf(argv[optind+9],"%d",&decm);
+    sscanf(argv[optind+10],"%f",&decs);
+    cf_verbose(1,"Right Ascension of target: %d h %d m %f s",rah,ram,ras);
+    cf_verbose(1,"Declination of target: %d deg %d m %f s",decd,decm,decs);
+    cf_verbose(1,"Heliocentric Modified Julian Day of closest approch on orbit: %lf",mjd0);
+  } else {
+    cf_verbose(1,"Geocentric Modified Julian Day of closest approch on orbit: %lf",mjd0);
+  }
+  
+  cf_verbose(1,"Period in seconds: %lf",period);
+  cf_verbose(1,"Maximum radial velocity in kilometers per second: %lf",vrmax);
+  
+  
+
+  FITS_open_file(&infits,input_filename,READONLY,&status);
+  FITS_read_key(infits,TDOUBLE,"EXPSTART",&(expstart),NULL,&status);
+   
+  FITS_create_file(&outfits,output_filename,&status);
+  FITS_copy_hdu(infits,outfits,0,&status);
+  
+  string_pointer=strrchr(output_filename,'/');
+  if (string_pointer==NULL) corrected_filename=output_filename;
+  else corrected_filename=&(string_pointer[1]);
+    
+  FITS_update_key(outfits,TSTRING,"FILENAME",corrected_filename,NULL,&status);
+
+  strcpy(tempstring,"");
+
+  FITS_update_key(outfits,TSTRING,"BPM_CAL",tempstring,NULL,&status);
+
+  
+  
+  FITS_movabs_hdu(infits,2,&hdutype,&status);
+  FITS_read_key(infits,TSTRING,"TFORM1",tempstring,NULL,&status);
+  sscanf(tempstring,"%ld%c",&nevents,&tempchar);
+
+  FITS_create_hdu(outfits,&status);
+  FITS_copy_hdu(infits,outfits,0,&status);
+  
+  
+  hdu2_time=(double *)malloc(nevents*sizeof(double));
+  hdu2_lambda=(double *)malloc(nevents*sizeof(double));
+
+    
+   
+  FITS_get_colnum(infits, TRUE, "TIME", &ncol, &status);
+  FITS_read_col(infits, TDOUBLE, ncol, 1, 1, nevents, &intnull,
+		hdu2_time, &anynull, &status);
+ 
+  FITS_get_colnum(infits, TRUE, "LAMBDA", &ncol, &status);
+  FITS_read_col(infits, TDOUBLE, ncol, 1, 1, nevents, &intnull,
+		hdu2_lambda, &anynull, &status);
+
+ 
+		
+  
+  cf_verbose(1,"Geocentric Modified Julian Day of start of observation/exposure is: %f",expstart);
+  if (helio_corr) {
+    mjd=gethmjd(expstart,rah,ram,ras,decd,decm,decs);
+    cf_verbose(1,"Heliocentric Modified Julian Day of start of observation/exposure is: %f",mjd);
+  }
+
+  for (i=0;i<nevents;i++){
+    
+    mjd=expstart+(hdu2_time[i])/SECONDS_PER_DAY;
+
+    if (helio_corr) mjd=gethmjd(mjd,rah,ram,ras,decd,decm,decs);
+      
+    delta_t=(mjd-mjd0)*SECONDS_PER_DAY;
+
+    hdu2_lambda[i]=hdu2_lambda[i]*(1-(vrmax/LIGHT_SPEED)*sin(2*M_PI*delta_t/period));        
+
+  }
+
+  FITS_get_colnum(outfits, TRUE, "LAMBDA", &ncol, &status);
+  FITS_write_col(outfits, TDOUBLE, ncol, 1, 1, nevents, hdu2_lambda, &status);
+
+
+  free(hdu2_time);
+  free(hdu2_lambda);
+
+   
+  FITS_movabs_hdu(infits,3,&hdutype,&status);
+  FITS_create_hdu(outfits,&status);
+  FITS_copy_hdu(infits,outfits,0,&status);
+  
+
+  FITS_movabs_hdu(infits,4,&hdutype,&status);
+  
+  if (do_timeline) {	
+
+    FITS_read_key(infits,TSTRING,"TFORM1",tempstring,NULL,&status);
+    sscanf(tempstring,"%ld%c",&nrecords,&tempchar);		
+
+    /* Generate the tform array */
+    sprintf(fmt_byte,  "%ldB", nrecords);
+    sprintf(fmt_float, "%ldE", nrecords);
+    sprintf(fmt_short, "%ldI", nrecords);
+  
+  
+  
+    hdu4_tform[0] = fmt_float;
+    hdu4_tform[1] = fmt_byte;
+
+    for (i=2; i<hdu4_tfields; i++)	hdu4_tform[i] = fmt_short;
+  
+    /* Set TSCALE and TZERO values */
+    /* Not all of these will be used; see below. */
+    for (i=2; i<hdu4_tfields; i++) {
+      sprintf(hdu4_tscal[i].keyword, "TSCAL%ld", i+1);
+      hdu4_tscal[i].value = 0.1;
+      sprintf(hdu4_tzero[i].keyword, "TZERO%ld", i+1);
+      hdu4_tzero[i].value = 0.;
+    }
+  
+    /* Need TZEROn = 3000. for tsunrise and tsunset. */
+    hdu4_tzero[2].value = hdu4_tzero[3].value = 3000.;
+
+    /* Let's keep three significant figures for vorb. */
+    hdu4_tscal[7].value = 0.01;
+
+    /* FEC_CNT_RATE and AIC_CNT_RATE can get big, so we
+       (essentially) store them as unsigned shorts. */
+    hdu4_tscal[11].value = 1;
+    hdu4_tscal[12].value = 1;
+    hdu4_tzero[11].value = 32768;
+    hdu4_tzero[12].value = 32768;
+    
+  
+    if (bigtime) { 
+      hdu4_tform[2]=hdu4_tform[3]=fmt_float; 
+    }
+
+    hdu4_tform[7]=fmt_float;
+	
+    /* Append a new empty binary table to the output file */
+    FITS_create_tbl(outfits, BINARY_TBL, 1, hdu4_tfields, hdu4_ttype, hdu4_tform,
+		    hdu4_tunit, hdu4_extname, &status);
+
+  
+	
+    /* Write TSCALE and TZERO entries to header */
+    for (i=2; i<hdu4_tfields; i++) {
+
+      /* If bigtime is TRUE, store tsunrise and tsunset as floats.*/
+      if ((i == 2 || i == 3) && bigtime) continue;
+    
+      /* Omit TSCALE and TZERO for these four arrays. */
+      if (i ==  8) continue;	/* HIGH_VOLTAGE */
+      if (i ==  9) continue;	/* LIF_CNT_RATE */
+      if (i == 10) continue;	/* SIC_CNT_RATE */
+      if (i == 13) continue;	/* BKGD_CNT_RATE */
+
+
+      /* Store ORBITAL_VEL as float */
+      if (i == 7) continue;
+
+
+      sprintf(keyword, "TUNIT%ld", i+1);
+      if (fits_read_keyword(outfits, keyword, card, NULL, &status))
+	cf_if_fits_error(status);
+      FITS_insert_key_flt(outfits, hdu4_tscal[i].keyword, hdu4_tscal[i].value,
+			  -1, NULL, &status);
+      FITS_insert_key_flt(outfits, hdu4_tzero[i].keyword, hdu4_tzero[i].value,
+			  -5, NULL, &status);
+    
+    } 
+  
+    floatlist=(float *)malloc(nrecords*sizeof(float));
+    shortlist=(short *)malloc(nrecords*sizeof(short));
+    charlist=(char *)malloc(nrecords*sizeof(char));
+    hdu4_time=(double *)malloc(nevents*sizeof(double));
+    hdu4_orbvel=(double *)malloc(nevents*sizeof(double));
+  
+    FITS_get_colnum(infits, TRUE, "TIME", &ncol, &status);
+    FITS_read_col(infits, TDOUBLE, ncol, 1, 1, nrecords, &intnull,
+		  hdu4_time, &anynull, &status);	
+    FITS_write_col(outfits, TDOUBLE, 1, 1, 1, nrecords, hdu4_time, &status);
+  
+    FITS_get_colnum(infits, TRUE, "STATUS_FLAGS", &ncol, &status);
+    FITS_read_col(infits, TBYTE, ncol, 1, 1, nrecords, &intnull,
+		  charlist, &anynull, &status);
+    FITS_write_col(outfits, TBYTE, 2, 1, 1, nrecords, charlist, &status);
+  
+    FITS_get_colnum(infits, TRUE, "TIME_SUNRISE", &ncol, &status);
+    FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecords, &intnull,
+		  floatlist, &anynull, &status);
+    FITS_write_col(outfits, TFLOAT, 3, 1, 1, nrecords, floatlist, &status);
+  
+    FITS_get_colnum(infits, TRUE, "TIME_SUNSET", &ncol, &status);
+    FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecords, &intnull,
+		  floatlist, &anynull, &status);
+    FITS_write_col(outfits, TFLOAT, 4, 1, 1, nrecords, floatlist, &status);
+  
+    FITS_get_colnum(infits, TRUE, "LIMB_ANGLE", &ncol, &status);
+    FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecords, &intnull,
+		  floatlist, &anynull, &status);
+    FITS_write_col(outfits, TFLOAT, 5, 1, 1, nrecords, floatlist, &status);
+  
+    FITS_get_colnum(infits, TRUE, "LONGITUDE", &ncol, &status);
+    FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecords, &intnull,
+		  floatlist, &anynull, &status);
+    FITS_write_col(outfits, TFLOAT, 6, 1, 1, nrecords, floatlist, &status);
+  
+    FITS_get_colnum(infits, TRUE, "LATITUDE", &ncol, &status);
+    FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecords, &intnull,
+		  floatlist, &anynull, &status);
+    FITS_write_col(outfits, TFLOAT, 7, 1, 1, nrecords, floatlist, &status);
+    
+    FITS_get_colnum(infits, TRUE, "ORBITAL_VEL", &ncol, &status);
+    FITS_read_col(infits, TDOUBLE, ncol, 1, 1, nrecords, &intnull,
+		  hdu4_orbvel, &anynull, &status);
+
+    for (i=0;i<nrecords;i++){
+    
+      mjd=expstart+(hdu4_time[i])/SECONDS_PER_DAY;
+
+      if (helio_corr) mjd=gethmjd(mjd,rah,ram,ras,decd,decm,decs);
+      
+      delta_t=(mjd-mjd0)*SECONDS_PER_DAY;
+
+      hdu4_orbvel[i]=hdu4_orbvel[i]-vrmax*sin(2*M_PI*delta_t/period);        
+
+    }
+
+
+    FITS_write_col(outfits, TDOUBLE, 8, 1, 1, nrecords, hdu4_orbvel, &status);
+    
+    FITS_get_colnum(infits, TRUE, "HIGH_VOLTAGE", &ncol, &status);
+    FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecords, &intnull,
+		  floatlist, &anynull, &status);
+    FITS_write_col(outfits, TFLOAT, 9, 1, 1, nrecords, floatlist, &status);
+    
+    FITS_get_colnum(infits, TRUE, "LIF_CNT_RATE", &ncol, &status);
+    FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecords, &intnull,
+		  floatlist, &anynull, &status);
+    FITS_write_col(outfits, TFLOAT, 10, 1, 1, nrecords, floatlist, &status);
+    
+    FITS_get_colnum(infits, TRUE, "SIC_CNT_RATE", &ncol, &status);
+    FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecords, &intnull,
+		  floatlist, &anynull, &status);
+    FITS_write_col(outfits, TFLOAT, 11, 1, 1, nrecords, floatlist, &status);
+		
+    FITS_get_colnum(infits, TRUE, "FEC_CNT_RATE", &ncol, &status);
+    FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecords, &intnull,
+		  floatlist, &anynull, &status);
+    FITS_write_col(outfits, TFLOAT, 12, 1, 1, nrecords, floatlist, &status);
+    
+    FITS_get_colnum(infits, TRUE, "AIC_CNT_RATE", &ncol, &status);
+    FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecords, &intnull,
+		  floatlist, &anynull, &status);
+    FITS_write_col(outfits, TFLOAT, 13, 1, 1, nrecords, floatlist, &status);
+    
+    FITS_get_colnum(infits, TRUE, "BKGD_CNT_RATE", &ncol, &status);
+    FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecords, &intnull,
+		  floatlist, &anynull, &status);	      
+    FITS_write_col(outfits, TFLOAT, 14, 1, 1, nrecords, floatlist, &status);
+    
+    FITS_get_colnum(infits, TRUE, "YCENT_LIF", &ncol, &status);
+    FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecords, &intnull,
+		  floatlist, &anynull, &status);
+    FITS_write_col(outfits, TFLOAT, 15, 1, 1, nrecords, floatlist, &status);
+    
+    FITS_get_colnum(infits, TRUE, "YCENT_SIC", &ncol, &status);
+    FITS_read_col(infits, TFLOAT, ncol, 1, 1, nrecords, &intnull,
+		  floatlist, &anynull, &status);
+    FITS_write_col(outfits, TFLOAT, 16, 1, 1, nrecords, floatlist, &status);
+    
+    
+    free(hdu4_time);
+    free(hdu4_orbvel);
+    
+    free(floatlist);
+    free(charlist);
+    free(shortlist);
+
+  } else {
+    FITS_create_hdu(outfits,&status);
+    FITS_copy_hdu(infits,outfits,0,&status);
+  }
+       
+  FITS_close_file(infits,&status);
+  FITS_close_file(outfits,&status);	
+    
+
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished execution.");
+  return EXIT_SUCCESS;
+  
+}
+
diff --git a/src/analysis/ttag_combine.c b/src/analysis/ttag_combine.c
new file mode 100644
index 0000000..77da230
--- /dev/null
+++ b/src/analysis/ttag_combine.c
@@ -0,0 +1,520 @@
+/*****************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *****************************************************************************
+ *
+ * Synopsis:	ttag_combine outfile file1 file2 file3 file4 file5 ...
+ *
+ * Description: Reads multiple contiguous ttag files and concatenates them 
+ *              into a single file.  For now, the input files should be
+ *              listed in time order.
+ *
+ * History:	08/16/99	emurphy	 Begin work
+ *              08/27/99        emurphy  Added comments.  Good time intervals
+ *                                       now match observing times.
+ *              10/09/99        emurphy  exptime now sum of individual exptimes
+ *              08/20/01 v1.2	wvd	 Complain if FPA moves between exposures.
+ *					 Set MAXGTI = 2000.
+ *              10/01/01 v1.3   RDR      Update all segment and active image counters
+ *                                       DATE keyword now contains the date 
+ *                                       NEVENTS reflects total number of events in
+ *                                         combined file
+ *                                       EXP_ID defaults to 999 to signify combined
+ *                                         data
+ *                                       Print warning if FPA x position changes
+ *                                         by more than 30 microns
+ *                                       PLANTIME now reflects total planned exposure
+ *                                       Will transfer DX, DY and DNFLG columns
+ *                                         if available 
+ *              10/09/01 v1.4	wvd	 Delete redundant check for FPA splits.
+ *					 Program complains if input files not in
+ *					 time order.
+ *              01/15/02 v1.5	wvd	 Update keyword EXPNIGHT.
+ *              02/13/02 v1.6	wvd	 Respond gracefully if EXPNIGHT does not exist.
+ *              02/20/02     	wvd	 Update keyword RAWTIME, if it exists.
+ *              04/26/02 v1.7	wvd	 Change vtime to type time_t
+ *              12/11/02 v1.8	wvd	 Change EXPNIGHT to type long
+ *              02/20/03 v1.9   wvd      Correct errors in pointer use.
+ *					 Change abs() to fabs().
+ *              03/22/04 v1.10  bjg      Change cf_fpa_pos() to cf_read_fpa_pos()
+ *              04/05/04 v1.11  bjg      Include math.h
+ *                                       Remove unused variables
+ *                                       Change formats to match arg type
+ *                                       in printf
+ *
+ *                                       
+ ****************************************************************************/
+
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include <time.h>
+#include <math.h>
+#include "calfuse.h"
+
+static char CF_PRGM_ID[] = "ttag_combine";
+static char CF_VER_NUM[] = "1.11";
+
+#define MAXGTI          2000      /*  Maximum number of good time intervals */
+
+static int 
+cf_dtcor_read_counters(fitsfile *infits, long *de, long *fe, long *ai1a,
+   long *ai1b, long *ai2a, long *ai2b, long *sic, long *lif, long *as,
+   double *ctm )
+{
+    char cntstr[FLEN_CARD], detstr[FLEN_CARD];
+    long de_b, de_e, fe_b, fe_e;
+    long ai1a_b, ai1a_e, ai1b_b, ai1b_e, ai2a_b, ai2a_e, ai2b_b, ai2b_e ;
+    long sic_b, sic_e, lif_b, lif_e, as_b, as_e ;
+    double ctm_b, ctm_e ;
+    int status=0;
+
+    FITS_read_key(infits, TSTRING, "DETECTOR", detstr, NULL, &status);
+
+    /* Segment 1A Counters */
+
+    sprintf(cntstr, "%1.1s%2.2s%4.4s","C",detstr,"DE_B");
+    FITS_read_key(infits, TLONG, cntstr, &de_b, NULL, &status);
+
+    sprintf(cntstr, "%1.1s%2.2s%4.4s","C",detstr,"DE_E");
+    FITS_read_key(infits, TLONG, cntstr, &de_e, NULL, &status);
+
+    sprintf(cntstr, "%1.1s%2.2s%4.4s","C",detstr,"FE_B");
+    FITS_read_key(infits, TLONG, cntstr, &fe_b, NULL, &status);
+
+    sprintf(cntstr, "%1.1s%2.2s%4.4s","C",detstr,"FE_E");
+    FITS_read_key(infits, TLONG, cntstr, &fe_e, NULL, &status);
+
+    sprintf(cntstr, "%1.1s%2.2s%5.5s","C",detstr,"SIC_B");
+    FITS_read_key(infits, TLONG, cntstr, &sic_b, NULL, &status);
+
+    sprintf(cntstr, "%1.1s%2.2s%5.5s","C",detstr,"SIC_E");
+    FITS_read_key(infits, TLONG, cntstr, &sic_e, NULL, &status);
+
+    sprintf(cntstr, "%1.1s%2.2s%5.5s","C",detstr,"LIF_B");
+    FITS_read_key(infits, TLONG, cntstr, &lif_b, NULL, &status);
+
+    sprintf(cntstr, "%1.1s%2.2s%5.5s","C",detstr,"LIF_E");
+    FITS_read_key(infits, TLONG, cntstr, &lif_e, NULL, &status);
+
+    sprintf(cntstr, "%1.1s%2.2s%4.4s","C",detstr,"AS_B");
+    FITS_read_key(infits, TLONG, cntstr, &as_b, NULL, &status);
+
+    sprintf(cntstr, "%1.1s%2.2s%4.4s","C",detstr,"AS_E");
+    FITS_read_key(infits, TLONG, cntstr, &as_e, NULL, &status);
+
+    /* Active Image Counters */
+    FITS_read_key(infits, TLONG, "C1AAI_B", &ai1a_b, NULL, &status);
+    FITS_read_key(infits, TLONG, "C1AAI_E", &ai1a_e, NULL, &status);
+    FITS_read_key(infits, TLONG, "C1BAI_B", &ai1b_b, NULL, &status);
+    FITS_read_key(infits, TLONG, "C1BAI_E", &ai1b_e, NULL, &status);
+    FITS_read_key(infits, TLONG, "C2AAI_B", &ai2a_b, NULL, &status);
+    FITS_read_key(infits, TLONG, "C2AAI_E", &ai2a_e, NULL, &status);
+    FITS_read_key(infits, TLONG, "C2BAI_B", &ai2b_b, NULL, &status);
+    FITS_read_key(infits, TLONG, "C2BAI_E", &ai2b_e, NULL, &status);
+    FITS_read_key(infits, TDOUBLE, "CTIME_B", &ctm_b, NULL, &status);
+    FITS_read_key(infits, TDOUBLE, "CTIME_E", &ctm_e, NULL, &status);
+
+
+    *de = de_e - de_b;
+    *fe= fe_e - fe_b;
+    *ai1a = ai1a_e - ai1a_b ;
+    *ai1b = ai1b_e - ai1b_b ;
+    *ai2a = ai2a_e - ai2a_b ;
+    *ai2b = ai2b_e - ai2b_b ;
+    *sic = sic_e - sic_b ;
+    *lif = lif_e - lif_b ;
+    *as = as_e - as_b ; 
+    *ctm = ctm_e - ctm_b ;
+
+    return 0;
+}
+
+int main(int argc, char *argv[])
+{
+    int      i, j, k;
+    char     buffer[FLEN_CARD], comment[FLEN_CARD], stime[FLEN_CARD];
+    char     cntstr[FLEN_CARD], detstr[FLEN_CARD];
+    char     expid[FLEN_CARD], procstep[FLEN_CARD] ;
+    long     de, fe, de_tot, fe_tot, fe_b, de_b, fe_e, de_e;
+    long     ai1a, ai1b, ai2a, ai2b, ai1a_tot, ai1b_tot, ai2a_tot;
+    long     ai2b_tot,ai1a_b, ai1a_e, ai1b_b, ai1b_e, ai2a_b ;
+    long     ai2a_e, ai2b_b, ai2b_e, sic_b, sic_e, sic_tot, sic ;
+    long     lif_b, lif_e, lif_tot, lif, as_b, as_e, as_tot, as ;
+    long     expnight, indnight;
+    int      status=0, nfiles=0, hdutype=0, nkeys, keynum, anynull;
+    fitsfile *infits, *outfits;
+    long     nevents, jrow, ngti, ngti_in;
+    char     *pha_in, *dnflg ;
+    short    *x_in, *y_in;
+    float    *time_in, *gti_start, *gti_stop;
+    float    *gti_start_in, *gti_stop_in, *dx, *dy ;
+    float    fpasx0, fpasx, fpalx0, fpalx, dfpasx, dfpalx ;
+    double   mjd_init, mjd_start, mjd_end, exptime, mjd_last=0, indtime;
+    double   rawtime, trawtime;
+    double   ctm, ctm_b, ctm_e, ctm_tot ;
+    int      plantime, procflg ;
+    long     tplantime ;
+    int      tcol_in,  xcol_in,  ycol_in,  phacol_in, startcol ,stopcol;
+    int      tcol_out, xcol_out, ycol_out, phacol_out;
+    int      dxcol_in, dxcol_out, dycol_in, dycol_out,dnflgcol_in;
+    int      dnflgcol_out ;
+    int      fpa_split = FALSE;
+    time_t   vtime;
+
+
+    if (argc < 3) {
+        printf("Incorrect number of arguments.\n");
+	printf("Calling sequence:ttag_combine output_file input_file1 input_file2 input_file3 ...\n");
+        exit(1);
+    }
+
+    /* Initialize error checking. */
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Started execution.");
+
+    /* get and display time */
+    vtime = time(NULL) ;
+    strcpy(stime,ctime(&vtime)) ;
+
+    jrow=1;
+    de_tot=0 ;
+    fe_tot=0 ;
+    ai1a_tot=0 ;
+    ai1b_tot=0 ;
+    ai2a_tot=0 ;
+    ai2b_tot=0 ;
+    sic_tot=0 ;
+    lif_tot=0 ;
+    as_tot=0 ;
+    ctm_tot=0. ;
+    procflg=-1 ;
+    gti_start  = (float *) cf_malloc(sizeof(float) * 1000);
+    gti_stop   = (float *) cf_malloc(sizeof(float) * 1000);
+
+    gti_start[0] = 0.0;
+    gti_stop[0] = 0.0;
+
+    nfiles = argc-1;
+
+    exptime=0.0;
+    expnight=0;
+    trawtime=0.0;
+    tplantime=0;
+
+    ngti=0; /* is the number of new good time intervals */
+
+    for (i=2; i<=nfiles; i++) {
+             printf("Processing %-60.60s\n",argv[i]);
+             FITS_open_file(&infits, argv[i], READONLY, &status);
+
+             if (i==2) {
+                 FITS_read_key(infits, TDOUBLE, "EXPSTART", &mjd_init, 
+                     NULL, &status);
+                 mjd_last=mjd_start=mjd_init;
+                 FITS_read_key(infits, TDOUBLE, "EXPEND", &mjd_end, 
+                     NULL, &status);
+                 FITS_read_key(infits, TSTRING, "INIT_COR", procstep,
+                     NULL, &status) ;
+		 cf_read_fpa_pos (infits, &fpasx0, &fpalx0);
+                 FITS_create_file(&outfits, argv[1], &status);
+                 FITS_copy_hdu(infits, outfits, 0, &status);
+                 FITS_create_hdu(outfits, &status);
+                 FITS_movabs_hdu(infits,2,&hdutype,&status);
+                 FITS_get_hdrpos(infits, &nkeys, &keynum, &status);
+                 for (j=1; j<=nkeys; j++) {
+                     FITS_read_record(infits, j, buffer, &status);
+                     FITS_write_record(outfits, buffer, &status);
+                 }
+	      /* adjust some initial keywords */
+                 nevents=0;
+                 FITS_update_key(outfits, TLONG, "NAXIS2", &nevents, 
+                                 NULL, &status);
+	      /* set a flag (procflg) if the file is processed in any way */
+		 if ( strncmp(procstep, "COMP", 4) == 0) {
+                    printf("file has been processed - setting flag \n") ;
+                    procflg = 1 ; }
+                  else printf("These are raw data files \n") ;
+     	     } else {
+                 FITS_read_key(infits, TDOUBLE, "EXPSTART", &mjd_start, 
+                     NULL, &status);
+                 if (mjd_start < mjd_last) 
+                     cf_if_error("Files must be in time order, first to last.");
+		 mjd_last=mjd_start;
+                 FITS_read_key(infits, TDOUBLE, "EXPEND", &mjd_end, 
+                     NULL, &status);
+		 cf_read_fpa_pos (infits, &fpasx, &fpalx);
+                 dfpasx = fpasx - fpasx0 ;
+                 dfpalx = fpalx - fpalx0 ;
+		 if (fabs((double)dfpasx) > 30.) {
+                    printf("\nLarge change in SIC FPA X position: %f \n",dfpasx) ;
+		    fpa_split = TRUE;
+		 }
+		 if (fabs((double)dfpalx) > 30.) {
+                    printf("\nLarge change in LIF FPA X position: %f \n",dfpalx) ;
+		    fpa_split = TRUE;
+		 }
+	     }
+
+             FITS_movabs_hdu(infits,1,&hdutype,&status);
+
+             FITS_read_key(infits, TDOUBLE, "EXPTIME", &indtime, 
+                           NULL, &status);
+             exptime+=indtime;
+
+	     fits_read_key(infits, TDOUBLE, "RAWTIME", &rawtime,
+                           NULL, &status);
+	     if (status) 
+		status = 0;
+	     else
+                trawtime+=rawtime;
+
+             FITS_read_key(infits, TINT, "PLANTIME", &plantime, 
+                           NULL, &status);
+             tplantime+=plantime ;
+
+	     fits_read_key(infits, TLONG, "EXPNIGHT", &indnight,
+                           NULL, &status);
+	     if (status) 
+		status = 0;
+	     else
+                expnight+=indnight;
+
+       cf_dtcor_read_counters(infits,&de,&fe,&ai1a,&ai1b,&ai2a,&ai2b,
+          &sic,&lif,&as,&ctm) ;
+
+             de_tot += de;
+             fe_tot += fe;
+             ai1a_tot += ai1a ;
+             ai1b_tot += ai1b ;
+             ai2a_tot += ai2a ;
+             ai2b_tot += ai2b ;
+             sic_tot += sic ;
+             lif_tot += lif ;
+             as_tot += as ;
+             ctm_tot += ctm ;
+
+             FITS_movabs_hdu(infits,2,&hdutype,&status);
+             /* Get the number of events in the input file. */
+             FITS_read_key(infits, TLONG, "NAXIS2", &nevents, NULL, &status);
+
+             printf("     EXPTIME=%10.3f  NEVENTS=%10ld\n",indtime,nevents);
+
+             /* Allocate space for the input and output times, coords, 
+                pha */
+             time_in  = (float *) cf_malloc(sizeof(float) * nevents);
+             x_in     = (short *) cf_malloc(sizeof(short) * nevents);
+             y_in     = (short *) cf_malloc(sizeof(short) * nevents);
+             pha_in   = (char *)  cf_malloc(sizeof(char) * nevents);
+             dx       = (float *) cf_malloc(sizeof(float) * nevents);
+             dy       = (float *) cf_malloc(sizeof(float) * nevents);
+             dnflg    = (char *) cf_malloc(sizeof(char) * nevents);
+
+             FITS_get_colnum(infits, TRUE, "TIME", &tcol_in, &status);
+             FITS_get_colnum(infits, TRUE, "X",    &xcol_in, &status);
+             FITS_get_colnum(infits, TRUE, "Y",    &ycol_in, &status);
+             FITS_get_colnum(infits, TRUE, "PHA",  &phacol_in, &status);
+	   if(procflg > 0) {
+            FITS_get_colnum(infits, TRUE, "DX",   &dxcol_in, &status);
+            FITS_get_colnum(infits, TRUE, "DY",   &dycol_in, &status);
+            FITS_get_colnum(infits, TRUE, "DNFLG",&dnflgcol_in, &status); }
+
+             FITS_get_colnum(outfits, TRUE, "TIME", &tcol_out, &status);
+             FITS_get_colnum(outfits, TRUE, "X",    &xcol_out, &status);
+             FITS_get_colnum(outfits, TRUE, "Y",    &ycol_out, &status);
+             FITS_get_colnum(outfits, TRUE, "PHA",  &phacol_out, &status);
+	   if (procflg > 0 ) {
+            FITS_get_colnum(outfits, TRUE, "DX",   &dxcol_out, &status);
+            FITS_get_colnum(outfits, TRUE, "DY",   &dycol_out, &status);
+            FITS_get_colnum(outfits, TRUE, "DNFLG",&dnflgcol_out, &status);}
+
+  	     FITS_read_col(infits, TFLOAT, tcol_in, 1, 1, nevents, NULL,
+                           time_in, &anynull, &status);
+	     FITS_read_col(infits, TSHORT, xcol_in, 1, 1, nevents, NULL,
+		           x_in, &anynull, &status);
+  	     FITS_read_col(infits, TSHORT, ycol_in, 1, 1, nevents, NULL,
+		           y_in, &anynull, &status);
+	     FITS_read_col(infits,  TBYTE, phacol_in, 1, 1, nevents, NULL,
+		           pha_in, &anynull, &status);
+	   if(procflg > 0) {
+	    FITS_read_col(infits,  TFLOAT, dxcol_in, 1, 1, nevents, NULL,
+		           dx, &anynull, &status);
+	    FITS_read_col(infits,  TFLOAT, dycol_in, 1, 1, nevents, NULL,
+		           dy, &anynull, &status);
+	    FITS_read_col(infits,  TBYTE, dnflgcol_in, 1, 1, nevents, NULL,
+		           dnflg, &anynull, &status);}
+
+             for (j=0; j<nevents; j++){
+                  time_in[j]+=(float) ((mjd_start-mjd_init)*86400.0);
+	     }
+
+             FITS_write_col(outfits, TFLOAT, tcol_out, jrow, 1,
+			       nevents, time_in, &status);
+	     FITS_write_col(outfits, TSHORT, xcol_out, jrow, 1,
+			       nevents, x_in, &status);
+	     FITS_write_col(outfits, TSHORT, ycol_out, jrow, 1,
+			       nevents, y_in, &status);
+	     FITS_write_col(outfits, TBYTE, phacol_out, jrow, 1,
+			       nevents, pha_in, &status);
+	   if (procflg > 0) {
+	    FITS_write_col(outfits, TFLOAT, dxcol_out, jrow, 1,
+			       nevents, dx, &status);
+	    FITS_write_col(outfits, TFLOAT, dycol_out, jrow, 1,
+			       nevents, dy, &status);
+	    FITS_write_col(outfits, TBYTE, dnflgcol_out, jrow, 1,
+			   nevents, dnflg, &status); }
+  	     jrow+=nevents;
+
+             free(time_in);
+             free(x_in);
+             free(y_in);
+             free(pha_in);
+             free(dx) ;
+             free(dy) ;
+             free(dnflg) ;
+
+
+             /* Copy GTI from input to output */
+             FITS_movabs_hdu(infits, 3, &hdutype, &status);
+             FITS_read_key(infits,   TLONG, "NAXIS2", &ngti_in, NULL, &status);
+             gti_start_in  = (float *) cf_malloc(sizeof(float) * ngti_in);
+             gti_stop_in   = (float *) cf_malloc(sizeof(float) * ngti_in);
+             FITS_get_colnum(infits, TRUE,  "START",  &startcol, &status);
+             FITS_get_colnum(infits, TRUE,  "STOP",   &stopcol, &status);
+             FITS_read_col(infits,   TFLOAT, startcol, 1, 1, ngti_in, 0,
+  		  gti_start_in, &anynull, &status);
+             FITS_read_col(infits,   TFLOAT, stopcol, 1, 1, ngti_in, 0,
+		  gti_stop_in, &anynull, &status);
+             for (k=0; k<ngti_in; k++) {
+                  gti_start[ngti]=gti_start_in[k]+
+                                  (float) ((mjd_start-mjd_init)*86400.0);;
+                  gti_stop[ngti]=gti_stop_in[k]+
+                                  (float) ((mjd_start-mjd_init)*86400.0);;
+                  ngti++;
+                  if (ngti >= MAXGTI) {
+                       sprintf(buffer, "More than %d good time intervals.",MAXGTI) ;
+                       cf_if_error(buffer);
+		  }
+	     }
+             free(gti_start_in);
+             free(gti_stop_in);
+
+             FITS_close_file(infits, &status);
+    }
+
+    FITS_flush_file(outfits, &status);
+    
+    FITS_movabs_hdu(outfits, 1, &hdutype, &status);
+     jrow=jrow-1 ;
+    FITS_update_key(outfits, TLONG, "NEVENTS", &jrow, 0, &status) ;
+    FITS_update_key(outfits, TDOUBLE, "EXPTIME", &exptime, 0, &status);
+    FITS_update_key(outfits, TDOUBLE, "EXPEND", &mjd_end, 0, &status);
+    FITS_update_key(outfits, TLONG, "PLANTIME", &tplantime, 0, &status) ;
+
+    if (expnight < 0)
+	expnight = 0;
+    FITS_update_key(outfits, TLONG, "EXPNIGHT", &expnight, 0, &status);
+
+    if (trawtime - exptime > -1.)
+        FITS_update_key(outfits, TDOUBLE, "RAWTIME", &trawtime, 0, &status);
+
+    FITS_read_key(outfits, TSTRING, "DETECTOR", detstr, NULL, &status);
+    sprintf(cntstr, "%1.1s%2.2s%4.4s","C",detstr,"FE_B");
+    FITS_read_key(outfits, TLONG, cntstr, &fe_b, NULL, &status);
+     sprintf(cntstr, "%1.1s%2.2s%4.4s","C",detstr,"DE_B");
+    FITS_read_key(outfits, TLONG, cntstr, &de_b, NULL, &status);
+    sprintf(cntstr, "%1.1s%2.2s%5.5s","C",detstr,"SIC_B");
+    FITS_read_key(outfits, TLONG, cntstr, &sic_b, NULL, &status);
+    sprintf(cntstr, "%1.1s%2.2s%5.5s","C",detstr,"LIF_B");
+    FITS_read_key(outfits, TLONG, cntstr, &lif_b, NULL, &status);
+    sprintf(cntstr, "%1.1s%2.2s%4.4s","C",detstr,"AS_B");
+    FITS_read_key(outfits, TLONG, cntstr, &as_b, NULL, &status);
+
+    FITS_read_key(outfits, TLONG, "C1AAI_B", &ai1a_b, NULL, &status);
+    FITS_read_key(outfits, TLONG, "C1BAI_B", &ai1b_b, NULL, &status);
+    FITS_read_key(outfits, TLONG, "C2AAI_B", &ai2a_b, NULL, &status);
+    FITS_read_key(outfits, TLONG, "C2BAI_B", &ai2b_b, NULL, &status);
+    FITS_read_key(outfits, TDOUBLE, "CTIME_B", &ctm_b, NULL, &status);
+ 
+    sprintf(comment, "New ID for combined data") ;
+    strncpy(expid,"999               ",18) ;
+     expid[18]='\0' ;
+    FITS_update_key(outfits, TSTRING, "EXP_ID", expid, comment, &status);
+
+    sprintf(comment, "Date and time file was created") ;
+    stime[24]='\0' ;
+    FITS_update_key(outfits, TSTRING, "DATE", stime, comment, &status) ;
+
+    de_e = de_tot + de_b;
+    fe_e = fe_tot + fe_b;
+    lif_e = lif_tot + lif_b ;
+    sic_e = sic_tot + sic_b ;
+    as_e = as_tot + as_b ;
+    ctm_e = ctm_tot + ctm_b ;
+    ai1a_e = ai1a_tot + ai1a_b ;
+    ai1b_e = ai1b_tot + ai1b_b ;
+    ai2a_e = ai2a_tot + ai2a_b ;
+    ai2b_e = ai2b_tot + ai2b_b ;
+
+    sprintf(cntstr, "%1.1s%2.2s%4.4s","C",detstr,"DE_E");
+    FITS_update_key(outfits, TLONG, cntstr, &de_e, NULL, &status);
+    sprintf(cntstr, "%1.1s%2.2s%4.4s","C",detstr,"FE_E");
+    FITS_update_key(outfits, TLONG, cntstr, &fe_e, NULL, &status);
+    sprintf(cntstr, "%1.1s%2.2s%5.5s","C",detstr,"SIC_E");
+    FITS_update_key(outfits, TLONG, cntstr, &sic_e, NULL, &status);
+    sprintf(cntstr, "%1.1s%2.2s%5.5s","C",detstr,"LIF_E");
+    FITS_update_key(outfits, TLONG, cntstr, &lif_e, NULL, &status);
+    sprintf(cntstr, "%1.1s%2.2s%4.4s","C",detstr,"AS_E");
+    FITS_update_key(outfits, TLONG, cntstr, &as_e, NULL, &status);
+
+    FITS_update_key(outfits, TLONG, "C1AAI_E", &ai1a_e, NULL, &status);
+    FITS_update_key(outfits, TLONG, "C1BAI_E", &ai1b_e, NULL, &status);
+    FITS_update_key(outfits, TLONG, "C2AAI_E", &ai2a_e, NULL, &status);
+    FITS_update_key(outfits, TLONG, "C2BAI_E", &ai2b_e, NULL, &status);
+    FITS_update_key(outfits, TDOUBLE, "CTIME_E", &ctm_e, NULL, &status);
+
+
+    FITS_write_comment(outfits, "  ", &status);
+    FITS_write_comment(outfits, "CF_TTAG_COMBINE", &status);
+    FITS_write_comment(outfits, "  ", &status);
+    FITS_write_comment(outfits, "This file is a concatenation of:", &status);
+    for (i=2; i<=nfiles; i++) {
+             FITS_write_comment(outfits, argv[i], &status);
+    }
+    
+
+    FITS_open_file(&infits, argv[2], READONLY, &status);
+
+    /* Move to the second extension which contains the goof time intervals. */
+    FITS_movabs_hdu(infits, 3, &hdutype, &status);
+
+    /* Create the second extension in the output file. */
+    FITS_create_hdu(outfits, &status);
+
+    /* Copy the header of the input file to the output file. */
+    FITS_get_hdrpos(infits, &nkeys, &keynum, &status);
+    for (i=1; i<=nkeys; i++) {
+	FITS_read_record(infits, i, buffer, &status);
+	FITS_write_record(outfits, buffer, &status);
+    }
+
+    FITS_get_colnum(outfits,TRUE,"START",&startcol,&status);
+    FITS_get_colnum(outfits,TRUE,"STOP",&stopcol,&status);
+
+    FITS_write_col(outfits, TFLOAT, startcol, 1, 1, ngti, gti_start, &status);
+    FITS_write_col(outfits, TFLOAT, stopcol, 1, 1, ngti, gti_stop, &status);
+
+    free(gti_start);
+    free(gti_stop);
+
+    FITS_close_file(infits, &status);
+    FITS_close_file(outfits, &status);
+
+    if (fpa_split)
+       cf_if_warning("FPA motion detected. Resolution may be compromised.\n");
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished execution.");
+    return 0;
+}
diff --git a/src/analysis/ttag_lightcurve.c b/src/analysis/ttag_lightcurve.c
new file mode 100644
index 0000000..f1a14fa
--- /dev/null
+++ b/src/analysis/ttag_lightcurve.c
@@ -0,0 +1,398 @@
+
+/*************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *************************************************************************
+ *
+ *
+ * Usage:
+ *     ttag_lightcurve [-hf] [-v level] input_file output_file windows_file 
+ *                                     bins LiForSiC
+ * 
+ *
+ * Arguments:
+ *   input_file     : ttag IDF file                                         
+ *   output_file    : ASCII file with 2 columns : 
+ *                        - time (MJD)         
+ *                        - countrate                       
+ *
+ *   windows_file   : input ASCII file with 2 columns : 
+ *                        - start of spectral windows 
+ *                        - stop of spectral windows  
+ *
+ *   bins           : bin size in seconds                                         
+ *   LiForSiC       : 1=LiF, 2=SiC
+ *
+ *
+ *
+ *
+ * Options:
+ *     -h:  this help message
+ *     -f:  output calibrated flux (erg/cm2/s) instead of countrate
+ *     -v:  verbosity level (=1; 0 is silent)
+ *          
+ *
+ *
+ *
+ * History:	10/06/04	bjg	v1.0              
+ *		06/03/05	wvd	v1.1 Delete unused variables.
+ *   
+ ***************************************************************************/
+
+
+
+#include <stdlib.h>
+#include <stdio.h>
+#include <string.h>
+#include <time.h>
+#include <unistd.h>
+#include <math.h>
+
+#include "calfuse.h"
+
+
+
+
+#define N_MAX_WIN 100   /* Maximum number of spectral windows */
+
+typedef struct {
+  float start;
+  float stop;
+} interval;             /* type to store a spectral window  */ 
+
+
+int is_inside(float val,interval * interval_ptr, int nintervals);
+int is_good_time(char timeflag,char * daynight);
+int is_in_lif_channel(char channel, char * aperture);
+int is_in_sic_channel(char channel, char * aperture);
+
+
+
+
+
+static char CF_PRGM_ID[]= "ttag_lightcurve";
+static char CF_VER_NUM[]= "1.1";
+
+
+
+
+int main(int argc,char *argv[]){
+  
+ 
+  
+  char       input_filename[FLEN_CARD];
+  char       output_filename[FLEN_CARD]; 
+  char       windefs_filename[FLEN_CARD];
+  
+  FILE     * output_file;
+  FILE     * windefs_file;
+
+  fitsfile * infits;
+
+  interval   swindows[N_MAX_WIN];   /* the spectral windows are stored 
+                                           in an array of intervals */
+  int        nwindows = 0;          /* number of spectral windows TBD */ 
+
+  float      bins;    
+
+  int        intnull=0,anynull;
+  int        status=0;
+  int        hdutype=0;
+
+  long       nevents;
+  long       i;
+  int        ncol;
+
+  char       tempchar;
+  char       tempstring[FLEN_CARD];
+
+  char       daynight[FLEN_CARD];
+  char       instmode[FLEN_CARD];
+  char       aperture[FLEN_CARD];
+
+  double *   hdu2_time;
+  double *   hdu2_lambda;
+  double *   hdu2_weight;
+  char   *   hdu2_channel;
+  char   *   hdu2_timeflgs;
+  char   *   hdu2_loc_flgs;
+
+  float  *   gti_start;
+  float  *   gti_stop;
+  int        ngtis;
+  
+  interval * gtis;
+
+  double t, tmax, ctot;
+
+  double expstart;
+
+  int badtime;
+
+  int LiForSiC;
+  
+
+  int optc;
+  
+  int do_flux=0;
+
+  char opts[] = "hfv:";
+  char usage[] = 
+    "Usage:\n"
+    "  ttag_lightcurve [-hf] [-v level] input_file output_file windows_file\n"
+    "                                  bins LiForSiC\n\n"
+    "Arguments:\n"
+    "  input_file     : ttag IDF file\n\n"
+    "  output_file    : ASCII file with 2 columns:\n" 
+    "                        - time (MJD)\n"
+    "                        - countrate corrected for deadtime\n\n"
+    "  windows_file   : input ASCII file with 2 columns :\n"
+    "                        - start of spectral windows\n"
+    "                        - stop of spectral windows\n\n"
+    "  bins           : bin size in seconds\n"
+    "  LiForSiC       : 1=LiF, 2=SiC\n";
+  char option[] =
+    "Options:\n"
+    "  -h:  this help message                 \n"
+    "  -f:  output calibrated flux (erg/cm2/s) instead of countrate  \n"
+    "  -v:  verbosity level (=1; 0 is silent) \n";
+
+  verbose_level = 1;
+  
+  
+  /* Check number of options and arguments */
+  while ((optc = getopt(argc, argv, opts)) != -1) {
+    switch(optc) {    
+    case 'h':
+      printf("%s\n%s", usage, option);
+      return EXIT_SUCCESS;
+    case 'v':
+      verbose_level = atoi(optarg);
+      break;
+    case 'f':
+      do_flux=1;
+      break;
+    }
+  }
+
+  /* Initialize error checking. */
+  cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+  if (argc != optind+5)
+    cf_if_error("%s\nIncorrect number of program arguments", usage);
+  
+  
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Started execution.");
+  
+  strcpy(input_filename,argv[optind]); 
+  strcpy(output_filename,argv[optind+1]);  
+  strcpy(windefs_filename,argv[optind+2]);   
+  sscanf(argv[optind+3],"%f",&bins);  
+  sscanf(argv[optind+4],"%d",&LiForSiC);
+
+  if ((LiForSiC>2)||(LiForSiC<1)) {
+    cf_if_error("%s\nLiForSiC value must be 1 (LiF) or 2 (SiC)", usage);
+  }
+  
+  
+  if (bins<=0) {
+    cf_if_error("Time interval is less than or equal to zero.");
+  }
+
+    
+  /* Open the spectral windows definition file */
+  if ((windefs_file = fopen (windefs_filename, "r")) == NULL){
+    cf_if_error ("Unable to open file %s\n", windefs_filename);
+  }
+
+
+  /* Read the spectral windows definition file and store the spectral windows */
+  while (fscanf(windefs_file,"%f %f",&((swindows[nwindows]).start),
+                                     &((swindows[nwindows]).stop))!=EOF)
+    {
+      nwindows++;
+    }
+
+  
+
+
+  for (i=0;i<nwindows;i++){
+    printf("Window %ld : %f - %f\n",i+1,swindows[i].start,swindows[i].stop);
+  }
+
+  
+
+  /* Create the output file */
+  if ((output_file = fopen(output_filename,"w")) == NULL){
+    fclose(windefs_file);
+    cf_if_error ("Unable to create file %s\n", output_filename);    
+  }
+  
+
+
+  FITS_open_file(&infits,input_filename,READONLY,&status);
+
+  FITS_read_key(infits,TSTRING,"INSTMODE",instmode,NULL,&status);
+  
+  if (strncasecmp(instmode,"TTAG",4)){
+    FITS_close_file(infits,&status);
+    fclose(windefs_file);
+    fclose(output_file);
+    cf_if_error("Input file is not TTAG.");
+  }
+  
+  FITS_read_key(infits,TDOUBLE,"EXPSTART",&expstart,NULL,&status);
+  
+  FITS_read_key(infits,TSTRING,"DAYNIGHT",daynight,NULL,&status);
+
+  FITS_read_key(infits,TSTRING,"APERTURE",aperture,NULL,&status);
+
+
+  FITS_movabs_hdu(infits,2,&hdutype,&status);
+  FITS_read_key(infits,TSTRING,"TFORM1",tempstring,NULL,&status);
+  sscanf(tempstring,"%ld%c",&nevents,&tempchar);
+
+ 
+  
+  
+  hdu2_time=(double *)malloc(nevents*sizeof(double));
+  hdu2_lambda=(double *)malloc(nevents*sizeof(double));
+  hdu2_weight=(double *)malloc(nevents*sizeof(double));
+  hdu2_channel=(char *)malloc(nevents*sizeof(char));
+  hdu2_timeflgs=(char *)malloc(nevents*sizeof(char));
+  hdu2_loc_flgs=(char *)malloc(nevents*sizeof(char));
+ 
+  FITS_get_colnum(infits, TRUE, "TIME", &ncol, &status);
+  FITS_read_col(infits, TDOUBLE, ncol, 1, 1, nevents, &intnull,
+		hdu2_time, &anynull, &status);
+ 
+  FITS_get_colnum(infits, TRUE, "LAMBDA", &ncol, &status);
+  FITS_read_col(infits, TDOUBLE, ncol, 1, 1, nevents, &intnull,
+		hdu2_lambda, &anynull, &status);
+
+  if (do_flux) {
+    FITS_get_colnum(infits, TRUE, "ERGCM2", &ncol, &status);
+    FITS_read_col(infits, TDOUBLE, ncol, 1, 1, nevents, &intnull,
+		  hdu2_weight, &anynull, &status);
+  } else {
+    FITS_get_colnum(infits, TRUE, "WEIGHT", &ncol, &status);
+    FITS_read_col(infits, TDOUBLE, ncol, 1, 1, nevents, &intnull,
+		  hdu2_weight, &anynull, &status);
+  }
+
+  FITS_get_colnum(infits, TRUE, "CHANNEL", &ncol, &status);
+  FITS_read_col(infits, TBYTE, ncol, 1, 1, nevents, &intnull,
+		hdu2_channel, &anynull, &status);
+
+  FITS_get_colnum(infits, TRUE, "TIMEFLGS", &ncol, &status);
+  FITS_read_col(infits, TBYTE, ncol, 1, 1, nevents, &intnull,
+		hdu2_timeflgs, &anynull, &status);
+  
+  FITS_get_colnum(infits, TRUE, "LOC_FLGS", &ncol, &status);
+  FITS_read_col(infits, TBYTE, ncol, 1, 1, nevents, &intnull,
+		hdu2_loc_flgs, &anynull, &status);
+
+
+  FITS_movabs_hdu(infits,3,&hdutype,&status);
+
+  ngtis=cf_read_col(infits,TFLOAT,"START",(void **) &gti_start);
+  ngtis=cf_read_col(infits,TFLOAT,"STOP",(void **) &gti_stop);
+
+  gtis=(interval *)malloc(ngtis*sizeof(interval));
+
+  for (i=0;i<ngtis;i++){
+    gtis[i].start=gti_start[i];
+    gtis[i].stop=gti_stop[i];
+  }
+
+
+
+  t=0.0;
+  tmax=bins;
+  i=0;
+  ctot=0.0;
+  badtime=0;  
+  while (i<nevents){
+
+    while (hdu2_time[i]>=tmax) {
+      if (!(is_inside(t,gtis,ngtis))) badtime=1;
+      if (!(is_inside(tmax,gtis,ngtis))) badtime=1;
+      if (!badtime) fprintf(output_file,"%15lf %15lf\n",expstart+t/(3600.0*24.0),ctot/bins);
+      t=tmax;
+      tmax=t+bins;
+      ctot=0.0;
+      badtime=0;
+    }
+
+    if (!(is_good_time(hdu2_timeflgs[i],daynight))) badtime=1;
+
+    if (is_inside(hdu2_lambda[i],swindows,nwindows)){
+      if (hdu2_loc_flgs[i]==0){	
+	if (LiForSiC==1){
+	  if (is_in_lif_channel(hdu2_channel[i],aperture)){
+	    ctot+=hdu2_weight[i];
+	  }
+	}
+	else {
+	  if (is_in_sic_channel(hdu2_channel[i],aperture)){
+	    ctot+=hdu2_weight[i];
+	  }
+	}
+      }       
+    }
+      
+    i++;
+  }
+    
+  free(hdu2_time);
+  free(hdu2_lambda);
+  free(hdu2_weight);
+  free(hdu2_channel);
+  free(hdu2_timeflgs);
+  free(hdu2_loc_flgs);
+ 
+
+       
+  FITS_close_file(infits,&status);
+  fclose(windefs_file);
+  fclose(output_file);
+
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished execution.");
+  return EXIT_SUCCESS;
+  
+}
+
+int is_inside(float val,interval * interval_ptr, int nintervals){
+  int i;
+  i=0;
+  while (i<nintervals){
+    if ((val<=interval_ptr[i].stop)&&(val>=interval_ptr[i].start)){
+      return 1;
+    }
+    i++;
+  }
+  return 0;
+}
+
+int is_good_time(char timeflag,char * daynight){
+
+    if (!(strncasecmp(daynight,"DAY"  ,3))) return (timeflag  == 1);
+    if (!(strncasecmp(daynight,"NIGHT",5))) return (timeflag  == 0);
+    
+    return ((timeflag&254) == 0);
+
+}
+
+int is_in_lif_channel(char channel, char * aperture){
+  if (!strncasecmp(aperture,"LWRS",4)) return (channel == 3);
+  if (!strncasecmp(aperture,"MDRS",4)) return (channel == 2);		 
+  if (!strncasecmp(aperture,"HIRS",4)) return (channel == 1);
+  return 0;
+}
+
+int is_in_sic_channel(char channel, char * aperture){
+  if (!strncasecmp(aperture,"LWRS",4)) return (channel == 7);
+  if (!strncasecmp(aperture,"MDRS",4)) return (channel == 6);		 
+  if (!strncasecmp(aperture,"HIRS",4)) return (channel == 5);
+  return 0;
+}
diff --git a/src/analysis/ttag_lightcurve_channel_sum.c b/src/analysis/ttag_lightcurve_channel_sum.c
new file mode 100644
index 0000000..9f76c37
--- /dev/null
+++ b/src/analysis/ttag_lightcurve_channel_sum.c
@@ -0,0 +1,183 @@
+
+/*************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *************************************************************************
+ *
+ *
+ * Usage:
+ *     ttag_lightcurve_channel_sum [-h] [-v level] output_file 
+ *                     input_file1 input_file2
+ * 
+ *
+ * Arguments:
+ *   input_files     : ASCII files with 2 columns : 
+ *                        - time         
+ *                        - signal
+ *                                        
+ *   output_file    : ASCII file with 2 columns : 
+ *                        - time         
+ *                        - signal                       
+ *
+ *
+ *
+ *
+ *
+ *
+ * Options:
+ *     -h:  this help message
+ *     -v:  verbosity level (=1; 0 is silent)
+ *          
+ *
+ *
+ *
+ * History:           10/06/04	bjg	v1.0
+ *                    11/04/04	bjg	v1.1  time equality criteria changed
+ *   
+ ***************************************************************************/
+
+
+
+#include <stdlib.h>
+#include <stdio.h>
+#include <string.h>
+#include <time.h>
+#include <unistd.h>
+#include <math.h>
+
+#include "calfuse.h"
+
+
+#define MAX_INPUT_FILE 20
+
+static char CF_PRGM_ID[]= "ttag_lightcurve_channel_sum";
+static char CF_VER_NUM[]= "1.1";
+
+
+int is_equal(double a, double b, double delta){
+
+  return ( ((a-b) <= delta) && ((a-b) > -delta) );
+
+}
+
+
+int main(int argc,char *argv[]){
+  
+ 
+  
+  char       input_filename1[FLEN_CARD]; 
+  char       input_filename2[FLEN_CARD];
+  char       output_filename[FLEN_CARD]; 
+
+  
+  FILE     * output_file;
+  FILE     * input_file1;
+  FILE     * input_file2;
+
+  double t1,v1,t2,v2, delta_t;
+
+  int end_of_file;
+
+  int optc;
+   
+  char opts[] = "hv:";
+  char usage[] = 
+    "Usage:\n"
+    "  ttag_lightcurve_channel_sum [-h] [-v level] output_file\n" 
+    "                  input_file1 input_file2\n\n"
+    "Arguments:\n"
+    "  input_files    : ASCII files with 2 columns :\n"  
+    "                     - time\n"        
+    "                     - signal\n\n"                                        
+    "  output_file    : ASCII file with 2 columns : \n" 
+    "                     - time \n"        
+    "                     - signal\n";
+  char option[] =
+    "Options:\n"
+    "  -h:  this help message                 \n"
+    "  -v:  verbosity level (=1; 0 is silent) \n";
+
+  verbose_level = 1;
+  
+  
+  /* Check number of options and arguments */
+  while ((optc = getopt(argc, argv, opts)) != -1) {
+    switch(optc) {    
+    case 'h':
+      printf("%s\n%s", usage, option);
+      return EXIT_SUCCESS;
+    case 'v':
+      verbose_level = atoi(optarg);
+      break;
+    }
+  }
+
+  /* Initialize error checking. */
+  cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+  if (argc != optind+3)
+    cf_if_error("%s\nIncorrect number of program arguments", usage);
+  
+  
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Started execution.");
+  
+  strcpy(output_filename,argv[optind]); 
+  strcpy(input_filename1,argv[optind+1]);  
+  strcpy(input_filename2,argv[optind+2]);   
+
+
+
+  if ((input_file1 = fopen(input_filename1,"r")) == NULL){
+    cf_if_error ("Unable to open file %s\n", input_filename1);    
+  }
+
+  if ((input_file2 = fopen(input_filename2,"r")) == NULL){
+    fclose(input_file1);
+    cf_if_error ("Unable to open file %s\n", input_filename2);    
+  }
+
+
+  /* Create the output file */
+  if ((output_file = fopen(output_filename,"w")) == NULL){
+    fclose(input_file1);
+    fclose(input_file2);
+    cf_if_error ("Unable to create file %s\n", output_filename);    
+  }
+  
+  fscanf(input_file1,"%lf %lf",&t1,&v1);
+  fscanf(input_file1,"%lf %lf",&t2,&v2);
+  delta_t=t2-t1;
+
+  fseek(input_file1,0,SEEK_SET);
+ 
+  
+  end_of_file=(fscanf(input_file2,"%lf %lf",&t2,&v2)==EOF)||(fscanf(input_file1,"%lf %lf",&t1,&v1)==EOF);
+  
+
+  while (!end_of_file){
+    if (is_equal(t2,t1,delta_t/2)){
+      fprintf(output_file,"%15lf  %15lf\n",t1,v1+v2);
+      end_of_file=(fscanf(input_file2,"%lf %lf",&t2,&v2)==EOF)||(fscanf(input_file1,"%lf %lf",&t1,&v1)==EOF);
+    } 
+    else if (t2<t1) {
+      end_of_file=(fscanf(input_file2,"%lf %lf",&t2,&v2)==EOF);
+    }
+    else {
+      end_of_file=(fscanf(input_file1,"%lf %lf",&t1,&v1)==EOF);
+    }
+
+
+
+  }
+  
+
+  fclose(input_file1);
+  fclose(input_file2);
+  fclose(output_file);
+
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished execution.");
+  return EXIT_SUCCESS;
+  
+}
+
+
diff --git a/src/analysis/ttag_lightcurve_combine.c b/src/analysis/ttag_lightcurve_combine.c
new file mode 100644
index 0000000..9947f69
--- /dev/null
+++ b/src/analysis/ttag_lightcurve_combine.c
@@ -0,0 +1,182 @@
+
+/*****************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *****************************************************************************
+ *
+ * Synopsis:	ttag_lightcurve_combine outfile file1 file2 file3 file4 ...
+ *
+ *
+ * History:	09/07/04   bjg   v1.0
+ *
+ *
+ ****************************************************************************/
+
+
+#include <unistd.h>
+#include <stdlib.h>
+#include <stdio.h>
+#include <string.h>
+#include <time.h>
+#include "calfuse.h"
+
+
+typedef char filename[FLEN_CARD];
+
+static char CF_PRGM_ID[]= "ttag_lightcurve_combine";
+static char CF_VER_NUM[]= "1.0";
+
+int main(int argc,char *argv[]){
+
+  char     stime[FLEN_CARD];
+  time_t   vtime;
+
+	
+  filename *filelist;
+  double   *expstartlist;
+ 
+  filename tempstring;
+  double   tempdouble;
+  
+  double   minexpstart;
+  int      minindex;
+  
+  long     nfiles, n2;
+  long     i,j;
+  
+  double   t,v;
+  FILE   * fin;
+  FILE   * fout;
+
+  int optc;
+
+  char opts[] = "hv:";
+  char usage[] = 
+    "Usage:\n"
+    "  ttag_lightcurve_combine [-h]  [-v level] output_file input_files\n";
+  char option[] =
+    "Options:\n"
+    "  -h:  this help message\n"
+    "  -v:  verbosity level (=1; 0 is silent)\n";
+
+  verbose_level = 1;
+
+  /* Check number of options and arguments */
+  while ((optc = getopt(argc, argv, opts)) != -1) {
+    switch(optc) {
+    case 'h':
+      printf("%s\n%s", usage, option);
+      return 0;
+    case 'v':
+      verbose_level = atoi(optarg);
+      break;
+    }
+  }
+
+  cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+  if (argc < optind+2) {
+    printf("%s", usage);
+    cf_if_error("Incorrect number of arguments");
+  }
+   
+    
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Started execution.");
+  
+  /* get and display time */
+  vtime = time(NULL) ;
+  strcpy(stime,ctime(&vtime));
+  
+      
+  nfiles=argc-optind-1;
+  
+  filelist     = (filename *)malloc(nfiles*sizeof(filename));
+  expstartlist = (double *)malloc(nfiles*sizeof(double));
+
+
+  cf_verbose(1,"GETTING INFORMATION ON INPUT FILES") ;
+
+  n2=0;
+
+  for (i=0; i<nfiles;i++) {
+
+    fin=fopen(argv[optind+i+1],"r");
+
+    if (fin==NULL){
+      cf_if_warning("Could not open file %s. Skipped.",argv[optind+i+1]);
+      continue;
+    }
+      
+    fscanf(fin,"%lf %lf",&t,&v);
+
+    expstartlist[n2]=t;
+    strcpy(filelist[n2],argv[optind+i+1]);
+
+    fclose(fin);
+		
+    n2++;
+  }
+
+  nfiles=n2;
+
+  if (nfiles==0){
+    cf_verbose(1,"No files to combine. Exiting.");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished execution.");
+    exit(0);
+  }
+  
+  cf_verbose(1,"SORTING INPUT FILES IN TIME ORDER") ;
+  
+  for (i=0; i<nfiles-1;i++) {
+    minexpstart=expstartlist[i];
+    minindex=i;
+    for (j=i+1; j<nfiles;j++) {
+      if (expstartlist[j]<minexpstart){
+	minexpstart=expstartlist[j];
+	minindex=j;
+      }
+    }
+    
+    strcpy(tempstring,filelist[minindex]);
+    strcpy(filelist[minindex],filelist[i]);
+    strcpy(filelist[i],tempstring);
+    
+    tempdouble=expstartlist[minindex];
+    expstartlist[minindex]=expstartlist[i];
+    expstartlist[i]=tempdouble;
+    
+  }
+
+  cf_verbose(2,"N: Filename                  ExpStart ");
+
+  for (i=0; i<nfiles;i++) {
+    cf_verbose(2,"%ld: %s %7.1f",i,filelist[i],expstartlist[i]);
+  }
+  
+  
+  cf_verbose(1,"CREATING OUTPUT FILE");
+  if ((fout = fopen(argv[optind],"w")) == NULL){
+    cf_if_error ("Unable to create file %s\n", argv[optind]);    
+  }
+
+  
+  
+  for (i=0; i<nfiles;i++) {
+    fin=fopen(filelist[i],"r");
+    while (fscanf(fin, "%lf %lf", &t, &v)!=EOF){
+      fprintf(fout, "%15lf %15lf\n", t, v);
+    }
+    fclose(fin);
+  }
+
+
+
+  fclose(fout);
+  
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished execution.");
+  return EXIT_SUCCESS;
+  
+}
+
+
diff --git a/src/analysis/ttag_lightcurve_mjd2hmjd.c b/src/analysis/ttag_lightcurve_mjd2hmjd.c
new file mode 100644
index 0000000..def1978
--- /dev/null
+++ b/src/analysis/ttag_lightcurve_mjd2hmjd.c
@@ -0,0 +1,151 @@
+
+/*************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *************************************************************************
+ *
+ *
+ * Usage:
+ *     ttag_lightcurve_mjd2hmjd [-h] [-v level] output_file input_file
+ *                                      hh mm ss dd mm ss     
+ *
+ *
+ * Arguments:
+ *   input_file     : ASCII file with 2 columns : 
+ *                        - time (MJD)        
+ *                        - signal
+ *                                        
+ *   output_file    : ASCII file with 2 columns : 
+ *                        - time (HMJD)      
+ *                        - signal                       
+ *
+ *   hh mm ss dd mm ss : RA and DEC of target 
+ *
+ *
+ *
+ *
+ * Options:
+ *     -h:  this help message
+ *     -v:  verbosity level (=1; 0 is silent)
+ *          
+ *
+ *
+ *
+ * History:     10/06/04  bjg   v1.0
+ *		06/03/05  wvd	v1.1	Delete unused variables.
+ *   
+ ***************************************************************************/
+
+
+
+#include <stdlib.h>
+#include <stdio.h>
+#include <string.h>
+#include <time.h>
+#include <unistd.h>
+#include <math.h>
+
+#include "calfuse.h"
+
+double gethmjd(double, int, int, float, int, int, float);
+
+static char CF_PRGM_ID[]= "ttag_lightcurve_mjd2hmjd";
+static char CF_VER_NUM[]= "1.1";
+
+
+int main(int argc,char *argv[]){
+  
+ 
+  
+  char       input_filename[FLEN_CARD]; 
+  char       output_filename[FLEN_CARD]; 
+
+  
+  FILE     * output_file;
+  FILE     * input_file;
+
+
+  double t,t2,v;
+  int    rah, ram, decd, decm;
+  float    ras, decs;
+
+
+  int optc;
+   
+  char opts[] = "hv:";
+  char usage[] = 
+    "Usage:\n"
+    "  ttag_lightcurve_mjd2hmjd [-h] [-v level] output_file input_file\n" 
+    "                                   hh mm ss dd mm ss\n\n"
+    "Arguments:\n"
+    "  input_file     : ASCII file with 2 columns :\n"  
+    "                     - time (MJD) \n"        
+    "                     - signal\n\n"       
+    "  output_file    : ASCII file with 2 columns : \n" 
+    "                     - time (HMJD) \n"        
+    "                     - signal \n\n"
+    "  hh mm ss dd mm ss : RA and DEC of target\n";
+  char option[] =
+    "Options:\n"
+    "  -h:  this help message                 \n"
+    "  -v:  verbosity level (=1; 0 is silent) \n";
+
+  verbose_level = 1;
+  
+  
+  /* Check number of options and arguments */
+  while ((optc = getopt(argc, argv, opts)) != -1) {
+    switch(optc) {    
+    case 'h':
+      printf("%s\n%s", usage, option);
+      return EXIT_SUCCESS;
+    case 'v':
+      verbose_level = atoi(optarg);
+      break;
+    }
+  }
+
+  /* Initialize error checking. */
+  cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+  if (argc != optind+8)
+    cf_if_error("%s\nIncorrect number of program arguments", usage);
+  
+  
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Started execution.");
+  
+  strcpy(output_filename,argv[optind]); 
+  strcpy(input_filename,argv[optind+1]);  
+  sscanf(argv[optind+2],"%d",&rah);
+  sscanf(argv[optind+3],"%d",&ram);
+  sscanf(argv[optind+4],"%f",&ras);
+  sscanf(argv[optind+5],"%d",&decd);
+  sscanf(argv[optind+6],"%d",&decm);
+  sscanf(argv[optind+7],"%f",&decs);
+
+
+  if ((input_file = fopen(input_filename,"r")) == NULL){
+    cf_if_error ("Unable to open file %s\n", input_filename);    
+  }
+
+  /* Create the output file */
+  if ((output_file = fopen(output_filename,"w")) == NULL){
+    fclose(input_file);
+    cf_if_error ("Unable to create file %s\n", output_filename);    
+  }
+  
+  while(fscanf(input_file,"%lf %lf",&t,&v)!=EOF) {
+    t2=gethmjd(t, rah, ram, ras, decd, decm, decs);
+   
+    fprintf(output_file,"%15lf  %15lf\n",t2,v);
+  }
+
+  fclose(input_file);
+  fclose(output_file);
+
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished execution.");
+  return EXIT_SUCCESS;
+  
+}
+
+
diff --git a/src/analysis/ttag_lightcurve_periodogram.c b/src/analysis/ttag_lightcurve_periodogram.c
new file mode 100644
index 0000000..939a1ec
--- /dev/null
+++ b/src/analysis/ttag_lightcurve_periodogram.c
@@ -0,0 +1,294 @@
+
+/****************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ ****************************************************************************
+ *
+ *
+ * Usage:
+ *    ttag_lightcurve_periodogram [-hs] [-v level] input_file output_file 
+ *                                                minf maxf stepf 
+ * 
+ *
+ * Arguments:
+ *    input_file  : an ASCII file with 2 columns : 
+ *                     - time (days) 
+ *                     - countrate
+ *
+ *    output_file : an ASCII file with 2 columns : 
+ *                     - frequency (Hz)
+ *                     - normalized estimated power spectral density
+ *   
+ *    minf        : start frequency (Hz)
+ *    maxf        :   end frequency (Hz)
+ *    stepf       :  frequency step (Hz)
+ *
+ *
+ *
+ * Options:
+ *     -h:  this help message
+ *     -v:  verbosity level (=1; 0 is silent)
+ *     -s:  time is in seconds instead of days
+ *
+ * 
+ **************************************************************************
+ *
+ *
+ *
+ * Description:
+ *
+ *     Computes the Lomb periodogram of signal h
+ *     from samples (hj) j=1..N at times (tj) j=1..N 
+ * 
+ *
+ *      w=2*pi*f
+ *
+ *
+ *
+ *              1      /  (sum_j[(hj-H)*cos(w(tj-tau))])^2 
+ * Pn(w) = ----------- | --------------------------------- 
+ *          2*sigma2   \     sum_j[(cos(w(tj-tau)))^2]           
+ *
+ *
+ *                              (sum_j[(hj-H)*sin(w(tj-tau))])^2 \
+ *                        +    --------------------------------- | 
+ *                                 sum_j[(cos(w(tj-tau)))^2]     /
+ *
+ *
+ *
+ *
+ * H=sum_i[hi]/N       sigma2=sum_i[(hi-H)^2]/(N-1)
+ * 
+ *
+ *                 sum_j[sin(2*w*tj)]  
+ * tan (2*w*tau) = ------------------ 
+ *                 sum_j[cos(2*w*tj)]
+ *
+ *
+ * PAINFULLY SLOW
+ * NEED TO BE REWRITTEN TO DO A FAST TRANSFORM (RECURSIVE)
+ *
+ *
+ *
+ *****************************************************************************
+ *
+ * History:	10/07/04	bjg	v1.0              
+ *              11/04/04        bjg     v1.1 
+ * 
+ *                         ----v1.1 CHANGES WERE CANCELLED ---
+ *              12/06/04        bjg     v1.2   
+ *              12/13/04        bjg     v1.3 Changed N and i to long   
+ *                                           Initialize N to 0  
+ *		06/03/05	wvd	v1.4 Delete unused variables.
+ * 
+ *
+ ***************************************************************************/
+
+
+
+#include <stdlib.h>
+#include <stdio.h>
+#include <string.h>
+#include <time.h>
+#include <unistd.h>
+#include <math.h>
+
+
+#include "calfuse.h"
+
+
+static char CF_PRGM_ID[]= "ttag_lightcurve_periodogram";
+static char CF_VER_NUM[]= "1.1";
+
+
+
+int main(int argc,char *argv[]){
+  
+ 
+  
+  char       input_filename[FLEN_CARD],output_filename[FLEN_CARD];
+  
+  FILE     * output_file;
+  FILE     * input_file;
+
+  float      minf,maxf;
+  float      stepf;
+
+
+  double     H;
+  double     sigma2;
+  double     tau;
+
+
+  double     val1,val2;
+  double   * t;
+  double   * h;
+  double     total1,total2,total3,total4;
+  double     aux;
+  double     Pn;
+  double     f;
+  double     j0=0;
+
+  long        i, N;
+  long ndx;
+
+  int        time_unit=0;
+
+  int optc;
+
+  char opts[] = "hsv:";
+
+  char usage[] = 
+    "Usage:\n"
+    "  ttag_lightcurve_periodogram [-hs] [-v level] input_file output_file\n"
+    "                                              minf, maxf, stepf\n"
+    "Arguments:\n"
+    "  input_file  : an ASCII file with 2 columns :\n"
+    "                   - time (JD or MJD, Helio- or Geo-centric)\n"
+    "                   - countrate\n\n"
+    "  output_file : an ASCII file with 2 columns :\n" 
+    "                   - frequency (Hz)\n"
+    "                   - normalized estimated power spectral density\n\n"
+    "  minf        : start frequency (Hz)\n"
+    "  maxf        :   end frequency (Hz)\n"
+    "  stepf       :  frequency step (Hz)\n";
+
+  char option[] =
+    "Options:\n"
+    "  -h:  this help message\n"
+    "  -v:  verbosity level (=1; 0 is silent)\n"
+    "  -s:  time is in seconds instead of days\n";
+
+  verbose_level = 1;
+  
+  
+  /* Check number of options and arguments */
+  while ((optc = getopt(argc, argv, opts)) != -1) {
+    switch(optc) {    
+    case 'h':
+      printf("%s\n%s", usage, option);
+      return EXIT_SUCCESS;
+    case 'v':
+      verbose_level = atoi(optarg);
+      break;
+    case 's':
+      time_unit=1;
+      break;
+    }
+  }
+
+  /* Initialize error checking. */
+  cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+  if (argc != optind+5)
+    cf_if_error("%s\nIncorrect number of program arguments", usage);
+  
+  
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Started execution.");
+  
+  strcpy(input_filename,argv[optind]); 
+  strcpy(output_filename,argv[optind+1]);     
+  sscanf(argv[optind+2],"%f",&minf);   
+  sscanf(argv[optind+3],"%f",&maxf);
+  sscanf(argv[optind+4],"%f",&stepf);          
+  
+    
+  
+  if ((input_file = fopen (input_filename, "r")) == NULL){
+    cf_if_error ("Unable to open file %s\n", input_filename);
+  }
+
+
+  N=0;
+  while (fscanf(input_file,"%lf %lf",&val1,&val2)!=EOF){
+    N++;
+  }
+
+  t=(double *)malloc(N*sizeof(double));
+  h=(double *)malloc(N*sizeof(double));
+
+
+  fseek(input_file,0,SEEK_SET);
+
+  i=0;
+  total1=0;
+  while (fscanf(input_file,"%lf %lf",&val1,&val2)!=EOF){
+    if (i==0) { 
+      t[i]=0.0; j0=val1;
+    }
+    else {
+      if (time_unit) t[i]=val1-j0;
+      else t[i]=(val1-j0)*3600.0*24;
+    }
+
+    h[i]=val2;
+
+    total1+=h[i];
+
+    i++;
+
+  }
+  
+  H=total1/N;
+
+  total1=0;
+  for (i=0;i<N;i++){
+    aux=(h[i]-H);
+    total1+=aux*aux;
+  }
+
+  sigma2=total1/(N-1);
+
+
+
+  if ((output_file = fopen(output_filename,"w")) == NULL){
+    fclose(input_file);
+    cf_if_error ("Unable to create file %s\n", output_filename);    
+  }
+  
+  ndx=0;
+  for (f=minf; f<=maxf; f+=stepf){
+    cf_verbose(4,"n=%ld;minf=%f;maxf=%f;freq=%lf",ndx,minf,maxf,f);
+    ndx++;
+    total1=0;
+    total2=0;
+    for (i=0;i<N;i++){
+      total1+=sin(4*M_PI*f*t[i]);
+      total2+=cos(4*M_PI*f*t[i]);
+    }
+
+
+    tau=atan(total1/total2)/(4*M_PI*f);
+
+
+
+    total1=0;
+    total2=0;
+    total3=0;
+    total4=0;
+
+    for (i=0;i<N;i++){
+      aux=cos(2*M_PI*f*(t[i]-tau));
+      total1+=(h[i]-H)*aux;
+      total2+=aux*aux;
+      aux=sin(2*M_PI*f*(t[i]-tau));
+      total3+=(h[i]-H)*aux;
+      total4+=aux*aux;
+    }
+
+    Pn=(total1*total1/total2+total3*total3/total4)/(2*sigma2);
+   
+      
+    fprintf(output_file,"%10lf  %10lf\n",f,Pn);
+
+  }
+
+  fclose(input_file);
+  fclose(output_file);
+  
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished execution.");
+  return EXIT_SUCCESS;
+  
+}
+
+
diff --git a/src/cal/geom/Makefile.orig.orig b/src/cal/geom/Makefile.orig.orig
new file mode 100644
index 0000000..5b23afd
--- /dev/null
+++ b/src/cal/geom/Makefile.orig.orig
@@ -0,0 +1,43 @@
+VERSION=	v1.8
+
+CALFUSEDIR=	${PWD}/../../..
+
+# Symbols for include directories
+FUSEINCLDIR=	-I${CALFUSEDIR}/include
+
+# Symbols used for compiling
+CC=		cc
+#  Romelfanger's optimizations
+# OPT=		-fast -xO5 -xtarget=ultra2 -xarch=v8plusa
+#
+#  SunWorld's optimizations
+# OPT=		-p -v -xO2 -xdepend -xchip=ultra -xarch=generic
+OPT=		-g
+#OPT=		-O -DCFORTRAN -KPIC -DSOLARIS
+CFLAGS=		${OPT} ${FUSEINCLDIR}
+
+# Symbols used for creating shared binaries
+FUSEBINDIR=	${CALFUSEDIR}/bin
+FUSELIBDIR=	-L${CALFUSEDIR}/lib
+LIBDIR=		-L/opt/SUNWspro/lib
+FUSELIBS=	-lsla -lcfitsio -lcf
+LIBS=		-lc -lm -lnsl -ldl -lsocket -lsunmath -lM77 -lF77
+LDFLAGS=	
+
+# binaries to be made
+
+BINS=		make_geom_file
+
+all:		${BINS}
+		chmod g+rw ${BINS}
+
+install:	all
+		/bin/cp ${BINS} ${FUSEBINDIR}
+
+clean:		
+		/bin/rm -f ${BINS}
+
+make_geom_file:
+		${CC} ${CFLAGS} -o make_geom_file make_geom_file.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
diff --git a/src/cal/geom/make_geom_file b/src/cal/geom/make_geom_file
new file mode 100755
index 0000000..caf2ab1
--- /dev/null
+++ b/src/cal/geom/make_geom_file
diff --git a/src/cal/geom/make_geom_file.c b/src/cal/geom/make_geom_file.c
new file mode 100644
index 0000000..52789e8
--- /dev/null
+++ b/src/cal/geom/make_geom_file.c
@@ -0,0 +1,185 @@
+/*******************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *******************************************************************************
+ *
+ * Synopsis:    make_geom_file
+ *
+ * Description: Make the geom(Y distortion) file:  copy the distortion
+ *		image from a FITS file produced by Rich Robinson, and
+ *		write it out in the format required by CALFUSE.
+ *
+ * Usage:	make_geom_file version
+ *
+ *		The program will read the files ydist_1a_2d.fit, 
+ *		ydist_1b_2d.fit, etc and write the files geom1axxx.fit
+ *		(where xxx is the version number specified on the command line).
+ *
+ *		The output file has an empty primary extension (containing
+ *		just header keywords), an empty extension for X distortions
+ *		(not presently used as such), and a full-size image containing
+ *		the Y distortion as a function of position (FLOAT's).
+ *
+ * History:     10/19/00        jwk     Begin work.
+ ******************************************************************************/
+
+#include <stdio.h>
+#include "calfuse.h"
+#define EFFMJD 50000.0
+#define NXMAX 16384
+#define NYMAX 1024
+
+static char CF_PRGM_ID[] = "make_geom_file";
+static char CF_VER_NUM[] = "1.1";
+
+
+int main(int argc, char *argv[])
+{
+    char *segment[]={"1A","1B","2A","2B"};
+    char *segments[]={"1a","1b","2a","2b"};
+    char extname[]="GEOMETRIC DISTORTION";
+    char infile[80];
+    char outfile[80];
+    int	version;
+    int   i, j, hdutype, status=0, nullval=0, anynull=0;
+    int   ix, iy;
+    int	ival;
+    int   naxis;
+    long  naxes[2];
+    int   nxpix, nypix;
+    float effmjd;
+    float bscale, bzero, datamin, datamax;
+    float *inbuf;
+    fitsfile *geomfits, *infits;
+
+    /* Initialize error checking */
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+    if (argc != 2)
+	{
+	fprintf (stderr, "Usage: make_geom_file version\n");
+	exit (-1);
+	}
+
+    version = (int) strtol (argv[1], (char **) NULL, 10);
+    if ((version <0) || (version > 999))
+	{
+	fprintf (stderr, "Illegal version value: %s\n", argv[1]);
+	exit (-1);
+	}
+
+
+for (i=0; i<4; i++) {  /* 1A,1B,2A,2B */
+    /* open the y-distortion file, move to first extension (the one with
+       the Y distortion image in it) */
+    sprintf(infile, "ydist_%2.2s_2d.fit", segments[i]);
+    FITS_open_file (&infits, infile, READONLY, &status);
+    FITS_movabs_hdu (infits, 2, &hdutype, &status);
+    FITS_read_key (infits, TINT, "NAXIS1", &nxpix, NULL, &status);
+    FITS_read_key (infits, TINT, "NAXIS2", &nypix, NULL, &status);
+    if (nxpix != NXMAX)
+	{
+	fprintf (stderr, "NAXIS1 = %d, not %d\n", nxpix, NXMAX);
+	exit (-1);
+	}
+
+    if (nypix != NYMAX)
+	{
+	fprintf (stderr, "NAXIS2 = %d, not %d\n", nypix, NYMAX);
+	exit (-1);
+	}
+
+    /* buffers to hold one row of data at a time */
+    inbuf = (float *) calloc (nxpix, sizeof(float));
+
+    /* create the output file */
+    naxis = 0;
+    naxes[0] = 0;
+    naxes[1] = 0;
+
+    sprintf(outfile,"geom%2.2s%03d.fit", segments[i], version);
+    printf("%20.20s\n",outfile); 
+
+    FITS_create_file (&geomfits,outfile,&status);
+    FITS_create_img (geomfits, SHORT_IMG, naxis, naxes, &status);
+
+    /* populate basic keywords */
+    FITS_write_key (geomfits, TSTRING, "CALFTYPE", "GEOM", 
+		   "Calibration file type", &status);
+
+    FITS_write_key (geomfits,TINT,"CALFVERS",&version,
+		   "Calibration file version", &status);
+
+    FITS_write_key (geomfits,TSTRING,"DETECTOR",segment[i],
+                   "detector (1A, 1B, 2A, 2B", &status);
+
+    effmjd=EFFMJD;
+    FITS_write_key (geomfits,TFLOAT,"EFFMJD",&effmjd,
+		   "Date on which file should be applied (MJD)", &status);
+
+    ival = 1;
+    FITS_write_key (geomfits, TINT, "SPECBINX", &ival,
+		"Binning in Detector X coordinate for HIST mode", &status);
+
+    FITS_write_key (geomfits, TINT, "SPECBINY", &ival,
+		"Binning in Detector Y coordinate for HIST mode", &status);
+
+    FITS_write_date (geomfits, &status);
+
+    FITS_write_key (geomfits,TSTRING,"AUTHOR","RICH ROBINSON",
+		   "Author of file", &status);
+
+    /* create empty first extension (HDU 2) for X distortions;
+     * not used presently, but is kept for possible later use.
+     */
+    FITS_create_img (geomfits, SHORT_IMG, naxis, naxes, &status);
+    FITS_write_comment (geomfits, "No x correction for geometric distortion",
+	&status);
+
+    /* now create extension to hold Y distortions */
+    naxis = 2;
+    naxes[0] = nxpix;
+    naxes[1] = nypix;
+    bzero = 0.;
+    bscale = 0.01;
+    datamin = 0.;
+    datamax = 0.;
+
+    /* use SHORT_IMG to force bitpix=16 */
+    FITS_create_img (geomfits, SHORT_IMG, naxis, naxes, &status);
+    FITS_write_key (geomfits, TFLOAT, "BSCALE", &bscale, "Scale factor",
+	&status);
+    FITS_write_key (geomfits, TFLOAT, "BZERO", &bzero, "Zero level",
+	&status);
+
+    /* now loop over rows of distortion image */
+    for (iy=0; iy<nypix; iy++)
+	{
+	FITS_read_img (infits, TFLOAT, nxpix*iy+1, nxpix, &nullval,
+		inbuf, &anynull, &status);
+	for (ix=0; ix<nxpix; ix++)
+		{
+		if (inbuf[ix] < datamin)
+			datamin = inbuf[ix];
+		if (inbuf[ix] > datamax)
+			datamax = inbuf[ix];
+		}
+	/* cfitsio will do conversion to SHORT using bscale, bzero */
+	FITS_write_img (geomfits, TFLOAT, nxpix*iy+1, nxpix, inbuf, &status);
+	}
+
+    FITS_write_key (geomfits, TFLOAT, "DATAMIN", &datamin, "Minimum value",
+	&status);
+    FITS_write_key (geomfits, TFLOAT, "DATAMAX", &datamax, "Maximum value",
+	&status);
+
+
+    /* done with this segment */
+    FITS_close_file(geomfits, &status);
+    FITS_close_file(infits, &status);
+
+} /* end of loop over segments */
+
+    return 0;
+}
diff --git a/src/cal/get_tle/GetTLE.class b/src/cal/get_tle/GetTLE.class
new file mode 100644
index 0000000..6d32037
--- /dev/null
+++ b/src/cal/get_tle/GetTLE.class
diff --git a/src/cal/get_tle/GetTLE.java b/src/cal/get_tle/GetTLE.java
new file mode 100644
index 0000000..68e88d3
--- /dev/null
+++ b/src/cal/get_tle/GetTLE.java
@@ -0,0 +1,110 @@
+/*
+ * GetTLE.java
+ *
+ * Created on January 16, 2005, 8:34 PM
+ */
+import java.net.URL;
+import java.net.URLConnection;
+import java.io.*;
+
+import java.util.Map;
+import java.util.List;
+/**
+ *
+ * @author fred
+ */
+public class GetTLE {
+    
+    /** Creates a new instance of GetTLE */
+    public GetTLE() {
+    }
+    
+    /**
+     * @param args the command line arguments
+     */
+    static final String host="www.space-track.org";
+    static final String loginURL="/perl/login.pl";
+    static final String dataURL="/perl/id_query.pl?ids=25791&timeframe=last5&common_name=yes&sort=catnum&descending=yes&ascii=yes&_submit=Submit&_submitted=1";
+    static final String username="mromelfanger";
+    static final String password="FuseJHU1";
+  
+    static final String outputFile = "/data1/fuse/calfuse/caltemp/five.tle";
+    static final String logFile = "/data1/fuse/calfuse/caltemp/get_tle.logfile";
+/*
+    static final String outputFile = "/caltemp/five.tle";
+    static final String logFile = "/caltemp/get_tle.logfile";
+*/
+    public static void main(String[] args) {
+        // TODO code application logic here
+        try {
+            /*
+             * Open the login url and get the session cookie back.
+             */
+            PrintWriter log = new PrintWriter(new OutputStreamWriter(new FileOutputStream(logFile)));
+            PrintWriter out = new PrintWriter(new OutputStreamWriter(new FileOutputStream(outputFile)));
+            
+            URL u = new URL("http://"+host+loginURL+"?username="+username+"&password="+password+"&_submitted=1&_submit=Submit");
+
+            URLConnection c = u.openConnection();
+            Map m = c.getHeaderFields();
+            List l = (List) m.get("Set-Cookie");
+            String session = null;
+            for(int i=0;i!=l.size();i++) {
+                String s = (String) l.get(i);
+                if(s.startsWith("spacetrack_session=")) {
+                    int end = s.indexOf(";");
+                    if(end < 0)
+                        end = s.length();
+                    session = s.substring(0, end);
+                    break;
+                }
+            }
+            InputStream is = c.getInputStream();
+            BufferedReader br = new BufferedReader(new InputStreamReader(is));
+            String s;
+            while((s = br.readLine()) != null)
+                log.println(s);
+            is.close();
+            
+            if(session == null) {
+                out.println("Could not get session id");
+                System.exit(1);
+            }
+
+            /*
+             * Use the session cookie to query for the fuse data.
+             */
+            
+            u = new URL("http://"+host+dataURL);
+            c = u.openConnection();
+            c.setRequestProperty("Cookie", session);
+            is = c.getInputStream();
+            br = new BufferedReader(new InputStreamReader(is));
+            /*
+             * Read each line and keep what is between the pre's, add an extra
+             * line at the end.
+             */
+            boolean collect = false;
+	    out.println();
+            while((s = br.readLine()) != null) {
+                log.println(s);
+                if(s.startsWith("<pre>")) {
+/*                    br.readLine(); */
+                    collect = true;
+                } else if(s.startsWith("</pre>")) {
+                    break;
+                } else if(collect) {
+                    out.println(s);
+                }
+            }
+            out.println();
+            br.close();
+            is.close();
+            out.close();
+            log.close();
+
+        } catch (Throwable e) {
+            e.printStackTrace();
+        }
+    }
+}
diff --git a/src/cal/get_tle/add_tle.pl b/src/cal/get_tle/add_tle.pl
new file mode 100755
index 0000000..feaa1ba
--- /dev/null
+++ b/src/cal/get_tle/add_tle.pl
@@ -0,0 +1,182 @@
+#!/usr/local/bin/perl
+use FileHandle;
+
+# ***************************************************
+# add_tle.pl
+# 
+# This Perl module will read in the latest five orbital elements
+# from the file five.tle (which was created by get_tle.pl) and
+# add any new orbital elements to the file FUSE.TLE.  The file
+# FUSE.TLE is in descending order (i.e. the most recent elements
+# are first).  In order to prepend the new TLE onto the old list
+# I found it was easiest to store everything in a temporary file
+# TEMP.TLE and rewrite FUSE.TLE.
+#
+# Author: Ed Murphy
+#
+# History:  Written  July 27, 1999
+#
+# ***************************************************
+
+# Define the file names.  old_maintle_filename is not actually opened,
+# but is used in a system call at the end of the program. 
+
+$input_filename = "/data1/fuse/calfuse/caltemp/five.tle";
+$maintle_filename = "/data1/fuse/calfuse/calfiles/FUSE.TLE";
+$old_maintle_filename = "/data1/fuse/calfuse/caltemp/FUSE.OLD";
+$temp_filename = "/data1/fuse/calfuse/caltemp/TEMP.TLE";
+
+# Open the files.
+open (TLE_INFILE, "<$input_filename") || die "Cannot open $input_filename";
+open (TLE_TEMPFILE, ">$temp_filename") || die "Cannot open $temp_filename";
+open (TLE_MAINFILE, "<$maintle_filename") || die "Cannot open $maintle_filename";
+
+# Read the first two lines from the maintle file to get the date of the
+# most recent set of TLEs.  Save these lines for later output.
+    $lineout1 = <TLE_MAINFILE>;
+    $lineout2 = <TLE_MAINFILE>;
+    $last_date = substr($lineout2,18,14);
+
+# get rid of the blank line at the beginning of five.tle file
+    $line = <TLE_INFILE>;  
+
+# Cycle through the five.tle file and look for files more recent than
+# last_date.  
+    while ($line1 = <TLE_INFILE>) {
+        $sat_name = substr($line1,0,4);
+        $line2 = <TLE_INFILE>;
+        $line3 = <TLE_INFILE>;
+        $tle_date = substr($line2,18,14);
+        $id2 = substr($line2, 2, 5);
+        $id3 = substr($line3, 2, 5);
+        # if the TLE is more recent, print it out to the TEMP file.
+        if (($tle_date > $last_date+0.05) && ($sat_name eq "FUSE") && ($id2 == 25791) && ($id3 == 25791)) {
+            &check_tle;
+            print TLE_TEMPFILE $line1;
+            print TLE_TEMPFILE $line2;
+            print TLE_TEMPFILE $line3;
+            # Send this output to screen to make sure TLEs look OK
+            if ($tle_flag != 0) {
+		print STDOUT "ERROR: Possible error in TLE:\n";
+            }
+            print STDOUT "The new TLEs are:\n";
+            print STDOUT $line1;
+            print STDOUT $line2;
+            print STDOUT $line3;
+	}
+
+    }
+
+# Now add the MAINTLE file to the end of the TEMPFILE
+    print TLE_TEMPFILE $lineout1;
+    print TLE_TEMPFILE $lineout2;
+    while ($line1 = <TLE_MAINFILE>) {
+            print TLE_TEMPFILE $line1;
+    }
+ 
+    close (TLE_INFILE);
+    close (TLE_MAINFILE);
+    close (TLE_TEMPFILE);
+
+# Move the MAINFILE into the old_maintle filename
+# Move the TEMPFILE to be the MAINFILE
+# Remove the five.tle file.
+    system("mv $maintle_filename $old_maintle_filename");
+    system("mv $temp_filename $maintle_filename");
+    system("chmod ug+rw $maintle_filename");
+    system("chgrp sdp $maintle_filename");
+    system("rm -f $input_filename");
+
+### end of Perl script
+
+sub check_tle {
+
+    $tle_flag = 0;
+
+    &parse_lines;
+
+    &calculate_a0;
+
+    &calculate_orbs;
+
+    if (($mean_mot > 14.391) || ($mean_mot < 14.389)) {
+	$tle_flag = 1;
+        print STDOUT "Possible error in mean motion $mean_mot \n";
+    }
+    if (($incl > 24.990) || ($incl < 24.975)) {
+	$tle_flag = 1;
+        print STDOUT "Possible error in inclination $incl \n";
+    }
+    if (($eccen > 0.00120) || ($eccen < 0.00108)) {
+	$tle_flag = 1;
+        print STDOUT "Possible error in eccentricity $eccen \n";
+    }
+    if (($semiax > 7145.0) || ($semiax < 7143.0)) {
+	$tle_flag = 1;
+        print STDOUT "Possible error in semi-major axis $semia \n";
+    }
+    if (($apogee > 777.0) || ($apogee < 773.0)) {
+	$tle_flag = 1;
+        print STDOUT "Possible error in apogee $apogee \n";
+    }
+    if (($perigee > 760.0) || ($perigee < 756.0)) {
+	$tle_flag = 1;
+        print STDOUT "Possible error in perigee $perigee \n";
+    }
+
+}
+
+sub parse_lines {
+$year = substr($line2, 18, 2);
+$doy = substr($line2, 20, 3);
+$dayfrac = substr($line2, 23, 9);
+$epoch = $year.$doy.$dayfrac;
+$incl = substr($line3, 9, 8);
+$raan = substr($line3, 17,8);
+$eccen = substr($line3, 26, 7);
+$eccen = "0." . $eccen;
+$mean_mot = substr($line3, 52, 11);
+$mean_anom = substr($line3, 43, 8);
+$arg_perig = substr($line3, 34, 8);
+
+
+if ($year > 50) {
+    $year += 1900;
+} else {
+    $year += 2000;
+}
+
+$dayfrac = "0".$dayfrac;
+
+}
+
+sub calculate_a0 {
+
+$mu = 3.986005E5;
+$pi = 3.14159265358979;
+$radian = 0.0174532925200;
+
+$mm=2.0*$pi*$mean_mot/(24.0*60.0);
+$ke=0.74366916E-1;
+$k2=5.413080E-4;
+$a1=($ke/$mm)**(2.0/3.0);
+$inrad = $incl * $radian;
+
+$d1=3.0/2.0*$k2/($a1*$a1)*(3.0*cos($inrad)*cos($inrad)-1.0)/((1.0-$eccen*$eccen)
+**(3.0/2.0));
+$a0=$a1*(1.0-$d1/3.0-$d1*$d1-134.0/81.0*$d1*$d1*$d1);
+$d0=3.0/2.0*$k2/($a0*$a0)*(3.0*cos($inrad)*cos($inrad)-1.0)/((1.0-$eccen*$eccen)
+**(3.0/2.0));
+$semiax=$a0/(1-$d0)*6378.135;
+
+}
+
+sub calculate_orbs {
+
+$period = 60.0*24.0/($mean_mot/(1+$d0));
+$cax=$eccen*$semiax;
+$perigee=$semiax-$cax-6378.1;
+$apogee=$semiax+$cax-6378.1;
+
+}
+
diff --git a/src/cal/get_tle/check_tle.dat b/src/cal/get_tle/check_tle.dat
new file mode 100644
index 0000000..ded4897
--- /dev/null
+++ b/src/cal/get_tle/check_tle.dat
@@ -0,0 +1,266 @@
+108.630 773.22 757.14 7143.28 310.64 24.9828 305.80  54.35 0.001125
+107.936 773.22 757.16 7143.29 314.88 24.9826 313.12  47.02 0.001124
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+210.108 774.90 758.26 7144.68 119.07 24.9830 180.03 180.02 0.001164
+209.137 774.92 758.24 7144.68 124.99 24.9829 190.07 170.00 0.001167
+208.859 774.88 758.28 7144.68 126.68 24.9830 192.78 167.30 0.001162
+208.166 774.88 758.29 7144.68 130.92 24.9829 200.09 160.00 0.001161
+207.126 774.81 758.36 7144.68 137.26 24.9830 210.54 149.58 0.001151
+206.155 774.77 758.40 7144.69 143.19 24.9831 220.62 139.52 0.001146
+205.114 774.74 758.44 7144.69 149.54 24.9835 231.12 129.03 0.001141
+204.213 774.68 758.50 7144.69 155.04 24.9835 240.13 120.03 0.001132
+203.172 774.62 758.57 7144.69 161.38 24.9835 250.92 109.26 0.001123
+202.132 774.57 758.62 7144.69 167.73 24.9837 261.69  98.49 0.001117
+201.161 774.54 758.65 7144.70 173.66 24.9837 271.78  88.39 0.001113
+200.190 774.54 758.65 7144.70 179.58 24.9838 281.91  78.26 0.001112
+200.121 774.52 758.67 7144.70 180.04 24.9842 284.37  75.80 0.001110
+199.219 774.51 758.68 7144.70 185.54 24.9840 293.67  66.50 0.001107
+198.179 774.47 758.73 7144.70 191.89 24.9844 304.62  55.53 0.001102
+197.208 774.43 758.77 7144.70 197.81 24.9845 315.10  45.03 0.001097
+196.167 774.41 758.80 7144.70 204.16 24.9848 326.28  33.84 0.001093
+195.404 774.40 758.81 7144.70 208.81 24.9845 334.28  25.82 0.001091
+195.266 774.39 758.81 7144.70 209.66 24.9847 335.90  24.21 0.001091
+194.225 774.39 758.82 7144.71 216.00 24.9849 347.09  12.99 0.001089
+193.185 774.39 758.82 7144.71 222.35 24.9850 358.14   1.91 0.001090
+192.145 774.40 758.82 7144.71 228.70 24.9850   9.20 350.84 0.001091
+191.243 774.42 758.80 7144.71 234.20 24.9852  18.68 341.33 0.001093
+189.578 774.47 758.75 7144.71 244.35 24.9847  35.63 324.35 0.001100
+188.538 774.53 758.70 7144.72 250.70 24.9847  46.49 313.47 0.001108
+187.567 774.56 758.68 7144.72 256.62 24.9847  56.72 303.22 0.001111
+187.220 774.58 758.66 7144.72 258.73 24.9849  60.33 299.61 0.001115
+186.596 774.58 758.66 7144.72 262.54 24.9848  66.84 293.09 0.001114
+185.556 774.61 758.64 7144.73 268.89 24.9850  77.79 282.14 0.001118
+184.585 774.64 758.62 7144.73 274.81 24.9851  87.90 272.03 0.001121
+183.614 774.64 758.63 7144.73 280.73 24.9851  98.00 261.93 0.001120
+182.643 774.66 758.62 7144.74 286.65 24.9852 108.11 251.82 0.001123
+181.533 774.65 758.63 7144.74 293.42 24.9851 119.74 240.20 0.001121
+180.423 774.66 758.64 7144.75 300.19 24.9851 131.33 228.62 0.001121
+179.730 774.66 758.64 7144.75 304.42 24.9851 138.60 221.36 0.001121
+178.689 774.66 758.65 7144.76 310.76 24.9851 149.51 210.48 0.001120
+178.551 774.66 758.65 7144.76 311.61 24.9851 150.96 209.03 0.001120
+177.926 774.68 758.64 7144.76 315.41 24.9853 157.55 202.45 0.001123
+176.955 774.50 758.84 7144.77 321.34 24.9860 169.04 190.98 0.001096
diff --git a/src/cal/get_tle/check_tle.pl b/src/cal/get_tle/check_tle.pl
new file mode 100755
index 0000000..483692e
--- /dev/null
+++ b/src/cal/get_tle/check_tle.pl
@@ -0,0 +1,100 @@
+#!/usr/local/bin/perl
+use FileHandle;
+
+# ***************************************************
+# add_tle.pl
+# 
+# This Perl module will read in the latest five orbital elements
+# from the file five.tle (which was created by get_tle.pl) and
+# add any new orbital elements to the file FUSE.TLE.
+#
+# Author: Ed Murphy
+#
+# History:  Written  July 27, 1999
+#
+# ***************************************************
+
+# Define the file names.  old_maintle_filename is not actually opened,
+# but is used in a system call at the end of the program. 
+
+$maintle_filename = "/data1/fuse/calfuse/calfiles/FUSE.TLE";
+$outtle_filename = "check_tle.dat";
+
+# Open the files.
+open (TLE_MAINFILE, "<$maintle_filename") || die "Cannot open $maintle_filename";
+open (TLE_OUT, ">$outtle_filename") || die "Cannot open $outtle_filename";
+
+# Read the first two lines from the maintle file to get the date of the
+# most recent set of TLEs.  Save these lines for later output.
+while ($line1 = <TLE_MAINFILE>) {
+    $line2 = <TLE_MAINFILE>;
+    $line3 = <TLE_MAINFILE>;
+
+    &parse_lines;
+
+    &calculate_a0;
+    &calculate_orbs;
+
+    printf TLE_OUT "%7.3f %6.2f %6.2f %7.2f %6.2f %7.4f %6.2f %6.2f %8.6f\n",$day, $apogee, $perigee, $semiax, $raan, $incl, $mean_anom, $arg_perig, $eccen;
+
+}
+
+    close (TLE_MAINFILE);
+    close (TLE_OUT);
+
+### end of Perl script
+
+
+sub parse_lines {
+$year = substr($line2, 18, 2);
+$doy = substr($line2, 20, 3);
+$dayfrac = substr($line2, 23, 9);
+$day=$doy.$dayfrac;
+$epoch = $year.$doy.$dayfrac;
+$incl = substr($line3, 9, 8);
+$raan = substr($line3, 17,8);
+$eccen = substr($line3, 26, 7);
+$eccen = "0." . $eccen;
+$mean_mot = substr($line3, 52, 11);
+$mean_anom = substr($line3, 43, 8);
+$arg_perig = substr($line3, 34, 8);
+
+
+if ($year > 50) {
+    $year += 1900;
+} else {
+    $year += 2000;
+}
+
+$dayfrac = "0".$dayfrac;
+
+}
+
+sub calculate_a0 {
+
+$mu = 3.986005E5;
+$pi = 3.14159265358979;
+$radian = 0.0174532925200;
+
+$mm=2.0*$pi*$mean_mot/(24.0*60.0);
+$ke=0.74366916E-1;
+$k2=5.413080E-4;
+$a1=($ke/$mm)**(2.0/3.0);
+$inrad = $incl * $radian;
+
+$d1=3.0/2.0*$k2/($a1*$a1)*(3.0*cos($inrad)*cos($inrad)-1.0)/((1.0-$eccen*$eccen)**(3.0/2.0));
+$a0=$a1*(1.0-$d1/3.0-$d1*$d1-134.0/81.0*$d1*$d1*$d1);
+$d0=3.0/2.0*$k2/($a0*$a0)*(3.0*cos($inrad)*cos($inrad)-1.0)/((1.0-$eccen*$eccen)**(3.0/2.0));
+$semiax=$a0/(1-$d0)*6378.135;
+
+}
+
+sub calculate_orbs {
+
+$period = 60.0*24.0/($mean_mot/(1+$d0));
+$cax=$eccen*$semiax;
+$perigee=$semiax-$cax-6378.1;
+$apogee=$semiax+$cax-6378.1;
+
+}
+
diff --git a/src/cal/get_tle/check_tle.pro b/src/cal/get_tle/check_tle.pro
new file mode 100644
index 0000000..5388d9d
--- /dev/null
+++ b/src/cal/get_tle/check_tle.pro
@@ -0,0 +1,73 @@
+;
+fname='check_tle.dat'
+get_lun,unit0
+openr,unit0,fname
+day=fltarr(1000)
+apogee=fltarr(1000)
+perigee=fltarr(1000)
+semiax=fltarr(1000)
+raan=fltarr(1000)
+incl=fltarr(1000)
+mean_anom=fltarr(1000)
+arg_perig=fltarr(1000)
+eccen=fltarr(1000)
+d=0.0
+a=0.0
+p=0.0
+sem=0.0
+ra=0.0
+inc=0.0
+ma=0.0
+ap=0.0
+ec=0.0
+j=0
+while (not EOF(unit0)) do begin
+   readf,unit0,d,a,p,sem,ra,inc,ma,ap,ec
+   day[j]=d
+   apogee[j]=a
+   perigee[j]=p
+   semiax[j]=sem
+   raan[j]=ra
+   incl[j]=inc
+   mean_anom[j]=ma
+   arg_perig[j]=ap
+   eccen[j]=ec
+   j=j+1
+endwhile
+day=day(0:j-1)
+apogee=apogee(0:j-1)
+perigee=perigee(0:j-1)
+semiax=semiax(0:j-1)
+raan=raan(0:j-1)
+incl=incl(0:j-1)
+mean_anom=mean_anom(0:j-1)
+arg_perig=arg_perig(0:j-1)
+eccen=eccen(0:j-1)
+close,unit0
+free_lun,unit0
+!x.title='Day of Year 1999'
+!y.title='Arbitrary units'
+!p.title='FUSE Orbital Elements'
+!x.style=1
+!y.range=[0,1000]
+!x.range=[170,day(0)+10]
+!p.charsize=1.7
+!p.linestyle=0
+plot,day,apogee
+oplot,day,perigee
+oplot,day,semiax*100.0-714470.0+700.0
+oplot,day,raan*2.0
+oplot,day,incl*3500.0-87445.0+900.0
+oplot,day,mean_anom*2.0
+oplot,day,arg_perig*2.0
+oplot,day,eccen/2E-6
+xyouts,day(0),apogee(0),"Apogee",charsize=1.0
+xyouts,day(0),perigee(0),"Perigee",charsize=1.0
+xyouts,day(0),semiax(0)*100.0-714470.0+700.0,"Semimajor axis*100",charsize=1.0
+xyouts,day(0),raan(0)*2.0,"RAAN*2",charsize=1.0
+xyouts,day(0),incl(0)*3500.0-87445.0+900.0,"incl*3500",charsize=1.0
+xyouts,day(0),mean_anom(0)*2.0,"mean anomaly*2",charsize=1.0
+xyouts,day(0),arg_perig(0)*2.0,"argument of perigee*2",charsize=1.0
+xyouts,day(0),eccen(0)/2E-6,"eccen/2E-6",charsize=1.0
+
+end
diff --git a/src/cal/get_tle/get_tle.pl b/src/cal/get_tle/get_tle.pl
new file mode 100755
index 0000000..33b72e5
--- /dev/null
+++ b/src/cal/get_tle/get_tle.pl
@@ -0,0 +1,148 @@
+#!/usr/local/bin/perl
+use FileHandle;
+use IPC::Open2;
+
+###
+# OIG TLE retrieval program
+# DJG - 6/14/98
+#
+# Uses a file called "one" which has sat numbers to get
+#
+# Places all output in a single file called "five.tle".
+#
+###
+
+### Configure:
+##$login = "emurphy";
+##$passwd = "bdr529";
+
+$login = "mromelfanger";
+$passwd = "fusejhu";
+$output_filename = "/data1/fuse/calfuse/caltemp/five.tle";
+$log_filename = "/data1/fuse/calfuse/caltemp/get_tle.logfile";
+
+### (end of configure section)
+
+# system("fixlist one tempone");
+# chop($satstoget = `cat tempone`);
+# system("rm -f tempone");
+
+$satstoget = "25791";
+
+# The "output" file collects debugging copies of everything that comes back.
+open(OUT,">$log_filename") || die "Could not open output file";
+
+# The following logs in to OIG and gets the first "continue" code
+
+$host = "oig1.gsfc.nasa.gov";
+#$url = "scripts/foxweb.dll/loginok\@app01?tdac=&ffv01=$login&ffv02=$passwd";
+$url = "scripts/foxweb.exe/loginok\@app01?tdac=&ffv01=$login&ffv02=$passwd";
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+while (<Reader>) {
+  print OUT "$_";  # copy each login screen line to the output file
+  if (/tdac=(\w+)\"/) {
+    $continuecode = $1;  # This code is the "continue" code
+  }
+}
+close(Reader);
+close(Writer);
+
+# $continuecode contains the very first "continue" code after login.
+
+print OUT "*** \n Starting User's Home Page output page \n***\n\n";
+
+# This url accesses the next screen (user home page)
+#$url = "scripts/foxweb.dll/favorhome\@app01?tdac=" . $continuecode;
+$url = "scripts/foxweb.exe/favorhome\@app01?tdac=" . $continuecode;
+# print $url; # debug print
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+
+while (<Reader>) {
+  print OUT "$_";      # copy each line to the output file
+
+  if(/tdac=(\w+)\"/) {
+
+#   Look for the "tle ad hoc query" code and save it
+    chop($word = "$_");
+    if ($word =~ /ftleadhoc.+tdac=(\w+)\"/) {
+      $tlequerycode = "$1";
+    }
+  }
+}
+# close(HOMEPAGE);
+# This access is to the "TLE ad hoc query" web page.
+#$url = "scripts/foxweb.dll/ftleadhoc\@app01?tdac=" . $tlequerycode;
+$url = "scripts/foxweb.exe/ftleadhoc\@app01?tdac=" . $tlequerycode;
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+
+while (<Reader>) {
+  print OUT "$_";  # copy each login screen line to the output file
+
+  # Look for the TLE "submit" code
+  chop($word = "$_");
+  if ($word =~ /tdac\" VALUE=\"(\w+)\"/) {
+    $gotcode2 = "$1";
+  }
+}
+close(Reader);
+close(Writer);
+
+# Compose the TLE query and submit it
+#$url = "scripts/foxweb.dll/ftleadhoc\@app01?tdac=" . $gotcode2;
+$url = "scripts/foxweb.exe/ftleadhoc\@app01?tdac=" . $gotcode2;
+$url .= "&ffv01=" . $satstoget . "&ffv02=standard&ffv03=catno&ffv04=five";
+
+# print "$url\n";  # debug print
+
+# Read the reply and copy the relevant lines to output_filename
+
+$copy = "no";
+open(TLEOUT,">$output_filename") || die "Error opening $output_filename";
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+
+while (<Reader>) {
+  if ($_ =~ /<P>/) {  # End copy operation
+    print "$_";       # write remaining limit to output file
+    $copy = "no";
+  }
+  if ($copy eq "yes") {
+    print TLEOUT "$_";   # copy every line to five.tle
+    # print "$_";          # and to the terminal
+  }
+  if (substr($_,0,5) eq "<PRE>") {  # Begin copy operation
+    $copy = "yes";
+  }
+}
+close(Reader);
+close(Writer);
+close(TLEOUT);
+
+# The following will remove all session files. You can comment it
+# out for debugging.
+# system("rm -f output");
+
+# The following script "fixes up" the output
+# system("fix/do.fix.one");
+
+### end of Perl script
+
diff --git a/src/cal/get_tle/get_tle.pl.OIG b/src/cal/get_tle/get_tle.pl.OIG
new file mode 100755
index 0000000..33b72e5
--- /dev/null
+++ b/src/cal/get_tle/get_tle.pl.OIG
@@ -0,0 +1,148 @@
+#!/usr/local/bin/perl
+use FileHandle;
+use IPC::Open2;
+
+###
+# OIG TLE retrieval program
+# DJG - 6/14/98
+#
+# Uses a file called "one" which has sat numbers to get
+#
+# Places all output in a single file called "five.tle".
+#
+###
+
+### Configure:
+##$login = "emurphy";
+##$passwd = "bdr529";
+
+$login = "mromelfanger";
+$passwd = "fusejhu";
+$output_filename = "/data1/fuse/calfuse/caltemp/five.tle";
+$log_filename = "/data1/fuse/calfuse/caltemp/get_tle.logfile";
+
+### (end of configure section)
+
+# system("fixlist one tempone");
+# chop($satstoget = `cat tempone`);
+# system("rm -f tempone");
+
+$satstoget = "25791";
+
+# The "output" file collects debugging copies of everything that comes back.
+open(OUT,">$log_filename") || die "Could not open output file";
+
+# The following logs in to OIG and gets the first "continue" code
+
+$host = "oig1.gsfc.nasa.gov";
+#$url = "scripts/foxweb.dll/loginok\@app01?tdac=&ffv01=$login&ffv02=$passwd";
+$url = "scripts/foxweb.exe/loginok\@app01?tdac=&ffv01=$login&ffv02=$passwd";
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+while (<Reader>) {
+  print OUT "$_";  # copy each login screen line to the output file
+  if (/tdac=(\w+)\"/) {
+    $continuecode = $1;  # This code is the "continue" code
+  }
+}
+close(Reader);
+close(Writer);
+
+# $continuecode contains the very first "continue" code after login.
+
+print OUT "*** \n Starting User's Home Page output page \n***\n\n";
+
+# This url accesses the next screen (user home page)
+#$url = "scripts/foxweb.dll/favorhome\@app01?tdac=" . $continuecode;
+$url = "scripts/foxweb.exe/favorhome\@app01?tdac=" . $continuecode;
+# print $url; # debug print
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+
+while (<Reader>) {
+  print OUT "$_";      # copy each line to the output file
+
+  if(/tdac=(\w+)\"/) {
+
+#   Look for the "tle ad hoc query" code and save it
+    chop($word = "$_");
+    if ($word =~ /ftleadhoc.+tdac=(\w+)\"/) {
+      $tlequerycode = "$1";
+    }
+  }
+}
+# close(HOMEPAGE);
+# This access is to the "TLE ad hoc query" web page.
+#$url = "scripts/foxweb.dll/ftleadhoc\@app01?tdac=" . $tlequerycode;
+$url = "scripts/foxweb.exe/ftleadhoc\@app01?tdac=" . $tlequerycode;
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+
+while (<Reader>) {
+  print OUT "$_";  # copy each login screen line to the output file
+
+  # Look for the TLE "submit" code
+  chop($word = "$_");
+  if ($word =~ /tdac\" VALUE=\"(\w+)\"/) {
+    $gotcode2 = "$1";
+  }
+}
+close(Reader);
+close(Writer);
+
+# Compose the TLE query and submit it
+#$url = "scripts/foxweb.dll/ftleadhoc\@app01?tdac=" . $gotcode2;
+$url = "scripts/foxweb.exe/ftleadhoc\@app01?tdac=" . $gotcode2;
+$url .= "&ffv01=" . $satstoget . "&ffv02=standard&ffv03=catno&ffv04=five";
+
+# print "$url\n";  # debug print
+
+# Read the reply and copy the relevant lines to output_filename
+
+$copy = "no";
+open(TLEOUT,">$output_filename") || die "Error opening $output_filename";
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+
+while (<Reader>) {
+  if ($_ =~ /<P>/) {  # End copy operation
+    print "$_";       # write remaining limit to output file
+    $copy = "no";
+  }
+  if ($copy eq "yes") {
+    print TLEOUT "$_";   # copy every line to five.tle
+    # print "$_";          # and to the terminal
+  }
+  if (substr($_,0,5) eq "<PRE>") {  # Begin copy operation
+    $copy = "yes";
+  }
+}
+close(Reader);
+close(Writer);
+close(TLEOUT);
+
+# The following will remove all session files. You can comment it
+# out for debugging.
+# system("rm -f output");
+
+# The following script "fixes up" the output
+# system("fix/do.fix.one");
+
+### end of Perl script
+
diff --git a/src/cal/get_tle/get_tle.pl.orig b/src/cal/get_tle/get_tle.pl.orig
new file mode 100755
index 0000000..28f9229
--- /dev/null
+++ b/src/cal/get_tle/get_tle.pl.orig
@@ -0,0 +1,144 @@
+#!/usr/local/bin/perl
+use FileHandle;
+use IPC::Open2;
+
+###
+# OIG TLE retrieval program
+# DJG - 6/14/98
+#
+# Uses a file called "one" which has sat numbers to get
+#
+# Places all output in a single file called "five.tle".
+#
+###
+
+### Configure:
+##$login = "emurphy";
+##$passwd = "bdr529";
+
+$login = "mromelfanger";
+$passwd = "fusejhu";
+$output_filename = "/data1/fuse/calfuse/caltemp/five.tle";
+$log_filename = "/data1/fuse/calfuse/caltemp/get_tle.logfile";
+
+### (end of configure section)
+
+# system("fixlist one tempone");
+# chop($satstoget = `cat tempone`);
+# system("rm -f tempone");
+
+$satstoget = "25791";
+
+# The "output" file collects debugging copies of everything that comes back.
+open(OUT,">$log_filename") || die "Could not open output file";
+
+# The following logs in to OIG and gets the first "continue" code
+
+$host = "oig1.gsfc.nasa.gov";
+$url = "scripts/foxweb.dll/loginok\@app01?tdac=&ffv01=$login&ffv02=$passwd";
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+while (<Reader>) {
+  print OUT "$_";  # copy each login screen line to the output file
+  if (/tdac=(\w+)\"/) {
+    $continuecode = $1;  # This code is the "continue" code
+  }
+}
+close(Reader);
+close(Writer);
+
+# $continuecode contains the very first "continue" code after login.
+
+print OUT "*** \n Starting User's Home Page output page \n***\n\n";
+
+# This url accesses the next screen (user home page)
+$url = "scripts/foxweb.dll/favorhome\@app01?tdac=" . $continuecode;
+# print $url; # debug print
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+
+while (<Reader>) {
+  print OUT "$_";      # copy each line to the output file
+
+  if(/tdac=(\w+)\"/) {
+
+#   Look for the "tle ad hoc query" code and save it
+    chop($word = "$_");
+    if ($word =~ /ftleadhoc.+tdac=(\w+)\"/) {
+      $tlequerycode = "$1";
+    }
+  }
+}
+# close(HOMEPAGE);
+# This access is to the "TLE ad hoc query" web page.
+$url = "scripts/foxweb.dll/ftleadhoc\@app01?tdac=" . $tlequerycode;
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+
+while (<Reader>) {
+  print OUT "$_";  # copy each login screen line to the output file
+
+  # Look for the TLE "submit" code
+  chop($word = "$_");
+  if ($word =~ /tdac\" VALUE=\"(\w+)\"/) {
+    $gotcode2 = "$1";
+  }
+}
+close(Reader);
+close(Writer);
+
+# Compose the TLE query and submit it
+$url = "scripts/foxweb.dll/ftleadhoc\@app01?tdac=" . $gotcode2;
+$url .= "&ffv01=" . $satstoget . "&ffv02=standard&ffv03=catno&ffv04=five";
+
+# print "$url\n";  # debug print
+
+# Read the reply and copy the relevant lines to output_filename
+
+$copy = "no";
+open(TLEOUT,">$output_filename") || die "Error opening $output_filename";
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+
+while (<Reader>) {
+  if ($_ =~ /<P>/) {  # End copy operation
+    print "$_";       # write remaining limit to output file
+    $copy = "no";
+  }
+  if ($copy eq "yes") {
+    print TLEOUT "$_";   # copy every line to five.tle
+    # print "$_";          # and to the terminal
+  }
+  if (substr($_,0,5) eq "<PRE>") {  # Begin copy operation
+    $copy = "yes";
+  }
+}
+close(Reader);
+close(Writer);
+close(TLEOUT);
+
+# The following will remove all session files. You can comment it
+# out for debugging.
+# system("rm -f output");
+
+# The following script "fixes up" the output
+# system("fix/do.fix.one");
+
+### end of Perl script
+
diff --git a/src/cal/get_tle/get_tle.pl.space-track b/src/cal/get_tle/get_tle.pl.space-track
new file mode 100755
index 0000000..60e59d5
--- /dev/null
+++ b/src/cal/get_tle/get_tle.pl.space-track
@@ -0,0 +1,148 @@
+#!/usr/local/bin/perl
+use FileHandle;
+use IPC::Open2;
+
+###
+# OIG TLE retrieval program
+# DJG - 6/14/98
+#
+# Uses a file called "one" which has sat numbers to get
+#
+# Places all output in a single file called "five.tle".
+#
+###
+
+### Configure:
+##$login = "emurphy";
+##$passwd = "bdr529";
+
+$login = "mromelfanger";
+$passwd = "FuseJHU1";
+$output_filename = "/data1/fuse/calfuse/caltemp/five.tle";
+$log_filename = "/data1/fuse/calfuse/caltemp/get_tle.logfile";
+
+### (end of configure section)
+
+# system("fixlist one tempone");
+# chop($satstoget = `cat tempone`);
+# system("rm -f tempone");
+
+$satstoget = "25791";
+
+# The "output" file collects debugging copies of everything that comes back.
+open(OUT,">$log_filename") || die "Could not open output file";
+
+# The following logs in to OIG and gets the first "continue" code
+
+$host = "www.space-track.org";
+#$url = "scripts/foxweb.dll/loginok\@app01?tdac=&ffv01=$login&ffv02=$passwd";
+$url = "scripts/foxweb.exe/loginok\@app01?tdac=&ffv01=$login&ffv02=$passwd";
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+while (<Reader>) {
+  print OUT "$_";  # copy each login screen line to the output file
+  if (/tdac=(\w+)\"/) {
+    $continuecode = $1;  # This code is the "continue" code
+  }
+}
+close(Reader);
+close(Writer);
+
+# $continuecode contains the very first "continue" code after login.
+
+print OUT "*** \n Starting User's Home Page output page \n***\n\n";
+
+# This url accesses the next screen (user home page)
+#$url = "scripts/foxweb.dll/favorhome\@app01?tdac=" . $continuecode;
+$url = "scripts/foxweb.exe/favorhome\@app01?tdac=" . $continuecode;
+# print $url; # debug print
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+
+while (<Reader>) {
+  print OUT "$_";      # copy each line to the output file
+
+  if(/tdac=(\w+)\"/) {
+
+#   Look for the "tle ad hoc query" code and save it
+    chop($word = "$_");
+    if ($word =~ /ftleadhoc.+tdac=(\w+)\"/) {
+      $tlequerycode = "$1";
+    }
+  }
+}
+# close(HOMEPAGE);
+# This access is to the "TLE ad hoc query" web page.
+#$url = "scripts/foxweb.dll/ftleadhoc\@app01?tdac=" . $tlequerycode;
+$url = "scripts/foxweb.exe/ftleadhoc\@app01?tdac=" . $tlequerycode;
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+
+while (<Reader>) {
+  print OUT "$_";  # copy each login screen line to the output file
+
+  # Look for the TLE "submit" code
+  chop($word = "$_");
+  if ($word =~ /tdac\" VALUE=\"(\w+)\"/) {
+    $gotcode2 = "$1";
+  }
+}
+close(Reader);
+close(Writer);
+
+# Compose the TLE query and submit it
+#$url = "scripts/foxweb.dll/ftleadhoc\@app01?tdac=" . $gotcode2;
+$url = "scripts/foxweb.exe/ftleadhoc\@app01?tdac=" . $gotcode2;
+$url .= "&ffv01=" . $satstoget . "&ffv02=standard&ffv03=catno&ffv04=five";
+
+# print "$url\n";  # debug print
+
+# Read the reply and copy the relevant lines to output_filename
+
+$copy = "no";
+open(TLEOUT,">$output_filename") || die "Error opening $output_filename";
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+
+while (<Reader>) {
+  if ($_ =~ /<P>/) {  # End copy operation
+    print "$_";       # write remaining limit to output file
+    $copy = "no";
+  }
+  if ($copy eq "yes") {
+    print TLEOUT "$_";   # copy every line to five.tle
+    # print "$_";          # and to the terminal
+  }
+  if (substr($_,0,5) eq "<PRE>") {  # Begin copy operation
+    $copy = "yes";
+  }
+}
+close(Reader);
+close(Writer);
+close(TLEOUT);
+
+# The following will remove all session files. You can comment it
+# out for debugging.
+# system("rm -f output");
+
+# The following script "fixes up" the output
+# system("fix/do.fix.one");
+
+### end of Perl script
+
diff --git a/src/cal/get_tle/make_cvzramtool.pl b/src/cal/get_tle/make_cvzramtool.pl
new file mode 100755
index 0000000..4cb2e01
--- /dev/null
+++ b/src/cal/get_tle/make_cvzramtool.pl
@@ -0,0 +1,215 @@
+#!/usr/local/bin/perl
+use FileHandle;
+
+# This program will read in the latest FUSE TLE and recreate the 
+# cvz_ram_tool.html web page.
+
+$output_filename = "/data2/violet/htdocs/support/tools/cvz_ram_tool.html";
+open (OUTF, ">$output_filename") || die "Cannot open cvz_ram_tool.html file";
+
+system("chmod ug+rw $output_filename");
+system("chgrp www $output_filename");
+
+$input_filename = "/data1/fuse/calfuse/calfiles/FUSE.TLE";
+open (INP_TLE, "<$input_filename") || die "Cannot open FUSE.TLE file";
+
+$line1 = <INP_TLE>;
+$line2 = <INP_TLE>;
+$line3 = <INP_TLE>;
+
+$id2 = substr($line2, 2, 5);
+$id3 = substr($line3, 2, 5);
+
+if (($id2 != 25791) || ($id3 != 25791)) {
+    print STDOUT "Error in TLE:\n";
+    print STDOUT $line1;
+    print STDOUT $line2;
+    print STDOUT $line3;
+    die "Error in TLE";
+}
+
+close (INP_TLE);
+
+$year = substr($line2, 18, 2);
+$doy = substr($line2, 20, 3);
+$dayfrac = substr($line2, 23, 9);
+$incl = substr($line3, 9, 8);
+$raan = substr($line3, 17,8);
+$eccen = substr($line3, 26, 7);
+$eccen = "0." . $eccen;
+$mean_mot = substr($line3, 52, 11);
+
+if ($year > 50) {
+    $year += 1900;
+} else {
+    $year += 2000;
+}
+
+$dayfrac = "0".$dayfrac;
+
+&convert_doy;
+&convert_dayfrac;
+&calculate_a0;
+
+$now=`date`;
+$datest = substr($now,4,3)." ".substr($now,8,2).", ".substr($now,24,4);
+
+print OUTF "<TITLE>FUSE CVZ/Ram Calculator</TITLE>\n";
+print OUTF "<h1>FUSE Continuous Viewing Zone and Orbit Ram Calculator V1.3</h1>\n";
+print OUTF "<h2>June 12, 1999 </h2>\n";
+
+print OUTF "The FUSE Continuous Viewing Zone and Orbit Ram \n";
+print OUTF "Calculator can determine when a given target \n";
+print OUTF "direction is in the continuous viewing zone. \n";
+print OUTF "It also calculates when a given target lies \n";
+print OUTF "within 20 degrees of the orbital plane and \n";
+print OUTF "cannot be observed due to ram avoidance\n";
+print OUTF "constraints. The default orbital elements \n";
+print OUTF "were last updated on $month $day, $year. \n";
+
+print OUTF "<HR>\n";
+print OUTF "<P>\n";
+print OUTF "<FORM METHOD=POST ACTION=\"http://fuse.pha.jhu.edu/cgi-bin/cvz_ram_tool\">\n";
+
+print OUTF "<INPUT TYPE=\"submit\" VALUE=\"Calculate CVZ visibilities\">\n";
+print OUTF "<INPUT TYPE=\"reset\" VALUE=\"Erase the input fields\">\n";
+print OUTF "<BR>\n";
+  
+print OUTF "<BR>\n";
+print OUTF "<B>Target Parameters:</B>\n";
+print OUTF "<BLOCKQUOTE>\n";
+print OUTF "<BR>\n";
+print OUTF "<B>Right Ascension (format HH:MM:SS.SS):</B>\n";
+print OUTF "<INPUT NAME=\"right_ascension\" SIZE=15> <B>(J2000.0)</B>\n";
+print OUTF "<BR>\n";
+print OUTF "<B>Declination (format -DD:MM:SS.S):</B>\n";
+print OUTF "<INPUT NAME=\"declination\" SIZE=15> <B>(J2000.0)</B>\n";
+print OUTF "<BR>\n";
+print OUTF "</BLOCKQUOTE>\n";
+print OUTF "<BR>\n";
+print OUTF "<B>Output table parameters:</B>\n";
+print OUTF "<BLOCKQUOTE>\n";
+print OUTF "<B> Minimum Earth limb angle: </B><INPUT NAME=\"limb_ang\" SIZE=4 VALUE=\"15.0\"> \n";
+print OUTF "<B>(deg)</B>\n";
+print OUTF "<BR>\n";
+print OUTF "<B>Start Date:</B>\n";
+print OUTF "<SELECT NAME=\"month\">\n";
+print OUTF "<OPTION> <B>$month</B>\n";
+print OUTF "<OPTION> January\n";
+print OUTF "<OPTION> February\n";
+print OUTF "<OPTION> March\n";
+print OUTF "<OPTION> April\n";
+print OUTF "<OPTION> May\n";
+print OUTF "<OPTION> June\n";
+print OUTF "<OPTION> July\n";
+print OUTF "<OPTION> August\n";
+print OUTF "<OPTION> September\n";
+print OUTF "<OPTION> October\n";
+print OUTF "<OPTION> November\n";
+print OUTF "<OPTION> December\n";
+print OUTF "</SELECT>\n";
+print OUTF "<INPUT NAME=\"day\" SIZE=4 VALUE=\"1\">\n";
+print OUTF "<INPUT NAME=\"year\" SIZE=8 VALUE=\"$year\">\n";
+print OUTF "<BR>\n";
+print OUTF "<B>Time step:<INPUT NAME=\"time_step\" SIZE=6 VALUE=\"1.0\">days</B><BR>\n";
+print OUTF "<B>Number of steps:<INPUT NAME=\"number_steps\" SIZE=6 VALUE=\"10\"></B><BR>\n";
+print OUTF "</BLOCKQUOTE>\n";
+print OUTF "<BR>\n";
+print OUTF "<B>FUSE classical Keplarian orbital elements:</B>\n";
+print OUTF "<BLOCKQUOTE>\n";
+print OUTF "<B>Epoch date of elements:</B>\n";
+print OUTF "<SELECT NAME=\"orb_month\">\n";
+print OUTF "<OPTION> $month\n";
+print OUTF "<OPTION> January\n";
+print OUTF "<OPTION> February\n";
+print OUTF "<OPTION> March\n";
+print OUTF "<OPTION> April\n";
+print OUTF "<OPTION> May\n";
+print OUTF "<OPTION> June\n";
+print OUTF "<OPTION> July\n";
+print OUTF "<OPTION> August\n";
+print OUTF "<OPTION> September\n";
+print OUTF "<OPTION> October\n";
+print OUTF "<OPTION> November\n";
+print OUTF "<OPTION> December\n";
+print OUTF "</SELECT>\n";
+print OUTF "<INPUT NAME=\"orb_day\" SIZE=4 VALUE=\"$day\">\n";
+print OUTF "<INPUT NAME=\"orb_year\" SIZE=8 VALUE=\"$year\">\n";
+print OUTF "<BR>\n";
+print OUTF "<B>Epoch UT time of elements (format HH:MM:SS.SS):</B>\n";
+printf OUTF "<INPUT NAME=\"orb_time\" SIZE=12 VALUE=\"%02d:%02d:%05.2f\">\n",$hour,$minute,$second;
+print OUTF "<BR>\n";
+print OUTF "<B>Semi-major axis (km):</B>\n";
+printf OUTF "<INPUT NAME=\"orb_a\" SIZE=15 value=\"%7.3f\"> \n",$semiax;
+print OUTF "<BR>\n";
+print OUTF "<B>Right ascension of the ascending node (degrees):</B>\n";
+print OUTF "<INPUT NAME=\"orb_raan\" SIZE=15 value=\"$raan\">\n";
+print OUTF "<BR>\n";
+print OUTF "<B>Orbit inclination (degrees):</B>\n";
+print OUTF "<INPUT NAME=\"orb_i\" SIZE=15 value=\"$incl\">\n";
+print OUTF "<BR>\n";
+print OUTF "<B>Eccentricity:</B>\n";
+print OUTF "<INPUT NAME=\"orb_e\" SIZE=15 value=\"$eccen\"> \n";
+print OUTF "</BLOCKQUOTE>\n";
+print OUTF "<BR>\n";
+print OUTF "<INPUT TYPE=\"submit\" VALUE=\"Calculate CVZ visibilities\">\n";
+print OUTF "<INPUT TYPE=\"reset\" VALUE=\"Erase the input fields\">\n";
+print OUTF "</FORM>\n";
+
+print OUTF "<HR>\n";
+print OUTF "This page uses the <a href=\"http://star-www.rl.ac.uk/\"> STARLINK </a>\n";
+print OUTF "set of astronomical subroutines.\n";
+print OUTF "<BR>\n";
+print OUTF "This page was automatically generated on $now";
+print OUTF "<BR>\n";
+print OUTF "<a href=\"mailto:emurphy\@pha.jhu.edu\"><address>emurphy\@pha.jhu.edu</address></a>\n";
+
+close (OUTF);
+
+### end of Perl script
+
+
+sub convert_doy {
+    @daytab1 = (0, 31, 29, 31, 30, 31, 30, 31, 31, 30, 31, 30, 31);
+    @daytab2 = (0, 31, 28, 31, 30, 31, 30, 31, 31, 30, 31, 30, 31);
+    @monthstr = ("", "January", "February", "March", "April", "May", "June", "July", "August", "September", "October", "November", "December");
+
+    if ((($year%4 == 0) && ($year%100 != 0)) || ($year%400 == 0)) {
+        # $year is a leap year use daytab1
+        for ($i = 1; $doy > $daytab1[$i]; $i++) {
+	    $doy -= $daytab1[$i];
+	}
+    } else {
+        # $year is not a leap year, use daytab2
+        for ($i = 1; $doy > $daytab2[$i]; $i++) {
+	    $doy -= $daytab2[$i];
+	}
+    }
+    $month = $monthstr[$i];
+    $day = $doy;
+}
+
+sub convert_dayfrac {
+    $dayfrac *= 24.0;
+    $hour = int($dayfrac);
+    $minute = int(($dayfrac-$hour)*60.0);
+    $second = ((($dayfrac-$hour)*60.0)-$minute)*60.0;
+}
+
+sub calculate_a0 {
+
+$mu = 3.986005E5;
+$pi = 3.14159265358979;
+$radian = 0.0174532925200;
+
+$mm=2.0*$pi*$mean_mot/(24.0*60.0);
+$ke=0.74366916E-1;
+$k2=5.413080E-4;
+$a1=($ke/$mm)**(2.0/3.0);
+$inrad = $incl * $radian;
+
+$d1=3.0/2.0*$k2/($a1*$a1)*(3.0*cos($inrad)*cos($inrad)-1.0)/((1.0-$eccen*$eccen)**(3.0/2.0));
+$a0=$a1*(1.0-$d1/3.0-$d1*$d1-134.0/81.0*$d1*$d1*$d1);
+$d0=3.0/2.0*$k2/($a0*$a0)*(3.0*cos($inrad)*cos($inrad)-1.0)/((1.0-$eccen*$eccen)**(3.0/2.0));
+$semiax=$a0/(1-$d0)*6378.135;
+}
diff --git a/src/cal/get_tle/make_orbit.pl b/src/cal/get_tle/make_orbit.pl
new file mode 100755
index 0000000..a8f00ff
--- /dev/null
+++ b/src/cal/get_tle/make_orbit.pl
@@ -0,0 +1,233 @@
+#!/usr/local/bin/perl
+use FileHandle;
+
+# Ed Murphy's program to rewrite the orbit page
+# Updated 03/27/00  Changed GSOC to Heavens Above
+
+$output_filename = "/data2/violet/htdocs/users/orbit.html";
+open (OUTF, ">$output_filename") || die "Cannot open $output_filename file";
+
+system("chmod ug+rw $output_filename");
+system("chgrp www $output_filename");
+
+$input_filename = "/data1/fuse/calfuse/calfiles/FUSE.TLE";
+open (INP_TLE, "<$input_filename") || die "Cannot open $input_filename file";
+
+$satid = 25791;
+
+&input_lines;
+
+close (INP_TLE);
+
+&parse_lines;
+
+&convert_doy;
+&convert_dayfrac;
+&calculate_a0;
+&calculate_orbs;
+
+$now=`date`;
+$datest = substr($now,4,3)." ".substr($now,8,2).", ".substr($now,24,4);
+
+print OUTF "<HTML>\n";
+print OUTF "<HEAD>\n";
+print OUTF "<title>FUSE Orbital Elements page</title>\n";
+print OUTF "</HEAD>\n";
+print OUTF "<BODY bgcolor=#ffffff ALINK=\"#000000\" VLINK=\"darkblue\">\n";
+print OUTF "<center>\n";
+print OUTF "<table width=640>\n";
+print OUTF "<tr><td>\n";
+print OUTF "<img src=\"/figures/purple_line2.gif\" width=640>\n";
+print OUTF "<table cellpadding=5 cellspacing=5 width=550>\n";
+print OUTF "<tr>\n";
+print OUTF "<td valign=top align=left>\n";
+print OUTF "<img src=\"/figures/andromeda_moo_small.gif\">\n";
+print OUTF "</td>\n";
+print OUTF "<td valign=top align=left>\n";
+print OUTF "<font size=+3><font color=\"#6666CC\">\n";
+print OUTF "<b>FUSE<P>\n";
+print OUTF "<i>Orbital Elements</font></font></i></b>\n";
+print OUTF "</td>\n";
+print OUTF "</tr>\n";
+print OUTF "</table>\n";
+print OUTF "<img src=\"/figures/purple_line2.gif\" width=640>\n";
+print OUTF "<p>\n";
+print OUTF "<center>\n";
+print OUTF "<font color=\"#CC0099\" size=4><b>\n";
+print OUTF "Where is FUSE now?<br></b></font>\n";
+print OUTF "<font size=4>Check out the\n";
+print OUTF "<a href=\"http://www.heavens-above.com/orbitdisplay.asp?lat=39.3&lng=-76.6&loc=BALTIMORE&TZ=EST&satid=25791\" >\n";
+print OUTF "Heavens-Above Satellite Predictions page </a></font>.\n";
+print OUTF "</center>\n";
+print OUTF "<P>\n";
+print OUTF "<hr>\n";
+print OUTF "<p><pre>\n";
+print OUTF " \n";
+print OUTF  "FUSE orbital elements:\n";
+print OUTF  "     NORAD number       25791\n";
+print OUTF  "     International ID  99035A\n";
+print OUTF  " \n";
+
+&print_orb;
+
+print OUTF "</pre>\n";
+
+&print_tail;
+
+close (OUTF);
+
+### end of Perl script
+
+
+sub convert_doy {
+    @daytab1 = (0, 31, 29, 31, 30, 31, 30, 31, 31, 30, 31, 30, 31);
+    @daytab2 = (0, 31, 28, 31, 30, 31, 30, 31, 31, 30, 31, 30, 31);
+    @monthstr = ("", "January", "February", "March", "April", "May", "June", "July", "August", "September", "October", "November", "December");
+
+    if ((($year%4 == 0) && ($year%100 != 0)) || ($year%400 == 0)) {
+        # $year is a leap year use daytab1
+        for ($i = 1; $doy > $daytab1[$i]; $i++) {
+	    $doy -= $daytab1[$i];
+	}
+    } else {
+        # $year is not a leap year, use daytab2
+        for ($i = 1; $doy > $daytab2[$i]; $i++) {
+	    $doy -= $daytab2[$i];
+	}
+    }
+    $month = $monthstr[$i];
+    $day = $doy;
+}
+
+sub convert_dayfrac {
+    $dayfrac *= 24.0;
+    $hour = int($dayfrac);
+    $minute = int(($dayfrac-$hour)*60.0);
+    $second = ((($dayfrac-$hour)*60.0)-$minute)*60.0;
+}
+
+sub input_lines {
+$line1 = <INP_TLE>;
+$line2 = <INP_TLE>;
+$line3 = <INP_TLE>;
+
+$id2 = substr($line2, 2, 5);
+$id3 = substr($line3, 2, 5);
+
+if (($id2 != $satid) || ($id3 != $satid)) {
+    print STDOUT "Error in TLE:\n";
+    print STDOUT $line1;
+    print STDOUT $line2;
+    print STDOUT $line3;
+#    die "Error in TLE";
+}
+
+}
+
+sub parse_lines {
+$year = substr($line2, 18, 2);
+$doy = substr($line2, 20, 3);
+$dayfrac = substr($line2, 23, 9);
+$epoch = $year.$doy.$dayfrac;
+$incl = substr($line3, 9, 8);
+$raan = substr($line3, 17,8);
+$eccen = substr($line3, 26, 7);
+$eccen = "0." . $eccen;
+$mean_mot = substr($line3, 52, 11);
+$mean_anom = substr($line3, 43, 8);
+$arg_perig = substr($line3, 34, 8);
+
+
+if ($year > 50) {
+    $year += 1900;
+} else {
+    $year += 2000;
+}
+
+$dayfrac = "0".$dayfrac;
+
+}
+
+sub calculate_a0 {
+
+$mu = 3.986005E5;
+$pi = 3.14159265358979;
+$radian = 0.0174532925200;
+
+$mm=2.0*$pi*$mean_mot/(24.0*60.0);
+$ke=0.74366916E-1;
+$k2=5.413080E-4;
+$a1=($ke/$mm)**(2.0/3.0);
+$inrad = $incl * $radian;
+
+$d1=3.0/2.0*$k2/($a1*$a1)*(3.0*cos($inrad)*cos($inrad)-1.0)/((1.0-$eccen*$eccen)**(3.0/2.0));
+$a0=$a1*(1.0-$d1/3.0-$d1*$d1-134.0/81.0*$d1*$d1*$d1);
+$d0=3.0/2.0*$k2/($a0*$a0)*(3.0*cos($inrad)*cos($inrad)-1.0)/((1.0-$eccen*$eccen)**(3.0/2.0));
+$semiax=$a0/(1-$d0)*6378.135;
+
+}
+
+sub calculate_orbs {
+
+$period = 60.0*24.0/($mean_mot/(1+$d0));
+$cax=$eccen*$semiax;
+$perigee=$semiax-$cax-6378.1;
+$apogee=$semiax+$cax-6378.1;
+
+}
+
+sub print_orb {
+print OUTF  "     Epoch           $epoch\n";
+printf OUTF "     Semimajor axis   %7.2f km\n",$semiax;
+printf OUTF "     Apogee            %5.2f km\n",$apogee;
+printf OUTF "     Perigee           %5.2f km\n",$perigee;
+print OUTF  "     Eccentricity   $eccen\n";
+printf OUTF  "     Inclination       %6.2f degrees\n",$incl;
+printf OUTF "     Period            %6.2f minutes\n",$period;
+printf OUTF "     RA of asc. node   %6.2f degrees\n",$raan;
+printf OUTF "     Arg. of perigee   %6.2f degrees\n",$arg_perig;
+printf OUTF "     Mean anomaly      %6.2f degrees\n",$mean_anom;
+print OUTF  " \n";
+
+}
+
+sub print_tail {
+print OUTF "<p>";
+
+print OUTF "The FUSE Delta II second stage (NORAD #25792) reentered on \n";
+print OUTF "the morning of August 4, 1999 during orbit number 708.  \n";
+print OUTF "According to predictions by Alan Pickup, reentry \n";
+print OUTF "occured within 90 minutes of 5:31 UT, probably over the \n";
+print OUTF "Arabian Sea or India.  The final orbit was 119 x 103 km (74 x 64 mi).\n";
+print OUTF "<p>";
+print OUTF "<center>";
+print OUTF "<font size=+2><font color=\"#6666CC\">\n";
+print OUTF "<a href=\"reentry.html\"> Could anything have survived reentry?</a></font></font><p>\n";
+print OUTF "</center>";
+print OUTF "<img align=center src=\"delta2decay.gif\">\n";
+print OUTF "<P>These numbers assume a Keplerian orbit; the actual apogee and perigee \n";
+print OUTF "will differ by a few km on an orbit-to-orbit basis.\n";
+print OUTF "<p>";
+print OUTF "<p>The NORAD Two-Line Elements (TLEs) for FUSE can be found in the file \n";
+print OUTF "<a href=\"./FUSE.TLE\" > FUSE.TLE </A>.\n";
+print OUTF "<p> \n";
+print OUTF "This page is automatically updated daily.  I wish to thank \n";
+print OUTF "<a href=\"mailto:deej\@deej.com\">Doyle Groves</a> \n";
+print OUTF "for providing a Perl script to access the NASA\n";
+print OUTF "Orbital Information Group web page.\n";
+print OUTF "<p> Ed Murphy, <a href=\"mailto:emurphy\@pha.jhu.edu\">\n";
+print OUTF "<address>emurphy\@pha.jhu.edu</address></a>\n";
+print OUTF "<P>\n";
+print OUTF "<img src=\"/figures/purple_line2.gif\" width=640>\n";
+print OUTF "<P>\n";
+print OUTF "Last changed: $datest.\n";
+print OUTF "<P>\n";
+print OUTF "<i><a href=\"/index.shtml\">Return to the FUSE home page.</a></i><br clear=left>\n";
+print OUTF "<p>\n";
+print OUTF "</td></tr>\n";
+print OUTF "</table>\n";
+print OUTF "</center>\n";
+print OUTF "</BODY>\n";
+print OUTF "</HTML>\n";
+
+}
diff --git a/src/cal/get_tle/test_get_tle.pl b/src/cal/get_tle/test_get_tle.pl
new file mode 100755
index 0000000..33b72e5
--- /dev/null
+++ b/src/cal/get_tle/test_get_tle.pl
@@ -0,0 +1,148 @@
+#!/usr/local/bin/perl
+use FileHandle;
+use IPC::Open2;
+
+###
+# OIG TLE retrieval program
+# DJG - 6/14/98
+#
+# Uses a file called "one" which has sat numbers to get
+#
+# Places all output in a single file called "five.tle".
+#
+###
+
+### Configure:
+##$login = "emurphy";
+##$passwd = "bdr529";
+
+$login = "mromelfanger";
+$passwd = "fusejhu";
+$output_filename = "/data1/fuse/calfuse/caltemp/five.tle";
+$log_filename = "/data1/fuse/calfuse/caltemp/get_tle.logfile";
+
+### (end of configure section)
+
+# system("fixlist one tempone");
+# chop($satstoget = `cat tempone`);
+# system("rm -f tempone");
+
+$satstoget = "25791";
+
+# The "output" file collects debugging copies of everything that comes back.
+open(OUT,">$log_filename") || die "Could not open output file";
+
+# The following logs in to OIG and gets the first "continue" code
+
+$host = "oig1.gsfc.nasa.gov";
+#$url = "scripts/foxweb.dll/loginok\@app01?tdac=&ffv01=$login&ffv02=$passwd";
+$url = "scripts/foxweb.exe/loginok\@app01?tdac=&ffv01=$login&ffv02=$passwd";
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+while (<Reader>) {
+  print OUT "$_";  # copy each login screen line to the output file
+  if (/tdac=(\w+)\"/) {
+    $continuecode = $1;  # This code is the "continue" code
+  }
+}
+close(Reader);
+close(Writer);
+
+# $continuecode contains the very first "continue" code after login.
+
+print OUT "*** \n Starting User's Home Page output page \n***\n\n";
+
+# This url accesses the next screen (user home page)
+#$url = "scripts/foxweb.dll/favorhome\@app01?tdac=" . $continuecode;
+$url = "scripts/foxweb.exe/favorhome\@app01?tdac=" . $continuecode;
+# print $url; # debug print
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+
+while (<Reader>) {
+  print OUT "$_";      # copy each line to the output file
+
+  if(/tdac=(\w+)\"/) {
+
+#   Look for the "tle ad hoc query" code and save it
+    chop($word = "$_");
+    if ($word =~ /ftleadhoc.+tdac=(\w+)\"/) {
+      $tlequerycode = "$1";
+    }
+  }
+}
+# close(HOMEPAGE);
+# This access is to the "TLE ad hoc query" web page.
+#$url = "scripts/foxweb.dll/ftleadhoc\@app01?tdac=" . $tlequerycode;
+$url = "scripts/foxweb.exe/ftleadhoc\@app01?tdac=" . $tlequerycode;
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+
+while (<Reader>) {
+  print OUT "$_";  # copy each login screen line to the output file
+
+  # Look for the TLE "submit" code
+  chop($word = "$_");
+  if ($word =~ /tdac\" VALUE=\"(\w+)\"/) {
+    $gotcode2 = "$1";
+  }
+}
+close(Reader);
+close(Writer);
+
+# Compose the TLE query and submit it
+#$url = "scripts/foxweb.dll/ftleadhoc\@app01?tdac=" . $gotcode2;
+$url = "scripts/foxweb.exe/ftleadhoc\@app01?tdac=" . $gotcode2;
+$url .= "&ffv01=" . $satstoget . "&ffv02=standard&ffv03=catno&ffv04=five";
+
+# print "$url\n";  # debug print
+
+# Read the reply and copy the relevant lines to output_filename
+
+$copy = "no";
+open(TLEOUT,">$output_filename") || die "Error opening $output_filename";
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+
+while (<Reader>) {
+  if ($_ =~ /<P>/) {  # End copy operation
+    print "$_";       # write remaining limit to output file
+    $copy = "no";
+  }
+  if ($copy eq "yes") {
+    print TLEOUT "$_";   # copy every line to five.tle
+    # print "$_";          # and to the terminal
+  }
+  if (substr($_,0,5) eq "<PRE>") {  # Begin copy operation
+    $copy = "yes";
+  }
+}
+close(Reader);
+close(Writer);
+close(TLEOUT);
+
+# The following will remove all session files. You can comment it
+# out for debugging.
+# system("rm -f output");
+
+# The following script "fixes up" the output
+# system("fix/do.fix.one");
+
+### end of Perl script
+
diff --git a/src/cal/get_tle/test_tle.csh b/src/cal/get_tle/test_tle.csh
new file mode 100755
index 0000000..5431552
--- /dev/null
+++ b/src/cal/get_tle/test_tle.csh
@@ -0,0 +1,50 @@
+#!/bin/csh -f
+#******************************************************************************
+#*              Johns Hopkins University
+#*              Center For Astrophysical Sciences
+#*              FUSE
+#*****************************************************************************
+#*
+#* Synopsis:    update_tle
+#*
+#* Description: Shell script for automatically downloading the latest
+#*              orbital elements from the GSFC OIG, and placing these
+#*              elements in the FUSE.TLE file.  It will also update 
+#*              the cvz_ram_tool.html calculator.
+#*		
+#*		All messages are to stdout or stderr.
+#*
+#* Arguments:   None
+#*
+#* Returns:     Exit codes:
+#*			0		successful execution
+#* 
+#* History:     07/27/99        emm     Begin work.
+#******************************************************************************/
+
+set tlestat=0
+
+# Step 1
+/usr/local/fusesw/calfuse/current/src/cal/get_tle/get_tle.pl
+set cfstat=$status
+
+# Step 2
+if !({$cfstat}) then
+    /usr/local/fusesw/calfuse/current/src/cal/get_tle/add_tle.pl
+    set cfstat=$status
+endif
+
+# Step 3
+if !({$cfstat}) then
+    /usr/local/fusesw/calfuse/current/src/cal/get_tle/make_cvzramtool.pl
+    set cfstat=$status
+endif
+
+# Step 4
+if !({$cfstat}) then
+    /usr/local/fusesw/calfuse/current/src/cal/get_tle/make_orbit.pl
+    set cfstat=$status
+endif
+
+exit($cfstat)
+
diff --git a/src/cal/get_tle/tmp/FUSE.OLD b/src/cal/get_tle/tmp/FUSE.OLD
new file mode 100644
index 0000000..75e788e
--- /dev/null
+++ b/src/cal/get_tle/tmp/FUSE.OLD
@@ -0,0 +1,5205 @@
+FUSE 1
+1 25791U 99035A   03334.81529517  .00000629  00000-0  13611-3 0    73
+2 25791  24.9828 141.7372 0010396 237.2837 122.6662 14.41449325233814
+FUSE 1
+1 25791U 99035A   03332.32285756  .00000721  00000-0  16400-3 0    51
+2 25791  24.9827 157.0092 0010498 210.6638 149.3252 14.41447882233456
+FUSE 1
+1 25791U 99035A   03331.90745146 +.00000729 +00000-0 +16628-3 0 00081
+2 25791 024.9828 159.5554 0010553 206.5242 153.4727 14.41447542233393
+FUSE 1
+1 25791U 99035A   03331.14587356  .00000725  00000-0  16505-3 0    40
+2 25791  24.9828 164.2238 0010646 198.4715 161.5398 14.41446726233287
+FUSE 1
+1 25791U 99035A   03329.89965515  .00000696  00000-0  15651-3 0    33
+2 25791  24.9826 171.8592 0010670 185.6347 174.4062 14.41445181233104
+FUSE 1
+1 25791U 99035A   03328.86113523 +.00000610 +00000-0 +13023-3 0 00030
+2 25791 024.9825 178.2061 0010624 174.6707 185.3915 14.41444336232953
+FUSE 1
+1 25791U 99035A   03328.79190076  .00000678  00000-0  15092-3 0    21
+2 25791  24.9829 178.6308 0010612 173.9957 186.0679 14.41444516232945
+FUSE 1
+1 25791U 99035A   03327.89185200 +.00000523 +00000-0 +10396-3 0 00058
+2 25791 024.9836 184.1428 0010625 164.7116 195.3708 14.41443393232811
+FUSE 1
+1 25791U 99035A   03327.06103806  .00000946  00000-0  23212-3 0    15
+2 25791  24.9839 189.2348 0010607 156.0117 204.0892 14.41443370232699
+FUSE 1
+1 25791U 99035A   03326.92256930 +.00001217 +00000-0 +31425-3 0 00068
+2 25791 024.9831 190.0850 0010666 154.7022 205.4026 14.41443784232675
+FUSE 1
+1 25791U 99035A   03325.81481645  .00001001  00000-0  24877-3 0    06
+2 25791  24.9833 196.8767 0010686 142.8583 217.2666 14.41441143232511
+FUSE 1
+1 25791U 99035A   03324.91476442 +.00000578 +00000-0 +12056-3 0 00021
+2 25791 024.9828 202.3884 0010744 133.5472 226.5911 14.41438825232381
+FUSE 1
+1 25791U 99035A   03323.94547862 +.00000358 +00000-0 +54039-4 0 00011
+2 25791 024.9832 208.3404 0010860 124.8670 235.2866 14.41437713232248
+FUSE 1
+1 25791U 99035A   03322.90695295 +.00000456 +00000-0 +83650-4 0 00009
+2 25791 024.9834 214.7019 0010853 115.1433 245.0191 14.41437815232091
+FUSE 1
+1 25791U 99035A   03321.93766319 +.00000482 +00000-0 +91492-4 0 00223
+2 25791 024.9834 220.6386 0010837 104.6262 255.5450 14.41437349231959
+FUSE 1
+1 25791U 99035A   03320.89913707 +.00000498 +00000-0 +96406-4 0 09969
+2 25791 024.9836 226.9996 0010817 093.6241 266.5508 14.41436631231802
+FUSE 1
+1 25791U 99035A   03319.92984440 +.00000599 +00000-0 +12716-3 0 09988
+2 25791 024.9836 232.9378 0010741 083.7324 276.4412 14.41436361231669
+FUSE 1
+1 25791U 99035A   03318.96055095 +.00000529 +00000-0 +10579-3 0 00064
+2 25791 024.9837 238.8759 0010678 074.0237 286.1451 14.41435571231521
+FUSE 1
+1 25791U 99035A   03317.92202182 +.00000413 +00000-0 +70728-4 0 00021
+2 25791 024.9840 245.2398 0010704 063.5995 296.5616 14.41434631231377
+FUSE 1
+1 25791U 99035A   03316.95272605 +.00000470 +00000-0 +88022-4 0 09972
+2 25791 024.9836 251.1803 0010590 053.6350 306.5138 14.41434475231239
+FUSE 1
+1 25791U 99035A   03315.91419451 +.00000359 +00000-0 +54432-4 0 09951
+2 25791 024.9837 257.5405 0010596 042.7776 317.3563 14.41433347231087
+FUSE 1
+1 25791U 99035A   03314.94489683 +.00000376 +00000-0 +59442-4 0 00177
+2 25791 024.9838 263.4782 0010541 032.5623 327.5544 14.41433068230946
+FUSE 1
+1 25791U 99035A   03313.97559885 +.00000299 +00000-0 +36081-4 0 09921
+2 25791 024.9837 269.4165 0010540 022.3690 337.7277 14.41432334230802
+FUSE 1
+1 25791U 99035A   03312.93706443 +.00000584 +00000-0 +12243-3 0 09931
+2 25791 024.9834 275.7793 0010504 011.6272 348.4499 14.41433055230652
+FUSE 1
+1 25791U 99035A   03311.96776569 +.00000350 +00000-0 +51482-4 0 09939
+2 25791 024.9833 281.7181 0010408 001.6598 358.3945 14.41431695230511
+FUSE 1
+1 25791U 99035A   03310.65228737 +.00000444 +00000-0 +80221-4 0 09930
+2 25791 024.9835 289.7793 0010257 347.5217 012.5005 14.41431193230320
+FUSE 1
+1 25791U 99035A   03309.40604522 +.00000467 +00000-0 +87049-4 0 00145
+2 25791 024.9835 297.4135 0010238 333.3895 026.6085 14.41430141230146
+FUSE 1
+1 25791U 99035A   03308.78292393 +.00000641 +00000-0 +13975-3 0 09895
+2 25791 024.9836 301.2316 0010231 327.1757 032.8108 14.41430126230051
+FUSE 1
+1 25791U 99035A   03307.39821018 +.00000487 +00000-0 +93143-4 0 09853
+2 25791 024.9836 309.7266 0009954 308.3405 051.6212 14.41427785229857
+FUSE 1
+1 25791U 99035A   03306.42890957 +.00001374 +00000-0 +36220-3 0 09920
+2 25791 024.9826 315.6681 0010109 298.0220 061.9265 14.41428485229712
+FUSE 1
+1 25791U 99035A   03305.45960939 +.00002012 +00000-0 +55551-3 0 00086
+2 25791 024.9823 321.6056 0010134 287.9208 072.0205 14.41427385229572
+FUSE 1
+1 25791U 99035A   03304.49030907 +.00002090 +00000-0 +57918-3 0 09839
+2 25791 024.9820 327.5453 0010274 277.3913 082.5438 14.41423770229439
+FUSE 1
+1 25791U 99035A   03303.52100790 +.00001430 +00000-0 +37917-3 0 09979
+2 25791 024.9824 333.4868 0010388 267.0794 092.8530 14.41418570229291
+FUSE 1
+1 25791U 99035A   03303.24406524  .00000959  00000-0  23638-3 0  9826
+2 25791  24.9827 335.1872 0010550 264.3245  95.6061 14.41416153229251
+FUSE 1
+1 25791U 99035A   03302.20552450  .00001096  00000-0  27769-3 0  9812
+2 25791  24.9825 341.5507 0010562 253.8882 106.0488 14.41414636229106
+FUSE 1
+1 25791U 99035A   03300.54385630  .00000645  00000-0  14088-3 0  9809
+2 25791  24.9828 351.7298 0010742 236.4738 123.4745 14.41411128228860
+FUSE 1
+1 25791U 99035A   03299.22836924  .00000522  00000-0  10377-3 0  9797
+2 25791  24.9826 359.7898 0010802 223.1838 136.7831 14.41409442228671
+FUSE 1
+1 25791U 99035A   03297.56670010  .00000441  00000-0  79217-4 0  9782
+2 25791  24.9828   9.9670 0010755 205.8604 154.1368 14.41407956228431
+FUSE 1
+1 25791U 99035A   03295.69732098 +.00000439 +00000-0 +78644-4 0 09778
+2 25791 024.9823 021.4161 0010726 186.3436 173.6933 14.41406877228169
+FUSE 1
+1 25791U 99035A   03294.58954049  .00000442  00000-0  79553-4 0  9760
+2 25791  24.9822  28.2003 0010717 174.4425 185.6202 14.41406259228003
+FUSE 1
+1 25791U 99035A   03293.68946830 +.00000437 +00000-0 +78059-4 0 09808
+2 25791 024.9822 033.7128 0010712 164.9748 195.1079 14.41405735227879
+FUSE 1
+1 25791U 99035A   03293.55099557  .00000435  00000-0  77377-4 0  9753
+2 25791  24.9823  34.5611 0010708 163.5206 196.5648 14.41405674227852
+FUSE 1
+1 25791U 99035A   03292.85863226 +.00000395 +00000-0 +65203-4 0 00006
+2 25791 024.9822 038.8017 0010732 156.0067 204.0939 14.41405084227759
+FUSE 1
+1 25791U 99035A   03292.09703250  .00000466  00000-0  86677-4 0  9749
+2 25791  24.9816  43.4715 0010662 147.9465 212.1683 14.41404859227645
+FUSE 1
+1 25791U 99035A   03290.98925305  .00000496  00000-0  95741-4 0  9736
+2 25791  24.9815  50.2722 0010596 136.9264 223.2143 14.41404097227489
+FUSE 1
+1 25791U 99035A   03289.81223159  .00000457  00000-0  84144-4 0  9725
+2 25791  24.9826  57.4936 0010620 125.6318 234.5184 14.41403544227318
+FUSE 1
+1 25791U 99035A   03288.77368245 +.00000424 +00000-0 +74086-4 0 09802
+2 25791 024.9826 063.8560 0010538 115.2199 244.9403 14.41402817227166
+FUSE 1
+1 25791U 99035A   03288.56597245  .00000409  00000-0  69342-4 0  9715
+2 25791  24.9830  65.1298 0010470 113.2118 246.9490 14.41402657227135
+FUSE 1
+1 25791U 99035A   03287.80436833 +.00000487 +00000-0 +93214-4 0 09863
+2 25791 024.9823 069.7945 0010522 105.3271 254.8405 14.41402718227026
+FUSE 1
+1 25791U 99035A   03286.83505381  .00000474  00000-0  89149-4 0  9701
+2 25791  24.9821  75.7317 0010429  95.3344 264.8358 14.41401993226884
+FUSE 1
+1 25791U 99035A   03285.86573823 +.00000465 +00000-0 +86378-4 0 09878
+2 25791 024.9822 081.6696 0010346 085.1348 275.0344 14.41401345226745
+FUSE 1
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diff --git a/src/cal/get_tle/tmp/FUSE.TLE b/src/cal/get_tle/tmp/FUSE.TLE
new file mode 100644
index 0000000..75e788e
--- /dev/null
+++ b/src/cal/get_tle/tmp/FUSE.TLE
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new file mode 100644
index 0000000..f70af2e
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diff --git a/src/cal/get_tle/tmp/FUSE.TLE.awf b/src/cal/get_tle/tmp/FUSE.TLE.awf
new file mode 100644
index 0000000..867ba5f
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diff --git a/src/cal/get_tle/tmp/FUSE.TLE.kruk b/src/cal/get_tle/tmp/FUSE.TLE.kruk
new file mode 100644
index 0000000..a15222b
--- /dev/null
+++ b/src/cal/get_tle/tmp/FUSE.TLE.kruk
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+2 25791 024.9851 305.5600 0011277 118.2109 241.9541 14.38957529009068
+FUSE 1
+1 25791U 99035A   99237.43380917  .00000519  00000-0  10841-3 0   178
+2 25791  24.9853 312.3322 0011217 106.6278 253.5464 14.38956402  8903
+FUSE 1
+1 25791U 99035A   99236.46284262 +.00000461 +00000-0 +90008-4 0 00705
+2 25791 024.9853 318.2560 0011086 096.8361 263.3410 14.38955295008762
+FUSE 1
+1 25791U 99035A   99236.25477872 +.00000452 +00000-0 +87040-4 0 00615
+2 25791 024.9853 319.5272 0011052 094.6665 265.5117 14.38955073008731
+FUSE 1
+1 25791U 99035A   99235.28381051 +.00000458 +00000-0 +89138-4 0 00470
+2 25791 024.9852 325.4528 0011033 084.2171 275.9597 14.38954552008598
+FUSE 1
+1 25791U 99035A   99233.61929130 +.00000451 +00000-0 +86895-4 0 00303
+2 25791 024.9853 335.6110 0010986 066.4129 293.7536 14.38953524008353
+FUSE 1
+1 25791U 99035A   99232.50961001  .00000368  00000-0  60512-4 0   162
+2 25791  24.9859 342.3821 0010848  54.6767 305.4755 14.38952340  8198
+FUSE 1
+1 25791U 99035A   99230.70637369 +.00000429 +00000-0 +79925-4 0 00424
+2 25791 024.9854 353.3830 0010964 035.3348 324.7888 14.38952031007934
+FUSE 1
+1 25791U 99035A   99229.59668927 +.00000395 +00000-0 +68969-4 0 00285
+2 25791 024.9857 000.1562 0010882 023.2043 336.8948 14.38951224007779
+FUSE 1
+1 25791U 99035A   99228.48700287 +.00000471 +00000-0 +93172-4 0 00221
+2 25791 024.9853 006.9252 0010851 011.6095 348.4667 14.38951260007619
+FUSE 1
+1 25791U 99035A   99227.72409421  .00000487  00000-0  98308-4 0   158
+2 25791  24.9851  11.5809 0010930   3.6815 356.3773 14.38950858  7502
+FUSE 1
+1 25791U 99035A   99223.56276789  .00000619  00000-0  14028-3 0   147
+2 25791  24.9842  36.9742 0011040 318.0438  41.9206 14.38948712  6903
+FUSE 1
+1 25791U 99035A   99218.63853449  .00000720  00000-0  17250-3 0   135
+2 25791  24.9828  67.0232 0011431 267.3032  92.6167 14.38944759  6193
+FUSE 1
+1 25791U 99035A   99216.97400544 +.00000683 +00000-0 +16063-3 0 00166
+2 25791 024.9829 077.1763 0011588 249.8240 110.1026 14.38942807005959
+FUSE 1
+1 25791U 99035A   99215.72561041  .00001104  00000-0  29513-3 0   127
+2 25791  24.9823  84.7905 0011295 237.0915 122.8597 14.38943232  5774
+FUSE 1
+1 25791U 99035A   99213.99172686 +.00000755 +00000-0 +18386-3 0 00281
+2 25791 024.9829 095.3690 0011291 219.0401 140.9295 14.38939332005520
+FUSE 1
+1 25791U 99035A   99213.02075147 +.00000641 +00000-0 +14744-3 0 00175
+2 25791 024.9830 101.2939 0011410 209.3286 150.6585 14.38937829005384
+FUSE 1
+1 25791U 99035A   99212.88204088  .00000581  00000-0  12826-3 0   112
+2 25791  24.9832 102.1415 0011463 208.2710 151.7177 14.38937383  5365
+FUSE 1
+1 25791U 99035A   99211.07879897 +.00000483 +00000-0 +96970-4 0 00493
+2 25791 024.9832 113.1440 0011683 189.9414 170.0864 14.38935491005102
+FUSE 1
+1 25791U 99035A   99210.10782220 +.00000457 +00000-0 +88695-4 0 00361
+2 25791 024.9830 119.0680 0011645 180.0206 180.0306 14.38934715004963
+FUSE 1
+1 25791U 99035A   99209.13684459 +.00000476 +00000-0 +94628-4 0 00215
+2 25791 024.9829 124.9914 0011669 170.0019 190.0732 14.38934254004820
+FUSE 1
+1 25791U 99035A   99208.85942248  .00000483  00000-0  96822-4 0   100
+2 25791  24.9830 126.6849 0011617 167.3014 192.7802 14.38934135  4785
+FUSE 1
+1 25791U 99035A   99208.16586648 +.00000509 +00000-0 +10534-3 0 00689
+2 25791 024.9829 130.9163 0011612 160.0034 200.0933 14.38933809004681
+FUSE 1
+1 25791U 99035A   99207.12553224 +.00000477 +00000-0 +95090-4 0 00537
+2 25791 024.9830 137.2648 0011506 149.5759 210.5420 14.38933010004534
+FUSE 1
+1 25791U 99035A   99206.15455295 +.00000436 +00000-0 +81952-4 0 00388
+2 25791 024.9831 143.1889 0011456 139.5200 220.6160 14.38932240004393
+FUSE 1
+1 25791U 99035A   99205.11421632 +.00000433 +00000-0 +81097-4 0 00221
+2 25791 024.9835 149.5359 0011411 129.0298 231.1227 14.38931694004248
+FUSE 1
+1 25791U 99035A   99204.21259024  .00000427  00000-0  79119-4 0    95
+2 25791  24.9835 155.0370 0011324 120.0292 240.1341 14.38931194  4119
+FUSE 1
+1 25791U 99035A   99203.17225182 +.00000414 +00000-0 +74992-4 0 00525
+2 25791 024.9835 161.3843 0011233 109.2556 250.9169 14.38930540003968
+FUSE 1
+1 25791U 99035A   99202.13191170 +.00000423 +00000-0 +77980-4 0 00383
+2 25791 024.9837 167.7323 0011168 098.4908 261.6865 14.38930164003818
+FUSE 1
+1 25791U 99035A   99201.16092631 +.00000440 +00000-0 +83410-4 0 00235
+2 25791 024.9837 173.6562 0011126 088.3941 271.7841 14.38929874003674
+FUSE 1
+1 25791U 99035A   99200.18994021  .00000454  00000-0  87696-4 0    88
+2 25791  24.9838 179.5806 0011119  78.2644 281.9107 14.38929532  3535
+FUSE 1
+1 25791U 99035A   99200.12059101 +.00000432 +00000-0 +80931-4 0 00725
+2 25791 024.9842 180.0407 0011095 075.8036 284.3701 14.38929430003528
+FUSE 1
+1 25791U 99035A   99199.21895964 +.00000465 +00000-0 +91252-4 0 00631
+2 25791 024.9840 185.5408 0011075 066.4980 293.6690 14.38929231003393
+FUSE 1
+1 25791U 99035A   99198.17861506 +.00000472 +00000-0 +93642-4 0 00475
+2 25791 024.9844 191.8880 0011017 055.5344 304.6202 14.38928745003245
+FUSE 1
+1 25791U 99035A   99197.20762573 +.00000483 +00000-0 +97242-4 0 00328
+2 25791 024.9845 197.8116 0010965 045.0350 315.1043 14.38928247003108
+FUSE 1
+1 25791U 99035A   99196.16727896 +.00000496 +00000-0 +10136-3 0 00130
+2 25791 024.9848 204.1584 0010927 033.8431 326.2770 14.38927757002952
+FUSE 1
+1 25791U 99035A   99195.40435724  .00000525  00000-0  11052-3 0    76
+2 25791  24.9845 208.8116 0010908  25.8212 334.2838 14.38927498  2842
+FUSE 1
+1 25791U 99035A   99195.26564445 +.00000515 +00000-0 +10744-3 0 00732
+2 25791 024.9847 209.6583 0010905 024.2058 335.8962 14.38927325002821
+FUSE 1
+1 25791U 99035A   99194.22529636 +.00000515 +00000-0 +10742-3 0 00547
+2 25791 024.9849 216.0045 0010895 012.9914 347.0873 14.38926634002672
+FUSE 1
+1 25791U 99035A   99193.18494715 +.00000545 +00000-0 +11704-3 0 00384
+2 25791 024.9850 222.3506 0010896 001.9128 358.1416 14.38926205002526
+FUSE 1
+1 25791U 99035A   99192.14459780 +.00000580 +00000-0 +12797-3 0 00193
+2 25791 024.9850 228.6966 0010908 350.8363 009.1951 14.38925741002370
+FUSE 1
+1 25791U 99035A   99191.24296126  .00000600  00000-0  13459-3 0    61
+2 25791  24.9852 234.1962 0010933 341.3306  18.6794 14.38925220  2248
+FUSE 1
+1 25791U 99035A   99189.57840234 +.00000688 +00000-0 +16244-3 0 00431
+2 25791 024.9847 244.3496 0011003 324.3520 035.6271 14.38924327002005
+FUSE 1
+1 25791U 99035A   99188.53805210 +.00000745 +00000-0 +18074-3 0 00304
+2 25791 024.9847 250.6956 0011082 313.4689 046.4896 14.38923665001857
+FUSE 1
+1 25791U 99035A   99187.56705911 +.00000776 +00000-0 +19053-3 0 00181
+2 25791 024.9847 256.6180 0011114 303.2228 056.7215 14.38922773001717
+FUSE 1
+1 25791U 99035A   99187.22027565  .00000809  00000-0  20103-3 0    57
+2 25791  24.9849 258.7334 0011145 299.6070  60.3328 14.38922625  1666
+FUSE 1
+1 25791U 99035A   99186.59606618 +.00000806 +00000-0 +20001-3 0 00658
+2 25791 024.9848 262.5402 0011144 293.0885 066.8449 14.38921812001577
+FUSE 1
+1 25791U 99035A   99185.55571694 +.00000781 +00000-0 +19209-3 0 00489
+2 25791 024.9850 268.8854 0011179 282.1384 077.7873 14.38920354001427
+FUSE 1
+1 25791U 99035A   99184.58472411 +.00000771 +00000-0 +18889-3 0 00356
+2 25791 024.9851 274.8074 0011210 272.0258 087.8967 14.38919111001282
+FUSE 1
+1 25791U 99035A   99183.61373101 +.00000806 +00000-0 +20014-3 0 00199
+2 25791 024.9851 280.7294 0011202 261.9284 097.9951 14.38918148001148
+FUSE
+1 25791U 99035A   99182.64273781  .00000831  00000-0  20827-3 0    48
+2 25791  24.9852 286.6514 0011228 251.8187 108.1089 14.38917064  1005
+FUSE
+1 25791U 99035A   99181.53303177 +.00000885 +00000-0 +22535-3 0 00326
+2 25791 024.9851 293.4193 0011207 240.2024 119.7372 14.38915842000848
+FUSE
+1 25791U 99035A   99180.42332586 +.00000769 +00000-0 +18844-3 0 00250
+2 25791 024.9851 300.1870 0011210 228.6224 131.3324 14.38913850000688
+FUSE
+1 25791U 99035A   99179.72975929 +.00000701 +00000-0 +16654-3 0 00225
+2 25791 024.9851 304.4168 0011211 221.3620 138.6046 14.38912818000589
+FUSE
+1 25791U 99035A   99178.68940879 +.00000540 +00000-0 +11515-3 0 00070
+2 25791 024.9851 310.7614 0011204 210.4757 149.5099 14.38911405000431
+FUSE
+1 25791U 99035A   99178.55069535  .00000518  00000-0  10814-3 0    39
+2 25791  24.9851 311.6073 0011204 209.0295 150.9590 14.38911233   410
+FUSE
+1 25791U 99035A   99177.92648488 +.00000082 +00000-0 -31136-4 0 00408
+2 25791 024.9853 315.4140 0011227 202.4549 157.5464 14.38909900000324
+FUSE
+1 25791U 99035A   99176.95549150 -.00001333 +00000-0 -48314-3 0 00075
+2 25791 024.9860 321.3361 0010962 190.9807 169.0438 14.38907601000185
diff --git a/src/cal/get_tle/tmp/add_tle.pl b/src/cal/get_tle/tmp/add_tle.pl
new file mode 100755
index 0000000..4bdda9e
--- /dev/null
+++ b/src/cal/get_tle/tmp/add_tle.pl
@@ -0,0 +1,182 @@
+#!/usr/local/bin/perl
+use FileHandle;
+
+# ***************************************************
+# add_tle.pl
+# 
+# This Perl module will read in the latest five orbital elements
+# from the file five.tle (which was created by get_tle.pl) and
+# add any new orbital elements to the file FUSE.TLE.  The file
+# FUSE.TLE is in descending order (i.e. the most recent elements
+# are first).  In order to prepend the new TLE onto the old list
+# I found it was easiest to store everything in a temporary file
+# TEMP.TLE and rewrite FUSE.TLE.
+#
+# Author: Ed Murphy
+#
+# History:  Written  July 27, 1999
+#
+# ***************************************************
+
+# Define the file names.  old_maintle_filename is not actually opened,
+# but is used in a system call at the end of the program. 
+
+$input_filename = "five.tle";
+$maintle_filename = "FUSE.TLE";
+$old_maintle_filename = "FUSE.OLD";
+$temp_filename = "TEMP.TLE";
+
+# Open the files.
+open (TLE_INFILE, "<$input_filename") || die "Cannot open $input_filename";
+open (TLE_TEMPFILE, ">$temp_filename") || die "Cannot open $temp_filename";
+open (TLE_MAINFILE, "<$maintle_filename") || die "Cannot open $maintle_filename";
+
+# Read the first two lines from the maintle file to get the date of the
+# most recent set of TLEs.  Save these lines for later output.
+    $lineout1 = <TLE_MAINFILE>;
+    $lineout2 = <TLE_MAINFILE>;
+    $last_date = substr($lineout2,18,14);
+
+# get rid of the blank line at the beginning of five.tle file
+    $line = <TLE_INFILE>;  
+
+# Cycle through the five.tle file and look for files more recent than
+# last_date.  
+    while ($line1 = <TLE_INFILE>) {
+        $sat_name = substr($line1,0,4);
+        $line2 = <TLE_INFILE>;
+        $line3 = <TLE_INFILE>;
+        $tle_date = substr($line2,18,14);
+        $id2 = substr($line2, 2, 5);
+        $id3 = substr($line3, 2, 5);
+        # if the TLE is more recent, print it out to the TEMP file.
+        if (($tle_date > $last_date+0.05) && ($sat_name eq "FUSE") && ($id2 == 25791) && ($id3 == 25791)) {
+            &check_tle;
+            print TLE_TEMPFILE $line1;
+            print TLE_TEMPFILE $line2;
+            print TLE_TEMPFILE $line3;
+            # Send this output to screen to make sure TLEs look OK
+            if ($tle_flag != 0) {
+		print STDOUT "ERROR: Possible error in TLE:\n";
+            }
+            print STDOUT "The new TLEs are:\n";
+            print STDOUT $line1;
+            print STDOUT $line2;
+            print STDOUT $line3;
+	}
+
+    }
+
+# Now add the MAINTLE file to the end of the TEMPFILE
+    print TLE_TEMPFILE $lineout1;
+    print TLE_TEMPFILE $lineout2;
+    while ($line1 = <TLE_MAINFILE>) {
+            print TLE_TEMPFILE $line1;
+    }
+ 
+    close (TLE_INFILE);
+    close (TLE_MAINFILE);
+    close (TLE_TEMPFILE);
+
+# Move the MAINFILE into the old_maintle filename
+# Move the TEMPFILE to be the MAINFILE
+# Remove the five.tle file.
+    system("mv $maintle_filename $old_maintle_filename");
+    system("mv $temp_filename $maintle_filename");
+    system("chmod ug+rw $maintle_filename");
+    system("chgrp sdp $maintle_filename");
+    system("rm -f $input_filename");
+
+### end of Perl script
+
+sub check_tle {
+
+    $tle_flag = 0;
+
+    &parse_lines;
+
+    &calculate_a0;
+
+    &calculate_orbs;
+
+    if (($mean_mot > 14.391) || ($mean_mot < 14.389)) {
+	$tle_flag = 1;
+        print STDOUT "Possible error in mean motion $mean_mot \n";
+    }
+    if (($incl > 24.990) || ($incl < 24.975)) {
+	$tle_flag = 1;
+        print STDOUT "Possible error in inclination $incl \n";
+    }
+    if (($eccen > 0.00120) || ($eccen < 0.00108)) {
+	$tle_flag = 1;
+        print STDOUT "Possible error in eccentricity $eccen \n";
+    }
+    if (($semiax > 7145.0) || ($semiax < 7143.0)) {
+	$tle_flag = 1;
+        print STDOUT "Possible error in semi-major axis $semia \n";
+    }
+    if (($apogee > 777.0) || ($apogee < 773.0)) {
+	$tle_flag = 1;
+        print STDOUT "Possible error in apogee $apogee \n";
+    }
+    if (($perigee > 760.0) || ($perigee < 756.0)) {
+	$tle_flag = 1;
+        print STDOUT "Possible error in perigee $perigee \n";
+    }
+
+}
+
+sub parse_lines {
+$year = substr($line2, 18, 2);
+$doy = substr($line2, 20, 3);
+$dayfrac = substr($line2, 23, 9);
+$epoch = $year.$doy.$dayfrac;
+$incl = substr($line3, 9, 8);
+$raan = substr($line3, 17,8);
+$eccen = substr($line3, 26, 7);
+$eccen = "0." . $eccen;
+$mean_mot = substr($line3, 52, 11);
+$mean_anom = substr($line3, 43, 8);
+$arg_perig = substr($line3, 34, 8);
+
+
+if ($year > 50) {
+    $year += 1900;
+} else {
+    $year += 2000;
+}
+
+$dayfrac = "0".$dayfrac;
+
+}
+
+sub calculate_a0 {
+
+$mu = 3.986005E5;
+$pi = 3.14159265358979;
+$radian = 0.0174532925200;
+
+$mm=2.0*$pi*$mean_mot/(24.0*60.0);
+$ke=0.74366916E-1;
+$k2=5.413080E-4;
+$a1=($ke/$mm)**(2.0/3.0);
+$inrad = $incl * $radian;
+
+$d1=3.0/2.0*$k2/($a1*$a1)*(3.0*cos($inrad)*cos($inrad)-1.0)/((1.0-$eccen*$eccen)
+**(3.0/2.0));
+$a0=$a1*(1.0-$d1/3.0-$d1*$d1-134.0/81.0*$d1*$d1*$d1);
+$d0=3.0/2.0*$k2/($a0*$a0)*(3.0*cos($inrad)*cos($inrad)-1.0)/((1.0-$eccen*$eccen)
+**(3.0/2.0));
+$semiax=$a0/(1-$d0)*6378.135;
+
+}
+
+sub calculate_orbs {
+
+$period = 60.0*24.0/($mean_mot/(1+$d0));
+$cax=$eccen*$semiax;
+$perigee=$semiax-$cax-6378.1;
+$apogee=$semiax+$cax-6378.1;
+
+}
+
diff --git a/src/cal/get_tle/tmp/check_tle.pl b/src/cal/get_tle/tmp/check_tle.pl
new file mode 100755
index 0000000..483692e
--- /dev/null
+++ b/src/cal/get_tle/tmp/check_tle.pl
@@ -0,0 +1,100 @@
+#!/usr/local/bin/perl
+use FileHandle;
+
+# ***************************************************
+# add_tle.pl
+# 
+# This Perl module will read in the latest five orbital elements
+# from the file five.tle (which was created by get_tle.pl) and
+# add any new orbital elements to the file FUSE.TLE.
+#
+# Author: Ed Murphy
+#
+# History:  Written  July 27, 1999
+#
+# ***************************************************
+
+# Define the file names.  old_maintle_filename is not actually opened,
+# but is used in a system call at the end of the program. 
+
+$maintle_filename = "/data1/fuse/calfuse/calfiles/FUSE.TLE";
+$outtle_filename = "check_tle.dat";
+
+# Open the files.
+open (TLE_MAINFILE, "<$maintle_filename") || die "Cannot open $maintle_filename";
+open (TLE_OUT, ">$outtle_filename") || die "Cannot open $outtle_filename";
+
+# Read the first two lines from the maintle file to get the date of the
+# most recent set of TLEs.  Save these lines for later output.
+while ($line1 = <TLE_MAINFILE>) {
+    $line2 = <TLE_MAINFILE>;
+    $line3 = <TLE_MAINFILE>;
+
+    &parse_lines;
+
+    &calculate_a0;
+    &calculate_orbs;
+
+    printf TLE_OUT "%7.3f %6.2f %6.2f %7.2f %6.2f %7.4f %6.2f %6.2f %8.6f\n",$day, $apogee, $perigee, $semiax, $raan, $incl, $mean_anom, $arg_perig, $eccen;
+
+}
+
+    close (TLE_MAINFILE);
+    close (TLE_OUT);
+
+### end of Perl script
+
+
+sub parse_lines {
+$year = substr($line2, 18, 2);
+$doy = substr($line2, 20, 3);
+$dayfrac = substr($line2, 23, 9);
+$day=$doy.$dayfrac;
+$epoch = $year.$doy.$dayfrac;
+$incl = substr($line3, 9, 8);
+$raan = substr($line3, 17,8);
+$eccen = substr($line3, 26, 7);
+$eccen = "0." . $eccen;
+$mean_mot = substr($line3, 52, 11);
+$mean_anom = substr($line3, 43, 8);
+$arg_perig = substr($line3, 34, 8);
+
+
+if ($year > 50) {
+    $year += 1900;
+} else {
+    $year += 2000;
+}
+
+$dayfrac = "0".$dayfrac;
+
+}
+
+sub calculate_a0 {
+
+$mu = 3.986005E5;
+$pi = 3.14159265358979;
+$radian = 0.0174532925200;
+
+$mm=2.0*$pi*$mean_mot/(24.0*60.0);
+$ke=0.74366916E-1;
+$k2=5.413080E-4;
+$a1=($ke/$mm)**(2.0/3.0);
+$inrad = $incl * $radian;
+
+$d1=3.0/2.0*$k2/($a1*$a1)*(3.0*cos($inrad)*cos($inrad)-1.0)/((1.0-$eccen*$eccen)**(3.0/2.0));
+$a0=$a1*(1.0-$d1/3.0-$d1*$d1-134.0/81.0*$d1*$d1*$d1);
+$d0=3.0/2.0*$k2/($a0*$a0)*(3.0*cos($inrad)*cos($inrad)-1.0)/((1.0-$eccen*$eccen)**(3.0/2.0));
+$semiax=$a0/(1-$d0)*6378.135;
+
+}
+
+sub calculate_orbs {
+
+$period = 60.0*24.0/($mean_mot/(1+$d0));
+$cax=$eccen*$semiax;
+$perigee=$semiax-$cax-6378.1;
+$apogee=$semiax+$cax-6378.1;
+
+}
+
diff --git a/src/cal/get_tle/tmp/five.tle.orig b/src/cal/get_tle/tmp/five.tle.orig
new file mode 100644
index 0000000..6949976
--- /dev/null
+++ b/src/cal/get_tle/tmp/five.tle.orig
@@ -0,0 +1,17 @@
+
+FUSE 1
+1 25791U 99035A   03334.81529517  .00000629  00000-0  13611-3 0    73
+2 25791  24.9828 141.7372 0010396 237.2837 122.6662 14.41449325233814
+FUSE 1
+1 25791U 99035A   03332.32285756  .00000721  00000-0  16400-3 0    51
+2 25791  24.9827 157.0092 0010498 210.6638 149.3252 14.41447882233456
+FUSE 1
+1 25791U 99035A   03331.90745146 +.00000729 +00000-0 +16628-3 0 00081
+2 25791 024.9828 159.5554 0010553 206.5242 153.4727 14.41447542233393
+FUSE 1
+1 25791U 99035A   03331.14587356  .00000725  00000-0  16505-3 0    40
+2 25791  24.9828 164.2238 0010646 198.4715 161.5398 14.41446726233287
+FUSE 1
+1 25791U 99035A   03330.86893587 +.00000724 +00000-0 +16482-3 0 00069
+2 25791 024.9826 165.9208 0010698 195.8086 164.2086 14.41446474233249
+
diff --git a/src/cal/get_tle/tmp/get_tle.logfile b/src/cal/get_tle/tmp/get_tle.logfile
new file mode 100644
index 0000000..570d7e1
--- /dev/null
+++ b/src/cal/get_tle/tmp/get_tle.logfile
@@ -0,0 +1,122 @@
+Trying 128.183.234.87...
+Connected to oig1.gsfc.nasa.gov.
+Escape character is '^]'.
+HTTP/1.0 200 OK
+Server: Microsoft-IIS/3.0
+Date: Mon, 01 Dec 2003 16:18:01 GMT
+Content-type: text/html
+
+<HTML>
+<HEAD>
+<TITLE>OIG Registered user login ok</TITLE>
+</HEAD>
+<H3><LEFT>Registered User Login OK</LEFT></H3>
+<H4><LEFT>2003/12/01 16:18:01 Session time remaining: 02:00:00</LEFT></H4>
+<HR>
+<BODY>
+<PRE>
+
+<B>This account will expire if not accessed at least once every 90 days.</B>
+
+You have sucessfully logged in as registered user: 
+  <B>Mary L. Romelfanger</B>
+
+Please select => <A HREF="/scripts/foxweb.exe/favorhome@app01?tdac=1JT4H2A7I2EJKMM9BXVO">[Continue]</A>
+</PRE>
+<HR>
+<FONT SIZE="-1"><B>&copy 2003  National Aeronautics and Space Administration (NASA). All rights reserved.</B></FONT>
+</BODY>
+</HTML>*** 
+ Starting User's Home Page output page 
+***
+
+Trying 128.183.234.87...
+Connected to oig1.gsfc.nasa.gov.
+Escape character is '^]'.
+HTTP/1.0 200 OK
+Server: Microsoft-IIS/3.0
+Date: Mon, 01 Dec 2003 16:18:02 GMT
+Content-type: text/html
+
+<HTML>
+<HEAD>
+<TITLE>OIG User home page</TITLE>
+</HEAD>
+<H3><CENTER>User Home Page</CENTER></H3>
+<H4><CENTER>2003/12/01 16:18:01 Session time remaining: 02:00:00</CENTER></H4>
+<HR><BODY><PRE>
+<B><center>Due to the existing National Security Restrictions all users must be
+an approved registered user to access data on this site. 10/01/2001
+</center></B>
+
+
+</PRE><HR>
+<PRE>
+<P><LI><A HREF="/scripts/foxweb.exe/ftleadhoc@app01?tdac=OLOW8A0XDA7LVBBJ49TI">TLE Query</A>
+     One time query for TLE's</LI>
+<P><LI><A HREF="/scripts/foxweb.exe/tlarq@app01?tdac=3AROP6H1C6SA5VV2TZUG">TLE Historical Request Form</A></LI>
+<P><LI><A HREF="/scripts/foxweb.exe/syspage@app01?tdac=UJT4H2A7I2EJKMM9BXVO">TLE Format (Standard and Obsolete)</A>
+     Break-out of a Two Line Element.</LI>
+<P><LI><A HREF="/scripts/foxweb.exe/favtle@app01?tdac=JF6A5YKG8YRF4ZZQ2CWH">Favorite TLE Query</A>
+     (the query limit is for any continuous 24 hour period)</LI>
+<P><LI><A HREF="/scripts/foxweb.exe/favtlec@app01?tdac=W0GI3H8ZQH10UTTAO2RC">Favorite TLE Query Configuration</A></LI>
+<P><LI><A HREF="/scripts/foxweb.exe/favhomec@app01?tdac=MZ5VI4W3R4PZ0YY1KSNU">User Home Page Configuration</A>
+     Select to modify what links will appear on this page.</LI>
+<P><LI><A HREF="/scripts/foxweb.exe/supappl@app01?tdac=DT3E9URY1ULTDHHV8KPS">Super-User Application</A>
+     Application to access all daily TLE(s)</LI></PRE>
+<HR><PRE>
+This is your home page configured links area!
+
+No user home page configured links.
+
+<B>You must select "User Home Page Configuration" to
+access other links on this site.</B></PRE><HR><PRE>
+<P><LI><A HREF="/scripts/foxweb.exe/syspage@app01?tdac=H7YF4S1HVS67JCCEQ8LK">General Information</A>
+     Formerly Main Home Page.</LI>
+<P><LI><A HREF="/scripts/foxweb.exe/msglist@app01?tdac=6XKMW1Z8T1HXLQQ7FEYV">Messages</A>
+     Messages to and from System Administrator</LI>
+<P><LI><A HREF="/scripts/foxweb.exe/changepw@app01?tdac=U5QP1E7AME25GIIND0CF">Change Password</A></LI></PRE><HR><FONT SIZE="-1"><B>&copy 2003  National Aeronautics and Space Administration (NASA). All rights reserved.</B></FONT>
+</BODY></HTML>Trying 128.183.234.87...
+Connected to oig1.gsfc.nasa.gov.
+Escape character is '^]'.
+HTTP/1.0 200 OK
+Server: Microsoft-IIS/3.0
+Date: Mon, 01 Dec 2003 16:18:02 GMT
+Content-type: text/html
+
+<HTML>
+<HEAD>
+<TITLE>OIG TLE Query</TITLE>
+</HEAD>
+<H3><CENTER>TLE Query</CENTER></H3>
+<H4><CENTER>2003/12/01 16:18:02 Session time remaining: 01:59:59</CENTER></H4>
+<HR><BODY><PRE>
+In this section you should select up to a maximum of 100 satellite catalog
+numbers, for which you can download the latest set of Two-Line elements.  Enter
+the satellite catalog numbers that you would like to query on, and click on
+submit.
+
+
+Enter the object numbers in the area below separated by spaces.
+Select the desired options.
+Select "Submit".
+(the query limit is for any continuous 24 hour period)</PRE><HR><FORM ACTION="/scripts/foxweb.exe/ftleadhocr@app01?" METHOD="POST">
+<INPUT TYPE="HIDDEN" NAME="tdac" VALUE="N1NKOB4PUBD1ALLSY305">
+<PRE>Enter satellite object numbers:
+<TEXTAREA name=ffv01 ROWS=10 COLS=75>
+</TEXTAREA>
+Format: 
+  <INPUT TYPE=RADIO NAME="ffv02" VALUE="standard"CHECKED>Standard
+  <INPUT TYPE=RADIO NAME="ffv02" VALUE="older">Obsolete<BR>
+Sort on: 
+  <INPUT TYPE=RADIO NAME="ffv03" VALUE="catno"CHECKED>Catalog number
+  <INPUT TYPE=RADIO NAME="ffv03" VALUE="intldes">Internationl designator<BR>
+Number of TLE(s): 
+  <INPUT TYPE=RADIO NAME="ffv04" VALUE="last"CHECKED>Latest One (1)
+  <INPUT TYPE=RADIO NAME="ffv04" VALUE="five">Latest Five (5)<BR>
+<P><INPUT TYPE="SUBMIT" VALUE="Submit"> <INPUT TYPE="RESET"><BR></P>
+</FORM>
+<A HREF="/scripts/foxweb.exe/favorhome@app01?tdac=1JT4H2A7I2EJKMM9BXVO">[ User home page ]</A>
+
+</PRE><HR><FONT SIZE="-1"><B>&copy 2003  National Aeronautics and Space Administration (NASA). All rights reserved.</B></FONT>
+</BODY></HTML>
\ No newline at end of file
diff --git a/src/cal/get_tle/tmp/get_tle.pl b/src/cal/get_tle/tmp/get_tle.pl
new file mode 100755
index 0000000..0693156
--- /dev/null
+++ b/src/cal/get_tle/tmp/get_tle.pl
@@ -0,0 +1,148 @@
+#!/usr/local/bin/perl
+use FileHandle;
+use IPC::Open2;
+
+###
+# OIG TLE retrieval program
+# DJG - 6/14/98
+#
+# Uses a file called "one" which has sat numbers to get
+#
+# Places all output in a single file called "five.tle".
+#
+###
+
+### Configure:
+##$login = "emurphy";
+##$passwd = "bdr529";
+
+$login = "mromelfanger";
+$passwd = "fusejhu";
+$output_filename = "five.tle";
+$log_filename = "get_tle.logfile";
+
+### (end of configure section)
+
+# system("fixlist one tempone");
+# chop($satstoget = `cat tempone`);
+# system("rm -f tempone");
+
+$satstoget = "25791";
+
+# The "output" file collects debugging copies of everything that comes back.
+open(OUT,">$log_filename") || die "Could not open output file";
+
+# The following logs in to OIG and gets the first "continue" code
+
+$host = "oig1.gsfc.nasa.gov";
+#$url = "scripts/foxweb.dll/loginok\@app01?tdac=&ffv01=$login&ffv02=$passwd";
+$url = "scripts/foxweb.exe/loginok\@app01?tdac=&ffv01=$login&ffv02=$passwd";
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+while (<Reader>) {
+  print OUT "$_";  # copy each login screen line to the output file
+  if (/tdac=(\w+)\"/) {
+    $continuecode = $1;  # This code is the "continue" code
+  }
+}
+close(Reader);
+close(Writer);
+
+# $continuecode contains the very first "continue" code after login.
+
+print OUT "*** \n Starting User's Home Page output page \n***\n\n";
+
+# This url accesses the next screen (user home page)
+#$url = "scripts/foxweb.dll/favorhome\@app01?tdac=" . $continuecode;
+$url = "scripts/foxweb.exe/favorhome\@app01?tdac=" . $continuecode;
+# print $url; # debug print
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+
+while (<Reader>) {
+  print OUT "$_";      # copy each line to the output file
+
+  if(/tdac=(\w+)\"/) {
+
+#   Look for the "tle ad hoc query" code and save it
+    chop($word = "$_");
+    if ($word =~ /ftleadhoc.+tdac=(\w+)\"/) {
+      $tlequerycode = "$1";
+    }
+  }
+}
+# close(HOMEPAGE);
+# This access is to the "TLE ad hoc query" web page.
+#$url = "scripts/foxweb.dll/ftleadhoc\@app01?tdac=" . $tlequerycode;
+$url = "scripts/foxweb.exe/ftleadhoc\@app01?tdac=" . $tlequerycode;
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+
+while (<Reader>) {
+  print OUT "$_";  # copy each login screen line to the output file
+
+  # Look for the TLE "submit" code
+  chop($word = "$_");
+  if ($word =~ /tdac\" VALUE=\"(\w+)\"/) {
+    $gotcode2 = "$1";
+  }
+}
+close(Reader);
+close(Writer);
+
+# Compose the TLE query and submit it
+#$url = "scripts/foxweb.dll/ftleadhoc\@app01?tdac=" . $gotcode2;
+$url = "scripts/foxweb.exe/ftleadhoc\@app01?tdac=" . $gotcode2;
+$url .= "&ffv01=" . $satstoget . "&ffv02=standard&ffv03=catno&ffv04=five";
+
+# print "$url\n";  # debug print
+
+# Read the reply and copy the relevant lines to output_filename
+
+$copy = "no";
+open(TLEOUT,">$output_filename") || die "Error opening $output_filename";
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+
+while (<Reader>) {
+  if ($_ =~ /<P>/) {  # End copy operation
+    print "$_";       # write remaining limit to output file
+    $copy = "no";
+  }
+  if ($copy eq "yes") {
+    print TLEOUT "$_";   # copy every line to five.tle
+    # print "$_";          # and to the terminal
+  }
+  if (substr($_,0,5) eq "<PRE>") {  # Begin copy operation
+    $copy = "yes";
+  }
+}
+close(Reader);
+close(Writer);
+close(TLEOUT);
+
+# The following will remove all session files. You can comment it
+# out for debugging.
+# system("rm -f output");
+
+# The following script "fixes up" the output
+# system("fix/do.fix.one");
+
+### end of Perl script
+
diff --git a/src/cal/get_tle/tmp/make_cvzramtool.pl b/src/cal/get_tle/tmp/make_cvzramtool.pl
new file mode 100755
index 0000000..4cb2e01
--- /dev/null
+++ b/src/cal/get_tle/tmp/make_cvzramtool.pl
@@ -0,0 +1,215 @@
+#!/usr/local/bin/perl
+use FileHandle;
+
+# This program will read in the latest FUSE TLE and recreate the 
+# cvz_ram_tool.html web page.
+
+$output_filename = "/data2/violet/htdocs/support/tools/cvz_ram_tool.html";
+open (OUTF, ">$output_filename") || die "Cannot open cvz_ram_tool.html file";
+
+system("chmod ug+rw $output_filename");
+system("chgrp www $output_filename");
+
+$input_filename = "/data1/fuse/calfuse/calfiles/FUSE.TLE";
+open (INP_TLE, "<$input_filename") || die "Cannot open FUSE.TLE file";
+
+$line1 = <INP_TLE>;
+$line2 = <INP_TLE>;
+$line3 = <INP_TLE>;
+
+$id2 = substr($line2, 2, 5);
+$id3 = substr($line3, 2, 5);
+
+if (($id2 != 25791) || ($id3 != 25791)) {
+    print STDOUT "Error in TLE:\n";
+    print STDOUT $line1;
+    print STDOUT $line2;
+    print STDOUT $line3;
+    die "Error in TLE";
+}
+
+close (INP_TLE);
+
+$year = substr($line2, 18, 2);
+$doy = substr($line2, 20, 3);
+$dayfrac = substr($line2, 23, 9);
+$incl = substr($line3, 9, 8);
+$raan = substr($line3, 17,8);
+$eccen = substr($line3, 26, 7);
+$eccen = "0." . $eccen;
+$mean_mot = substr($line3, 52, 11);
+
+if ($year > 50) {
+    $year += 1900;
+} else {
+    $year += 2000;
+}
+
+$dayfrac = "0".$dayfrac;
+
+&convert_doy;
+&convert_dayfrac;
+&calculate_a0;
+
+$now=`date`;
+$datest = substr($now,4,3)." ".substr($now,8,2).", ".substr($now,24,4);
+
+print OUTF "<TITLE>FUSE CVZ/Ram Calculator</TITLE>\n";
+print OUTF "<h1>FUSE Continuous Viewing Zone and Orbit Ram Calculator V1.3</h1>\n";
+print OUTF "<h2>June 12, 1999 </h2>\n";
+
+print OUTF "The FUSE Continuous Viewing Zone and Orbit Ram \n";
+print OUTF "Calculator can determine when a given target \n";
+print OUTF "direction is in the continuous viewing zone. \n";
+print OUTF "It also calculates when a given target lies \n";
+print OUTF "within 20 degrees of the orbital plane and \n";
+print OUTF "cannot be observed due to ram avoidance\n";
+print OUTF "constraints. The default orbital elements \n";
+print OUTF "were last updated on $month $day, $year. \n";
+
+print OUTF "<HR>\n";
+print OUTF "<P>\n";
+print OUTF "<FORM METHOD=POST ACTION=\"http://fuse.pha.jhu.edu/cgi-bin/cvz_ram_tool\">\n";
+
+print OUTF "<INPUT TYPE=\"submit\" VALUE=\"Calculate CVZ visibilities\">\n";
+print OUTF "<INPUT TYPE=\"reset\" VALUE=\"Erase the input fields\">\n";
+print OUTF "<BR>\n";
+  
+print OUTF "<BR>\n";
+print OUTF "<B>Target Parameters:</B>\n";
+print OUTF "<BLOCKQUOTE>\n";
+print OUTF "<BR>\n";
+print OUTF "<B>Right Ascension (format HH:MM:SS.SS):</B>\n";
+print OUTF "<INPUT NAME=\"right_ascension\" SIZE=15> <B>(J2000.0)</B>\n";
+print OUTF "<BR>\n";
+print OUTF "<B>Declination (format -DD:MM:SS.S):</B>\n";
+print OUTF "<INPUT NAME=\"declination\" SIZE=15> <B>(J2000.0)</B>\n";
+print OUTF "<BR>\n";
+print OUTF "</BLOCKQUOTE>\n";
+print OUTF "<BR>\n";
+print OUTF "<B>Output table parameters:</B>\n";
+print OUTF "<BLOCKQUOTE>\n";
+print OUTF "<B> Minimum Earth limb angle: </B><INPUT NAME=\"limb_ang\" SIZE=4 VALUE=\"15.0\"> \n";
+print OUTF "<B>(deg)</B>\n";
+print OUTF "<BR>\n";
+print OUTF "<B>Start Date:</B>\n";
+print OUTF "<SELECT NAME=\"month\">\n";
+print OUTF "<OPTION> <B>$month</B>\n";
+print OUTF "<OPTION> January\n";
+print OUTF "<OPTION> February\n";
+print OUTF "<OPTION> March\n";
+print OUTF "<OPTION> April\n";
+print OUTF "<OPTION> May\n";
+print OUTF "<OPTION> June\n";
+print OUTF "<OPTION> July\n";
+print OUTF "<OPTION> August\n";
+print OUTF "<OPTION> September\n";
+print OUTF "<OPTION> October\n";
+print OUTF "<OPTION> November\n";
+print OUTF "<OPTION> December\n";
+print OUTF "</SELECT>\n";
+print OUTF "<INPUT NAME=\"day\" SIZE=4 VALUE=\"1\">\n";
+print OUTF "<INPUT NAME=\"year\" SIZE=8 VALUE=\"$year\">\n";
+print OUTF "<BR>\n";
+print OUTF "<B>Time step:<INPUT NAME=\"time_step\" SIZE=6 VALUE=\"1.0\">days</B><BR>\n";
+print OUTF "<B>Number of steps:<INPUT NAME=\"number_steps\" SIZE=6 VALUE=\"10\"></B><BR>\n";
+print OUTF "</BLOCKQUOTE>\n";
+print OUTF "<BR>\n";
+print OUTF "<B>FUSE classical Keplarian orbital elements:</B>\n";
+print OUTF "<BLOCKQUOTE>\n";
+print OUTF "<B>Epoch date of elements:</B>\n";
+print OUTF "<SELECT NAME=\"orb_month\">\n";
+print OUTF "<OPTION> $month\n";
+print OUTF "<OPTION> January\n";
+print OUTF "<OPTION> February\n";
+print OUTF "<OPTION> March\n";
+print OUTF "<OPTION> April\n";
+print OUTF "<OPTION> May\n";
+print OUTF "<OPTION> June\n";
+print OUTF "<OPTION> July\n";
+print OUTF "<OPTION> August\n";
+print OUTF "<OPTION> September\n";
+print OUTF "<OPTION> October\n";
+print OUTF "<OPTION> November\n";
+print OUTF "<OPTION> December\n";
+print OUTF "</SELECT>\n";
+print OUTF "<INPUT NAME=\"orb_day\" SIZE=4 VALUE=\"$day\">\n";
+print OUTF "<INPUT NAME=\"orb_year\" SIZE=8 VALUE=\"$year\">\n";
+print OUTF "<BR>\n";
+print OUTF "<B>Epoch UT time of elements (format HH:MM:SS.SS):</B>\n";
+printf OUTF "<INPUT NAME=\"orb_time\" SIZE=12 VALUE=\"%02d:%02d:%05.2f\">\n",$hour,$minute,$second;
+print OUTF "<BR>\n";
+print OUTF "<B>Semi-major axis (km):</B>\n";
+printf OUTF "<INPUT NAME=\"orb_a\" SIZE=15 value=\"%7.3f\"> \n",$semiax;
+print OUTF "<BR>\n";
+print OUTF "<B>Right ascension of the ascending node (degrees):</B>\n";
+print OUTF "<INPUT NAME=\"orb_raan\" SIZE=15 value=\"$raan\">\n";
+print OUTF "<BR>\n";
+print OUTF "<B>Orbit inclination (degrees):</B>\n";
+print OUTF "<INPUT NAME=\"orb_i\" SIZE=15 value=\"$incl\">\n";
+print OUTF "<BR>\n";
+print OUTF "<B>Eccentricity:</B>\n";
+print OUTF "<INPUT NAME=\"orb_e\" SIZE=15 value=\"$eccen\"> \n";
+print OUTF "</BLOCKQUOTE>\n";
+print OUTF "<BR>\n";
+print OUTF "<INPUT TYPE=\"submit\" VALUE=\"Calculate CVZ visibilities\">\n";
+print OUTF "<INPUT TYPE=\"reset\" VALUE=\"Erase the input fields\">\n";
+print OUTF "</FORM>\n";
+
+print OUTF "<HR>\n";
+print OUTF "This page uses the <a href=\"http://star-www.rl.ac.uk/\"> STARLINK </a>\n";
+print OUTF "set of astronomical subroutines.\n";
+print OUTF "<BR>\n";
+print OUTF "This page was automatically generated on $now";
+print OUTF "<BR>\n";
+print OUTF "<a href=\"mailto:emurphy\@pha.jhu.edu\"><address>emurphy\@pha.jhu.edu</address></a>\n";
+
+close (OUTF);
+
+### end of Perl script
+
+
+sub convert_doy {
+    @daytab1 = (0, 31, 29, 31, 30, 31, 30, 31, 31, 30, 31, 30, 31);
+    @daytab2 = (0, 31, 28, 31, 30, 31, 30, 31, 31, 30, 31, 30, 31);
+    @monthstr = ("", "January", "February", "March", "April", "May", "June", "July", "August", "September", "October", "November", "December");
+
+    if ((($year%4 == 0) && ($year%100 != 0)) || ($year%400 == 0)) {
+        # $year is a leap year use daytab1
+        for ($i = 1; $doy > $daytab1[$i]; $i++) {
+	    $doy -= $daytab1[$i];
+	}
+    } else {
+        # $year is not a leap year, use daytab2
+        for ($i = 1; $doy > $daytab2[$i]; $i++) {
+	    $doy -= $daytab2[$i];
+	}
+    }
+    $month = $monthstr[$i];
+    $day = $doy;
+}
+
+sub convert_dayfrac {
+    $dayfrac *= 24.0;
+    $hour = int($dayfrac);
+    $minute = int(($dayfrac-$hour)*60.0);
+    $second = ((($dayfrac-$hour)*60.0)-$minute)*60.0;
+}
+
+sub calculate_a0 {
+
+$mu = 3.986005E5;
+$pi = 3.14159265358979;
+$radian = 0.0174532925200;
+
+$mm=2.0*$pi*$mean_mot/(24.0*60.0);
+$ke=0.74366916E-1;
+$k2=5.413080E-4;
+$a1=($ke/$mm)**(2.0/3.0);
+$inrad = $incl * $radian;
+
+$d1=3.0/2.0*$k2/($a1*$a1)*(3.0*cos($inrad)*cos($inrad)-1.0)/((1.0-$eccen*$eccen)**(3.0/2.0));
+$a0=$a1*(1.0-$d1/3.0-$d1*$d1-134.0/81.0*$d1*$d1*$d1);
+$d0=3.0/2.0*$k2/($a0*$a0)*(3.0*cos($inrad)*cos($inrad)-1.0)/((1.0-$eccen*$eccen)**(3.0/2.0));
+$semiax=$a0/(1-$d0)*6378.135;
+}
diff --git a/src/cal/get_tle/tmp/make_orbit.pl b/src/cal/get_tle/tmp/make_orbit.pl
new file mode 100755
index 0000000..a8f00ff
--- /dev/null
+++ b/src/cal/get_tle/tmp/make_orbit.pl
@@ -0,0 +1,233 @@
+#!/usr/local/bin/perl
+use FileHandle;
+
+# Ed Murphy's program to rewrite the orbit page
+# Updated 03/27/00  Changed GSOC to Heavens Above
+
+$output_filename = "/data2/violet/htdocs/users/orbit.html";
+open (OUTF, ">$output_filename") || die "Cannot open $output_filename file";
+
+system("chmod ug+rw $output_filename");
+system("chgrp www $output_filename");
+
+$input_filename = "/data1/fuse/calfuse/calfiles/FUSE.TLE";
+open (INP_TLE, "<$input_filename") || die "Cannot open $input_filename file";
+
+$satid = 25791;
+
+&input_lines;
+
+close (INP_TLE);
+
+&parse_lines;
+
+&convert_doy;
+&convert_dayfrac;
+&calculate_a0;
+&calculate_orbs;
+
+$now=`date`;
+$datest = substr($now,4,3)." ".substr($now,8,2).", ".substr($now,24,4);
+
+print OUTF "<HTML>\n";
+print OUTF "<HEAD>\n";
+print OUTF "<title>FUSE Orbital Elements page</title>\n";
+print OUTF "</HEAD>\n";
+print OUTF "<BODY bgcolor=#ffffff ALINK=\"#000000\" VLINK=\"darkblue\">\n";
+print OUTF "<center>\n";
+print OUTF "<table width=640>\n";
+print OUTF "<tr><td>\n";
+print OUTF "<img src=\"/figures/purple_line2.gif\" width=640>\n";
+print OUTF "<table cellpadding=5 cellspacing=5 width=550>\n";
+print OUTF "<tr>\n";
+print OUTF "<td valign=top align=left>\n";
+print OUTF "<img src=\"/figures/andromeda_moo_small.gif\">\n";
+print OUTF "</td>\n";
+print OUTF "<td valign=top align=left>\n";
+print OUTF "<font size=+3><font color=\"#6666CC\">\n";
+print OUTF "<b>FUSE<P>\n";
+print OUTF "<i>Orbital Elements</font></font></i></b>\n";
+print OUTF "</td>\n";
+print OUTF "</tr>\n";
+print OUTF "</table>\n";
+print OUTF "<img src=\"/figures/purple_line2.gif\" width=640>\n";
+print OUTF "<p>\n";
+print OUTF "<center>\n";
+print OUTF "<font color=\"#CC0099\" size=4><b>\n";
+print OUTF "Where is FUSE now?<br></b></font>\n";
+print OUTF "<font size=4>Check out the\n";
+print OUTF "<a href=\"http://www.heavens-above.com/orbitdisplay.asp?lat=39.3&lng=-76.6&loc=BALTIMORE&TZ=EST&satid=25791\" >\n";
+print OUTF "Heavens-Above Satellite Predictions page </a></font>.\n";
+print OUTF "</center>\n";
+print OUTF "<P>\n";
+print OUTF "<hr>\n";
+print OUTF "<p><pre>\n";
+print OUTF " \n";
+print OUTF  "FUSE orbital elements:\n";
+print OUTF  "     NORAD number       25791\n";
+print OUTF  "     International ID  99035A\n";
+print OUTF  " \n";
+
+&print_orb;
+
+print OUTF "</pre>\n";
+
+&print_tail;
+
+close (OUTF);
+
+### end of Perl script
+
+
+sub convert_doy {
+    @daytab1 = (0, 31, 29, 31, 30, 31, 30, 31, 31, 30, 31, 30, 31);
+    @daytab2 = (0, 31, 28, 31, 30, 31, 30, 31, 31, 30, 31, 30, 31);
+    @monthstr = ("", "January", "February", "March", "April", "May", "June", "July", "August", "September", "October", "November", "December");
+
+    if ((($year%4 == 0) && ($year%100 != 0)) || ($year%400 == 0)) {
+        # $year is a leap year use daytab1
+        for ($i = 1; $doy > $daytab1[$i]; $i++) {
+	    $doy -= $daytab1[$i];
+	}
+    } else {
+        # $year is not a leap year, use daytab2
+        for ($i = 1; $doy > $daytab2[$i]; $i++) {
+	    $doy -= $daytab2[$i];
+	}
+    }
+    $month = $monthstr[$i];
+    $day = $doy;
+}
+
+sub convert_dayfrac {
+    $dayfrac *= 24.0;
+    $hour = int($dayfrac);
+    $minute = int(($dayfrac-$hour)*60.0);
+    $second = ((($dayfrac-$hour)*60.0)-$minute)*60.0;
+}
+
+sub input_lines {
+$line1 = <INP_TLE>;
+$line2 = <INP_TLE>;
+$line3 = <INP_TLE>;
+
+$id2 = substr($line2, 2, 5);
+$id3 = substr($line3, 2, 5);
+
+if (($id2 != $satid) || ($id3 != $satid)) {
+    print STDOUT "Error in TLE:\n";
+    print STDOUT $line1;
+    print STDOUT $line2;
+    print STDOUT $line3;
+#    die "Error in TLE";
+}
+
+}
+
+sub parse_lines {
+$year = substr($line2, 18, 2);
+$doy = substr($line2, 20, 3);
+$dayfrac = substr($line2, 23, 9);
+$epoch = $year.$doy.$dayfrac;
+$incl = substr($line3, 9, 8);
+$raan = substr($line3, 17,8);
+$eccen = substr($line3, 26, 7);
+$eccen = "0." . $eccen;
+$mean_mot = substr($line3, 52, 11);
+$mean_anom = substr($line3, 43, 8);
+$arg_perig = substr($line3, 34, 8);
+
+
+if ($year > 50) {
+    $year += 1900;
+} else {
+    $year += 2000;
+}
+
+$dayfrac = "0".$dayfrac;
+
+}
+
+sub calculate_a0 {
+
+$mu = 3.986005E5;
+$pi = 3.14159265358979;
+$radian = 0.0174532925200;
+
+$mm=2.0*$pi*$mean_mot/(24.0*60.0);
+$ke=0.74366916E-1;
+$k2=5.413080E-4;
+$a1=($ke/$mm)**(2.0/3.0);
+$inrad = $incl * $radian;
+
+$d1=3.0/2.0*$k2/($a1*$a1)*(3.0*cos($inrad)*cos($inrad)-1.0)/((1.0-$eccen*$eccen)**(3.0/2.0));
+$a0=$a1*(1.0-$d1/3.0-$d1*$d1-134.0/81.0*$d1*$d1*$d1);
+$d0=3.0/2.0*$k2/($a0*$a0)*(3.0*cos($inrad)*cos($inrad)-1.0)/((1.0-$eccen*$eccen)**(3.0/2.0));
+$semiax=$a0/(1-$d0)*6378.135;
+
+}
+
+sub calculate_orbs {
+
+$period = 60.0*24.0/($mean_mot/(1+$d0));
+$cax=$eccen*$semiax;
+$perigee=$semiax-$cax-6378.1;
+$apogee=$semiax+$cax-6378.1;
+
+}
+
+sub print_orb {
+print OUTF  "     Epoch           $epoch\n";
+printf OUTF "     Semimajor axis   %7.2f km\n",$semiax;
+printf OUTF "     Apogee            %5.2f km\n",$apogee;
+printf OUTF "     Perigee           %5.2f km\n",$perigee;
+print OUTF  "     Eccentricity   $eccen\n";
+printf OUTF  "     Inclination       %6.2f degrees\n",$incl;
+printf OUTF "     Period            %6.2f minutes\n",$period;
+printf OUTF "     RA of asc. node   %6.2f degrees\n",$raan;
+printf OUTF "     Arg. of perigee   %6.2f degrees\n",$arg_perig;
+printf OUTF "     Mean anomaly      %6.2f degrees\n",$mean_anom;
+print OUTF  " \n";
+
+}
+
+sub print_tail {
+print OUTF "<p>";
+
+print OUTF "The FUSE Delta II second stage (NORAD #25792) reentered on \n";
+print OUTF "the morning of August 4, 1999 during orbit number 708.  \n";
+print OUTF "According to predictions by Alan Pickup, reentry \n";
+print OUTF "occured within 90 minutes of 5:31 UT, probably over the \n";
+print OUTF "Arabian Sea or India.  The final orbit was 119 x 103 km (74 x 64 mi).\n";
+print OUTF "<p>";
+print OUTF "<center>";
+print OUTF "<font size=+2><font color=\"#6666CC\">\n";
+print OUTF "<a href=\"reentry.html\"> Could anything have survived reentry?</a></font></font><p>\n";
+print OUTF "</center>";
+print OUTF "<img align=center src=\"delta2decay.gif\">\n";
+print OUTF "<P>These numbers assume a Keplerian orbit; the actual apogee and perigee \n";
+print OUTF "will differ by a few km on an orbit-to-orbit basis.\n";
+print OUTF "<p>";
+print OUTF "<p>The NORAD Two-Line Elements (TLEs) for FUSE can be found in the file \n";
+print OUTF "<a href=\"./FUSE.TLE\" > FUSE.TLE </A>.\n";
+print OUTF "<p> \n";
+print OUTF "This page is automatically updated daily.  I wish to thank \n";
+print OUTF "<a href=\"mailto:deej\@deej.com\">Doyle Groves</a> \n";
+print OUTF "for providing a Perl script to access the NASA\n";
+print OUTF "Orbital Information Group web page.\n";
+print OUTF "<p> Ed Murphy, <a href=\"mailto:emurphy\@pha.jhu.edu\">\n";
+print OUTF "<address>emurphy\@pha.jhu.edu</address></a>\n";
+print OUTF "<P>\n";
+print OUTF "<img src=\"/figures/purple_line2.gif\" width=640>\n";
+print OUTF "<P>\n";
+print OUTF "Last changed: $datest.\n";
+print OUTF "<P>\n";
+print OUTF "<i><a href=\"/index.shtml\">Return to the FUSE home page.</a></i><br clear=left>\n";
+print OUTF "<p>\n";
+print OUTF "</td></tr>\n";
+print OUTF "</table>\n";
+print OUTF "</center>\n";
+print OUTF "</BODY>\n";
+print OUTF "</HTML>\n";
+
+}
diff --git a/src/cal/get_tle/tmp/test_get_tle.pl b/src/cal/get_tle/tmp/test_get_tle.pl
new file mode 100755
index 0000000..33b72e5
--- /dev/null
+++ b/src/cal/get_tle/tmp/test_get_tle.pl
@@ -0,0 +1,148 @@
+#!/usr/local/bin/perl
+use FileHandle;
+use IPC::Open2;
+
+###
+# OIG TLE retrieval program
+# DJG - 6/14/98
+#
+# Uses a file called "one" which has sat numbers to get
+#
+# Places all output in a single file called "five.tle".
+#
+###
+
+### Configure:
+##$login = "emurphy";
+##$passwd = "bdr529";
+
+$login = "mromelfanger";
+$passwd = "fusejhu";
+$output_filename = "/data1/fuse/calfuse/caltemp/five.tle";
+$log_filename = "/data1/fuse/calfuse/caltemp/get_tle.logfile";
+
+### (end of configure section)
+
+# system("fixlist one tempone");
+# chop($satstoget = `cat tempone`);
+# system("rm -f tempone");
+
+$satstoget = "25791";
+
+# The "output" file collects debugging copies of everything that comes back.
+open(OUT,">$log_filename") || die "Could not open output file";
+
+# The following logs in to OIG and gets the first "continue" code
+
+$host = "oig1.gsfc.nasa.gov";
+#$url = "scripts/foxweb.dll/loginok\@app01?tdac=&ffv01=$login&ffv02=$passwd";
+$url = "scripts/foxweb.exe/loginok\@app01?tdac=&ffv01=$login&ffv02=$passwd";
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+while (<Reader>) {
+  print OUT "$_";  # copy each login screen line to the output file
+  if (/tdac=(\w+)\"/) {
+    $continuecode = $1;  # This code is the "continue" code
+  }
+}
+close(Reader);
+close(Writer);
+
+# $continuecode contains the very first "continue" code after login.
+
+print OUT "*** \n Starting User's Home Page output page \n***\n\n";
+
+# This url accesses the next screen (user home page)
+#$url = "scripts/foxweb.dll/favorhome\@app01?tdac=" . $continuecode;
+$url = "scripts/foxweb.exe/favorhome\@app01?tdac=" . $continuecode;
+# print $url; # debug print
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+
+while (<Reader>) {
+  print OUT "$_";      # copy each line to the output file
+
+  if(/tdac=(\w+)\"/) {
+
+#   Look for the "tle ad hoc query" code and save it
+    chop($word = "$_");
+    if ($word =~ /ftleadhoc.+tdac=(\w+)\"/) {
+      $tlequerycode = "$1";
+    }
+  }
+}
+# close(HOMEPAGE);
+# This access is to the "TLE ad hoc query" web page.
+#$url = "scripts/foxweb.dll/ftleadhoc\@app01?tdac=" . $tlequerycode;
+$url = "scripts/foxweb.exe/ftleadhoc\@app01?tdac=" . $tlequerycode;
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+
+while (<Reader>) {
+  print OUT "$_";  # copy each login screen line to the output file
+
+  # Look for the TLE "submit" code
+  chop($word = "$_");
+  if ($word =~ /tdac\" VALUE=\"(\w+)\"/) {
+    $gotcode2 = "$1";
+  }
+}
+close(Reader);
+close(Writer);
+
+# Compose the TLE query and submit it
+#$url = "scripts/foxweb.dll/ftleadhoc\@app01?tdac=" . $gotcode2;
+$url = "scripts/foxweb.exe/ftleadhoc\@app01?tdac=" . $gotcode2;
+$url .= "&ffv01=" . $satstoget . "&ffv02=standard&ffv03=catno&ffv04=five";
+
+# print "$url\n";  # debug print
+
+# Read the reply and copy the relevant lines to output_filename
+
+$copy = "no";
+open(TLEOUT,">$output_filename") || die "Error opening $output_filename";
+
+open2 (\*Reader, \*Writer, "telnet $host 80") || die "Error opening connection";
+Writer->autoflush();
+
+print Reader "telnet $host 80\n";
+print Writer "GET \/$url\n";
+
+while (<Reader>) {
+  if ($_ =~ /<P>/) {  # End copy operation
+    print "$_";       # write remaining limit to output file
+    $copy = "no";
+  }
+  if ($copy eq "yes") {
+    print TLEOUT "$_";   # copy every line to five.tle
+    # print "$_";          # and to the terminal
+  }
+  if (substr($_,0,5) eq "<PRE>") {  # Begin copy operation
+    $copy = "yes";
+  }
+}
+close(Reader);
+close(Writer);
+close(TLEOUT);
+
+# The following will remove all session files. You can comment it
+# out for debugging.
+# system("rm -f output");
+
+# The following script "fixes up" the output
+# system("fix/do.fix.one");
+
+### end of Perl script
+
diff --git a/src/cal/get_tle/tmp/test_tle.csh b/src/cal/get_tle/tmp/test_tle.csh
new file mode 100755
index 0000000..5431552
--- /dev/null
+++ b/src/cal/get_tle/tmp/test_tle.csh
@@ -0,0 +1,50 @@
+#!/bin/csh -f
+#******************************************************************************
+#*              Johns Hopkins University
+#*              Center For Astrophysical Sciences
+#*              FUSE
+#*****************************************************************************
+#*
+#* Synopsis:    update_tle
+#*
+#* Description: Shell script for automatically downloading the latest
+#*              orbital elements from the GSFC OIG, and placing these
+#*              elements in the FUSE.TLE file.  It will also update 
+#*              the cvz_ram_tool.html calculator.
+#*		
+#*		All messages are to stdout or stderr.
+#*
+#* Arguments:   None
+#*
+#* Returns:     Exit codes:
+#*			0		successful execution
+#* 
+#* History:     07/27/99        emm     Begin work.
+#******************************************************************************/
+
+set tlestat=0
+
+# Step 1
+/usr/local/fusesw/calfuse/current/src/cal/get_tle/get_tle.pl
+set cfstat=$status
+
+# Step 2
+if !({$cfstat}) then
+    /usr/local/fusesw/calfuse/current/src/cal/get_tle/add_tle.pl
+    set cfstat=$status
+endif
+
+# Step 3
+if !({$cfstat}) then
+    /usr/local/fusesw/calfuse/current/src/cal/get_tle/make_cvzramtool.pl
+    set cfstat=$status
+endif
+
+# Step 4
+if !({$cfstat}) then
+    /usr/local/fusesw/calfuse/current/src/cal/get_tle/make_orbit.pl
+    set cfstat=$status
+endif
+
+exit($cfstat)
+
diff --git a/src/cal/get_tle/tmp/update_tle.csh b/src/cal/get_tle/tmp/update_tle.csh
new file mode 100755
index 0000000..5c076bd
--- /dev/null
+++ b/src/cal/get_tle/tmp/update_tle.csh
@@ -0,0 +1,55 @@
+#!/bin/csh -f
+#******************************************************************************
+#*              Johns Hopkins University
+#*              Center For Astrophysical Sciences
+#*              FUSE
+#*****************************************************************************
+#*
+#* Synopsis:    update_tle
+#*
+#* Description: Shell script for automatically downloading the latest
+#*              orbital elements from the GSFC OIG, and placing these
+#*              elements in the FUSE.TLE file.  It will also update 
+#*              the cvz_ram_tool.html calculator.
+#*		
+#*		All messages are to stdout or stderr.
+#*
+#* Arguments:   None
+#*
+#* Returns:     Exit codes:
+#*			0		successful execution
+#* 
+#* History:     07/27/99        emm     Begin work.
+#*              10/23/00        mlr     changed path from v1.4 to current
+#******************************************************************************/
+
+set tlestat=0
+
+# Step 1
+#/usr/local/fusesw/calfuse/v1.4/src/cal/get_tle/get_tle.pl
+/usr/local/fusesw/calfuse/current/src/cal/get_tle/get_tle.pl
+set cfstat=$status
+
+# Step 2
+if !({$cfstat}) then
+#    /usr/local/fusesw/calfuse/v1.4/src/cal/get_tle/add_tle.pl
+    /usr/local/fusesw/calfuse/current/src/cal/get_tle/add_tle.pl
+    set cfstat=$status
+endif
+
+# Step 3
+if !({$cfstat}) then
+#    /usr/local/fusesw/calfuse/v1.4/src/cal/get_tle/make_cvzramtool.pl
+    /usr/local/fusesw/calfuse/current/src/cal/get_tle/make_cvzramtool.pl
+    set cfstat=$status
+endif
+
+# Step 4
+if !({$cfstat}) then
+#    /usr/local/fusesw/calfuse/v1.4/src/cal/get_tle/make_orbit.pl
+    /usr/local/fusesw/calfuse/current/src/cal/get_tle/make_orbit.pl
+    set cfstat=$status
+endif
+
+exit($cfstat)
+
diff --git a/src/cal/get_tle/update_tle.csh b/src/cal/get_tle/update_tle.csh
new file mode 100755
index 0000000..bc9ae34
--- /dev/null
+++ b/src/cal/get_tle/update_tle.csh
@@ -0,0 +1,57 @@
+#!/bin/csh -f
+#******************************************************************************
+#*              Johns Hopkins University
+#*              Center For Astrophysical Sciences
+#*              FUSE
+#*****************************************************************************
+#*
+#* Synopsis:    update_tle
+#*
+#* Description: Shell script for automatically downloading the latest
+#*              orbital elements from the GSFC OIG, and placing these
+#*              elements in the FUSE.TLE file.  It will also update 
+#*              the cvz_ram_tool.html calculator.
+#*		
+#*		All messages are to stdout or stderr.
+#*
+#* Arguments:   None
+#*
+#* Returns:     Exit codes:
+#*			0		successful execution
+#* 
+#* History:     07/27/99        emm     Begin work.
+#*              10/23/00        mlr     changed path from v1.4 to current
+#******************************************************************************/
+
+set tlestat=0
+
+# Step 1
+#/usr/local/fusesw/calfuse/v1.4/src/cal/get_tle/get_tle.pl
+#/usr/local/fusesw/calfuse/current/src/cal/get_tle/get_tle.pl
+#/usr/local/j2sdk1.4.2_06/bin/java -classpath /usr/local/fusesw/calfuse/current/src/cal/get_tle GetTLE
+/usr/local/java/bin/java -classpath /usr/local/fusesw/calfuse/current/src/cal/get_tle GetTLE
+set cfstat=$status
+
+# Step 2
+if !({$cfstat}) then
+#    /usr/local/fusesw/calfuse/v1.4/src/cal/get_tle/add_tle.pl
+    /usr/local/fusesw/calfuse/current/src/cal/get_tle/add_tle.pl
+    set cfstat=$status
+endif
+
+# Step 3
+if !({$cfstat}) then
+#    /usr/local/fusesw/calfuse/v1.4/src/cal/get_tle/make_cvzramtool.pl
+    /usr/local/fusesw/calfuse/current/src/cal/get_tle/make_cvzramtool.pl
+    set cfstat=$status
+endif
+
+# Step 4
+if !({$cfstat}) then
+#    /usr/local/fusesw/calfuse/v1.4/src/cal/get_tle/make_orbit.pl
+    /usr/local/fusesw/calfuse/current/src/cal/get_tle/make_orbit.pl
+    set cfstat=$status
+endif
+
+exit($cfstat)
+
diff --git a/src/cal/jitter/Makefile.Linux.orig b/src/cal/jitter/Makefile.Linux.orig
new file mode 100644
index 0000000..aafa61d
--- /dev/null
+++ b/src/cal/jitter/Makefile.Linux.orig
@@ -0,0 +1,43 @@
+
+FITSVER=	2.470
+CALFUSEDIR=	${PWD}/../../..
+
+# Symbols for include directories
+FUSEINCLDIR=	-I${CALFUSEDIR}/include
+
+# Symbols used for compiling
+CC=		cc
+OPT=		-g -Wall -DCFORTRAN -Dg77Fortran -Df2cFortran
+CFLAGS=		${OPT} ${FUSEINCLDIR}
+
+# Symbols used for creating shared binaries
+FUSEBINDIR=	${CALFUSEDIR}/bin
+FUSELIBDIR=	-L${CALFUSEDIR}/lib
+FUSELIBS=	-lsla -lcfitsio-${FITSVER} -lcf
+LIBS=		-lc -lm -lnsl -ldl -lgfortran
+LDFLAGS=	-Wl,-R${CALFUSEDIR}/lib
+
+# binaries to be made
+
+BINS=		cf_jitter_diag cf_jitter
+
+all:		${BINS}
+		chmod g+rw ${BINS}
+
+install:	all
+		/bin/cp ${BINS} ${FUSEBINDIR}
+
+clean:
+		/bin/rm -f *.o ${BINS}
+
+distclean:
+		/bin/rm -f *.o ${BINS}
+		cd ../../../bin; /bin/rm -f ${BINS}
+
+cf_jitter_diag:	cf_jitter_diag.c
+		${CC} ${CFLAGS} -o cf_jitter_diag cf_jitter_diag.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_jitter:	cf_jitter.c
+		${CC} ${CFLAGS} -o cf_jitter cf_jitter.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
diff --git a/src/cal/jitter/Makefile.Linux64.orig b/src/cal/jitter/Makefile.Linux64.orig
new file mode 100644
index 0000000..f6cf992
--- /dev/null
+++ b/src/cal/jitter/Makefile.Linux64.orig
@@ -0,0 +1,42 @@
+
+CALFUSEDIR=	${PWD}/../../..
+
+# Symbols for include directories
+FUSEINCLDIR=	-I${CALFUSEDIR}/include
+
+# Symbols used for compiling
+CC=		cc
+OPT=		-g -Wall -DCFORTRAN -Dg77Fortran -Df2cFortran
+CFLAGS=		${OPT} ${FUSEINCLDIR}
+
+# Symbols used for creating shared binaries
+FUSEBINDIR=	${CALFUSEDIR}/bin
+FUSELIBDIR=	-L${CALFUSEDIR}/lib
+FUSELIBS=	-lsla -lcf
+LIBS=		-lc -lm -lnsl -ldl -lgfortran -lcfitsio
+LDFLAGS=	-Wl,-R${CALFUSEDIR}/lib
+
+# binaries to be made
+
+BINS=		cf_jitter_diag cf_jitter
+
+all:		${BINS}
+		chmod g+rw ${BINS}
+
+install:	all
+		/bin/cp ${BINS} ${FUSEBINDIR}
+
+clean:
+		/bin/rm -f *.o ${BINS}
+
+distclean:
+		/bin/rm -f *.o ${BINS}
+		cd ../../../bin; /bin/rm -f ${BINS}
+
+cf_jitter_diag:	cf_jitter_diag.c
+		${CC} ${CFLAGS} -o cf_jitter_diag cf_jitter_diag.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_jitter:	cf_jitter.c
+		${CC} ${CFLAGS} -o cf_jitter cf_jitter.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
diff --git a/src/cal/jitter/Makefile.MacOSX.orig b/src/cal/jitter/Makefile.MacOSX.orig
new file mode 100644
index 0000000..fc408c9
--- /dev/null
+++ b/src/cal/jitter/Makefile.MacOSX.orig
@@ -0,0 +1,46 @@
+
+FITSVER=	2.470
+CALFUSEDIR=	${PWD}/../../..
+MACOSX_DEPLOYMENT_TARGET=       10.2
+
+# Symbols for include directories
+FUSEINCLDIR=	-I${CALFUSEDIR}/include
+
+# Symbols used for compiling
+CC=		cc
+OPT=            -O3 -Wall -DCFORTRAN -Dg77Fortran -Df2cFortran
+CFLAGS=		${OPT} ${FUSEINCLDIR}
+
+# Symbols used for creating shared binaries
+FUSEBINDIR=	${CALFUSEDIR}/bin
+FUSELIBDIR=	-L${CALFUSEDIR}/lib
+FUSELIBS=	-lsla -lcfitsio -lcf
+LIBS=           -lc -lm -ldl -L/sw/lib/ -lgfortran
+
+# Binaries to be made
+
+BINS=		cf_jitter_diag cf_jitter
+
+all:		${BINS}
+		chmod g+rw ${BINS}
+
+install:
+		MACOSX_DEPLOYMENT_TARGET="${MACOSX_DEPLOYMENT_TARGET}"; \
+		export MACOSX_DEPLOYMENT_TARGET; \
+		make all
+		/bin/cp ${BINS} ${FUSEBINDIR}
+
+clean:
+		/bin/rm -f *.o ${BINS}
+
+distclean:
+		/bin/rm -f *.o ${BINS}
+		cd ../../../bin; /bin/rm -f ${BINS}
+
+cf_jitter_diag:	cf_jitter_diag.c
+		${CC} ${CFLAGS} -o cf_jitter_diag cf_jitter_diag.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_jitter:	cf_jitter.c
+		${CC} ${CFLAGS} -o cf_jitter cf_jitter.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
diff --git a/src/cal/jitter/Makefile.Solaris.orig b/src/cal/jitter/Makefile.Solaris.orig
new file mode 100644
index 0000000..f182b16
--- /dev/null
+++ b/src/cal/jitter/Makefile.Solaris.orig
@@ -0,0 +1,50 @@
+
+FITSVER=	2.470
+CALFUSEDIR=	${PWD}/../../..
+
+# Symbols for include directories
+FUSEINCLDIR=	-I${CALFUSEDIR}/include
+
+# Symbols used for compiling
+CC=		cc
+#  Romelfanger's optimizations
+# OPT=		-fast -xO5 -xtarget=ultra2 -xarch=v8plusa
+#
+#  SunWorld's optimizations
+# OPT=		-p -v -xO2 -xdepend -xchip=ultra -xarch=generic
+OPT=		-O -DCFORTRAN -KPIC -DSOLARIS
+CFLAGS=		${OPT} ${FUSEINCLDIR}
+
+# Symbols used for creating shared binaries
+FUSEBINDIR=	${CALFUSEDIR}/bin
+FUSELIBDIR=	-L${CALFUSEDIR}/lib
+LIBDIR=		-L/opt/SUNWspro/lib
+FUSELIBS=	-lsla -lcfitsio-${FITSVER} -lcf
+LIBS=		-lc -lm -lnsl -ldl -lsocket -lsunmath -lM77 -lF77
+LDFLAGS=	-Wl,-R${CALFUSEDIR}/lib
+
+# binaries to be made
+
+BINS=		cf_jitter_diag cf_jitter
+
+all:		${BINS}
+		chmod g+rw ${BINS}
+
+install:	all
+		/bin/cp ${BINS} ${FUSEBINDIR}
+
+clean:
+		/bin/rm -f *.o ${BINS}
+
+distclean:
+		/bin/rm -f *.o ${BINS}
+		cd ../../../bin; /bin/rm -f ${BINS}
+
+cf_jitter_diag:	cf_jitter_diag.c
+		${CC} ${CFLAGS} -o cf_jitter_diag cf_jitter_diag.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_jitter:	cf_jitter.c
+		${CC} ${CFLAGS} -o cf_jitter cf_jitter.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
diff --git a/src/cal/jitter/Makefile.orig.orig b/src/cal/jitter/Makefile.orig.orig
new file mode 100644
index 0000000..f182b16
--- /dev/null
+++ b/src/cal/jitter/Makefile.orig.orig
@@ -0,0 +1,50 @@
+
+FITSVER=	2.470
+CALFUSEDIR=	${PWD}/../../..
+
+# Symbols for include directories
+FUSEINCLDIR=	-I${CALFUSEDIR}/include
+
+# Symbols used for compiling
+CC=		cc
+#  Romelfanger's optimizations
+# OPT=		-fast -xO5 -xtarget=ultra2 -xarch=v8plusa
+#
+#  SunWorld's optimizations
+# OPT=		-p -v -xO2 -xdepend -xchip=ultra -xarch=generic
+OPT=		-O -DCFORTRAN -KPIC -DSOLARIS
+CFLAGS=		${OPT} ${FUSEINCLDIR}
+
+# Symbols used for creating shared binaries
+FUSEBINDIR=	${CALFUSEDIR}/bin
+FUSELIBDIR=	-L${CALFUSEDIR}/lib
+LIBDIR=		-L/opt/SUNWspro/lib
+FUSELIBS=	-lsla -lcfitsio-${FITSVER} -lcf
+LIBS=		-lc -lm -lnsl -ldl -lsocket -lsunmath -lM77 -lF77
+LDFLAGS=	-Wl,-R${CALFUSEDIR}/lib
+
+# binaries to be made
+
+BINS=		cf_jitter_diag cf_jitter
+
+all:		${BINS}
+		chmod g+rw ${BINS}
+
+install:	all
+		/bin/cp ${BINS} ${FUSEBINDIR}
+
+clean:
+		/bin/rm -f *.o ${BINS}
+
+distclean:
+		/bin/rm -f *.o ${BINS}
+		cd ../../../bin; /bin/rm -f ${BINS}
+
+cf_jitter_diag:	cf_jitter_diag.c
+		${CC} ${CFLAGS} -o cf_jitter_diag cf_jitter_diag.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_jitter:	cf_jitter.c
+		${CC} ${CFLAGS} -o cf_jitter cf_jitter.c \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
diff --git a/src/cal/jitter/cf_jitter.c b/src/cal/jitter/cf_jitter.c
new file mode 100644
index 0000000..c1035a6
--- /dev/null
+++ b/src/cal/jitter/cf_jitter.c
@@ -0,0 +1,1239 @@
+/**************************************************************************
+ *           Johns Hopkins University  
+ *          Center for Astrophysical Sciences     
+ *           FUSE
+ *************************************************************************
+ *
+ * synopsis:    cf_jitter input_file output_file     
+ *
+ * Description: Reads a FITS file containing housekeeping data and
+ *              generates a FITS file containing the jitter information 
+ *              for the exposure.
+ *
+ * Arguments: input_file    Input raw FITS housekeeping file for an exposure
+ *                          The header of this file is used as a template
+ *                          for the output file
+ *            output_file   FITS table containing the jitter information 
+ *     
+ * 
+ * Contents of output file: 
+ *   1. Time of sample (in seconds from start)
+ *   2. Shifts dx and dy (in arcsec) of the pointing from a reference position
+ *   3. Tracking quality flag
+ *	5 = dx, dy from known FPDs and q_cmd from telemetry
+ *	4 = good dx, dy from ACS q_est and q_cmd from telemetry
+ *	3 = maybe good dx, dy from ACS q_est
+ *	2 = dx, dy from known FPDs, but q_cmd from FITS header coordinates
+ *	1 = dx, dy from ACS q_est, but q_cmd from FITS header coordinates
+ *	0 = no pointing information (missing telemetry)
+ *     -1 = Pointing is assumed to be bad (never achieved known track)
+ *
+ * Codes to JIT_STAT keyword:
+ *	0	All OK
+ *	1	Problems with jitter data
+ *	2	AT_CMD_ATT flag never set
+ *	3	Commanded ACS quaternions not available
+ *	4	No star field information
+ *	5	Problems with tabulated start time
+ *
+ *                                 
+ * HISTORY:
+ *       01/22/02   v1.0     Robinson  Begin work
+ *       08/14/02   v1.1     Robinson  Populate JIT_STATUS keyword
+ *       09/20/02   v1.11    Robinson  - update FILENAME, FILETYPE keywords
+ *                                     - change EXP_DUR keyword to reflect
+ *                                       total time duration of jitter data
+ *       11/04/02   v1.2     Robinson  Change method in which gaps are filled.
+ *                                     We no longer assume that the data is 
+ *                                     tabulated at regular intervals. Also 
+ *                                     check that tabulated times start BEFORE
+ *                                     the exposure start time
+ *       12/17/02   v1.3     Robinson  Slight change in definitions of TRAKFLG
+ *                                     values.
+ *       01/17/03   v1.4     Robinson  Slight change in calculating summary of
+ *                                     jitter properties
+ *       05/22/03   v1.5     rdr       Change initialization of arrays
+ *       06/10/03   v1.6     rdr       Correct problem in determining ref 
+ *                                     quaternion
+ *       06/23/03   v1.7     rdr       Adjust calculation on some of the
+ *                                     keywords
+ *       06/25/03   v1.8     rdr       Correct fault in setting the SLEWFLG
+ *                                     keyword
+ *       06/27/03   v1.9     rdr       Corrected error in selecting the 
+ *					reference quaternion
+ *       04/05/05   v2.0     wvd       Modify logic for setting TRAKFLG.
+ *					Use only FPD quaternions for dx & dy.
+ *       06/24/05   v2.1     wvd       De-bug code for use in Linux boxes.
+ *       07/06/05   v2.2     wvd       Add JIT_VERS keyword to jitter file.
+ *       11/30/05   v2.3     wvd       Don't add 0.5 to tval and time[i] 
+ *					before converting to type long.
+ *       06/28/06   v2.4     wvd       Add "JITTER KEYWORDS" to file header.
+ *       08/21/06   v2.5     wvd       Always calculate dx and dy.
+ *					For data taken in one-wheel mode,
+ *					jitter is bad if sfknown < 1.
+ *       08/25/06   v2.6     wvd       Three-wheel mode was BEFORE DEC2001,
+ *					not after.  Use qvalid flag to check
+ *					validity of FPD quaternions.
+ *       08/25/06   v2.7     wvd       New tracking flag values:
+ *					5 = FPD, 4 = ACS, 0 = no info
+ *       11/30/06   v3.0     wvd       New code from Tom Ake:
+ *					If telemetry unavailable, use
+ *					target coordinates to generate
+ *					commanded quaternion.
+ *					Modify logic of tracking flags.
+ *       12/19/06   v3.1     wvd       Add flag to force use of target
+ *					coordinates.
+ *       03/29/07   v3.2     wvd       Modify to handle time period when
+ *					ACS telemetry rate was cut in half. 
+ *					Make code generally more robust.
+ *       03/30/07   v3.2.1   wvd       Correct typos in last change.
+ *       04/07/07   v3.3     wvd       Add #include <unistd.h>
+ *       04/13/07   v3.4     wvd       If program fails, set NEXTEND = 0
+ *					in jitter file header.
+ *       05/04/07   v3.5     wvd       Force fourth component of q_meas
+ *					to be positive.
+ *	 08/24/07   v3.6     bot       changed TINT to TLONG for time l.1191.
+ *	 05/30/08   v3.7     wvd       If computing coordinates from file
+ *					header and aperture = RFPT, do not
+ *					add an aperture offset.
+ *
+ **************************************************************************/
+
+#include <unistd.h>
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include <math.h>
+#include "calfuse.h"
+
+#define HSKPVERS_MIN    3.1
+
+static char CF_PRGM_ID[] = "cf_jitter";    
+static char CF_VER_NUM[] = "3.7";  
+
+
+/* Subroutine to normalize a quaternion */
+
+void qnorm(double *quat) {
+
+  double quat3_sq;
+
+  quat3_sq = 1. - quat[0]*quat[0] - quat[1]*quat[1] - quat[2]*quat[2];
+  if (quat3_sq > 0) quat[3] = sqrt(quat3_sq);
+  else quat[3] = 0.;
+
+}
+
+
+/* Subroutine to perform matrix multiplication of two quaternions */
+
+void quatprod(double *tquat, double *quat_ref, double *dquat) {
+
+  int i, j ;
+  double multmat[4][4] ; 
+
+  /* fill in the array with values from the tquat vector */
+  multmat[0][0] =  tquat[3] ;
+  multmat[0][1] = -tquat[2] ;
+  multmat[0][2] =  tquat[1] ;
+  multmat[0][3] = -tquat[0] ;
+  multmat[1][0] =  tquat[2] ;
+  multmat[1][1] =  tquat[3] ;
+  multmat[1][2] = -tquat[0] ;
+  multmat[1][3] = -tquat[1] ;
+  multmat[2][0] = -tquat[1] ; 
+  multmat[2][1] =  tquat[0] ;
+  multmat[2][2] =  tquat[3] ;
+  multmat[2][3] = -tquat[2] ;
+  multmat[3][0] =  tquat[0] ;
+  multmat[3][1] =  tquat[1] ;
+  multmat[3][2] =  tquat[2] ;
+  multmat[3][3] =  tquat[3] ;
+  
+  /* do the matrix multiplication */
+  for (i=0 ; i<4 ; i++) {
+     dquat[i] = 0. ;
+     for (j=0; j<4 ; j++) dquat[i] = dquat[i] + multmat[j][i] * quat_ref[j] ; 
+  }
+
+  if (dquat[3] < 0) for (i=0; i<4 ; i++) dquat[i] = -dquat[i];
+
+}
+
+
+int main(int argc, char *argv[])  
+{
+  fitsfile *infits, *outfits ;
+  int hdutype, tfields, dstatus ;
+  int nvalid, nvalid5, rtime ;
+  int pflg=0 ;
+  int tflg, qvalidt ;
+  int tcolnum, fpdquat1_colnum,  fpdquat2_colnum,  fpdquat3_colnum ;
+  int aquat1_colnum, aquat2_colnum, aquat3_colnum, slew_colnum ;
+  int status, tcol, nextend=0;
+  int dxcol, dycol, trkcol, anynull, intnull=0 ;
+  int qvalid_colnum, cents1_colnum, cents2_colnum, cents3_colnum;
+  int cents4_colnum, cents5_colnum, cents6_colnum, acaflg_colnum ;
+  int acscmd1_colnum, acscmd2_colnum, acscmd3_colnum, sfknown_colnum ;
+  int frow, felem, slewflg, ngs_used, jitlgx, jitlgy ;
+  int *cents1, *cents2, *cents3, *cents4, *cents5, *cents6 , *qvalid ;
+  int *sfknown, *slew;
+  int cents1t=0, cents2t=0, cents3t=0, cents4t=0, cents5t=0, cents6t=0 ;
+  int sfknownt=0 , slewt=0, slewtime=0 ;
+  long i, numq5, numq4, numq3, numq2, numq1, numq0, numqa ; 
+  long  npts, tval, n_invert=0;
+  long *time, qtime=0 ;
+  float tfine, tcoarse, tnull, knowntrk, acstrk, fjitlgx, fjitlgy ;
+  float targtrk ;
+  float ngs1, ngs2, ngs3, ngs4, ngs5, ngs6, gs_used, expdur, exptime ;
+  float dxrms, dyrms, dxave, dyave, dxrms5, dyrms5 ;
+  float *acaflg ;
+  float *dx , *dy ;
+  double *fq1, *fq2,*fq3, *mjd ;
+  double *acscmd1, *acscmd2, *acscmd3, fq1t, fq2t, fq3t  ;
+  double tstrt ;
+  double tquat[4], dquat[4], quat_ref[4] ;
+  double *aq1, *aq2, *aq3, aq1t, aq2t, aq3t ;
+  short *trakflg ;
+  char buffer[FLEN_CARD];
+  char *ttype[] = { "TIME", "DX", "DY", "TRKFLG" } ;
+  char *tform[] = { "1J", "1E", "1E", "1I" } ;
+  char *tunit[] = { "seconds", "arcsec", "arcsec", " "} ;
+  char textname[7]="jitter" ;
+  char blank[]="                                                                                ";
+  char jitter_keywords[]="              JITTER KEYWORDS                                                   ";
+
+  /* New variables (11/30/06) */
+  int maxi, qcmd_prob, trakflg_init, *aqsok, aq_fill ;
+  float targ_ra, targ_dec, targ_roll, x_off, y_off, fpalif1x, fpalif2x ;
+  double cra, sra, cdc, sdc, crl, srl, rad2deg ;
+  double dq_sid[4], aq_old[4], rot[9] ;
+  char aper_id[FLEN_VALUE], fescent[FLEN_VALUE], hskpvers[FLEN_VALUE];
+
+  /* New variables (12/19/06) */
+  int optc;
+  int force_target_coords = FALSE;
+
+  char opts[] = "hfv:";
+  char usage[] =
+    "Usage:\n"
+    "  cf_jitter [-hf] [-v level] housekeeping_file jitter_file\n";
+  char option[] =
+    "Options:\n"
+    "  -h:  this help message\n"
+    "  -f:  force use of target coordinates \n"
+    "  -v:  verbosity level (=1; 0 is silent)\n";
+
+  verbose_level = 1;
+
+  /* Check number of options and arguments */
+  while ((optc = getopt(argc, argv, opts)) != -1) {
+    switch(optc) {
+    case 'h':
+      printf("%s\n%s", usage, option);
+      return 0;
+    case 'f':
+      force_target_coords=TRUE;
+      break;
+    case 'v':
+      verbose_level = atoi(optarg);
+      break;
+    }
+  }
+
+  cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+  if (argc < optind+2) {
+    printf("%s", usage);
+    return 1;
+  }
+
+
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Started execution.");
+
+
+  /* initialize necessary variables */
+     hdutype=0 ;
+     status=0 ;
+     frow=1 ;
+     felem=1 ;
+     anynull=0 ;
+
+  /* Open the input FITS file */
+     cf_verbose(3, "opening the file %s for input",argv[optind]);
+     FITS_open_file(&infits, argv[optind], READONLY, &status); 
+
+  /* Read the starting time and duration from the FITS header */
+     FITS_read_key(infits, TDOUBLE, "EXPSTART", &tstrt, buffer, &status) ;
+     cf_verbose(2, "start time (MJD) = %15.9f",tstrt) ;
+     FITS_read_key(infits, TFLOAT, "EXPTIME", &exptime, buffer, &status) ;
+     cf_verbose(2, "expected exposure duration (sec) = %.0f",exptime) ;
+ 
+  /* Create the output file */
+     FITS_create_file(&outfits, argv[optind+1], &status); 
+
+  /* Copy the header and empty primary image of the input file to 
+     the output */
+     FITS_copy_hdu(infits, outfits, 0, &status) ;
+
+  /* Add "JITTER KEYWORDS" string to header. */
+     FITS_write_record(outfits, blank, &status);
+     FITS_write_record(outfits, jitter_keywords, &status);
+     FITS_write_record(outfits, blank, &status);
+
+  /* Populate the STATUS keyword with 1.
+     Reset keyword if everything goes well. */
+     dstatus = 1 ;
+     FITS_update_key(outfits, TINT, "JIT_STAT", &dstatus, 
+         "Problems with jitter data", &status) ;
+
+  /* Update FILENAME and FILETYPE keywords */
+     FITS_update_key(outfits, TSTRING, "FILENAME",argv[2], NULL, &status) ;
+     FITS_update_key(outfits, TSTRING, "FILETYPE","JITTER", NULL, &status) ;
+
+  /* Insert JIT_VERS keyword */
+     FITS_update_key(outfits, TSTRING, "JIT_VERS", CF_VER_NUM,
+	"cf_jitter version number", &status) ;
+
+  /* Read coordinate information in case we can't determine quat_ref from telemetry */
+     /* Don't bother reading these keywords if the HSKPVERS is too low. */
+     fits_read_key(infits, TSTRING, "HSKPVERS", hskpvers, NULL, &status);
+     if (status != 0 || atof(hskpvers) < HSKPVERS_MIN) {
+        status = 0;
+        cf_verbose(1, "Housekeeping file format is out of date.");
+     }
+     else {
+	FITS_read_key(infits, TFLOAT, "RA_TARG", &targ_ra, buffer, &status) ;
+	FITS_read_key(infits, TFLOAT, "DEC_TARG", &targ_dec, buffer, &status) ;
+	FITS_read_key(infits, TFLOAT, "APER_PA", &targ_roll, buffer, &status) ;
+	FITS_read_key(infits, TSTRING, "APERTURE", &aper_id, buffer, &status) ;
+	FITS_read_key(infits, TFLOAT, "FPALIF1X", &fpalif1x, buffer, &status) ;
+	FITS_read_key(infits, TFLOAT, "FPALIF2X", &fpalif2x, buffer, &status) ;
+	FITS_read_key(infits, TSTRING, "FESCENT", &fescent, buffer, &status) ;
+     }
+
+  /* move to the first extension, which contains the table */
+     FITS_movabs_hdu(infits, 2, &hdutype, &status) ;
+
+  /* determine the number of times which have been tabulated */
+     FITS_read_key(infits, TLONG, "NAXIS2", &npts, NULL, &status) ;
+     cf_verbose(2, "number of samples in the table = %ld", npts) ;
+
+  /*   set up arrays to contain the data to be read from the table  */
+           mjd = (double *) cf_calloc(npts, sizeof(double)) ;
+           qvalid = (int *) cf_calloc(npts, sizeof(int)) ;
+           fq1 = (double *) cf_calloc(npts, sizeof(double) ) ;
+           fq2 = (double *) cf_calloc(npts, sizeof(double) ) ;
+           fq3 = (double *) cf_calloc(npts, sizeof(double) ) ;
+           aq1 = (double *) cf_calloc(npts, sizeof(double) ) ;
+           aq2 = (double *) cf_calloc(npts, sizeof(double) ) ;
+           aq3 = (double *) cf_calloc(npts, sizeof(double)) ; 
+           acaflg = (float *) cf_calloc(npts, sizeof(float)) ;
+           acscmd1 = (double *) cf_calloc(npts, sizeof(double)) ; 
+           acscmd2 = (double *) cf_calloc(npts, sizeof(double) ) ; 
+           acscmd3 = (double *) cf_calloc(npts, sizeof(double) ) ; 
+           cents1 = (int *) cf_calloc(npts, sizeof(int)) ;
+           cents2 = (int *) cf_calloc(npts, sizeof(int) ) ;
+           cents3 = (int *) cf_calloc(npts, sizeof(int) ) ;
+           cents4 = (int *) cf_calloc(npts, sizeof(int) ) ;
+           cents5 = (int *) cf_calloc(npts, sizeof(int) ) ;
+           cents6 = (int *) cf_calloc(npts, sizeof(int) ) ;
+           sfknown = (int *) cf_calloc(npts, sizeof(int) ) ;
+           slew = (int *) cf_calloc(npts, sizeof(int) ) ;
+
+  /* read the data */
+	   FITS_get_colnum(infits, CASEINSEN, "MJD", &tcolnum, &status) ;
+	   FITS_read_col(infits, TDOUBLE, tcolnum, frow, felem, npts, &intnull,
+			   mjd, &anynull, &status) ;
+
+	   FITS_get_colnum(infits, CASEINSEN, "I_FPD_MEAS_Q_VALID",
+		&qvalid_colnum, &status) ;
+	   FITS_read_col(infits, TINT, qvalid_colnum, frow, felem, npts,
+		&intnull, qvalid, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "I_FPD_Q_ECI2BDY_1",
+		&fpdquat1_colnum, &status) ;
+	   FITS_read_col(infits, TDOUBLE, fpdquat1_colnum , frow, felem, npts,
+		&intnull, fq1, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "I_FPD_Q_ECI2BDY_2",
+		&fpdquat2_colnum, &status) ;
+	   FITS_read_col(infits, TDOUBLE, fpdquat2_colnum , frow, felem, npts,
+		&intnull, fq2, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "I_FPD_Q_ECI2BDY_3",
+		&fpdquat3_colnum, &status) ;
+	   FITS_read_col(infits, TDOUBLE, fpdquat3_colnum , frow, felem, npts,
+		&intnull, fq3, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "AATTQECI2BDY_1",
+		&aquat1_colnum, &status) ;
+	   FITS_read_col(infits, TDOUBLE, aquat1_colnum , frow, felem, npts,
+		&intnull, aq1, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "AATTQECI2BDY_2",
+		&aquat2_colnum, &status) ;
+	   FITS_read_col(infits, TDOUBLE, aquat2_colnum, frow, felem, npts,
+		&intnull, aq2, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "AATTQECI2BDY_3",
+		&aquat3_colnum, &status) ;
+	   FITS_read_col(infits, TDOUBLE, aquat3_colnum, frow, felem, npts,
+		&intnull, aq3, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "I_AT_CMD_ATT", &acaflg_colnum,
+		&status) ;
+	   FITS_read_col(infits, TFLOAT, acaflg_colnum, frow, felem, npts,
+		&intnull, acaflg, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "AQECI2BDYCMD_1",
+		&acscmd1_colnum, &status) ;
+	   FITS_read_col(infits, TDOUBLE, acscmd1_colnum, frow, felem, npts,
+		&intnull, acscmd1, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "AQECI2BDYCMD_2",
+		&acscmd2_colnum, &status) ;
+	   FITS_read_col(infits, TDOUBLE, acscmd2_colnum, frow, felem, npts,
+		&intnull, acscmd2, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "AQECI2BDYCMD_3",
+		&acscmd3_colnum, &status) ;
+	   FITS_read_col(infits, TDOUBLE, acscmd3_colnum, frow, felem, npts,
+		&intnull, acscmd3, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "CENTROID1_STATUS",
+		&cents1_colnum, &status) ;
+	   FITS_read_col(infits, TINT, cents1_colnum, frow, felem, npts,
+		&intnull, cents1, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "CENTROID2_STATUS",
+		&cents2_colnum, &status) ;
+	   FITS_read_col(infits, TINT, cents2_colnum, frow, felem, npts,
+		&intnull, cents2, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "CENTROID3_STATUS",
+		&cents3_colnum, &status) ;
+	   FITS_read_col(infits, TINT, cents3_colnum, frow, felem, npts,
+		&intnull, cents3, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "CENTROID4_STATUS",
+		&cents4_colnum, &status) ;
+	   FITS_read_col(infits, TINT, cents4_colnum, frow, felem, npts,
+		&intnull, cents4, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "CENTROID5_STATUS",
+		&cents5_colnum, &status) ;
+	   FITS_read_col(infits, TINT, cents5_colnum, frow, felem, npts,
+		&intnull, cents5, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "CENTROID6_STATUS",
+		&cents6_colnum, &status) ;
+	   FITS_read_col(infits, TINT, cents6_colnum, frow, felem, npts,
+		&intnull, cents6, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "I_FPD_STARFLD_KNWN",
+		&sfknown_colnum, &status) ;
+	   FITS_read_col(infits, TINT, sfknown_colnum, frow, felem, npts,
+		&intnull, sfknown, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "I_FPD_NEW_CMD_Q", &slew_colnum,
+                &status) ;
+	   FITS_read_col(infits, TINT, slew_colnum, frow, felem, npts,
+		&intnull, slew, &anynull, &status) ;
+
+  /* close the input file */
+      FITS_close_file(infits, &status) ;
+
+  /* Check that the tabulated times start BEFORE the start of the
+	exposure.  Otherwise there may be missing data or an error
+	in the tabulated start time. */
+     tval=cf_nlong(floor((mjd[0]-tstrt) * 86400.));
+     if (tval > 0) {
+        cf_if_warning("Possible missing data or error in the start time.  "
+        "The first tabulated time is %ld seconds from obs start.", tval) ;
+	/* update JIT_STAT keyword */
+        dstatus = 5 ;
+        FITS_update_key(outfits, TINT, "JIT_STAT", &dstatus, 
+            "Problems with tab start time", &status) ;
+     }      
+
+  /* fill in the gaps in the data set 
+
+     - ACS quaternions are generally tabulated every other second
+     - FPD quaternions can be every second or every other second
+     - ACS flags (acaflg) - tabulated every 16 seconds
+
+     NOTE:  there can be irregularities in the spacing.  Thus, save the last
+     tabulated value and use this to fill in missing data for a given time. */
+
+  /* Array to track whether we can trust ACS q_meas for dx,dy computation */
+     aqsok = (int *) cf_calloc(npts, sizeof(int) ) ;
+
+  /* ACS quaternions. Fill up to aq_fill missing values with the last good one.
+     Set aqsok[i] to -1 if we leave a missing value missing.*/
+
+     /* aq_fill = 2 ; replace up to 2 consecutive missing values */
+
+     /* Fix for 2007:072:18:02 - 085:13:38, when ACS telemetry rate
+	was cut in half (MOCR 1902). */
+     aq_fill = 4;
+     aq1t = 0. ;
+     aq2t = 0. ;
+     aq3t = 0. ;
+     tflg = -1 ;
+
+     /* If the first ACS aq_fill values are missing,
+	use the one aq_fill steps later. */
+     for (i = aq_fill; i > 0; i--) if (aq1[i] > -1 && aq2[i] > -1) {
+	aq1t = aq1[i];
+	aq2t = aq2[i];
+	aq3t = aq3[i];
+	tflg = aq_fill;
+     }
+
+     for (i=0 ; i<npts ; i++) {
+       aqsok[i] = -1 ; /* assume q_meas is missing */
+       if ( aq1[i] > -1 && aq2[i] > -1 ) {
+         aqsok[i] = 0 ;
+         aq1t = aq1[i] ;
+         aq2t = aq2[i] ;
+         aq3t = aq3[i] ;
+         tflg = aq_fill ; /* fill factor */
+       } 
+       else if (tflg > 0) {
+         aqsok[i] = 0 ;
+         aq1[i] = aq1t ;
+         aq2[i] = aq2t ;
+         aq3[i] = aq3t ;
+         tflg-- ;
+       }
+     }    
+
+      /* FPD quaternions and qvalid flags 
+         Only update the one following a good quaternion. If there is
+	 another one with no quaternion after that, do not update it. */
+
+     fq1t = 0. ;
+     fq2t = 0. ;
+     fq3t = 0. ;
+     qvalidt = 0 ;
+     tflg = -1 ;
+      for (i=0 ; i<npts ; i++) {
+        if ( (fabs(fq1[i]) > 0.) && (fabs(fq2[i]) > 0.) ){
+
+   /* The ACS has a strict convention that the 4th component of the
+   quaternion be positive. But if it is close to zero, the IDS FPD
+   component may be negative. The housekeeping file only has components
+   1-3. As a best estimate, we will choose the sign of the FPD 4th
+   component so that the quaternion is closest in pointing to the ACS
+   quaternion. Only known tracking FPDs need to be corrected. */
+
+
+if (aq1[i] > -1 && aq2[i] > -1 && sfknown[i] == 1) {
+  quat_ref[0] = -aq1[i] ;
+  quat_ref[1] = -aq2[i] ;
+  quat_ref[2] = -aq3[i] ;
+  qnorm(quat_ref) ;
+  if (quat_ref[3] < 0.03) {
+    tquat[0] = fq1[i] ;
+    tquat[1] = fq2[i] ;
+    tquat[2] = fq3[i] ;
+    qnorm(tquat) ;
+    quatprod(tquat,quat_ref,dquat) ;
+    fq1t = dquat[0]*dquat[0] + dquat[1]*dquat[1] ;
+    tquat[3] = -tquat[3] ;
+    quatprod(tquat,quat_ref,dquat) ;
+    if (dquat[0]*dquat[0]+dquat[1]*dquat[1] < fq1t) {
+      fq1[i] = -fq1[i] ;
+      fq2[i] = -fq2[i] ;
+      fq3[i] = -fq3[i] ; 
+      n_invert++;
+    }
+  }
+}
+
+	  fq1t=fq1[i] ;
+	  fq2t=fq2[i] ;
+	  fq3t=fq3[i] ; 
+          qvalidt = qvalid[i] ;
+          cents1t = cents1[i] ;
+          cents2t = cents2[i] ;
+          cents3t = cents3[i] ;
+          cents4t = cents4[i] ;
+          cents5t = cents5[i] ;
+          cents6t = cents6[i] ;
+          sfknownt = sfknown[i] ;
+          slewt = slew[i] ;
+          tflg = 1 ; }
+        else if (tflg > 0) {
+          fq1[i] = fq1t ;
+          fq2[i] = fq2t ;
+          fq3[i] = fq3t ;
+          qvalid[i] = qvalidt ;
+          cents1[i] = cents1t ; 
+          cents2[i] = cents2t ; 
+          cents3[i] = cents3t ; 
+          cents4[i] = cents4t ; 
+          cents5[i] = cents5t ; 
+          cents6[i] = cents6t ; 
+          sfknown[i] = sfknownt ;
+          slew[i] = slewt ;
+          tflg = -1 ; }
+	}
+if (n_invert > 0) cf_verbose(1, "Number of known FPD quaternions inverted: %ld", n_invert);
+
+
+       /* ACAFLG flag */
+
+       tflg = -10 ;          
+
+       /* Assume that the first real ACA value is the one to start with. */
+	for (i = 0; i < npts-1; i++) if (acaflg[i] > -1) {
+	    tflg = acaflg[i];
+	    break;
+	}
+
+       for (i=0 ; i<npts-1 ; i++) {
+         if (acaflg[i] > -1) tflg = acaflg[i] ;
+         else acaflg[i] = tflg ;
+        } 
+		       
+
+ /********** derive the final quats arrays and the tracking flags *******/
+
+  /*    set up arrays to contain the data */
+         time = (long *) cf_calloc(npts, sizeof(long) ) ;
+	 trakflg = (short *) cf_calloc(npts, sizeof(short) ) ; 
+         dx = (float *) cf_calloc(npts, sizeof(float) ) ;
+         dy = (float *) cf_calloc(npts, sizeof(float) ) ;
+
+ /* fill in the time array with times (in seconds) from the start
+	of the exposure */
+	 for (i=0 ; i<npts ; i++) 
+           time[i] = cf_nlong(floor((mjd[i]-tstrt) * 86400.));
+
+
+   /* Determine the reference quat by looking at the commanded ACS
+   quaternion (in arrays acscmd1, acscmd2 and acscmd3) when they have
+   converged to the fpd commanded quaternion - i.e. when the AT_CMD_ATT
+   flag is 1 (held in the array acaflg).  Make sure that the time of
+   convergence is AFTER the start of the exposure and that the star field
+   is known (i.e. sfknown = 1).  Also, because of the 16s sample time of
+   the ascflg array, require that the condition exists for at least 30
+   consecutive seconds before accepting the quaternions.  qtime = time at
+   which the quaternions were found. This is the earliest time in the
+   exposure for which reliable positions are available. */
+
+    rtime=0 ;
+    qtime = 0;
+    for (i=0; i<npts; i++) {
+	if (acaflg[i] == 1 && time[i] > 0 && sfknown[i] == 1) {
+	    rtime++ ;
+	    if (rtime == 1) qtime=time[i] ;
+	    if (rtime > 30 && acscmd1[i] > -1 &&
+	    	acscmd2[i] > -1 && acscmd3[i] > -1 ) {
+		quat_ref[0]=acscmd1[i] ;
+		quat_ref[1]=acscmd2[i] ;
+		quat_ref[2]=acscmd3[i] ;
+		qnorm(quat_ref);
+		qcmd_prob = 0;
+		break;
+	    }
+	}
+	else rtime=0 ; 
+    }
+
+     /* If rtime <= 30, then the flag was never set
+	and the reference quaternion not determined */
+    if (rtime <= 30 || force_target_coords) {
+
+	/* If user has requested target coordinates... */
+	if (force_target_coords) {
+	    cf_verbose(1, "Computing reference quaternion from target coordinates.");
+            dstatus = 2 ;
+            FITS_update_key(outfits, TINT, "JIT_STAT", &dstatus, 
+               "User requests use of target coordinates", &status) ;
+	}
+	/* If something is wrong... */
+	else {
+	 cf_verbose(1, "Problem determining the reference quaternions") ;
+         pflg = 0 ;
+	 for (i=0 ; i<npts; i++) if (acaflg[i] == 1) pflg=1 ;
+	 if (pflg == 0) {
+               cf_verbose(1, " AT_CMD_ATT flag was never set.") ;
+         	/* update JIT_STAT keyword */
+               dstatus = 2 ;
+               FITS_update_key(outfits, TINT, "JIT_STAT", &dstatus, 
+               "AT_CMD_ATT flag never set", &status) ;
+	 }
+
+         pflg = 0 ;
+	 for (i=0 ; i<npts; i++) if (acscmd1[i] > -1 &&
+                acscmd2[i] > -1 && acscmd3[i] > -1) pflg++ ;
+	 if (pflg <= 30) {
+               cf_verbose(1, " Commanded ACS quaternions not available.") ;
+         	/* update JIT_STAT keyword */
+               dstatus = 3 ;
+               FITS_update_key(outfits, TINT, "JIT_STAT", &dstatus, 
+               "Commanded ACS quaternions not available", &status) ;
+	 }
+
+         pflg = 0 ;
+	 for (i=0 ; i<npts; i++) if (sfknown[i] == 1) pflg++;
+	    if (pflg <= 30)  {
+                cf_verbose(1, " NO STAR FIELD INFORMATION") ;
+   	        /* update JIT_STAT keyword */
+                dstatus = 4 ;
+                FITS_update_key(outfits, TINT, "JIT_STAT", &dstatus, 
+               "No star field information", &status) ;
+	    }
+	}
+
+     /* If we lack a reference quaternion and can't calculate one from
+	information in the housekeeping file header, set the JIT_STAT
+	keyword to 1, close the jitter file, and return. */
+     if (atof(hskpvers) < HSKPVERS_MIN) {
+	dstatus = 1 ;
+	FITS_update_key(outfits, TINT, "NEXTEND",  &nextend, NULL, &status);
+        FITS_update_key(outfits, TINT, "JIT_STAT", &dstatus, NULL, &status);
+	FITS_close_file(outfits, &status);
+	cf_verbose(1, "Unable to calculate reference quaternion from target coordinates.");
+	return 1;
+     }
+
+     /* Compute quat_ref from the target coordinates instead */
+     qcmd_prob = -3 ;
+     rad2deg = 57.2957951 ;
+     cra = cos(targ_ra/rad2deg) ;
+     sra = sin(targ_ra/rad2deg) ;
+     cdc = cos(targ_dec/rad2deg) ;
+     sdc = sin(targ_dec/rad2deg) ;
+     targ_roll=270.-targ_roll ;
+     crl = cos(targ_roll/rad2deg) ;
+     srl = sin(targ_roll/rad2deg) ;
+     
+     /* The FUSE rotation matrix */
+     rot[0] = -srl*sra + crl*sdc*cra ; 
+     rot[1] = -crl*sra - srl*sdc*cra ; 
+     rot[2] =  cdc*cra ;
+     rot[3] =  srl*cra + crl*sdc*sra ;
+     rot[4] =  crl*cra - srl*sdc*sra ;
+     rot[5] =  cdc*sra ;
+     rot[6] = -crl*cdc ;
+     rot[7] =  srl*cdc ;
+     rot[8] =  sdc ;
+     
+     /*  quat_ref for the target, before updating for aperture and FPA position */
+     
+     quat_ref[0] = 0.5 * sqrt(1. + rot[0] + rot[4] + rot[8]) ;
+     quat_ref[1] = 0.5 * sqrt(1. + rot[0] - rot[4] - rot[8]) ;
+     quat_ref[2] = 0.5 * sqrt(1. + rot[4] - rot[0] - rot[8]) ;
+     quat_ref[3] = 0.5 * sqrt(1. + rot[8] - rot[0] - rot[4]) ;
+     
+     maxi=0 ; /* going to choose the largest divisor */
+     for (i=1 ; i<4 ; i++) if (quat_ref[i] > quat_ref[maxi]) maxi=i;
+     switch (maxi) {
+       case 0:  quat_ref[3] = quat_ref[0] ;
+                quat_ref[0] = (rot[7] - rot[5])/quat_ref[3]/4. ;
+                quat_ref[1] = (rot[2] - rot[6])/quat_ref[3]/4. ;
+                quat_ref[2] = (rot[3] - rot[1])/quat_ref[3]/4. ;
+                break ;
+       case 1:  quat_ref[0] = quat_ref[1] ;
+                quat_ref[3] = (rot[7] - rot[5])/quat_ref[0]/4. ;
+                if (quat_ref[3] < 0) {
+                  quat_ref[0] = -quat_ref[0] ;
+                  quat_ref[3] = -quat_ref[3] ;
+                } 
+                quat_ref[1] = (rot[1] + rot[3])/quat_ref[0]/4. ;
+                quat_ref[2] = (rot[2] + rot[6])/quat_ref[0]/4. ;
+                 break ; 
+       case 2:  quat_ref[1] = quat_ref[2] ;
+                quat_ref[3] = (rot[2] - rot[6])/quat_ref[1]/4. ;
+                if (quat_ref[3] < 0) {
+                  quat_ref[1] = -quat_ref[1] ; 
+                  quat_ref[3] = -quat_ref[3] ;
+                }
+                quat_ref[0] = (rot[1] + rot[3])/quat_ref[1]/4. ;
+                quat_ref[2] = (rot[5] + rot[7])/quat_ref[1]/4. ;
+                break ;
+       default: quat_ref[2] = quat_ref[3] ;
+                quat_ref[3]=(rot[3] - rot[1])/quat_ref[2]/4. ;
+                if (quat_ref[3] < 0) {
+                  quat_ref[2] = -quat_ref[2] ;
+                  quat_ref[3] = -quat_ref[3] ;
+                }
+                quat_ref[0] = (rot[6] + rot[2])/quat_ref[2]/4. ;
+                quat_ref[1] = (rot[5] + rot[7])/quat_ref[2]/4. ;
+     } 
+     
+     /* Compute x_offset due to FPA shift, first in microns, then in arcsec */
+     if (!strncmp(fescent, "FES A", 5)) x_off = 117. - fpalif1x;
+     else x_off = 175. - fpalif2x ;
+     x_off = x_off/10.88*cos(30.5/rad2deg) ;
+     y_off = 0. ;
+     
+     /* Now add in the aperture offset (in arcsec) */
+     if (strncmp(aper_id, "RFPT", 4)) {		/* If not RFPT, assume LWRS. */
+        x_off = x_off + 55.18 ;
+        y_off = 118.07 ;
+        if (!strncmp(aper_id, "MDRS", 4)) y_off = -90.18;
+        else if (!strncmp(aper_id, "HIRS", 4)) y_off = 10.27;
+        if (tstrt < 51708.9167) {
+          y_off = 112.07 ;
+          if (!strncmp(aper_id, "MDRS", 4)) y_off = -97.18;
+          else if (!strncmp(aper_id, "HIRS", 4)) y_off = 2.27;
+        } else if (tstrt < 51796.3000) {
+          y_off = 116.07 ;
+          if (!strncmp(aper_id, "MDRS", 4)) y_off = -93.18;
+          else if (!strncmp(aper_id, "HIRS", 4)) y_off = 6.27;
+        }
+     }
+     
+     /* Set up a slew for the offsets and update quat_ref to be the expected q_cmd */
+     dquat[0] = -y_off/2./206264.81; 
+     dquat[1] =  x_off/2./206264.81; 
+     dquat[2] = 0.; 
+     qnorm(dquat) ;
+     quatprod(dquat,quat_ref,tquat); 
+     for (i=0 ; i<4 ; i++) quat_ref[i] = tquat[i]; 
+
+    }
+
+    if (qcmd_prob < 0) {
+       FITS_update_key(outfits,TSTRING,"QREF_SRC","COORDINATES","Source of reference quaternion", &status) ;
+       cf_verbose(1, "Reference quat values derived from FITS header coordinates.");
+       cf_verbose(1, "Used x_off = %7.2f, y_off = %7.2f arcseconds.", x_off, y_off);
+    }
+    else {
+       FITS_update_key(outfits,TSTRING,"QREF_SRC","TELEMETRY","Source of reference quaternion", &status) ;
+       cf_verbose(1, "Reference quat values represent ACS commanded position.");
+    }
+
+    for (i=0; i<4 ; i++) cf_verbose(2, "for i=%ld, quat=%18.15f",i,quat_ref[i]) ;              
+    FITS_update_key(outfits,TDOUBLE,"QREF_0",quat_ref,"Reference quaternion", &status) ;
+    FITS_update_key(outfits,TDOUBLE,"QREF_1",quat_ref+1, NULL, &status) ;
+    FITS_update_key(outfits,TDOUBLE,"QREF_2",quat_ref+2, NULL, &status) ;
+    FITS_update_key(outfits,TDOUBLE,"QREF_3",quat_ref+3, NULL, &status) ;
+
+      /* Determine the shift in the quaternions and derive the changes
+	 in x and y that they represent:
+         DX (from q2 values : q2=dx/2) and DY (from q1 values : q1=-dy/2)
+         in arcseconds - the conversion factor used is the number of arcsec
+         per radian * 2 */
+
+/* Determine initial trakflg. If we had IDS telemetry but never reached known
+track, we want to start with trakflg_init=-1. If telemetry missing, temporarily
+set trakflg_init to -2. */
+
+trakflg_init=0 ; tflg=0 ;
+for (i=0 ; i<npts ; i++){
+  if (sfknown[i] == 1) {
+    tflg=1 ;
+    break ; 
+  }
+} 
+if (tflg == 0) { /* known track flag never set */
+  trakflg_init = -1 ;
+  for (i=0 ; i<npts ; i++) {
+    if (acaflg[i] > -1) {  /* use ACA flag to say if IDS tlm missing */
+      tflg = 1 ;
+      break ;
+    }
+  }  
+  if (tflg == 0) trakflg_init = -2;   /* ktrk flag never=1 because IDS tlm missing */
+}
+
+/* set up aqsok array to flag whether ACS q_meas is a good estimate of pointing
+ -1 = ACS q_meas missing (from filling in the gaps earlier)
+  0 = don't trust it (e.g., in unknown track)
+  1 = trust it (had been in known track, so good for a while)
+  2 = maybe ok (started expo with IDS idled (or missing FPDs) and ACA=1)
+  3 = we corrected ACS q_meas during unknown track period from the 1st known q 
+*/
+
+/* First, if we got to known track at some point, correct ACS q's during unknown
+track that eventually got to known track (aqsok=3) by going backward in time.
+Look for transition from known to unknown and use the delta in ACS q's as an
+estimate of the dq from starID (dq_sid). Apply this to ACS q's while in unknown
+track. Because we filled missing ACS q's with previous ones, we have to skip by
+aq_fill values to make sure we have new q's when calculating dq_sid. */
+
+if (trakflg_init > -1) {
+  tflg = 0  ; /* used to indicate we have a dq_sid to apply */
+  for (i=npts-1 ; i>aq_fill ; i--) {
+    if (sfknown[i] == 1 && sfknown[i-aq_fill-1] == 1) {
+      tflg = 0 ; /* don't use previous dq_sid anymore */
+    }
+    else if (sfknown[i] == 1 && 	/* Now in known track */
+	(sfknown[i-aq_fill-1] == 0 && qvalid[i-aq_fill-1] == 1) &&  /* Were in unknown track */
+	tflg == 0 &&		/* We need to compute a quaternion. */
+        aqsok[i] > -1 && aqsok[i-aq_fill-1] > -1) {    /* calculate dq_sid */
+      tquat[0] = fq1[i] ;
+      tquat[1] = fq2[i] ;
+      tquat[2] = fq3[i] ;
+      qnorm(tquat) ;
+      aq_old[0] = -aq1[i-aq_fill-1] ;
+      aq_old[1] = -aq2[i-aq_fill-1] ;
+      aq_old[2] = -aq3[i-aq_fill-1] ;
+      qnorm(aq_old) ;
+      quatprod(tquat,aq_old,dq_sid) ;
+      tflg=1 ;
+    }
+    else if (sfknown[i] == 0 && tflg == 1 && aqsok[i] > -1) { /* correct ACS q_meas */
+      aq_old[0]=aq1[i] ;
+      aq_old[1]=aq2[i] ;
+      aq_old[2]=aq3[i] ;
+      qnorm(aq_old) ;
+      quatprod(dq_sid,aq_old,tquat) ;
+      aq1[i]=tquat[0] ;
+      aq2[i]=tquat[1] ;
+      aq3[i]=tquat[2] ;
+      aqsok[i]=3 ; /* ACS q_meas now believable */
+    }
+    else if (sfknown[i] == -1) {
+        tflg = 0 ; /* IDS idled or missing tlm */
+    }
+  }
+}               /* end trakflg > -1 */
+
+/* If IDS telemetry missing, start with trakflg=0, else don't trust ACS q's yet (trkflg = -1). */
+if (trakflg_init == -2) trakflg_init = 0; 
+else trakflg_init = -1;
+
+/* If we start in corrected unknown track, initialize trakflg to 4 or 1, else trakflg_init = -1. */
+if (aqsok[0] == 3) trakflg_init = 4 + qcmd_prob;
+
+/* If we're already in known track at the start, trakflg_init = 5 or 2. */
+if (sfknown[0] == 1) trakflg_init = 5 + qcmd_prob;
+
+/* Now assign aqsok 1-2 cases, trakflg, and compute dqs. First we need to 
+make quat_ref its inverse */
+quat_ref[3] = -quat_ref[3] ;
+
+/* if start with no FPDs and ACA=1, there may have been a previous exposure
+that lost track at the end. Set first aqsok to maybe ok. */
+if (sfknown[0] == -1 && acaflg[0] == 1 && aqsok[0] > -1) {
+	aqsok[0] = 2;
+	trakflg_init = 3;
+}
+
+trakflg[0] = trakflg_init ;
+for (i=1 ; i<npts; i++) {
+  trakflg[i] = trakflg_init ;
+  if (sfknown[i] == 1) {
+    aqsok[i] = 1 ; /* show we can start trusting the ACS q's if we lose stars later */
+    trakflg[i] = 5 + qcmd_prob ; /* will be 5 or 2 */
+    tquat[0]=fq1[i] ;
+    tquat[1]=fq2[i] ; 
+    tquat[2]=fq3[i] ;
+    qnorm(tquat) ; 
+    trakflg_init = 0 ;
+  } 
+  else if (aqsok[i-1] > 0 || aqsok[i] > 0) { /* 1,2,3 = already had been trusting the ACS q's */
+     /* continue to trust them under the following conditions:
+        - we haven't done a slew and we started with q's maybe ok or corrected 
+        - IDS is idled or we have missing FPDs
+     */
+     if ( (aqsok[i-1] == 2 && acaflg[i] == 1) || (qvalid[i] < 1) || (aqsok[i] == 3) ) {
+	/* continue to trust them */
+      if (aqsok[i] != 3) aqsok[i] = aqsok[i-1]; 
+      if (aq1[i] == -1 && aq2[i] == -1) trakflg[i] = 0;
+      else if (aqsok[i] == 2) trakflg[i] = 3 ;
+      else trakflg[i] = 4 + qcmd_prob ;		/* aqsok=1,3 */
+
+      tquat[0]=aq1[i] ;
+      tquat[1]=aq2[i] ;
+      tquat[2]=aq3[i] ;
+      qnorm(tquat) ;
+      trakflg_init = 0 ;
+    } 
+    else if (qvalid[i] == 1) {
+	trakflg[i] = -1 ;
+	trakflg_init = -1;
+    }
+  }
+
+  if (trakflg[i] > 0 && tquat[0] > -1 && tquat[1] > -1) { 
+    quatprod(tquat,quat_ref,dquat) ;
+    dx[i] = (float) dquat[1]*206264.81*2. ;
+    dy[i] = (float) -dquat[0]*206264.81*2. ;
+  } 
+  else {
+    dx[i] = 0. ; dy[i] = 0. ;
+  }
+}
+
+
+/*Provide keywords in the top-level header which describe the exposure */
+
+   /* determine the time span in the jitter file (in seconds) and set EXP_DUR to
+        this value  */
+       expdur = (float) (time[npts-1] - time[0]) + 1. ;
+       FITS_update_key(outfits, TFLOAT, "EXP_DUR", &expdur, 
+         "[s] duration of jitter data", &status) ;
+
+       /* check for a short exposure and reset exptime if necessary */
+       if (time[npts-1] < exptime) {
+	 exptime = time[npts-1] ;
+         cf_verbose(1, "Short exposure. Reset exptime to %.0f",exptime) ;
+       }
+
+	 /* determine the statistics of the guiding */
+         numq5=0 ;
+         numq4=0 ;
+         numq3=0 ;
+         numq2=0 ;
+         numq1=0 ;
+         numq0=0 ;
+         numqa=0 ;
+
+	 for (i=0; i<npts ; i++) {
+	   cf_verbose(4, "at i=%5d, trakflg=%2d, qvalid=%2d, time=%4ld",
+	      i,trakflg[i], qvalid[i], time[i] );
+           if(trakflg[i] == 5 && qvalid[i] > 0 && time[i] > 0 &&
+		time[i] <= exptime) 
+                   numq5++ ;
+           if(trakflg[i] == 4 && time[i] > 0 && time[i] <= exptime) numq4++ ;
+           if(trakflg[i] == 3 && time[i] > 0 && time[i] <= exptime) numq3++ ;
+           if(trakflg[i] == 2 && time[i] > 0 && time[i] <= exptime) numq2++ ;
+           if(trakflg[i] == 1 && time[i] > 0 && time[i] <= exptime) numq1++ ;
+           if(trakflg[i] == 0 && time[i] > 0 && time[i] <= exptime) numq0++ ;
+           if(trakflg[i] ==-1 && time[i] > 0 && time[i] <= exptime) numqa++ ; }
+
+         cf_verbose(2, "duration of jitter data = %.0f, exposure time = %.0f",
+		expdur, exptime) ;
+	 cf_verbose(2, "number of samples with trkflg =  5: %ld", numq5);
+	 cf_verbose(2, "number of samples with trkflg =  4: %ld", numq4);
+	 cf_verbose(2, "number of samples with trkflg =  3: %ld", numq3);
+	 cf_verbose(2, "number of samples with trkflg =  2: %ld", numq2);
+	 cf_verbose(2, "number of samples with trkflg =  1: %ld", numq1);
+	 cf_verbose(2, "number of samples with trkflg =  0: %ld", numq0);
+	 cf_verbose(2, "number of samples with trkflg = -1: %ld", numqa);
+
+
+       /* tfine, tcoarse and tnull are the fraction of the total exposure
+          when the exposure is in fine track, coarse track and no track */
+       tfine = (float) (numq2+numq5) /  exptime ;
+       tcoarse = (float) (numq1+numq3+numq4) /  exptime ;
+       tnull = (float) (numqa+numq0) /  exptime ;
+       FITS_update_key(outfits, TFLOAT, "KNOWNTRK", &tfine, 
+           "fraction of exp in known track", &status) ;
+       FITS_update_key(outfits, TFLOAT, "ACSTRK", &tcoarse, 
+           "fraction of exp in ACS track", &status) ;
+       FITS_update_key(outfits, TFLOAT, "NOGDEINF", &tnull, 
+           "fraction of exp with no guiding info", &status) ;
+
+       /* determine the properties of the guide stars */
+       ngs1=0. ;
+       ngs2=0. ;
+       ngs3=0. ;
+       ngs4=0. ;
+       ngs5=0. ;
+       ngs6=0. ;
+       for (i=0; i<npts ; i++) {
+         if (cents1[i] == 2 && sfknown[i] == 1 && time[i] > 0 && time[i] <= exptime) ngs1+=1. ;
+         if (cents2[i] == 2 && sfknown[i] == 1 && time[i] > 0 && time[i] <= exptime) ngs2+=1. ;
+         if (cents3[i] == 2 && sfknown[i] == 1 && time[i] > 0 && time[i] <= exptime) ngs3+=1. ;
+         if (cents4[i] == 2 && sfknown[i] == 1 && time[i] > 0 && time[i] <= exptime) ngs4+=1. ;
+         if (cents5[i] == 2 && sfknown[i] == 1 && time[i] > 0 && time[i] <= exptime) ngs5+=1. ;
+         if (cents6[i] == 2 && sfknown[i] == 1 && time[i] > 0 && time[i] <= exptime) ngs6+=1. ; }
+
+       /* convert to fraction of observing time */
+       ngs1 = ngs1 / exptime ;
+       ngs2 = ngs2 / exptime ;
+       ngs3 = ngs3 / exptime ;
+       ngs4 = ngs4 / exptime ;
+       ngs5 = ngs5 / exptime ;
+       ngs6 = ngs6 / exptime ;
+
+	/* determine the number of guide stars used during the exposure */
+	ngs_used = 0 ;
+	if (ngs1 > 0) ngs_used += 1 ; 
+	if (ngs2 > 0) ngs_used += 1 ; 
+	if (ngs3 > 0) ngs_used += 1 ; 
+	if (ngs4 > 0) ngs_used += 1 ; 
+	if (ngs5 > 0) ngs_used += 1 ; 
+	if (ngs6 > 0) ngs_used += 1 ; 
+	cf_verbose(2, "maximum number of guide stars used: %d",ngs_used) ;
+
+       /* Populate header keywords */
+        FITS_update_key(outfits, TINT, "NGS_USED", &ngs_used, 
+           "number of guide stars used", &status) ;
+        FITS_update_key(outfits, TFLOAT, "GS1_USED", &ngs1, 
+           "fraction of exp using known guide star 1", &status) ;
+        FITS_update_key(outfits, TFLOAT, "GS2_USED", &ngs2, 
+           "fraction of exp using known guide star 2", &status) ;
+        FITS_update_key(outfits, TFLOAT, "GS3_USED", &ngs3, 
+           "fraction of exp using known guide star 3", &status) ;
+        FITS_update_key(outfits, TFLOAT, "GS4_USED", &ngs4, 
+           "fraction of exp using known guide star 4", &status) ;
+        FITS_update_key(outfits, TFLOAT, "GS5_USED", &ngs5, 
+           "fraction of exp using known guide star 5", &status) ;
+        FITS_update_key(outfits, TFLOAT, "GS6_USED", &ngs6, 
+           "fraction of exp using known guide star 6", &status) ;
+
+	/* Determine times of known and unknown tracking and
+		tracking on the target */ 
+	knowntrk = 0. ;
+        acstrk = 0. ;
+        targtrk = 0. ;
+        gs_used = 0. ;
+	for (i=0 ; i< npts ; i++) {
+          if (qvalid[i] == 1 && time[i] > 0 && time[i] <= exptime) gs_used+=1.;
+          if ((trakflg[i] == 5 || trakflg[i] == 2) &&
+		fabs(dx[i]) < 15 && fabs(dy[i]) < 15 && time[i] > 0 && time[i] <= exptime) 
+                knowntrk += 1. ;
+          if ((trakflg[i] == 4 || trakflg[i] == 3 || trakflg[i] == 1) &&
+		fabs(dx[i]) < 15 && fabs(dy[i]) < 15 && time[i] > 0 && time[i] <= exptime) 
+                acstrk += 1. ; 
+          if (trakflg[i] > 0 &&
+                fabs(dx[i]) < 15 && fabs(dy[i]) < 15 && time[i] > 0 && time[i] <= exptime)
+	        targtrk += 1. ;
+     }
+        cf_verbose(2, "seconds when guide stars are used: %.0f",gs_used ) ;
+        cf_verbose(2, "seconds tracking on known stars with error < 15 arcsec: %.0f",knowntrk) ;
+        cf_verbose(2, "seconds tracking on ACS with error < 15 arcsec: %.0f", acstrk) ;
+        cf_verbose(2, "seconds tracking on target with error < 15 arcsec: %.0f",targtrk ) ;
+	knowntrk = knowntrk /  exptime ;
+	acstrk = acstrk / exptime ;
+        targtrk = targtrk / exptime ;
+        gs_used = gs_used / exptime ;
+         FITS_update_key(outfits, TFLOAT, "KTRKFINE", &knowntrk, 
+            "exp fraction, err < 15 arcsec, known stars", &status) ;
+         FITS_update_key(outfits, TFLOAT, "ATRKFINE", &acstrk, 
+            "exp fraction, err < 15 arcsec, ACS", &status) ;
+        FITS_update_key(outfits, TFLOAT, "TOTLFINE", &targtrk, 
+            "exp fraction, err < 15 arcsec, total", &status) ;
+        FITS_update_key(outfits, TFLOAT, "GS_INUSE", &gs_used, 
+            "fraction of exp tracking on guide stars", &status) ;
+
+
+	/* determine whether a new attitude is commanded during the exposure */
+        slewflg = -1 ;
+	for (i=0; i<npts ; i++) 
+          if(slew[i] > 0 && time[i] > 0 && time[i] <= exptime) {
+		slewflg = 1 ;
+		break;
+	}
+        FITS_update_key(outfits, TINT, "SLEWFLG", &slewflg, 
+            "Slew commanded during obs (if > 0)", &status) ;
+        if (slewflg > 0) cf_verbose(1, "SLEW COMMANDED DURING EXPOSURE!!!") ; 
+
+	/* determine the slewing time - note that there is a 16s time
+           resolution on the sampling of acaflg. Thus, slews of less than 16s
+           are not real */
+        slewtime=0 ;
+        FITS_update_key(outfits, TINT, "SLEWTIME", &slewtime, 
+            "time spent slewing (sec)", &status) ;
+
+        for (i=0; i<npts; i++) 
+	  if (acaflg[i] < 1 && time[i] > 0 && time[i] <= exptime ) slewtime++ ;
+        if (slewtime > 16) {
+             FITS_update_key(outfits, TINT, "SLEWTIME", &slewtime, 
+                "time spent slewing (sec)", &status) ;
+             slewflg=1 ;
+             FITS_update_key(outfits, TINT, "SLEWFLG", &slewflg, 
+                "slew commanded during obs (if > 0)", &status) ;
+             cf_verbose(1, "SLEW OCCURRED DURING EXPOSURE!!!") ;
+             cf_verbose(2, "Time (sec) spent slewing = %d",slewtime) ;
+	} 
+
+	/* determine basic properties of the jitter */
+	dxrms = 0. ;
+        dxrms5 = 0. ;
+        dyrms = 0. ;
+        dyrms5 = 0. ;
+        dxave = 0. ;
+        dyave = 0. ;
+        nvalid = 0 ;
+        nvalid5 = 0 ;
+	for (i=0 ; i< npts ; i++) 
+	  if(sfknown[i] == 1 && acaflg[i] == 1 && time[i] > qtime && time[i] <= exptime) {
+	    cf_verbose(4, "i = %ld, dx = %f, dy = %f", i, dx[i], dy[i]);
+            nvalid += 1 ;
+            dxrms += dx[i]*dx[i]  ;
+            dxave += dx[i] ;
+            dyrms += dy[i] * dy[i] ;
+            dyave += dy[i] ;
+            if (fabs(dx[i]) < 15 && fabs(dy[i]) < 15) {
+              dxrms5 += dx[i] * dx[i] ;
+              dyrms5 += dy[i] * dy[i] ;
+              nvalid5 += 1 ; }
+	  }
+        cf_verbose(2, "number of points used to determine rms jitter = %d", nvalid) ;
+  
+	if (nvalid > 0) dxrms = sqrt( dxrms / (float) nvalid) ;
+	if (nvalid > 0) dyrms = sqrt( dyrms / (float) nvalid) ;
+	if (nvalid5 > 0) dxrms5 = sqrt( dxrms5 / (float) nvalid5) ;
+	if (nvalid5 > 0) dyrms5 = sqrt( dyrms5 / (float) nvalid5) ;
+        if (nvalid > 0) dxave = dxave / (float) nvalid ;
+        if (nvalid > 0) dyave = dyave / (float) nvalid ;
+        cf_verbose(2, "jitter properties:") ;
+	cf_verbose(2, "dxave = %f, dxrms=%f, dxrms5 = %f", dxave, dxrms, dxrms5) ;
+	cf_verbose(2, "dyave = %f, dyrms=%f, dyrms5 = %f", dyave, dyrms, dyrms5) ;
+          FITS_update_key(outfits, TFLOAT, "POSAVG_X", &dxave, 
+            "[arcsec] mean DX during known track", &status) ;
+          FITS_update_key(outfits, TFLOAT, "POSAVG_Y", &dyave, 
+            "[arcsec] mean DY during known track", &status) ;
+
+          FITS_update_key(outfits, TFLOAT, "X_JITTER", &dxrms, 
+            "[arcsec] sigma of DX during known track", &status) ;
+          FITS_update_key(outfits, TFLOAT, "Y_JITTER", &dyrms, 
+            "[arcsec] sigma of DY during known track", &status) ;
+
+          FITS_update_key(outfits, TFLOAT, "XJIT_15", &dxrms5, 
+            "[arcsec] sigma of DX for err < 15 arcsec", &status) ;
+          FITS_update_key(outfits, TFLOAT, "YJIT_15", &dyrms5, 
+            "[arcsec] sigma of DY for err < 15 arcsec", &status) ;
+
+  /* determine fraction of exposure where the dy and dx values exceed 2 
+     sigma from the mean */
+          jitlgx=0 ;
+          jitlgy=0 ;
+	  for (i=0 ; i<npts ; i++) {
+            if ( fabs(dx[i]) > 2.*dxrms) jitlgx++ ;
+            if ( fabs(dy[i]) > 2.*dyrms) jitlgy++ ;
+		}
+
+	  fjitlgx= (float) jitlgx / (float) npts ;
+	  fjitlgy = (float) jitlgy / (float) npts ;
+
+          FITS_update_key(outfits, TFLOAT, "X_JITLRG", &fjitlgx, 
+            "frac of DX more than 2-sigma from POSAVE_X", &status) ;
+          FITS_update_key(outfits, TFLOAT, "Y_JITLRG", &fjitlgy, 
+            "frac of DY more than 2-sigma from POSAVE_Y", &status) ;
+
+
+
+  /******* Generate the table and put in guiding info *****/
+  
+      tfields = 4 ; 
+  	 FITS_create_tbl(outfits, BINARY_TBL, 0, tfields, ttype,
+		  tform, tunit, textname, &status) ;
+
+      fits_get_colnum(outfits, TRUE, "TIME", &tcol, &status) ;
+      FITS_write_col(outfits, TLONG, tcol, 1, 1, npts, time, &status) ;
+      fits_get_colnum(outfits, TRUE, "DX", &dxcol, &status) ;
+      FITS_write_col(outfits, TFLOAT, dxcol, 1, 1, npts, dx, &status) ;
+      fits_get_colnum(outfits, TRUE, "DY", &dycol, &status) ;
+      FITS_write_col(outfits, TFLOAT, dycol, 1, 1, npts, dy, &status) ;
+      fits_get_colnum(outfits, TRUE, "TRKFLG", &trkcol, &status) ;
+      FITS_write_col(outfits, TSHORT, trkcol, 1, 1, npts, trakflg, &status) ;
+
+ /**********************************************************************/
+
+    /* Set the status flag to 0 -- unless it has already been changed. */
+    if (dstatus == 1) {
+       FITS_movabs_hdu(outfits, 1, &hdutype, &status) ;
+       dstatus = 0 ;
+       FITS_update_key(outfits, TINT, "JIT_STAT", &dstatus, 
+            "Status of jitter data is good", &status) ;
+    }
+
+    /* close the output file */
+    FITS_close_file(outfits, &status) ; 
+
+    /* free up storage space */
+    free(mjd) ;
+    free(qvalid) ;
+    free(fq1) ;
+    free(fq2) ;
+    free(fq3) ;
+    free(aq1) ;
+    free(aq2) ;
+    free(aq3) ;
+    free(aqsok) ;
+    free(acscmd1) ;
+    free(acscmd2) ;
+    free(acscmd3) ;
+    free(time) ;
+    free(trakflg) ;
+    free(dx) ;
+    free(dy) ;
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished execution.");
+
+    return 0 ;
+} 
diff --git a/src/cal/jitter/cf_jitter_diag.c b/src/cal/jitter/cf_jitter_diag.c
new file mode 100644
index 0000000..1908458
--- /dev/null
+++ b/src/cal/jitter/cf_jitter_diag.c
@@ -0,0 +1,916 @@
+/**************************************************************************
+ *           Johns Hopkins University  
+ *          Center for Astrophysical Sciences    
+ *           FUSE
+ *************************************************************************
+ *
+ * synopsis:    cf_jitter_diag input_file raw_file output_file      
+ *
+ * Description: Reads a FITS file containing housekeeping data and
+ *              generates a FITS file containing the jitter information 
+ *              for the observation. This program is used to generate 
+ *              diagnostics of the jitter performance during an observation
+ *
+ * Arguments: input_file    Input raw FITS housekeeping file for an observation
+ *                            The header of this is used as a template
+ *                            for the output file
+ *            raw_file      Raw data file - used to get the start time and the 
+ *                            exposure time
+ *            output_file   FITS table containing the jitter information 
+ *     
+ * 
+ *Contents of output file: 
+ *   1. Time of sample (in seconds from start)
+ *   2. shifts dx and dy (in arcsec) of the pointing from a reference position
+ *   3. tracking quality flag (best=5, worst=0)
+ *
+ *                                 
+ * HISTORY:       01/22/02   v1.0     Robinson  Begin work
+ *                08/14/02   v1.1     Robinson  populate JIT_STATUS keyword
+ *                09/20/02   v1.11    Robinson  - update FILENAME, FILETYPE keywords
+ *                                              - change EXP_DUR keyword to reflect
+ *                                                total time duration of jitter data
+ *                11/04/02   v1.2     Robinson  change method in which gaps are filled
+ *                                              we no longer assume that the data is 
+ *                                              tabulated at regular intervals. Also 
+ *                                              checks that tabulated times start BEFORE
+ *                                              the observation start time
+ *                12/17/02   v1.3     Robinson  Slight change in definitions of TRAKFLG
+ *                                              values.
+ *                01/17/03   v1.4     Robinson  slight change in calculating summary of
+ *                                              jitter properties
+ *                05/22/03   v1.5     rdr       changed initialization of arrays
+ *                06/10/03   v1.6     rdr       Correct problem in determining ref 
+ *                                              quaternian
+ *                06/23/03   v1.7     rdr       Adjust calculation on some of the 
+ *                                               keywords
+ *                06/25/03   v1.8     rdr       Added call to raw data file to determine
+ *                                               actual start and exposure times
+ *                06/27/03   v1.9     rdr       Corrected procedure for determining 
+ *                                               reference quaternian
+ *                03/03/04   v1.10    bjg       include unistd.h
+ *		  06/24/05   v1.11    wvd       Delete unused variables.
+ *		  08/24/07   v1.12    bot       changed TINT to TLONG for time l.826.
+ *
+ **************************************************************************/
+#include <unistd.h>
+#include <string.h>   
+#include <stdio.h>
+#include <stdlib.h>
+#include <math.h>
+#include "calfuse.h"
+
+static char CF_PRGM_ID[] = "cf_jitter_diag";   
+static char CF_VER_NUM[] = "1.12";  
+
+int quatprod(double *, double *, double *) ;    
+
+int main(int argc, char *argv[])  
+{
+  FILE *output, *ftest ;
+  fitsfile *infits, *outfits ;
+  int hdutype, tfields, dstatus ;
+  int nvalid, nvalid5, optc, rtime ;
+  int aattmode_colnum, pflg=0 ;
+  int *aattflg, tflg, qvalidt ;
+  int tcolnum, fpdquat1_colnum,  fpdquat2_colnum,  fpdquat3_colnum ;
+  int aquat1_colnum, aquat2_colnum, aquat3_colnum, slew_colnum ;
+  int status, tcol;
+  int dxcol, dycol, trkcol, anynull, intnull=0 ;
+  int fpdexp_colnum, qvalid_colnum, cents1_colnum, cents2_colnum, cents3_colnum ;
+  int cents4_colnum, cents5_colnum, cents6_colnum, acsflg_colnum ;
+  int acscmd1_colnum, acscmd2_colnum, acscmd3_colnum, sfknwn_colnum ;
+  int frow, felem, slewflg, ngs_used, jitlgx, jitlgy ;
+  int *cents1, *cents2, *cents3, *cents4, *cents5, *cents6 , *qvalid ;
+  int *sfknwn, *slew ;
+  int cents1t=0, cents2t=0, cents3t=0, cents4t=0, cents5t=0, cents6t=0 ;
+  int sfknwnt=0 , slewt=0, slewtime=0 ;
+  long i, j, numq4, numq5, numq3, numq2, numqa, numq0 ; 
+  long  npts, tval ;
+  long *time, qtime=0;
+  float tfine, tcoarse, tnull, knowntrk, unknowntrk, fjitlgx, fjitlgy ;
+  float targtrk ;
+  float ngs1, ngs2, ngs3, ngs4, ngs5, ngs6, gs_used, expdur, exptime ;
+  float dxrms, dyrms, dxave, dyave, dxrms5, dyrms5 ;
+  float *fpdexp, *acsflg ;
+  float *dx , *dy ;
+  double *fq1, *fq2,*fq3, *dq1, *dq2, *dq3, *mjd ;
+  double *acscmd1, *acscmd2, *acscmd3, fq1t, fq2t, fq3t  ;
+  double tstrt ;
+  double tquat[4], dquat[4], quat_ref[4] ;
+  double *aq1, *aq2, *aq3, aq1t, aq2t, aq3t ;
+  short *trakflg ;
+  char buffer[FLEN_CARD];
+  char *ttype[] = { "TIME", "DX", "DY", "TRKFLG" } ;
+  char *tform[] = { "1J", "1E", "1E", "1I" } ;
+  char *tunit[] = { "seconds", "arcsec", "arcsec", " "} ;
+  char textname[7]="jitter" ;
+
+char opts[] = "hv:";
+    char usage[] =
+	"Usage:\n"
+	"  cf_jitr_diag [-h] [-v level] hskpfile rawfile outfile\n";
+    char option[] = 
+	"Options:\n"
+	"  -h:  this help message\n"
+	"  -v:  verbosity level (=1; 0 is silent)\n";
+
+    verbose_level = 1;
+
+    while ((optc = getopt(argc, argv, opts)) != -1) {
+	switch(optc) {
+
+	case 'h':
+	    printf("%s\n%s", usage, option);
+	    return 0;
+	case 'v':
+	    verbose_level = atoi(optarg);
+	    break;
+	}
+    }
+
+  cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+    if (argc != optind+3) {
+        printf("%s", usage);
+        cf_if_error("Incorrect number of arguments");
+    }
+
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin execution");
+
+  /* initialize necessary variables */
+  hdutype=0 ;
+  status=0 ;
+  frow=1 ;
+  felem=1 ;
+  anynull=0 ;
+
+
+  /* check that the housekeeping and raw data files are available */
+  cf_verbose(3,"checking for housekeeping file : %s ",argv[optind]) ;
+  ftest=fopen(argv[optind],"r") ;
+   if (ftest == NULL) {
+      cf_verbose(1,"No input housekeeping file available - returning ") ;
+      return 0; }
+   fclose( ftest ) ;
+  ftest=fopen(argv[optind+1],"r") ;
+   if (ftest == NULL) {
+      cf_verbose(1,"No input raw data file available - returning ") ;
+      return 0; }
+   fclose( ftest ) ;
+
+ /* Open the input raw data FITS file and read the start and exposure times */
+  cf_verbose(3,"opening the file %s for input ",argv[optind+1]);
+  FITS_open_file(&infits, argv[optind+1], READONLY, &status); 
+ 
+  /* read the starting time and duration  from the FITS header */
+  FITS_read_key(infits, TDOUBLE, "EXPSTART", &tstrt, buffer, &status) ;
+  cf_verbose(3,"start time (MJD) = %15.9f ",tstrt) ;
+  FITS_read_key(infits, TFLOAT, "EXPTIME", &exptime, buffer, &status) ;
+  exptime=(int) exptime ;
+   cf_verbose(3,"exposure duration (sec) = %f ",exptime) ;
+
+   /* close the raw data file and open the housekeeping file */
+      FITS_close_file(infits, &status) ;
+      FITS_open_file(&infits, argv[optind], READONLY, &status); 
+ 
+      /* check for the existance of the output file */      
+      output = fopen(argv[optind+2], "r") ; 
+      if (output != NULL) {
+        cf_verbose(1,"output file already exists - returning ") ;
+        return 1 ; } 
+      else fclose(output) ;  
+
+  /* Create the output file */
+     FITS_create_file(&outfits, argv[optind+2], &status); 
+
+  /* Copy the header and empty primary image of the input file to 
+     the output */
+     FITS_copy_hdu(infits, outfits, 0, &status) ;
+
+     /* populate the STATUS keyword with 1 - 
+        will reset keyword if everyhing goes well */
+     dstatus = 1 ;
+       FITS_update_key(outfits, TINT, "JIT_STAT", &dstatus, 
+            "problems with jitter data", &status) ;
+
+   /* update FILENAME, FILETYPE, EXPTIME and EXPSTART keywords */
+     FITS_update_key(outfits, TSTRING, "FILENAME",argv[optind+2], NULL, &status) ;
+     FITS_update_key(outfits, TSTRING, "FILETYPE","JITTER", NULL, &status) ;
+     FITS_update_key(outfits, TFLOAT, "EXPTIME",&exptime, NULL, &status) ;
+     FITS_update_key(outfits, TDOUBLE, "EXPSTART",&tstrt, NULL, &status) ;
+
+  /* move to the first extension, which contains the table */
+     FITS_movabs_hdu(infits, 2, &hdutype, &status) ;
+
+  /* determine the number of times which have been tabulated */
+     FITS_read_key(infits, TLONG, "NAXIS2", &npts, NULL, &status) ;
+     cf_verbose(3,"number of samples in the table = %d ",npts) ;
+
+  /*   set up arrays to contain the data to be read from the table  */
+           mjd = (double *) cf_calloc(npts, sizeof(double)) ;
+           fpdexp = (float *) cf_calloc(npts, sizeof(float) ) ;
+           qvalid = (int *) cf_calloc(npts, sizeof(int)) ;
+           fq1 = (double *) cf_calloc(npts, sizeof(double) ) ;
+           fq2 = (double *) cf_calloc(npts, sizeof(double) ) ;
+           fq3 = (double *) cf_calloc(npts, sizeof(double) ) ;
+           aq1 = (double *) cf_calloc(npts, sizeof(double) ) ;
+           aq2 = (double *) cf_calloc(npts, sizeof(double) ) ;
+           aq3 = (double *) cf_calloc(npts, sizeof(double)) ; 
+	   aattflg = (int *) cf_calloc(npts, sizeof(int)) ;
+           acsflg = (float *) cf_calloc(npts, sizeof(float)) ;
+           acscmd1 = (double *) cf_calloc(npts, sizeof(double)) ; 
+           acscmd2 = (double *) cf_calloc(npts, sizeof(double) ) ; 
+           acscmd3 = (double *) cf_calloc(npts, sizeof(double) ) ; 
+           cents1 = (int *) cf_calloc(npts, sizeof(int)) ;
+           cents2 = (int *) cf_calloc(npts, sizeof(int) ) ;
+           cents3 = (int *) cf_calloc(npts, sizeof(int) ) ;
+           cents4 = (int *) cf_calloc(npts, sizeof(int) ) ;
+           cents5 = (int *) cf_calloc(npts, sizeof(int) ) ;
+           cents6 = (int *) cf_calloc(npts, sizeof(int) ) ;
+           sfknwn = (int *) cf_calloc(npts, sizeof(int) ) ;
+           slew = (int *) cf_calloc(npts, sizeof(int) ) ;
+
+  /* read the data */
+	   FITS_get_colnum(infits, CASEINSEN, "MJD", &tcolnum, &status) ;
+	   cf_verbose(5,"column number for time = %d ",tcolnum) ; 
+	     FITS_read_col(infits, TDOUBLE, tcolnum, frow, felem, npts, &intnull,
+			   mjd, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "I_FPD_EXP_DURATION", &fpdexp_colnum, 
+                   &status) ;
+	   /*printf("column number for fdpexp = %d \n",fpdexp_colnum) ;*/
+	     FITS_read_col(infits, TFLOAT, fpdexp_colnum, frow, felem, npts, &intnull,
+		     fpdexp, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "I_FPD_MEAS_Q_VALID", &qvalid_colnum, 
+                  &status) ;
+	   /*printf("column number for qvalid = %d \n",qvalid_colnum) ;*/
+	     FITS_read_col(infits, TINT, qvalid_colnum, frow, felem, npts, &intnull,
+			   qvalid, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "I_FPD_Q_ECI2BDY_1", &fpdquat1_colnum, 
+                  &status) ;
+	   /*printf("column number for fq1 = %d \n",fpdquat1_colnum) ;*/
+	     FITS_read_col(infits, TDOUBLE, fpdquat1_colnum , frow, felem, npts, &intnull,
+			  fq1, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "I_FPD_Q_ECI2BDY_2", &fpdquat2_colnum, 
+                  &status) ;
+	   /*printf("column number for fq2 = %d \n",fpdquat2_colnum) ;*/
+	     FITS_read_col(infits, TDOUBLE, fpdquat2_colnum , frow, felem, npts, &intnull,
+			   fq2, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "I_FPD_Q_ECI2BDY_3", &fpdquat3_colnum, 
+                  &status) ;
+	   /*printf("column number for fq3 = %d \n",fpdquat3_colnum) ;*/
+	     FITS_read_col(infits, TDOUBLE, fpdquat3_colnum , frow, felem, npts, &intnull,
+			   fq3, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "AATTQECI2BDY_1", &aquat1_colnum, &status) ;
+	   /*printf("column number for aq1 = %d \n",aquat1_colnum) ;*/
+	     FITS_read_col(infits, TDOUBLE, aquat1_colnum , frow, felem, npts, &intnull,
+			   aq1, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "AATTQECI2BDY_2", &aquat2_colnum, &status) ;
+	   /*printf("column number for aq2 = %d \n",aquat2_colnum) ;*/
+	     FITS_read_col(infits, TDOUBLE, aquat2_colnum, frow, felem, npts, &intnull,
+			   aq2, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "AATTQECI2BDY_3", &aquat3_colnum, &status) ;
+	   /*printf("column number for aq3 = %d \n",aquat3_colnum) ;*/
+	     FITS_read_col(infits, TDOUBLE, aquat3_colnum, frow, felem, npts, &intnull,
+			   aq3, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "AATTMODE", &aattmode_colnum, &status) ;
+	   /*printf("column number for aattmode = %d \n",aattmode_colnum) ;*/
+	     FITS_read_col(infits, TINT, aattmode_colnum, frow, felem, npts, &intnull,
+			   aattflg, &anynull, &status) ;
+
+	   FITS_get_colnum(infits, CASEINSEN, "I_AT_CMD_ATT", &acsflg_colnum, &status) ;
+	   /*printf("column number for acsflg = %d \n",acsflg_colnum) ;*/
+	     FITS_read_col(infits, TFLOAT, acsflg_colnum, frow, felem, npts, &intnull,
+			   acsflg, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "AQECI2BDYCMD_1", &acscmd1_colnum, &status) ;
+	   /*printf("column number for acscmd1 = %d \n",acscmd1_colnum) ;*/
+	     FITS_read_col(infits, TDOUBLE, acscmd1_colnum, frow, felem, npts, &intnull,
+			   acscmd1, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "AQECI2BDYCMD_2", &acscmd2_colnum, &status) ;
+	   /*printf("column number for acscmd2 = %d \n",acscmd2_colnum) ;*/
+	     FITS_read_col(infits, TDOUBLE, acscmd2_colnum, frow, felem, npts, &intnull,
+			   acscmd2, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "AQECI2BDYCMD_3", &acscmd3_colnum, &status) ;
+	   /* printf("column number for acscmd3 = %d \n",acscmd3_colnum) ;*/
+	     FITS_read_col(infits, TDOUBLE, acscmd3_colnum, frow, felem, npts, &intnull,
+			   acscmd3, &anynull, &status) ;
+
+	   FITS_get_colnum(infits, CASEINSEN, "CENTROID1_STATUS", &cents1_colnum,
+                &status) ;
+	   /* printf("column number for guide star 1 status = %d \n",cents1_colnum) ; */
+	     FITS_read_col(infits, TINT, cents1_colnum, frow, felem, npts, &intnull,
+			   cents1, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "CENTROID2_STATUS", &cents2_colnum,
+                &status) ;
+	   /* printf("column number for guide star 2 status = %d \n",cents2_colnum) ; */
+	     FITS_read_col(infits, TINT, cents2_colnum, frow, felem, npts, &intnull,
+			   cents2, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "CENTROID3_STATUS", &cents3_colnum,
+                &status) ;
+	   /* printf("column number for guide star 3 status = %d \n",cents3_colnum) ; */
+	     FITS_read_col(infits, TINT, cents3_colnum, frow, felem, npts, &intnull,
+			   cents3, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "CENTROID4_STATUS", &cents4_colnum,
+                &status) ;
+	   /* printf("column number for guide star 4 status = %d \n",cents4_colnum) ; */
+	     FITS_read_col(infits, TINT, cents4_colnum, frow, felem, npts, &intnull,
+			   cents4, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "CENTROID5_STATUS", &cents5_colnum,
+                &status) ;
+	   /* printf("column number for guide star 5 status = %d \n",cents5_colnum) ; */
+	     FITS_read_col(infits, TINT, cents5_colnum, frow, felem, npts, &intnull,
+			   cents5, &anynull, &status) ;
+	   FITS_get_colnum(infits, CASEINSEN, "CENTROID6_STATUS", &cents6_colnum,
+                &status) ;
+	   /* printf("column number for guide star 6 status = %d \n",cents6_colnum) ; */
+	     FITS_read_col(infits, TINT, cents6_colnum, frow, felem, npts, &intnull,
+			   cents6, &anynull, &status) ;
+
+	   FITS_get_colnum(infits, CASEINSEN, "I_FPD_STARFLD_KNWN", &sfknwn_colnum,
+                &status) ;
+	   /* printf("column number for starfield known status = %d \n",sfknwn_colnum) ; */
+	     FITS_read_col(infits, TINT, sfknwn_colnum, frow, felem, npts, &intnull,
+			   sfknwn, &anynull, &status) ;
+
+	   FITS_get_colnum(infits, CASEINSEN, "I_FPD_NEW_CMD_Q", &slew_colnum,
+                &status) ;
+	   /* printf("column number for slew status = %d \n",slew_colnum) ; */
+	     FITS_read_col(infits, TINT, slew_colnum, frow, felem, npts, &intnull,
+			   slew, &anynull, &status) ;
+
+
+  /* close the input file */
+      FITS_close_file(infits, &status) ;
+
+  /* check for problems with the tabulated start time */
+      if (fabs(mjd[0]-tstrt) > 1) {
+	cf_verbose(1,"Problems with tabulated start time ") ;
+        cf_verbose(1,"  Value of tabulated start time = %15.7f ",tstrt) ;
+        cf_verbose(1,"  First tabulated MJD = %15.7f ",mjd[0]) ;
+	/* update JIT_STAT keyword */
+          dstatus = 1 ;
+          FITS_update_key(outfits, TINT, "JIT_STAT", &dstatus, 
+            "problems with tab start time", &status) ;
+        FITS_close_file(outfits, &status) ;
+	return 1; }
+
+  /* make sure that the tabulates times start BEFORE the start of the observation,
+     Otherwise there may be missing data or an error in the tabulated start time */
+       tval=(long) (0.5 + (mjd[0]-tstrt) * 86400.) ;
+      if (tval > 0) {
+       cf_verbose(1,"WARNING: There may be missing data or an error in the start time \n") ;
+       cf_verbose(1,"         The first tabulated time is %d seconds from obs start ", tval) ;
+	/* update JIT_STAT keyword */
+          dstatus = 1 ;
+          FITS_update_key(outfits, TINT, "JIT_STAT", &dstatus, 
+            "problems with tab start time", &status) ;
+        FITS_close_file(outfits, &status) ;
+        return 1 ;
+ }      
+
+
+  /* fill in the gaps in the data set 
+
+     - ACS quaternians are generally tabulated every other second
+     - FPD quaternians can be every second or every other second
+     - AATTMODE flags tabulates every 5 seconds
+     - ACS flags (acsflg) - tabulated every 16 seconds
+
+NOTE:  there can be irregularities in the spacing. Thus, save the last
+tabulated value and use this in filling in missing data for a given time */
+
+      /* ACS quaternians */
+      aq1t = 0. ;
+      aq2t = 0. ;
+      aq3t = 0. ;
+      for (i=0 ; i<npts ; i++) {
+        if ( aq1[i] > -1 && aq2[i] > -1){
+	  aq1t=aq1[i] ;
+	  aq2t=aq2[i] ;
+	  aq3t=aq3[i] ; }
+        else {
+          aq1[i] = aq1t ;
+          aq2[i] = aq2t ;
+          aq3[i] = aq3t ; }
+	}
+
+      /* FPD quaternians and qvalid flags 
+         only update the one following a good quaternian. if there is another one
+         with no quaternian after that, do not update it */
+
+     fq1t = 0. ;
+     fq2t = 0. ;
+     fq3t = 0. ;
+     qvalidt = 0 ;
+     tflg = -1 ;
+      for (i=0 ; i<npts ; i++) {
+        if ( (fabs(fq1[i]) > 0.) && (fabs(fq2[i]) > 0.) ){
+	  fq1t=fq1[i] ;
+	  fq2t=fq2[i] ;
+	  fq3t=fq3[i] ; 
+          qvalidt = qvalid[i] ;
+          cents1t = cents1[i] ;
+          cents2t = cents2[i] ;
+          cents3t = cents3[i] ;
+          cents4t = cents4[i] ;
+          cents5t = cents5[i] ;
+          cents6t = cents6[i] ;
+          sfknwnt = sfknwn[i] ;
+          slewt = slew[i] ;
+          tflg = 1 ; }
+        else if (tflg > 0) {
+          fq1[i] = fq1t ;
+          fq2[i] = fq2t ;
+          fq3[i] = fq3t ;
+          qvalid[i] = qvalidt ;
+          cents1[i] = cents1t ; 
+          cents2[i] = cents2t ; 
+          cents3[i] = cents3t ; 
+          cents4[i] = cents4t ; 
+          cents5[i] = cents5t ; 
+          cents6[i] = cents6t ; 
+          sfknwn[i] = sfknwnt ;
+          slew[i] = slewt ;
+          tflg = -1 ; }
+	}
+
+
+       /* AATTMODE flag - update as long as quaternians are
+          present */
+ 
+       tflg = -1 ;          
+       for (i=0 ; i<npts-1 ; i++) {
+         if (aattflg[i] > -1) tflg = aattflg[i] ;
+         else {
+	     aattflg[i] = -10 ;
+             if (aq1[i] > -1) aattflg[i]=3 ;
+      	     if ((fabs(fq1[i]) > 0.) && ( fabs(fq2[i]) > 0. ) ) aattflg[i]=tflg ; }
+        } 
+
+
+       /* ACSFLG flag */
+
+       tflg = -10 ;          
+       for (i=0 ; i<npts-1 ; i++) {
+         if (acsflg[i] > -1) tflg = acsflg[i] ;
+         else acsflg[i] = tflg ;
+        } 
+		       
+
+ /********** derive the final quats arrays and the tracking flags *******/
+
+  /*    set up arrays to contain the data */
+         time = (long *) cf_calloc(npts, sizeof(long) ) ;
+	 trakflg = (short *) cf_calloc(npts, sizeof(short) ) ; 
+         dq1 = (double *) cf_calloc(npts, sizeof(double) ) ;
+         dq2 = (double *) cf_calloc(npts, sizeof(double)) ;
+         dq3 = (double *) cf_calloc(npts, sizeof(double) ) ;
+         dx = (float *) cf_calloc(npts, sizeof(float) ) ;
+         dy = (float *) cf_calloc(npts, sizeof(float) ) ;
+
+ /* fill in the time array with times (in seconds) from the start of the observation */
+	 for (i=0 ; i<npts ; i++) {
+           tval=(long) (0.5 + (mjd[i]-tstrt) * 86400.) ;
+           time[i] = tval ; }
+
+
+ /* determine the reference quat by looking at the commanded ACS quaternian (in arrays
+     acscmd1, acscmd2 and acscmd3) when they have converged to the fpd commanded
+     quaternian - i.e. when the AT_CMD_ATT flag is 1 (held in the array acsflg) -
+     Make sure that the time for convergence is AFTER the start of the observation and that
+     the starfield is known (i.e. sfknwn = 1). Also, because of the 16s sample time of 
+     the ascflg array, require that the condition exists for at least 30 consequtive seconds 
+     before accepting the quaternians.
+       qtime = time at which the quaternians were found. This is the earliest time in the exposure
+               for which reliable positions are available*/
+
+	 rtime=0 ;
+	 for (i=0 ; i<npts; i++) {
+           if (acsflg[i] == 1 &&  time[i] > 0 && sfknwn[i] == 1) {
+             rtime += 1 ;
+             cf_verbose(4,"quat ref cond exists at time=%d, rtime=%d ",time[i],rtime) ;
+	     if(rtime == 1) qtime=time[i] ;
+             if (rtime > 30 && acscmd1[i] > -1 && acscmd2[i] > -1 && acscmd3[i] > -1 ) {
+  	       quat_ref[0]=acscmd1[i] ;
+               quat_ref[1]=acscmd2[i] ;
+               quat_ref[2]=acscmd3[i] ;
+               quat_ref[3]=sqrt( 1. - quat_ref[0]*quat_ref[0] - quat_ref[1]*quat_ref[1] - quat_ref[2]*quat_ref[2] ) ;
+	       goto skip ; }
+	   }
+           else rtime=0 ; 
+	 }
+
+     /* if we are here, then the flag was never set and the reference quat not determined */
+	 cf_verbose(1," Problem determining the reference quaternians ") ;
+	 /* determine cause of failure */
+         pflg = 0 ;
+	 for (i=0 ; i<npts; i++) if (acsflg[i] == 1) pflg=1 ;
+	   if (pflg == 0) {
+               cf_verbose(1," AT_CMD_ATT flag was never set  ") ;
+         	/* update JIT_STAT keyword */
+                   dstatus = 2 ;
+                   FITS_update_key(outfits, TINT, "JIT_STAT", &dstatus, 
+                   "AT_CMD_ATT flg never set", &status) ;
+	   }
+         pflg = 0 ;
+	 for (i=0 ; i<npts; i++) if (sfknwn[i] == 1) pflg=1 ;
+	   if (pflg == 0)  {
+               printf(" UNKNOWN STAR FIELD \n") ;
+   	         /* update JIT_STAT keyword */
+                    dstatus = 3 ;
+                    FITS_update_key(outfits, TINT, "JIT_STAT", &dstatus, 
+                      "unknown star field", &status) ;
+	   }
+         FITS_close_file(outfits, &status) ;
+         return 1 ;
+ skip: ;
+	cf_verbose(3," ") ;
+        cf_verbose(3,"reference quat values - from ACS commanded pos ") ;
+        cf_verbose(3,"found at time %d \n",qtime) ;
+      for (i=0; i<4 ; i++) cf_verbose(3,"for i=%d, quat=%18.15f ",i,quat_ref[i]) ;              
+
+      /* determine the value of the tracking flags and identify which quaternians to use */
+
+	 for (i=0; i<npts ; i++) {
+           if (fq1[i] > -1 && fq2[i] > -1 && qvalid[i] > 0) {
+             dq1[i] = fq1[i] ; 
+             dq2[i] = fq2[i] ;
+             dq3[i] = fq3[i] ;
+             if (sfknwn[i] == 1 && aattflg[i] == 5) trakflg[i] = (short) 5 ;
+             if (sfknwn[i] == 0 && aattflg[i] == 5) trakflg[i] = (short) 4 ; 
+             if (aattflg[i] == 4) trakflg[i] = (short) 3 ; }
+	   else if (aq1[i] > -1 && aq2[i] > -1 ) {
+             dq1[i] = aq1[i] ;
+             dq2[i] = aq2[i] ;
+             dq3[i] = aq3[i] ;
+             if(aattflg[i] == 4) trakflg[i] = (short) 2 ;
+             if(aattflg[i] == 3) trakflg[i] = (short) 1 ;}
+           else {
+             dq1[i] = -10. ;
+             dq2[i] = -10. ;
+             dq3[i] = -10. ; 
+             trakflg[i]= (short) 0 ; }
+       	   }
+
+
+      /* determine the shift in the quaturnians and derive the changes
+	 in x and y which they represent :
+           DX (from q2 values : dq2=dx/2) and DY (from q1 values : dq1=-dy/2)
+           in arcseconds - the conversion factor used is the number of arcsec
+            per radian * 2 */
+       for (i=0l ; i<npts ; i++) {
+	 if (trakflg[i] > 0) {
+            tquat[0] = dq1[i] ;
+            tquat[1] = dq2[i] ;
+            tquat[2] = dq3[i] ;
+            tquat[3] = sqrt(1. - dq1[i]*dq1[i] - dq2[i]*dq2[i] - dq3[i]*dq3[i] ) ;
+
+	  /* initialize dquat */
+	    for (j=0; j<4 ; j++) dquat[j]=0. ;
+
+ 	  /* now determine the change in quat */
+	     quatprod(tquat, quat_ref, dquat) ;
+
+ 	  /* convert of arcsec in x and y */
+ 	    dy[i] = (float) -dquat[0] * 412541. ;
+	    dx[i] = (float) dquat[1] * 412541. ; } 
+	 else {
+	    dx[i] = -999. ;
+            dy[i] = -999. ; }
+    }
+
+/****** provide keywords in the top level header which describe the observations ****/
+
+    /* determine the time span in the jitter file (in seconds) and set EXP_DUR to
+        this value  */
+       expdur = (float) (time[npts-1] - time[0]) + 1. ;
+       FITS_update_key(outfits, TFLOAT, "EXP_DUR", &expdur, 
+         "duration of jitter data (sec)", &status) ;
+
+       /* check for a short exposure and reset exptime if necessary */
+       if (time[npts-1] < exptime) {
+	 exptime = time[npts-1] ;
+         cf_verbose(2,"short exposure- reset exptime to %f ",exptime) ;
+       }
+
+	 /* determine the statistics of the guiding */
+         numq4=0 ;
+         numq5=0 ;
+         numq3=0 ;
+         numq2=0 ;
+         numqa=0 ;
+         numq0=0 ;
+	 cf_verbose(3,"exposure duration = %f ",expdur) ;
+
+	 for (i=0; i<npts ; i++) {
+	   cf_verbose(6,"at i=%d, trakflg=%d, qvalid=%d, time=%f ",
+	      i,trakflg[i], qvalid[i], time[i] ) ;
+           if(trakflg[i] == 5 && qvalid[i] > 0 && time[i] > 0 && time[i] <= exptime) 
+                   numq5+=1 ;
+           if(trakflg[i] == 4 && time[i] > 0 && time[i] <= exptime) numq4+=1 ;
+           if(trakflg[i] == 3 && time[i] > 0 && time[i] <= exptime) numq3+=1 ;
+           if(trakflg[i] == 2 && time[i] > 0 && time[i] <= exptime) numq2+=1 ;
+           if(trakflg[i] == 1 && time[i] > 0 && time[i] <= exptime) numqa+=1 ;
+           if(trakflg[i] == 0 && time[i] > 0 && time[i] <= exptime) numq0+=1 ; }
+
+         cf_verbose(3," ") ;
+         cf_verbose(3,"duration of jitter data =%f, exposure time = %f ",expdur,exptime) ;
+	 cf_verbose(3,"number of samples in fine track with known GS = %d ",numq5) ;
+	 cf_verbose(3,"number of samples in fine track with unknown GS = %d ",numq4) ;
+         cf_verbose(3,"number of samples in coarse track = %d ",numq3) ;
+         cf_verbose(3,"number of samples using ACS quaternians = %d ",numq2) ;
+         cf_verbose(3,"number of samples with no quaternians = %d ",numq0) ;
+
+
+       /* tfine, tcoarse and tnull are the fraction of the total exposure
+          when the observation is in fine track, coarse track and no track */
+       tfine = (float) (numq5+numq4) /  exptime ;
+       tcoarse = (float) (numq3+numq2+numqa) /  exptime ;
+       tnull = (float) numq0 /  exptime ;
+       FITS_update_key(outfits, TFLOAT, "FINE_GDE", &tfine, 
+           "fraction of exp in fine guide", &status) ;
+       FITS_update_key(outfits, TFLOAT, "COARSGDE", &tcoarse, 
+           "fraction of exp in coarse guide", &status) ;
+       FITS_update_key(outfits, TFLOAT, "NOGDEINF", &tnull, 
+           "fraction of exp with no guiding info", &status) ;
+
+       /* determine the properties of the guide stars */
+       ngs1=0. ;
+       ngs2=0. ;
+       ngs3=0. ;
+       ngs4=0. ;
+       ngs5=0. ;
+       ngs6=0. ;
+       for (i=0; i<npts ; i++) {
+         if (cents1[i] == 2 && time[i] > 0 && time[i] <= exptime) ngs1+=1. ;
+         if (cents2[i] == 2 && time[i] > 0 && time[i] <= exptime) ngs2+=1. ;
+         if (cents3[i] == 2 && time[i] > 0 && time[i] <= exptime) ngs3+=1. ;
+         if (cents4[i] == 2 && time[i] > 0 && time[i] <= exptime) ngs4+=1. ;
+         if (cents5[i] == 2 && time[i] > 0 && time[i] <= exptime) ngs5+=1. ;
+         if (cents6[i] == 2 && time[i] > 0 && time[i] <= exptime) ngs6+=1. ; }
+       /* convet to fraction of observing time and put into keywords */
+       ngs1 = ngs1 / exptime ;
+        FITS_update_key(outfits, TFLOAT, "GS1_USED", &ngs1, 
+           "fraction of exp using guide star 1", &status) ;
+       ngs2 = ngs2 / exptime ;
+        FITS_update_key(outfits, TFLOAT, "GS2_USED", &ngs2, 
+           "fraction of exp using guide star 2", &status) ;
+       ngs3 = ngs3 / exptime ;
+        FITS_update_key(outfits, TFLOAT, "GS3_USED", &ngs3, 
+           "fraction of exp using guide star 3", &status) ;
+       ngs4 = ngs4 / exptime ;
+        FITS_update_key(outfits, TFLOAT, "GS4_USED", &ngs4, 
+           "fraction of exp using guide star 4", &status) ;
+       ngs5 = ngs5 / exptime ;
+        FITS_update_key(outfits, TFLOAT, "GS5_USED", &ngs5, 
+           "fraction of exp using guide star 5", &status) ;
+       ngs6 = ngs6 / exptime ;
+        FITS_update_key(outfits, TFLOAT, "GS6_USED", &ngs6, 
+           "fraction of exp using guide star 6", &status) ;
+
+	/* determine the number of guide stars used during the observation */
+	ngs_used = 0 ;
+	if (ngs1 > 0) ngs_used += 1 ; 
+	if (ngs2 > 0) ngs_used += 1 ; 
+	if (ngs3 > 0) ngs_used += 1 ; 
+	if (ngs4 > 0) ngs_used += 1 ; 
+	if (ngs5 > 0) ngs_used += 1 ; 
+	if (ngs6 > 0) ngs_used += 1 ; 
+        FITS_update_key(outfits, TINT, "NGS_USED", &ngs_used, 
+           "number of guide stars used", &status) ;
+        cf_verbose(3," ") ;
+	cf_verbose(3,"number of guide stars used = %d \n",ngs_used) ;
+
+
+	/* determine times of known and unknown tracking and tracking on the target*/ 
+	knowntrk = 0. ;
+        unknowntrk = 0. ;
+        targtrk = 0. ;
+        gs_used = 0. ;
+	for (i=0 ; i< npts ; i++) {
+          if (qvalid[i] == 1 && time[i] > 0 && time[i] <= exptime) gs_used+=1. ;
+          if (sfknwn[i] == 1 && qvalid[i] ==1 && time[i] > 0 && time[i] <= exptime) 
+                knowntrk+=1. ;
+          if (sfknwn[i] == 0 && qvalid[i] ==1 && time[i] > 0 && time[i] <= exptime) 
+                unknowntrk+=1. ; 
+          if (sfknwn[i] == 1 && acsflg[i] == 1 && time[i] > 0 && time[i] <= exptime)
+	    targtrk += 1. ;
+     }
+
+	/* check for digitization errors in targtrk (caused by the 16s cadence of acsflg) */
+	if (targtrk+16 > exptime) targtrk = exptime ;
+
+        cf_verbose(3,"seconds when guide stars are used = %f",gs_used ) ;
+        cf_verbose(3,"seconds tracking on known stars = %f ",knowntrk) ;
+        cf_verbose(3,"seconds tracking on unknown stars = %f ",unknowntrk) ;
+        cf_verbose(3,"seconds tracking on the target = %f ",targtrk ) ;
+	knowntrk = knowntrk /  exptime ;
+	unknowntrk = unknowntrk / exptime ;
+        targtrk = targtrk / exptime ;
+        gs_used = gs_used / exptime ;
+         FITS_update_key(outfits, TFLOAT, "KNOWNTRK", &knowntrk, 
+            "fraction of exp tracking on known stars", &status) ;
+         FITS_update_key(outfits, TFLOAT, "UNKWNTRK", &unknowntrk, 
+            "fraction of exp tracking on unknown stars", &status) ;
+        FITS_update_key(outfits, TFLOAT, "TARGTRK", &targtrk, 
+            "fraction of exp tracking on target", &status) ;
+        FITS_update_key(outfits, TFLOAT, "GS_INUSE", &gs_used, 
+            "fraction of exp tracking on guide stars", &status) ;
+
+
+	/* determine whether a new attitude is commanded during the exposure */
+        slewflg = -1 ;
+	for (i=0; i<npts ; i++) 
+          if(time[i] > 0 && slew[i] > 0 && time[i] <= exptime) slewflg = 1 ;
+        FITS_update_key(outfits, TINT, "SLEWFLG", &slewflg, 
+            "slew commanded during obs (if > 0)", &status) ;
+        if (slewflg > 0) {
+	  cf_verbose(1," ") ;
+          cf_verbose(1,"SLEW COMMANDED DURING OBSERVATION!!! ") ; }
+
+	/* determine the slewing time - note that there is a 16s time
+           resolution on the sampling of acsflg. Thus, slews of less than 16s
+           are not real */
+        slewtime=0 ;
+        FITS_update_key(outfits, TINT, "SLEWTIME", &slewtime, 
+            "time spent slewing (sec)", &status) ;
+
+        for (i=0; i<npts; i++) 
+	  if (acsflg[i] < 1 && time[i] > 0 && time[i] <= exptime ) slewtime+=1 ;
+        if (slewtime > 16) {
+             FITS_update_key(outfits, TINT, "SLEWTIME", &slewtime, 
+                "time spent slewing (sec)", &status) ;
+             slewflg=1 ;
+             FITS_update_key(outfits, TINT, "SLEWFLG", &slewflg, 
+                "slew commanded during obs (if > 0)", &status) ;
+             cf_verbose(3,"SLEW OCCURRED DURING OBSERVATION!!! ") ;
+             cf_verbose(3,"Time (sec) spent slewing = %d \n",slewtime) ;
+	} 
+
+	/* determine basic properties of the jitter 
+            - these properties are only determined during the time of the exposure where the 
+              spacecraft is guiding on the target */
+	dxrms = 0. ;
+        dxrms5 = 0. ;
+        dyrms = 0. ;
+        dyrms5 = 0. ;
+        dxave = 0. ;
+        dyave = 0. ;
+        nvalid = 0 ;
+        nvalid5 = 0 ;
+	for (i=0 ; i< npts ; i++) 
+	  if(sfknwn[i] == 1 && acsflg[i] == 1 && time[i] > qtime  && time[i] <= exptime) {
+            nvalid += 1 ;
+            dxrms = dxrms + dx[i]*dx[i]  ;
+            dxave = dxave + dx[i] ;
+            dyrms = dyrms + dy[i] * dy[i] ;
+            dyave = dyave + dy[i] ;
+            if (time[i] > exptime -  300) {
+              dxrms5 = dxrms5 + dx[i] * dx[i] ;
+              dyrms5 =dyrms5 + dy[i] * dy[i] ;
+              nvalid5 += 1 ; }
+	  }
+        cf_verbose(3,"number of points used to determine rms jitter = %d ",nvalid) ;
+  
+	if (nvalid > 0) dxrms = sqrt( dxrms / (float) nvalid) ;
+	if (nvalid > 0) dyrms = sqrt( dyrms / (float) nvalid) ;
+	if (nvalid5 > 0) dxrms5 = sqrt( dxrms5 / (float) nvalid5) ;
+	if (nvalid5 > 0) dyrms5 = sqrt( dyrms5 / (float) nvalid5) ;
+        if (nvalid > 0) dxave = dxave / (float) nvalid ;
+        if (nvalid > 0) dyave = dyave / (float) nvalid ;
+        cf_verbose(3," ") ;
+        cf_verbose(3,"jitter properties ") ;
+	cf_verbose(3,"dxave = %f, dxrms=%f, dxrms5 = %f ", dxave, dxrms, dxrms5) ;
+	cf_verbose(3,"dyave = %f, dyrms=%f, dyrms5 = %f ", dyave, dyrms, dyrms5) ;
+          FITS_update_key(outfits, TFLOAT, "POSAVG_X", &dxave, 
+            "[arcsec] mean DX during exposure", &status) ;
+          FITS_update_key(outfits, TFLOAT, "POSAVG_Y", &dyave, 
+            "[arcsec] mean DY during exposure", &status) ;
+
+          FITS_update_key(outfits, TFLOAT, "X_JITTER", &dxrms, 
+            "[arcsec] sigma of DX during exposure", &status) ;
+          FITS_update_key(outfits, TFLOAT, "Y_JITTER", &dyrms, 
+            "[arcsec] sigma of DY during exposure", &status) ;
+
+          FITS_update_key(outfits, TFLOAT, "X_JIT_5M", &dxrms5, 
+            "[arcsec] sigma of DX during last 5 min of exp", &status) ;
+          FITS_update_key(outfits, TFLOAT, "Y_JIT_5M", &dyrms5, 
+            "[arcsec] sigma of DY during last 5 min of exp", &status) ;
+
+  /* determine fraction of exposure where the dy and dx values exceed 2 
+     sigma from the mean */
+          jitlgx=0 ;
+          jitlgy=0 ;
+	  for (i=0 ; i<npts ; i++) {
+            if ( fabs(dx[i]) > 2.*dxrms) jitlgx++ ;
+            if ( fabs(dy[i]) > 2.*dyrms) jitlgy++ ;
+		}
+
+	  fjitlgx= (float) jitlgx / (float) npts ;
+	  fjitlgy = (float) jitlgy / (float) npts ;
+
+          FITS_update_key(outfits, TFLOAT, "X_JITLRG", &fjitlgx, 
+            "frac of DX more than 2-sigma from POSAVE_X", &status) ;
+          FITS_update_key(outfits, TFLOAT, "Y_JITLRG", &fjitlgy, 
+            "frac of DY more than 2-sigma from POSAVE_Y", &status) ;
+
+
+
+  /******* Generate the table and put in guiding info *****/
+  
+      tfields = 4 ; 
+  	 FITS_create_tbl(outfits, BINARY_TBL, 0, tfields, ttype,
+		  tform, tunit, textname, &status) ;
+
+      fits_get_colnum(outfits, TRUE, "TIME", &tcol, &status) ;
+      FITS_write_col(outfits, TLONG, tcol, 1, 1, npts, time, &status) ;
+      fits_get_colnum(outfits, TRUE, "DX", &dxcol, &status) ;
+      FITS_write_col(outfits, TFLOAT, dxcol, 1, 1, npts, dx, &status) ;
+      fits_get_colnum(outfits, TRUE, "DY", &dycol, &status) ;
+      FITS_write_col(outfits, TFLOAT, dycol, 1, 1, npts, dy, &status) ;
+      fits_get_colnum(outfits, TRUE, "TRKFLG", &trkcol, &status) ;
+      FITS_write_col(outfits, TSHORT, trkcol, 1, 1, npts, trakflg, &status) ;
+
+
+ /**********************************************************************/
+
+      /* set the status flag as good */
+       FITS_movabs_hdu(outfits, 1, &hdutype, &status) ;
+       dstatus = 0 ;
+       FITS_update_key(outfits, TINT, "JIT_STAT", &dstatus, 
+            "status of jitter data is good", &status) ;
+
+      /* close the output file */
+    FITS_close_file(outfits, &status) ; 
+
+    /* free up storage space */
+    free(mjd) ;
+    free(fpdexp) ;
+    free(qvalid) ;
+    free(fq1) ;
+    free(fq2) ;
+    free(fq3) ;
+    free(aq1) ;
+    free(aq2) ;
+    free(aq3) ;
+    free(aattflg) ;
+    free(acscmd1) ;
+    free(acscmd2) ;
+    free(acscmd3) ;
+    free(time) ;
+    free(trakflg) ;
+    free(dq1) ;
+    free(dq2) ;
+    free(dq3) ;
+    free(dx) ;
+    free(dy) ;
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished execution.");
+
+    return 0 ;
+
+} 
+
+
+/* procedure to do a matrix multiplication of two quaturnians to determine
+   the displacement of a measured value from a reference */
+ 
+int quatprod(double *tquat, double *quat_ref, double *dquat) {
+
+  int i, j ;
+  double multmat[4][4], qinv[4] ; 
+
+  /* fill in the array with values from the tquat vector */
+  multmat[0][0] =  tquat[3] ;
+  multmat[0][1] = -tquat[2] ;
+  multmat[0][2] =  tquat[1] ;
+  multmat[0][3] = -tquat[0] ;
+  multmat[1][0] =  tquat[2] ;
+  multmat[1][1] =  tquat[3] ;
+  multmat[1][2] = -tquat[0] ;
+  multmat[1][3] = -tquat[1] ;
+  multmat[2][0] = -tquat[1] ; 
+  multmat[2][1] =  tquat[0] ;
+  multmat[2][2] =  tquat[3] ;
+  multmat[2][3] = -tquat[2] ;
+  multmat[3][0] =  tquat[0] ;
+  multmat[3][1] =  tquat[1] ;
+  multmat[3][2] =  tquat[2] ;
+  multmat[3][3] =  tquat[3] ;
+  
+
+  /* specify the inverse of quat_ref */
+  qinv[0] = -quat_ref[0] ;
+  qinv[1] = -quat_ref[1] ;
+  qinv[2] = -quat_ref[2] ;
+  qinv[3] =  quat_ref[3] ;
+ 
+  /* do the matrix multiplication */
+  for (i=0 ; i<4 ; i++) {
+    dquat[i] = 0. ;
+     for (j=0; j<4 ; j++) dquat[i] = dquat[i] + multmat[j][i]*qinv[j] ; 
+}
+
+  return 0 ;
+
+}
diff --git a/src/cal/parm/Makefile.orig.orig b/src/cal/parm/Makefile.orig.orig
new file mode 100644
index 0000000..c0d69c1
--- /dev/null
+++ b/src/cal/parm/Makefile.orig.orig
@@ -0,0 +1,52 @@
+VERSION=	v1.8
+
+CALFUSEDIR=	$(PWD)/../../..
+
+# Symbols for include directories
+FUSEINCLDIR=	$(CALFUSEDIR)/include
+
+# Symbols used for creating shared libraries
+O=		.a
+LDSTATIC=	ld
+
+# Symbols used for creating shared libraries
+SO=		.so
+LDSHARED=	ld
+CCSHARED=	-G
+
+# Symbols used for compiling
+CC=		cc
+#  Romelfanger's optimizations
+# OPT=		-fast -xO5 -xtarget=ultra2 -xarch=v8plusa
+#
+#  SunWorld's optimizations
+# OPT=		-p -v -xO2 -xdepend -xchip=ultra -xarch=generic
+OPT=		-O -KPIC -DSOLARIS -DCFORTRAN
+CFLAGS=		$(OPT) -I$(FUSEINCLDIR)
+
+# Symbols used for creating shared binaries
+FUSELIBDIR=	$(CALFUSEDIR)/lib
+FUSEBINDIR=	$(CALFUSEDIR)/bin
+LIBDIR=		/opt/SUNWspro/lib
+#FUSELIBS=	-lcf -lsla -lcalfits -lcfitsio
+FUSELIBS=	-lsla -lcfitsio -lcf
+LIBS=		-lsocket -lnsl -ldl -lsunmath -lm -lc -lM77 -lF77
+LDFLAGS=	
+
+# binaries to be made
+
+BINS=		make_parm_file
+
+all:		$(BINS)
+		chmod g+rw $(BINS)
+
+install:	all
+		/bin/cp $(BINS) $(FUSEBINDIR)
+
+clean:		
+		/bin/rm -f $(BINS)
+
+make_parm_file:
+		$(CC) $(CFLAGS) -o make_parm_file make_parm_file.c \
+		-L$(FUSELIBDIR) -L$(LIBDIR) $(FUSELIBS) $(LIBS) $(LDFLAGS)
+
diff --git a/src/cal/parm/make_parm_file.c b/src/cal/parm/make_parm_file.c
new file mode 100644
index 0000000..9b224da
--- /dev/null
+++ b/src/cal/parm/make_parm_file.c
@@ -0,0 +1,109 @@
+/*******************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *******************************************************************************
+ *
+ * Synopsis:    make_screen_file
+ *
+ * Description: Make the screening parameters file.
+ *
+ * History:     07/14/98        emm     Begin work.
+ *              07/08/99        peb     Added PHAMIN and PHAMAX keywords.
+ *              07/29/99        emm     Added SAA_SCR and LIMB_SCR keywords
+ ******************************************************************************/
+
+#include <stdio.h>
+#include "calfuse.h"
+#define VERSION 3
+#define EFFMJD 50000.0
+
+int main()
+{
+char *channel[]={"LiF","SiC"};
+char *segment[]={"1A","1B","2A","2B"};
+char *segments[]={"1a","1b","2a","2b"};
+char *aperture[]={"HIRS","MDRS","LWRS","PINH"};
+char dummy[30];
+char extname[]="PARAMETER FILE";
+char filename[80];
+
+
+    int   i, status=0, vers;
+    long  numbl, dumar[2]={0, 0};
+    float numb, effmjd;
+    fitsfile *parmfits;
+
+for (i=0; i<4; i++) {  /* 1A,1B,2A,2B */
+
+    sprintf(filename,"parm%2.2s%03d.fit", segments[i],VERSION);
+    printf("%20.20s\n",filename); 
+
+    FITS_create_file(&parmfits,filename,&status);
+    FITS_create_img(parmfits, SHORT_IMG, 0, dumar, &status);
+
+    FITS_write_key(parmfits, TSTRING, "CALFTYPE", "PARM", 
+		   "Calibration file type", &status);
+
+    vers=VERSION;
+    FITS_write_key(parmfits,TINT,"CALFVERS",&vers,
+		   "Calibration file version", &status);
+
+    FITS_write_key(parmfits,TSTRING,"DETECTOR",segment[i],
+                   "detector (1A, 1B, 2A, 2B", &status);
+
+    effmjd=EFFMJD;
+    FITS_write_key(parmfits,TFLOAT,"EFFMJD",&effmjd,
+		   "Date on which file should be applied (MJD)", &status);
+
+    FITS_write_date(parmfits, &status);
+
+    FITS_write_key(parmfits,TSTRING,"AUTHOR","EDWARD MURPHY",
+		   "Author of file", &status);
+
+    FITS_write_comment(parmfits, "  ", &status);
+    FITS_write_comment(parmfits, "The SPEX_SIC and SPEX_LIF keywords allow "
+        "the user to center the extraction windows along a given row rather "
+        "than having the pipeline try to centroid the spectrum.  A number "
+        "less than 0 or greater than 1023 will default to pipeline "
+        "centroiding.  A value between 0 and 1023 will define the center "
+        "of the extraction window.  Since the pipeline expands histogram "
+        "images out to 1023 pixels in Y, the number must be given for a "
+        "full 1023 image height.  That is, if the center is determined "
+        "from binned images, the center must be multiplied by the binning "
+        "factor before entering it in this file.", &status);
+    FITS_write_comment(parmfits, "  ", &status);
+
+    numbl = -1;
+    FITS_write_key(parmfits, TLONG, "SPEX_SIC",&numbl,
+		   "SiC extraction window Y center (0-1023)", &status);
+
+    numbl = -1;
+    FITS_write_key(parmfits, TLONG, "SPEX_LIF",&numbl,
+		   "LiF extraction window Y center (0-1023)", &status);
+
+    FITS_write_comment(parmfits, "  ", &status);
+    FITS_write_comment(parmfits, "The EMAX_SIC and EMAX_LIF keywords allow "
+        "the user to limit the amount that the pipeline can shift the "
+        "extraction windows based on the centroid of the spectrum.  In "
+        "cases where the source is very faint, the centroid routine "
+        "may find bright detector artifacts or other apertures instead "
+        "of the desired aperture.  If the calculated centroid differs from "
+        "the predicted centroid by more than EMAX_SIC or EMAX_LIF, the "
+        "pipeline uses the default extraction window location.", &status);
+    FITS_write_comment(parmfits, "  ", &status);
+
+    numbl = 20;
+    FITS_write_key(parmfits, TLONG, "EMAX_SIC",&numbl,
+		   "SiC extraction window maximum Y movement", &status);
+
+    numbl = 20;
+    FITS_write_key(parmfits, TLONG, "EMAX_LIF",&numbl,
+		   "LiF extraction window maximum Y movement", &status);
+
+    FITS_close_file(parmfits, &status);
+
+}
+
+    return 0;
+}
diff --git a/src/cal/saa/Makefile.orig.orig b/src/cal/saa/Makefile.orig.orig
new file mode 100644
index 0000000..09b0736
--- /dev/null
+++ b/src/cal/saa/Makefile.orig.orig
@@ -0,0 +1,19 @@
+CFDIR = /usr/local/fusesw/calfuse/v1.2
+BIN = ${CFDIR}/bin
+CC = cc
+CFLAGS = -v -xO2 -I${CFDIR}/include -I/usr/local/include 
+LIBS = -L${CFDIR}/lib -lcf -L/usr/local/lib -lcfitsio -lm -lsocket -lnsl
+
+#       -  <<-- ignore error code
+
+all: make_saa_file
+
+make_saa_file:   make_saa_file.o
+	${CC} $(CFLAGS) -o make_saa_file make_saa_file.o \
+	$(LIBS)
+
+clean:
+	-	/bin/rm -f *.o make_saa_file
+
+install:	all
+	-	/bin/cp make_saa_file 	${BIN}/make_saa_file
diff --git a/src/cal/saa/make_saa_file.c b/src/cal/saa/make_saa_file.c
new file mode 100644
index 0000000..2f0df04
--- /dev/null
+++ b/src/cal/saa/make_saa_file.c
@@ -0,0 +1,81 @@
+/*******************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *******************************************************************************
+ *
+ * Synopsis:    saa output_file
+ *
+ * Description: Writes a FITS ASCII table with the SAA contours.
+ *              
+ *
+ * History:     07/21/98  E. Murphy   Begin work.
+ *
+ * References:  SAA contours from Scott Friedman 07/16/98, same contours as
+ *              used in SPIKE.  Note that the contours do not extend below
+ *              a latitude of 30 degrees.
+ *
+ ******************************************************************************/
+
+#include <stdio.h>
+#include <math.h>
+#include "calfuse.h"
+ 
+#define VERSION 2
+#define EFFMJD 50000.0
+
+int main(int argc, char *argv[])
+
+{
+
+/* Define variables. */
+int i, retcode, status=0, anynull, hdutype;
+int numlimits=10;
+double maxlat, maxlon, minlon, delta;
+int nrows=10;
+int tfields=3;
+float saa_lat[10]=   {-30.0,-25.0, -20.0, -15.0,-10.0,  0.0,  5.0,  10.0, 12.0, 13.0};
+float saa_minlon[10]={-91.0,-98.0,-102.0,-100.0,-93.0,-68.3,-56.0, -42.0,-32.0,-27.0};
+float saa_maxlon[10]={ 24.1, 47.0,  41.0,  33.0, 25.0,  8.0, -3.0, -14.0,-20.0,-27.0};
+float floatnull;
+fitsfile *outfits, *infits;
+long dumar[2]={0,0};
+char extname[]="SAA_CONTOURS";
+char *ttype[]={"LATITUDE","MIN_LONGITUDE","MAX_LONGITUDE"};
+char *tform[]={"F8.3","F8.3","F8.3"};
+char *tunit[]={"deg","deg","deg"};
+int  vers;
+float effmjd;
+
+FITS_create_file(&outfits, "saac002.fit", &status);
+
+FITS_create_img(outfits, SHORT_IMG, 0, dumar, &status);
+
+     FITS_write_key(outfits, TSTRING, "CALFTYPE", "SAAC", 
+                    "Calibration file type", &status);
+
+     vers=VERSION;
+     FITS_write_key(outfits,TINT,"CALFVERS",&vers,
+                    "Calibration file version", &status);
+
+     effmjd=EFFMJD;
+     FITS_write_key(outfits,TFLOAT,"EFFMJD",&effmjd,
+                    "Date on which file should be applied (MJD)", &status);
+
+     FITS_write_date(outfits, &status);
+
+     FITS_write_key(outfits,TSTRING,"AUTHOR","EDWARD MURPHY",
+                    "Author of file", &status);
+
+FITS_create_tbl(outfits, ASCII_TBL, nrows, tfields, ttype, tform, tunit, 
+extname, &status);
+
+FITS_write_col(outfits, TFLOAT, 1, 1, 1, nrows, saa_lat, &status);
+FITS_write_col(outfits, TFLOAT, 2, 1, 1, nrows, saa_minlon, &status);
+FITS_write_col(outfits, TFLOAT, 3, 1, 1, nrows, saa_maxlon, &status);
+
+FITS_close_file(outfits, &status);
+
+return 0;
+
+}
diff --git a/src/cal/screen/Makefile.orig.orig b/src/cal/screen/Makefile.orig.orig
new file mode 100644
index 0000000..7579595
--- /dev/null
+++ b/src/cal/screen/Makefile.orig.orig
@@ -0,0 +1,28 @@
+VERSION=	v1.7
+
+CFDIR=		/usr/local/fusesw/calfuse/$(VERSION)
+BIN=		${CFDIR}/bin
+FITSINCLDIR=	/usr/local/include
+FUSEINCLDIR=	$(CFDIR)/include
+CC=		cc
+OPT=		-O -KPIC
+CFLAGS=		$(OPT) -I${FUSEINCLDIR} -I$(FITSINCLDIR)
+
+LDSHARED=	ld
+FUSELIBDIR=	$(CFDIR)/lib
+FUSELIBS=	-lcf -lsla -lcalfits -lcfitsio
+LIBS=		-lm -lsocket -lnsl -ldl
+
+#       -  <<-- ignore error code
+
+all:		make_screen_file
+
+make_screen_file:
+		${CC} $(CFLAGS) -o make_screen_file make_screen_file.c \
+		-L$(FUSELIBDIR) $(FUSELIBS) $(LIBS) $(LDFLAGS)
+
+clean:
+	-	/bin/rm -f *.o make_screen_file
+
+install:	all
+	-	/bin/cp make_screen_file 	${BIN}/make_screen_file
diff --git a/src/cal/screen/make_screen_file b/src/cal/screen/make_screen_file
new file mode 100755
index 0000000..ae0f83b
--- /dev/null
+++ b/src/cal/screen/make_screen_file
diff --git a/src/cal/screen/make_screen_file.c b/src/cal/screen/make_screen_file.c
new file mode 100644
index 0000000..01b41da
--- /dev/null
+++ b/src/cal/screen/make_screen_file.c
@@ -0,0 +1,122 @@
+/*******************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *******************************************************************************
+ *
+ * Synopsis:    make_screen_file
+ *
+ * Description: Make the screening parameters file.
+ *
+ * History:     07/14/98        emm     Begin work.
+ *              07/08/99        peb     Added PHAMIN and PHAMAX keywords.
+ *              07/29/99        emm     Added SAA_SCR and LIMB_SCR keywords
+ ******************************************************************************/
+
+#include <stdio.h>
+#include "calfuse.h"
+#define VERSION 3
+#define EFFMJD 50000.0
+
+int main()
+{
+char *channel[]={"LiF","SiC"};
+char *segment[]={"1A","1B","2A","2B"};
+char *segments[]={"1a","1b","2a","2b"};
+char *aperture[]={"HIRS","MDRS","LWRS","PINH"};
+char dummy[30];
+char extname[]="SCREENING PARAMETERS";
+char filename[80];
+
+
+    int   i, status=0, vers;
+    long  numbl, dumar[2]={0, 0};
+    float numb, effmjd;
+    fitsfile *parmfits;
+
+for (i=0; i<4; i++) {  /* 1A,1B,2A,2B */
+
+    sprintf(filename,"scrn%2.2s%03d.fit", segments[i],VERSION);
+    printf("%20.20s\n",filename); 
+
+    FITS_create_file(&parmfits,filename,&status);
+    FITS_create_img(parmfits, SHORT_IMG, 0, dumar, &status);
+
+    FITS_write_key(parmfits, TSTRING, "CALFTYPE", "SCRN", 
+		   "Calibration file type", &status);
+
+    vers=VERSION;
+    FITS_write_key(parmfits,TINT,"CALFVERS",&vers,
+		   "Calibration file version", &status);
+
+    FITS_write_key(parmfits,TSTRING,"DETECTOR",segment[i],
+                   "detector (1A, 1B, 2A, 2B", &status);
+
+    effmjd=EFFMJD;
+    FITS_write_key(parmfits,TFLOAT,"EFFMJD",&effmjd,
+		   "Date on which file should be applied (MJD)", &status);
+
+    FITS_write_date(parmfits, &status);
+
+    FITS_write_key(parmfits,TSTRING,"AUTHOR","EDWARD MURPHY",
+		   "Author of file", &status);
+
+    numb=10.0;
+    FITS_write_key(parmfits,TFLOAT,"TIMESTEP",&numb,
+		   "[sec] Screening time step", &status);
+
+    FITS_write_key(parmfits,TSTRING,"SAA_SCR","ON",
+		   "SAA screening ON/OFF", &status);
+
+    FITS_write_key(parmfits,TSTRING,"LIMB_SCR","ON",
+		   "Limb angle screening ON/OFF", &status);
+
+    FITS_write_key(parmfits,TSTRING,"DAYNIGHT","BOTH",
+		   "Use only DAY, NIGHT or BOTH", &status);
+
+    numbl = 0;
+    FITS_write_key(parmfits, TLONG, "PHALOW",&numbl,
+		   "Minimum acceptable PHA value", &status);
+
+    numbl = 31;
+    FITS_write_key(parmfits, TLONG, "PHAHIGH",&numbl,
+		   "Maximum acceptable PHA value", &status);
+
+    numb = 1.0;
+    FITS_write_key(parmfits, TFLOAT, "PHA_BKGD",&numb,
+		   "Background scaling factor for PHA screening", &status);
+
+    numb=15.0;
+    FITS_write_key(parmfits,TFLOAT,"BRITLIMB",&numb,
+		   "[deg] Bright limb avoidance angle", &status);
+
+    numb=10.0;
+    FITS_write_key(parmfits,TFLOAT,"DARKLIMB",&numb,
+		   "[deg] Dark limb avoidance angle", &status);
+
+    numbl=0;
+    FITS_write_key(parmfits,TLONG,"NUSERGTI",&numbl,
+		   "Number of user defined good time intervals",&status);
+
+    numb=0.0;
+    FITS_write_key(parmfits,TFLOAT,"GTIBEG01",&numb,
+		   "[sec] Beginning good time interval", &status);
+
+    numb=0.0;
+    FITS_write_key(parmfits,TFLOAT,"GTIEND01",&numb,
+		   "[sec] Ending good time interval", &status);
+
+    numb=0.0;
+    FITS_write_key(parmfits,TFLOAT,"GTIBEG02",&numb,
+		   "[sec] Beginning good time interval", &status);
+
+    numb=0.0;
+    FITS_write_key(parmfits,TFLOAT,"GTIEND02",&numb,
+		   "[sec] Ending good time interval", &status);
+
+    FITS_close_file(parmfits, &status);
+
+}
+
+    return 0;
+}
diff --git a/src/configure.linux.orig b/src/configure.linux.orig
new file mode 100755
index 0000000..c8cf8ef
--- /dev/null
+++ b/src/configure.linux.orig
@@ -0,0 +1,68 @@
+#!/bin/sh
+
+echo "***********************************"
+echo "***** Preparing Makefiles *********"
+echo "******** for Linux ****************"
+echo "***********************************"
+
+cp Makefile.Linux Makefile
+cp fuv/Makefile.Linux fuv/Makefile
+cp fes/Makefile.Linux fes/Makefile
+cp analysis/Makefile.Linux analysis/Makefile
+cp libcf/Makefile.Linux libcf/Makefile
+cp cal/jitter/Makefile.Linux cal/jitter/Makefile
+cp slalib/mk.sv slalib/mk
+
+echo "***********************************"
+echo "***** Configuring cfitsio *********"
+echo "***********************************"
+
+
+cd cfitsio
+./configure
+cd ..
+
+echo "***********************************"
+echo "***** Done configuring cfitsio ****"
+echo "***********************************"
+
+FC=""
+for ac_prog in gfortran g77
+do
+# Extract the first word of "$ac_prog", so it can be a program name with args.
+  set dummy $ac_prog; ac_word=$2
+  echo "checking for $ac_word..."  
+  IFS="${IFS= 	}"; ac_save_ifs="$IFS"; IFS=":"
+  ac_dummy="$PATH"
+  for ac_dir in $ac_dummy; do
+    test -z "$ac_dir" && ac_dir=.
+    if test -f $ac_dir/$ac_word; then
+      FC="$ac_prog"
+      break
+    fi
+  done
+  IFS="$ac_save_ifs"
+  if test -n "$FC"; then
+    echo "     yes"
+  else
+    echo "     no"
+  fi
+  test -n "$FC" && break
+done
+test -n "$FC" || FC="nope"
+
+if test $FC = 'nope' ; then
+  echo "Warning: No acceptable fortran compiler was found. Please install one from the GNU compilers."
+  echo "Read INSTALLING_CalFUSEv3.2.1 for details."
+else
+  if test $FC = 'g77' ; then
+    for mk in Makefile fuv/Makefile analysis/Makefile libcf/Makefile cal/jitter/Makefile
+    do
+      mv $mk ${mk}.sv
+      sed -e "s/-lgfortran/-lg2c/g" ${mk}.sv > $mk
+    done  
+    sed -e "s/gfortran/g77/g" slalib/mk.sv > slalib/mk
+  fi 
+  echo
+  echo "Type 'make clean' then 'make -e install'"
+fi
diff --git a/src/configure.linux64.orig b/src/configure.linux64.orig
new file mode 100755
index 0000000..e0c989b
--- /dev/null
+++ b/src/configure.linux64.orig
@@ -0,0 +1,74 @@
+#!/bin/sh
+
+echo "***********************************"
+echo "***** Preparing Makefiles *********"
+echo "******** for Linux 64 *************"
+echo "***********************************"
+
+cp Makefile.Linux64 Makefile
+cp fuv/Makefile.Linux64 fuv/Makefile
+cp fes/Makefile.Linux64 fes/Makefile
+cp analysis/Makefile.Linux64 analysis/Makefile
+cp libcf/Makefile.Linux64 libcf/Makefile
+cp cal/jitter/Makefile.Linux64 cal/jitter/Makefile
+cp slalib/mk.sv slalib/mk
+
+FC=""
+for ac_prog in gfortran g77 
+do
+# Extract the first word of "$ac_prog", so it can be a program name with args.
+  set dummy $ac_prog; ac_word=$2
+  echo "checking for $ac_word..."  
+  IFS="${IFS= 	}"; ac_save_ifs="$IFS"; IFS=":"
+  ac_dummy="$PATH"
+  for ac_dir in $ac_dummy; do
+    test -z "$ac_dir" && ac_dir=.
+    if test -f $ac_dir/$ac_word; then
+      FC="$ac_prog"
+      break
+    fi
+  done
+  IFS="$ac_save_ifs"
+  if test -n "$FC"; then
+    echo "     yes"
+  else
+    echo "     no"
+  fi
+  test -n "$FC" && break
+done
+test -n "$FC" || FC="nope"
+
+if test $FC = 'nope' ; then
+  echo "Warning: No acceptable fortran compiler was found. Please install one from the GNU compilers."
+  echo " Read INSTALLING_CalFUSEv3.2.1 for details."
+else
+  echo "checking for cfitsio..."
+  if ! test -d /usr/include/cfitsio ; then
+    echo "     no"
+    echo ""
+    echo "Warning: CFITSIO was not found in /usr/include"
+    echo " Please install CFITSIO for Linux 64 as explained in the installation notes"
+    echo " If you already did so and still get this message, please copy the cfitsio"
+    echo " repertory in '/usr/include'"
+    echo " If you don't have permission to do so, follow the instructions in the"
+    echo " Installation notes."
+    echo ""
+  else
+    echo "     yes"
+    cp /usr/include/cfitsio/* ../include/
+    cp /usr/include/cfitsio/* ../include/cfitsio/
+
+    if test $FC = 'g77' ; then
+      for mk in Makefile fuv/Makefile analysis/Makefile libcf/Makefile cal/jitter/Makefile
+      do
+        mv $mk ${mk}.sv
+        sed -e "s/-lgfortran/-lg2c/g" ${mk}.sv > $mk
+#cfit	mv $mk ${mk}.sv2
+#cfit	sed -e "s#-lcfitsio#-lcfitsio -L/usr/include/cfitsio/lib#g" ${mk}.sv2 > $mk
+      done  
+      sed -e "s/gfortran/g77/g" slalib/mk.sv > slalib/mk
+    fi 
+    echo
+    echo "Type 'make clean' then 'make -e install'"
+  fi
+fi
diff --git a/src/configure.macosx.orig b/src/configure.macosx.orig
new file mode 100755
index 0000000..e391b24
--- /dev/null
+++ b/src/configure.macosx.orig
@@ -0,0 +1,78 @@
+#!/bin/sh
+
+echo "***********************************"
+echo "***** Preparing Makefiles *********"
+echo "******** for Mac OS X *************"
+echo "***********************************"
+
+cp Makefile.MacOSX Makefile
+cp fuv/Makefile.MacOSX fuv/Makefile
+# cp fes/Makefile.MacOSX fes/Makefile
+cp analysis/Makefile.MacOSX analysis/Makefile
+cp libcf/Makefile.MacOSX libcf/Makefile
+cp cal/jitter/Makefile.MacOSX cal/jitter/Makefile
+cp slalib/mk.sv slalib/mk
+
+echo "***********************************"
+echo "***** Configuring cfitsio *********"
+echo "***********************************"
+
+
+cd cfitsio
+./configure
+cd ..
+
+echo "***********************************"
+echo "***** Done configuring cfitsio ****"
+echo "***********************************"
+echo
+
+FC=""
+for ac_prog in gfortran g77 
+do
+# Extract the first word of "$ac_prog", so it can be a program name with args.
+  set dummy $ac_prog; ac_word=$2
+  echo "checking for $ac_word..."  
+  IFS="${IFS= 	}"; ac_save_ifs="$IFS"; IFS=":"
+  ac_dummy="$PATH"
+  for ac_dir in $ac_dummy; do
+    test -z "$ac_dir" && ac_dir=.
+    if test -f $ac_dir/$ac_word; then
+      FC="$ac_prog"
+      break
+    fi
+  done
+  IFS="$ac_save_ifs"
+  if test -n "$FC"; then
+    echo "     yes"
+  else
+    echo "     no"
+  fi
+  test -n "$FC" && break
+done
+test -n "$FC" || FC="nope"
+
+if test $FC = 'nope' ; then
+  echo "Warning: No acceptable fortran compiler was found. Please install one from the GNU compilers."
+  echo "Read INSTALLING_CalFUSEv3.2.1 for details."
+else
+  if test $FC = 'g77' ; then
+    for mk in Makefile fuv/Makefile analysis/Makefile libcf/Makefile cal/jitter/Makefile
+    do
+      mv $mk ${mk}.sv
+      sed -e "s/-lgfortran/-lg2c/g" ${mk}.sv > $mk
+    done  
+    sed -e "s/gfortran/g77/g" slalib/mk.sv > slalib/mk
+  fi
+  if ! test -d /sw/lib ; then
+    libfort=""
+    test -d /usr/local/lib && libfort="-L\/usr\/local\/lib\/ "
+    for mk in Makefile fuv/Makefile analysis/Makefile libcf/Makefile cal/jitter/Makefile
+    do
+      mv $mk ${mk}.sv2
+      sed -e "s/-L\/sw\/lib\/ /${libfort}/g" ${mk}.sv2 > ${mk}
+    done
+  fi
+  echo
+  echo "Type 'make clean' then 'make -e install'"
+fi
diff --git a/src/configure.solaris.orig b/src/configure.solaris.orig
new file mode 100755
index 0000000..5818ee9
--- /dev/null
+++ b/src/configure.solaris.orig
@@ -0,0 +1,98 @@
+#!/bin/sh
+
+echo "***********************************"
+echo "***** Preparing Makefiles *********"
+echo "******** for Solaris **************"
+echo "***********************************"
+
+cp Makefile.Solaris Makefile
+cp fuv/Makefile.Solaris fuv/Makefile
+cp fes/Makefile.Solaris fes/Makefile
+cp analysis/Makefile.Solaris analysis/Makefile
+cp libcf/Makefile.Solaris libcf/Makefile
+cp cal/jitter/Makefile.Solaris cal/jitter/Makefile
+cp slalib/mk.sv slalib/mk
+
+echo "***********************************"
+echo "***** Configuring cfitsio *********"
+echo "***********************************"
+
+cd cfitsio
+./configure
+cd ..
+
+echo "***********************************"
+echo "***** Done configuring cfitsio ****"
+echo "***********************************"
+
+FC=""
+for ac_prog in f77 g77 gfortran f90 
+do
+# Extract the first word of "$ac_prog", so it can be a program name with args.
+  set dummy $ac_prog; ac_word=$2
+  echo "checking for $ac_word..."  
+  IFS="${IFS= 	}"; ac_save_ifs="$IFS"; IFS=":"
+  ac_dummy="$PATH"
+  for ac_dir in $ac_dummy; do
+    test -z "$ac_dir" && ac_dir=.
+    if test -f $ac_dir/$ac_word; then
+      FC="$ac_prog"
+      break
+    fi
+  done
+  IFS="$ac_save_ifs"
+  if test -n "$FC"; then
+    echo "     yes"
+  else
+    echo "     no"
+  fi
+  test -n "$FC" && break
+done
+test -n "$FC" || FC="nope"
+
+if test $FC = 'nope' ; then
+  echo "Warning: No acceptable fortran 77 compiler was found."
+  echo "Please install one either from the GNU compilers GCC, either from Sun Studio."
+  echo "Read INSTALLING_CalFUSEv3.2.1 for details."
+else
+  FFLAGS="-fno-second-underscore -O -fPIC"
+  if test $FC = 'f90' ; then
+    for mk in Makefile analysis/Makefile cal/jitter/Makefile fes/Makefile
+    do
+      mv $mk ${mk}.sv
+      sed -e "s/-lM77 -lF77/-lfui -lfsu/g" ${mk}.sv > $mk
+    done 
+    FFLAGS="-f77 -ftrap=%none -O -PIC"
+  fi
+  if test $FC = 'gfortran' ; then
+    for mk in Makefile analysis/Makefile cal/jitter/Makefile fes/Makefile
+    do
+      mv $mk ${mk}.sv
+      sed -e "s/-lM77 -lF77/-lgfortran/g" ${mk}.sv > $mk
+    done  
+  fi
+  if test $FC = 'g77' ; then
+    for mk in Makefile analysis/Makefile cal/jitter/Makefile fes/Makefile
+    do
+      mv $mk ${mk}.sv
+      sed -e "s/-lM77 -lF77/-lg2c/g" ${mk}.sv > $mk
+    done  
+  fi
+  if test $FC = 'f77' ; then
+    if f77 2> /dev/null | grep -c f90 ; then
+      for mk in Makefile analysis/Makefile cal/jitter/Makefile fes/Makefile
+      do
+        mv $mk ${mk}.sv
+        sed -e "s/-lM77 -lF77/-lfui -lfsu/g" ${mk}.sv > $mk
+      done  
+    fi
+  else
+    sed -e "s/f77/${FC}/g" slalib/mk.sv > slalib/mk.sv2
+    sed -e "s/FFLAGS='-O -PIC'/FFLAGS='${FFLAGS}'/g" slalib/mk.sv2 > slalib/mk
+    rm -f slalib/mk.sv2
+  fi
+  echo
+  echo "Type 'make clean' then 'make -e install'"
+fi
+
+
diff --git a/src/fes/Makefile.Linux.orig b/src/fes/Makefile.Linux.orig
new file mode 100644
index 0000000..af548ac
--- /dev/null
+++ b/src/fes/Makefile.Linux.orig
@@ -0,0 +1,44 @@
+
+SHARED=		-shared
+FITSVER=	2.470
+CALFUSEDIR=	${PWD}/../..
+
+# Symbols for include directories
+FUSEINCLDIR=    -I${CALFUSEDIR}/include
+
+# Symbols used for compiling
+CC=             cc
+OPT=            -g -Wall -DCFORTRAN -Dg77Fortran -Df2cFortran
+CFLAGS =	${OPT} ${FUSEINCLDIR}
+
+# Symbols used for creating shared binaries
+FUSEBINDIR=     ${CALFUSEDIR}/bin
+FUSELIBDIR=     -L${CALFUSEDIR}/lib
+LIBDIR=         
+FUSELIBS=       -lsla -lcfitsio-${FITSVER} -lcf
+LIBS=           -lc -lm -lnsl -ldl -lgfortran
+LDFLAGS=        -Wl,-R${CALFUSEDIR}/lib
+
+OBJECTS=	cf_calfes.o cf_fes_init.o cf_fes_read.o cf_fes_write.o \
+		cf_fes_cal.o cf_fes_get_cal_image.o cf_limbang.o \
+		cf_fes_apply_bias.o cf_fes_apply_flat.o cf_fes_apply_mask.o 
+
+all:		cf_calfes
+
+cf_calfes:	${OBJECTS}
+		${CC} ${CFLAGS} -o cf_calfes ${OBJECTS} \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+		chmod g+rw cf_calfes
+
+install:	cf_calfes
+		/bin/cp cf_calfes ${FUSEBINDIR}
+
+clean:
+		/bin/rm -f ${OBJECTS} cf_calfes
+
+distclean:
+		/bin/rm -f ${OBJECTS} cf_calfes
+		cd ../../bin; /bin/rm -f cf_calfes
+
+lint:		${SOURCES}
+		lint ${SOURCES}
diff --git a/src/fes/Makefile.Linux64.orig b/src/fes/Makefile.Linux64.orig
new file mode 100644
index 0000000..87e47c2
--- /dev/null
+++ b/src/fes/Makefile.Linux64.orig
@@ -0,0 +1,43 @@
+
+SHARED=		-shared
+CALFUSEDIR=	${PWD}/../..
+
+# Symbols for include directories
+FUSEINCLDIR=    -I${CALFUSEDIR}/include
+
+# Symbols used for compiling
+CC=             cc
+OPT=            -g -Wall -DCFORTRAN -Dg77Fortran -Df2cFortran
+CFLAGS =	${OPT} ${FUSEINCLDIR}
+
+# Symbols used for creating shared binaries
+FUSEBINDIR=     ${CALFUSEDIR}/bin
+FUSELIBDIR=     -L${CALFUSEDIR}/lib
+LIBDIR=         
+FUSELIBS=       -lsla -lcf
+LIBS=           -lc -lm -lnsl -ldl -lgfortran -lcfitsio
+LDFLAGS=        -Wl,-R${CALFUSEDIR}/lib
+
+OBJECTS=	cf_calfes.o cf_fes_init.o cf_fes_read.o cf_fes_write.o \
+		cf_fes_cal.o cf_fes_get_cal_image.o cf_limbang.o \
+		cf_fes_apply_bias.o cf_fes_apply_flat.o cf_fes_apply_mask.o 
+
+all:		cf_calfes
+
+cf_calfes:	${OBJECTS}
+		${CC} ${CFLAGS} -o cf_calfes ${OBJECTS} \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+		chmod g+rw cf_calfes
+
+install:	cf_calfes
+		/bin/cp cf_calfes ${FUSEBINDIR}
+
+clean:
+		/bin/rm -f ${OBJECTS} cf_calfes
+
+distclean:
+		/bin/rm -f ${OBJECTS} cf_calfes
+		cd ../../bin; /bin/rm -f cf_calfes
+
+lint:		${SOURCES}
+		lint ${SOURCES}
diff --git a/src/fes/Makefile.Solaris.orig b/src/fes/Makefile.Solaris.orig
new file mode 100644
index 0000000..23f189b
--- /dev/null
+++ b/src/fes/Makefile.Solaris.orig
@@ -0,0 +1,44 @@
+
+SHARED=		-shared
+FITSVER=	2.470
+CALFUSEDIR=	${PWD}/../..
+
+# Symbols for include directories
+FUSEINCLDIR=    -I${CALFUSEDIR}/include
+
+# Symbols used for compiling
+CC=             cc
+OPT=            -O -DCFORTRAN -KPIC -DSOLARIS
+CFLAGS =	${OPT} ${FUSEINCLDIR}
+
+# Symbols used for creating shared binaries
+FUSEBINDIR=     ${CALFUSEDIR}/bin
+FUSELIBDIR=     -L${CALFUSEDIR}/lib
+LIBDIR=         -L/opt/SUNWspro/lib
+FUSELIBS=       -lsla -lcfitsio-${FITSVER} -lcf
+LIBS=           -lc -lm -lnsl -ldl -lsocket -lsunmath -lM77 -lF77
+LDFLAGS=        -Wl,-R${CALFUSEDIR}/lib
+
+OBJECTS=	cf_calfes.o cf_fes_init.o cf_fes_read.o cf_fes_write.o \
+		cf_fes_cal.o cf_fes_get_cal_image.o cf_limbang.o \
+		cf_fes_apply_bias.o cf_fes_apply_flat.o cf_fes_apply_mask.o 
+
+all:		cf_calfes
+
+cf_calfes:	${OBJECTS}
+		${CC} ${CFLAGS} -o cf_calfes ${OBJECTS} \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+		chmod g+rw cf_calfes
+
+install:	cf_calfes
+		/bin/cp cf_calfes ${FUSEBINDIR}
+
+clean:
+		/bin/rm -f ${OBJECTS} cf_calfes
+
+distclean:
+		/bin/rm -f ${OBJECTS} cf_calfes
+		cd ../../bin; /bin/rm -f cf_calfes
+
+lint:		${SOURCES}
+		lint ${SOURCES}
diff --git a/src/fes/Makefile.orig.orig b/src/fes/Makefile.orig.orig
new file mode 100644
index 0000000..23f189b
--- /dev/null
+++ b/src/fes/Makefile.orig.orig
@@ -0,0 +1,44 @@
+
+SHARED=		-shared
+FITSVER=	2.470
+CALFUSEDIR=	${PWD}/../..
+
+# Symbols for include directories
+FUSEINCLDIR=    -I${CALFUSEDIR}/include
+
+# Symbols used for compiling
+CC=             cc
+OPT=            -O -DCFORTRAN -KPIC -DSOLARIS
+CFLAGS =	${OPT} ${FUSEINCLDIR}
+
+# Symbols used for creating shared binaries
+FUSEBINDIR=     ${CALFUSEDIR}/bin
+FUSELIBDIR=     -L${CALFUSEDIR}/lib
+LIBDIR=         -L/opt/SUNWspro/lib
+FUSELIBS=       -lsla -lcfitsio-${FITSVER} -lcf
+LIBS=           -lc -lm -lnsl -ldl -lsocket -lsunmath -lM77 -lF77
+LDFLAGS=        -Wl,-R${CALFUSEDIR}/lib
+
+OBJECTS=	cf_calfes.o cf_fes_init.o cf_fes_read.o cf_fes_write.o \
+		cf_fes_cal.o cf_fes_get_cal_image.o cf_limbang.o \
+		cf_fes_apply_bias.o cf_fes_apply_flat.o cf_fes_apply_mask.o 
+
+all:		cf_calfes
+
+cf_calfes:	${OBJECTS}
+		${CC} ${CFLAGS} -o cf_calfes ${OBJECTS} \
+		${FUSELIBDIR} ${LIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+		chmod g+rw cf_calfes
+
+install:	cf_calfes
+		/bin/cp cf_calfes ${FUSEBINDIR}
+
+clean:
+		/bin/rm -f ${OBJECTS} cf_calfes
+
+distclean:
+		/bin/rm -f ${OBJECTS} cf_calfes
+		cd ../../bin; /bin/rm -f cf_calfes
+
+lint:		${SOURCES}
+		lint ${SOURCES}
diff --git a/src/fes/cf_calfes.c b/src/fes/cf_calfes.c
new file mode 100644
index 0000000..43e913c
--- /dev/null
+++ b/src/fes/cf_calfes.c
@@ -0,0 +1,151 @@
+/*******************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *******************************************************************************
+ *
+ * Synopsis:    cf_calfes rootname
+ *                   where rootname is the exposure root name
+ *
+ * Description: 
+ *      This main program calls all the routines below to apply 
+ *      FES processing steps.  It
+ *         1) Opens the input and output FES FITS files;
+ *         2) Loops through all images present:
+ *              a) Calls the procedures listed below to process all the images;
+ *              b) Writes the current processed image out to the 
+ *                    current output HDU.
+ *         3) Closes the input and output files.
+ *
+ * Arguments:  rootname exposure_root_name
+ *
+ * Returns:    0 upon successful completion
+ *
+ * History:    07/08/98    gak    calfes_design.070898 design documented
+ *             07/15/98    mlr    begin work
+ *             04/12/99    mlr    modified to only write each image only
+ *                                once - now passing the image in addition
+ *                                to the fits hdu to each subroutine.
+ *             04/19/99    mlr    finished modifications to utilize
+ *                                libcf and FITSIO.h(error handling).
+ *	       08/23/04	   wvd    Change cf_velang_calc to cf_velang.
+ *
+ ******************************************************************************/
+
+#include <string.h>
+#include "calfuse.h"
+#include "cf_calfes.h"
+
+#define CF_PRGM_ID      "cf_calfes"
+#define CF_VER_NUM	"1.4"
+#define RAW_FES "RAW FES           "
+#define CAL_FES "CALIBRATED FES    "
+
+int main(int argc, char *argv[])
+{
+    fitsfile   *infits, *outfits;
+    int        i, status;
+    int        hdu, hdutype, num_of_hdus;
+    int        naxes1, naxes2;
+    long       bitpix;
+    float      bscale, bzero;
+    double     mjd_start, mjd_end;
+
+    char       infilename[30], outfilename[30];
+    char       file_type[20];
+    float      *image;
+
+        /* Enter a timestamp into the log. */
+    	cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+        cf_error_init(CF_PRGM_ID,CF_VER_NUM, stdout);
+
+        if (argc != 2)
+           cf_if_error("Usage: cf_calfes filerootname ");
+
+        /* determine file names of the input file and the output file */
+	strcpy(infilename, argv[1]);
+        strcat(infilename, "raw.fit");
+
+        strcpy(outfilename, argv[1]);
+        strcat(outfilename, "cal.fit");
+
+        status=0;
+
+        /* open the input FES FITS file  and verify that it is a RAW FES file*/
+	FITS_open_file(&infits, infilename, READONLY, &status);
+
+        FITS_read_key(infits, TSTRING, "FILETYPE", &file_type, NULL, &status);
+
+        if (strncmp(file_type, RAW_FES, 7) != 0)
+                cf_if_error("The input file is not a RAW FES file.");
+
+        /* open the output file for calibrated FES data, copy the primary
+           header from the input FES file to the output FES file, then 
+           modify keywords as needed. 
+        */
+	FITS_create_file(&outfits, outfilename, &status);
+        FITS_copy_header(infits, outfits, &status);
+
+        bitpix = FLOAT_IMG;
+        FITS_update_key(outfits, TLONG,   "BITPIX",   &bitpix, NULL, &status);
+        FITS_update_key(outfits, TSTRING, "FILETYPE", CAL_FES, NULL, &status);
+
+        read_tle(outfits);
+
+        /* Determine how many extensions there are in this file.
+           There is 1 FES image in each extension.  So this tells us how
+           many images there are in this file and controls the loop that
+           processes each one.
+        */
+
+        FITS_read_key(infits, TINT, "NEXTEND ", &num_of_hdus, NULL, &status);
+
+        printf("This file %s has %d FES image(s).\n", infilename, num_of_hdus);
+        hdutype = -1;
+
+        for (i=1 ; i <= num_of_hdus; i++)
+        {
+            hdu = i + 1;
+
+	    FITS_create_hdu(outfits, &status);
+	    FITS_movabs_hdu(infits, hdu, &hdutype, &status);
+            FITS_copy_header(infits, outfits, &status);
+
+            bitpix = FLOAT_IMG;
+            bzero = 0.0; 
+            bscale = 1.0;
+            FITS_update_key(outfits, TLONG,  "BITPIX", &bitpix, NULL, &status);
+            FITS_update_key(outfits, TFLOAT, "BZERO",  &bzero,  NULL, &status);
+            FITS_update_key(outfits, TFLOAT, "BSCALE", &bscale, NULL, &status);
+
+            FITS_read_key(outfits,TDOUBLE,"EXPSTART",&mjd_start,NULL, &status);
+            FITS_read_key(outfits,TDOUBLE,"EXPEND",  &mjd_end,  NULL, &status);
+            cf_velang(outfits, (mjd_start+mjd_end)/2.0 );
+            cf_min_limbang(outfits, mjd_start, mjd_end);
+ 
+             status =+ cf_fes_read(infits, &image, &naxes1, &naxes2);
+             status =+ cf_fes_init(outfits);
+             status =+ cf_fes_write(outfits, hdu, image); 
+
+             status =+ cf_fes_cal(FES_MASK, outfits, &image, naxes1, naxes2);
+             status =+ cf_fes_cal(FES_BIAS, outfits, &image, naxes1, naxes2);
+             status =+ cf_fes_cal(FES_FLAT, outfits, &image, naxes1, naxes2);
+             status =+ cf_fes_write(outfits, hdu, image); 
+
+
+             free(image);
+
+             if (status != 0)
+        	cf_if_error("cf_calfes failed.");
+	}
+
+        /* close the FES FITS files */
+	FITS_close_file(infits, &status);
+	FITS_close_file(outfits, &status);
+
+
+        /* Enter a timestamp into the log. */
+        cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done Processing");
+
+	return(status);
+}
diff --git a/src/fes/cf_calfes.h b/src/fes/cf_calfes.h
new file mode 100644
index 0000000..d4944fa
--- /dev/null
+++ b/src/fes/cf_calfes.h
@@ -0,0 +1,10 @@
+#define FES_GOOD_PIX    0.0
+#define FES_BAD_PIX   -20.0
+#define FES_FLAT          1
+#define FES_MASK          2
+#define FES_BIAS          3
+
+int cf_fes_apply_flat(fitsfile *, float **, float *, int, int);
+int cf_fes_apply_mask(fitsfile *, float **, float *, int, int);
+int cf_fes_apply_bias(fitsfile *, float **, float *, int, int);
+
diff --git a/src/fes/cf_cp_hdr.c b/src/fes/cf_cp_hdr.c
new file mode 100644
index 0000000..7642f05
--- /dev/null
+++ b/src/fes/cf_cp_hdr.c
@@ -0,0 +1,71 @@
+/*******************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *******************************************************************************
+ *
+ * Synopsis:	cf_cp_hdr(fitsfile *infits, int inhdu, fitsfile *outfits,
+ *			int outhdu)
+ *
+ * Description: Copies the header, with no changes, from HDU inhdu of the
+ *	 	input FITS file infits to HDU outhdu of the output FITS file
+ *		outfits.
+ *
+ * Arguments:	fitsfile	*infits		Input FITS file pointer
+ *		int		inhdu		HDU to be copied from
+ *		fitsfile	*outfits	Output FITS file pointer
+ *		int		outhdu		HDU to be copied to
+ *
+ * Returns:	none
+ *
+ * History:	04/02/98	gak	Begin work
+ *		08/27/98	gak	Initialized status, hdutype;
+ *					return status
+ *
+ ******************************************************************************/
+
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include "calfuse.h"
+
+#define CF_PRGM_ID      "cf_cp_hdr"
+#define CF_VER_NUM      "1.1"
+
+int cf_cp_hdr(fitsfile *infits, int inhdu, fitsfile *outfits, int outhdu)
+{
+	char		buffer[FLEN_CARD];
+	int 		status, hdutype; 
+	int		nkeys, keynum;
+	int		i;
+
+	status = 0;
+	hdutype = 0;
+
+	if ( fits_movabs_hdu(infits, inhdu, &hdutype, &status) ) {
+		cf_if_error(status);
+		exit(status);
+	}
+	if ( fits_movabs_hdu(outfits, outhdu, &hdutype, &status) ) {
+		cf_if_error(status);
+		exit(status);
+	}
+
+	/* Get number of keywords in the input header, loop & copy. */
+	if ( fits_get_hdrpos(infits, &nkeys, &keynum, &status) ) {
+		cf_if_error(status);
+		exit(status);
+	}
+	for ( i = 1; i <= nkeys; i++) {
+		if ( fits_read_record(infits, i, buffer, &status) ) {
+			cf_if_error(status);
+			exit(status);
+		}
+		if ( fits_write_record(outfits, buffer, &status) ) {
+			cf_if_error(status);
+			exit(status);
+		}
+	}
+
+	return status;
+}
diff --git a/src/fes/cf_fes_apply_bias.c b/src/fes/cf_fes_apply_bias.c
new file mode 100644
index 0000000..7591757
--- /dev/null
+++ b/src/fes/cf_fes_apply_bias.c
@@ -0,0 +1,98 @@
+/*******************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *******************************************************************************
+ *
+ * Synopsis: cf_apply_fes_bias(fitsfile *fesfits, float **image, 
+ *                                       float *bias, int axis1, int axis2)
+ *
+ * Description: Apply FES bias in *bias to the raw FES image in **image
+ *     To apply the bias, I simply loop through the 
+ *     bias image pixel by pixel and subtract that 
+ *     value from the given FES image.
+ *
+ * Arguments:	fitsfile *fesfits       fits file for image so that we can add
+ *                                      history/comment lines to the HDU
+ *              float   **image 	FES image
+ *              float   *bias	 	FES bias image
+ *              int     axis1, axis2    size of each axis of the images.
+ *                                      This presumes that both images are 
+ *                                      the same size when they get here.
+ *
+ * Returns:	0 upon successful completion
+ *
+ * History:	07/08/98	gak     calfes_design.070898 design documented
+ *              07/22/98        mlr     started work
+ *              04/06/99        mlr     Broke this actual subroutine out
+ *                                      from cf_fes_bias.c
+ *              08/10/99        mlr     added fesfits to the argument list
+ *              04/25/02        wvd	initialize status to zero
+ *
+ ******************************************************************************/
+
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include "calfuse.h"
+#include "cf_calfes.h"
+
+#define CF_PRGM_ID      "cf_fes_apply_bias"
+#define CF_VER_NUM      "1.4"
+
+int cf_fes_apply_bias(fitsfile *fesfits, float **image,  
+                               float *bias, int naxis1, int naxis2)
+{
+        int i, j;  /*loop counters */
+        int status=0;
+        float os_bias, os_data;
+        float factor;
+        char buffer[80];
+
+        cf_timestamp(CF_PRGM_ID,CF_VER_NUM, "Applying FES bias");
+        
+        os_bias=0.;
+        os_data=0.;
+
+	if (naxis1 == 520)  /* 1x1 binning */
+   	{
+           for (j=0; j<520; j++)
+	      for (i=512; i<520; i++)
+              {
+	         os_bias += bias[j*naxis1+i];
+	         os_data += (*image)[j*naxis1+1];
+              }
+        }
+        else if (naxis1 == 260)  /* 2x2 binning */
+        {
+           for (j=0; j<260; j++)
+               for (i=256; i<260; i++)
+               {
+	         os_bias += bias[j*naxis1+i];
+	         os_data += (*image)[j*naxis1+1];
+               }
+        }
+        else   /*bail out -- unsupported image size or binning */
+            exit(-1);
+
+      factor = os_data / os_bias;
+      sprintf(buffer, "FES BIAS FACTOR = %lf",factor);
+      cf_timestamp(CF_PRGM_ID, CF_VER_NUM, buffer);
+
+/*      FITS_write_history(fesfits, buffer, &status); */
+
+      for (j=0; j<naxis2; j++)
+         for (i=0; i<naxis1; i++)
+         {
+/*     printf("pixel[%d, %d] = %lf\n",i,j, (*image)[j*naxis1+i]); */
+                    if ( (*image)[j*naxis1+i] != FES_BAD_PIX )
+                          (*image)[j*naxis1+i] -= bias[j*naxis1+i] * factor;
+                    else
+                        printf("bad pixel[%d, %d]\n",i,j);
+          }
+
+      cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished FES bias");
+
+      return(status);
+
+}
diff --git a/src/fes/cf_fes_apply_flat.c b/src/fes/cf_fes_apply_flat.c
new file mode 100644
index 0000000..21d8ddc
--- /dev/null
+++ b/src/fes/cf_fes_apply_flat.c
@@ -0,0 +1,67 @@
+/*******************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *******************************************************************************
+ *
+ * Synopsis: cf_apply_fes_flat(fitsfile *fesfits, float **image, 
+ *                                       float *flat, int axis1, int axis2)
+ *
+ * Description: Apply FES flatfield in *flat to the raw FES image in **image
+ *     To apply the flatfield, I simply loop through the 
+ *     flatfield image pixel by pixel and 
+ *    If the flatfield pixel value != 0.0
+ *    then fes image[] pixel value =  image[]pixel value/mask[]pixel value.
+ *    else (If the flatfield pixel value == 0.0)
+ *    then fes image[] pixel value =  FES_BAD_PIX.
+ *
+ * Arguments:	fitsfile *fesfits       fits file for image..  so that we can add
+ *                                      history/comment lines to the HDU
+ *              float   **image 	FES image
+ *              float   *mask	 	FES mask
+ *              int     axis1, axis2    size of each axis of the images.
+ *                                      This presumes that both images are 
+ *                                      the same size before they get here.
+ *
+ * Returns:	0 upon successful completion
+ *
+ * History:	07/08/98	gak     calfes_design.070898 design documented
+ *              07/22/98        mlr     started work
+ *              04/06/99        mlr     Broke this actual subroutine out
+ *                                      from cf_fes_mask.c
+ *              04/20/99        mlr     instead of calculating the image row
+ *                                      size each time -- pass it in
+ *              08/10/99        mlr     added fesfits to argument list
+ *
+ ******************************************************************************/
+
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include "calfuse.h"
+#include "cf_calfes.h"
+
+#define CF_PRGM_ID      "cf_fes_apply_flat"
+#define CF_VER_NUM      "1.4"
+
+int cf_fes_apply_flat(fitsfile *fesfits, float **image,  
+                            float *flat, int naxis1, int naxis2)
+{
+        int i, j;  /*loop counters */
+        int pixel;
+
+        cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Applying FES flatfield");
+        for (j=0; j < naxis2; j++)
+             for (i=0; i < naxis1; i++)
+             {
+               pixel = j* naxis1+ i;            
+               if ((*image)[pixel] != FES_BAD_PIX)
+                   if (flat[pixel] != 0.0 )
+                        (*image)[pixel] /= flat[pixel];
+                   else 
+                      (*image)[pixel] = FES_BAD_PIX;
+             }
+       cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done applying FES flat");
+
+       return(0);
+}
diff --git a/src/fes/cf_fes_apply_mask.c b/src/fes/cf_fes_apply_mask.c
new file mode 100644
index 0000000..c083121
--- /dev/null
+++ b/src/fes/cf_fes_apply_mask.c
@@ -0,0 +1,56 @@
+/*******************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *******************************************************************************
+ *
+ * Synopsis: cf_apply_fes_mask(fitsfile *fesfits, float **image, 
+ *                                       float *mask, int axis1, int axis2)
+ *
+ * Description: Apply FES mask in *mask to the raw FES image in **image
+ *     To apply the mask I simply loop through the 
+ *     mask image pixel by pixel and 
+ *    If the mask pixel value != 0.0
+ *    then fes image pixel value = mask pixel value.
+ *
+ * Arguments:	fitsfile *fesfits       fits file for image, so that we can add
+ *                                      history/comment lines to the HDU
+ *              float   **image 	FES image
+ *              float   *mask	 	FES mask
+ *              int     axis1, axis2    size of each axis of the images.
+ *                                      This presumes that both images are 
+ *                                      the same size when they get here.
+ *
+ * Returns:	0 upon successful completion
+ *
+ * History:	07/08/98	gak     calfes_design.070898 design documented
+ *              07/22/98        mlr     started work
+ *              04/06/99        mlr     Broke subroutine out from cf_fes_mask.c
+ *              08/10/99        mlr     added fesfits to the argument list
+ *
+ *
+ ******************************************************************************/
+
+#include "calfuse.h"
+#include "cf_calfes.h"
+
+#define CF_PRGM_ID      "cf_fes_apply_mask"
+#define CF_VER_NUM      "1.4"
+
+int cf_fes_apply_mask(fitsfile *fesfits, float **image,  
+                               float *mask, int naxis1, int naxis2)
+{
+        int i, j;  /*loop counters */
+
+        cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Applying FES pixel mask");
+
+        for (j=0; j < naxis2; j++)
+             for (i=0; i < naxis1; i++)
+               if (mask[j*naxis1+i] != FES_GOOD_PIX )
+                     (*image)[j*naxis1+i] = mask[j*naxis1+i];
+
+
+       cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done applying FES  mask");
+
+       return(0);
+}
diff --git a/src/fes/cf_fes_cal.c b/src/fes/cf_fes_cal.c
new file mode 100644
index 0000000..0f08bbd
--- /dev/null
+++ b/src/fes/cf_fes_cal.c
@@ -0,0 +1,115 @@
+/*******************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *******************************************************************************
+ *
+ * Synopsis:	int cf_fes_cal(int cal_type, fitsfile *fesfits, float **image, 
+ *                                    int inaxis1, int inaxis2)
+ *
+ * Description: Get bias calibration filename for the raw FES image in
+ *                  the current hdu pointed at by *infits.
+ *              Call cf_fes_get_cal_image() to open the cal file and get
+ *                                          the calibration image.
+ *              Call cf_fes_apply_flat();
+ *              return the modified image to the calling routine.
+ *              4/10/99  MLR removed int inhdu as an argument and removed
+ *                       the call to fits_movabs_hdu.  This requires any
+ *                       user of this subroutine to do these steps before
+ *                       calling cf_fes_flat.
+ *              4/10/99  MLR removed (fitsfile *outfits, int outhdu) from 
+ *                       the argument list.  We will leave writing the image
+ *                       out to the calling routine.
+ *   
+ *
+ * Arguments:	fitsfile   *infits	Input FITS file pointer
+ *              float **image           already read in FES image
+ *              int inaxis1             image size  of the input image
+ *              int inaxis2
+ *
+ * Returns:	none
+ *
+ * History:	07/08/98	gak     calfes_design.070898 design documented
+ *              07/22/98        mlr     started work
+ *              04/10/99        mlt     pulled the actual work out of this
+ *                                      routine and into cf_fes_apply_flat
+ *              04/12/99        mlr     modified the input arguments(see above)
+ *                                      use the now generic cf_fes_read to
+ *                                      get the calibration image.
+ *              04/14/99        mlr     pulled the reading out and put it 
+ *                                      into cf_fes_get_cal_image.c
+ *              04/16/99        mlr     finished modifications to utilize
+ *                                      libcf and FITSIO.h(error handling).
+ *
+ * ToDo:  4/12/99 I have added the naxis1 and naxis2 parameters to the 
+ *                argument list.  I need to use them to compare binning
+ *                factors in the two images.
+ *                I should combine cf_fes_mask, cf_fes_bias, cf_fes_flat
+ *                into one generic cf_fes_do_cal("cf_fes_mask", *fesfits,...etc)
+ *
+ ******************************************************************************/
+
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include "calfuse.h"
+#include "cf_calfes.h"
+
+#define CF_VER_NUM  "1.4"
+
+int cf_fes_cal(int cal_type, fitsfile *fesfits, float **image, 
+                              int inaxis1, int inaxis2)
+{
+	char	buffer[FLEN_CARD];
+        char    calfilename[30];
+        fitsfile *calfile;
+	int 	status; 
+        float   *calimage;
+	char *prog_id, *msg, *keyword, *msg2;
+
+	int (*func)(fitsfile *, float **, float *, int, int);
+
+        status = 0;
+
+        switch (cal_type) {
+           case FES_FLAT:
+		prog_id = "cf_fes_flat";
+		msg = "Begin FES flatfield";
+		msg2 = "Done  FES flatfield";
+		keyword = "FFLT1FCL";
+		func =  cf_fes_apply_flat;
+		break;
+           case FES_MASK:
+		prog_id = "cf_fes_mask";
+		msg = "Begin FES mask";
+		msg2 = "Done  FES mask";
+		keyword = "MASK_FCL";
+		func =  cf_fes_apply_mask;
+		break;
+           case FES_BIAS:
+		prog_id = "cf_fes_bias";
+		msg = "Begin FES bias";
+		msg2 = "Done  FES bias";
+		keyword = "BIAS1FCL";
+		func =  cf_fes_apply_bias;
+		break;
+	}
+
+
+	cf_timestamp(prog_id, CF_VER_NUM, msg);
+
+        FITS_read_key(fesfits, TSTRING, keyword, calfilename, buffer, &status);
+
+        if (cf_fes_get_cal_image(calfilename, &calimage, inaxis1, inaxis2) == -1)
+           return (-1);
+       
+        (*func)(fesfits, image, calimage, inaxis1, inaxis2);
+
+        cf_fes_proc_update(fesfits, prog_id, "COMPLETE");
+
+        free(calimage);
+
+        cf_timestamp(prog_id, CF_VER_NUM, msg2);
+
+        return(status);
+}
diff --git a/src/fes/cf_fes_get_cal_image.c b/src/fes/cf_fes_get_cal_image.c
new file mode 100644
index 0000000..2e5e8f0
--- /dev/null
+++ b/src/fes/cf_fes_get_cal_image.c
@@ -0,0 +1,71 @@
+ /*******************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *******************************************************************************
+ *
+ * Synopsis:int cf_fes_get_cal_image(char cal_file_name[], float **cal_image, 
+ *                                                  int naxis1, int naxis2)
+ *
+ * Description: open the specified calibration file for an FES image
+ *              loop through each extension in the calibration file
+ *             until you find the one that has the same size naxis1 and
+ *              naxis2 as the input image.
+ *              read the image in that extention into *cal_image
+ *              close the calibration file
+ *
+ * Arguments:	char cal_file_name[], 
+ *              float **cal_image, 
+ *              int naxis1, int naxis2
+ *
+ * Returns:	none
+ *
+ * History:	04/14/99        mlr     started work
+ *              04/16/99        mlr     modified to use libcf and FITSIO.h
+ *
+ ******************************************************************************/
+
+#include "calfuse.h"
+
+#define CF_PRGM_ID      "cf_fes_get_cal_image"
+#define CF_VER_NUM      "1.4"
+
+int cf_fes_get_cal_image(char cal_file_name[], float **cal_image, 
+                                  int naxis1, int naxis2)
+{
+      fitsfile *fes_cal_file;
+      int status;
+      int i, hdu, hdutype, num_exts;
+      int cal_axis1, cal_axis2;
+      char buffer[FLEN_CARD];
+ 
+      cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin getting Cal image");
+
+      status = 0;
+
+      /* open the input FES CALIBRATION file */
+
+      FITS_open_file(&fes_cal_file,cf_cal_file(cal_file_name),READONLY,&status);
+
+      FITS_read_key(fes_cal_file, TINT, "NEXTEND", &num_exts, buffer, &status);
+
+      for (i = 1; i<= num_exts; i++)
+      {
+ 	  hdu = i + 1;
+          FITS_movabs_hdu(fes_cal_file, hdu, &hdutype, &status);
+          cf_fes_read(fes_cal_file, cal_image, &cal_axis1, &cal_axis2);
+          if ((cal_axis1 == naxis1) && (cal_axis2 == naxis2))
+                   break;
+      }
+      FITS_close_file(fes_cal_file, &status);
+
+      if (i>num_exts) 
+      { 
+          *cal_image=NULL;
+          cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "No Cal image of requested size");
+          return(-1);
+      }
+       
+      cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done getting Cal image");
+      return(status);
+}
diff --git a/src/fes/cf_fes_init.c b/src/fes/cf_fes_init.c
new file mode 100644
index 0000000..fcbb34c
--- /dev/null
+++ b/src/fes/cf_fes_init.c
@@ -0,0 +1,294 @@
+
+/*******************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *******************************************************************************
+ *
+ * Synopsis:    cf_fes_init(fitsfile *fptr)
+ *
+ * Description: cf_fes_init performs two functions.  First, populates the 
+ *              data processing step keywords based upon the type of 
+ *              data (FESA or FESB).  Second, it populates the calibration
+ *              file keywords based on the time and date of observation,
+ *              the detector segment, and the interpolation status of the
+ *              calibration file.
+ *
+ * Arguments:   fitsfile    *fptr	Pointer to input file
+ *
+ * History:     05/21/98        emm     Begin work.
+ *              06/17/98        emm     Modified keywords to reflect updated
+ *                                      calfuse design
+ *              07/15/98        mlr     copied from emm
+ *		08/23/04	wvd	Change from fits_modify_key_str to
+ *					FITS_update_key throughout.
+ ******************************************************************************/
+
+#include <stdio.h>
+#include <string.h>
+#include "calfuse.h"
+
+#define  MAXCHARS 120
+#define  MASTER_CAL_FILE "master_fes_calib_file.dat"
+#define  CF_PRGM_ID      "cf_fes_init"
+#define  CF_VER_NUM      "1.4"
+
+int cf_fes_init(fitsfile *fptr) 
+{
+int   i,j,k,l,flg;
+char  comment[FLEN_CARD], instmode[FLEN_CARD], detector[FLEN_CARD];
+char  fes[2];
+char  keyword_in[9], segment_in[3];
+char  filename_in[19]="                  \0";
+char  keyword_out1[9], keyword_out2[9];
+char  complete[19], error[19], blank[19];
+char  linin[120];
+int   status, interp_in;
+float expstart, aftermjd_in;
+
+struct fes_keyword_tab keytab[NUM_FES_PROC_STEPS]=FES_CALIBRATION_STEP_KEYS;
+struct cal_file_tab calkey[NUM_FES_CAL_KEYS]=FES_CALIBRATION_FILE_KEYS;
+FILE  *fpin;
+
+cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin initializing header");
+cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+status=0;
+
+   strncpy(complete,"COMPLETE          \0",19);
+   strncpy(error,   "ERROR             \0",19);
+   strncpy(blank,   "                  \0",19);
+
+/*  Populate data processing keywords. */
+
+   for (i=0; i<NUM_FES_PROC_STEPS; i++)
+        FITS_update_key(fptr,TSTRING,keytab[i].name,
+                   keytab[i].value,NULL,&status);
+
+
+/*  Populate calibration file keywords based on the date of the 
+ *  observation and the segment/channel number. */
+
+   FITS_read_key(fptr, TFLOAT, "EXPSTART", &expstart, comment, &status);
+   FITS_read_key(fptr, TSTRING, "FES_ID", instmode, comment, &status);
+   sscanf(instmode,"%*3c %1c",fes);
+
+/*  Open the Master calibration database file. */
+
+   fpin=NULL;
+   fpin=fopen(cf_cal_file(MASTER_CAL_FILE),"r");
+   if (fpin == NULL)
+             cf_if_warning("Master calibration database file not found");
+
+   /*  Cycle through the master cal file until we run out of lines. */
+
+   /*  Here's how this section works.  We need to keep track of 3 calibration
+    *  files for each keyword: the cal file which immediately preceedes the 
+    *  date of observation, the cal file which immediately preceedes the cal
+    *  file which immediately preceedes the observation, and the cal file 
+    *  immediately after the observation.  These are stored in strut calkey
+    *  in:
+    *     calkey[i].filenames[0] => second cal file preceeding observation
+    *     calkey[i].filenames[1] => cal file immediately preceeding observation
+    *     calkey[i].filenames[2] => cal file immediately after observation
+    *
+    *  Here is the plan.  Cycle through the master cal file, reading each
+    *  line.  Determine the keyword for each line, and use that to determine
+    *  the appropriate index [i] for calkey.  Then, if the detector segment 
+    *  is correct, determine where the new file fits into the structure above.
+    *  If it is more recent than one or both of the preceeding cal files, 
+    *  but is older than the observation (expstart) replace either 
+    *  filenames[0] or filenames[1].  If filenames[1] is replaced, shift
+    *  the old value down into filenames[0].  If the file is more recent 
+    *  than the observation, and closer to the observation than the file 
+    *  in filenames[2], replace filenames[2].  The values 
+    *  calkey[i].aftermjd[] and calkey[i].interp[] store the date and 
+    *  interpolation status of the best files.  This organization allows
+    *  the master calibration database file to be written in any order.
+    */
+
+   while (fgets(linin, MAXCHARS, fpin) != NULL) {
+
+        /* Check for comment lines */
+
+       if ((linin[0] != '#') && (linin[0] != '\n')) {
+              sscanf(linin, "%4c %1c %12c %9f %1d",keyword_in,
+                           segment_in,filename_in,&aftermjd_in,&interp_in);
+
+	      /* Determine which keyword we just read in. */
+              i=0;
+              while ((strncmp(calkey[i].name,keyword_in,4) != 0) && 
+                                      (i < NUM_FES_CAL_KEYS)) i++;
+
+              if (i >= NUM_FES_CAL_KEYS) {
+                   cf_if_warning("Unrecognized keyword in master calibration file");
+              } else {
+                   if ((strncmp(segment_in,"  ",1) == 0) || 
+                       (strncmp(segment_in,fes,1) == 0)) {
+                        j=0;
+                        if ((aftermjd_in < expstart) && 
+                            (aftermjd_in > calkey[i].aftermjd[0]) &&
+                            (aftermjd_in > calkey[i].aftermjd[1])) {
+                                  strncpy(calkey[i].filenames[0],
+                                          calkey[i].filenames[1],18);
+                                  calkey[i].aftermjd[0]=calkey[i].aftermjd[1];
+                                  calkey[i].interp[0]=calkey[i].interp[1];
+                                  strncpy(calkey[i].filenames[1],
+                                          filename_in,18);
+                                  calkey[i].aftermjd[1]=aftermjd_in;
+                                  calkey[i].interp[1]=interp_in;
+                         } else if ((aftermjd_in < expstart) && 
+                            (aftermjd_in > calkey[i].aftermjd[0])) {
+                                  strncpy(calkey[i].filenames[0],
+                                          filename_in,18);
+                                  calkey[i].aftermjd[0]=aftermjd_in;
+                                  calkey[i].interp[0]=interp_in;
+			 }
+     
+                        if ((aftermjd_in > expstart) && 
+                            (aftermjd_in < calkey[i].aftermjd[2])) {
+                                  strncpy(calkey[i].filenames[2],
+                                          filename_in,18);
+                                  calkey[i].aftermjd[2]=aftermjd_in;
+                                  calkey[i].interp[2]=interp_in;
+			}
+		   } /* Endif segment match */
+	      } /* end else unrecognized keyword */		   
+	}  /* end while linin not comment */
+   } /* end while(linin != NULL) */
+
+   fclose(fpin);
+
+   /*  OK, now that we have identified the closest two files before
+    *  the observation, and the file after the observation, we can
+    *  decide what to do with them.  First, the easy part:  if 
+    *  calkey[i].numfiles=1, no interpolation is possible, so we
+    *  write out calkey[i].filenames[1], which is the file immediately
+    *  preceeding the observation.  If calkey[i].numfiles=2, interpolation
+    *  is possible, and we will have to write two keywords into the header.
+    *  The decision as to which two keywords to write follows these rules:
+    *  Rule 1: If an observation occurs between two files which can be 
+    *          interpolated, then an interpolation must be done. 
+    *  Rule 2: If the calibration file immediately preceeding an 
+    *          observation is to be used in a stepwise manner, then said
+    *          file shall be used in stepwise manner. 
+    *  Rule 3: If the two calibration files immediately preceeding an 
+    *          observation can be interpolated, but the following file 
+    *          cannot, then the two previous files will be extrapolated 
+    *          forward in time. 
+    *  Rule 4: If the closest preceeding calibration file has an interpolation
+    *          flag, but the file preceeding it has a stepwise flag, the the 
+    *          closest preceeding file will be used in a sterpwise manner.
+    *  Rule 5: Never interpolate backward in time.
+    *
+    *  In fact, there are only 8 possible cases:
+    *
+    *  Remember, the files were sorted such that the observation 
+    *  always occurs between [1] and [2].  Also remember that 
+    *  interp[i]=0 => stepwise):
+    *
+    *    Case               Action
+    *
+    *  interp[0] = 0
+    *  interp[1] = 0    filenames[1] will be used in a stepwise manner
+    *  interp[2] = 0
+    *
+    *  interp[0] = 0
+    *  interp[1] = 0    filenames[1] will be used in a stepwise manner
+    *  interp[2] = 1
+    *
+    *  interp[0] = 0
+    *  interp[1] = 1    filenames[1] will be used in a stepwise manner
+    *  interp[2] = 0
+    *
+    *  interp[0] = 1
+    *  interp[1] = 0    filenames[1] will be used in a stepwise manner
+    *  interp[2] = 0
+    *
+    *  interp[0] = 1
+    *  interp[1] = 0    filenames[1] will be used in a stepwise manner
+    *  interp[2] = 1
+    *
+    *  interp[0] = 0
+    *  interp[1] = 1    filenames[1] and filenames[2] will be interpolated
+    *  interp[2] = 1
+    *
+    *  interp[0] = 1
+    *  interp[1] = 1    filenames[0] and filenames[1] will be extrapolated
+    *  interp[2] = 0
+    *
+    *  interp[0] = 1
+    *  interp[1] = 1    filenames[1] and filenames[2] will be interpolated
+    *  interp[2] = 1
+    *
+    */
+
+   /*  Write the calibration files into the header keywords. */
+   /*  Cycle through the keywords. */
+   for (i=0; i<NUM_FES_CAL_KEYS; i++) {
+
+     if (calkey[i].numfiles == 1) {
+
+          /*  This is the easy case, no interpolation is possible. */
+
+          sprintf(keyword_out1,"%4.4s%1.1s%3.3s",calkey[i].name,"_",
+                    calkey[i].extension);
+          FITS_update_key(fptr,TSTRING,keyword_out1,calkey[i].filenames[1],
+                    NULL,&status); 
+     } else {
+
+          /*  OK, interpolation is possible, now decide which two files
+           *  to write out. */
+
+          /* Create the two output keywords */
+          sprintf(keyword_out1,"%4.4s%1.1s%3.3s",calkey[i].name,"1",
+                    calkey[i].extension);
+          sprintf(keyword_out2,"%4.4s%1.1s%3.3s",calkey[i].name,"2",
+                    calkey[i].extension);
+
+       if (calkey[i].interp[1] == 0) {
+
+	 /*  Easy, preceeding file is a 0, so write filenames[1] to 
+          *  both keywords.  Takes care of cases 000, 001, 100, 101.
+          */
+          FITS_update_key(fptr,TSTRING,keyword_out1,calkey[i].filenames[1],
+                    NULL,&status); 
+          FITS_update_key(fptr,TSTRING,keyword_out2,calkey[i].filenames[1],
+                    NULL,&status); 
+       } else if ((calkey[i].interp[1] == 1) && (calkey[i].interp[2] == 1)) {
+	 /* Case 011 and 111 */
+          FITS_update_key(fptr,TSTRING,keyword_out1,calkey[i].filenames[1],
+                    NULL,&status); 
+          FITS_update_key(fptr,TSTRING,keyword_out2,calkey[i].filenames[2],
+                    NULL,&status); 
+       } else if ((calkey[i].interp[0] == 1) && (calkey[i].interp[1] == 1) 
+		  && (calkey[i].interp[2] == 0)){
+	 /* Case 110 */
+          FITS_update_key(fptr,TSTRING,keyword_out1,calkey[i].filenames[0],
+                    NULL,&status); 
+          FITS_update_key(fptr,TSTRING,keyword_out2,calkey[i].filenames[1],
+                    NULL,&status); 
+
+       } else if ((calkey[i].interp[0] == 0) && (calkey[i].interp[1] == 1) 
+		  && (calkey[i].interp[2] == 0)){
+	  /* Case 010 */
+          FITS_update_key(fptr,TSTRING,keyword_out1,calkey[i].filenames[1],
+                    NULL,&status); 
+          FITS_update_key(fptr,TSTRING,keyword_out2,calkey[i].filenames[1],
+                    NULL,&status); 
+
+       } else cf_if_warning("The interpolation/stepwise logic has failed.  I am confused.");
+
+     } /* end else calkey.numfiles == 1 */
+
+   } /* end for i=0; i<NUMCALKEYS */
+
+
+FITS_update_key(fptr,TSTRING,"INIT_FES",complete,NULL,&status);
+
+cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done initializing header");    
+
+return status;
+}
+
+
diff --git a/src/fes/cf_fes_read.c b/src/fes/cf_fes_read.c
new file mode 100644
index 0000000..47fbf20
--- /dev/null
+++ b/src/fes/cf_fes_read.c
@@ -0,0 +1,76 @@
+/*******************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *******************************************************************************
+ *
+ * Synopsis:	cf_fes_read(fitsfile *infits, float **image, 
+ *                                            int *naxis1, int *naxis2);
+ *
+ * Description: reads an FES image from the current hdu in the FITS file
+ *              pointed to by *infits and stores it in the array pointed
+ *              to by *image.  
+ *              *infits may contain an FES image where each pixel is 
+ *              stored as unsigned shorts or as floats. cf_fes_read
+ *              determines this from BITPIX in the current hdu and proceeds 
+ *              accordingly.
+ *              cf_fes_read also takes care of any binning by determining 
+ *              the image size from NAXIS1 and NAXIS2 in the current hdu.
+ *              4/12/99  MLR These two values are now returned to the 
+ *                           calling routine for reference.
+ *              4/10/99  MLR removed int inhdu as an argument and removed
+ *                       the call to fits_movabs_hdu.  This requires any
+ *                       user of this subroutine to do these steps before
+ *                       calling cf_fes_read. 
+ *
+ * Arguments:	fitsfile   *infits	Input FITS file pointer
+ *		float      **image  	Pointer to array holding FES image
+ *              int        *naxis1      Image size parameters
+ *              int        *naxis2
+ * 
+ * Returns:	0 upon successfule completion
+ *
+ * History:	07/08/98	gak     calfes_design.070898 design documented
+ *              07/16/98        mlr     started work
+ *              04/12/99        mlr     modified the input arguments(see above)
+ *              04/16/99        mlr     finished modifications to utilize
+ *                                      libcf and FITSIO.h(error handling).
+ ******************************************************************************/
+
+#include "calfuse.h"
+
+#define CF_PRGM_ID      "cf_fes_read"
+#define CF_VER_NUM      "1.4"
+
+int cf_fes_read(fitsfile *infits, float**image, int *naxis1, int *naxis2)
+{
+	char	buffer[FLEN_CARD];
+	int 	status; 
+	int	bitpix, nullval, anynull, npixels;
+        int     i, j, hdutype;  
+        short   *short_image;
+
+        status = 0;
+        hdutype=-1;
+
+	FITS_read_key(infits, TINT, "NAXIS1", naxis1, buffer, &status);
+ 
+        FITS_read_key(infits, TINT, "NAXIS2", naxis2, buffer, &status);
+
+        npixels = (*naxis1) * (*naxis2);
+
+        cf_if_memory_error(*image = (float *) malloc(sizeof(float) * npixels)); 
+
+        FITS_read_key(infits, TINT, "BITPIX", &bitpix, buffer, &status);
+
+        nullval = 0;
+        if (bitpix == 16 || bitpix == -32)
+
+             FITS_read_img(infits, TFLOAT, 1, npixels, 
+                                     &nullval, *image, &anynull, &status);
+
+        else 
+             cf_if_error("INVALID data type for FES image. ");
+
+        return(status);
+}
diff --git a/src/fes/cf_fes_write.c b/src/fes/cf_fes_write.c
new file mode 100644
index 0000000..baa678b
--- /dev/null
+++ b/src/fes/cf_fes_write.c
@@ -0,0 +1,60 @@
+/*******************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *******************************************************************************
+ *
+ * Synopsis:	cf_fes_write(fitsfile *outfits, int hdu, float *image);
+ *
+ * Description: writes an FES image into HDU number hdu in the FITS file
+ *              pointed to by *fptr.  Currently cf_fes_write extracts
+ *              BITPIX, NAXIS1, and NAXIS2 from the specified HDU and 
+ *              uses those values to write the image.  
+ *
+ * Arguments:	fitsfile   *outfits	output FITS file pointer
+ *		int	   hdu 		HDU to be written to
+ *		float      *image  	Pointer to array holding FES image
+ *
+ * Returns:	none
+ *
+ * History:	07/08/98    gak    calfes_design.070898 design documented
+ *              07/20/98    mlr    started work
+ *              04/19/99    mlr    finished modifications to utilize
+ *                                 libcf and FITSIO.h(error handling).
+ * ToDO:  I may at somepoint modify this subroutine to pass in the image
+ *        type and size in as parameters... I already have the information
+ *        I shouldn't read it in... or perhaps I should just verify that 
+ *        they match???
+ * ToDo:  I should check bitpix and write out the requested size.  At the
+ *        moment I only write float.
+ * 
+ ******************************************************************************/
+
+#include "calfuse.h"
+
+#define CF_PRGM_ID      "cf_fes_write"
+
+int cf_fes_write(fitsfile *outfits, int hdu, float *image)
+{
+	char	buffer[FLEN_CARD];
+	int 	status, hdutype; 
+	int	naxis, naxis1, naxis2;
+        int     fpixel, npixels, bitpix;
+        short   *short_image;
+
+        hdutype = -1;       
+        status = 0;
+
+	FITS_movabs_hdu(outfits, hdu, &hdutype, &status);
+        
+        FITS_read_key(outfits, TINT, "NAXIS1", &naxis1, buffer, &status);
+        FITS_read_key(outfits, TINT, "NAXIS2", &naxis2, buffer, &status);
+        FITS_read_key(outfits, TINT, "BITPIX", &bitpix, buffer, &status);
+
+        fpixel = 1;
+        npixels = naxis1 * naxis2;
+
+        FITS_write_img(outfits, TFLOAT, fpixel, npixels, image, &status);
+
+        return(status);
+}
diff --git a/src/fes/cf_limbang.c b/src/fes/cf_limbang.c
new file mode 100644
index 0000000..8bd230f
--- /dev/null
+++ b/src/fes/cf_limbang.c
@@ -0,0 +1,100 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_limbang_calc(fitsfile *outfits, double mjd)
+ *              cf_min_limbang(fitsfile *outfits, 
+ *                                           double mjd_start, double mjd_end)
+ * Description: cf_limbang_calc - Calculates the limb angle at a given mjd
+ *              cf_min_limbang  - determines the minimum limb angle between
+ *                                 the start and end times. The limb angle is
+ *                                 calculated every 8.6 seconds( .0001 MJD)
+ *
+ * Arguments:   fitsfile  *outfits       Pointer to FITS file containing the
+ *                                      input data and orbital elements
+ *              double    mjd           The limb angle calculation is done for
+ *                                       this time.  The time is given as 
+ *                                       a Modified Julian Date.
+ *              double mjd_start        The range of times for which the minimum
+ *              double mjd_end          limb angle should be determined.
+ *                                      Both are given as Modified Julian Dates.
+ *
+ * History:     08/09/99        mlr     copied cf_velang.c to start
+ *              08/09/99        mlr     removed excess calls then made the
+ *                                      limb_ang calls - same as cf_check_point
+ *
+ ****************************************************************************/
+
+#include <stdio.h>
+#include "calfuse.h"
+#include "sgp4.h"
+static char CF_PRGM_ID[] = "cf_limbang";
+ 
+SGP4   set_orbit_parms(fitsfile *);
+
+double cf_limbang_calc(fitsfile *outfits, double mjd)
+{
+    int    status=0, isday_dummy;
+    char   comment[FLEN_CARD];
+    double ra, dec, pos[3], vel[3];
+    double lim_ang, zdist_dummy;
+    SGP4   sgp4;
+
+    sgp4 = set_orbit_parms(outfits);
+
+    /* get the state vector at time mjd */
+    SGP4_getStateVector(sgp4, mjd, pos, vel);
+    SGP4_precess(pos, mjd, MJD2000); SGP4_precess(vel, mjd, MJD2000);
+
+    FITS_read_key(outfits, TDOUBLE, "RA_TARG", &ra, comment, &status);
+    FITS_read_key(outfits, TDOUBLE, "DEC_TARG", &dec, comment, &status);
+
+    lim_ang = state_limb(pos, mjd, ra, dec, &zdist_dummy, &isday_dummy);
+
+    return(lim_ang);
+}
+
+void cf_min_limbang(fitsfile *outfits, double mjd_start, double mjd_end)
+{
+     
+     int status = 0;
+     double lim_ang, min_lim;
+     double mjd;     
+
+    mjd = mjd_start;
+    min_lim = cf_limbang_calc(outfits, mjd);
+
+#ifdef DEBUG
+    printf("mjd: %lf mjd_end = %lf minlim = %lf\n", mjd, mjd_end, min_lim);
+#endif
+    /* .0001 = 8.6 seconds */
+    while ( (mjd_end - mjd) > .0001 )
+    {
+          mjd = mjd + .0001;
+          lim_ang = cf_limbang_calc(outfits, mjd);
+#ifdef DEBUG
+          printf("mjd: %lf mjd_end = %lf minlim = %lf, limang = %lf\n", 
+                    mjd, mjd_end, min_lim, lim_ang);
+#endif
+          if (lim_ang < min_lim) min_lim = lim_ang;
+    }
+
+    mjd = mjd_end;
+    lim_ang = cf_limbang_calc(outfits, mjd);
+
+#ifdef DEBUG
+    printf("mjd: %lf mjd_end = %lf minlim = %lf, limang = %lf\n", 
+                 mjd, mjd_end, min_lim, lim_ang);
+#endif
+
+    if (lim_ang < min_lim)  min_lim = lim_ang;
+
+#ifdef DEBUG
+    printf("mjd: %lf mjd_end = %lf minlim = %lf\n", mjd, mjd_end, min_lim);    
+#endif
+
+    FITS_update_key(outfits, TDOUBLE, "MIN_LIMB", &min_lim, NULL, &status);
+
+}
diff --git a/src/fuv/Makefile.Linux.orig b/src/fuv/Makefile.Linux.orig
new file mode 100644
index 0000000..da60b24
--- /dev/null
+++ b/src/fuv/Makefile.Linux.orig
@@ -0,0 +1,75 @@
+
+CALFUSEDIR=	${PWD}/../..
+SHARED=		-shared
+FITSVER=	2.470
+
+# Symbols for include directories
+FUSEINCLDIR=	-I${CALFUSEDIR}/include
+
+# Symbols used for compiling
+CC=		cc
+OPT=		-g -Wall -DCFORTRAN -Dg77Fortran -Df2cFortran
+CFLAGS=		${OPT} ${FUSEINCLDIR}
+
+FUSEBINDIR=	${CALFUSEDIR}/bin
+FUSELIBDIR=	-L${CALFUSEDIR}/lib 
+FUSELIBS=	-lcfitsio-${FITSVER} -lsla -lcf
+LIBS=		-lc -lm -lnsl -ldl -lgfortran
+LDFLAGS=	-Wl,-R${CALFUSEDIR}/lib,-R${CALFUSEDIR}/src/libcf
+
+# Symbols used for creating shared libraries
+
+BINS=		cf_hist_init cf_ttag_init cf_convert_to_farf cf_remove_motions \
+                cf_assign_wavelength cf_screen_photons cf_flux_calibrate \
+		cf_extract_spectra cf_countmap cf_gainmap cf_bad_pixels
+
+all:		${BINS}
+		chmod g+w ${BINS}
+
+install:	all
+		/bin/cp -p ${BINS} ${FUSEBINDIR}
+
+clean: 
+	-	/bin/rm -f ${BINS}
+
+distclean: 
+	-	/bin/rm -f ${BINS}
+		cd ../../bin; /bin/rm -f ${BINS} calfuse
+
+cf_hist_init:
+		${CC} ${CFLAGS} -o cf_hist_init cf_hist_init.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_ttag_init:
+		${CC} ${CFLAGS} -o cf_ttag_init cf_ttag_init.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_convert_to_farf:
+		${CC} ${CFLAGS} -o cf_convert_to_farf cf_convert_to_farf.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_remove_motions:
+		${CC} ${CFLAGS} -o cf_remove_motions cf_remove_motions.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_assign_wavelength:
+		${CC} ${CFLAGS} -o cf_assign_wavelength \
+		cf_assign_wavelength.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_screen_photons:
+		${CC} ${CFLAGS} -o cf_screen_photons cf_screen_photons.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_flux_calibrate:
+		${CC} ${CFLAGS} -o cf_flux_calibrate cf_flux_calibrate.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_extract_spectra:
+		${CC} ${CFLAGS} -o cf_extract_spectra cf_extract_spectra.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_countmap:
+		${CC} ${CFLAGS} -o cf_countmap cf_countmap.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_gainmap:
+		${CC} ${CFLAGS} -o cf_gainmap cf_gainmap.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_bad_pixels:
+		${CC} ${CFLAGS} -o cf_bad_pixels cf_bad_pixels.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
diff --git a/src/fuv/Makefile.Linux64.orig b/src/fuv/Makefile.Linux64.orig
new file mode 100644
index 0000000..6fbead0
--- /dev/null
+++ b/src/fuv/Makefile.Linux64.orig
@@ -0,0 +1,74 @@
+
+CALFUSEDIR=	${PWD}/../..
+SHARED=		-shared
+
+# Symbols for include directories
+FUSEINCLDIR=	-I${CALFUSEDIR}/include
+
+# Symbols used for compiling
+CC=		cc
+OPT=		-g -Wall -DCFORTRAN -Dg77Fortran -Df2cFortran
+CFLAGS=		${OPT} ${FUSEINCLDIR}
+
+FUSEBINDIR=	${CALFUSEDIR}/bin
+FUSELIBDIR=	-L${CALFUSEDIR}/lib 
+FUSELIBS=	-lsla -lcf
+LIBS=		-lc -lm -lnsl -ldl -lgfortran -lcfitsio
+LDFLAGS=	-Wl,-R${CALFUSEDIR}/lib,-R${CALFUSEDIR}/src/libcf
+
+# Symbols used for creating shared libraries
+
+BINS=		cf_hist_init cf_ttag_init cf_convert_to_farf cf_remove_motions \
+                cf_assign_wavelength cf_screen_photons cf_flux_calibrate \
+		cf_extract_spectra cf_countmap cf_gainmap cf_bad_pixels
+
+all:		${BINS}
+		chmod g+w ${BINS}
+
+install:	all
+		/bin/cp -p ${BINS} ${FUSEBINDIR}
+
+clean: 
+	-	/bin/rm -f ${BINS}
+
+distclean: 
+	-	/bin/rm -f ${BINS}
+		cd ../../bin; /bin/rm -f ${BINS} calfuse
+
+cf_hist_init:
+		${CC} ${CFLAGS} -o cf_hist_init cf_hist_init.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_ttag_init:
+		${CC} ${CFLAGS} -o cf_ttag_init cf_ttag_init.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_convert_to_farf:
+		${CC} ${CFLAGS} -o cf_convert_to_farf cf_convert_to_farf.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_remove_motions:
+		${CC} ${CFLAGS} -o cf_remove_motions cf_remove_motions.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_assign_wavelength:
+		${CC} ${CFLAGS} -o cf_assign_wavelength \
+		cf_assign_wavelength.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_screen_photons:
+		${CC} ${CFLAGS} -o cf_screen_photons cf_screen_photons.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_flux_calibrate:
+		${CC} ${CFLAGS} -o cf_flux_calibrate cf_flux_calibrate.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_extract_spectra:
+		${CC} ${CFLAGS} -o cf_extract_spectra cf_extract_spectra.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_countmap:
+		${CC} ${CFLAGS} -o cf_countmap cf_countmap.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_gainmap:
+		${CC} ${CFLAGS} -o cf_gainmap cf_gainmap.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_bad_pixels:
+		${CC} ${CFLAGS} -o cf_bad_pixels cf_bad_pixels.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
diff --git a/src/fuv/Makefile.MacOSX.orig b/src/fuv/Makefile.MacOSX.orig
new file mode 100644
index 0000000..acbfaf7
--- /dev/null
+++ b/src/fuv/Makefile.MacOSX.orig
@@ -0,0 +1,76 @@
+
+CALFUSEDIR=	${PWD}/../..
+FITSVER=	2.470
+MACOSX_DEPLOYMENT_TARGET=	10.2
+
+# Symbols for include directories
+FUSEINCLDIR=	-I${CALFUSEDIR}/include
+
+# Symbols used for compiling
+CC=		cc
+OPT=		-O3 -Wall -DCFORTRAN -Dg77Fortran -Df2cFortran
+CFLAGS=		${OPT} ${FUSEINCLDIR}
+
+FUSEBINDIR=	${CALFUSEDIR}/bin
+FUSELIBDIR=	-L${CALFUSEDIR}/lib 
+# FUSELIBS=	-lcfitsio-${FITSVER} -lsla -lcf
+FUSELIBS=	-lcfitsio -lsla -lcf
+LIBS=		-lc -lm -ldl -L/sw/lib/ -lgfortran
+
+BINS=		cf_hist_init cf_ttag_init cf_convert_to_farf cf_remove_motions \
+                cf_assign_wavelength cf_screen_photons cf_flux_calibrate \
+		cf_extract_spectra cf_countmap cf_gainmap cf_bad_pixels
+
+all:		${BINS}
+		chmod g+w ${BINS}
+
+install:	
+		MACOSX_DEPLOYMENT_TARGET="${MACOSX_DEPLOYMENT_TARGET}"; \
+		export MACOSX_DEPLOYMENT_TARGET; \
+		make all
+		/bin/cp -p ${BINS} ${FUSEBINDIR}
+
+clean: 
+	-	/bin/rm -f ${BINS}
+
+distclean: 
+	-	/bin/rm -f ${BINS}
+		cd ../../bin; /bin/rm -f ${BINS} calfuse
+
+cf_hist_init:
+		${CC} ${CFLAGS} -o cf_hist_init cf_hist_init.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS}
+cf_ttag_init:
+		${CC} ${CFLAGS} -o cf_ttag_init cf_ttag_init.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS}
+cf_convert_to_farf:
+		${CC} ${CFLAGS} -o cf_convert_to_farf cf_convert_to_farf.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS}
+cf_remove_motions:
+		${CC} ${CFLAGS} -o cf_remove_motions cf_remove_motions.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS}
+cf_assign_wavelength:
+		${CC} ${CFLAGS} -o cf_assign_wavelength \
+		cf_assign_wavelength.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS}
+cf_screen_photons:
+		${CC} ${CFLAGS} -o cf_screen_photons cf_screen_photons.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS}
+cf_flux_calibrate:
+		${CC} ${CFLAGS} -o cf_flux_calibrate cf_flux_calibrate.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS}
+cf_extract_spectra:
+		${CC} ${CFLAGS} -o cf_extract_spectra cf_extract_spectra.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS}
+cf_countmap:
+		${CC} ${CFLAGS} -o cf_countmap cf_countmap.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS}
+
+cf_gainmap:
+		${CC} ${CFLAGS} -o cf_gainmap cf_gainmap.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS}
+
+cf_bad_pixels:
+		${CC} ${CFLAGS} -o cf_bad_pixels cf_bad_pixels.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS}
+
diff --git a/src/fuv/Makefile.Solaris.orig b/src/fuv/Makefile.Solaris.orig
new file mode 100644
index 0000000..528e6bc
--- /dev/null
+++ b/src/fuv/Makefile.Solaris.orig
@@ -0,0 +1,75 @@
+
+CALFUSEDIR=	${PWD}/../..
+SHARED=		-G
+FITSVER=	2.470
+
+# Symbols for include directories
+FUSEINCLDIR=	-I${CALFUSEDIR}/include
+
+# Symbols used for compiling
+CC=		cc
+OPT=		-O -DCFORTRAN -KPIC
+CFLAGS=		${OPT} ${FUSEINCLDIR}
+
+FUSEBINDIR=	${CALFUSEDIR}/bin
+FUSELIBDIR=	-L${CALFUSEDIR}/lib 
+FUSELIBS=	-lcfitsio-${FITSVER} -lsla -lcf
+LIBS=		-lc -lm -lnsl -ldl -lsocket -lsunmath
+LDFLAGS=	-Wl,-R${CALFUSEDIR}/lib,-R${CALFUSEDIR}/src/libcf
+
+# Symbols used for creating shared libraries
+
+BINS=		cf_hist_init cf_ttag_init cf_convert_to_farf cf_remove_motions \
+                cf_assign_wavelength cf_screen_photons cf_flux_calibrate \
+		cf_extract_spectra cf_countmap cf_gainmap cf_bad_pixels
+
+all:		${BINS}
+		chmod g+w ${BINS}
+
+install:	all
+		/bin/cp -p ${BINS} ${FUSEBINDIR}
+
+clean: 
+	-	/bin/rm -f ${BINS}
+
+distclean: 
+	-	/bin/rm -f ${BINS}
+		cd ../../bin; /bin/rm -f ${BINS} calfuse
+
+cf_hist_init:
+		${CC} ${CFLAGS} -o cf_hist_init cf_hist_init.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_ttag_init:
+		${CC} ${CFLAGS} -o cf_ttag_init cf_ttag_init.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_convert_to_farf:
+		${CC} ${CFLAGS} -o cf_convert_to_farf cf_convert_to_farf.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_remove_motions:
+		${CC} ${CFLAGS} -o cf_remove_motions cf_remove_motions.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_assign_wavelength:
+		${CC} ${CFLAGS} -o cf_assign_wavelength \
+		cf_assign_wavelength.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_screen_photons:
+		${CC} ${CFLAGS} -o cf_screen_photons cf_screen_photons.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_flux_calibrate:
+		${CC} ${CFLAGS} -o cf_flux_calibrate cf_flux_calibrate.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_extract_spectra:
+		${CC} ${CFLAGS} -o cf_extract_spectra cf_extract_spectra.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_countmap:
+		${CC} ${CFLAGS} -o cf_countmap cf_countmap.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_gainmap:
+		${CC} ${CFLAGS} -o cf_gainmap cf_gainmap.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_bad_pixels:
+		${CC} ${CFLAGS} -o cf_bad_pixels cf_bad_pixels.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
diff --git a/src/fuv/Makefile.orig.orig b/src/fuv/Makefile.orig.orig
new file mode 100644
index 0000000..528e6bc
--- /dev/null
+++ b/src/fuv/Makefile.orig.orig
@@ -0,0 +1,75 @@
+
+CALFUSEDIR=	${PWD}/../..
+SHARED=		-G
+FITSVER=	2.470
+
+# Symbols for include directories
+FUSEINCLDIR=	-I${CALFUSEDIR}/include
+
+# Symbols used for compiling
+CC=		cc
+OPT=		-O -DCFORTRAN -KPIC
+CFLAGS=		${OPT} ${FUSEINCLDIR}
+
+FUSEBINDIR=	${CALFUSEDIR}/bin
+FUSELIBDIR=	-L${CALFUSEDIR}/lib 
+FUSELIBS=	-lcfitsio-${FITSVER} -lsla -lcf
+LIBS=		-lc -lm -lnsl -ldl -lsocket -lsunmath
+LDFLAGS=	-Wl,-R${CALFUSEDIR}/lib,-R${CALFUSEDIR}/src/libcf
+
+# Symbols used for creating shared libraries
+
+BINS=		cf_hist_init cf_ttag_init cf_convert_to_farf cf_remove_motions \
+                cf_assign_wavelength cf_screen_photons cf_flux_calibrate \
+		cf_extract_spectra cf_countmap cf_gainmap cf_bad_pixels
+
+all:		${BINS}
+		chmod g+w ${BINS}
+
+install:	all
+		/bin/cp -p ${BINS} ${FUSEBINDIR}
+
+clean: 
+	-	/bin/rm -f ${BINS}
+
+distclean: 
+	-	/bin/rm -f ${BINS}
+		cd ../../bin; /bin/rm -f ${BINS} calfuse
+
+cf_hist_init:
+		${CC} ${CFLAGS} -o cf_hist_init cf_hist_init.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_ttag_init:
+		${CC} ${CFLAGS} -o cf_ttag_init cf_ttag_init.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_convert_to_farf:
+		${CC} ${CFLAGS} -o cf_convert_to_farf cf_convert_to_farf.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_remove_motions:
+		${CC} ${CFLAGS} -o cf_remove_motions cf_remove_motions.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_assign_wavelength:
+		${CC} ${CFLAGS} -o cf_assign_wavelength \
+		cf_assign_wavelength.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_screen_photons:
+		${CC} ${CFLAGS} -o cf_screen_photons cf_screen_photons.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_flux_calibrate:
+		${CC} ${CFLAGS} -o cf_flux_calibrate cf_flux_calibrate.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_extract_spectra:
+		${CC} ${CFLAGS} -o cf_extract_spectra cf_extract_spectra.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+cf_countmap:
+		${CC} ${CFLAGS} -o cf_countmap cf_countmap.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_gainmap:
+		${CC} ${CFLAGS} -o cf_gainmap cf_gainmap.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+cf_bad_pixels:
+		${CC} ${CFLAGS} -o cf_bad_pixels cf_bad_pixels.c \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
diff --git a/src/fuv/cf_assign_wavelength.c b/src/fuv/cf_assign_wavelength.c
new file mode 100644
index 0000000..d84c7a0
--- /dev/null
+++ b/src/fuv/cf_assign_wavelength.c
@@ -0,0 +1,178 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_assign_wavelength options intermediate_data_file
+ *
+ * Description: Assign a wavelength to each photon, correcting for
+ *              spacecraft motion and instrumental astigmatism.  
+ *		The final wavelength scale is heliocentric.
+ *
+ *              By default all corrections are performed.  Command-line
+ *              options allow one or more corrections to be omitted.
+ *
+ * Arguments:   input_file              FARF-corrected intermediate data file
+ *
+ * Calibration files:                   ASTG_CAL, WAVE_CAL
+ *
+ * Returns:     0 on successful completion
+ *
+ * Calls:       cf_astigmatism, cf_dispersion, cf_doppler_and_heliocentric
+ *
+ * History:     11/05/02   1.1   peb    Begin work
+ *		12/16/02   1.2   wvd    Install subroutines.
+ *		02/12/03   1.3   wvd    Change ORBITAL_VELOCITY to ORBITAL_VEL
+ *              03/10/03   1.4   peb    Added verbose_level, changed channel to
+ *                                      char *, and added unistd.h for getopt
+ *                                      portability
+ *		03/12/03   1.5   wvd    If lambda[k] is undefined,
+ *					set channel[k] = 0 in IDF
+ *		03/23/03   1.6   wvd    If -w option is set, write astigmatism-
+ *					corrected X values to IDF.
+ *		06/11/03   1.7   wvd    Pass datatype to cf_read_col and
+ *					cf_write_col.
+ *		08/25/03   1.8   wvd	Change coltype from string to int in
+ *					cf_read_col and cf_write_col.
+ *		09/16/03   1.9   wvd	Write comment lines to IDF header if
+ *					-w option is requested.
+ *		10/31/03   1.10  wvd	Change channel to unsigned char.
+ *		12/03/03   1.11  wvd	Initialize astig_return to 1.
+ *              04/06/04   1.12  bjg    Function returns EXIT_SUCCESS
+ *                                      Fix option[]
+ *		06/21/04   1.13  wvd	If -w flag is set, run the program
+ *					even if it's been run before.
+ *		05/20/05   1.14  wvd	Clean up i/o.
+ *		05/15/06   1.15  wvd	Divide cf_astigmatism_and_dispersion
+ *					into two routines.  Note that wave-
+ *					length calibration is performed even
+ *					if astigmatism correction is not.
+ *
+ ****************************************************************************/
+
+#include <unistd.h>
+#include <stdlib.h>
+#include "calfuse.h"
+
+int
+main(int argc,  char *argv[])
+{
+    char CF_PRGM_ID[] = "cf_assign_wavelength";
+    char CF_VER_NUM[] = "1.15";
+
+    char comment[FLEN_CARD], datestr[FLEN_CARD];
+    unsigned char *channel=NULL;
+    int  astig_corr=1, doppler_corr=1, status=0, optc, timeref;
+    int  astig_return=1, wavecal = FALSE;
+    long nevents, nseconds;
+    float *time=NULL, *x=NULL, *y=NULL, *lambda=NULL, *timeline=NULL;
+    float *velocity=NULL;
+    fitsfile *header;
+    
+    char opts[]  = "hadwv:";
+    char usage[] = 
+	"Usage:\n"
+	"  cf_assign_wavelength [-hadw] [-v level] idf_file\n";
+    char option[] =
+	"Options:\n"
+	"  -h:  this help message\n"
+	"  -v:  verbose mode (default is 1; 0 is silent)\n"
+	"  -a:  no astigmatism correction\n"
+	"  -d:  no doppler correction\n"
+	"  -w:  write astigmatism-corrected X values to IDF\n";
+
+    verbose_level = 1;
+
+    while ((optc = getopt(argc, argv, opts)) != -1) {
+	switch(optc) {
+
+	case 'h':
+	    printf("%s\n%s", usage, option);
+	    return 0;
+	case 'v':
+	    verbose_level = atoi(optarg);
+	    break;
+	case 'a':
+	    astig_corr = 0;
+	    break;
+	case 'd':
+	    doppler_corr = 0;
+	    break;
+	case 'w':
+	    wavecal = TRUE;
+	    break;
+	}
+    }
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    if (argc <= optind) {
+        printf("%s", usage);
+        cf_if_error("Incorrect number of program arguments");
+    }
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    FITS_open_file(&header, argv[optind], READWRITE, &status);
+
+    FITS_movabs_hdu(header, 2, NULL, &status);
+    nevents = cf_read_col(header, TFLOAT, "TIME",   (void **) &time);
+    nevents = cf_read_col(header, TFLOAT, "X",      (void **) &x);
+    nevents = cf_read_col(header, TFLOAT, "Y",      (void **) &y);
+    nevents = cf_read_col(header, TBYTE,  "CHANNEL",(void **) &channel);
+    nevents = cf_read_col(header, TFLOAT, "LAMBDA", (void **) &lambda);
+
+    FITS_movabs_hdu(header, 4, NULL, &status);
+    nseconds = cf_read_col(header, TFLOAT, "TIME",        (void **) &timeline);
+    nseconds = cf_read_col(header, TFLOAT, "ORBITAL_VEL", (void **) &velocity);
+    FITS_movabs_hdu(header, 1, NULL, &status);
+
+    if (wavecal) {
+        FITS_update_key(header, TSTRING, "WAVE_COR", "PERFORM", NULL, &status);
+        FITS_update_key(header, TSTRING, "DOPP_COR", "PERFORM", NULL, &status);
+    }
+
+    /* Correct X coordinate for 2-D astigmatism. */
+    if (astig_corr)
+	astig_return = cf_astigmatism(header, nevents, x, y, channel);
+
+    /* Assign wavelength to each photon event according to channel and X */
+    cf_dispersion(header, nevents, x, channel, lambda);
+
+    /* Correct for spacecraft motion and shift to heliocentric wavelength scale. */
+    if (doppler_corr)
+	cf_doppler_and_heliocentric(header, nevents, time, channel,
+	    lambda, nseconds, timeline, velocity);
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+    FITS_movabs_hdu(header, 2, NULL, &status);
+    cf_write_col(header, TBYTE,  "CHANNEL", (void *) channel, nevents);
+    cf_write_col(header, TFLOAT, "LAMBDA",  (void *) lambda, nevents);
+
+    /* If -w option is requested and astigmatism correction was applied,
+	write astigmatism-corrected X array to IDF. */
+    if (wavecal && !astig_return) {
+	cf_write_col(header, TFLOAT, "X", (void *) x, nevents);
+        FITS_movabs_hdu(header, 1, NULL, &status);
+	sprintf(comment, "Writing astigmatism-corrected X array to IDF.");
+        cf_if_warning(comment);
+        FITS_write_comment(header, "  ", &status);
+        FITS_write_comment(header, comment, &status);
+        fits_get_system_time(datestr, &timeref, &status);
+        sprintf(comment, "CalFUSE v%s   %.10s", CALFUSE_VERSION, datestr);
+        FITS_write_comment(header, comment, &status);
+        FITS_write_comment(header, "  ", &status);
+    }
+
+    FITS_close_file(header, &status);
+
+    free(velocity);
+    free(timeline);
+    free(lambda);
+    free(channel);
+    free(y);
+    free(x);
+    free(time);
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return EXIT_SUCCESS;
+}
diff --git a/src/fuv/cf_bad_pixels.c b/src/fuv/cf_bad_pixels.c
new file mode 100644
index 0000000..a10ed20
--- /dev/null
+++ b/src/fuv/cf_bad_pixels.c
@@ -0,0 +1,1001 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_bad_pixels options input_file
+ *
+ * Description: Determines a map of the bad pixels on the detector, after
+ *		correction for image motions during the observation. The
+ *		procedure works by generating a series of pseudo photons
+ *		corresponding to bad pixels within the area of the detector
+ *		seen by the target aperture. This list of pseudo photons is
+ *		repeated for each second of the observation where the data
+ *		is expected to be acceptable (i.e., it excludes times of
+ *		bursts, SAA passages, etc). The list is then run through
+ *		various routines in the pipeline which correct for photon
+ *		motions. A map is then generated from the final photon
+ *		list.  
+ *
+ * Arguments:   input_file              FARF-corrected intermediate data
+ *                                      file
+ * Calibration files:  QUAL_CAL                 
+ *
+ * Returns:     file containing the bad pixel map 
+ *
+ *
+ * History:     04/08/03   1.0   rdr   Begin work
+ *		04/30/03   1.1   wvd   Install
+ *		05/22/03   1.2   wvd   Modify call to cf_set_photon_flags
+ *              05/28/03   1.3   rdr   Made adjustments for HIST data and 
+ *                                      correct some bugs
+ *		05/04/03   1.4   wvd   Reset JITR_COR and FLAG_COR to PERFORM.
+ *				 	Pass weights to cf_set_photon_flags.
+ *              09/06/03   1.5   rdr   Incorporate tscreen flag.
+ *		06/11/03   1.6   wvd   Pass datatype to cf_read_col and
+ *					cf_write_col.
+ *		08/22/03   1.7   wvd   Change channel array to unsigned char.
+ *					Delete GTI from call to
+ *					cf_satellite_jitter.
+ *		08/25/03   1.8   wvd   Change coltype from string to int in
+ *					cf_read_col.
+ *              10/17/03   1.9   wvd   If EXPTIME = 0, exit without
+ *                                      generating a bad-pixel file.
+ *              11/05/03   1.10  wvd   Change chan_pix to unsigned char
+ *              11/05/03   1.11  wvd   Use fits_create_tbl alone to make
+ *					binary table extension.
+ *              12/01/03   1.12  bjg   Update FILENAME, FILETYPE and IDF_FILE
+ *                                      keywords.
+ *              12/01/03   1.13  bjg   Minor changes.
+ *              12/21/03   1.14  wvd   Remove underscore from idf and bpm
+ *					filenames.
+ *              02/24/04   1.15  rdr   change maximum size of the output
+ *                                     arrays in cf_combine_pothole_data
+ *              03/03/04   1.16  rdr   make sure that lif_cnt and sic_cnt arrays 
+ *                                     are non-zero
+ *              04/06/04   1.19  bjg   Include ctype.h and strings.h
+ *                                     Change formats to match arg types in 
+ *                                     printf
+ *                                     Change ( a<b & a>c ) to ((a<b)&&(a>c)) 
+ *                                     in cf_combine_pothole_data
+ *                                     Create potholes from HIST FILL_DATA
+ *              06/07/04   1.20  wvd   Add exp_jitr to cf_satellite_jitter(),
+ *				   	delete timeline from cf_apply_filters.
+ *              07/21/04   1.21  wvd   Delete unused variable nmax in
+ *					cf_generate_pseudo_photons
+ *              10/29/04   1.22  bjg   Added check for selected potholes that
+ *                                     fall out the extraction window
+ *              12/02/04   1.23  wvd   If a processing step was skipped for
+ *                                      the data file, skip it also for the
+ *                                      bpm file.
+ *              01/27/05   1.24  wvd   Ignore LIMB, SAA, and BRST when 
+ *					determining good times for HIST data.
+ *		02/01/05   1.25  wvd   In cf_generate_pseudo_photons, pad
+ *					extraction windows by ten pixels
+ *					when making pothole list.  
+ *				       In cf_combine_pothole_data, toss any
+ *					potholes that drift out of extraction
+ *					window.  Call cf_get_extraction_limits
+ *					only when the aperture changes.
+ *		02/17/05   1.26  wvd   Increase estimated size of output 
+ *					pixel arrays (nmax) by 20%.
+ *					Add additional diagnostic output.
+ *		03/15/05   1.27  wvd   Replace cf_get_extraction_limits with
+ *					cf_extraction_limits
+ *		03/16/05   1.28  wvd   Pass srctype to cf_extraction_limits.
+ *              03/22/05   1.29  wvd   Change TIME_SUNRISE and TIME_SUNSET
+ *                                      from floats to shorts.
+ *              03/22/05   1.30  wvd   In cf_combine_pothole_data, use fabs()
+ *					when looking for changes in the time
+ *					array.
+ *              04/12/05   1.31  wvd   Add -n flag, which forces creation
+ *                                      of night-only BPM file.  Its argument
+ *                                      is the name of the output BPM file.
+ *					This file name is NOT written to the
+ *					IDF file header.
+ *              06/03/05   1.32  wvd   Include math.h
+ *              11/25/05   1.33  wvd   Use cf_x2lambda and cf_get_potholes
+ *					rather than writing new routines here.
+ *					Don't add random numbers to output
+ *					pixel coordinates.
+ *              05/15/06   1.34  wvd    Divide cf_astigmatism_and_dispersion
+ *                                      into two routines.  Note that wave-
+ *                                      length calibration is performed even
+ *                                      if astigmatism correction is not.
+ *					Add ASTG_COR to list of updated
+ *					keywords.
+ *              06/13/06   1.35  wvd    In cf_combine_pothole_data,
+ *					initialize nfill to 0 before each
+ *					iteration and ignore bad pixels that
+ *					lie outside of the extraction window.
+ *              03/20/07   1.36  wvd    In cf_combine_pothole_data, if the
+ *					entire dead spot falls outside of the
+ *					aperture, stop and move on to the
+ *					next one.
+ *              03/21/07   1.37  wvd    Replace "break" with "continue" in
+ *					cf_combine_pothole_data.
+ *		04/03/07   1.38  wvd	Scale nmax by 1.5.  Call cf_error_init
+ *					after each call to cf_extraction_limits.
+ *					Make CF_PRGM_ID and CF_VER_NUM static
+ *					variables.
+ *		04/03/07   1.39  bot	In cf_generate_pseduo_photons, l.198
+ *					and l.219 added a test on LOCATION_SHLD
+ * 					for FILL DATA.
+ *		07/18/08   1.40  wvd	If EXP_STAT = 2, target is bright
+ *					earth/airglow. Mask out limb-angle flag.
+ *
+ ****************************************************************************/
+
+#include <strings.h>
+#include <string.h>
+#include <stdio.h>
+#include <unistd.h>
+#include <stdlib.h>
+#include <ctype.h>
+#include <math.h>
+#include "calfuse.h"
+
+static char CF_PRGM_ID[] = "cf_bad_pixels"; 
+static char CF_VER_NUM[] = "1.40";
+
+
+/****************************************************************************
+ *
+ *              CF_GENERATE_PSEUDO_PHOTONS
+ *
+ *   Procedure to generate an array of pseudo photons to represent the
+ *   locations of the detector potholes
+ *
+ ****************************************************************************/
+
+int cf_generate_pseudo_photons(fitsfile *header, long ngood, long *good_index, 
+        float *timeline, unsigned char *statflag, float *lif_cnt,
+	float *sic_cnt, long *nevents, float **time, float **weight,
+	float **x, float **y, unsigned char **channel, float **rx,
+	float **ry, unsigned char **timeflag, unsigned char **loc_flag) {
+
+  char instmode[FLEN_CARD] ;
+  long nevts, npot, nfill=0, npot_sel; 
+  int *bpndx, npot2, status=0, hdutype ;
+  int srctype, ap[2], bymax, bymin, pad=10 ;
+  short *ylow, *yhigh; 
+  long npts, i, j, k, xndx, num, num_tot, ndx, tndx ;
+  float *xpot, *ypot, *rxpot, *rypot ;
+  float *xpot2, *ypot2, *rxpot2, *rypot2 ;
+  float *xval, *yval, *rxval, *ryval, *xout, *yout, *rxout, *ryout ;
+  float *time_out, *weight_out, tval, ctot_lif, ctot_sic ;
+  float wval_lif, wval_sic ;
+  short binx, biny, xmin, xmax;
+  unsigned char *chan, *chan_out;
+  unsigned char *tflag_out, tflag_val ;
+  char * hdu2_loc_flgs;
+  float * hdu2_xfarf, * hdu2_yfarf;
+
+
+  cf_verbose(3, "Generating pseudo-photons") ;
+
+  /* read the instrument mode for the data */
+    FITS_movabs_hdu(header, 1, &hdutype, &status);
+    FITS_read_key(header, TSTRING, "INSTMODE", instmode, NULL, &status) ;
+    FITS_read_key(header, TSHORT, "SPECBINX", &binx, NULL, &status) ;
+    FITS_read_key(header, TSHORT, "SPECBINY", &biny, NULL, &status) ;
+
+  /* read the header and determine the target apertures for the exposure */
+  srctype = cf_source_aper(header, ap) ;
+  cf_verbose(3,"Target apertures = %d and %d ",ap[0],ap[1]) ;
+
+  /* read in the pothole positions */
+  npot2 = cf_get_potholes(header, &xpot2, &ypot2, &rxpot2, &rypot2) ; 
+  cf_verbose(3, "number of potholes found = %d ",npot2) ;
+
+  if (!(strncasecmp(instmode,"HIST",4))) {
+    FITS_movabs_hdu(header, 2, &hdutype, &status);
+    nevts=cf_read_col(header,TBYTE,"LOC_FLGS",(void **) &hdu2_loc_flgs);
+    nevts=cf_read_col(header,TFLOAT,"XFARF",(void **) &hdu2_xfarf);
+    nevts=cf_read_col(header,TFLOAT,"YFARF",(void **) &hdu2_yfarf);
+    for (j=0;j<nevts;++j) {
+      if (!((hdu2_loc_flgs[j] & LOCATION_FILL) == 0) &&
+	   ((hdu2_loc_flgs[j] & LOCATION_SHLD) == 0)) ++nfill;
+    }
+    cf_verbose(3, "number of FILL DATA potholes found = %d ",nfill) ;
+    npot=npot2+nfill;
+
+    xpot=(float *) cf_calloc(npot, sizeof(float)) ;
+    ypot=(float *) cf_calloc(npot, sizeof(float)) ;
+    rxpot=(float *) cf_calloc(npot, sizeof(float)) ;
+    rypot=(float *) cf_calloc(npot, sizeof(float)) ;
+
+    for (j=0;j<npot2;++j){
+      xpot[j]=xpot2[j];
+      ypot[j]=ypot2[j];
+      rxpot[j]=rxpot2[j];
+      rypot[j]=rypot2[j];
+    }
+
+    k=npot2;
+
+    for (j=0;j<nevts;++j){
+      if (!((hdu2_loc_flgs[j] & LOCATION_FILL) == 0) &&
+	   ((hdu2_loc_flgs[j] & LOCATION_SHLD) == 0)) {
+	
+	xpot[k]=hdu2_xfarf[j];
+	ypot[k]=hdu2_yfarf[j];
+	rxpot[k]=binx;
+	rypot[k]=biny;
+	k++;
+
+      }
+    }
+    free(hdu2_loc_flgs) ;
+    free(hdu2_xfarf) ;
+    free(hdu2_yfarf) ;
+  }
+  else {
+    npot=npot2;
+    xpot=xpot2;
+    ypot=ypot2;
+    rxpot=rxpot2;
+    rypot=rypot2;
+  }  
+
+  /* allocate space to hold the pothole list (for 1 second of data) */
+  xval = (float *) cf_calloc(npot, sizeof(float)) ;
+  yval = (float *) cf_calloc(npot, sizeof(float)) ;
+  rxval = (float *) cf_calloc(npot, sizeof(float)) ;
+  ryval = (float *) cf_calloc(npot, sizeof(float)) ;
+  chan = (unsigned char *) cf_calloc(npot, sizeof(char)) ;
+  num=-1 ;
+
+
+    cf_verbose(3, "For initial pothole selection, "
+	"we pad extraction windows by %d pixels in Y.", pad);
+
+  /* do each aperture separately */
+
+  for (j=0 ; j<2; j++) {
+
+  /* get the extraction limits for the relevant apertures */
+    npts = cf_extraction_limits(header, ap[j], srctype,
+	&ylow, &yhigh, &xmin, &xmax) ;
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+    /* select potholes located within the extraction window */
+    bpndx = (int *) cf_calloc(npot, sizeof(int)) ;
+    npot_sel = -1 ; 
+    for (i=0; i<npot; i++) {
+      xndx = (int) (xpot[i] + 0.5) ;
+      bymax = (int) (ypot[i]+rypot[i]+0.5) ;
+      bymin = (int) (ypot[i]-rypot[i]) ;
+      if ( bymax >= ylow[xndx] - pad  && bymin <= yhigh[xndx] + pad ) {
+        npot_sel += 1 ;
+        bpndx[npot_sel] = i ;
+	cf_verbose(3, "pothole %d selected: x=%d, y=%d, rx=%d, ry=%d ", i,
+	cf_nint(xpot[i]),cf_nint(ypot[i]),cf_nint(rxpot[i]),cf_nint(rypot[i]));
+      }
+    }
+
+    /* convert npot_sel from an array index to a number of potholes selected */
+    npot_sel++ ;
+    cf_verbose(3, "number of potholes selected for ap %d = %d ",
+	ap[j], npot_sel) ;
+
+    /* put the locations into the output arrays */
+    for (i=0; i<npot_sel; i++) {
+      num+=1 ;
+      ndx = bpndx[i] ;
+      xval[num] = xpot[ndx] ;
+      yval[num] = ypot[ndx] ; 
+      chan[num] = ap[j] ;
+      rxval[num] = rxpot[ndx] ;
+      ryval[num] = rypot[ndx] ;
+    }
+  }
+
+  /* convert num from an index to the number of potholes found */
+  num+=1 ;
+  cf_verbose(3, "total number of potholes found = %d ",num) ;
+
+  /* generate a timeline with only the good times included */
+  num_tot = num * ngood ;
+
+  /* copy the non-zero values into the output arrays */
+  time_out = (float *) cf_calloc(num_tot, sizeof(float)) ;
+  weight_out = (float *) cf_calloc(num_tot, sizeof(float)) ;
+  xout = (float *) cf_calloc(num_tot, sizeof(float)) ;
+  yout = (float *) cf_calloc(num_tot, sizeof(float)) ;
+  rxout = (float *) cf_calloc(num_tot, sizeof(float)) ;
+  ryout = (float *) cf_calloc(num_tot, sizeof(float)) ;
+  chan_out = (unsigned char *) cf_calloc(num_tot, sizeof(char)) ;
+  tflag_out = (unsigned char *) cf_calloc(num_tot, sizeof(char)) ;
+  *loc_flag = (unsigned char *) cf_calloc(num_tot, sizeof(char)) ;
+
+  tndx=-1 ;
+  ctot_lif = 0. ;
+  ctot_sic = 0. ;
+  for (j=0; j<ngood; j++) {
+    ndx=good_index[j] ;
+      tval = timeline[ndx] ;
+      ctot_lif += lif_cnt[ndx] ;
+      ctot_sic += sic_cnt[ndx] ;
+      wval_lif = lif_cnt[ndx] ;
+      wval_sic = sic_cnt[ndx] ;
+      tflag_val = statflag[ndx] ;
+    for (i=0; i<num; i++) {
+      tndx += 1;
+      if (tndx > num_tot -1) {
+          cf_verbose(2, "overflow tndx while filling pothole array ") ;
+          tndx= num_tot-1 ; }
+      time_out[tndx] = tval ;
+        if (chan[i] < 4) weight_out[tndx] = wval_lif ;
+        else weight_out[tndx] = wval_sic ;
+      xout[tndx] = xval[i] ;
+      yout[tndx] = yval[i] ;
+      rxout[tndx] = rxval[i] ;
+      ryout[tndx] = ryval[i] ;
+      chan_out[tndx] = chan[i] ;
+      tflag_out[tndx] = tflag_val ;
+    }
+  }
+
+  /* normalize the weights for TTAG data and set to 1 for HIST data*/
+  if (!strncmp(instmode,"T",1)) 
+    for (i=0; i<num_tot; i++) {
+      if (chan_out[i] < 4) weight_out[i] /= ctot_lif ;
+      else weight_out[i] /= ctot_sic ;
+  }
+  else for (i=0; i<num_tot; i++) weight_out[i] = 1. ;
+
+  /* assign pointers to output variables */
+  *x = xout ;
+  *y = yout ;
+  *rx = rxout ;
+  *ry = ryout ;
+  *channel = chan_out ;
+  *timeflag = tflag_out ;
+  *nevents = num_tot ;
+  *weight = weight_out ;
+  *time = time_out ;
+
+  free(xval) ;
+  free(yval) ;
+  free(rxval) ;
+  free(ryval) ;
+  free(chan) ;
+  free(bpndx) ;
+
+  return 0;
+
+}
+
+
+/*******************************************************************************
+ *
+ *                     CF_CORRECT_DOPPLER_MOTIONS
+ *  
+ *    procedure to correct the pothole centroid positions for doppler effects
+ *
+ ******************************************************************************/
+
+ int cf_correct_doppler_motions(fitsfile *header, long nevents, float *time,
+	float *x, unsigned char *channel, long nseconds, float *timeline,
+	float *velocity)
+{
+    char  	wave_file[FLEN_FILENAME];
+    float	*wavelength, v_helio, vel, lam, dlam, dx;
+    fitsfile 	*wavefits;
+    int   	status=0, anynull;
+    int	  	fcol, targ_ap[2], ap, ii;
+    long	i, k, ndx ;
+
+    /* get the information needed in the analysis */
+
+    /* first determine the target apertures */
+    cf_source_aper(header, targ_ap) ;
+    cf_verbose(3, "target apertures = %d and %d ",targ_ap[0], targ_ap[1]) ;
+
+    /* read in the wavelength calibration */
+    FITS_read_key(header, TSTRING, "WAVE_CAL", wave_file, NULL, &status);
+    FITS_open_file(&wavefits, cf_cal_file(wave_file), READONLY, &status);
+    wavelength = (float *) cf_calloc(NXMAX, sizeof(float));
+
+    /* read the heliocentric velocity from the header */
+     FITS_read_key(header, TFLOAT, "V_HELIO", &v_helio, NULL, &status);
+    cf_verbose(3, "heliocentric velocity = %f ",v_helio) ;
+
+    /* Go through each target aperture  */
+    for (i = 0; i < 2; i++) {
+      ap = targ_ap[i] ;
+
+    	FITS_movabs_hdu(wavefits, ap+1, NULL, &status);
+        FITS_get_colnum(wavefits, TRUE, "WAVELENGTH", &fcol, &status);
+        fits_read_col(wavefits, TFLOAT, fcol, 1, 1, NXMAX, NULL, wavelength, 
+			&anynull, &status);
+
+	ndx = 0 ;
+       for (k = 0; k < nevents; k++) 
+	    if (channel[k] == ap) {
+	      while (time[k] >= timeline[ndx] )	ndx++ ; 
+	      if (ndx > nseconds-1 ) ndx=nseconds-1 ;
+	        ii = (int) (x[k] + 0.5);
+		if (ii >= 1 && ii < NXMAX) {
+	            lam = wavelength[ii];
+                    vel = velocity[ndx] + v_helio ;
+	            dlam = vel * lam / C ;
+                    dx = dlam / ( wavelength[ii] - wavelength[ii-1]) ;
+		    x[k] += dx ;
+		    if (vel > 100 || vel < -100 ) 
+                         cf_if_warning ("at k=%ld, time=%f, lam=%f, vel=%f, "
+				"dlam=%f, dx=%f \n",
+				 k, time[k], lam, vel, dlam, dx) ;
+		}
+	    }
+
+    }
+    free(wavelength);
+    FITS_close_file(wavefits, &status);
+
+    return status;
+}
+
+
+/*******************************************************************************
+ *
+ *                     CF_COMBINE_POTHOLE_DATA
+ *
+ *    procedure to combine the centroid data as a function of time with the 
+ *    pothole size information to generate a list of affected pixels on the
+ *    detector
+ *
+ ******************************************************************************/
+
+ long cf_combine_pothole_data(fitsfile *header, long nevents, float *time, 
+        float *weight, float *x, float *rx, float *y, float *ry,
+	unsigned char *channel, unsigned char *timeflag, float **xpix,
+	float **ypix, unsigned char **chan_pix, float **wt_pix) {
+
+   int srctype, expstat, aperture[2];
+   int  npot, xndx, yndx, ap, nfill ;
+   short sxmin, sxmax, *ylow, *yhigh ;
+   int  xdim1, ydim1, xmin1, xmax1, ymin1, ymax1 ;
+   int xminp, xmaxp, yminp, ymaxp ;
+   long i, j, k, l, m, num, numt ;
+   long nout, nmax, npts1, npts2, xdim, ydim, ndx, ndxp ;
+   float *xpixt, *ypixt, *wt_pixt, xmin, xmax, ymin, ymax ;
+   float *array1, *array2, wtot, wval, wmax ;
+   float xv2, yv2, rx2, ry2, pos, xval, yval ;
+   float rxp, ryp, xv, yv, time0 ;  
+   unsigned char *chan_pixt;
+
+   int status=0;
+   char instmode[FLEN_VALUE];
+   unsigned char TEMPORAL_MASK;
+
+   cf_verbose(3, "Combining pothole data") ;
+
+    /* 
+     *  Read INSTMODE keyword.  If in HIST mode, mask out
+     *  LIMB, SAA, and BRST flags.  TEMPORAL_DAY is the default.
+     */
+    TEMPORAL_MASK = TEMPORAL_DAY;
+    FITS_read_key(header, TSTRING, "INSTMODE", instmode, NULL, &status);
+    if (!strncmp(instmode, "HIST", 4)) {
+	TEMPORAL_MASK |= TEMPORAL_LIMB;
+	TEMPORAL_MASK |= TEMPORAL_SAA;
+	TEMPORAL_MASK |= TEMPORAL_BRST;
+    }
+    /*
+     * If EXP_STAT = 2, target is bright earth/airglow.  Mast out limb-angle flag.
+     */
+    FITS_read_key(header, TINT, "EXP_STAT", &expstat, NULL, &status);
+    if (expstat == 2) TEMPORAL_MASK |= TEMPORAL_LIMB;
+
+   /* Read source type from header. */
+   srctype = cf_source_aper(header, aperture) ;
+
+   /* determine the number of potholes by looking at the number
+	of entries for time=time[0] */
+
+   time0 = time[0] ;
+   i = 1 ;
+   while (fabs((time[i] - time0)) < 0.5) i++ ;
+   cf_verbose(3, "Number of potholes found = %d ", npot = i) ;
+
+   nmax = 0;
+   /* estimate size of the array needed to store the data and open
+      arrays to contain it */   
+    for (i=0; i<npot; i++) nmax += (60.+2.*rx[i]) * (30.+2*ry[i]) ;
+	nmax *= 1.5;
+      cf_verbose(3, "Estimated storage space needed for output array = %d ",
+	nmax) ;
+      xpixt = (float *) cf_calloc(nmax, sizeof(float)) ;
+      ypixt = (float *) cf_calloc(nmax, sizeof(float)) ;
+      wt_pixt = (float *) cf_calloc(nmax, sizeof(float)) ;
+      chan_pixt = (unsigned char *) cf_calloc(nmax, sizeof(char)) ;
+
+      /* initialize nout = total number of pixels affected by potholes */
+      nout = -1 ;
+
+      /* process each pothole individually */ 
+
+      ap = -1;
+      for (i=0; i<npot; i++) {
+
+	nfill = 0;
+
+	/* If channel has changed, get the new extraction limits */
+	if (ap != (int) channel[i]) {
+	    ap = (int) channel[i] ;
+            (void) cf_extraction_limits(header, ap, srctype,
+		&ylow, &yhigh, &sxmin, &sxmax);
+    	    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+	}
+	
+    	/* determine the range in X and Y for the pothole centroid positions */
+	xmin = 17000. ;
+        xmax = 0. ;
+        ymin = 1024. ;
+        ymax = 0. ;
+        numt = 0 ;
+        for (j=i; j<nevents ; j+= npot) { 
+	  numt ++ ;
+	     if ((x[j] > xmax) && (x[j] < 16383)) xmax = x[j] ;
+             if ((x[j] < xmin) && (x[j] > 0)) xmin = x[j] ;
+             if ((y[j] > ymax) && (y[j] < 1023)) ymax = y[j] ;
+             if ((y[j] < ymin) && (y[j] > 0)) ymin = y[j] ;
+	}
+      cf_verbose(3,"For pothole %.1d, xmin=%.1d, "
+	"xmax=%.1d, ymin=%.1d, ymax=%.1d",
+	i, cf_nint(xmin), cf_nint(xmax), cf_nint(ymin), cf_nint(ymax)) ;
+
+      /* set up a 2D array which contains all of the movement in the pothole */
+      xdim = (long) (xmax - xmin + 1.5) ;
+      ydim = (long) (ymax - ymin + 1.5) ;
+      npts1 = xdim * ydim  ;
+      cf_verbose(3, "Setting up array1: xdim=%d, ydim=%d, npts=%d ",
+		xdim, ydim, npts1) ;
+      array1 = (float *) cf_calloc(npts1, sizeof(float)) ;
+
+      /* Determine the 2D distribution of positions for the pothole */
+      num = 0 ;
+      for (j=i ; j<nevents ; j+= npot) 
+        if (!(timeflag[j] & ~TEMPORAL_MASK)) {
+	  num++ ;
+	xndx = cf_nint(x[j] - xmin) ;
+	  if (xndx < 0 ) xndx = 0 ;
+          if (xndx > xdim-1) xndx = xdim-1 ;
+        yndx = cf_nint(y[j] - ymin) ;
+    	  if (yndx < 0 ) yndx = 0 ;
+          if (yndx > ydim-1) yndx = ydim-1 ;
+        ndx = xndx + yndx*xdim ;
+	  if (ndx > npts1-1) ndx=npts1-1 ;
+        array1[ndx] += weight[j] ;
+      }
+
+      if (i == 0 ) cf_verbose(3, "%d good seconds out of a total of %d  ",
+		num, numt) ;
+
+      wtot=0. ;
+      for(j=0; j<ydim; j++)
+        for (k=0; k<xdim; k++)  wtot += array1[j*xdim + k] ;
+      cf_verbose(3, "wtot for array 1= %d", cf_nint(wtot)) ;
+
+      /* specify the size of the pothole */
+         rxp = rx[i]  ;
+         rx2 = rxp * rxp ;
+         ryp = ry[i]  ;
+         ry2 = ryp * ryp ;
+	 cf_verbose(3,"pothole size: rx=%d, ry=%d ",cf_nint(rxp),cf_nint(ryp));
+
+      /* set up a target array to contain the image of the full pothole, after
+         reconstruction */
+      xmax1 = xmax + rxp ;
+      xmin1 = xmin - rxp ;
+        xdim1 = (int) (xmax1 - xmin1 + 1.5) ;
+        xndx = (long) x[i] ;
+      ymax1 = ymax + ryp ;
+      ymin1 = ymin - ryp ;
+        cf_verbose(3,"area of the detector covered by pothole :") ;
+	cf_verbose(3, "     xmin=%d, xmax=%d, ymin=%d, ymax=%d ",
+		xmin1,xmax1,ymin1,ymax1) ;
+        cf_verbose(3,"extraction window extends from %d to %d ",ylow[xndx], yhigh[xndx]) ;
+
+	/* Include only pixels that lie within extraction window. */
+	if (ymin1 < ylow[xndx])  ymin1 = ylow[xndx];
+	if (ymax1 > yhigh[xndx]) ymax1 = yhigh[xndx];
+        ydim1 = (int) (ymax1 - ymin1 + 1.5) ;
+
+	/* If no pixels overlap the extraction window, skip to the next one. */
+	if (ydim1 <= 0) {
+	   cf_verbose(3, "This pothole does not overlap the extraction window.  We'll skip it.");
+	   continue;
+	}
+
+      npts2 = xdim1 * ydim1 ;
+      cf_verbose(3, "setting up array2: xdim = %d, ydim = %d, npts2 = %d ", 
+         xdim1, ydim1, npts2) ;
+      array2 = (float *) cf_calloc(npts2, sizeof(float)) ;
+
+      /* fill in array2
+         - scan all of the positions specified in array1  */
+      for (j=0 ; j<ydim ; j++) 
+	for (k=0 ; k<xdim ; k++){
+	  /* specify the properties of the pothole at this location */
+	  xval = k + xmin ;
+          yval = j + ymin ;
+	  ndx = j*xdim + k ;
+	  if (ndx > npts1-1) ndx=npts1-1 ;
+            wval = array1[ndx] ;
+
+	if (wval > 0) {
+	  /* set limits to the region of array2 affected by the pothole */
+	  xminp = (int) (xval - rxp - xmin1 + 0.5)  ;
+          xmaxp = (int) (xval + rxp - xmin1 + 0.5)  ;
+          yminp = (int) (yval - ryp - ymin1 + 0.5) ;
+          ymaxp = (int) (yval + ryp - ymin1 + 0.5)  ;
+	    if (yminp < 0) yminp = 0 ;
+            if (ymaxp > ydim1-1) ymaxp = ydim1-1 ;
+            if (xminp < 0) xminp = 0 ;
+            if (xmaxp > xdim1-1) xmaxp = xdim1-1 ;
+
+	/* fill in the array for this pothole location */
+	  for (l=yminp; l<=ymaxp; l++) 
+            for (m=xminp; m <= xmaxp ; m++) {
+              ndxp = l * xdim1 + m ;
+	         if (ndxp > npts2-1) ndxp = npts2 -1 ;
+	      xv = m + xmin1 - xval ;
+              yv = l + ymin1 - yval ;
+              xv2= xv * xv ;
+              yv2 = yv * yv ;
+              pos = (xv2/rx2) + (yv2/ry2)  ; 
+	      if ( pos <= 1)  array2[ndxp] += wval ; 
+	      nfill++;
+	    }
+	 } 
+      }
+
+	cf_verbose(3,"number of pixels affected by this pothole = %d ",nfill);
+
+      /* determine the maximum weights across the pothole map */
+      wmax=0. ;
+      for(j=0; j<ydim1; j++)
+        for (k=0; k<xdim1; k++) {
+	  ndx = j * xdim1 + k ;
+          if (array2[ndx] > wmax) wmax = array2[ndx] ;
+	}
+      cf_verbose(3, "wmax for array2 = %d ", cf_nint(wmax)) ;
+
+      /* normalize the values of the affected pixels to the maximum and put 
+         their locations into the output array */
+      for(j=0; j<ydim1; j++)
+        for (k=0; k<xdim1; k++) {
+	  ndx = j * xdim1 + k ;
+          if (array2[ndx] > 0) {
+	    if (nout < nmax-1) {
+              nout ++ ;
+	      xpixt[nout] = k + xmin1;
+              ypixt[nout] = j + ymin1;
+              wt_pixt[nout] = array2[ndx]/wmax ;
+              chan_pixt[nout] = channel[i] ;
+            }
+	    else {
+	      cf_if_warning("Array overflow.  Truncating pseudo-photon list.");
+	      break;
+	    }
+          }
+	}
+
+
+      cf_verbose(3, "%d points tabulated after processing pothole %d\n",nout,i);
+
+      free(array1) ;
+      free(array2) ;
+      }
+
+      /* assign output pointers */
+      *xpix = xpixt ;
+      *ypix = ypixt ;
+      *wt_pix = wt_pixt ;
+      *chan_pix = chan_pixt ;
+
+      cf_verbose(3, "Total number of pixels tabulated = %d ", nout) ;
+
+      return nout ;
+}
+
+
+/****************************************************************************/
+
+int
+main(int argc,  char *argv[])
+{
+    unsigned char  *timeflag=NULL, *statflag=NULL, *locflag=NULL;
+    unsigned char *loc_flag=NULL, *channel=NULL ;
+    int  grating_motion=1, mirror_motion=1, fpa_pos=1;
+    int  jitter=1, doppler_motion=1, astig=1, tscreen=1, night_only=FALSE;
+    int  status=0, hdutype, optc;
+    long nevents, nseconds, i, nrows=1, npixels ;
+    long ngood, *good_index, dtime, ntime ;
+    float exptime, *time=NULL, *x=NULL, *y=NULL, *velocity=NULL;
+    float *rx=NULL, *ry=NULL, *xpix, *ypix, *wt_pix ;
+    float *lif_cnt=NULL, *sic_cnt=NULL, *lambda=NULL ;
+    float *timeline=NULL, *weight=NULL;
+    short *tsunrise=NULL, *tsunset=NULL ;
+    fitsfile *header, *bpmfits, *memp;
+    char rootname[FLEN_VALUE]={'\0'}, bpm_file[FLEN_FILENAME]={'\0'};
+    char idf_file[FLEN_FILENAME]={'\0'}, det[FLEN_VALUE]={'\0'}; 
+    char *keywords[] = {"GRAT_COR","FPA__COR","MIRR_COR","ASTG_COR","WAVE_COR"};
+    char keyval[FLEN_VALUE];
+    unsigned char *chan_pix ;
+
+    char extname[]="POTHOLE_DATA", fmt_float[FLEN_VALUE], fmt_byte[FLEN_VALUE] ;
+    char instmode[FLEN_VALUE] ;
+    int tfields=5 ;
+    char *ttype[]={ "X", "Y", "CHANNEL", "WEIGHT", "LAMBDA"} ;
+    char *tform[5] ;  /* we will define the tform once the number of 
+                         array elements is known */
+    char *tunit[]={ "pixels", "pixels",  "unitless", "unitless", "Angstroms"} ;
+    
+    char opts[]  = "hgmfjdasn:v:";
+    char usage[] = 
+	"Usage:\n"
+	"  cf_bad_pixels [-hvgmfjdas] [-n bpm_filename] [-v level] idffile\n";
+    char option[] =
+	"Options:\n"
+	"  -h:  this help message\n"
+        "  -v:  verbosity level (=1; 0 is silent)\n" 
+        "  -g:  no grating motion correction \n"
+        "  -m:  no mirror motion correction \n" 
+        "  -n:  Create BPM file for nighttime fraction of exposure.\n" 
+	"       Argument is the name of the output BPM file.\n"
+        "  -f:  no fpa motion correction \n" 
+        "  -j:  no jitter correction \n" 
+        "  -d:  no doppler correction \n" 
+        "  -a:  no astigmatism correction \n"
+        "  -s:  no screening on time flags (if 0)" ;
+
+    verbose_level = 1;
+
+    while ((optc = getopt(argc, argv, opts)) != -1) {
+	switch(optc) {
+
+	case 'h':
+	    printf("%s\n%s", usage, option);
+	    return 0;
+	case 'v':
+	   verbose_level = atoi(optarg);
+	    break;
+        case 'g':
+	    grating_motion = 0 ;
+            break;
+        case 'm':
+	  mirror_motion = 0 ;
+          break ;
+        case 'n':
+            sprintf(bpm_file,"%s", optarg) ;
+            night_only = TRUE;
+            break;
+        case 'f':
+          fpa_pos = 0 ;
+          break ;
+        case 'j':
+          jitter = 0 ;
+          break ;
+        case 'a':
+          astig = 0 ;
+          break;
+        case 'd':
+          doppler_motion = 0 ;
+          break ;
+        case 's':
+          tscreen = 0 ;
+          break ;
+
+	}
+    }
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    if (argc <= optind) {
+        printf("%s", usage);
+	return -1;
+    }
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    /* Open the input IDF file. */
+    FITS_open_file(&header, argv[optind], READWRITE, &status);
+    FITS_read_key(header, TSTRING, "INSTMODE", instmode, NULL, &status) ;
+
+    /* If EXPTIME < 1, exit without generating a bad-pixel file. */
+    FITS_read_key(header, TFLOAT, "EXPTIME", &exptime, NULL, &status);
+    if (night_only)
+	FITS_read_key(header, TFLOAT, "EXPNIGHT", &exptime, NULL, &status);
+    if (exptime < 1.) {
+        cf_verbose(1, "EXPTIME = %g.  "
+	    "Will not attempt to generate bad-pixel map.", exptime);
+	cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+        return 0;
+    }
+
+    /* Read timeline data from the input file */
+    FITS_movabs_hdu(header, 4, &hdutype, &status);
+    nseconds = cf_read_col(header, TFLOAT, "TIME",         (void **) &timeline);
+    nseconds = cf_read_col(header, TBYTE,  "STATUS_FLAGS", (void **) &statflag);
+    nseconds = cf_read_col(header, TSHORT, "TIME_SUNRISE", (void **) &tsunrise);
+    nseconds = cf_read_col(header, TSHORT, "TIME_SUNSET",  (void **) &tsunset) ;
+    nseconds = cf_read_col(header, TFLOAT, "ORBITAL_VEL",  (void **) &velocity);
+    nseconds = cf_read_col(header, TFLOAT, "LIF_CNT_RATE", (void **) &lif_cnt) ;
+    nseconds = cf_read_col(header, TFLOAT, "SIC_CNT_RATE", (void **) &sic_cnt) ;
+    FITS_movabs_hdu(header, 1, NULL, &status);
+
+   /*  
+    *  If night-only spectrum is requested from the command line, copy 
+    *  IDF header into memory, close the IDF, modify copy, and pass it
+    *  to subsequent routines.
+    */
+    if (night_only) {
+        cf_verbose(3, "Night-only spectrum requested from command line.");
+	FITS_create_file(&memp, "mem://", &status);
+	FITS_copy_hdu(header, memp, 0, &status);
+	if (!strncmp(instmode, "H",1)) {
+	    FITS_movabs_hdu(header, 2, NULL, &status);
+	    FITS_copy_hdu(header, memp, 0, &status);
+	}
+	FITS_close_file(header, &status);
+	header = memp;
+
+	FITS_movabs_hdu(header, 1, NULL, &status);
+        FITS_update_key(header, TFLOAT, "EXPTIME",  &exptime, NULL, &status);
+        FITS_update_key(header, TSTRING, "DAYNIGHT", "NIGHT", NULL, &status);
+    }
+    else { 		/* Generate name of output file */
+	FITS_read_key(header, TSTRING, "ROOTNAME", rootname, NULL, &status) ;
+	FITS_read_key(header, TSTRING, "DETECTOR", det, NULL, &status) ;
+	det[1]=tolower(det[1]) ;
+	if (!strncmp(instmode, "T",1)) 
+	    sprintf(bpm_file,"%11s%2sttagfbpm.fit",rootname,det) ;
+	else
+	    sprintf(bpm_file,"%11s%2shistfbpm.fit",rootname,det) ;
+    }
+
+    /* Write name of BPM file to header of IDF. */
+    cf_verbose(3,"Output bad pixel map to file %s", bpm_file) ;
+    FITS_update_key(header, TSTRING, "BPM_CAL", bpm_file, NULL, &status);
+
+    /* Create the output file and copy header from the input */
+    FITS_create_file(&bpmfits, bpm_file, &status) ;
+    FITS_copy_hdu(header, bpmfits, 0, &status) ;
+
+    FITS_update_key(bpmfits, TSTRING, "FILENAME", bpm_file, 
+		    NULL, &status) ;
+    FITS_update_key(bpmfits, TSTRING, "FILETYPE", "BAD PIXEL MAP", 
+		    NULL, &status) ; 
+
+    FITS_read_key(header, TSTRING, "FILENAME", idf_file, NULL, &status) ;
+    FITS_update_key(bpmfits, TSTRING, "IDF_FILE", idf_file, 
+		    NULL, &status) ;
+     
+    /* Reset analysis keywords in the top level of the output file */
+    FITS_movabs_hdu(bpmfits, 1, &hdutype, &status);
+    for (i = 0; i < 5; i++) {
+        FITS_read_key(bpmfits, TSTRING, keywords[i], keyval, NULL, &status);
+        if (!strncmp(keyval, "COMPLETE", 8))
+            FITS_update_key(bpmfits, TSTRING, keywords[i], "PERFORM", NULL,
+		&status) ;
+        else
+            FITS_update_key(bpmfits, TSTRING, keywords[i], "OMIT", NULL,
+		&status) ;
+    }
+
+    /* Make sure that the count rates are non-zero */
+    for (i=0; i<nseconds; i++) {
+      if (lif_cnt[i] < 0.01) lif_cnt[i] = 0.01 ;
+      if (sic_cnt[i] < 0.01) sic_cnt[i] = 0.01 ;
+    }
+
+    /* generate a null array for locflag */
+    locflag = (unsigned char *) cf_calloc(nseconds, sizeof(unsigned char)) ;
+
+    /* select only the good times */ 
+    FITS_movabs_hdu(header, 1, &hdutype, &status);
+    cf_apply_filters(header, tscreen, nseconds, statflag, locflag, nseconds,
+		     statflag, &dtime, &ntime, &ngood, &good_index) ;
+
+    free(locflag) ;
+
+    cf_verbose(3, "nseconds=%d, dtime=%d, ntime=%d, ngood=%d ",
+	   nseconds, dtime, ntime, ngood) ;
+
+    /* Generate the pseudo photons */
+    cf_generate_pseudo_photons(header, ngood, good_index, timeline, statflag,
+			       lif_cnt, sic_cnt, &nevents, &time, &weight, &x,
+			       &y, &channel, &rx, &ry, &timeflag, &loc_flag) ;
+
+    if (night_only)
+	FITS_delete_file(header, &status);
+    else
+	FITS_close_file(header, &status);
+
+    cf_verbose(3, "number of pseudo photon events = %d ",nevents) ;
+
+    /* Call routines to remove motions */
+    if (grating_motion) {
+      cf_verbose(4,"Correcting for grating motions") ;
+       cf_grating_motion(bpmfits, nevents, time, x, y, channel,  
+			 nseconds, timeline, tsunrise) ; }
+    if (fpa_pos) {
+      cf_verbose(4,"Correcting for fpa motions ") ;
+      cf_fpa_position(bpmfits, nevents, x, channel) ;}
+    if (mirror_motion) {
+      cf_verbose(4,"Correcting for mirror motions") ;
+      cf_mirror_motion(bpmfits, nevents, time, x, y, channel,
+		       nseconds, timeline, tsunset) ; }
+    if (jitter) {
+      cf_verbose(4,"Correcting for satellite jitter ") ;
+      cf_satellite_jitter(bpmfits, nevents, time, x, y, channel, nseconds, 
+	 timeline, statflag) ;
+      }
+
+     /* correct for the Doppler motions */
+     if (doppler_motion)
+        cf_correct_doppler_motions(bpmfits, nevents, time, x, channel, 
+				   nseconds, timeline, velocity) ;
+
+    /* combine the pothole centroid information and generate a pothole map by
+	including the pothole sizes and shapes */
+    npixels = cf_combine_pothole_data(bpmfits, nevents, time, weight,
+	x, rx, y, ry, channel, timeflag, &xpix, &ypix, &chan_pix, &wt_pix) ;
+
+    /* generate a blank wavelength array */
+    lambda = (float *) cf_calloc( npixels, sizeof(float) ) ;
+
+    /* correct for astigmatism and assign wavelengths  */
+    if (astig) cf_astigmatism(bpmfits, npixels, xpix, ypix, chan_pix) ; 
+    cf_dispersion(bpmfits, npixels, xpix, chan_pix, lambda);
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+ 
+    /* create a table and output the results to the file */
+    /* first set tform values */
+    cf_verbose(3, "Writing pseudo-pixel information to output file.");
+    sprintf(fmt_float, "%1ldE", npixels) ;
+    sprintf(fmt_byte, "%1ldB", npixels) ;
+    tform[0]=fmt_float ;
+    tform[1]=fmt_float ;
+    tform[2]=fmt_byte ;
+    tform[3]=fmt_float ;
+    tform[4]=fmt_float ;
+
+    /* put the data into the table */
+    FITS_create_tbl(bpmfits, BINARY_TBL, nrows, tfields, ttype, tform,
+		     tunit, extname, &status) ;
+    cf_verbose(3, "    Photon list created.");
+    FITS_write_col(bpmfits, TFLOAT, 1, 1L, 1L, npixels, xpix, &status) ;
+    cf_verbose(3, "    X array has been written.");
+    FITS_write_col(bpmfits, TFLOAT, 2, 1L, 1L, npixels, ypix, &status) ;
+    cf_verbose(3, "    Y array has been written.");
+    FITS_write_col(bpmfits, TBYTE, 3, 1L, 1L, npixels, chan_pix, &status) ;
+    cf_verbose(3, "    Channel array has been written.");
+    FITS_write_col(bpmfits, TFLOAT, 4, 1L, 1L, npixels, wt_pix, &status) ;
+    cf_verbose(3, "    Weights array has been written.");
+    FITS_write_col(bpmfits, TFLOAT, 5, 1L, 1L, npixels, lambda, &status) ; 
+    cf_verbose(3, "    Lambda array has been written.");
+
+    FITS_close_file(bpmfits, &status);
+
+    free(statflag);
+    free(timeline);
+    free(timeflag);
+    free(rx) ;
+    free(ry) ;
+    free(y);
+    free(x);
+    free(time);
+    free(xpix) ;
+    free(ypix) ;
+    free(chan_pix) ;
+    free(wt_pix) ;
+    free(lambda) ;
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return 0;
+}
diff --git a/src/fuv/cf_convert_to_farf.c b/src/fuv/cf_convert_to_farf.c
new file mode 100644
index 0000000..a50dd2e
--- /dev/null
+++ b/src/fuv/cf_convert_to_farf.c
@@ -0,0 +1,268 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_convert_to_farf options intermediate_file
+ *
+ * Description: Corrects the RAW data for IDS and electronic deadtime
+ *              and for thermal, count rate, geometric, and PHA distortions.
+ *              The resulting data are in the Flight Aligned Reference
+ *              Frame (FARF), the location of an event on an ideal
+ *              detector.  The input file is modified in place.
+ *
+ *              By default all corrections are performed.  Command line
+ *              options allow one or more corrections to be omitted.
+ *
+ * Arguments:   input_file              Intermediate data file
+ *
+ * Calibration files:                   
+ *
+ * Returns:     0 on successful completion
+ *
+ * Calls:       cf_ids_dead_time, cf_electronics_dead_time,
+ *              cf_thermal_distort, cf_count_rate_y_distort,
+ *              cf_geometric_distort, cf_pha_x_distort
+ *
+ * History:     08/08/02   peb    1.1   Begin work
+ *              10/27/02   peb    1.3   Added IDS and electronics dead time
+ *                                      corrections and time-dependent
+ *                                      correction for count_rate_y_distort.
+ *                                      Changed the help option to -h.
+ *                                      Corrected function description.
+ *              11/12/02   peb    1.4   Added argument to cf_thermal_distort,
+ *                                      cf_count_rate_y_distort, and
+ *                                      cf_geometric_distort calls, so
+ *                                      stim-pulse flag can be set.
+ *                                      Added function to flag events in
+ *                                      inactive regions.
+ *		12/09/02   wvd    1.5   Set keyword TOT_DEAD to mean value
+ *					for exposure.
+ *		01/28/03   wvd    1.6   Added cf_check_digitizer
+ *              03/10/03   peb    1.7   Added verbose_level option and unistd.h
+ *                                      so getopt.h will be portable.
+ *              03/10/03   peb    1.8   Changed locflgs to unsigned char *
+ *              03/10/03   peb    1.9   Changed pha to unsigned char *
+ *		06/11/03   wvd    1.10  Pass datatype to cf_read_col and
+ *					cf_write_col.
+ *              06/16/03   rdr    1.11  Correct datatype in reading LOC_FLGS
+ *		08/01/03   wvd    1.12  Add cf_apply_dead_time to properly
+ *					correct both TTAG and HIST data.
+ *		08/04/03   wvd    1.13  Convert count-rate arrays to shorts.
+ *		08/25/03   wvd    1.14  Change coltype from string to int in
+ *					cf_read_col and cf_write_col.
+ *		11/26/03   wvd    1.15  Read aic_rate and fec_rate as floats.
+ *		02/09/04   wvd    1.16  Don't pass aic_rate to
+ *					cf_apply_dead_time().
+ *              02/27/04   rdr    1.17  Added weight to cf_thermal_distortion
+ *              03/02/05   wvd    1.18	Must assign channel numbers and pulse-
+ *					height values to HIST data before walk
+ *					correction.
+ *					Read XFARF and YFARF from XRAW and YRAW.
+ *		05/20/05   wvd    1.19  Clean up i/o.
+ *		11/02/06   wvd    1.20  Add call to cf_time_xy_distort.
+ *              12/29/06   wvd    1.21  Move cf_screen_fifo_overflow from
+ *                                      cf_screen_photons.  Rename it
+ *					cf_fifo_dead_time.  Set all dead-time
+ *					keywords to 1.0 by default.
+ *              02/08/08   wvd    1.22  For HIST data, write modified PHA
+ *					values to the IDF.
+ *
+ ****************************************************************************/
+
+#include <stdlib.h>
+#include <string.h>
+#include <unistd.h>
+#include "calfuse.h"
+
+int
+main(int argc,  char *argv[])
+{
+    char CF_PRGM_ID[] = "cf_convert_to_farf";
+    char CF_VER_NUM[] = "1.22";
+
+    unsigned char *pha=NULL, *locflags=NULL;
+    char instmode[FLEN_VALUE], aperture[FLEN_VALUE];
+    int  check_digitizer=1, ids_deadtime=1, elec_deadtime=1, fifo_deadtime=1;
+    int  thermal_corr=1;
+    int  countrate_corr=1, geometric_corr=1, pha_corr=1, active_flag=1;
+    int  temporal_corr=1, status=0, hdutype, last_call, optc, pad;
+    long i, nevents, nseconds;
+    float *elec_dtc=NULL, *ids_dtc=NULL, unity = 1.0;
+    float *time=NULL, *xfarf=NULL, *yfarf=NULL, *weight=NULL;
+    float *timeline=NULL; 
+    float *aic_rate=NULL, *fec_rate=NULL;
+    fitsfile *header;
+    
+    char opts[]  = "hceiftrsgpav:";
+    char usage[] = 
+	"Usage:\n"
+	"  cf_convert_to_farf [-hceiftrsgpa] [-v level] idf_file\n";
+    char option[] =
+	"Options:\n"
+	"  -h:  this help message\n"
+        "  -v:  verbosity level (default is 1; 0 is silent)\n"
+	"  -c:  no check of digitizer values\n"
+	"  -e:  no electronics deadtime correction\n"
+	"  -i:  no IDS deadtime correction\n"
+	"  -f:  no FIFO deadtime correction\n"
+	"  -t:  no thermal distortion correction\n"
+	"  -r:  no count-rate distortion correction\n"
+	"  -s:  no time-dependent distortion correction\n"
+	"  -g:  no geometric distortion correction\n"
+	"  -p:  no PHA distortion correction\n"
+	"  -a:  do not flag events beyond active region\n";
+
+    verbose_level=1;
+
+    while ((optc = getopt(argc, argv, opts)) != -1) {
+	switch(optc) {
+
+	case 'h':
+	    printf("%s\n%s", usage, option);
+	    return 0;
+	case 'v':
+	    verbose_level = atoi(optarg);
+	    break;
+	case 'c':
+	    check_digitizer = 0;
+	    break;
+	case 'i':
+	    ids_deadtime = 0;
+	    break;
+	case 'e':
+	    elec_deadtime = 0;
+	    break;
+	case 'f':
+	    fifo_deadtime = 0;
+	    break;
+	case 't':
+	    thermal_corr = 0;
+	    break;
+	case 'r':
+	    countrate_corr = 0;
+	    break;
+	case 's':
+	    temporal_corr = 0;
+	    break;
+	case 'g':
+	    geometric_corr = 0;
+	    break;
+	case 'p':
+	    pha_corr = 0;
+	    break;
+	case 'a':
+	    active_flag = 0;
+	    break;
+	}
+    }
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    if (argc <= optind) {
+        printf("%s", usage);
+        cf_if_error("Incorrect number of program arguments");
+    }
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    FITS_open_file(&header, argv[optind], READWRITE, &status);
+
+    /* Read a couple of keywords from the file header. */
+    FITS_read_key(header, TSTRING, "INSTMODE", instmode, NULL, &status);
+    FITS_read_key(header, TSTRING, "APERTURE", aperture, NULL, &status);
+
+    FITS_movabs_hdu(header, 2, &hdutype, &status);
+    nevents = cf_read_col(header, TFLOAT, "TIME",   (void **) &time);
+    nevents = cf_read_col(header, TBYTE,  "PHA",    (void **) &pha);
+    nevents = cf_read_col(header, TFLOAT, "XRAW",   (void **) &xfarf);
+    nevents = cf_read_col(header, TFLOAT, "YRAW",   (void **) &yfarf);
+    nevents = cf_read_col(header, TFLOAT, "WEIGHT", (void **) &weight);
+    nevents = cf_read_col(header, TBYTE,  "LOC_FLGS", (void **) &locflags);
+
+    FITS_movabs_hdu(header, 4, &hdutype, &status);
+    nseconds = cf_read_col(header, TFLOAT, "TIME",  (void **) &timeline);
+    nseconds = cf_read_col(header, TFLOAT, "FEC_CNT_RATE", (void **) &fec_rate);
+    nseconds = cf_read_col(header, TFLOAT, "AIC_CNT_RATE", (void **) &aic_rate);
+    FITS_movabs_hdu(header, 1, &hdutype, &status);
+
+    /* Initialize dead-time correction arrays and header keywords. */
+    FITS_update_key (header, TFLOAT, "DET_DEAD", &unity, NULL, &status);
+    FITS_update_key (header, TFLOAT, "IDS_DEAD", &unity, NULL, &status);
+    FITS_update_key (header, TFLOAT, "TOT_DEAD", &unity, NULL, &status);
+    elec_dtc = (float *) cf_malloc(sizeof(float) * nseconds);
+    ids_dtc  = (float *) cf_malloc(sizeof(float) * nseconds);
+    for (i = 0; i < nseconds; i++) elec_dtc[i] = ids_dtc[i] = 1.0;
+
+    if (check_digitizer)
+	cf_check_digitizer(header);
+
+    if (elec_deadtime)
+	cf_electronics_dead_time(header, nseconds, fec_rate, elec_dtc);
+
+    if (ids_deadtime)
+	cf_ids_dead_time(header, nseconds, aic_rate, ids_dtc);
+
+    if (fifo_deadtime)
+        cf_fifo_dead_time(header, nevents, time,
+                nseconds, timeline, aic_rate, ids_dtc);
+
+    if (ids_deadtime || elec_deadtime || fifo_deadtime)
+	cf_apply_dead_time(header, nevents, time, weight,
+			 nseconds, timeline, ids_dtc, elec_dtc);
+
+    if (thermal_corr)
+	cf_thermal_distort(header, nevents, xfarf, yfarf, weight, locflags);
+
+    if (countrate_corr)
+	cf_count_rate_y_distort(header, nevents, time, yfarf, locflags,
+				nseconds, timeline, fec_rate);
+    if (temporal_corr)
+	cf_time_xy_distort(header, nevents, xfarf, yfarf, locflags);
+
+    if (geometric_corr)
+	cf_geometric_distort(header, nevents, xfarf, yfarf, locflags);
+
+    /* Must assign PHA values to HIST data before applying walk correction. */
+    if (pha_corr && !strncmp(instmode, "HIST", 4)) {
+	unsigned char *channel;
+	channel = cf_calloc(nevents, sizeof(unsigned char));
+	if (!strncmp(aperture, "RFPT", 4)) pad = 10;
+	else pad = 100;
+	cf_identify_channel(header, nevents, xfarf, yfarf, channel, locflags,
+	    pad, last_call=FALSE);
+	cf_modify_hist_pha(header, nevents, pha, channel);
+	free(channel);
+    }
+
+    if (pha_corr)
+	cf_pha_x_distort(header, nevents, pha, xfarf, locflags);
+
+    if (active_flag)
+	cf_active_region(header, nevents, xfarf, yfarf, locflags);
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+    FITS_movabs_hdu(header, 2, &hdutype, &status);
+    if (pha_corr && !strncmp(instmode, "HIST", 4))
+	cf_write_col(header, TBYTE,  "PHA", (void *) pha, nevents);
+    cf_write_col(header, TFLOAT, "WEIGHT", (void *) weight, nevents);
+    cf_write_col(header, TFLOAT, "XFARF",  (void *) xfarf,  nevents);
+    cf_write_col(header, TFLOAT, "YFARF",  (void *) yfarf,  nevents);
+    cf_write_col(header, TBYTE,  "LOC_FLGS", (void *) locflags, nevents);
+
+    FITS_close_file(header, &status);
+
+    free(fec_rate);
+    free(aic_rate);
+    free(timeline);
+    free(locflags);
+    free(weight);
+    free(yfarf);
+    free(xfarf);
+    free(pha);
+    free(time);
+    free(elec_dtc);
+    free(ids_dtc);
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return 0;
+}
diff --git a/src/fuv/cf_countmap.c b/src/fuv/cf_countmap.c
new file mode 100644
index 0000000..2d62b14
--- /dev/null
+++ b/src/fuv/cf_countmap.c
@@ -0,0 +1,541 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_countmap input_files
+ *
+ * Description: Adds the counts from a list of input idf files into
+ *              the count map. The accumulated count map cube is
+ *              determined by reading the COUNT_CAL keyword in the
+ *              input file's header. To prevent multiple copies
+ *              of reprocessed input files from being added to
+ *              the total exposure map, if the input file has been
+ *              previously added, it is skipped over and a message is
+ *              printed out.
+ *
+ * 
+ * Arguments:   input_files     Input initialized ttag FITS file names
+ *
+ * Calibration files required:  None
+ *
+ * Returns:     int  0 = successful completion
+ *
+ * Note:  This routine requires significantly more memory than your
+ *        average routine.  Its design has not been optimized to 
+ *        reduce memory usage.
+ *
+ * History:     03/25/03    1.1  peb  Begin and finish work. Based on
+ *                                    cf_ttag_to_image
+ *              03/31/03    1.2  peb  Removed filtering of photons and fixed
+ *                                    exposure time bug when subtracting data
+ *		06/11/03    1.3  wvd  Pass datatype to cf_read_col
+ *		08/25/03    1.4  wvd  Change coltype from string to int in
+ *					cf_read_col.
+ *		08/25/03    1.5  wvd  Change CHIDCOR1 to CHID_COR
+ *              02/17/04    1.6  bjg  Added scaling option
+ *                                    Routine name changed from 
+ *                                    cf_ttag_countmap to cf_countmap.
+ *              02/26/04    1.7  bjg  Added option to select coordinates
+ *                                    to use: RAW, FARF (default), final
+ *              04/08/04    1.8  bjg  Remove unused function get_xy_columns
+ *              04/27/04    1.9  bjg  Change author name of countfile
+ *              08/25/04    1.10 bjg  Added lower and upper limits option
+ *                                    for PHA. In force mode, issue a warning 
+ *                                    if file already included. 
+ *              03/02/05    1.11 wvd  Don't write AUTHOR keyword to header.
+ *              08/24/07    1.12 bot  Changed nx and ny to long and called
+ *				      as TLONG ; changed binx and biny to int
+ *				      and called as TINT.
+ *
+ ****************************************************************************/
+
+#include <unistd.h>
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>  
+#include "calfuse.h"
+
+#define ROOT_LENGTH 13
+#define MAXCHARS 120
+#define MASTER_CAL_FILE "master_calib_file.dat"
+#define IMAGE_EXT 1
+#define INDEX_EXT 2
+
+static char CF_PRGM_ID[] = "cf_countmap";
+static char CF_VER_NUM[] = "1.12";
+
+
+static int
+new_imagfile(char *newfile, char *detector, float effmjd, int binx, int biny)
+{
+    char  date[FLEN_CARD]={'\0'};
+    char  *ttype[] = {"ROOTNAME", "OBSDATE", "COUNTS", "EXPTIME", "ADDDATE", "SCALE", "PHAMIN", "PHAMAX"};
+    char  *tform[] = {"13A"     , "19A"    , "1J"    , "1E"     , "19A"    , "1E"   , "1I"    , "1I"    };
+    char  *tunit[] = {" "       , " "      , "counts", "seconds", " "      , " "    , " "     , " "     };
+    int   status=0, version=1, tref = 0, tfields = 8;
+    long  axis[2];
+    float exptime=0.;
+    double nevents=0.;
+    fitsfile *imagfits;
+
+    FITS_create_file(&imagfits, newfile, &status);
+    
+    axis[0] = NXMAX/binx;
+    axis[1] = NYMAX/biny;
+    
+    FITS_create_img(imagfits, FLOAT_IMG, 2, axis, &status);
+    FITS_write_key(imagfits, TINT,    "SPECBINX",    &binx,
+		   "Binsize in detector X coordinate", &status);
+    FITS_write_key(imagfits, TINT,    "SPECBINY",    &biny,
+		   "Binsize in detector Y coordinate", &status);
+    FITS_write_key(imagfits, TSTRING, "CALFTYPE", "COUNT",
+		   "Calibration file type", &status);
+    FITS_write_key(imagfits, TINT,    "CALFVERS", &version,
+		   "Calibration file version", &status);
+    FITS_write_key(imagfits, TSTRING, "DETECTOR", detector,
+		   "detector (1A, 1B, 2A, 2B)", &status);
+    FITS_write_key(imagfits, TFLOAT,  "EFFMJD",   &effmjd,
+		   "Date on which file should be applied (MJD)", &status);
+    fits_get_system_time(date, &tref, &status);
+    FITS_write_key(imagfits, TSTRING, "DATE",     date,
+		   "file creation date (YYYY-MM-DDThh:mm:ss UTC)", &status);
+    FITS_write_key(imagfits, TDOUBLE,   "NEVENTS",  &nevents,
+		   "Accumulated events", &status);
+    FITS_write_key(imagfits, TFLOAT,  "EXPTIME",  &exptime,
+		   "Accumulated exposure time", &status);
+
+    FITS_create_tbl(imagfits, BINARY_TBL, 0, tfields, ttype, tform, tunit,
+		    "PROCESSED FILES", &status);
+
+    FITS_close_file(imagfits, &status);
+    return status;
+}
+
+static int
+_check_index(fitsfile *imagfits, char *rootname, float *scale, int *phamin, int *phamax)
+{
+    int   status=0, anynull=0, hdutype;
+    float *scal;
+    int *phami, *phama;
+    long  j, nrows, frow=1, felem=1;
+    char  **filename, strnull[] = "          ";
+
+    FITS_movabs_hdu(imagfits, INDEX_EXT, &hdutype, &status);
+    FITS_read_key(imagfits, TLONG, "NAXIS2", &nrows, NULL, &status);
+
+    filename = (char **) cf_malloc(nrows * sizeof(char *));
+    filename[0] = (char *) cf_malloc(nrows*(ROOT_LENGTH+1)*sizeof(char));
+    scal = (float *) cf_malloc(nrows * sizeof(float));
+    phami = (int *) cf_malloc(nrows * sizeof(int));
+    phama = (int *) cf_malloc(nrows * sizeof(int));
+    for (j=1; j<nrows; j++)
+	filename[j] = filename[j-1]+(ROOT_LENGTH+1);
+
+    FITS_read_col(imagfits, TSTRING, 1, frow, felem, nrows, strnull,
+		  filename, &anynull, &status);
+    FITS_read_col(imagfits, TFLOAT,  6, frow, felem, nrows, strnull,
+		  scal, &anynull, &status);
+    FITS_read_col(imagfits, TINT,  7, frow, felem, nrows, strnull,
+		  phami, &anynull, &status);
+    FITS_read_col(imagfits, TINT,  8, frow, felem, nrows, strnull,
+		  phama, &anynull, &status);
+
+    for (j=0; j<nrows; j++) {
+        if (strncmp(filename[j], rootname, strlen(rootname)) == 0) {
+	    *scale = scal[j];
+	    *phamin = phami[j];
+	    *phamax = phama[j];
+            free(filename[0]);
+            free(filename);
+	    free(scal);
+            return j+1;
+	}
+    }
+    free(filename[0]);
+    free(filename);
+    free(scal);
+    free(phami);
+    free(phama);
+    return 0;
+}
+
+static int
+_update_index(fitsfile *imagfits, char *rootname, char *obsdate,
+	      double nevents, float exptime, float scale, int phamin, int phamax)
+{
+    char  *strptr[1], adddate[FLEN_CARD]={'\0'};
+    int   status=0, hdutype, tref=0;
+    long  nrows;
+
+    FITS_movabs_hdu(imagfits, INDEX_EXT, &hdutype, &status);
+    FITS_read_key(imagfits, TLONG, "NAXIS2", &nrows, NULL, &status);
+
+    strptr[0] = rootname;
+    FITS_write_col(imagfits, TSTRING, 1, nrows+1, 1, 1, strptr, &status);
+    strptr[0] = obsdate;
+    FITS_write_col(imagfits, TSTRING, 2, nrows+1, 1, 1, strptr, &status);
+    FITS_write_col(imagfits, TDOUBLE, 3, nrows+1, 1, 1, &nevents, &status);
+    FITS_write_col(imagfits, TFLOAT,  4, nrows+1, 1, 1, &exptime, &status);
+    fits_get_system_time(adddate, &tref, &status);
+    strptr[0] = adddate;
+    fits_write_col(imagfits, TSTRING, 5, nrows+1, 1, 1, strptr, &status);
+    FITS_write_col(imagfits, TFLOAT,  6, nrows+1, 1, 1, &scale, &status); 
+    FITS_write_col(imagfits, TINT,    7, nrows+1, 1, 1, &phamin,  &status);
+    FITS_write_col(imagfits, TINT,    8, nrows+1, 1, 1, &phamax,  &status);
+    return 0;
+}
+
+
+
+static double
+add_events(fitsfile *infits, char *xcolumn, char *ycolumn, float scale,
+	   int phamin, int phamax, fitsfile *imagfits)
+{
+    int    binx, biny, status=0, hdutype, anynull=0;
+    long   nx, ny, nevents, j;
+    float  *xpos, *ypos, *weight, *image;
+    char   *pha;
+    double ncounts=0.;
+    
+    FITS_movabs_hdu(infits, 2, &hdutype, &status);
+    nevents = cf_read_col(infits, TFLOAT, xcolumn,  (void **) &xpos);
+    nevents = cf_read_col(infits, TFLOAT, ycolumn,  (void **) &ypos);
+    nevents = cf_read_col(infits, TFLOAT, "WEIGHT", (void **) &weight);
+    nevents = cf_read_col(infits, TBYTE, "PHA", (void **) &pha);
+
+    FITS_movabs_hdu(imagfits, IMAGE_EXT, &hdutype, &status);
+    FITS_read_key(imagfits, TLONG, "NAXIS1",   &nx,   NULL, &status);
+    FITS_read_key(imagfits, TLONG, "NAXIS2",   &ny,   NULL, &status);
+    FITS_read_key(imagfits, TINT, "SPECBINX", &binx, NULL, &status);
+    FITS_read_key(imagfits, TINT, "SPECBINY", &biny, NULL, &status);
+    
+    image = (float *) cf_malloc(sizeof(float)*nx*ny);
+    FITS_read_img(imagfits, TFLOAT, 1, nx*ny, NULL, image, &anynull, &status);
+
+    for (j=0; j<nevents; j++) {
+      if ((pha[j]>=phamin) && (pha[j]<=phamax)){
+	int x, y;
+	x = xpos[j];
+	y = ypos[j];
+	if ((x >= 0) && (x < nx*binx)  &&  (y >= 0) && (y < ny*biny)) {
+	  image[(y/biny)*nx + (x/binx)] += weight[j]*scale;
+	  ncounts += weight[j]*scale;
+	}
+      }
+    }
+    FITS_write_img(imagfits, TFLOAT, 1, nx*ny, image, &status);
+
+    free(image);
+    free(weight);
+    free(ypos);
+    free(xpos);
+    return ncounts;
+}
+
+static double
+subtract_events(fitsfile *infits, char *xcolumn, char *ycolumn,
+		float scale, int phamin, int phamax, fitsfile *imagfits)
+{
+    int    binx, biny, status=0, hdutype, anynull=0;
+    long   nx, ny, nevents, j;
+    float  *xpos, *ypos, *weight, *image;
+    double ncounts=0.;
+    char    *pha;
+    
+    FITS_movabs_hdu(infits, 2, &hdutype, &status);
+    nevents = cf_read_col(infits, TFLOAT, xcolumn,  (void **) &xpos);
+    nevents = cf_read_col(infits, TFLOAT, ycolumn,  (void **) &ypos);
+    nevents = cf_read_col(infits, TFLOAT, "WEIGHT", (void **) &weight);
+    nevents = cf_read_col(infits, TBYTE, "PHA",    (void **) &pha);
+
+    FITS_movabs_hdu(imagfits, IMAGE_EXT, &hdutype, &status);
+    FITS_read_key(imagfits, TLONG, "NAXIS1",   &nx,   NULL, &status);
+    FITS_read_key(imagfits, TLONG, "NAXIS2",   &ny,   NULL, &status);
+    FITS_read_key(imagfits, TINT, "SPECBINX", &binx, NULL, &status);
+    FITS_read_key(imagfits, TINT, "SPECBINY", &biny, NULL, &status);
+    
+    image = (float *) cf_malloc(sizeof(float)*nx*ny);
+    FITS_read_img(imagfits, TFLOAT, 1, nx*ny, NULL, image, &anynull, &status);
+
+    for (j=0; j<nevents; j++) {
+      if ((pha[j]>=phamin) && (pha[j]<=phamax)){
+	int x, y;
+	x = xpos[j];
+	y = ypos[j];
+	if ((x >= 0) && (x < nx*binx)  &&  (y >= 0) && (y < ny*biny)) {
+	  image[(y/biny)*nx + (x/binx)] -= weight[j]*scale;
+	  ncounts += weight[j]*scale;
+	}
+      }
+    }
+    FITS_write_img(imagfits, TFLOAT, 1, nx*ny, image, &status);
+
+    free(image);
+    free(weight);
+    free(ypos);
+    free(xpos);
+    return ncounts;
+}
+
+
+int main(int argc, char *argv[])
+{
+    char  *newfile = NULL, *detector = NULL, buffer[FLEN_CARD]={'\0'};
+    int   subtract=0, force=0, newbinx=1, newbiny=1, status=0, optc;
+    float effmjd = 0.,scale=1.,old_scale;
+    int phamin=0, phamax=31;
+    int old_phamin, old_phamax;
+    
+    char   xcolumn[FLEN_CARD]={'\0'}, ycolumn[FLEN_CARD]={'\0'};
+
+    char opts[] = "hv:fsrcn:d:j:w:x:y:l:u:";
+    char usage[] =
+        "Usage:\n"
+	"  cf_countmap [-hfsrc] [-v level] [-n filename] [-d segment]\n"
+        "    [-w scale] [-j effmjd] [-x xbin] [-y ybin] \n"
+        "    [-l phamin] [-u phamax] idffiles\n";
+    char option[] =
+	"Options:\n"
+	"  -h:  this help message\n"
+        "  -v:  verbosity level (=1; 0 is silent)\n"
+	"  -f:  force processing\n"
+	"  -s:  subtract files\n"
+	"  -n:  image map file\n"
+	"  -d:  image map segment (no default for new file)\n"
+	"  -j:  effective MJD (=0.0)\n"
+	"  -w:  weighting factor for image (=1.0)\n"
+	"  -x:  X-bin size (=1)\n"
+	"  -y:  Y-bin size (=1)\n"
+        "  -r:  use raw XY coordinates instead of farf\n"
+        "  -c:  use final XY coordinates instead of farf\n"
+        "  -l:  lower limit for pha (=0) \n"
+        "  -u:  upper limit for pha (=31) \n";
+
+    verbose_level = 1;
+
+    strcpy(xcolumn, "XFARF");
+    strcpy(ycolumn, "YFARF");
+
+    /* Check number of options and arguments */
+    while ((optc = getopt(argc, argv, opts)) != -1) {
+	switch(optc) {
+	    
+	case 'h':
+	    printf("%s\n%s", usage, option);
+	    return 0;
+	case 'v':
+	    verbose_level = atoi(optarg);
+	    break;
+	case 'f':
+	    force = 1;
+	    break;
+	case 's':
+	    subtract = 1;
+	    break;
+	case 'n':
+	    newfile = optarg;
+	    break;
+	case 'd':
+	    detector = optarg;
+	    break;
+	case 'j':
+	    effmjd = atof(optarg);
+	    break;
+	case 'w':
+	    scale = atof(optarg);
+	    break;
+	case 'x':
+	    newbinx = atoi(optarg);
+	    break;
+	case 'y':
+	    newbiny = atoi(optarg);
+	    break;
+	case 'r':
+	    strcpy(xcolumn, "XRAW");
+	    strcpy(ycolumn, "YRAW");
+	    break;
+	case 'c':
+	    strcpy(xcolumn, "X");
+	    strcpy(ycolumn, "Y");
+	    break;
+	case 'l':
+	    phamin = atoi(optarg);
+	    break;
+	case 'u':
+	    phamax = atoi(optarg);
+	    break;
+	}
+    }
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    if (argc <= optind) {
+        cf_if_error("%s\nIncorrect number of program arguments", usage);
+    }
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin processing");
+    
+    while (optind < argc) {
+
+	char   imagfile[FLEN_CARD], rootname[FLEN_CARD]={'\0'};
+	char   segment[FLEN_CARD] = {'\0'};
+	int    hdutype;
+	FILE   *fptr;
+	fitsfile *infits, *imagfits;
+
+	FITS_open_file(&infits, argv[optind], READONLY, &status);
+	FITS_movabs_hdu(infits, 1, &hdutype, &status);
+
+	if (newfile) {
+	    strcpy(imagfile, newfile);
+
+	    if ((fptr = fopen(imagfile, "r")))
+		fclose(fptr);
+	    else {
+		if (!detector)
+		    cf_if_error("No detector segment specified: "
+				"1A, 1B, 2A, 2B");
+		status = new_imagfile(imagfile, detector, effmjd,
+				       newbinx, newbiny);
+	    }
+	    FITS_open_file(&imagfits, imagfile, READWRITE, &status);
+	    FITS_movabs_hdu(imagfits, IMAGE_EXT, &hdutype, &status);
+	    detector = buffer;
+	    FITS_read_key(imagfits, TSTRING, "DETECTOR", detector, NULL,
+			  &status);
+	}
+	else {
+	    FITS_read_key(infits, TSTRING, "TCNT_MAP", imagfile, NULL,
+			  &status);
+	    detector = buffer;
+	    FITS_read_key(infits, TSTRING, "DETECTOR", detector, NULL,
+			  &status);
+
+	    if ((fptr = fopen(cf_hist_file(imagfile), "r"))) {
+		fclose(fptr);
+	    } else {
+		char  keyword[FLEN_CARD]={'\0'}, segment[FLEN_CARD]={'\n'};
+		char  linin[MAXCHARS]={'\0'}, filename[FLEN_CARD]={'\0'};
+		int   interp;
+		float aftermjd;
+		FILE  *master;
+		/*
+		 * Get the effective MJD from the master calibration file
+		 */
+		master = fopen(cf_parm_file(MASTER_CAL_FILE), "r");
+		if (master == NULL)
+		    cf_if_error("Master calibration database file not found");
+		while (fgets(linin, MAXCHARS, master) != NULL) {
+		    /*
+		     * Check for comment lines
+		     */
+		    if ((linin[0] != '#') && (linin[0] != '\n')) {
+			sscanf(linin, "%4c%*2c%2c%*2c%13c%*2c%9f%*2c%1d",
+			       keyword, segment, filename, &aftermjd, &interp);
+			if (strcmp(filename, imagfile) == 0) {
+			    effmjd = aftermjd;
+			    break;
+			}
+		    }
+		}
+		fclose(master);
+
+		status = new_imagfile(cf_hist_file(imagfile), detector,
+				      effmjd, newbinx, newbiny);
+	    }
+	    FITS_open_file(&imagfits, cf_hist_file(imagfile), READWRITE,
+			   &status);
+	}
+
+	strncpy(rootname, argv[optind], ROOT_LENGTH);
+	FITS_read_key(infits, TSTRING,  "DETECTOR", segment, NULL,
+			  &status);
+	if (strcmp(detector, segment) != 0) {
+	    cf_if_warning("%s segment is not the same as %s.",
+			  argv[optind], imagfile);
+	}
+	else if (subtract) {
+	    int  index;
+	    if ((index = _check_index(imagfits, rootname, &scale, &phamin, &phamax))) {
+		
+		int    hdutype;
+		float  exptime=0., acctime=0.;
+		double nevents, accevnt=0.;
+
+		FITS_read_key(infits, TFLOAT,  "EXPTIME", &exptime, NULL,
+			      &status);
+
+		
+		nevents = subtract_events(infits, xcolumn, ycolumn, scale, phamin, phamax, imagfits);
+
+		FITS_movabs_hdu(imagfits, IMAGE_EXT, &hdutype, &status);
+		FITS_read_key(imagfits, TDOUBLE, "NEVENTS",  &accevnt,
+			      NULL, &status);
+		FITS_read_key(imagfits, TFLOAT, "EXPTIME", &acctime,
+			      NULL, &status);
+		accevnt -= nevents;
+		acctime -= exptime;
+		FITS_update_key(imagfits, TDOUBLE,  "NEVENTS", &accevnt,
+				NULL, &status);
+		FITS_update_key(imagfits, TFLOAT, "EXPTIME", &acctime,
+				NULL, &status);
+
+		FITS_movabs_hdu(imagfits, INDEX_EXT, &hdutype, &status);
+		FITS_delete_rows(imagfits, index, 1, &status);
+		cf_verbose(1, "%s is subtracted from %s",
+			   argv[optind], imagfile);
+	    } else {
+	      cf_if_warning("%s is not in %s.", argv[optind], imagfile);
+	    }
+	} else {
+	    if (!force && _check_index(imagfits, rootname, &old_scale, &old_phamin, &old_phamax)) {
+	      cf_if_warning("%s is already in %s with scale = %f, phamin = %d, phamax=%d.",
+			    argv[optind], imagfile, old_scale, old_phamin, old_phamax);
+	    } else {
+		char   obsdate[FLEN_CARD]={'\0'}, dateobs[FLEN_CARD]={'\0'};
+		char   timeobs[FLEN_CARD]={'\0'};
+		
+		float  exptime=0., acctime=0.;
+		double nevents, accevnt=0;
+
+		FITS_movabs_hdu(imagfits, IMAGE_EXT, &hdutype, &status);
+		FITS_read_key(infits, TSTRING, "DATEOBS", dateobs, NULL,
+			      &status);
+		FITS_read_key(infits, TSTRING, "TIMEOBS", timeobs, NULL,
+			      &status);
+		obsdate[0] = '\0';
+		sprintf(obsdate, "%s%s%s", dateobs, "T", timeobs);
+		FITS_read_key(infits, TFLOAT,  "EXPTIME", &exptime, NULL,
+			      &status);
+
+		if ((force) && _check_index(imagfits, rootname, &old_scale, &old_phamin, &old_phamax)) 
+		  cf_if_warning("FORCE MODE - %s is already in %s with scale = %f, phamin = %d, phamax=%d.",
+				argv[optind], imagfile, old_scale, old_phamin, old_phamax);
+
+		nevents = add_events(infits, xcolumn, ycolumn, scale, phamin, phamax, imagfits);
+
+		FITS_movabs_hdu(imagfits, IMAGE_EXT, &hdutype, &status);
+		FITS_read_key(imagfits, TDOUBLE, "NEVENTS",  &accevnt,
+			      NULL, &status);
+		FITS_read_key(imagfits, TFLOAT, "EXPTIME", &acctime,
+			      NULL, &status);
+		accevnt += nevents;
+		acctime += exptime;
+		FITS_update_key(imagfits, TDOUBLE, "NEVENTS", &accevnt,
+				NULL, &status);
+		FITS_update_key(imagfits, TFLOAT, "EXPTIME", &acctime,
+				NULL, &status);
+
+		status = _update_index(imagfits, rootname, obsdate, nevents,
+				       exptime, scale, phamin, phamax);
+		cf_verbose(1, "%s is added to %s", argv[optind], imagfile);
+	    }
+	}
+	FITS_close_file(imagfits, &status);
+	FITS_close_file(infits, &status);
+	optind ++;
+    }
+    
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished processing");
+    return 0;
+}
diff --git a/src/fuv/cf_extract_spectra.c b/src/fuv/cf_extract_spectra.c
new file mode 100644
index 0000000..6e06119
--- /dev/null
+++ b/src/fuv/cf_extract_spectra.c
@@ -0,0 +1,336 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences 
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_extract_spectra options intermediate_file  
+ *
+ * Description: This module computes a background model, reads the various
+ *		calibration files, and performs either a standard or optimal
+ *		extraction for the target spectrum in each of the LiF and
+ *		SiC channels.
+ *
+ *		Note: some of the routines called by this module modify values
+ *		in the IDF file header.  We want those changes to appear in
+ *		the final, extracted spectral files, but not in the archived
+ *		IDF, so we make a copy in memory of the IDF header and pass it
+ *		to the various routines.  We delete it at the end.
+ *
+ * Arguments:   input_file              Intermediate data file
+ *
+ * Calibration files:                   
+ *
+ * Returns:     0 on successful completion
+ *
+ * Calls:       cf_apply_filters, cf_scale_bkgd, cf_make_wave_array,
+ *		cf_rebin_and_flux_calibrate, cf_rebin_probability_array,
+ *              cf_standard_or_optimal_extraction, cf_optimal_extraction
+ *              cf_write_extracted_spectrum
+ *
+ * History:     02/13/03   peb    1.1   Begin work
+ *		03/02/03   wvd    1.3	Add cf_standard_or_optimal_extraction()
+ *              03/10/03   peb    1.4   Added verbose_level, unistd.h for
+ *                                      getopt portability, and remove debug
+ *                                      print statements
+ *		04/08/03   wvd    1.6	Copy header of IDF into memory
+ *					so that subsequent routines can
+ *					modify it without changing IDF.
+ *					Delete this virtual header when done.
+ *					Read arrays from timeline table and
+ *					pass to cf_apply_filters.
+ *              05/06/03   rdr    1.7   Read from column ERGCM2 rather than
+ *                                      ERGCM2S
+ *              05/07/03   wvd    1.8   Change ergcm2 to ergcm2 throughout
+ *              05/28/03   rdr    1.9   Read pothole mask
+ *              06/09/03   rdr    1.10  Incorporate the tscreen flag
+ *		06/11/03   wvd    1.11  Pass datatype to cf_read_col
+ *		08/25/03   wvd    1.12 	Change coltype from string to int in
+ *					cf_read_col.
+ *		09/29/03   wvd    1.13 	Move standard_or_optimal so that it
+ *					runs just once.  Don't check return
+ *					values from subroutines.
+ *		10/08/03   wvd    1.14 	Change counts_out array to type long.
+ *		10/16/03   wvd    1.15 	If EXPTIME = 0, generate a pair of
+ *					null-valued spectra and exit.
+ *		10/31/03   wvd    1.16 	Change channel to unsigned char.
+ *		12/12/03   wvd    1.18 	Clean up i/o.
+ *		03/16/04   wvd    1.19 	Don't pass wave_out to optimal
+ *					extraction subroutine.
+ *					Change pycent from int to float.
+ *		03/24/04   wvd    1.20 	Eliminate got_no_data(); fold into
+ *					main routine.  If either EXPTIME = 0
+ *					or NEVENTS = 0, write null spectrum.
+ *		04/26/04   wvd    1.21 	Replace cf_rebin_and_flux_calibrate
+ *					background with cf_rebin_background.
+ *					cf_optimal_extraction now returns
+ *					flux_out and sigma_out in units of
+ *					counts; must flux-calibrate each.
+ *		06/10/04   wvd    1.22 	Don't pass time array from timeline
+ *					table to cf_apply_filters.
+ *              06/11/04   peb    1.23  Add the -r option to override the
+ *                                      default rootname.
+ *		01/28/05   wvd    1.24	If EXP_STAT < 0, generate a pair of
+ *                                      null-valued spectra and exit.
+ *		03/09/05   wvd    1.25	Change cf_ttag_bkgd to cf_scale_bkgd,
+ *					pass weights array to it.
+ *		04/12/05   wvd    1.27	Add -n flag, which forces extraction
+ *					of night-only spectrum.  Its argument
+ *					is the name of a night-only BPM file.
+ *		06/15/05   wvd    1.28  BUG FIX: program always read the
+ *					point-source probability arrays from
+ *					the WGTS_CAL file.  Now uses value
+ *					of extended to determine which HDU
+ *					to read.
+ *		11/23/05   wvd    1.29  Add flag to disable optimal 
+ *					extraction from the command line.
+ *		01/27/06   wvd    1.30  Add flag to force use of optimal 
+ *					extraction from the command line.
+ *		05/19/06   wvd    1.31	Don't discard spectra with non-zero
+ *					values of EXP_STAT.
+ *		06/12/06   wvd    1.32	Change cf_if_warning to cf_verbose.
+ *
+ ****************************************************************************/
+
+#include <unistd.h>
+#include <stdlib.h>
+#include <string.h>
+#include "calfuse.h"
+
+static char CF_PRGM_ID[] = "cf_extract_spectra";
+static char CF_VER_NUM[] = "1.32";
+
+int
+main(int argc, char *argv[])
+{
+    char  *bpm_file=NULL, *outrootname = NULL;
+    unsigned char *channel=NULL, *timeflags=NULL, *loc_flags=NULL;
+    unsigned char *time_status=NULL;
+    int   extended, status=0, optc, j, tscreen=1;
+    int   binx, biny, bnx[2], bny[2], bymin[2], aper[2];
+    int   night_only=FALSE, optimal=FALSE;
+    int   force_optimal=FALSE, override_optimal=FALSE;
+    long  nevents=0, ntimes=0, ngood=0, dtime=0, ntime=0, *good_index=NULL;
+    float *weight=NULL, *x=NULL, *y=NULL, *lambda=NULL;
+    float exptime, *bpmask=NULL ;
+    float *bimage[2]={NULL, NULL};
+
+    fitsfile *memp, *header;
+    
+    char opts[]  = "hn:ofr:sv:";
+    char usage[] = 
+	"Usage:\n"
+	"  cf_extract_spectra [-hsof] [-n bpm_filename] [-r rootname] [-v level]"
+		" idf_file\n";
+    char option[] =
+	"Options:\n"
+	"  -h:  this help message\n"
+	"  -n:  extract night-only spectrum using given bad-pixel map\n"
+	"  -o:  disable optimal extraction\n"
+	"  -f:  force optimal extraction\n"
+        "  -r:  override the default rootname\n"
+        "  -s:  do not perform screening on time flags\n" 
+        "  -v:  verbosity level (=1; 0 is silent)\n" ;
+
+    verbose_level = 1;
+
+    while ((optc = getopt(argc, argv, opts)) != -1) {
+	switch(optc) {
+
+	case 'h':
+	    printf("%s\n%s", usage, option);
+	    return 0;
+        case 'n':
+            bpm_file = optarg;
+	    night_only = TRUE;
+            break;
+        case 'o':
+	    override_optimal = TRUE;
+            break;
+        case 'f':
+	    force_optimal = TRUE;
+            break;
+        case 'r':
+            outrootname = optarg;
+            break;
+	case 'v':
+	    verbose_level = atoi(optarg);
+	    break;
+        case 's':
+	  tscreen = 0 ;
+          break;
+	}
+    }
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    if (argc <= optind) {
+        printf("%s", usage);
+	return -1;
+    }
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    /* Open input data file. */
+    FITS_open_file(&header, argv[optind], READONLY, &status);
+    FITS_read_key(header, TFLOAT, "EXPTIME", &exptime, NULL, &status);
+
+    FITS_movabs_hdu(header, 2, NULL, &status);
+    nevents = cf_read_col(header, TFLOAT, "WEIGHT",  (void **) &weight);
+    nevents = cf_read_col(header, TFLOAT, "X",       (void **) &x);
+    nevents = cf_read_col(header, TFLOAT, "Y",       (void **) &y);
+    nevents = cf_read_col(header, TBYTE,  "CHANNEL", (void **) &channel);
+    nevents = cf_read_col(header, TBYTE,  "TIMEFLGS", (void **) &timeflags);
+    nevents = cf_read_col(header, TBYTE,  "LOC_FLGS", (void **) &loc_flags);
+    nevents = cf_read_col(header, TFLOAT, "LAMBDA",  (void **) &lambda);
+
+    FITS_movabs_hdu(header, 4, NULL, &status);
+    ntimes = cf_read_col(header, TBYTE, "STATUS_FLAGS", (void **) &time_status);
+
+   /* 
+    *  Copy header of IDF into memory, close IDF,
+    *  and pass copy of header to subsequent routines.
+    */
+    FITS_movabs_hdu(header, 1, NULL, &status);
+    FITS_create_file(&memp, "mem://", &status);
+    FITS_copy_hdu(header, memp, 0, &status);
+    FITS_close_file(header, &status);
+    header = memp;
+
+    /* If night-only spectrum is requested, modify header accordingly. */
+    if (night_only) {
+	cf_verbose(3, "Night-only spectrum requested from command line.");
+	FITS_read_key(header,  TFLOAT, "EXPNIGHT", &exptime, NULL, &status);
+	FITS_update_key(header, TFLOAT, "EXPTIME",  &exptime, NULL, &status);
+	FITS_update_key(header, TSTRING, "DAYNIGHT", "NIGHT", NULL, &status);
+	FITS_update_key(header, TSTRING, "BPM_CAL", bpm_file, NULL, &status);
+    }
+
+    extended = cf_source_aper(header, aper);
+
+    /* Determine whether to attempt optimal extraction. */
+    if (override_optimal) {
+	cf_verbose (1, "User set -o flag.  No optimal extraction.");
+	optimal=FALSE;
+    }
+    else if (force_optimal) {
+	cf_verbose (1, "User set -f flag.  Forcing use of optimal extraction.");
+	optimal=TRUE;
+    }
+    else cf_standard_or_optimal_extraction(header, &optimal);
+
+    /* Make list of all photons that satisfy requested screenings. */
+    cf_apply_filters(header, tscreen, nevents, timeflags, loc_flags,
+	ntimes, time_status, &dtime, &ntime, &ngood, &good_index);
+
+    /* Generate model backgrounds for LiF and SiC channels. */
+    cf_scale_bkgd(header, nevents, x, y, weight, channel, timeflags,
+	loc_flags, ngood, good_index, dtime, ntime, &binx, &biny,
+	&bnx[0], &bny[0], &bymin[0], &bimage[0],
+	&bnx[1], &bny[1], &bymin[1], &bimage[1]);
+
+    /* Run once for each of LiF and SiC target channels. */
+    for (j=0; j<2; j++) {
+	int   pny, valid_spectrum=TRUE;
+	float pycent, wpc;
+        long *counts_out=NULL, i, nout=0, nphotons=0;
+	float *wave_out=NULL, *bkgd_out=NULL, *flux_out=NULL, *sigma_out=NULL;
+	float *weights_out=NULL, *barray=NULL, *parray=NULL;
+        short *bpix_out=NULL;
+	unsigned char *channel_temp=NULL;
+
+	/* Generate output wavelength array. */
+	cf_make_wave_array(header, aper[j], &nout, &wave_out);
+
+	/* If no data, generate null-valued output arrays. */
+	for (i = 0; i < ngood; i++) {
+	    if (channel[good_index[i]] == aper[j]) {
+		nphotons++;
+		break;
+	    }
+	}
+	if (exptime < 1. || nphotons < 1) {
+            bkgd_out = (float *) cf_calloc(nout, sizeof(float));
+            bpix_out = (short *) cf_calloc(nout, sizeof(short));
+            counts_out = (long *) cf_calloc(nout, sizeof(long));
+            flux_out = (float *) cf_calloc(nout, sizeof(float));
+            sigma_out = (float *) cf_calloc(nout, sizeof(float));
+            weights_out = (float *) cf_calloc(nout, sizeof(float));
+	    valid_spectrum=FALSE;	
+	    cf_verbose(1, "No data for aperture %d.  Generating "
+		"null-valued output spectrum.", aper[j]);
+	}
+	else {			/* Extract target spectrum. */
+
+	/* Bin background model to match output wavelength array. */
+	    cf_rebin_background(header, aper[j], nout, wave_out,
+		binx, biny, bnx[j], bny[j], bimage[j], &barray);
+
+	/* Use QUAL_CAL files to create a bad-pixel mask for this exposure. */
+            cf_make_mask(header, aper[j], nout, wave_out, bny[j], bymin[j],
+		&bpmask);
+
+	/* Bin the weights/probability array to match output wave array. */
+	    cf_rebin_probability_array(header, extended, aper[j], nout,
+		wave_out, &pny, &pycent, &parray);
+
+	/* Use optimal extraction if possible, standard extraction otherwise. */
+	    cf_optimal_extraction(header, optimal, aper[j],
+		weight, y, channel, lambda, ngood, good_index,
+		barray, bpmask, pny, pycent, parray, nout, wave_out, &flux_out,
+		&sigma_out, &counts_out, &weights_out, &bkgd_out, &bpix_out);
+
+	/* Optimal-extraction routine returns flux_out and sigma_out in units
+	   of counts.  Must flux-calibrate both arrays. */
+	    channel_temp =
+		(unsigned char *) cf_malloc(sizeof(unsigned char) * nout);
+	    memset (channel_temp, aper[j], sizeof(unsigned char) * nout);
+	    FITS_read_key(header, TFLOAT, "WPC", &wpc, NULL, &status);
+	    FITS_update_key(header, TSTRING, "FLUX_COR", "PERFORM", NULL,
+		&status) ;
+	    cf_convert_to_ergs(header, nout, flux_out, flux_out, channel_temp,
+		wave_out);
+	    FITS_update_key(header, TSTRING, "FLUX_COR", "PERFORM", NULL,
+		&status) ;
+	    cf_convert_to_ergs(header, nout, sigma_out, sigma_out, channel_temp,
+		wave_out);
+	    free(channel_temp);
+
+	/* Divide flux and errors by EXPTIME * WPC to get units of erg/cm2/s/A. */
+	    for (i = 0; i < nout; i++) {
+		flux_out[i]  /= exptime * wpc;
+		sigma_out[i] /= exptime * wpc;
+	    }
+	}
+
+	/* Write extracted spectrum to output file. */
+	cf_write_extracted_spectrum(header, aper[j], valid_spectrum,
+		nout, wave_out, flux_out, sigma_out, counts_out,
+		weights_out, bkgd_out, bpix_out, outrootname);
+
+	free(counts_out);
+	free(bkgd_out);
+	free(weights_out);
+	free(sigma_out);
+	free(flux_out);
+	free(wave_out);
+        free(bpix_out) ;
+	free(parray);
+	free(barray);
+    }
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+    FITS_delete_file(header, &status);
+
+    free(bimage[1]);
+    free(bimage[0]);
+    free(lambda);
+    free(loc_flags);
+    free(timeflags);
+    free(channel);
+    free(y);
+    free(x);
+    free(weight);
+    free(time_status);
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return 0;
+}
diff --git a/src/fuv/cf_flux_calibrate.c b/src/fuv/cf_flux_calibrate.c
new file mode 100644
index 0000000..2ad92e6
--- /dev/null
+++ b/src/fuv/cf_flux_calibrate.c
@@ -0,0 +1,173 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_flux_calibrate options intermediate_file
+ *
+ * Description: Flux calibrate each photon assigned to a channel.
+ *
+ *		** NEXT STEPS COMMENTED OUT FOR NOW **
+ *		For each photon in the target aperture,
+ *		apply astigmatism correction to XFARF array and use the
+ *		resulting coordinate system to apply flat-field and
+ *		worm corrections to photon weights.
+ *
+ *              By default all corrections are performed.  Command line
+ *              options allow one or more corrections to be omitted.
+ *
+ * Arguments:   input_file              Intermediate data file
+ *
+ * Calibration files:                   AEFF_CAL
+ *
+ * Returns:     0 on successful completion
+ *
+ * Calls:       cf_effective_area, cf_astig_farf, cf_flat_field,
+ *		cf_worm_correction
+ *
+ * History:     12/06/02   wvd    1.1   Begin work
+ *		02/12/03   wvd    1.2   Read ERGCM2S from IDF
+ *					Move cf_convert_to_ergs to end of
+ *                                      module
+ *		03/11/03   wvd    1.3   Change channel to type char
+ *		03/12/03   wvd    1.4   If ERGCM2S[i] is undefined,
+ *					set channel[i] = 0
+ *              03/19/03   peb    1.5   Added verbose_level option.
+ *              05/06/03   rdr    1.6   Read from column ERGCM2 rather
+ *                                      than ERGCM2S
+ *              05/07/03   wvd    1.7   Change ergcm2s to ergcm2
+ *		06/11/03   wvd    1.8   Pass datatype to cf_read_col and
+ *					cf_write_col.
+ *					Comment out call to cf_astig_farf().
+ *		08/25/03   wvd    1.9   Change coltype from string to int in
+ *					cf_read_col and cf_write_col.
+ *		09/17/03   wvd    1.10  Add some documentation.
+ *		09/17/03   wvd    1.11  Change channel to unsigned char.
+ *		05/20/05   wvd    1.12  Clean up i/o.
+ *
+ ****************************************************************************/
+
+#include <unistd.h>
+#include <stdlib.h>
+#include "calfuse.h"
+
+static char CF_PRGM_ID[] = "cf_flux_calibrate";
+static char CF_VER_NUM[] = "1.12";
+
+int
+main(int argc,  char *argv[])
+{
+    unsigned char *channel=NULL;
+    int  effective_area=1, astig_farf=1, flat_field=1, worm_correction=1;
+    int  status=0, hdutype, optc;
+    long nevents, nseconds;
+    float *time=NULL, *ttime=NULL, *xfarf=NULL, *yfarf=NULL, *weight=NULL;
+    float *lambda=NULL, *ycentl=NULL, *ycents=NULL, *ergcm2=NULL;
+    fitsfile *header;
+    
+    char opts[]  = "heafwv:";
+    char usage[] = 
+	"Usage:\n"
+	"  cf_flux_calibrate [-heafw] [-v level] idf_file\n";
+    char option[] =
+	"Options:\n"
+	"  -h:  this help message\n"
+	"  -v:  verbosity level (default is 1; 0 is silent)\n"
+	"  -e:  no effective-area calibration\n"
+	"  -a:  no astigmatism correction of XFARF array\n"
+	"  -f:  no flat-field correction\n"
+	"  -w:  no worm correction\n";
+
+    verbose_level = 1;
+ 
+    while ((optc = getopt(argc, argv, opts)) != -1) {
+	switch(optc) {
+
+	case 'h':
+	    printf("%s\n%s", usage, option);
+	    return 0;
+	case 'v':
+	    verbose_level = atoi(optarg);
+	    break;
+	case 'e':
+	    effective_area = 0;
+	    break;
+	case 'a':
+	    astig_farf = 0;
+	    break;
+	case 'f':
+	    flat_field = 0;
+	    break;
+	case 'w':
+	    worm_correction = 0;
+	    break;
+	}
+    }
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    if (argc != optind+1) {
+        printf("%s", usage);
+        cf_if_error("Incorrect number of command-line arguments");
+    }
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    FITS_open_file(&header, argv[optind], READWRITE, &status);
+
+    FITS_movabs_hdu(header, 2, &hdutype, &status);
+    nevents = cf_read_col(header, TFLOAT, "TIME",   (void **) &time);
+    nevents = cf_read_col(header, TFLOAT, "WEIGHT",  (void **) &weight);
+    nevents = cf_read_col(header, TFLOAT, "XFARF",  (void **) &xfarf);
+    nevents = cf_read_col(header, TFLOAT, "YFARF",  (void **) &yfarf);
+    nevents = cf_read_col(header, TBYTE,  "CHANNEL", (void **) &channel);
+    nevents = cf_read_col(header, TFLOAT, "LAMBDA",  (void **) &lambda);
+    nevents = cf_read_col(header, TFLOAT, "ERGCM2",  (void **) &ergcm2);
+
+    FITS_movabs_hdu(header, 4, &hdutype, &status) ;
+    nseconds = cf_read_col(header, TFLOAT, "TIME", (void **) &ttime) ;
+    nseconds = cf_read_col(header, TFLOAT, "YCENT_LIF", (void **) &ycentl) ;
+    nseconds = cf_read_col(header, TFLOAT, "YCENT_SIC", (void **) &ycents) ;
+
+    FITS_movabs_hdu(header, 1, &hdutype, &status);
+
+   /***************************************************************************
+    * Since we currently have no flat-field or worm correction,
+    * these subroutines are commented out.
+    *
+    if (astig_farf)
+	cf_astig_farf(header, nevents, xfarf, yfarf, channel, time,
+		nseconds, ttime, ycentl, ycents);
+    if (flat_field)
+	cf_flat_field(header, nevents, time, weight, xfarf, yfarf, channel,
+		nseconds, ttime, ycentl, ycents);
+
+    if (worm_correction)
+	cf_worm_correction(header, nevents, time, weight, xfarf, yfarf, channel,
+		nseconds, ttime, ycentl, ycents);
+    ***************************************************************************/
+
+    if (effective_area)
+	cf_convert_to_ergs(header, nevents, weight, ergcm2, channel, lambda);
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+    FITS_movabs_hdu(header, 2, &hdutype, &status);
+    cf_write_col(header, TFLOAT, "WEIGHT",  (void *) weight, nevents);
+    cf_write_col(header, TBYTE,  "CHANNEL", (void *) channel, nevents);
+    cf_write_col(header, TFLOAT, "ERGCM2",  (void *) ergcm2, nevents);
+
+    FITS_close_file(header, &status);
+
+    free(time);
+    free(weight);
+    free(xfarf);
+    free(yfarf);
+    free(channel);
+    free(lambda);
+    free(ergcm2);
+    free(ttime);
+    free(ycentl);
+    free(ycents);
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return 0;
+}
diff --git a/src/fuv/cf_gainmap.c b/src/fuv/cf_gainmap.c
new file mode 100644
index 0000000..63ed3f7
--- /dev/null
+++ b/src/fuv/cf_gainmap.c
@@ -0,0 +1,610 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_gainmap input_files
+ *
+ * Description: Adds the counts from a list of input ttag idf files into
+ *              the gain map.  The accumulated gain map cube is
+ *              determined by reading the GAIN_CAL keyword in the
+ *              input file's header.  To prevent multiple copies
+ *              of reprocessed input files from being added to
+ *              the total exposure map, the gain map contains an
+ *              index list of the files which have been added.
+ *              The new file is skipped if it is in the list.
+ * 
+ * 
+ * Arguments:   input_files     Input ttag IDF FITS file name
+ *
+ * Calibration files required:  None
+ *
+ * Returns:     int  0 = successful completion
+ *
+ * Note:  This routine requires significantly more memory than your
+ *        average routine.  Its design has not been optimized to 
+ *        reduce memory usage.
+ *
+ * History:     03/31/03    1.1  peb  Finished work.
+ *                                    Based on cf_ttag_countmap.
+ *		06/11/03    1.2  wvd  Pass datatype to cf_read_col
+ *		08/25/03    1.3  wvd  Change coltype from string to int in
+ *					cf_read_col.
+ *              01/09/04    1.4  bjg  Change CHIDCOR1 to CHID_COR
+ *              02/17/04    1.5  bjg  Added scaling option 
+ *                                    histogram files given in the argument 
+ *                                    list are ignored
+ *              02/26/04    1.6  bjg  Bug Fix. Routine name changed from 
+ *                                    cf_ttag_gainmap to cf_gainmap.
+ *                                    Added option to select coordinates
+ *                                    to use: RAW, FARF (default), final
+ *                                    Print ignored HIST files
+ *              04/08/04    1.7  bjg  Remove unused function get_xy_columns
+ *                                    Use cf_verbose instead of printf
+ *              04/27/04    1.8  bjg  Added lower and upper limits option
+ *                                    for PHA 
+ *                                    Change author name of gainfile
+ *              08/26/04    1.9  bjg  In force mode, issue a warning 
+ *                                    if file already included. 
+ *              03/02/05    1.10 wvd  Use FLOAT_IMG to insure that output
+ *					images are written as floats.
+ *              03/02/05    1.11 wvd  Don't write AUTHOR keyword to header.
+ *              04/11/05    1.12 wvd  Force detector string to be upper case.
+ *					Add -t option, which prevents creation
+ *					of detector image for PHA=31.  It's
+ *					required if you don't bin the data.
+ *              06/03/05    1.13 wvd  Include ctype.h
+ *              09/09/05    1.14 wvd  Update list of allowed options.
+ *              08/24/07    1.15 bot  Changed nx and ny to long and called
+ *				      as TLONG ; changed binx and biny to int
+ *				      and called as TINT.
+ *
+ ****************************************************************************/
+
+#include <ctype.h>
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include <unistd.h>
+#include "calfuse.h"
+
+#define ROOT_LENGTH 13
+#define MAXCHARS 120
+#define MASTER_CAL_FILE "master_calib_file.dat"
+#define IMAGE_EXT 1
+#define INDEX_EXT 34
+
+static char CF_PRGM_ID[] = "cf_gainmap";
+static char CF_VER_NUM[] = "1.15";
+
+
+static int
+new_gainfile(char *newfile, char *detector, float effmjd, int binx, int biny, int truncate)
+{
+    char  date[FLEN_CARD]={'\0'};
+    char  *ttype[] = {"ROOTNAME", "OBSDATE", "COUNTS", "EXPTIME", "ADDDATE", "SCALE", "PHAMIN", "PHAMAX"};
+    char  *tform[] = {"13A",      "19A",     "1D",     "1E",      "19A",     "1E",     "1I",    "1I"};
+    char  *tunit[] = {" ",        " ",       "counts", "seconds", " ",       " ",      " ",     " "};
+    int   naxis=2, status=0, version=1, tref=0, tfields=8, phaext;
+    long  axis[2], naxis2=0;
+    float exptime=0.;
+    double ncounts=0.;
+    fitsfile *gainfits;
+
+    cf_verbose(3, "Entering subroutine new_gainfile");
+    cf_verbose(3, "Creating file %s", newfile);
+
+    FITS_create_file(&gainfits, newfile, &status);
+
+    FITS_create_img(gainfits, 8, 0, NULL, &status);
+    FITS_write_key(gainfits, TSTRING, "CALFTYPE", "GAIN",
+		   "Calibration file type", &status);
+    FITS_write_key(gainfits, TINT,    "CALFVERS", &version,
+		   "Calibration file version", &status);
+    FITS_write_key(gainfits, TSTRING, "DETECTOR", detector,
+		   "detector (1A, 1B, 2A, 2B)", &status);
+    FITS_write_key(gainfits, TFLOAT,  "EFFMJD",   &effmjd,
+		   "Date on which file should be applied (MJD)", &status);
+    fits_get_system_time(date, &tref, &status);
+    FITS_write_key(gainfits, TSTRING, "DATE",     date,
+		   "file creation date (YYYY-MM-DDThh:mm:ss UTC)", &status);
+    FITS_write_key(gainfits, TDOUBLE, "NEVENTS",  &ncounts,
+		   "Accumulated weighted events", &status);
+    FITS_write_key(gainfits, TFLOAT,  "EXPTIME",  &exptime,
+		   "Accumulated exposure time", &status);
+
+    axis[0] = NXMAX/binx;
+    axis[1] = NYMAX/biny;
+    for (phaext=0; phaext<32-truncate; phaext++) {
+	
+	cf_verbose(3, "Creating extension %d", phaext);
+	FITS_create_img(gainfits, FLOAT_IMG, naxis, axis, &status);
+	FITS_write_key(gainfits, TINT,    "PHA",         &phaext,
+		       "PHA value of image", &status);
+	FITS_write_key(gainfits, TINT,    "SPECBINX",    &binx,
+		       "Binsize in detector X coordinate", &status);
+	FITS_write_key(gainfits, TINT,    "SPECBINY",    &biny,
+		       "Binsize in detector Y coordinate", &status);
+
+    }
+
+    cf_verbose(3, "Creating binary table extension");
+    FITS_create_tbl(gainfits, BINARY_TBL, naxis2, tfields, ttype, tform, tunit,
+		    "PROCESSED FILES", &status);
+
+    cf_verbose(3, "Closing file %s", newfile);
+    FITS_close_file(gainfits, &status);
+    cf_verbose(3, "Exiting new_gainfile");
+    return status;
+}
+
+static int
+_check_index(fitsfile *gainfits, char *rootname, float *scale, int *phamin,
+	int *phamax, int truncate)
+{
+    int   status=0, anynull=0, hdutype;
+    float *scal; 
+    int *phami, *phama;
+    long  j, nrows, frow=1, felem=1;
+    char  **filename, strnull[] = "          ";
+
+    FITS_movabs_hdu(gainfits, INDEX_EXT-truncate, &hdutype, &status);
+    FITS_read_key(gainfits, TLONG, "NAXIS2", &nrows, NULL, &status);
+
+    filename = (char **) cf_malloc(nrows * sizeof(char *));
+    filename[0] = (char *) cf_malloc(nrows*(ROOT_LENGTH+1)*sizeof(char));
+    scal = (float *) cf_malloc(nrows * sizeof(float));
+    phami = (int *) cf_malloc(nrows * sizeof(int));
+    phama = (int *) cf_malloc(nrows * sizeof(int));
+    for (j=1; j<nrows; j++)
+	filename[j] = filename[j-1]+(ROOT_LENGTH+1);
+
+    FITS_read_col(gainfits, TSTRING, 1, frow, felem, nrows, strnull,
+		  filename, &anynull, &status);
+    FITS_read_col(gainfits, TFLOAT,  6, frow, felem, nrows, strnull,
+		  scal, &anynull, &status);
+    FITS_read_col(gainfits, TINT,  7, frow, felem, nrows, strnull,
+		  phami, &anynull, &status);
+    FITS_read_col(gainfits, TINT,  8, frow, felem, nrows, strnull,
+		  phama, &anynull, &status);
+
+    for (j=0; j<nrows; j++) {
+	if (strncmp(filename[j], rootname, strlen(rootname)) == 0) {
+	    *scale = scal[j];
+	    *phamin = phami[j];
+	    *phamax = phama[j];
+	    free(filename[0]);
+	    free(filename);
+	    free(scal);
+	    free(phami);
+	    free(phama);
+            return j+1;
+	}
+    }
+    free(filename[0]);
+    free(filename);
+    free(scal);
+    free(phami);
+    free(phama);
+    return 0;
+}
+
+static int
+_update_index(fitsfile *gainfits, char *rootname, char *obsdate,
+     double ncounts, float exptime, float scale, int phamin, int phamax,
+     int truncate)
+{
+    char  *strptr[1], adddate[FLEN_CARD]={'\0'};
+    int   status=0, hdutype, tref=0;
+    long  nrows;
+
+    FITS_movabs_hdu(gainfits, INDEX_EXT-truncate, &hdutype, &status);
+    FITS_read_key(gainfits, TLONG, "NAXIS2", &nrows, NULL, &status);
+
+    strptr[0] = rootname;
+    FITS_write_col(gainfits, TSTRING, 1, nrows+1, 1, 1, strptr,   &status);
+    strptr[0] = obsdate;
+    FITS_write_col(gainfits, TSTRING, 2, nrows+1, 1, 1, strptr,   &status);
+    FITS_write_col(gainfits, TDOUBLE, 3, nrows+1, 1, 1, &ncounts, &status);
+    FITS_write_col(gainfits, TFLOAT,  4, nrows+1, 1, 1, &exptime, &status);
+    fits_get_system_time(adddate, &tref, &status);
+    strptr[0] = adddate;
+    fits_write_col(gainfits, TSTRING, 5, nrows+1, 1, 1, strptr,   &status);
+    FITS_write_col(gainfits, TFLOAT,  6, nrows+1, 1, 1, &scale,   &status);
+    fits_write_col(gainfits, TINT,    7, nrows+1, 1, 1, &phamin,  &status);
+    FITS_write_col(gainfits, TINT,    8, nrows+1, 1, 1, &phamax,  &status);
+    return 0;
+}
+
+
+static double
+add_events(fitsfile *infits, char *xcolumn, char *ycolumn, float scale,
+	   int phamin, int phamax, fitsfile *gainfits)
+{
+    char   *pha;
+    int    binx, biny, phaext, status=0, hdutype, anynull=0;
+    long   nevents, j;
+    long   nx, ny;
+    float  *xpos, *ypos, *weight, *image;
+    double ncounts=0.;
+
+    cf_verbose(3,"Entering add_events");
+
+    FITS_movabs_hdu(infits, 2, &hdutype, &status);
+    nevents = cf_read_col(infits, TFLOAT, xcolumn,  (void **) &xpos);
+    nevents = cf_read_col(infits, TFLOAT, ycolumn,  (void **) &ypos);
+    nevents = cf_read_col(infits, TBYTE,  "PHA",    (void **) &pha);
+    nevents = cf_read_col(infits, TFLOAT, "WEIGHT", (void **) &weight);
+
+    for (phaext=phamin; phaext<=phamax; phaext++) {
+	FITS_movabs_hdu(gainfits, phaext+2, &hdutype, &status);
+	if (hdutype == BINARY_TBL) {
+	    cf_if_warning("Can't find image extension for PHA = %d", phaext);
+	    break;
+	}
+	FITS_read_key(gainfits, TLONG, "NAXIS1",   &nx,   NULL, &status);
+	FITS_read_key(gainfits, TLONG, "NAXIS2",   &ny,   NULL, &status);
+	FITS_read_key(gainfits, TINT, "SPECBINX", &binx, NULL, &status);
+	FITS_read_key(gainfits, TINT, "SPECBINY", &biny, NULL, &status);
+    
+	image = (float *) cf_malloc(sizeof(float)*nx*ny);
+	FITS_read_img(gainfits, TFLOAT, 1, nx*ny, NULL, image,
+		      &anynull, &status);
+
+	for (j=0; j<nevents; j++) {
+	    if (pha[j] == phaext) {
+		int x, y;
+		x = xpos[j];
+		y = ypos[j];
+		if ((x >= 0) && (x < nx*binx) && (y >= 0) && (y < ny*biny)) {
+		    image[(y/biny)*nx + (x/binx)] += weight[j]*scale;
+		    ncounts += weight[j]*scale;
+		}
+	    }
+	}
+	FITS_write_img(gainfits, TFLOAT, 1, nx*ny, image, &status);
+	free(image);
+    }
+
+    free(weight);
+    free(pha);
+    free(ypos);
+    free(xpos);
+    return ncounts;
+}
+
+static double
+subtract_events(fitsfile *infits, char *xcolumn, char *ycolumn, 
+		float scale, int phamin, int phamax, fitsfile *gainfits)
+{
+    char   *pha;
+    long   nx, ny;
+    int    phaext, status=0, hdutype, anynull=0, binx, biny;
+    long   nevents, j;
+    float  *xpos, *ypos, *weight, *image;
+    double ncounts=0.;
+
+    FITS_movabs_hdu(infits, 2, &hdutype, &status);
+    nevents = cf_read_col(infits, TFLOAT, xcolumn,  (void **) &xpos);
+    nevents = cf_read_col(infits, TFLOAT, ycolumn,  (void **) &ypos);
+    nevents = cf_read_col(infits, TBYTE, "PHA",    (void **) &pha);
+    nevents = cf_read_col(infits, TFLOAT, "WEIGHT", (void **) &weight);
+
+    for (phaext=phamin; phaext<=phamax; phaext++) {
+	FITS_movabs_hdu(gainfits, phaext+2, &hdutype, &status);
+	FITS_read_key(gainfits, TLONG, "NAXIS1", &nx, NULL, &status);
+	FITS_read_key(gainfits, TLONG, "NAXIS2", &ny, NULL, &status);
+	FITS_read_key(gainfits, TINT, "SPECBINX", &binx, NULL, &status);
+	FITS_read_key(gainfits, TINT, "SPECBINY", &biny, NULL, &status);
+
+	image = (float *) cf_malloc(sizeof(float) * nx*ny);
+	FITS_read_img(gainfits, TFLOAT, 1, nx*ny, NULL, image,
+		      &anynull, &status);
+
+	for (j=0; j<nevents; j++) {
+	    if (pha[j] == phaext) {
+		int x, y;
+		x = xpos[j];
+		y = ypos[j];
+		if ((x >=0) && (x < nx*binx) && (y >= 0) && (y < ny*biny)) {
+		    image[(y/biny)*nx + (x/binx)] -= weight[j]*scale;
+		    ncounts += weight[j]*scale;
+		}
+	    }
+	}
+	FITS_write_img(gainfits, TFLOAT, 1, nx*ny, image, &status);
+	free(image);
+    }
+
+    free(weight);
+    free(pha);
+    free(ypos);
+    free(xpos);
+    return ncounts;
+}
+
+
+int main(int argc, char *argv[])
+{
+    char  *newfile = NULL, *detector = NULL, buffer[FLEN_CARD]={'\0'}, instmode[FLEN_CARD]={'\0'};
+    int   subtract=0, force=0, newbinx=8, newbiny=4, status=0, optc;
+    int   truncate=0;
+    float effmjd = 0.,scale=1., old_scale;
+    int phamin=0, phamax=31; 
+    int old_phamin, old_phamax;
+
+    char   xcolumn[FLEN_CARD]={'\0'}, ycolumn[FLEN_CARD]={'\0'};
+
+    char opts[] = "hv:fsrtcn:d:j:w:x:y:l:u:";
+    char usage[] = 
+	"Usage:\n"
+	"  cf_gainmap [-hfsrtc] [-v level] [-n filename] [-d segment]\n"
+	"    [-w scale] [-j effmjd] [-x xbin] [-y ybin] \n"
+        "    [-l phamin] [-u phamax] idffiles\n";
+    char option[] =
+	"Options:\n"
+	"  -h:  this help message\n"
+        "  -v:  verbosity level (=1; 0 is silent)\n"
+	"  -f:  force the files\n"
+	"  -s:  subtract files\n"
+	"  -n:  gain map file\n"
+	"  -d:  gain map segment (no default for new file)\n"
+        "  -j:  effective MJD (=0.0)\n"
+        "  -w:  weighting factor for image (=1.0)\n"
+	"  -x:  X-bin size (=8)\n"
+	"  -y:  Y-bin size (=4)\n"
+        "  -r:  use raw XY coordinates instead of farf\n"
+        "  -t:  truncate map at PHA = 30\n"
+        "  -c:  use final XY coordinates instead of farf\n"
+        "  -l:  lower limit for pha (=0) \n"
+        "  -u:  upper limit for pha (=31) \n";
+
+    verbose_level = 1;
+
+    strcpy(xcolumn, "XFARF");
+    strcpy(ycolumn, "YFARF");
+
+   
+
+    /* Check number of options and arguments */
+    while ((optc = getopt(argc, argv, opts)) != -1) {
+	switch(optc) {
+	    
+	case 'h':
+	    printf("%s\n%s", usage, option);
+	    return 0;
+	case 'v':
+	    verbose_level = atoi(optarg);
+	    break;
+	case 'f':
+	    force = 1;
+	    break;
+	case 's':
+	    subtract = 1;
+	    break;
+	case 'n':
+	    newfile = optarg;
+	    break;
+	case 'd':
+	    detector = optarg;
+	    break;
+	case 'j':
+	    effmjd = atof(optarg);
+	    break;
+	case 'w':
+	    scale = atof(optarg);
+	    break;
+	case 'x':
+	    newbinx = atoi(optarg);
+	    break;
+	case 'y':
+	    newbiny = atoi(optarg);
+	    break;
+	case 'r':
+	    strcpy(xcolumn, "XRAW");
+	    strcpy(ycolumn, "YRAW");
+	    break;
+	case 't':
+	    truncate = 1;
+	    break;
+	case 'c':
+	    strcpy(xcolumn, "X");
+	    strcpy(ycolumn, "Y");
+	    break;
+	case 'l':
+	    phamin = atoi(optarg);
+	    break;
+	case 'u':
+	    phamax = atoi(optarg);
+	    break;
+	}
+    }
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    if (argc <= optind)
+        cf_if_error("%s\nIncorrect number of program arguments", usage);
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin processing");
+    
+    while (optind < argc) {
+
+	char   gainfile[FLEN_CARD], rootname[FLEN_CARD]={'\0'};
+	char   segment[FLEN_CARD] = {'\0'};
+	int    hdutype;
+	FILE   *fptr;
+	fitsfile *infits, *gainfits;
+
+	FITS_open_file(&infits, argv[optind], READONLY, &status);
+	FITS_movabs_hdu(infits, 1, &hdutype, &status);
+
+	FITS_read_key(infits, TSTRING, "INSTMODE", instmode, NULL,
+			  &status);
+
+	if (strncmp(instmode,"TTAG",4)){
+	  FITS_close_file(infits, &status);
+	  cf_verbose(1,"Skipped HIST file: %s\n",argv[optind]);
+	  optind ++;
+	  continue;
+	}
+
+	if (newfile) {
+	    cf_verbose(3, "newfile is TRUE");
+	    strcpy(gainfile, newfile);
+
+	    if ((fptr = fopen(gainfile, "r")))
+		fclose(fptr);
+	    else {
+		if (!detector)
+		    cf_if_error("No detector segment specified: "
+				"1A, 1B, 2A, 2B");
+		detector[1] = toupper(detector[1]);
+		status = new_gainfile(gainfile, detector, effmjd,
+				      newbinx, newbiny, truncate);
+	    }
+	    FITS_open_file(&gainfits, gainfile, READWRITE, &status);
+	    FITS_movabs_hdu(gainfits, 1, &hdutype, &status);
+	    detector = buffer;
+	    FITS_read_key(gainfits, TSTRING, "DETECTOR", detector, NULL,
+			  &status);
+	} else {
+	    cf_verbose(3, "newfile is FALSE");
+	    FITS_read_key(infits, TSTRING, "GAIN_MAP", gainfile, NULL,
+			  &status);
+	    detector = buffer;
+	    FITS_read_key(infits, TSTRING, "DETECTOR", detector, NULL,
+			  &status);
+
+	    if ((fptr = fopen(cf_hist_file(gainfile), "r"))) {
+		fclose(fptr);
+	    } else {
+		char  keyword[FLEN_CARD]={'\0'}, segment[FLEN_CARD]={'\n'};
+		char  linin[MAXCHARS]={'\0'}, filename[FLEN_CARD]={'\0'};
+		int   interp;
+		float aftermjd;
+		FILE  *master;
+		/*
+		 * Get the effective MJD from the master calibration file
+		 */
+		master = fopen(cf_parm_file(MASTER_CAL_FILE), "r");
+		if (master == NULL)
+		    cf_if_error("Master calibration database file not found");
+		while (fgets(linin, MAXCHARS, master) != NULL) {
+		    /*
+		     * Check for comment lines
+		     */
+		    if ((linin[0] != '#') && (linin[0] != '\n')) {
+			sscanf(linin, "%4c%*2c%2c%*2c%13c%*2c%9f%*2c%1d",
+			       keyword, segment, filename, &aftermjd, &interp);
+			if (strcmp(filename, gainfile) == 0) {
+			    effmjd = aftermjd;
+			    break;
+			}
+		    }
+		}
+		fclose(master);
+
+		status = new_gainfile(cf_hist_file(gainfile), detector,
+				      effmjd, newbinx, newbiny, truncate);
+	    }
+	    FITS_open_file(&gainfits, cf_hist_file(gainfile), READWRITE,
+			   &status);
+	}
+
+	strncpy(rootname, argv[optind], ROOT_LENGTH);
+	FITS_read_key(infits, TSTRING,  "DETECTOR", segment, NULL, &status);
+	if (strcmp(detector, segment) != 0) {
+	    cf_if_warning("%s segment is not the same as %s",
+			  argv[optind], gainfile);
+	}
+	else if (subtract) {
+	    int  index;
+	    if ((index = _check_index(gainfits, rootname, &scale, &phamin,
+		&phamax, truncate))) {
+		
+		int    hdutype;
+		float  exptime=0., acctime=0.;
+		double ncounts=0, accevnt=0;
+
+		FITS_read_key(infits, TFLOAT,  "EXPTIME", &exptime, NULL,
+			      &status);
+
+		
+		ncounts = subtract_events(infits, xcolumn, ycolumn, scale, phamin,
+			phamax-truncate, gainfits);
+
+		FITS_movabs_hdu(gainfits, IMAGE_EXT, &hdutype, &status);
+		FITS_read_key(gainfits, TDOUBLE, "NEVENTS",  &accevnt,
+			      NULL, &status);
+		FITS_read_key(gainfits, TFLOAT, "EXPTIME", &acctime,
+			      NULL, &status);
+		accevnt -= ncounts;
+		acctime -= exptime;
+		FITS_update_key(gainfits, TDOUBLE,  "NEVENTS", &accevnt,
+				NULL, &status);
+		FITS_update_key(gainfits, TFLOAT, "EXPTIME", &acctime,
+				NULL, &status);
+
+		FITS_movabs_hdu(gainfits, INDEX_EXT-truncate, &hdutype, &status);
+		FITS_delete_rows(gainfits, index, 1, &status);
+		cf_verbose(1, "%s is subtracted from %s",
+			   argv[optind], gainfile);
+	    } else {
+		cf_if_warning("%s is not in %s.", argv[optind], gainfile);
+	    }
+	} else {
+	    cf_verbose(3, "Adding new data file.");
+	    if (!force && _check_index(gainfits, rootname, &old_scale, 
+		&old_phamin, &old_phamax, truncate)) {
+		cf_if_warning("%s is already in %s with scale = %f, "
+		"phamin = %d, phamax=%d.",
+		argv[optind], gainfile, old_scale, old_phamin, old_phamax);
+	    } else {
+		char   obsdate[FLEN_CARD]={'\0'}, dateobs[FLEN_CARD]={'\0'};
+		char   timeobs[FLEN_CARD]={'\0'};
+		
+		float  exptime=0., acctime=0.;
+		double ncounts=0, accevnt=0;
+
+		FITS_read_key(infits, TSTRING, "DATEOBS", dateobs, NULL,
+			      &status);
+		FITS_read_key(infits, TSTRING, "TIMEOBS", timeobs, NULL,
+			      &status);
+		obsdate[0] = '\0';
+		sprintf(obsdate, "%s%s%s", dateobs, "T", timeobs);
+		FITS_read_key(infits, TFLOAT,  "EXPTIME", &exptime, NULL,
+			      &status);
+
+		if ((force) && _check_index(gainfits, rootname, &old_scale,
+		   &old_phamin, &old_phamax, truncate)) 
+		   cf_if_warning("FORCE MODE - %s is already in %s with scale = %f, "
+			"phamin = %d, phamax=%d.",
+			argv[optind], gainfile, old_scale, old_phamin, old_phamax);
+		
+		ncounts = add_events(infits, xcolumn, ycolumn, scale, phamin,
+			phamax-truncate, gainfits);
+
+		FITS_movabs_hdu(gainfits, IMAGE_EXT, &hdutype, &status);
+		FITS_read_key(gainfits, TDOUBLE, "NEVENTS",  &accevnt,
+			      NULL, &status);
+		FITS_read_key(gainfits, TFLOAT, "EXPTIME", &acctime,
+			      NULL, &status);
+		accevnt += ncounts;
+		acctime += exptime;
+		FITS_update_key(gainfits, TDOUBLE,  "NEVENTS", &accevnt,
+				NULL, &status);
+		FITS_update_key(gainfits, TFLOAT, "EXPTIME", &acctime,
+				NULL, &status);
+
+		status = _update_index(gainfits, rootname, obsdate, ncounts,
+				       exptime, scale, phamin, phamax, truncate);
+		cf_verbose(1, "%s is added to %s", argv[optind], gainfile);
+	    }
+	}
+	FITS_close_file(gainfits, &status);
+	FITS_close_file(infits, &status);
+	optind ++;
+    }
+    
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished processing");
+    return 0;
+}
diff --git a/src/fuv/cf_hist_init.c b/src/fuv/cf_hist_init.c
new file mode 100644
index 0000000..5829707
--- /dev/null
+++ b/src/fuv/cf_hist_init.c
@@ -0,0 +1,653 @@
+/*****************************************************************************
+ *	        Johns Hopkins University
+ *	        Center For Astrophysical Sciences 
+ *	        FUSE
+ *****************************************************************************
+ *
+ * Synopsis:	cf_hist_init input_file output_file 
+ *
+ * Description: Reads a raw hist file and generates a list of the pixels
+ *              that contain counts. This list has the same format 
+ *              as a TTAG list, so analysis can be carried out using
+ *		many of the modules in the TTAG pipeline.
+ *
+ *              The output file will have the same format as a TTAG 
+ *              file, with the following definitions:
+ *
+ *              TIME            FLOAT   all equal to the midpoint of the exp.
+ *              XRAW            INT     raw x position 
+ *              YRAW            INT     raw y position (midpoint of 8 pixel bin)
+ *              PHA             BYTE    all 20 - indicating a good point
+ *              WEIGHT          FLOAT   number of photons falling in that bin
+ *              XFARF           FLOAT   x position in geometrically
+ *                                      corrected frame
+ *              YFARF           FLOAT   y position in geometrically
+ *                                      corrected frame
+ *              X               FLOAT   final x position (after correcting
+ *                                      for motions)
+ *              Y               FLOAT   final y position (after correcting
+ *                                      for motions)
+ *              CHANNEL         CHAR    aperture ID for the photon
+ *              TIMEFLGS        CHAR    temporal flags - various bits set 
+ *              LOC_FLGS        CHAR    location flags - various bits set 
+ *              LAMBDA          FLOAT   wavelength for each photon
+ *		ERGCM2		FLOAT	flux calibration for each photon
+ *
+ *              This routine calls cf_fuv_init to populate the calibration
+ *              entries in the header.
+ *
+ *              In addition, the routine creates a timeline table containing
+ *              the orbital information, count rates, and high-voltage
+ *              information to be used by later pipeline modules.
+ * 
+ *
+ * Returns:	Zero upon successful completion.
+ *
+ * History:	05/09/03   v1.1   rdr	Adapted from cf_ttag_init
+ *		06/04/03   v1.4   wvd	Add call to cf_proc_check
+ *              06/10/03   v1.5   rdr   Scan for hot pixels and remove 
+ *		06/11/03   v1.6   wvd	Compress data with TSCALE and TZERO
+ *		06/11/03   v1.7   wvd	Changed calfusettag.h to calfuse.h
+ *		07/17/03   v1.8   wvd   Move various subroutines to libcf.
+ *		07/22/03   v1.9   wvd   Read all extensions of raw hist file.
+ *					Test for hot pixels only in active
+ *					region and only if img[j]>15.
+ *		07/28/03   v1.10  wvd   Close ELEC_CAL.
+ *		10/26/03   v1.11  wvd   Increase morekeys to 38.
+ *		11/05/03   v1.12  wvd   Added stdlib.h and unistd.h.
+ *              12/05/03          bjg   Modified cf_make_pixel_list
+ *                                      to unbin data in y.
+ *              12/10/03   v1.13  bjg   Unbin is now optional 
+ *                                      Update keyword SPECBINY
+ *              03/03/04   v1.14  rdr   Exit if no photons found
+ *              03/05/04   v1.15  rdr   Warning if data is missing
+ *              03/09/04   v1.16  rdr   Fix error in correcting hot pixels
+ *              03/26/04   v1.17  rdr   Continue when there is no data
+ *              03/30/04   v1.20  wvd   Clean up i/o.
+ *              03/31/04   v1.21  bjg   functions return EXIT_SUCCESS instead
+ *                                      of zero. 
+ *                                      >>>Include math.h for fmod<<<
+ *                                      Type conversion for
+ *                                      double fmod(double, double)
+ *              04/06/04   v1.22  bjg   Remove unused variables
+ *                                      Change format to match arg type
+ *                                      in printf
+ *                                      Remove static keyword in struct key 
+ *                                      definition
+ *                                      Add braces in TSCAL and TZERO
+ *                                      definitions
+ *                                      Test for fill data
+ *              10/15/04   v1.23  bjg   Fill Data Photon gets flag
+ *                                      LOCATION_FILL only if it is
+ *                                      in Active Aperture
+ *              12/24/2004 v1.24  bjg   npix_max now takes binx and biny into
+ *                                      account
+ *		01/24/2005 v1.25  wvd   Modify cf_make_pixel_list to ignore
+ *					duplicate data, which can sneak in
+ *					with the stim pulses.
+ *		02/11/2005 v1.26  wvd   Hot pixels and fill data cause the
+ *					header keyword NEVENTS to be too 
+ *					large, so we correct/exclude these
+ *					points and update NEVENTS.
+ *		03/10/2005 v1.27  wvd   Move flagging of airglow photons to
+ *					cf_screen_airglow.
+ *					Initialize XFARF and YFARF with zero.
+ *		05/20/2005 v1.28  wvd   Clean up i/o.
+ *		05/31/2006 v1.29  wvd   OPUS has been updated, so we can set
+ *					morekeys to 0.
+ *		06/12/2006 v1.30  wvd   Call cf_verbose rather than 
+ *					cf_if_warning when an extension 
+ *					contains no photons.
+ *		02/23/2007 v1.31  wvd   If a raw hist file contains no 
+ *					extensions, set EXP_STAT to -1.
+ *					Make active-area limits inclusive.
+ *		11/07/2008 v1.32  wvd   Clean up i/o. 
+ *
+ ****************************************************************************/
+
+#include <stdlib.h>
+#include <string.h>
+#include <unistd.h>
+#include <math.h>
+
+#include "calfuse.h" 
+
+struct key {
+        char keyword[FLEN_KEYWORD];
+        float value;
+        };
+
+
+/*****************************************************************************/
+
+static int
+cf_make_pixel_list(fitsfile *infits, fitsfile *outfits, char unbin) {
+
+/*****************************************************************************
+ *
+ * Description: procedure to take input data from the raw HIST data file and 
+ *              generate a table with 14 columns. This table lists
+ *              all pixels that contain counts. The
+ *              table is designed to mimic a TTAG list, so that it can be used
+ *              with various modules in the TTAG pipeline
+ *
+ ****************************************************************************/
+
+    fitsfile *elecfits; 
+    char  fmt_byte[FLEN_CARD], fmt_float[FLEN_CARD], fmt_short[FLEN_CARD];
+    char  *inpha, *dumarrb;
+    char  elecfile[FLEN_CARD];
+    char  keyword[FLEN_CARD], card[FLEN_CARD];
+    unsigned char *dumarrbu ;
+    int   status=0, anynull=0, hdutype;
+    int	  colval;
+    int   tfields = 14;      /*  output table will have 14 columns */
+    int   active_l, active_r ;
+    long  i, j, k, nevents, nfdp;
+    long  frow=1, felem=1, nrows=1; /* output table will have 1 row */
+    float sum_weights;
+    float *intime, *dumarrf;
+
+    int   sia_index[512], sia_temp[512];  /* Indices of SIA rectangles */
+    int   sia_width = 2048, sia_height = 16;  /* Dimensions of SIA recs */
+    int   xx, yy;		/* Pixel coordinates (unbinned) */
+
+    int x0, y0, xstart, ystart ;
+    int nx, ny, yndx, binx, biny ;
+    int nhot, nhot_total=0;
+    short *xpix, *ypix, *img, *fill_data_pix, nmask, nullval;
+    long npix, npix_max, npts ;
+    float *wtpix, exptime, mtime, nave;
+    
+
+    char extname[]="TTAG DATA";   /* name of the extension containing 
+                                        the binary table holding the data */
+
+    char *ttype[]={"TIME", "XRAW", "YRAW", "PHA", "WEIGHT", "XFARF", 
+		   "YFARF",  "X", "Y", "CHANNEL", "TIMEFLGS",
+		   "LOC_FLGS", "LAMBDA", "ERGCM2" };
+
+    char *tform[14];  /* will asign values when we find out 
+                         the number of elements in the data set */
+
+
+    char *tunit[]={"SECONDS", "PIXELS", "PIXELS", " ", " ", "PIXELS",
+		   "PIXELS", "PIXELS", "PIXELS", "UNITLESS",
+		   "UNITLESS", "UNITLESS", "ANGSTROMS","ERG CM^-2"};
+
+    struct key tscal[] = {{"TSCAL6", 0.25},  {"TSCAL7", 0.1},
+                          {"TSCAL8", 0.25},  {"TSCAL9", 0.1}};
+    struct key tzero[] = {{"TZERO6", 8192.}, {"TZERO7", 0.},
+                          {"TZERO8", 8192.}, {"TZERO9", 0.}};
+
+    /* Initialize the sia_index array. */
+    (void) memset((void *)sia_index, 0, sizeof(int)*512);
+ 
+    /*********************************************************************
+             Read information to be used in the screening analysis.
+    **********************************************************************/
+
+    /* Read the limits to the active area of the detector */
+    FITS_read_key(outfits, TSTRING, "ELEC_CAL", elecfile, NULL, &status);
+    FITS_open_file(&elecfits, cf_cal_file(elecfile), READONLY, &status);
+    FITS_read_key(elecfits, TINT, "ACTIVE_L", &active_l, NULL,
+		  &status);
+    FITS_read_key(elecfits, TINT, "ACTIVE_R", &active_r, NULL,
+		  &status);
+    FITS_close_file(elecfits, &status);
+    cf_verbose(3, "Limits to the active area: left=%d, right=%d",
+	   active_l, active_r);
+
+    /* Determine the exposure time */
+    FITS_movabs_hdu(infits, 1, &hdutype, &status);
+    FITS_read_key(infits, TFLOAT, "EXPTIME", &exptime, NULL, &status);
+    cf_verbose(3, "exptime = %d ", cf_nint(exptime)) ;
+
+    /* Determine the binning factors in x and y */
+    FITS_read_key(infits, TINT, "SPECBINX", &binx, NULL, &status);
+    FITS_read_key(infits, TINT, "SPECBINY", &biny, NULL, &status);
+    cf_verbose(3, "binx=%d, biny=%d \n", binx, biny) ;
+
+
+   /***********************************************************************
+              Get information from the raw data file.
+   ************************************************************************/
+
+    /* Set up arrays to contain the positions of each pixel with counts 
+        (xpix and ypix) and the number of counts in that pixel (wtpix) */
+	if (unbin) npix_max = (NXMAX * NYMAX) / binx ;
+	else npix_max = (NXMAX * NYMAX) / (binx * biny) ;
+        npix = -1 ;
+        xpix =  (short *) cf_calloc(npix_max, sizeof(short)) ;
+        ypix =  (short *) cf_calloc(npix_max, sizeof(short)) ;
+        wtpix = (float *) cf_calloc(npix_max, sizeof(float)) ;
+	fill_data_pix = (short *) cf_calloc(npix_max, sizeof(short)) ;
+         
+    /*
+     *  Loop over all extensions in the input file, and place contents
+     *  of each extension into outbuff.  Keep trying to read a new HDU
+     *  in the input file until we hit the EOF.
+     *
+     *  Note that the next line cannot use FITS_movrel_hdu because
+     *  that routine automatically exits upon error.
+     */
+    for (i = 1; !(fits_movrel_hdu(infits, 1, &hdutype, &status)); i++) {
+        FITS_read_key(infits, TINT, "NAXIS1",  &nx, NULL, &status);
+        FITS_read_key(infits, TINT, "NAXIS2",  &ny, NULL, &status);
+        FITS_read_key(infits, TINT, "XORIGIN", &x0, NULL, &status);
+        FITS_read_key(infits, TINT, "YORIGIN", &y0, NULL, &status);
+
+	npts = nx * ny ;
+        cf_verbose(3, "Reading extension %d ", i) ;
+        cf_verbose(3, "nx=%d, ny=%d, npts=%d ", nx, ny, npts) ;
+
+	/* Initialize the sia_temp array */
+	(void) memset((void *)sia_temp, 0, sizeof(int)*512);
+ 
+        /*
+         *  Allocate space for and read the input image
+         */
+        img = cf_malloc(sizeof(short) * npts);
+        FITS_read_img(infits, TSHORT, 1L, npts, &nullval,
+                      img, &anynull, &status);
+
+	/* Specify the starting positions in x and y.
+	    Place the point in the middle of the bin */
+	xstart = x0 * binx + binx / 2;
+        ystart = y0 * biny + biny / 2;
+	cf_verbose(3, "x0=%d, y0=%d, xstart=%d, ystart=%d",
+		x0, y0, xstart, ystart) ;
+      
+	/* Go through the image and tabulate the pixels with counts. */
+	nhot=0 ;
+        for (j=0; j<npts; j++) 
+          if (img[j] > 0) {
+
+	    /* If this pixel falls in an SIA rectangle that has already
+		been written to the output data list, skip it and move to
+		the next SIA rectangle. */
+
+		xx = (x0 + (j % nx)) * binx;
+		yy = (y0 + (j / nx)) * biny;
+		k = xx / sia_width + yy / sia_height * 8;
+		if (k < 0 || k >= 512) continue;
+		if (sia_index[k] == 1) {
+			j += sia_width / binx - 1;
+			continue;
+		}
+		sia_temp[k] = 1;
+
+	    /* Check for a hot pixel by comparing the value in the pixel with
+               those on either side.  Ignore pixels outside of detector active
+               area or with fewer than 16 counts. */
+
+            if ((img[j] > 15) && (img[j] != FILL_DATA) && 
+		(xx >= active_l) && (xx <= active_r)) {
+                nave = (img[j-2] + img[j-1] + img[j+1] + img[j+2]) / 4. ;
+		  if (nave > 32000.) nave=32000. ;
+                  if (nave < 1.) nave=1. ;
+	        if (img[j] > 8*nave) {
+		  nhot++ ;
+		  cf_verbose(3,"hot pixel at point %d: val=%d, ave=%f", 
+                       j, img[j], nave) ;
+		  /* Repair hot pixel */
+                  nmask=1 ;
+		  while(nmask < 8*nave && nmask < 16000) nmask*=2 ; 
+		  nmask-=1 ;
+		  img[j] = (img[j] & nmask) ;
+                  cf_verbose(3,"corrected value = %d ",img[j]) ;
+		}
+	    }
+
+	    yndx = (int) ( j / nx ) ;
+
+            if (unbin){
+	      for (k=0;k<biny;k++){
+		npix++ ;
+		xpix[npix]  = (short) (xstart + (j - (yndx * nx)) * binx) ;
+		ypix[npix]  = (short) (ystart + yndx*biny + k) ;
+		wtpix[npix] = (float) ( ((float) img[j]) / ((float) biny) ) ;
+
+		fill_data_pix[npix]=0;
+		if (img[j] == FILL_DATA) {
+		  wtpix[npix]=0.0;
+		  fill_data_pix[npix]=1;
+		}
+
+
+	      }
+	    }
+	    else {
+	      npix++ ;
+	      xpix[npix]  = (short) (xstart + (j - (yndx * nx)) * binx) ;
+	      ypix[npix]  = (short) (ystart + yndx*biny) ;
+	      wtpix[npix] = (float) img[j];
+	      
+	      fill_data_pix[npix]=0;
+	      if (img[j] == FILL_DATA) {
+		wtpix[npix]=0.0;
+		fill_data_pix[npix]=1;
+	      }
+	    }
+
+	   
+	  }
+
+	nhot_total += nhot;
+        cf_verbose(2, "%d hot pixels found in extn %d  ",nhot, i) ;
+        cf_verbose(3, "total number of pixels with counts = %d \n", npix) ;
+        if (nhot > 10) cf_if_warning("More than 10 hot pixels found.") ;
+
+        free(img) ;
+
+	/* Copy new SIA indices to sia_index array. */
+	for (k = 0; k < 512; k++)
+		if (sia_temp[k]) sia_index[k] = 1;
+
+    }  /* Finished loop over all extensions in infits */
+    /*
+     *  Status upon completion of loop through extensions should be
+     *  "end of file."
+     *  If it is, reset value of status.  If not, there was an
+     *  unexpected error.  Print and exit.
+     */
+    if( status == END_OF_FILE ) {  /* !!! This might cause a problem */
+        status = 0;
+    } else  {
+        cf_if_fits_error(status);
+    }
+
+    cf_verbose(3, "Finished reading data ") ;
+
+    if (npix < 0) {
+	npix = 1 ;
+        xpix[0]=0 ;
+        ypix[0]=0 ;
+        wtpix[0]=1. ;
+	fill_data_pix[0]=0;
+    }
+
+   /*************************************************************************
+           Output the analysis to a table
+   ***************************************************************************/  
+
+    /* Generate the tform array */
+    sprintf(fmt_byte,  "%ldB", npix);
+    sprintf(fmt_float, "%ldE", npix);
+    sprintf(fmt_short, "%ldI", npix);
+
+    tform[0] = fmt_float;
+    tform[1] = fmt_short;
+    tform[2] = fmt_short;
+    tform[3] = fmt_byte;
+    tform[4] = fmt_float;
+    for (i=5; i<9; i++)
+        tform[i] = fmt_short;
+    for ( ; i<12; i++)
+        tform[i] = fmt_byte;
+    tform[12] = fmt_float;
+    tform[13] = fmt_float;
+
+   /* Append a new empty binary table to the output file */
+
+    cf_verbose(3, "Creating table") ;
+    FITS_movabs_hdu(outfits, 1, &hdutype, &status);
+    FITS_create_tbl(outfits, BINARY_TBL, nrows, tfields, ttype, tform,
+                        tunit, extname, &status);
+
+    /* Write TSCALE and TZERO entries to header */
+    for (i=0; i<4; i++) {
+        sprintf(keyword, "TUNIT%ld", i+6);
+        if (fits_read_keyword(outfits, keyword, card, NULL, &status))
+		cf_if_fits_error(status);
+        FITS_insert_key_flt(outfits, tscal[i].keyword, tscal[i].value, -2,
+		NULL, &status);
+        FITS_insert_key_flt(outfits, tzero[i].keyword, tzero[i].value, -4,
+		NULL, &status);
+    }
+   
+    /*   Allocate space for the new output columns */
+  
+    cf_verbose(3, "Allocating space for arrays ") ;
+    dumarrf  = (float *) cf_malloc(sizeof(float) * npix);
+    dumarrb  = (char *) cf_malloc(sizeof(char) * npix);
+    dumarrbu  = (unsigned char *) cf_malloc(sizeof(unsigned char) * npix);
+ 
+    cf_verbose(3, "Filling columns") ;  
+    /* Specify a time array - assign the same time to all pixels */
+    intime = (float *) cf_calloc(npix, sizeof(float) ) ;
+    mtime = exptime/2. ;
+    for (i=0; i<npix; i++) intime[i]=mtime ;
+    FITS_write_col(outfits, TFLOAT, 1, frow, felem, npix, intime, &status);
+
+    /* Output X and Y positions  */
+    FITS_write_col(outfits, TSHORT, 2, frow, felem, npix, xpix, &status);
+    FITS_write_col(outfits, TSHORT, 3, frow, felem, npix, ypix, &status);
+
+    /* Now do the PHA column - assume 20 */
+    inpha = (char *) cf_calloc(npix, sizeof(char) ) ;
+    for (i=0; i<npix; i++) inpha[i] = 20 ;
+    FITS_write_col(outfits, TBYTE, 4, frow, felem, npix, inpha, &status);
+
+    /* Fill weights column with counts per pixel */ 
+    FITS_write_col(outfits, TFLOAT, 5, frow, felem, npix, wtpix, &status);
+
+    /* Fill XFARF, YFARF, X and Y arrays with 0 */
+    for (i=0; i<npix; i++) dumarrf[i] = 0.;
+    for (colval=6; colval<10; colval++) {
+        FITS_write_col(outfits, TFLOAT, colval, frow, felem, npix,
+		dumarrf, &status);
+    }
+
+    /* Initialize the channel and temporal flag arrays with 0 - byte */
+    for (i=0;i<npix; i++)
+	dumarrb[i] = 0;
+    FITS_write_col(outfits, TBYTE, 10, frow, felem, npix, dumarrb, &status);
+    for (i=0;i<npix; i++)
+	dumarrbu[i] = 0;
+    FITS_write_col(outfits, TBYTE, 11, frow, felem, npix, dumarrbu, &status);
+
+    /* Flag events that lie outside of the active area or
+	in fill-data regions. */
+    for (i=0 ; i<npix ; i++) {
+	dumarrbu[i] = 0 ;
+
+	/* Flag photons that lie outside the active area. */
+	if (xpix[i] < active_l || xpix[i] > active_r) 
+	    dumarrbu[i] = dumarrbu[i] | LOCATION_SHLD ;
+
+	/* If inside, is it fill data? */
+	else if (fill_data_pix[i])
+	    dumarrbu[i] = dumarrbu[i] | LOCATION_FILL ; 
+    }
+
+    FITS_movabs_hdu(outfits, 2, &hdutype, &status);
+    FITS_write_col(outfits, TBYTE, 12, frow, felem, npix,
+		       dumarrbu, &status);
+
+    /* Fill lambda and energy arrays with 0 */
+    FITS_write_col(outfits, TFLOAT, 13, frow, felem, npix, dumarrf, &status);
+    FITS_write_col(outfits, TFLOAT, 14, frow, felem, npix, dumarrf, &status);
+
+    /* If file contains hot pixels or fill data, recalculate NEVENTS. */
+    nfdp = 0;
+    sum_weights = 0.;
+    for (i=0; i<npix; i++) {
+	nfdp += fill_data_pix[i];
+	sum_weights += wtpix[i];
+    }
+    if (nfdp > 0 || nhot_total > 0) {
+	nevents = cf_nlong(sum_weights);
+	FITS_movabs_hdu(outfits, 1, &hdutype, &status);
+	FITS_update_key(outfits, TLONG, "NEVENTS", &nevents, NULL, &status);
+	cf_verbose(1, "Image contains bad pixels.  Updating NEVENTS = %ld",
+	nevents);
+    }
+
+    free(intime);
+    free(xpix);
+    free(ypix);
+    free(wtpix) ;
+    free(inpha);
+    free(dumarrf);
+    free(dumarrb);
+
+    cf_verbose(3, "Leaving cf_make_pixel_list") ;
+
+    return EXIT_SUCCESS ;
+}
+
+
+/******************************************************************************
+ *
+ *                   CF_MAKE_GTI_TABLE
+ *
+ *      Procedure to generate a table of GTI values and put it into the second
+ *      extension of the output file. There is assumed to be only one GTI, 
+ *      starting at 0 and ending at the exposure time.
+ *
+ ******************************************************************************/
+
+int cf_make_gti_table (fitsfile *outfits) {
+
+    int status=0, nrows=1, hdutype, frow=1, felem=1  ;
+    float exptime ;
+    double start[1]={0.}, stop[1] ;
+
+    char extname[]="GTI";
+    int tfields=2;	/* output table will have 2 columns */
+    char *ttype[]={"START", "STOP"};
+
+    char *tform[]={"1D","1D"}; 
+    char *tunit[]={"seconds", "seconds"};
+
+    cf_verbose(3, "Entering cf_make_gti_table ") ;
+
+    /* read the exposure time from the output file */
+    FITS_movabs_hdu(outfits, 1, &hdutype, &status);
+    FITS_read_key(outfits, TFLOAT, "EXPTIME", &exptime, NULL, &status);
+    stop[0] = (double) exptime ;
+
+
+    /* Append a new empty binary table to the output file */
+    FITS_movabs_hdu(outfits, 2, &hdutype, &status);
+    FITS_create_tbl(outfits, BINARY_TBL, nrows, tfields, ttype, tform,
+			tunit, extname, &status);
+
+    /* Write the data to the table */
+    FITS_write_col(outfits, TDOUBLE, 1, frow, felem, nrows, start, &status);
+    FITS_write_col(outfits, TDOUBLE, 2, frow, felem, nrows, stop, &status);
+
+    return EXIT_SUCCESS ;
+}
+
+/*****************************************************************************/
+
+
+int main(int argc, char *argv[])
+{
+    char CF_PRGM_ID[] = "cf_hist_init"; 
+    char CF_VER_NUM[] = "1.32";
+
+    fitsfile *infits, *outfits;
+   
+    int   morekeys=0;		/* Change to zero when OPUS is updated. */
+    int   status=0, optc;
+   
+    int one=1, nextn=0;
+    long nphot ;
+    char unbin=0;
+
+    char opts[] = "hsv:";
+    char usage[] =
+	"Usage:\n"
+	"  cf_hist_init [-h] [-s] [-v level] rawhistfile idf_file\n";
+    char option[] = 
+	"Options:\n"
+	"  -h:  this help message\n"
+        "  -s:  to unbin the data in Y\n"
+        "  -v:  verbosity level (default is 1; 0 is silent)\n";
+      
+
+    verbose_level = 1;
+
+    while ((optc = getopt(argc, argv, opts)) != -1) {
+	switch(optc) {
+
+	case 'h':
+	    printf("%s\n%s", usage, option);
+	    return 0;
+	case 's':
+	    unbin=1;
+	    break;
+	case 'v':
+	    verbose_level = atoi(optarg);
+	    break;
+	}
+    }
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    if (argc != optind+2) {
+        printf("%s", usage);
+        cf_if_error("Incorrect number of arguments");
+    }
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin execution");
+
+    FITS_open_file(&infits, argv[optind++], READONLY, &status);
+
+    /*  Exit if data are not in HIST mode. */
+    if ( cf_proc_check(infits, CF_PRGM_ID) ) {
+        FITS_close_file(infits, &status);
+        return (-1);
+    }
+
+    /* Issue warning message if data are missing. */
+    FITS_read_key(infits, TLONG, "NEVENTS", &nphot, NULL, &status); 
+    FITS_read_key(infits, TINT, "NEXTEND", &nextn, NULL, &status); 
+    cf_verbose(3,"Number of extensions to the file = %d ", nextn) ;
+    if (nphot < 1) cf_verbose(1, "%s contains no photons.", argv[optind-1]);
+    if (nextn < 1) cf_if_warning("%s contains no extensions.", argv[optind-1]); 
+    else if (nextn < 4) cf_verbose(1, "%s contains only %d extensions.",
+	argv[optind-1], nextn) ; 
+
+    /*  Create output file. */
+    FITS_create_file(&outfits, argv[optind], &status);
+    /*  Copy primary image header from the input file. */
+    FITS_copy_hdu(infits, outfits, morekeys, &status);
+
+    /* Update header keywords. */
+    FITS_update_key(outfits, TSTRING, "FILENAME", argv[optind], NULL, &status);
+    FITS_update_key(outfits, TSTRING, "FILETYPE",
+                 "INTERMEDIATE DATA FILE", NULL, &status);
+
+    if (unbin) FITS_update_key(outfits, TINT, "SPECBINY", &one, NULL, &status);
+
+    /* If input file contains no extensions, set EXP_STAT to -1. */
+    if (nextn < 1) {
+	char comment[] = "Raw file contains no data.";
+	int eflag = -1; 
+	FITS_update_key(outfits, TINT, "EXP_STAT", &eflag, comment, &status);
+    }
+
+    /* Populate the calibration keywords in the primary header. */
+    cf_fuv_init(outfits);
+
+    /* Fill in the first extension with the photon information */
+    cf_make_pixel_list(infits, outfits, unbin) ;
+
+    /* Generate a good-times table and put it in the second extension. */
+    cf_make_gti_table(outfits);
+  
+    /*  Append a table containing the orbital timeline */
+    cf_timeline(outfits);
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+    /*  Update processing flags. */
+    cf_proc_update(outfits, CF_PRGM_ID, "COMPLETE");
+
+    FITS_close_file(infits, &status);
+    FITS_close_file(outfits, &status);
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished execution.");
+
+    return EXIT_SUCCESS ;
+}
diff --git a/src/fuv/cf_remove_motions.c b/src/fuv/cf_remove_motions.c
new file mode 100644
index 0000000..ec2b332
--- /dev/null
+++ b/src/fuv/cf_remove_motions.c
@@ -0,0 +1,316 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences 
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_remove_motions options intermediate_file     
+ *
+ * Description: Associates a photon with an aperture and corrects for grating,
+ *              mirror, spacecraft (jitter) and focal plane assembly (FPA)
+ *              motion.  The position of the Y centroid is also determined
+ *		both as a function of time (before correction for s/c motion)
+ *		and for the entire exposure (after motion correction).
+ *              The resulting coordinates represent the data obtained by a
+ *		motionless instrument. 
+ *
+ *              By default, all corrections are performed.  Command line
+ *              options allow one or more corrections to be omitted.
+ *
+ * Arguments:   input_file              Intermediate data file
+ *
+ * Calibration files:                   
+ *
+ * Returns:     0 on successful completion
+ *
+ * Calls:       cf_find_spectra, cf_calculate_ycent_motion,
+ *              cf_grating_motion, cf_fpa_position, cf_mirror_motion,
+ *              cf_satellite_jitter, cf_calculate_y_centroid
+ *
+ * History:     09/30/02   peb    1.1   Begin work
+ *		12/04/02   wvd    1.5   Install Y centroid routines.
+ *                                      Modify call to cf_satellite_jitter
+ *		12/12/02   wvd    1.6   Change infits -> header throughout
+ *              03/04/03   peb    1.10  Minor code changes to remove gcc -Wall
+ *                                      messages: unused j in main.
+ *                                      Added unistd.h, so getopt is portable
+ *		03/05/03   wvd    1.11  Added cf_target_count_rate
+ *              03/10/03   peb    1.12  Added verbose_level, unistd.h for
+ *                                      getopt portability, and changed
+ *                                      locflags to unsigned char *.
+ *              03/13/03   rdr    1.13  corrected small error in tabulating
+ *                                      count rate_sic
+ *              04/17/03   wvd	  1.17  Add cf_find_spectra for initial
+ *					assignment of photons to
+ *					target apertures.  Add last_call to
+ *					cf_identify_channel, last_call and
+ *					weight to cf_calculate_y_centroid
+ *		04/21/03   wvd    1.18  Pass tsunrise to cf_grating_motion,
+ *					tsunset to cf_mirror_motion,
+ *					channel to cf_satellite_jitter.
+ *		06/02/03   wvd    1.20  Don't modify count-rate arrays
+ *					for HIST data.
+ *		06/11/03   wvd    1.21  Pass datatype to cf_read_col and
+ *					cf_write_col.
+ *		08/01/03   wvd    1.23  Add cf_error_init after calls to
+ *					subroutines.
+ *		08/06/03   wvd    1.24  Change channel to unsigned char.
+ *					Remove GTI's from cf_satellite_jitter.
+ *		08/25/03   wvd    1.25  Change coltype from string to int in
+ *					cf_read_col and cf_write_col.
+ *		09/18/03   wvd    1.26  Pass locflags to cf_identify_channel
+ *		10/21/03   wvd    1.27  For HIST data, don't write blank
+ *					LiF and SiC count-rate arrays to IDF.
+ *		10/27/03   wvd    1.28  Pass pha array to cf_find_spectra.
+ *					Delete last_call from argument list
+ *					of cf_calculate_y_centroid.
+ *		10/31/03   wvd    1.29  Treat channel as unsigned char
+ *					throughout.
+ *              04/06/04   bjg    1.30  Remove unused variables
+ *		05/03/04   wvd    1.31  Improve documentation.
+ *					Move first call of cf_identify_channel
+ *					from cf_find_spectra to this routine.
+ *		06/02/04   wvd    1.32  Copy/move cf_set_photon_flags(),
+ *					cf_set_good_time_intervals(), and
+ *					cf_modify_hist_times() from 
+ *					cf_screen_photons.  Run them only if
+ *					cf_satellite_jitter rejects some time
+ *					AND if they were already run before.
+ *					Pass timeflags to cf_find_spectra()
+ *					and cf_calculate_y_centroid().
+ *					Get exp_jitr from cf_satellite_jitter.
+ *		07/21/04   wvd    1.33  Add include file <string.h>
+ *		03/10/05   wvd    1.34  Change use of variable pad.  Now add
+ *					10 to user_pad on first call to 
+ *					cf_identify_channel, 0 on second call.
+ *		03/22/05   wvd    1.35  Change TIME_SUNRISE and TIME_SUNSET
+ *					from floats to shorts.
+ *		05/20/05   wvd    1.36  Clean up i/o.
+ *		09/09/05   wvd    1.37  Add -j to list of allowed options.
+ *		11/29/05   wvd    1.38  Separate cf_satellite_jitter into two
+ *					routines.  Screening is performed 
+ *					earlier, so we need not copy flags.
+ *		08/30/06   wvd    1.39  Add -a to list of allowed options.
+ *		12/29/06   wvd    1.40  Pass weights array and initial LiF
+ *					and SiC counts arrays to 
+ *					cf_target_count_rate.  Make arrays
+ *					rate_lif and rate_sic floats.  If 
+ *					they are too large to store as shorts, 
+ *					store as unsigned shorts.
+ *		02/02/07   wvd    1.41  If LiF or SiC count rate is too large
+ *					for an unsigned int, set to zero.
+ *
+ ****************************************************************************/
+
+#include <unistd.h>
+#include <stdlib.h>
+#include <string.h>
+#include "calfuse.h"
+
+static char CF_PRGM_ID[] = "cf_remove_motions";
+static char CF_VER_NUM[] = "1.41";
+
+int
+main(int argc,  char *argv[])
+{
+    unsigned char *channel=NULL, *timeflags=NULL, *locflags=NULL,
+	*statflag=NULL;
+    int  grating_motion=1, fpa_position=1, mirror_motion=1, sat_jitter=1;
+    int  last_call, set_times=FALSE, set_gtis=FALSE, airglow_centroid=FALSE;
+    int  user_pad=0, status=0, set_rate=FALSE, optc;
+    long i, nevents, ntimes;
+    float *time=NULL, *ttime=NULL, *xfarf=NULL, *yfarf=NULL, *x, *y;
+    float *weight=NULL, *ycent_lif, *ycent_sic;
+    float max_rate_lif=0, max_rate_sic=0, *rate_lif=NULL, *rate_sic=NULL;
+    float tscale=1, tzero=32768; 
+    short *tsunrise=NULL, *tsunset=NULL;
+    GTI  gti;
+    fitsfile *header;
+    
+    char opts[]  = "hagfmjp:v:";
+    char usage[] = 
+	"Usage:\n"
+	"  cf_remove_motions [-hagfmj] [-p pad] [-v level] idf_file\n";
+    char option[] =
+	"Options:\n"
+	"  -h:  this help message\n"
+	"  -v:  verbose level (default is 1; 0 is silent)\n"
+	"  -a:  use airglow lines to determine spectral centroid\n"
+	"  -p:  aperture padding in pixels (default is 10)\n"
+	"  -g:  no grating motion correction\n"
+	"  -f:  no fpa position correction\n"
+	"  -m:  no mirror motion correction\n"
+	"  -j:  no satellite jitter correction\n";
+
+    verbose_level = 1;
+
+    while ((optc = getopt(argc, argv, opts)) != -1) {
+	switch(optc) {
+
+	case 'h':
+	    printf("%s\n%s", usage, option);
+	    return 0;
+	case 'v':
+	    verbose_level = atoi(optarg);
+	    break;
+	case 'p':
+	    user_pad = atoi(optarg);
+	    break;
+	case 'g':
+	    grating_motion = 0;
+	    break;
+	case 'f':
+	    fpa_position = 0;
+	    break;
+	case 'a':
+	    airglow_centroid = TRUE;
+	    break;
+	case 'm':
+	    mirror_motion = 0;
+	    break;
+	case 'j':
+	    sat_jitter = 0;
+	    break;
+	}
+    }
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+    if (argc <= optind) {
+        printf("%s", usage);
+        cf_if_error("Incorrect number of command-line arguments");
+    }
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    FITS_open_file(&header, argv[optind], READWRITE, &status);
+ 
+    FITS_movabs_hdu(header, 2, NULL, &status);
+    nevents = cf_read_col(header, TFLOAT, "TIME",   (void **) &time);
+    nevents = cf_read_col(header, TFLOAT, "WEIGHT", (void **) &weight);
+    nevents = cf_read_col(header, TFLOAT, "XFARF",  (void **) &xfarf);
+    nevents = cf_read_col(header, TFLOAT, "YFARF",  (void **) &yfarf);
+    nevents = cf_read_col(header, TBYTE,  "TIMEFLGS", (void **) &timeflags);
+    nevents = cf_read_col(header, TBYTE,  "LOC_FLGS", (void **) &locflags);
+    channel = cf_calloc(nevents, sizeof(unsigned char));
+
+    FITS_movabs_hdu(header, 4, NULL, &status) ;
+    ntimes = cf_read_col(header, TFLOAT, "TIME", (void **) &ttime) ;
+    ntimes = cf_read_col(header, TBYTE,  "STATUS_FLAGS", (void **) &statflag);
+    ntimes = cf_read_col(header, TSHORT, "TIME_SUNRISE", (void **) &tsunrise) ;
+    ntimes = cf_read_col(header, TSHORT, "TIME_SUNSET",  (void **) &tsunset) ;
+    ntimes = cf_read_col(header, TFLOAT, "LIF_CNT_RATE",  (void **) &rate_lif) ;
+    ntimes = cf_read_col(header, TFLOAT, "SIC_CNT_RATE",  (void **) &rate_sic) ;
+    ycent_lif=(float *) cf_calloc(ntimes, sizeof(float)) ;
+    ycent_sic=(float *) cf_calloc(ntimes, sizeof(float)) ;
+
+    FITS_movabs_hdu(header, 1, NULL, &status);
+    x = xfarf;
+    y = yfarf;
+
+    /* Find all six spectra and compute centroids. */
+    cf_find_spectra(header, nevents, weight, x, y, channel, timeflags,
+        locflags, airglow_centroid);
+
+    /* Initial assignment of channel numbers to photons */
+    cf_identify_channel(header, nevents, xfarf, yfarf, channel, locflags,
+	user_pad+10, last_call=FALSE);
+
+    /* Track Y centroids of moving spectra. */
+    cf_calculate_ycent_motion(header, nevents, time, y, channel, locflags,
+	ntimes, ttime, ycent_lif, ycent_sic);
+
+    /* Correct for detector motion during exposure. */
+    if (grating_motion)
+	cf_grating_motion(header, nevents, time, x, y, channel,
+		ntimes, ttime, tsunrise);
+
+    /* Shift spectra in X to account for position of the FPA. */
+    if (fpa_position)
+	cf_fpa_position(header, nevents, x, channel);
+
+    /* Correct for mirror motion during exposure. */
+    if (mirror_motion)
+	cf_mirror_motion(header, nevents, time, x, y, channel,
+		ntimes, ttime, tsunset);
+
+    /* Correct for spacecraft motion during exposure. */
+    if (sat_jitter)
+	cf_satellite_jitter(header, nevents, time, x, y, channel,
+		ntimes, ttime, statflag);
+ 
+    /* Compute centroids of motion-corrected spectra. */
+    cf_calculate_y_centroid(header, nevents, weight, x, y, channel, 
+	timeflags, locflags);
+
+    /* Final assignment of channel numbers to photons */
+    cf_identify_channel(header, nevents, x, y, channel, locflags,
+	user_pad, last_call=TRUE); 
+
+    /* Compute count rates for TTAG target spectra. */
+    set_rate = !(cf_target_count_rate(header, nevents, time, weight,
+	channel, locflags, ntimes, ttime, rate_lif, rate_sic)); 
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+    cf_verbose(3, "Writing X, Y, CHANNEL to IDF");
+    FITS_movabs_hdu(header, 2, NULL, &status);
+    if (set_times)
+        cf_write_col(header, TFLOAT, "TIME", (void *) time, nevents);
+    cf_write_col(header, TFLOAT, "X",      (void *) x,   nevents);
+    cf_write_col(header, TFLOAT, "Y",      (void *) y,   nevents);
+    cf_write_col(header, TBYTE, "CHANNEL", (void *) channel, nevents);
+
+    if (set_gtis) {
+	cf_verbose(3, "Writing good-time intervals to IDF");
+	FITS_movabs_hdu(header, 3, NULL, &status);
+	cf_write_col(header, TDOUBLE, "START", (void *) gti.start, gti.ntimes);
+	cf_write_col(header, TDOUBLE, "STOP", (void *) gti.stop, gti.ntimes);
+	free(gti.stop);
+	free(gti.start);
+    }
+
+    FITS_movabs_hdu(header, 4, NULL, &status);
+    cf_verbose(3, "Writing timeline information to IDF");
+    if (set_rate) {
+	for (i = 0; i < ntimes; i++) {
+	    if (rate_lif[i] > 65535) rate_lif[i] = 0;
+	    if (rate_sic[i] > 65535) rate_sic[i] = 0;
+	    if (max_rate_lif < rate_lif[i]) max_rate_lif = rate_lif[i];
+	    if (max_rate_sic < rate_sic[i]) max_rate_sic = rate_sic[i];
+	}
+	cf_verbose(2, "max_rate_lif = %.0f", max_rate_lif);
+	cf_verbose(2, "max_rate_sic = %.0f", max_rate_sic);
+	if (max_rate_lif > 32767) {
+	    FITS_update_key(header, TFLOAT, "TSCAL10", &tscale, NULL, &status);
+	    FITS_update_key(header, TFLOAT, "TZERO10", &tzero, NULL, &status);
+	    fits_set_tscale(header, 10, (double)tscale, (double)tzero, &status);
+	}
+	if (max_rate_sic > 32767) {
+	    FITS_update_key(header, TFLOAT, "TSCAL11", &tscale, NULL, &status);
+	    FITS_update_key(header, TFLOAT, "TZERO11", &tzero, NULL, &status);
+	    fits_set_tscale(header, 11, (double)tscale, (double)tzero, &status);
+	}
+	FITS_write_col(header, TFLOAT, 10, 1, 1, ntimes, rate_lif, &status);
+	FITS_write_col(header, TFLOAT, 11, 1, 1, ntimes, rate_sic, &status);
+    }
+    cf_write_col(header, TFLOAT, "YCENT_LIF", (void *) ycent_lif, ntimes);
+    cf_write_col(header, TFLOAT, "YCENT_SIC", (void *) ycent_sic, ntimes);
+    cf_verbose(3, "IDF updates complete");
+
+    FITS_close_file(header, &status);
+
+    free(time);
+    free(weight);
+    free(xfarf);
+    free(yfarf);
+    free(locflags);
+    free(timeflags);
+    free(channel);
+    free(ttime);
+    free(rate_lif);
+    free(rate_sic);
+    free(ycent_lif);
+    free(ycent_sic);
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return status;
+}
diff --git a/src/fuv/cf_screen_photons.c b/src/fuv/cf_screen_photons.c
new file mode 100644
index 0000000..bd82bba
--- /dev/null
+++ b/src/fuv/cf_screen_photons.c
@@ -0,0 +1,298 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_screen_photons options intermediate_file
+ *
+ * Description: Filters events in the intermediate data file (IDF) for limb
+ *              angle, SAA crossing, high voltage changes, bursts, and PHA.
+ *              Sets the event flags and GTIs.  Data are modified in place.
+ *
+ *              By default all corrections are performed.  Command line
+ *              options allow one or more corrections to be omitted.
+ *
+ * Arguments:   input_file              FARF-corrected intermediate data file
+ *
+ * Calibration files:                   
+ *
+ * Returns:     0 on successful completion
+ *
+ * Calls:       cf_screen_limb_angle, cf_screen_saa, cf_screen_high_voltage,
+ *              cf_screen_burst, cf_screen_jitter,
+ *		cf_set_user_gtis, cf_set_photon_flags, cf_modify_hist_times, 
+ *		cf_screen_pulse_height, cf_screen_airglow, cf_screen_bad_pixels
+ *
+ * History:     11/05/02   1.1   peb    Begin work
+ *              11/13/02   1.2   peb    Added screening functions to program
+ *              11/14/02   1.3   peb    Added burst-screening function
+ *              11/18/02   1.4   peb    Corrected logic dealing with reading,
+ *                                      writing, and freeing of GTI struct.
+ *                                      Corrected some grammatical errors.
+ *              12/10/02   1.5   rdr    changed call to cf_screen_bursts
+ *              12/18/02   1.6   rdr    updated names of some columns in
+ *                                      the calls to the timeline extension
+ *              12/20/02   1.7   wvd    Change flags to unsigned char
+ *              03/10/03   1.9   peb    Added verbose_level and added unistd.h
+ *                                      for getopt portability
+ *              05/10/03   1.10  wvd    Pass locflag to cf_set_photon_flags
+ *              05/30/03   1.11  wvd    Pass weight to cf_set_photon_flags
+ *              06/11/03   1.12  wvd    Treat HV as array of shorts.
+ *		                        Pass datatype to cf_read_col and
+ *					cf_write_col.
+ *		08/25/03   1.13  wvd	Change coltype from string to int in
+ *					cf_read_col and cf_write_col.
+ *		09/10/03   1.14  wvd	Change background array to type short.
+ *					Add cf_set_user_gtis().
+ *		10/02/03   1.15  wvd	Pass locflag array to
+ *					cf_screen_pulse_height; write to IDF
+ *		02/10/04   1.16  wvd	Add cf_screen_fifo_overflow()
+ *		06/02/04   1.17  wvd	Add cf_modify_hist_times()
+ *		06/03/04   1.18  wvd	Read XFARF and YFARF, not X and Y.
+ *					If INSTMODE = TTAG, don't bother to
+ *					call cf_modify_hist_times().
+ *		02/02/05   1.19  wvd	Pass rate_aic to cf_screen_burst
+ *		03/10/05   1.20  wvd	Add cf_screen_airglow()
+ *		03/30/05   1.21  wvd	Don't change TIME_COR to SKIPPED
+ *					for TTAG data.  Leave as OMIT.
+ *		05/20/05   1.22  wvd	Clean up i/o.
+ *		06/03/05   1.23  wvd	Fix typo in CF_VER_NUM.
+ *		09/09/05   1.24  wvd	Update list of allowed options.
+ *		11/09/05   1.25  wvd	Change argument list for
+ *					cf_screen_fifo_overflow.
+ *		11/22/05   1.26  wvd	Add cf_screen_jitter and
+ *					cf_screen_bad_pixels.
+ *		01/24/06   1.27  wvd	Move cf_screen_airglow before
+ *					cf_screen_burst
+ *              12/29/06   1.28  wvd    Move cf_screen_fifo_overflow to
+ *                                      cf_convert_to_farf.
+ *              07/18/08   1.29  wvd    Write STATUS_FLAGS to IDF before
+ *					calling cf_set_photon_flags, which
+ *					may change the array.
+ *
+ ****************************************************************************/
+
+#include <unistd.h>
+#include <stdlib.h>
+#include <string.h>
+#include "calfuse.h"
+
+int
+main(int argc, char *argv[])
+{
+    char CF_PRGM_ID[] = "cf_screen_photons";
+    char CF_VER_NUM[] = "1.29";
+
+    char instmode[FLEN_VALUE];
+    unsigned char *pha=NULL, *timeflag=NULL, *statflag=NULL, *locflag=NULL;
+    int  limb_screening=1, saa_screening=1, voltage_screening=1;
+    int  burst_screening=1, set_flags=1, airglow_screening=1, pha_screening=1;
+    int  modify_times=1, set_gtis=1, set_user_gtis=1;
+    int  bad_pixel_screening=1, set_times=FALSE, jitter_screening=1;
+    int  status=0, optc;
+    long nevents, nseconds;
+    short *background=NULL, *rate_lif=NULL, *rate_sic=NULL, *voltage=NULL;
+    float *time=NULL, *x=NULL, *y=NULL, *weight=NULL;
+    float *timeline=NULL, *limb=NULL, *longitude=NULL, *latitude=NULL;
+    float *rate_aic=NULL;
+    GTI  gti;
+    fitsfile *header;
+    
+    char opts[]  = "halstbjufimdpv:";
+    char usage[] = 
+	"Usage:\n"
+	"  cf_screen_photons [-halstbjufimdp] [-v level] idf_file\n";
+    char option[] =
+	"Options:\n"
+	"  -h:  this help message\n"
+	"  -v:  verbosity level (default is 1; 0 is silent)\n"
+	"  -a:  no airglow screening\n"
+	"  -l:  no limb screening\n"
+	"  -s:  no SAA screening\n"
+	"  -t:  no high voltage screening\n"
+	"  -b:  no burst screening\n"
+	"  -j:  no jitter screening\n"
+	"  -u:  no user-defined good-time intervals\n"
+	"  -f:  do not set photon event flags\n"
+        "  -i:  do not update GTI arrays\n"
+	"  -m:  do not modify HIST photon times\n"
+	"  -d:  no bad-pixel screening\n"
+	"  -p:  no PHA screening\n";
+
+    verbose_level = 1;
+
+    while ((optc = getopt(argc, argv, opts)) != -1) {
+	switch(optc) {
+
+	case 'h':
+	    printf("%s\n%s", usage, option);
+	    return 0;
+	case 'v':
+	    verbose_level = atoi(optarg);
+	    break;
+	case 'l':
+	    limb_screening = 0;
+	    break;
+	case 't':
+	    voltage_screening = 0;
+	    break;
+	case 's':
+	    saa_screening = 0;
+	    break;
+	case 'b':
+	    burst_screening = 0;
+	    break;
+	case 'j':
+	    jitter_screening = 0;
+	    break;
+	case 'u':
+	    set_user_gtis = 0;
+	    break;
+	case 'f':
+	    set_flags = 0;
+	    break;
+        case 'i':
+            set_gtis = 0;
+            break;
+	case 'm':
+	    modify_times = 0;
+	    break;
+	case 'a':
+	    airglow_screening = 0;
+	    break;
+	case 'd':
+	    bad_pixel_screening = 0;
+	    break;
+	case 'p':
+	    pha_screening = 0;
+	    break;
+	}
+    }
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    if (argc <= optind) {
+        printf("%s", usage);
+        cf_if_error("Incorrect number of program arguments");
+    }
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    FITS_open_file(&header, argv[optind], READWRITE, &status);
+
+    FITS_movabs_hdu(header, 2, NULL, &status);
+    nevents = cf_read_col(header, TFLOAT, "TIME",   (void **) &time);
+    nevents = cf_read_col(header, TBYTE,  "PHA",    (void **) &pha);
+    nevents = cf_read_col(header, TFLOAT, "WEIGHT", (void **) &weight);
+    nevents = cf_read_col(header, TFLOAT, "XFARF",  (void **) &x);
+    nevents = cf_read_col(header, TFLOAT, "YFARF",  (void **) &y);
+    nevents = cf_read_col(header, TBYTE,  "TIMEFLGS", (void **) &timeflag);
+    nevents = cf_read_col(header, TBYTE,  "LOC_FLGS", (void **) &locflag);
+
+    if (burst_screening) {
+	FITS_movabs_hdu(header, 3, NULL, &status);
+	gti.ntimes = cf_read_col(header, TDOUBLE, "START",(void **) &gti.start);
+	gti.ntimes = cf_read_col(header, TDOUBLE, "STOP", (void **) &gti.stop);
+    }
+    FITS_movabs_hdu(header, 4, NULL, &status);
+    nseconds = cf_read_col(header, TFLOAT, "TIME",         (void **) &timeline);
+    nseconds = cf_read_col(header, TBYTE,  "STATUS_FLAGS", (void **) &statflag);
+    nseconds = cf_read_col(header, TFLOAT, "LIMB_ANGLE",   (void **) &limb);
+    nseconds = cf_read_col(header, TFLOAT, "LONGITUDE",   (void **) &longitude);
+    nseconds = cf_read_col(header, TFLOAT, "LATITUDE",     (void **) &latitude);
+    nseconds = cf_read_col(header, TSHORT, "HIGH_VOLTAGE", (void **) &voltage);
+    nseconds = cf_read_col(header, TSHORT, "LIF_CNT_RATE", (void **) &rate_lif);
+    nseconds = cf_read_col(header, TSHORT, "SIC_CNT_RATE", (void **) &rate_sic);
+    nseconds = cf_read_col(header, TFLOAT, "AIC_CNT_RATE", (void **) &rate_aic);
+    background = (short *) cf_calloc(nseconds, sizeof(short)) ;
+
+    /* If INSTMODE = TTAG, don't bother to call cf_modify_hist_times. */
+    FITS_movabs_hdu(header, 1, NULL, &status);
+    FITS_read_key(header, TSTRING, "INSTMODE", instmode, NULL, &status);
+    if (!strncmp(instmode, "TTAG", 4)) modify_times = FALSE;
+
+    if (airglow_screening)
+	cf_screen_airglow(header, nevents, x, y, locflag);
+
+    if (limb_screening)
+	cf_screen_limb_angle(header, nseconds, statflag, limb);
+
+    if (saa_screening)
+	cf_screen_saa(header, nseconds, statflag, longitude, latitude);
+
+    if (voltage_screening)
+	cf_screen_high_voltage(header, nseconds, statflag, voltage);
+
+    if (burst_screening) {
+	cf_screen_burst(header, nevents, time, x, y, locflag, &gti,
+			nseconds, timeline, statflag, rate_aic, background);
+	free(gti.stop);
+	free(gti.start);
+    }
+
+    if (jitter_screening)
+	cf_screen_jitter(header, nseconds, timeline, statflag);
+
+    if (set_user_gtis)
+	cf_set_user_gtis(header, nseconds, timeline, statflag);
+
+    /* Write STATUS_FLAGS array to IDF before calling cf_set_photon_flags. */
+    FITS_movabs_hdu(header, 4, NULL, &status);
+    cf_write_col(header, TBYTE, "STATUS_FLAGS", (void *) statflag, nseconds);
+    FITS_movabs_hdu(header, 1, NULL, &status);
+
+    if (set_flags)
+	cf_set_photon_flags(header, nevents, time, weight, timeflag,
+		locflag, nseconds, timeline, statflag);
+
+    if (set_gtis)
+        cf_set_good_time_intervals(header, nseconds, timeline,
+                statflag, &gti);
+
+    if (modify_times)
+	set_times = !(cf_modify_hist_times(header, nevents, time, &gti));
+
+    if (bad_pixel_screening)
+	cf_screen_bad_pixels(header, nevents, x, y, locflag);
+
+    if (pha_screening)
+	cf_screen_pulse_height(header, nevents, pha, locflag);
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+    FITS_movabs_hdu(header, 2, NULL, &status);
+    if (set_times)
+	cf_write_col(header, TFLOAT, "TIME", (void *) time, nevents);
+    cf_write_col(header, TBYTE, "TIMEFLGS", (void *) timeflag, nevents);
+    cf_write_col(header, TBYTE, "LOC_FLGS", (void *) locflag, nevents);
+
+    if (set_gtis) {
+        FITS_movabs_hdu(header, 3, NULL, &status);
+        cf_write_col(header, TDOUBLE, "START", (void *) gti.start, gti.ntimes);
+        cf_write_col(header, TDOUBLE, "STOP", (void *) gti.stop, gti.ntimes);
+        free(gti.stop);
+        free(gti.start);
+    }
+
+    if (burst_screening) {
+	FITS_movabs_hdu(header, 4, NULL, &status);
+        cf_write_col(header, TSHORT, "BKGD_CNT_RATE", (void *) background,
+	nseconds);
+    }
+
+    FITS_close_file(header, &status);
+
+    free(background);
+    free(voltage);
+    free(latitude);
+    free(longitude);
+    free(limb);
+    free(statflag);
+    free(timeline);
+    free(timeflag);
+    free(pha);
+    free(y);
+    free(x);
+    free(time);
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return 0;
+}
diff --git a/src/fuv/cf_ttag_init.c b/src/fuv/cf_ttag_init.c
new file mode 100644
index 0000000..ec11f19
--- /dev/null
+++ b/src/fuv/cf_ttag_init.c
@@ -0,0 +1,594 @@
+/*****************************************************************************
+ *	        Johns Hopkins University
+ *	        Center For Astrophysical Sciences 
+ *	        FUSE
+ *****************************************************************************
+ *
+ * Synopsis:	cf_ttag_init input_file output_file 
+ *
+ * Description: Reads a raw ttag file, which is a FITS binary table
+ *              consisting of four columns:
+ *
+ *              TIME            FLOAT 
+ *              X               INT
+ *              Y               INT
+ *              PHA             BYTE
+ *
+ *              This routine will convert the raw ttag file to another binary
+ *              table with 13 columns the values for most of these columns
+ *              will be added by various modules of the pipeline:
+ *
+ *              TIME            FLOAT   time of arrival for photon
+ *              XRAW            INT     raw x position
+ *              YRAW            INT     raw y position
+ *              PHA             BYTE    pha value
+ *              WEIGHT          FLOAT   effective area and flux calibration
+ *              XFARF           FLOAT   x position in geometrically
+ *                                      corrected frame
+ *              YFARF           FLOAT   y position in geometrically
+ *                                      corrected frame
+ *              X               FLOAT   final x position (after correcting
+ *                                      for motions)
+ *              Y               FLOAT   final y position (after correcting
+ *                                      for motions)
+ *              CHANNEL         CHAR    aperture ID for the photon
+ *              TIMEFLGS        CHAR    temporal flags - various bits set 
+ *              LOC_FLGS        CHAR    location flags - various bits set 
+ *              LAMBDA          FLOAT   wavelength for each photon
+ *		ERGCM2		FLOAT	flux calibration for each photon
+ *
+ *              This routine calls cf_fuv_init to set up the calibration
+ *              entries in the header.
+ *
+ *              In addition, the routine creates a timeline containing
+ *              orbital information, count rates, and high-voltage
+ *              information which is used in later pipeline modules.
+ *
+ *		Turns out that OPUS good-time intervals may exclude SAA
+ *		passes that remain in the photon-event list.  This means
+ *		that there may be photons in the photon-event list whose
+ *		times are not listed in the timeline table.  To catch
+ *		them, we set all photon status flags to TEMPORAL_HV.
+ * 
+ *
+ * Returns:	Zero upon successful completion
+ *
+ * History:	03/30/98	gak	Begin work
+ *              03/18/99        emm     Modified header.
+ *              04/06/99        emm     Added check on nrows to be no
+ *                                        larger than nevents.
+ *              04/15/99    barrett     Deleted FF and DY columns,
+ *                                        added FITS wrapper functions,
+ *                                        tidied code.
+ *              04/22/99    emm         Program now returns int.
+ *              04/23/99    emm         Fixed two bugs causing segmentation
+ *                                      faults (pha was being written as
+ *                                      long, at definition of outdx was
+ *                                      given as 1B instead of 1E.) Added
+ *                                      check on number of arguments.
+ *              04/29/99    emm         Added check on nrows to make sure
+ *                                      it is smaller than nevents.
+ *              04/30/99    peb         Added cf_malloc functions.
+ *              06/07/99    peb         Added reporting of version number.
+ *              18/07/99 1.12    jm     Populate APER_ACT keyword
+ *              10/28/99 1.14   emm     Added DY column.
+ *              12/02/99 1.15   emm     Added corrections to some keywords
+ *                                      removed APER_ACT keyword update
+ *              12/21/00 1.16   peb     Fixed type mismatches in cfitsio
+ *                                      calls
+ *              05/16/01 1.17   rdr     added night/day flag column (dnflg)
+ *              08/20/01 1.18   wvd	Check keywords SPECBINX and SPECBINY;
+ *					if 0, set to 1
+ *              10/19/01 1.19   wvd	Move correction of SPECBINX, etc.
+ *					from cf_ttag_image.
+ *              04/03/02 1.20   wvd	Clean up keywords in photon-event list.
+ *              08/02/02 1.21   rdr     - changed the format of the binary
+ *                                        tables to improve speed
+ *                                      - added new columns to the table
+ *              09/15/02 1.22   rdr     added extension containing timeline
+ *              11/07/02 1.23   peb     Modified columns for event and
+ *                                      timeline flags.  Removed temporary
+ *                                      keywords.  Changed include files to
+ *                                      use calfusettag.h
+ *              11/13/02 1.24   rdr     Added ycentl and ycents columns to
+ *					timeline.
+ *                                      Added section to flag geocoronal photons
+ *                                      and photons in the inactive part of the 
+ *                                      detector. Moved processing of the 
+ *                                      photon list into a separate subroutine.
+ *                                      Fixed problem of program crashing when
+ *                                      needed columns are not in the hskp file
+ *              12/06/02 1.25   rdr     removed variables which were not being 
+ *					used
+ *		12/12/02 1.5	wvd	Installed program.
+ *              12/18/02 1.6    rdr     use AIRG calibration file for airglow
+ *                                      locations
+ *              12/20/02 1.7    rdr     - check for negative count rates and
+ *                                        correct
+ *                                      - convert status flags to unsigned char
+ *                                      - flag photons near start and end of
+ *                                        GTI
+ *              01/24/03 1.8    rdr     - correct situation where hskp file
+ *                                        has blank columns
+ *              02/11/03 1.9    rdr     Added ERGCM2S column to photon table
+ *              03/04/03 1.10   rdr     removed YFARFC column and deleted some
+ *                                      unused variables
+ *              03/19/03 1.12   peb     Added command-line options and
+ *                                      verbose_level parameter
+ *                                      Changed all printf calls to cf_verbose
+ *                                      calls with verbose level == 1
+ *              03/25/03 1.13   peb     Changed a cf_verbose to cf_timestamp.
+ *              04/01/03 1.15   wvd     Call cf_error_init after cf_timeline.
+ *              04/04/03 1.16   wvd     Update FILETYPE keyword. Set verbose
+ *					level of each call to cf_verbose.
+ *              04/07/03 1.17   wvd     Update FILENAME keyword.
+ *              04/07/03 1.18   wvd     Add FPADXLIF and FPADXSIC to header.
+ *              04/09/03 1.19   rdr     Correct error in determining the name
+ *                                      of the housekeeping file
+ *              04/29/03 1.21   wvd	Allow possiblity that housekeeping
+ *                                      filename is in lower-case letters.
+ *              05/06/03 1.22   rdr     Add daynight keyword, bkg_max and
+ *                                      bkg_min keywords, and changed the 
+ *                                      column ergcm2s to ergcm2
+ *              05/10/03 1.23   wvd	Modify internal copy of GTI's.
+ *					Make number of timeline entries more
+ *				 	nearly equal to EXPTIME.  Discard
+ *					photons with bad time markers.
+ *              06/03/03 1.24   wvd	Add call to cf_proc_check.
+ *					Keep trying to get GTI's right.
+ *              06/09/03 1.25   wvd	Compress data with TSCALE and TZERO.
+ *		06/11/03 1.26   wvd     Change calfusettag.h to calfuse.h
+ *              07/07/03 1.27   rdr     Correct initialization of dn_flag_last
+ *                                      when searching for time_sunrise and
+ *                                      time_sunset 
+ *		07/17/03 1.28   wvd     Move various subroutines to library.
+ *		07/23/03 1.29   wvd     Close ELEC_CAL file.
+ *					Delete goto statement.
+ *		09/15/03 1.31   wvd     Set temporal flags to TEMPORAL_HV.
+ *		10/02/03 1.32   wvd     Delete reference to LOCATION_GTI flag
+ *		10/26/03 1.33   wvd     Increase to morekeys to 38.
+ *		11/05/03 1.34   wvd     Added stdlib.h and unistd.h
+ *              03/03/04 1.35   rdr     Exit if no photons found.
+ *              04/06/04 1.37   bjg     Change formats to match arg types 
+ *                                      in printf
+ *                                      Functions return EXIT_SUCCESS
+ *                                      Remove static keyword in struct key 
+ *                                      definition
+ *                                      Add braces in TSCAL and TZERO
+ *                                      definitions
+ *                                      When no events are present in
+ *                                      the raw file, create a photon list
+ *                                      with a dummy event.
+ *		03/10/05 1.38   wvd	Move airglow screening to 
+ *					cf_screen_airglow.
+ *					Initialize XFARF and YFARF to zero.
+ *		05/20/05 1.39   wvd	Clean up i/o.
+ *		05/31/06 1.40   wvd     OPUS has been updated, so we can set
+ *					morekeys to 0.
+ *		06/12/06 1.41   wvd     Change cf_if_warning to cf_verbose.
+ *		08/21/07 1.42   wvd     Add -e flag to set HKEXISTS to YES.
+ *
+ ****************************************************************************/
+
+#include <stdlib.h>
+#include <unistd.h>
+#include "calfuse.h" 
+
+struct key {
+	char keyword[FLEN_KEYWORD];
+	float value;
+	};
+
+static int
+cf_init_null_photon_list(fitsfile *outfits) {
+       
+    int   status=0;
+
+    long i;
+
+    char  keyword[FLEN_CARD], card[FLEN_CARD];
+      
+    char extname[]="TTAG DATA";   /* Name of this extension */
+
+    char *ttype[]={"TIME", "XRAW", "YRAW", "PHA", "WEIGHT", "XFARF", 
+		   "YFARF",  "X", "Y", "CHANNEL", "TIMEFLGS",
+		   "LOC_FLGS", "LAMBDA", "ERGCM2" };
+
+    char *tform[14]={"1E","1I","1I","1B","1E","1I","1I",
+		     "1I","1I","1B","1B","1B","1E","1E"};  
+
+    char *tunit[]={"SECONDS", "PIXELS", "PIXELS", "UNITLESS", "UNITLESS",
+		   "PIXELS", "PIXELS", "PIXELS", "PIXELS", "UNITLESS",
+		   "UNITLESS", "UNITLESS", "ANGSTROMS", "ERG CM^-2"};
+
+    struct key tscal[] = {{"TSCAL6", 0.25},  {"TSCAL7", 0.1}, 
+                          {"TSCAL8", 0.25},  {"TSCAL9", 0.1}};
+    struct key tzero[] = {{"TZERO6", 8192.}, {"TZERO7", 0.}, 
+                          {"TZERO8", 8192.}, {"TZERO9", 0.}};
+
+    float   hdu2_time[1]      =  {0.0};
+    short   hdu2_xraw[1]      =  {0};
+    short   hdu2_yraw[1]      =  {0};
+    char    hdu2_pha[1]       =  {0};
+    float   hdu2_weight[1]    =  {0.0};
+    float   hdu2_xfarf[1]     =  {0.0};
+    float   hdu2_yfarf[1]     =  {0.0}; 
+    float   hdu2_x[1]         =  {0.0};
+    float   hdu2_y[1]         =  {0.0};
+    char    hdu2_channel[1]   =  {0};
+    char    hdu2_timeflgs[1]  =  {TEMPORAL_HV};
+    char    hdu2_loc_flgs[1]  =  {LOCATION_SHLD};
+    float   hdu2_lambda[1]    =  {0.0};
+    float   hdu2_ergcm2s[1]   =  {0.0};
+
+    cf_verbose(3, "Entering cf_init_null_photon_list.");
+
+    /* Append a new empty binary table to the output file */
+    FITS_create_tbl(outfits, BINARY_TBL, 1, 14, ttype, tform,
+			tunit, extname, &status);
+
+    /* Write TSCALE and TZERO entries to header */
+    for (i=0; i<4; i++) {
+	sprintf(keyword, "TUNIT%ld", i+6);
+	if (fits_read_keyword(outfits, keyword, card, NULL, &status))
+		cf_if_fits_error(status);
+	FITS_insert_key_flt(outfits, tscal[i].keyword, tscal[i].value,
+		-2, NULL, &status);
+	FITS_insert_key_flt(outfits, tzero[i].keyword, tzero[i].value,
+		-4, NULL, &status);
+    }
+
+
+
+  
+    FITS_write_col(outfits, TFLOAT,  1, 1, 1, 1, hdu2_time     , &status);
+    FITS_write_col(outfits, TSHORT,  2, 1, 1, 1, hdu2_xraw     , &status);
+    FITS_write_col(outfits, TSHORT,  3, 1, 1, 1, hdu2_yraw     , &status);
+    FITS_write_col(outfits, TBYTE ,  4, 1, 1, 1, hdu2_pha      , &status);
+    FITS_write_col(outfits, TFLOAT,  5, 1, 1, 1, hdu2_weight   , &status);
+    FITS_write_col(outfits, TFLOAT,  6, 1, 1, 1, hdu2_xfarf    , &status);
+    FITS_write_col(outfits, TFLOAT,  7, 1, 1, 1, hdu2_yfarf    , &status);
+    FITS_write_col(outfits, TFLOAT,  8, 1, 1, 1, hdu2_x        , &status);
+    FITS_write_col(outfits, TFLOAT,  9, 1, 1, 1, hdu2_y        , &status);
+    FITS_write_col(outfits, TBYTE , 10, 1, 1, 1, hdu2_channel  , &status);
+    FITS_write_col(outfits, TBYTE , 11, 1, 1, 1, hdu2_timeflgs , &status);
+    FITS_write_col(outfits, TBYTE , 12, 1, 1, 1, hdu2_loc_flgs , &status);
+    FITS_write_col(outfits, TFLOAT, 13, 1, 1, 1, hdu2_lambda   , &status);
+    FITS_write_col(outfits, TFLOAT, 14, 1, 1, 1, hdu2_ergcm2s  , &status);
+
+    cf_verbose(3, "Exiting cf_init_null_photon_list.");
+    return EXIT_SUCCESS;
+}
+
+/*****************************************************************************/
+
+static int
+cf_init_photon_list(fitsfile *infits, fitsfile *outfits) {
+
+/*****************************************************************************
+ *
+ * Description: procedure to take input data from the raw data file and 
+ *              generate a table with 14 columns. These columns
+ *              will be modified by later pipeline modules.
+ *
+ * ARGUMENTS:
+ *              infits        fitsfile  name of the input raw data file
+ *              outfits       fitsfile  name of the output intermediate data
+ *                                      file
+ * INPUT DATA: 
+ *              TIME            FLOAT   time of arrival for each photon
+ *              XRAW            INT     x position of photon
+ *              YRAW            INT     y position of photon
+ *              PHA             BYTE    pha value of the photon
+ *
+ * OUTPUT DATA: 
+ *              TIME            FLOAT   time of arrival for photon
+ *              XRAW            INT     raw x position
+ *              YRAW            INT     raw y position
+ *              PHA             BYTE    pha value
+ *              WEIGHT          FLOAT   effective area and flux calibration
+ *              XFARF           FLOAT   x position in geometrically
+ *                                      corrected frame
+ *              YFARF           FLOAT   y position in geometrically
+ *                                      corrected frame
+ *              X               FLOAT   final x position (after correcting
+ *                                      for motions)
+ *              Y               FLOAT   final y position (after correcting
+ *                                      for motions)
+ *              CHANNEL         CHAR    aperture ID for the photon
+ *              TIMEFLGS        CHAR    temporal flags - various bits set 
+ *              LOC_FLGS        CHAR    location flags - various bits set 
+ *              LAMBDA          FLOAT   wavelength for each photon
+ *		ERGCM2		FLOAT	flux cal for each photon
+ *
+ ****************************************************************************/
+
+    fitsfile *elecfits; 
+    char  fmt_byte[FLEN_CARD], fmt_float[FLEN_CARD], fmt_short[FLEN_CARD];
+    char  *inpha;
+    char  elecfile[FLEN_FILENAME];
+    char  keyword[FLEN_CARD], card[FLEN_CARD];
+    unsigned char *channel, *location, *temporal;
+    short *inx, *iny ;
+    int   status=0, intnull=0, anynull, hdutype;
+    int	  tcol, xcol, ycol, phacol, colval;
+    int   tfields = 14;      /*  output table will have 14 columns */
+    int   active_l, active_r;
+    long  i;
+    long  frow=1, felem=1, nevents, nrows=1; /* output table will have 1 row */
+    float *intime, *dumarrf;
+
+    char extname[]="TTAG DATA";   /* Name of this extension */
+
+    char *ttype[]={"TIME", "XRAW", "YRAW", "PHA", "WEIGHT", "XFARF", 
+		   "YFARF",  "X", "Y", "CHANNEL", "TIMEFLGS",
+		   "LOC_FLGS", "LAMBDA", "ERGCM2" };
+
+    char *tform[14];  /* We'll assign values when we know 
+                         the number of elements in the data set. */
+
+
+    char *tunit[]={"SECONDS", "PIXELS", "PIXELS", "UNITLESS", "UNITLESS",
+		   "PIXELS", "PIXELS", "PIXELS", "PIXELS", "UNITLESS",
+		   "UNITLESS", "UNITLESS", "ANGSTROMS", "ERG CM^-2"};
+
+    struct key tscal[] = {{"TSCAL6", 0.25},  {"TSCAL7", 0.1}, 
+                          {"TSCAL8", 0.25},  {"TSCAL9", 0.1}};
+    struct key tzero[] = {{"TZERO6", 8192.}, {"TZERO7", 0.}, 
+                          {"TZERO8", 8192.}, {"TZERO9", 0.}};
+
+    cf_verbose(3, "Entering cf_init_photon_list.");
+
+    /*  Move to the extension of the input file containing the data. */
+    FITS_movabs_hdu(infits, 2, &hdutype, &status);
+
+    /* Read the limits to the active area of the detector. */
+    FITS_read_key(outfits, TSTRING, "ELEC_CAL", elecfile, NULL, &status);
+    FITS_open_file(&elecfits, cf_cal_file(elecfile), READONLY, &status);
+    FITS_read_key(elecfits, TINT, "ACTIVE_L", &active_l, NULL, &status);
+    FITS_read_key(elecfits, TINT, "ACTIVE_R", &active_r, NULL, &status);
+    FITS_close_file(elecfits, &status);
+    cf_verbose(3, "Limits to the active area: left=%d, right=%d",
+	   active_l, active_r);
+
+    /*
+     *  Get the number of events in the input file.
+     */
+    FITS_read_key(infits, TLONG, "NAXIS2", &nevents, NULL, &status);
+    cf_verbose(3, "Raw data file contains %ld entries", nevents);
+
+    /* Generate the tform array */
+    sprintf(fmt_byte,  "%ldB", nevents);
+    sprintf(fmt_float, "%ldE", nevents);
+    sprintf(fmt_short, "%ldI", nevents);
+
+    tform[0] = fmt_float;
+    tform[1] = fmt_short;
+    tform[2] = fmt_short;
+    tform[3] = fmt_byte;
+    tform[4] = fmt_float;
+    for (i=5; i<9; i++)
+	tform[i] = fmt_short;
+    for ( ; i<12; i++)
+	tform[i] = fmt_byte;
+    tform[12] = fmt_float;
+    tform[13] = fmt_float;
+
+    /* Append a new empty binary table to the output file */
+    FITS_create_tbl(outfits, BINARY_TBL, nrows, tfields, ttype, tform,
+			tunit, extname, &status);
+
+    /* Write TSCALE and TZERO entries to header */
+    for (i=0; i<4; i++) {
+	sprintf(keyword, "TUNIT%ld", i+6);
+	if (fits_read_keyword(outfits, keyword, card, NULL, &status))
+		cf_if_fits_error(status);
+	FITS_insert_key_flt(outfits, tscal[i].keyword, tscal[i].value,
+		-2, NULL, &status);
+	FITS_insert_key_flt(outfits, tzero[i].keyword, tzero[i].value,
+		-4, NULL, &status);
+    }
+
+    /*
+     *  Allocate space for the input times, coords, and pha.
+     */
+    intime = (float *) cf_malloc(sizeof(float) * nevents);
+    inx    = (short *) cf_malloc(sizeof(short) * nevents);
+    iny    = (short *) cf_malloc(sizeof(short) * nevents);
+    inpha  = (char *)  cf_malloc(sizeof(char)  * nevents);
+    /*
+     *  Allocate space for the new output columns.
+     */
+    dumarrf  = (float *) cf_malloc(sizeof(float) * nevents);
+    channel  = (unsigned char *) cf_calloc(nevents, sizeof(unsigned char));
+    location = (unsigned char *) cf_calloc(nevents, sizeof(unsigned char));
+    temporal = (unsigned char *) cf_calloc(nevents, sizeof(unsigned char));
+
+    /*
+     *  Read the data from the input file and write to the output
+     *  file in a new format
+     *
+     *  read the times
+     */
+    FITS_get_colnum(infits, TRUE, "TIME", &tcol, &status);
+    FITS_read_col(infits, TFLOAT, tcol, frow, felem, nevents, &intnull,
+		  intime, &anynull, &status);
+    FITS_write_col(outfits, TFLOAT, 1, frow, felem, nevents, intime, &status);
+
+    /* process X and Y positions  */
+    FITS_get_colnum(infits, TRUE, "X", &xcol, &status);
+    FITS_read_col(infits, TSHORT, xcol, frow, felem, nevents, &intnull,
+		  inx, &anynull, &status);
+    FITS_write_col(outfits, TSHORT, 2, frow, felem, nevents, inx, &status);
+  
+    FITS_get_colnum(infits, TRUE, "Y", &ycol, &status);
+    FITS_read_col(infits, TSHORT, ycol, frow, felem, nevents, &intnull,
+		  iny, &anynull, &status);
+    FITS_write_col(outfits, TSHORT, 3, frow, felem, nevents, iny, &status);
+
+    /* now do the PHA column */
+    FITS_get_colnum(infits, TRUE, "PHA", &phacol, &status);
+    FITS_read_col(infits, TBYTE, phacol, frow, felem, nevents, &intnull,
+		  inpha, &anynull, &status);
+    FITS_write_col(outfits, TBYTE, 4, frow, felem, nevents, inpha, &status);
+
+    /* fill weights with a dummy float - all equal to 1. */ 
+    for (i=0; i<nevents; i++)
+	dumarrf[i] = 1.;
+    FITS_write_col(outfits, TFLOAT, 5, frow, felem, nevents, dumarrf, &status);
+
+    /* fill XFARF, YFARF, X and Y arrays with 0. */
+    for (i=0; i<nevents; i++)
+	dumarrf[i] = 0.;
+    for (colval=6; colval<10; colval++) {
+        FITS_write_col(outfits, TFLOAT, colval, frow, felem, nevents,
+		       dumarrf, &status);
+    }
+
+    /* Default value of temporal array is TEMPORAL_HV */
+    for (i=0; i<nevents; i++)
+	temporal[i] = TEMPORAL_HV;
+    FITS_write_col(outfits, TBYTE, 10, frow, felem, nevents, channel, &status);
+    FITS_write_col(outfits, TBYTE, 11, frow, felem, nevents, temporal, &status);
+
+    /* Set flags in the screening array for photons outside of the active
+	region of the detector. */
+    for (i=0; i<nevents; i++) 
+	if (inx[i] < active_l || inx[i] > active_r) 
+	    location[i] = location[i] | LOCATION_SHLD;
+
+    /* Write location flags to output file. */
+    FITS_movabs_hdu(outfits, 2, &hdutype, &status);
+    FITS_write_col(outfits, TBYTE, 12, frow, felem, nevents,
+		       location, &status);
+
+    /* Fill lambda and energy arrays with 0. */
+    FITS_write_col(outfits, TFLOAT, 13, frow, felem, nevents, dumarrf,
+	   &status);
+    FITS_write_col(outfits, TFLOAT, 14, frow, felem, nevents, dumarrf,
+	   &status);
+
+    free(intime);
+    free(inx);
+    free(iny);
+    free(inpha);
+    free(dumarrf);
+    free(channel);
+    free(location);
+    free(temporal);
+
+    cf_verbose(3, "Exiting cf_init_photon_list.");
+    return EXIT_SUCCESS;
+}
+
+
+/*****************************************************************************/
+
+int main(int argc, char *argv[])
+
+/*****************************************************************************/
+{
+    char CF_PRGM_ID[] = "cf_ttag_init"; 
+    char CF_VER_NUM[] = "1.42";
+
+    fitsfile *infits, *outfits;
+    int   morekeys=0;
+    int   modify_hkexists=FALSE;
+    int	  status=0, hdutype, optc;
+    long  nphot ;
+
+    char opts[] = "ehv:";
+    char usage[] =
+	"Usage:\n"
+	"  cf_ttag_init [-he] [-v level] rawttagfile idf_file\n";
+    char option[] = 
+	"Options:\n"
+	"  -h:  this help message\n"
+	"  -e:  set header keyword HKEXISTS to YES in IDF file\n"
+	"  -v:  verbosity level (default is 1; 0 is silent)\n";
+ 
+    verbose_level = 1;
+
+    while ((optc = getopt(argc, argv, opts)) != -1) {
+	switch(optc) {
+
+	case 'h':
+	    printf("%s\n%s", usage, option);
+	    return 0;
+        case 'e':
+            modify_hkexists = TRUE;
+            break;
+	case 'v':
+	    verbose_level = atoi(optarg);
+	    break;
+	}
+    }
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    if (argc != optind+2) {
+        printf("%s", usage);
+        cf_if_error("Incorrect number of arguments");
+    }
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin execution");
+
+    FITS_open_file(&infits, argv[optind++], READONLY, &status);
+
+    /*  Exit if data are not in TTAG mode. */
+    if ( cf_proc_check(infits, CF_PRGM_ID) ) {
+	FITS_close_file(infits, &status);
+	return (-1);
+    }
+
+    /* Issue warning if there are no events in the data set. */
+    FITS_read_key(infits, TLONG, "NEVENTS", &nphot, NULL, &status); 
+    cf_verbose(3,"Number of events = %d ",nphot) ;
+    if (nphot < 1) {
+       cf_verbose(1, "No photons found in the data.") ;
+    } 
+
+
+    /*  Create output file. */
+    FITS_create_file(&outfits, argv[optind], &status);
+    /*  Copy primary image header from the input file. */
+    FITS_copy_hdu(infits, outfits, morekeys, &status);
+
+    /* Update header keywords. */
+    FITS_update_key(outfits, TSTRING, "FILENAME", argv[optind], NULL, &status);
+    FITS_update_key(outfits, TSTRING, "FILETYPE",
+    		             "INTERMEDIATE DATA FILE", NULL, &status);
+    if (modify_hkexists)
+	FITS_update_key(outfits, TSTRING, "HKEXISTS", "YES", NULL, &status);
+
+    /* Populate the calibration keywords in the primary header. */
+    cf_fuv_init(outfits);
+
+    /* Write background limits to file header */
+     cf_set_background_limits(outfits); 
+
+    /* Fill in the first extension with the photon information */
+     if (nphot<1) {
+       cf_init_null_photon_list(outfits);
+     }
+     else {
+       cf_init_photon_list(infits, outfits);
+     }
+
+    /* Copy good-time intervals from input to output. */
+    cf_verbose(3, "Copying good-time intervals from input to output.");
+    FITS_movabs_hdu(infits, 3, &hdutype, &status);
+    FITS_create_hdu(outfits, &status);
+    FITS_copy_hdu(infits, outfits, 0, &status);
+
+    /*  Append a table containing the orbital timeline */
+    cf_timeline(outfits);
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+    /*  Update processing flags. */
+    cf_proc_update(outfits, CF_PRGM_ID, "COMPLETE");
+
+    FITS_close_file(infits, &status);
+    FITS_close_file(outfits, &status);
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished execution.");
+    return EXIT_SUCCESS;
+}
diff --git a/src/libcf/Makefile.Linux.orig b/src/libcf/Makefile.Linux.orig
new file mode 100644
index 0000000..43b2e31
--- /dev/null
+++ b/src/libcf/Makefile.Linux.orig
@@ -0,0 +1,152 @@
+LIBRARY=	libcf
+
+CALFUSEDIR=	${PWD}/../..
+SHARED=		-shared
+FITSVER=	2.470
+
+# Symbols for include directories
+FUSEINCLDIR=	-I${CALFUSEDIR}/include
+
+# Symbols used for compiling
+CC=		cc
+OPT=		-g -Wall -DCFORTRAN -Dg77Fortran -Df2cFortran
+CFLAGS=		${OPT} ${FUSEINCLDIR}
+
+FUSELIBDIR=	-L${CALFUSEDIR}/lib
+FUSELIBS=	-lcfitsio-${FITSVER} -lsla
+LIBS=		-lc -lm -lnsl -ldl -lgfortran
+LDFLAGS=	
+
+# Symbols used for creating shared libraries
+
+SO=		.so
+
+OBJS=		calfits.o sgp4.o eclipse.o saa.o \
+		state_limb.o state_geod.o space_vel.o helio_vel.o \
+		geod_mag.o pole_ang.o solar_ang.o lsrd_vel.o lsrk_vel.o \
+		month_day.o read_tle.o cf_velang.o \
+		set_orbit_parms.o cf_error_msg.o \
+		cf_cal_file.o cf_proc_check.o cf_proc_update.o \
+		cf_timestamp.o cf_fuv_init.o cf_header_io.o \
+		cf_check_digitizer.o cf_nint.o \
+		cf_idf_io.o cf_ids_dead_time.o cf_electronics_dead_time.o \
+		cf_fifo_dead_time.o cf_apply_dead_time.o \
+		cf_thermal_distort.o cf_count_rate_y_distort.o cf_time_xy_distort.o \
+		cf_geometric_distort.o cf_pha_x_distort.o \
+		cf_active_region.o cf_find_spectra.o cf_identify_channel.o \
+		cf_calculate_ycent_motion.o cf_source_aper.o\
+		cf_grating_motion.o cf_fpa_position.o cf_read_fpa_pos.o \
+		cf_make_mask.o cf_mirror_motion.o \
+		cf_satellite_jitter.o cf_calculate_y_centroid.o \
+		cf_target_count_rate.o \
+		cf_screen_jitter.o cf_screen_limb_angle.o cf_screen_saa.o \
+		cf_screen_high_voltage.o cf_screen_burst.o cf_screen_airglow.o \
+		cf_screen_bad_pixels.o cf_set_user_gtis.o \
+		cf_set_photon_flags.o cf_set_good_time_intervals.o \
+		cf_modify_hist_times.o cf_screen_pulse_height.o \
+		cf_convert_to_ergs.o cf_extraction_limits.o \
+		cf_astigmatism.o cf_dispersion.o cf_doppler_and_heliocentric.o \
+		cf_apply_filters.o cf_scale_bkgd.o \
+		cf_make_wave_array.o cf_rebin_background.o \
+		cf_rebin_probability_array.o cf_optimal_extraction.o \
+		cf_write_extracted_spectrum.o cf_standard_or_optimal_extraction.o \
+		cf_init_support.o cf_modify_hist_pha.o \
+		cf_fes_proc_check.o cf_fes_proc_update.o
+
+all:		${OBJS}
+		${CC} ${SHARED} -o ${LIBRARY}${SO} ${OBJS} \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+install:	all
+		chmod g+w ${OBJS} ${LIBRARY}${SO}
+		/bin/cp -p ${LIBRARY}${SO} ${CALFUSEDIR}/lib/${LIBRARY}${SO}
+
+clean: 
+	-	/bin/rm -f *.o ${LIBRARY}${SO} ${LIBRARY}${O}
+
+distclean: 
+	-	/bin/rm -f *.o ${LIBRARY}${SO} ${LIBRARY}${O}
+		cd ../../lib; /bin/rm -f ${LIBRARY}${SO}
+
+calfits.o: calfits.c
+sgp4.o: sgp4.c
+eclipse.o: eclipse.c
+set_orbit_parms.o: set_orbit_parms.c
+saa.o: saa.c
+state_limb.o: state_limb.c
+state_geod.o: state_geod.c
+space_vel.o: space_vel.c
+helio_vel.o: helio_vel.c
+geod_mag.o: geod_mag.c
+pole_ang.o: pole_ang.c
+solar_ang.o: solar_ang.c
+lsrd_vel.o: lsrd_vel.c
+lsrk_vel.o: lsrk_vel.c
+month_day.o: month_day.c
+read_tle.o: read_tle.c
+
+cf_error_msg.o: cf_error_msg.c
+cf_cal_file.o: cf_cal_file.c
+cf_fes_proc_check.o: cf_fes_proc_check.c
+cf_fes_proc_update.o: cf_fes_proc_update.c
+cf_proc_check.o: cf_proc_check.c
+cf_proc_update.o: cf_proc_update.c
+cf_fuv_init.o: cf_fuv_init.c
+cf_velang.o: cf_velang.c
+cf_timestamp.o: cf_timestamp.c
+
+cf_header_io.o: cf_header_io.c
+cf_check_digitizer.o: cf_check_digitizer.c
+cf_nint.o: cf_nint.c
+cf_idf_io.o: cf_idf_io.c
+cf_ids_dead_time.o: cf_ids_dead_time.c
+cf_electronics_dead_time.o: cf_electronics_dead_time.c
+cf_fifo_dead_time.o: cf_fifo_dead_time.c
+cf_apply_dead_time.o: cf_apply_dead_time.c
+cf_thermal_distort.o: cf_thermal_distort.c
+cf_count_rate_y_distort.o: cf_count_rate_y_distort.c
+cf_time_xy_distort.o : cf_time_xy_distort.c
+cf_geometric_distort: cf_geometric_distort.c
+cf_pha_x_distort.o: cf_pha_x_distort.c
+cf_active_region.o: cf_active_region.c
+cf_find_spectra.o: cf_find_spectra.c
+cf_identify_channel.o: cf_identify_channel.c
+cf_init_support.o: cf_init_support.c
+cf_target_count_rate.o: cf_target_count_rate.c
+cf_calculate_ycent_motion.o: cf_calculate_ycent_motion.c
+cf_source_aper.o: cf_source_aper.c
+cf_grating_motion.o: cf_grating_motion.c
+cf_fpa_position.o: cf_fpa_position.c
+cf_read_fpa_pos.o: cf_read_fpa_pos.c
+cf_make_mask.o: cf_make_mask.c
+cf_mirror_motion.o: cf_mirror_motion.c
+cf_satellite_jitter.o: cf_satellite_jitter.c
+cf_calculate_y_centroid.o: cf_calculate_y_centroid.c
+cf_screen_airglow.o: cf_screen_airglow.c
+cf_screen_bad_pixels.o: cf_screen_bad_pixels.c
+cf_screen_jitter.o: cf_screen_jitter.c
+cf_screen_limb_angle.o: cf_screen_limb_angle.c
+cf_screen_saa.o: cf_screen_saa.c
+cf_screen_high_voltage.o: cf_screen_high_voltage.c
+cf_screen_burst.o: cf_screen_burst.c
+cf_set_user_gtis.o: cf_set_user_gtis.c 
+cf_set_photon_flags.o: cf_set_photon_flags.c
+cf_set_good_time_intervals.o: cf_set_good_time_intervals.c
+cf_modify_hist_pha.o: cf_modify_hist_pha.c
+cf_modify_hist_times.o: cf_modify_hist_times.c
+cf_screen_pulse_height.o: cf_screen_pulse_height.c
+cf_convert_to_ergs.o: cf_convert_to_ergs.c
+cf_extraction_limits.o: cf_extraction_limits.c
+cf_astigmatism.o: cf_astigmatism.c
+cf_dispersion.o: cf_dispersion.c
+cf_doppler_and_heliocentric.o: cf_doppler_and_heliocentric.c
+cf_apply_filters.o: cf_apply_filters.c
+cf_scale_bkgd.o: cf_scale_bkgd.c
+cf_make_mask.o: cf_make_mask.c
+cf_make_wave_array.o: cf_make_wave_array.c
+cf_rebin_background.o: cf_rebin_background.c
+cf_rebin_probability_array.o: cf_rebin_probability_array.c
+cf_standard_or_optimal_extraction.o: cf_standard_or_optimal_extraction.c
+cf_optimal_extraction.o: cf_optimal_extraction.c
+cf_write_extracted_spectrum.o: cf_write_extracted_spectrum.c
+
diff --git a/src/libcf/Makefile.Linux64.orig b/src/libcf/Makefile.Linux64.orig
new file mode 100644
index 0000000..3b00b44
--- /dev/null
+++ b/src/libcf/Makefile.Linux64.orig
@@ -0,0 +1,151 @@
+LIBRARY=	libcf
+
+CALFUSEDIR=	${PWD}/../..
+SHARED=		-shared -fPIC
+
+# Symbols for include directories
+FUSEINCLDIR=	-I${CALFUSEDIR}/include
+
+# Symbols used for compiling
+CC=		cc
+OPT=		-g -Wall -DCFORTRAN -Dg77Fortran -Df2cFortran
+CFLAGS=		${OPT} ${FUSEINCLDIR}
+
+FUSELIBDIR=	-L${CALFUSEDIR}/lib
+FUSELIBS=	-lsla
+LIBS=		-lc -lm -lnsl -ldl -lgfortran -lcfitsio
+LDFLAGS=	
+
+# Symbols used for creating shared libraries
+
+SO=		.so
+
+OBJS=		calfits.o sgp4.o eclipse.o saa.o \
+		state_limb.o state_geod.o space_vel.o helio_vel.o \
+		geod_mag.o pole_ang.o solar_ang.o lsrd_vel.o lsrk_vel.o \
+		month_day.o read_tle.o cf_velang.o \
+		set_orbit_parms.o cf_error_msg.o \
+		cf_cal_file.o cf_proc_check.o cf_proc_update.o \
+		cf_timestamp.o cf_fuv_init.o cf_header_io.o \
+		cf_check_digitizer.o cf_nint.o \
+		cf_idf_io.o cf_ids_dead_time.o cf_electronics_dead_time.o \
+		cf_fifo_dead_time.o cf_apply_dead_time.o \
+		cf_thermal_distort.o cf_count_rate_y_distort.o cf_time_xy_distort.o \
+		cf_geometric_distort.o cf_pha_x_distort.o \
+		cf_active_region.o cf_find_spectra.o cf_identify_channel.o \
+		cf_calculate_ycent_motion.o cf_source_aper.o\
+		cf_grating_motion.o cf_fpa_position.o cf_read_fpa_pos.o \
+		cf_make_mask.o cf_mirror_motion.o \
+		cf_satellite_jitter.o cf_calculate_y_centroid.o \
+		cf_target_count_rate.o \
+		cf_screen_jitter.o cf_screen_limb_angle.o cf_screen_saa.o \
+		cf_screen_high_voltage.o cf_screen_burst.o cf_screen_airglow.o \
+		cf_screen_bad_pixels.o cf_set_user_gtis.o \
+		cf_set_photon_flags.o cf_set_good_time_intervals.o \
+		cf_modify_hist_times.o cf_screen_pulse_height.o \
+		cf_convert_to_ergs.o cf_extraction_limits.o \
+		cf_astigmatism.o cf_dispersion.o cf_doppler_and_heliocentric.o \
+		cf_apply_filters.o cf_scale_bkgd.o \
+		cf_make_wave_array.o cf_rebin_background.o \
+		cf_rebin_probability_array.o cf_optimal_extraction.o \
+		cf_write_extracted_spectrum.o cf_standard_or_optimal_extraction.o \
+		cf_init_support.o cf_modify_hist_pha.o \
+		cf_fes_proc_check.o cf_fes_proc_update.o
+
+all:		${OBJS}
+		${CC} ${SHARED} -o ${LIBRARY}${SO} ${OBJS} \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+install:	all
+		chmod g+w ${OBJS} ${LIBRARY}${SO}
+		/bin/cp -p ${LIBRARY}${SO} ${CALFUSEDIR}/lib/${LIBRARY}${SO}
+
+clean: 
+	-	/bin/rm -f *.o ${LIBRARY}${SO} ${LIBRARY}${O}
+
+distclean: 
+	-	/bin/rm -f *.o ${LIBRARY}${SO} ${LIBRARY}${O}
+		cd ../../lib; /bin/rm -f ${LIBRARY}${SO}
+
+calfits.o: calfits.c
+sgp4.o: sgp4.c
+eclipse.o: eclipse.c
+set_orbit_parms.o: set_orbit_parms.c
+saa.o: saa.c
+state_limb.o: state_limb.c
+state_geod.o: state_geod.c
+space_vel.o: space_vel.c
+helio_vel.o: helio_vel.c
+geod_mag.o: geod_mag.c
+pole_ang.o: pole_ang.c
+solar_ang.o: solar_ang.c
+lsrd_vel.o: lsrd_vel.c
+lsrk_vel.o: lsrk_vel.c
+month_day.o: month_day.c
+read_tle.o: read_tle.c
+
+cf_error_msg.o: cf_error_msg.c
+cf_cal_file.o: cf_cal_file.c
+cf_fes_proc_check.o: cf_fes_proc_check.c
+cf_fes_proc_update.o: cf_fes_proc_update.c
+cf_proc_check.o: cf_proc_check.c
+cf_proc_update.o: cf_proc_update.c
+cf_fuv_init.o: cf_fuv_init.c
+cf_velang.o: cf_velang.c
+cf_timestamp.o: cf_timestamp.c
+
+cf_header_io.o: cf_header_io.c
+cf_check_digitizer.o: cf_check_digitizer.c
+cf_nint.o: cf_nint.c
+cf_idf_io.o: cf_idf_io.c
+cf_ids_dead_time.o: cf_ids_dead_time.c
+cf_electronics_dead_time.o: cf_electronics_dead_time.c
+cf_fifo_dead_time.o: cf_fifo_dead_time.c
+cf_apply_dead_time.o: cf_apply_dead_time.c
+cf_thermal_distort.o: cf_thermal_distort.c
+cf_count_rate_y_distort.o: cf_count_rate_y_distort.c
+cf_time_xy_distort.o : cf_time_xy_distort.c
+cf_geometric_distort: cf_geometric_distort.c
+cf_pha_x_distort.o: cf_pha_x_distort.c
+cf_active_region.o: cf_active_region.c
+cf_find_spectra.o: cf_find_spectra.c
+cf_identify_channel.o: cf_identify_channel.c
+cf_init_support.o: cf_init_support.c
+cf_target_count_rate.o: cf_target_count_rate.c
+cf_calculate_ycent_motion.o: cf_calculate_ycent_motion.c
+cf_source_aper.o: cf_source_aper.c
+cf_grating_motion.o: cf_grating_motion.c
+cf_fpa_position.o: cf_fpa_position.c
+cf_read_fpa_pos.o: cf_read_fpa_pos.c
+cf_make_mask.o: cf_make_mask.c
+cf_mirror_motion.o: cf_mirror_motion.c
+cf_satellite_jitter.o: cf_satellite_jitter.c
+cf_calculate_y_centroid.o: cf_calculate_y_centroid.c
+cf_screen_airglow.o: cf_screen_airglow.c
+cf_screen_bad_pixels.o: cf_screen_bad_pixels.c
+cf_screen_jitter.o: cf_screen_jitter.c
+cf_screen_limb_angle.o: cf_screen_limb_angle.c
+cf_screen_saa.o: cf_screen_saa.c
+cf_screen_high_voltage.o: cf_screen_high_voltage.c
+cf_screen_burst.o: cf_screen_burst.c
+cf_set_user_gtis.o: cf_set_user_gtis.c 
+cf_set_photon_flags.o: cf_set_photon_flags.c
+cf_set_good_time_intervals.o: cf_set_good_time_intervals.c
+cf_modify_hist_pha.o: cf_modify_hist_pha.c
+cf_modify_hist_times.o: cf_modify_hist_times.c
+cf_screen_pulse_height.o: cf_screen_pulse_height.c
+cf_convert_to_ergs.o: cf_convert_to_ergs.c
+cf_extraction_limits.o: cf_extraction_limits.c
+cf_astigmatism.o: cf_astigmatism.c
+cf_dispersion.o: cf_dispersion.c
+cf_doppler_and_heliocentric.o: cf_doppler_and_heliocentric.c
+cf_apply_filters.o: cf_apply_filters.c
+cf_scale_bkgd.o: cf_scale_bkgd.c
+cf_make_mask.o: cf_make_mask.c
+cf_make_wave_array.o: cf_make_wave_array.c
+cf_rebin_background.o: cf_rebin_background.c
+cf_rebin_probability_array.o: cf_rebin_probability_array.c
+cf_standard_or_optimal_extraction.o: cf_standard_or_optimal_extraction.c
+cf_optimal_extraction.o: cf_optimal_extraction.c
+cf_write_extracted_spectrum.o: cf_write_extracted_spectrum.c
+
diff --git a/src/libcf/Makefile.MacOSX.orig b/src/libcf/Makefile.MacOSX.orig
new file mode 100644
index 0000000..eade1ea
--- /dev/null
+++ b/src/libcf/Makefile.MacOSX.orig
@@ -0,0 +1,152 @@
+LIBRARY=	libcf
+
+CALFUSEDIR=	${PWD}/../..
+SHARED=		-dynamiclib
+FITSVER=	2.470
+
+# Symbols for include directories
+FUSEINCLDIR=	-I${CALFUSEDIR}/include
+
+# Symbols used for compiling
+CC=		cc
+OPT=		-O3 -Wall -DCFORTRAN -Dg77Fortran -Df2cFortran
+CFLAGS=		${OPT} ${FUSEINCLDIR}
+
+FUSELIBDIR=	-L${CALFUSEDIR}/lib
+# FUSELIBS=	-lcfitsio-${FITSVER} -lsla
+FUSELIBS=	-lcfitsio -lsla
+LIBS=		-lc -lm -ldl -L/sw/lib/ -lgfortran
+
+# Symbols used for creating shared libraries
+
+SO=		.dylib
+
+OBJS=		calfits.o sgp4.o eclipse.o saa.o \
+		state_limb.o state_geod.o space_vel.o helio_vel.o \
+		geod_mag.o pole_ang.o solar_ang.o lsrd_vel.o lsrk_vel.o \
+		month_day.o read_tle.o cf_velang.o \
+		set_orbit_parms.o cf_error_msg.o \
+		cf_cal_file.o cf_proc_check.o cf_proc_update.o \
+		cf_timestamp.o cf_fuv_init.o cf_header_io.o \
+		cf_check_digitizer.o cf_nint.o \
+		cf_idf_io.o cf_ids_dead_time.o cf_electronics_dead_time.o \
+		cf_fifo_dead_time.o cf_apply_dead_time.o \
+		cf_thermal_distort.o cf_count_rate_y_distort.o cf_time_xy_distort.o \
+		cf_geometric_distort.o cf_pha_x_distort.o \
+		cf_active_region.o cf_find_spectra.o cf_identify_channel.o \
+		cf_calculate_ycent_motion.o cf_source_aper.o\
+		cf_grating_motion.o cf_fpa_position.o cf_read_fpa_pos.o \
+		cf_make_mask.o cf_mirror_motion.o \
+		cf_satellite_jitter.o cf_calculate_y_centroid.o \
+		cf_target_count_rate.o \
+		cf_screen_jitter.o cf_screen_limb_angle.o cf_screen_saa.o \
+		cf_screen_high_voltage.o cf_screen_burst.o cf_screen_airglow.o \
+		cf_screen_bad_pixels.o cf_set_user_gtis.o \
+		cf_set_photon_flags.o cf_set_good_time_intervals.o \
+		cf_modify_hist_times.o cf_screen_pulse_height.o \
+		cf_convert_to_ergs.o cf_extraction_limits.o \
+		cf_astigmatism.o cf_dispersion.o cf_doppler_and_heliocentric.o \
+		cf_apply_filters.o cf_scale_bkgd.o \
+		cf_make_wave_array.o cf_rebin_background.o \
+		cf_rebin_probability_array.o cf_optimal_extraction.o \
+		cf_write_extracted_spectrum.o cf_standard_or_optimal_extraction.o \
+		cf_init_support.o cf_modify_hist_pha.o \
+		cf_fes_proc_check.o cf_fes_proc_update.o
+
+all:		${OBJS}
+		${CC} ${SHARED} -o ${LIBRARY}${SO} ${OBJS} \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS}
+
+install:	all
+		chmod g+w ${OBJS} ${LIBRARY}${SO}
+		/bin/cp -p ${LIBRARY}${SO} ${CALFUSEDIR}/lib/${LIBRARY}${SO}
+
+clean: 
+	-	/bin/rm -f *.o ${LIBRARY}${SO} ${LIBRARY}${O}
+
+distclean: 
+	-	/bin/rm -f *.o ${LIBRARY}${SO} ${LIBRARY}${O}
+		cd ../../lib; /bin/rm -f ${LIBRARY}${SO}
+
+calfits.o: calfits.c
+sgp4.o: sgp4.c
+eclipse.o: eclipse.c
+set_orbit_parms.o: set_orbit_parms.c
+saa.o: saa.c
+state_limb.o: state_limb.c
+state_geod.o: state_geod.c
+space_vel.o: space_vel.c
+helio_vel.o: helio_vel.c
+geod_mag.o: geod_mag.c
+pole_ang.o: pole_ang.c
+solar_ang.o: solar_ang.c
+lsrd_vel.o: lsrd_vel.c
+lsrk_vel.o: lsrk_vel.c
+month_day.o: month_day.c
+read_tle.o: read_tle.c
+
+cf_error_msg.o: cf_error_msg.c
+cf_cal_file.o: cf_cal_file.c
+cf_fes_proc_check.o: cf_fes_proc_check.c
+cf_fes_proc_update.o: cf_fes_proc_update.c
+cf_proc_check.o: cf_proc_check.c
+cf_proc_update.o: cf_proc_update.c
+cf_fuv_init.o: cf_fuv_init.c
+cf_velang.o: cf_velang.c
+cf_timestamp.o: cf_timestamp.c
+
+cf_header_io.o: cf_header_io.c
+cf_check_digitizer.o: cf_check_digitizer.c
+cf_nint.o: cf_nint.c
+cf_idf_io.o: cf_idf_io.c
+cf_ids_dead_time.o: cf_ids_dead_time.c
+cf_electronics_dead_time.o: cf_electronics_dead_time.c
+cf_apply_dead_time.o: cf_apply_dead_time.c
+cf_fifo_dead_time.o: cf_fifo_dead_time.c
+cf_thermal_distort.o: cf_thermal_distort.c
+cf_count_rate_y_distort.o: cf_count_rate_y_distort.c
+cf_time_xy_distort.o : cf_time_xy_distort.c
+cf_geometric_distort: cf_geometric_distort.c
+cf_pha_x_distort.o: cf_pha_x_distort.c
+cf_active_region.o: cf_active_region.c
+cf_find_spectra.o: cf_find_spectra.c
+cf_identify_channel.o: cf_identify_channel.c
+cf_init_support.o: cf_init_support.c
+cf_target_count_rate.o: cf_target_count_rate.c
+cf_calculate_ycent_motion.o: cf_calculate_ycent_motion.c
+cf_source_aper.o: cf_source_aper.c
+cf_grating_motion.o: cf_grating_motion.c
+cf_fpa_position.o: cf_fpa_position.c
+cf_read_fpa_pos.o: cf_read_fpa_pos.c
+cf_make_mask.o: cf_make_mask.c
+cf_mirror_motion.o: cf_mirror_motion.c
+cf_satellite_jitter.o: cf_satellite_jitter.c
+cf_calculate_y_centroid.o: cf_calculate_y_centroid.c
+cf_screen_airglow.o: cf_screen_airglow.c
+cf_screen_bad_pixels.o: cf_screen_bad_pixels.c
+cf_screen_jitter.o: cf_screen_jitter.c
+cf_screen_limb_angle.o: cf_screen_limb_angle.c
+cf_screen_saa.o: cf_screen_saa.c
+cf_screen_high_voltage.o: cf_screen_high_voltage.c
+cf_screen_burst.o: cf_screen_burst.c
+cf_set_user_gtis.o: cf_set_user_gtis.c 
+cf_set_photon_flags.o: cf_set_photon_flags.c
+cf_set_good_time_intervals.o: cf_set_good_time_intervals.c
+cf_modify_hist_pha.o: cf_modify_hist_pha.c
+cf_modify_hist_times.o: cf_modify_hist_times.c
+cf_screen_pulse_height.o: cf_screen_pulse_height.c
+cf_convert_to_ergs.o: cf_convert_to_ergs.c
+cf_extraction_limits.o: cf_extraction_limits.c
+cf_astigmatism.o: cf_astigmatism.c
+cf_dispersion.o: cf_dispersion.c
+cf_doppler_and_heliocentric.o: cf_doppler_and_heliocentric.c
+cf_apply_filters.o: cf_apply_filters.c
+cf_scale_bkgd.o: cf_scale_bkgd.c
+cf_make_mask.o: cf_make_mask.c
+cf_make_wave_array.o: cf_make_wave_array.c
+cf_rebin_background.o: cf_rebin_background.c
+cf_rebin_probability_array.o: cf_rebin_probability_array.c
+cf_standard_or_optimal_extraction.o: cf_standard_or_optimal_extraction.c
+cf_optimal_extraction.o: cf_optimal_extraction.c
+cf_write_extracted_spectrum.o: cf_write_extracted_spectrum.c
+
diff --git a/src/libcf/Makefile.Solaris.orig b/src/libcf/Makefile.Solaris.orig
new file mode 100644
index 0000000..f817dfe
--- /dev/null
+++ b/src/libcf/Makefile.Solaris.orig
@@ -0,0 +1,152 @@
+LIBRARY=	libcf
+
+CALFUSEDIR=	${PWD}/../..
+SHARED=		-G
+FITSVER=	2.470
+
+# Symbols for include directories
+FUSEINCLDIR=	-I${CALFUSEDIR}/include
+
+# Symbols used for compiling
+CC=		cc
+# OPT=		-p -v -xO2 -xdepend -xchip=ultra -xarch=generic
+OPT=		-O -DCFORTRAN -KPIC
+CFLAGS=		${OPT} ${FUSEINCLDIR}
+
+FUSELIBDIR=	-L${CALFUSEDIR}/lib
+FUSELIBS=	-lcfitsio-${FITSVER} -lsla
+LIBS=		-lc -lm -lnsl -ldl -lsocket
+LDFLAGS=	
+
+# Symbols used for creating shared libraries
+
+SO=		.so
+
+OBJS=		calfits.o sgp4.o eclipse.o saa.o \
+		state_limb.o state_geod.o space_vel.o helio_vel.o \
+		geod_mag.o pole_ang.o solar_ang.o lsrd_vel.o lsrk_vel.o \
+		month_day.o read_tle.o cf_velang.o \
+		set_orbit_parms.o cf_error_msg.o \
+		cf_cal_file.o cf_proc_check.o cf_proc_update.o \
+		cf_timestamp.o cf_fuv_init.o cf_header_io.o \
+		cf_check_digitizer.o cf_nint.o \
+		cf_idf_io.o cf_ids_dead_time.o cf_electronics_dead_time.o \
+		cf_fifo_dead_time.o cf_apply_dead_time.o \
+		cf_thermal_distort.o cf_count_rate_y_distort.o cf_time_xy_distort.o \
+		cf_geometric_distort.o cf_pha_x_distort.o \
+		cf_active_region.o cf_find_spectra.o cf_identify_channel.o \
+		cf_calculate_ycent_motion.o cf_source_aper.o\
+		cf_grating_motion.o cf_fpa_position.o cf_read_fpa_pos.o \
+		cf_make_mask.o cf_mirror_motion.o \
+		cf_satellite_jitter.o cf_calculate_y_centroid.o \
+		cf_target_count_rate.o \
+		cf_screen_jitter.o cf_screen_limb_angle.o cf_screen_saa.o \
+		cf_screen_high_voltage.o cf_screen_burst.o cf_screen_airglow.o \
+		cf_screen_bad_pixels.o cf_set_user_gtis.o \
+		cf_set_photon_flags.o cf_set_good_time_intervals.o \
+		cf_modify_hist_times.o cf_screen_pulse_height.o \
+		cf_convert_to_ergs.o cf_extraction_limits.o \
+		cf_astigmatism.o cf_dispersion.o cf_doppler_and_heliocentric.o \
+		cf_apply_filters.o cf_scale_bkgd.o \
+		cf_make_wave_array.o cf_rebin_background.o \
+		cf_rebin_probability_array.o cf_optimal_extraction.o \
+		cf_write_extracted_spectrum.o cf_standard_or_optimal_extraction.o \
+		cf_init_support.o cf_modify_hist_pha.o \
+		cf_fes_proc_check.o cf_fes_proc_update.o
+
+all:		${OBJS}
+		${CC} ${SHARED} -o ${LIBRARY}${SO} ${OBJS} \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+install:	all
+		chmod g+w ${OBJS} ${LIBRARY}${SO}
+		/bin/cp -p ${LIBRARY}${SO} ${CALFUSEDIR}/lib/${LIBRARY}${SO}
+
+clean: 
+	-	/bin/rm -f *.o ${LIBRARY}${SO} ${LIBRARY}${O}
+
+distclean: 
+	-	/bin/rm -f *.o ${LIBRARY}${SO} ${LIBRARY}${O}
+		cd ../../lib; /bin/rm -f ${LIBRARY}${SO}
+
+calfits.o: calfits.c
+sgp4.o: sgp4.c
+eclipse.o: eclipse.c
+set_orbit_parms.o: set_orbit_parms.c
+saa.o: saa.c
+state_limb.o: state_limb.c
+state_geod.o: state_geod.c
+space_vel.o: space_vel.c
+helio_vel.o: helio_vel.c
+geod_mag.o: geod_mag.c
+pole_ang.o: pole_ang.c
+solar_ang.o: solar_ang.c
+lsrd_vel.o: lsrd_vel.c
+lsrk_vel.o: lsrk_vel.c
+month_day.o: month_day.c
+read_tle.o: read_tle.c
+
+cf_error_msg.o: cf_error_msg.c
+cf_cal_file.o: cf_cal_file.c
+cf_fes_proc_check.o: cf_fes_proc_check.c
+cf_fes_proc_update.o: cf_fes_proc_update.c
+cf_proc_check.o: cf_proc_check.c
+cf_proc_update.o: cf_proc_update.c
+cf_fuv_init.o: cf_fuv_init.c
+cf_velang.o: cf_velang.c
+cf_timestamp.o: cf_timestamp.c
+
+cf_header_io.o: cf_header_io.c
+cf_check_digitizer.o: cf_check_digitizer.c
+cf_nint.o: cf_nint.c
+cf_idf_io.o: cf_idf_io.c
+cf_ids_dead_time.o: cf_ids_dead_time.c
+cf_electronics_dead_time.o: cf_electronics_dead_time.c
+cf_apply_dead_time.o: cf_apply_dead_time.c
+cf_fifo_dead_time.o: cf_fifo_dead_time.c
+cf_thermal_distort.o: cf_thermal_distort.c
+cf_count_rate_y_distort.o: cf_count_rate_y_distort.c
+cf_time_xy_distort.o : cf_time_xy_distort.c
+cf_geometric_distort: cf_geometric_distort.c
+cf_pha_x_distort.o: cf_pha_x_distort.c
+cf_active_region.o: cf_active_region.c
+cf_find_spectra.o: cf_find_spectra.c
+cf_identify_channel.o: cf_identify_channel.c
+cf_init_support.o: cf_init_support.c
+cf_target_count_rate.o: cf_target_count_rate.c
+cf_calculate_ycent_motion.o: cf_calculate_ycent_motion.c
+cf_source_aper.o: cf_source_aper.c
+cf_grating_motion.o: cf_grating_motion.c
+cf_fpa_position.o: cf_fpa_position.c
+cf_read_fpa_pos.o: cf_read_fpa_pos.c
+cf_make_mask.o: cf_make_mask.c
+cf_mirror_motion.o: cf_mirror_motion.c
+cf_satellite_jitter.o: cf_satellite_jitter.c
+cf_calculate_y_centroid.o: cf_calculate_y_centroid.c
+cf_screen_airglow.o: cf_screen_airglow.c
+cf_screen_bad_pixels.o: cf_screen_bad_pixels.c
+cf_screen_jitter.o: cf_screen_jitter.c
+cf_screen_limb_angle.o: cf_screen_limb_angle.c
+cf_screen_saa.o: cf_screen_saa.c
+cf_screen_high_voltage.o: cf_screen_high_voltage.c
+cf_screen_burst.o: cf_screen_burst.c
+cf_set_user_gtis.o: cf_set_user_gtis.c 
+cf_set_photon_flags.o: cf_set_photon_flags.c
+cf_set_good_time_intervals.o: cf_set_good_time_intervals.c
+cf_modify_hist_pha.o: cf_modify_hist_pha.c
+cf_modify_hist_times.o: cf_modify_hist_times.c
+cf_screen_pulse_height.o: cf_screen_pulse_height.c
+cf_convert_to_ergs.o: cf_convert_to_ergs.c
+cf_extraction_limits.o: cf_extraction_limits.c
+cf_astigmatism.o: cf_astigmatism.c
+cf_dispersion.o: cf_dispersion.c
+cf_doppler_and_heliocentric.o: cf_doppler_and_heliocentric.c
+cf_apply_filters.o: cf_apply_filters.c
+cf_scale_bkgd.o: cf_scale_bkgd.c
+cf_make_mask.o: cf_make_mask.c
+cf_make_wave_array.o: cf_make_wave_array.c
+cf_rebin_background.o: cf_rebin_background.c
+cf_rebin_probability_array.o: cf_rebin_probability_array.c
+cf_standard_or_optimal_extraction.o: cf_standard_or_optimal_extraction.c
+cf_optimal_extraction.o: cf_optimal_extraction.c
+cf_write_extracted_spectrum.o: cf_write_extracted_spectrum.c
diff --git a/src/libcf/Makefile.orig.orig b/src/libcf/Makefile.orig.orig
new file mode 100644
index 0000000..f817dfe
--- /dev/null
+++ b/src/libcf/Makefile.orig.orig
@@ -0,0 +1,152 @@
+LIBRARY=	libcf
+
+CALFUSEDIR=	${PWD}/../..
+SHARED=		-G
+FITSVER=	2.470
+
+# Symbols for include directories
+FUSEINCLDIR=	-I${CALFUSEDIR}/include
+
+# Symbols used for compiling
+CC=		cc
+# OPT=		-p -v -xO2 -xdepend -xchip=ultra -xarch=generic
+OPT=		-O -DCFORTRAN -KPIC
+CFLAGS=		${OPT} ${FUSEINCLDIR}
+
+FUSELIBDIR=	-L${CALFUSEDIR}/lib
+FUSELIBS=	-lcfitsio-${FITSVER} -lsla
+LIBS=		-lc -lm -lnsl -ldl -lsocket
+LDFLAGS=	
+
+# Symbols used for creating shared libraries
+
+SO=		.so
+
+OBJS=		calfits.o sgp4.o eclipse.o saa.o \
+		state_limb.o state_geod.o space_vel.o helio_vel.o \
+		geod_mag.o pole_ang.o solar_ang.o lsrd_vel.o lsrk_vel.o \
+		month_day.o read_tle.o cf_velang.o \
+		set_orbit_parms.o cf_error_msg.o \
+		cf_cal_file.o cf_proc_check.o cf_proc_update.o \
+		cf_timestamp.o cf_fuv_init.o cf_header_io.o \
+		cf_check_digitizer.o cf_nint.o \
+		cf_idf_io.o cf_ids_dead_time.o cf_electronics_dead_time.o \
+		cf_fifo_dead_time.o cf_apply_dead_time.o \
+		cf_thermal_distort.o cf_count_rate_y_distort.o cf_time_xy_distort.o \
+		cf_geometric_distort.o cf_pha_x_distort.o \
+		cf_active_region.o cf_find_spectra.o cf_identify_channel.o \
+		cf_calculate_ycent_motion.o cf_source_aper.o\
+		cf_grating_motion.o cf_fpa_position.o cf_read_fpa_pos.o \
+		cf_make_mask.o cf_mirror_motion.o \
+		cf_satellite_jitter.o cf_calculate_y_centroid.o \
+		cf_target_count_rate.o \
+		cf_screen_jitter.o cf_screen_limb_angle.o cf_screen_saa.o \
+		cf_screen_high_voltage.o cf_screen_burst.o cf_screen_airglow.o \
+		cf_screen_bad_pixels.o cf_set_user_gtis.o \
+		cf_set_photon_flags.o cf_set_good_time_intervals.o \
+		cf_modify_hist_times.o cf_screen_pulse_height.o \
+		cf_convert_to_ergs.o cf_extraction_limits.o \
+		cf_astigmatism.o cf_dispersion.o cf_doppler_and_heliocentric.o \
+		cf_apply_filters.o cf_scale_bkgd.o \
+		cf_make_wave_array.o cf_rebin_background.o \
+		cf_rebin_probability_array.o cf_optimal_extraction.o \
+		cf_write_extracted_spectrum.o cf_standard_or_optimal_extraction.o \
+		cf_init_support.o cf_modify_hist_pha.o \
+		cf_fes_proc_check.o cf_fes_proc_update.o
+
+all:		${OBJS}
+		${CC} ${SHARED} -o ${LIBRARY}${SO} ${OBJS} \
+		${FUSELIBDIR} ${FUSELIBS} ${LIBS} ${LDFLAGS}
+
+install:	all
+		chmod g+w ${OBJS} ${LIBRARY}${SO}
+		/bin/cp -p ${LIBRARY}${SO} ${CALFUSEDIR}/lib/${LIBRARY}${SO}
+
+clean: 
+	-	/bin/rm -f *.o ${LIBRARY}${SO} ${LIBRARY}${O}
+
+distclean: 
+	-	/bin/rm -f *.o ${LIBRARY}${SO} ${LIBRARY}${O}
+		cd ../../lib; /bin/rm -f ${LIBRARY}${SO}
+
+calfits.o: calfits.c
+sgp4.o: sgp4.c
+eclipse.o: eclipse.c
+set_orbit_parms.o: set_orbit_parms.c
+saa.o: saa.c
+state_limb.o: state_limb.c
+state_geod.o: state_geod.c
+space_vel.o: space_vel.c
+helio_vel.o: helio_vel.c
+geod_mag.o: geod_mag.c
+pole_ang.o: pole_ang.c
+solar_ang.o: solar_ang.c
+lsrd_vel.o: lsrd_vel.c
+lsrk_vel.o: lsrk_vel.c
+month_day.o: month_day.c
+read_tle.o: read_tle.c
+
+cf_error_msg.o: cf_error_msg.c
+cf_cal_file.o: cf_cal_file.c
+cf_fes_proc_check.o: cf_fes_proc_check.c
+cf_fes_proc_update.o: cf_fes_proc_update.c
+cf_proc_check.o: cf_proc_check.c
+cf_proc_update.o: cf_proc_update.c
+cf_fuv_init.o: cf_fuv_init.c
+cf_velang.o: cf_velang.c
+cf_timestamp.o: cf_timestamp.c
+
+cf_header_io.o: cf_header_io.c
+cf_check_digitizer.o: cf_check_digitizer.c
+cf_nint.o: cf_nint.c
+cf_idf_io.o: cf_idf_io.c
+cf_ids_dead_time.o: cf_ids_dead_time.c
+cf_electronics_dead_time.o: cf_electronics_dead_time.c
+cf_apply_dead_time.o: cf_apply_dead_time.c
+cf_fifo_dead_time.o: cf_fifo_dead_time.c
+cf_thermal_distort.o: cf_thermal_distort.c
+cf_count_rate_y_distort.o: cf_count_rate_y_distort.c
+cf_time_xy_distort.o : cf_time_xy_distort.c
+cf_geometric_distort: cf_geometric_distort.c
+cf_pha_x_distort.o: cf_pha_x_distort.c
+cf_active_region.o: cf_active_region.c
+cf_find_spectra.o: cf_find_spectra.c
+cf_identify_channel.o: cf_identify_channel.c
+cf_init_support.o: cf_init_support.c
+cf_target_count_rate.o: cf_target_count_rate.c
+cf_calculate_ycent_motion.o: cf_calculate_ycent_motion.c
+cf_source_aper.o: cf_source_aper.c
+cf_grating_motion.o: cf_grating_motion.c
+cf_fpa_position.o: cf_fpa_position.c
+cf_read_fpa_pos.o: cf_read_fpa_pos.c
+cf_make_mask.o: cf_make_mask.c
+cf_mirror_motion.o: cf_mirror_motion.c
+cf_satellite_jitter.o: cf_satellite_jitter.c
+cf_calculate_y_centroid.o: cf_calculate_y_centroid.c
+cf_screen_airglow.o: cf_screen_airglow.c
+cf_screen_bad_pixels.o: cf_screen_bad_pixels.c
+cf_screen_jitter.o: cf_screen_jitter.c
+cf_screen_limb_angle.o: cf_screen_limb_angle.c
+cf_screen_saa.o: cf_screen_saa.c
+cf_screen_high_voltage.o: cf_screen_high_voltage.c
+cf_screen_burst.o: cf_screen_burst.c
+cf_set_user_gtis.o: cf_set_user_gtis.c 
+cf_set_photon_flags.o: cf_set_photon_flags.c
+cf_set_good_time_intervals.o: cf_set_good_time_intervals.c
+cf_modify_hist_pha.o: cf_modify_hist_pha.c
+cf_modify_hist_times.o: cf_modify_hist_times.c
+cf_screen_pulse_height.o: cf_screen_pulse_height.c
+cf_convert_to_ergs.o: cf_convert_to_ergs.c
+cf_extraction_limits.o: cf_extraction_limits.c
+cf_astigmatism.o: cf_astigmatism.c
+cf_dispersion.o: cf_dispersion.c
+cf_doppler_and_heliocentric.o: cf_doppler_and_heliocentric.c
+cf_apply_filters.o: cf_apply_filters.c
+cf_scale_bkgd.o: cf_scale_bkgd.c
+cf_make_mask.o: cf_make_mask.c
+cf_make_wave_array.o: cf_make_wave_array.c
+cf_rebin_background.o: cf_rebin_background.c
+cf_rebin_probability_array.o: cf_rebin_probability_array.c
+cf_standard_or_optimal_extraction.o: cf_standard_or_optimal_extraction.c
+cf_optimal_extraction.o: cf_optimal_extraction.c
+cf_write_extracted_spectrum.o: cf_write_extracted_spectrum.c
diff --git a/src/libcf/calfits.c b/src/libcf/calfits.c
new file mode 100644
index 0000000..29b3a08
--- /dev/null
+++ b/src/libcf/calfits.c
@@ -0,0 +1,658 @@
+/*****************************************************************************
+ *            Johns Hopkins University
+ *            Center For Astrophysical Sciences
+ *            FUSE
+ *****************************************************************************
+ *
+ * Description: Wrappers for cfitsio routines which includes error checking.
+ *
+ * History:     04/14/99        peb   Finished work on subset of routines
+ *                                    from cfitsio v2.031.  
+ *              04/15/99        emm   Replaced #include FITSIO.h with 
+ *                                    #include calfuse.h
+ *              04/15/99    barrett   Added FITS_get_rowsize.
+ *              04/16/99    barrett   Added FITS_get_hdu_num.
+ *              04/20/99    barrett   Added FITS_insert_key_[str, log, lng,
+ *                                      fixflt, flt, fixdbl, dbl, fixcmp,
+ *                                      cmp, fixdblcmp, dblcmp]
+ *              04/23/99    emurphy   Deleted error checking from
+ *                                    cf_get_hdu_num
+ *		04/04/01    kruk      Force casesen to FALSE in FITS_get_colnum
+ *              12/18/03    bjg       Change calfusettag.h to calfuse.h
+ *
+ ****************************************************************************/
+
+#include "fitsio.h"
+#include "calfuse.h"
+
+int FITS_open_file(fitsfile **fptr, const char *filename, int iomode,
+                   int *status)
+{
+    ffopen(fptr, filename, iomode, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_reopen_file(fitsfile *openfptr, fitsfile **newfptr, int *status)
+{
+    ffreopen(openfptr, newfptr, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_create_file(fitsfile **fptr, const char *filename, int *status)
+{
+    ffinit(fptr, filename, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_flush_file(fitsfile *fptr, int *status)
+{
+    ffflus(fptr, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_close_file(fitsfile *fptr, int *status)
+{
+    ffclos(fptr, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_delete_file(fitsfile *fptr, int *status)
+{
+    ffdelt(fptr, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_file_name(fitsfile *fptr, char *filename, int *status)
+{
+    ffflnm(fptr, filename, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_file_mode(fitsfile *fptr, int *filemode, int *status)
+{
+    ffflmd(fptr, filemode, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_write_record(fitsfile *fptr, const char *card, int *status)
+{
+    ffprec(fptr, card, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_write_key(fitsfile *fptr, int datatype, char *keyname, void *value,
+                   char *comm, int *status)
+{
+    ffpky(fptr, datatype, keyname, value,
+          comm, status);
+    if (*status) fprintf(stderr, "Error writing keyword %16.16s\n",keyname);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_write_comment(fitsfile *fptr, const char *comm, int *status)
+{
+    ffpcom(fptr, comm, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_write_history(fitsfile *fptr, const char *history, int *status)
+{
+    ffphis(fptr, history, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_write_date(fitsfile *fptr, int *status)
+{
+    ffpdat(fptr, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_copy_key(fitsfile *infptr,fitsfile *outfptr,int incol,int outcol,
+                  char *rootname, int *status)
+{
+    ffcpky(infptr,outfptr,incol,outcol,
+           rootname, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_write_imghdr(fitsfile *fptr, int bitpix, int naxis, long naxes[],
+                      int *status)
+{
+    ffphps( fptr, bitpix, naxis, naxes, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_write_grphdr(fitsfile *fptr, int simple, int bitpix, int naxis,
+                      long naxes[], long pcount, long gcount, int extend,
+                      int *status)
+{
+    ffphpr( fptr, simple, bitpix, naxis, naxes,
+            pcount, gcount, extend, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_write_btblhdr(fitsfile *fptr, long naxis2, int tfields, char **ttype,
+                       char **tform, char **tunit, char *extname, long pcount,
+                       int *status)
+{
+    ffphbn(fptr, naxis2, tfields, ttype,
+          tform, tunit, extname, pcount, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_get_hdrpos(fitsfile *fptr, int *nexist, int *position, int *status)
+{
+    ffghps(fptr, nexist, position, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_read_record(fitsfile *fptr, int nrec, char *card, int *status)
+{
+    ffgrec(fptr, nrec, card, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_read_card(fitsfile *fptr, char *keyname, char *card, int *status)
+{
+    ffgcrd(fptr, keyname, card, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_read_key(fitsfile *fptr, int datatype, char *keyname, void *value,
+                  char *comm, int *status)
+{
+    ffgky( fptr, datatype, keyname, value,
+           comm, status);
+    if (*status) fprintf(stderr, "Error reading keyword %16.16s\n",keyname);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_read_imghdr(fitsfile *fptr, int maxdim, int *simple, int *bitpix,
+                     int *naxis, long naxes[], long *pcount, long *gcount,
+                     int *extend, int *status)
+{
+    ffghpr(fptr, maxdim, simple, bitpix, naxis,
+          naxes, pcount, gcount, extend, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_read_btblhdr(fitsfile *fptr, int maxfield, long *naxis2, int *tfields,
+                      char **ttype, char **tform, char **tunit, char *extname,
+                      long *pcount, int *status)
+{
+    ffghbn(fptr, maxfield, naxis2, tfields,
+           ttype, tform, tunit, extname,
+           pcount, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_update_card(fitsfile *fptr, char *keyname, char *card, int *status)
+{
+    ffucrd(fptr, keyname, card, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_update_key(fitsfile *fptr, int datatype, char *keyname, void *value,
+                    char *comm, int *status)
+{
+    ffuky(fptr, datatype, keyname, value,
+          comm, status);
+    if (*status) fprintf(stderr, "Error updating keyword %16.16s\n",keyname);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_modify_record(fitsfile *fptr, int nkey, char *card, int *status)
+{
+    ffmrec(fptr, nkey, card, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_modify_card(fitsfile *fptr, char *keyname, char *card, int *status)
+{
+    ffmcrd(fptr, keyname, card, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_modify_comment(fitsfile *fptr, char *keyname, char *comm, int *status)
+{
+    ffmcom(fptr, keyname, comm, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_insert_record(fitsfile *fptr, int nkey, char *card, int *status)
+{
+    ffirec(fptr, nkey, card, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_insert_key_str(fitsfile *fptr, char *keyname, char *value,
+			char *comment, int *status)
+{
+    ffikys(fptr, keyname, value, comment, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_insert_key_log(fitsfile *fptr, char *keyname, int value,
+			char *comment, int *status)
+{
+    ffikyl(fptr, keyname, value, comment, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_insert_key_lng(fitsfile *fptr, char *keyname, long value,
+			char *comment, int *status)
+{
+    ffikyj(fptr, keyname, value, comment, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_insert_key_flt(fitsfile *fptr, char *keyname, float value,
+			int decimals, char *comment, int *status)
+{
+    ffikye(fptr, keyname, value, decimals, comment, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_insert_key_fixflt(fitsfile *fptr, char *keyname, float value,
+			   int decimals, char *comment, int *status)
+{
+    ffikyf(fptr, keyname, value, decimals, comment, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_insert_key_dbl(fitsfile *fptr, char *keyname, double value,
+			int decimals, char *comment, int *status)
+{
+    ffikyd(fptr, keyname, value, decimals, comment, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_insert_key_fixdbl(fitsfile *fptr, char *keyname, double value,
+			   int decimals, char *comment, int *status)
+{
+    ffikyg(fptr, keyname, value, decimals, comment, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_insert_key_cmp(fitsfile *fptr, char *keyname, float *value,
+			int decimals, char *comment, int *status)
+{
+    ffikyc(fptr, keyname, value, decimals, comment, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_insert_key_dblcmp(fitsfile *fptr, char *keyname, double *value,
+			   int decimals, char *comment, int *status)
+{
+    ffikym(fptr, keyname, value, decimals, comment, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_insert_key_fixcmp(fitsfile *fptr, char *keyname, float *value,
+			   int decimals, char *comment, int *status)
+{
+    ffikfc(fptr, keyname, value, decimals, comment, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_insert_key_fixdblcmp(fitsfile *fptr, char *keyname, double *value,
+			      int decimals, char *comment, int *status)
+{
+    ffikfm(fptr, keyname, value, decimals, comment, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_insert_key_null(fitsfile *fptr, char *keyname, char *comment,
+			 int *status)
+{
+    ffikyu(fptr, keyname, comment, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_delete_key(fitsfile *fptr, char *keyname, int *status)
+{
+    ffdkey(fptr, keyname, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_delete_record(fitsfile *fptr, int keypos, int *status)
+{
+    ffdrec(fptr, keypos, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_get_hdu_num(fitsfile *fptr, int *hdunum)
+{
+    /* This routine returns the HDU number instead of status.  Therefore,
+     * it should not use any error checking. */
+    int status;
+    status = ffghdn(fptr, hdunum);
+    return status;
+}
+
+int FITS_get_hdu_type(fitsfile *fptr, int *exttype, int *status)
+{
+    ffghdt(fptr, exttype, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_movabs_hdu(fitsfile *fptr, int hdunum, int *exttype, int *status)
+{
+    ffmahd(fptr, hdunum, exttype, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_movrel_hdu(fitsfile *fptr, int hdumov, int *exttype, int *status)
+{
+    ffmrhd(fptr, hdumov, exttype, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_movnam_hdu(fitsfile *fptr, int exttype, char *hduname, int hduvers,
+                    int *status)
+{
+    ffmnhd(fptr, exttype, hduname, hduvers,
+           status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_get_num_hdus(fitsfile *fptr, int *nhdu, int *status)
+{
+    ffthdu(fptr, nhdu, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_create_img(fitsfile *fptr, int bitpix, int naxis, long *naxes,
+                    int *status)
+{
+    ffcrim(fptr, bitpix, naxis, naxes, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_create_tbl(fitsfile *fptr, int tbltype, long naxis2, int tfields,
+                    char **ttype, char **tform, char **tunit, char *extname,
+                    int *status)
+{
+    ffcrtb(fptr, tbltype, naxis2, tfields, ttype,
+           tform, tunit, extname, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_create_hdu(fitsfile *fptr, int *status)
+{
+    ffcrhd(fptr, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_insert_img(fitsfile *fptr, int bitpix, int naxis, long *naxes,
+                    int *status)
+{
+    ffiimg(fptr, bitpix, naxis, naxes, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_insert_atbl(fitsfile *fptr, long naxis1, long naxis2, int tfields,
+                     char **ttype, long *tbcol, char **tform, char **tunit,
+                     char *extname, int *status)
+{
+    ffitab(fptr, naxis1, naxis2, tfields, ttype,
+           tbcol, tform, tunit, extname, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_insert_btbl(fitsfile *fptr,long naxis2, int tfields, char **ttype,
+                     char **tform, char **tunit, char *extname, long pcount,
+                     int *status)
+{
+    ffibin(fptr,naxis2, tfields, ttype, tform,
+           tunit, extname, pcount, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_delete_hdu(fitsfile *fptr, int *hdutype, int *status)
+{
+    ffdhdu(fptr, hdutype, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_copy_hdu(fitsfile *infptr, fitsfile *outfptr, int morekeys,
+                  int *status)
+{
+    ffcopy(infptr, outfptr, morekeys, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_copy_header(fitsfile *infptr, fitsfile *outfptr, int *status)
+{
+    ffcphd(infptr, outfptr, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_copy_data(fitsfile *infptr, fitsfile *outfptr, int *status)
+{
+    ffcpdt(infptr, outfptr, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_get_colnum(fitsfile *fptr, int casesen, char *templt, int  *colnum,
+                    int *status)
+{
+    /* force casesen to FALSE, in accordance with the FITS standard */
+    casesen = FALSE;
+    ffgcno(fptr, casesen, templt, colnum,
+           status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_get_colname(fitsfile *fptr, int casesen, char *templt, char *colname,
+                     int *colnum, int *status)
+{
+    ffgcnn(fptr, casesen, templt, colname,
+           colnum, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_get_coltype(fitsfile *fptr, int colnum, int *typecode, long *repeat,
+                     long *width, int *status)
+{
+    ffgtcl(fptr, colnum, typecode, repeat,
+           width, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_get_num_rows(fitsfile *fptr, long *nrows, int *status)
+{
+    ffgnrw(fptr, nrows, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_get_rowsize(fitsfile *fptr, long *nrows, int *status)
+{
+    ffgrsz(fptr, nrows, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_get_num_cols(fitsfile *fptr, int  *ncols, int *status)
+{
+    ffgncl(fptr, ncols, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_get_acolparms(fitsfile *fptr, int colnum, char *ttype, long *tbcol,
+                       char *tunit, char *tform, double *tscal, double *tzero,
+                       char *tnull, char *tdisp, int *status)
+{
+    ffgacl(fptr, colnum, ttype, tbcol,
+           tunit, tform, tscal, tzero,
+           tnull, tdisp, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_get_bcolparms(fitsfile *fptr, int colnum, char *ttype, char *tunit,
+                       char *dtype, long *repeat, double *tscal, double *tzero,
+                       long *tnull, char *tdisp, int  *status)
+{
+    ffgbcl(fptr, colnum, ttype, tunit,
+           dtype, repeat, tscal, tzero,
+           tnull, tdisp, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_read_img(fitsfile *fptr, int  datatype, long firstelem, long nelem,
+                  void *nulval, void *array, int *anynul, int  *status)
+{
+    ffgpv(fptr,  datatype, firstelem, nelem,
+          nulval, array, anynul, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_read_col( fitsfile *fptr, int datatype, int colnum, long firstrow,
+                   long firstelem, long nelem, void *nulval, void *array,
+                   int *anynul, int  *status)
+{
+    ffgcv( fptr, datatype, colnum, firstrow,
+           firstelem, nelem, nulval, array, anynul,
+           status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_write_img(fitsfile *fptr, int datatype, long  firstelem, long  nelem,
+                   void  *array, int  *status)
+{
+    ffppr(fptr, datatype,  firstelem,  nelem,
+          array, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_write_col(fitsfile *fptr, int datatype, int colnum, long firstrow,
+                   long firstelem, long nelem, void *array, int *status)
+{
+    ffpcl(fptr, datatype, colnum, firstrow,
+          firstelem, nelem, array, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_insert_rows(fitsfile *fptr, long firstrow, long nrows, int *status)
+{
+    ffirow(fptr, firstrow, nrows, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_delete_rows(fitsfile *fptr, long firstrow, long nrows, int *status)
+{
+    ffdrow(fptr, firstrow, nrows, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_delete_rowlist(fitsfile *fptr, long *rownum,  long nrows, int *status)
+{
+    ffdrws(fptr, rownum,  nrows, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_insert_col(fitsfile *fptr, int numcol, char *ttype, char *tform,
+                    int *status)
+{
+    fficol(fptr, numcol, ttype, tform, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_insert_cols(fitsfile *fptr, int firstcol, int ncols, char **ttype,
+                     char **tform, int *status)
+{
+    fficls(fptr, firstcol, ncols, ttype,
+           tform, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_delete_col(fitsfile *fptr, int numcol, int *status)
+{
+    ffdcol(fptr, numcol, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
+int FITS_copy_col(fitsfile *infptr, fitsfile *outfptr, int incol, int outcol, 
+                  int create_col, int *status)
+{
+    ffcpcl(infptr, outfptr, incol, outcol, 
+           create_col, status);
+    cf_if_fits_error(*status);
+    return *status;
+}
+
diff --git a/src/libcf/cf_active_region.c b/src/libcf/cf_active_region.c
new file mode 100644
index 0000000..8a3fd6e
--- /dev/null
+++ b/src/libcf/cf_active_region.c
@@ -0,0 +1,90 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_active_region(fitsfile *header, long nevents, float *xfarf,
+ *			float *yfarf, unsigned char *locflags)
+ *
+ * Description: Flags events outside of detector active area.
+ *
+ *		Note: Both cf_ttag_init and cf_hist_init set LOCATION_SHLD
+ *		when initializing IDF, but they look only at XRAW and use
+ *		limits that are less restrictive than those used here.
+ *
+ * Arguments:   fitsfile  *header       Pointer to FITS file containing the
+ *                                      header of the intermediate data file
+ *              long      nevents       The number of events
+ *              float     *xfarf        An array of event X positions
+ *              float     *yfarf        An array of event Y positions
+ *              unsigned char *locflags Location flags of each event
+ *
+ * Calls:
+ *
+ * Return:      0  on success
+ *
+ * History:     11/12/02   1.1    peb   Begin and finish work
+ *		03/11/03   1.2    wvd   Changed locflags to unsigned char
+ *              05/20/03   1.3    rdr   Added call to cf_proc_check 
+ *		07/29/03   1.4    wvd   If cf_proc_check fails, return errflg.
+ *              04/07/07   1.5    wvd	Clean up compiler warnings.
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include <stdlib.h>
+#include "calfuse.h"
+
+int
+cf_active_region(fitsfile *header, long nevents, float *xfarf, float *yfarf,
+		 unsigned char *locflags)
+{
+    char CF_PRGM_ID[] = "cf_active_region";
+    char CF_VER_NUM[] = "1.5";
+
+    char  elecfile[FLEN_VALUE]={'\0'};
+    char  keyword[FLEN_KEYWORD]={'\0'}, detector[FLEN_VALUE]={'\0'};
+    int   errflg=0, status=0, active_l, active_r, active_b, active_t;
+    long  j;
+    fitsfile *elecfits=NULL;
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    if ((errflg = cf_proc_check(header, CF_PRGM_ID))) return errflg;
+
+    FITS_read_key(header, TSTRING, "DETECTOR", detector, NULL, &status);
+    /*
+     *  Read keywords from ELEC_CAL file
+     */
+    FITS_read_key(header, TSTRING, "ELEC_CAL", elecfile, NULL, &status);
+    FITS_open_file(&elecfits, cf_cal_file(elecfile), READONLY, &status);
+    sprintf(keyword, "ACTVL_%s", detector);
+    FITS_read_key(elecfits, TINT, keyword, &active_l, NULL, &status);
+    sprintf(keyword, "ACTVR_%s", detector);
+    FITS_read_key(elecfits, TINT, keyword, &active_r, NULL, &status);
+    sprintf(keyword, "ACTVB_%s", detector);
+    FITS_read_key(elecfits, TINT, keyword, &active_b, NULL, &status);
+    sprintf(keyword, "ACTVT_%s", detector);
+    FITS_read_key(elecfits, TINT, keyword, &active_t, NULL, &status);
+    FITS_close_file(elecfits, &status);
+    cf_verbose(3, "Active area limits: X from %d to %d, Y from %d to %d",
+	active_l, active_r, active_b, active_t);
+    /*
+     *  Apply active region flags to each event.
+     */
+    for(j=0; j<nevents; j++) {
+	/*
+	 *  Flag events that fall outside of detector active region.
+	 */
+	if (xfarf[j] < active_l || xfarf[j] > active_r ||
+	    yfarf[j] < active_b || yfarf[j] > active_t) {
+	    locflags[j] |= LOCATION_SHLD;
+	}
+    }
+
+    cf_proc_update(header, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return 0;
+}
diff --git a/src/libcf/cf_apply_dead_time.c b/src/libcf/cf_apply_dead_time.c
new file mode 100644
index 0000000..a714a28
--- /dev/null
+++ b/src/libcf/cf_apply_dead_time.c
@@ -0,0 +1,142 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_apply_dead_time(fitsfile *header, long nevents, float *time,
+ *                      float *weight, long nseconds, float *timeline, 
+ *			float *ids_dtc, float *elec_dtc)
+ *
+ * Description: Applies dead-time correction to all photons.  For HIST data,
+ *		uses mean of dead-time arrays.  Writes mean dead-time
+ *		values to file header.  Issue warning if DET_DEAD > 1.5.
+ *
+ * Arguments:   fitsfile  *header       Pointer to FITS file containing the
+ *                                      header of the intermediate data file
+ *              long      nevents       The number of events
+ *              float     *time         An array of event times
+ *              float     *weight       An array of event weights
+ *              long      nseconds      The number of timeline values
+ *              float     *timeline     An array of timeline times
+ *              float     *aic_rate     Active Image Counter rate
+ *              float     *ids_dtc      Output of cf_ids_dead_time
+ *              float     *elec_dtc     Output of cf_elec_dead_time
+ *
+ * Calls:
+ *
+ * Return:      0  on success
+ *
+ * History:     08/01/03   1.1    wvd   Begin work
+ *		08/04/03   1.2    wvd	Convert aic_rate to type short.
+ *		11/25/03   1.3    wvd	For HIST data, require that
+ *					mean_tot_dtc be >= 1.
+ *		11/26/03   1.4    wvd	Change aic_rate to type float.
+ *		02/09/04   1.5    wvd	Re-write with new logic.
+ *              04/09/04   1.6    bjg   Include stdlib.h
+ *		11/07/05   1.7    wvd	Add a test to catch bad DTC values.
+ *		03/10/06   1.8    wvd	Clean up i/o.
+ *		12/29/06   1.9    wvd	Check DET_DEAD rather than TOT_DEAD.
+ *		04/07/07   1.10   wvd	Clean up compiler errors.
+ *
+ ****************************************************************************/
+#include <stdlib.h>
+#include <string.h>
+#include "calfuse.h"
+
+int
+cf_apply_dead_time(fitsfile *header, long nevents, float *time, float *weight,
+	long nseconds, float *timeline, float *ids_dtc, float *elec_dtc)
+{
+    char CF_PRGM_ID[] = "cf_apply_dead_time";
+    char CF_VER_NUM[] = "1.10";
+
+    char comment[FLEN_CARD], datestr[FLEN_CARD], instmode[FLEN_VALUE];
+    char hkexists[FLEN_VALUE];
+    double ctimeb, ctimee, eng_time;
+    int  errflg=0, status=0, timeref;
+    int  det_flag=FALSE, ids_flag=FALSE;
+    long j, k;
+    float *tot_dtc, det_dead, ids_dead, mean_tot_dtc=0.;
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+    if ((errflg = cf_proc_check(header, CF_PRGM_ID))) return errflg;
+
+    /* Read header keywords.  Set flag if DET_DEAD > 1.5 */
+    FITS_read_key(header, TSTRING, "INSTMODE", instmode, NULL, &status);
+    FITS_read_key(header, TSTRING, "HKEXISTS", hkexists, NULL, &status);
+    FITS_read_key(header, TFLOAT, "DET_DEAD", &det_dead, NULL, &status);
+    if (det_dead > 1.5) det_flag = TRUE;
+
+    /*
+     *  If there is no housekeeping file, AND the engineering snapshot times
+     *  are bad, AND the mean value of any DTC array is > 1.5, set the 
+     *  combined DTC array to unity and issue a warning.
+     */
+    if(!strncasecmp(hkexists, "N", 1)) {
+	FITS_read_key(header, TDOUBLE, "CTIME_B", &ctimeb, NULL, &status);
+        FITS_read_key(header, TDOUBLE, "CTIME_E", &ctimee, NULL, &status);
+        if ((eng_time = (ctimee-ctimeb) * 86400.) < 1.) {
+            FITS_read_key(header, TFLOAT, "IDS_DEAD", &ids_dead, NULL, &status);
+	    if (ids_dead > 1.5) ids_flag = TRUE;
+	}
+    }
+
+    /*
+     *  Compute total dead-time correction and its mean.
+     */
+    tot_dtc = (float *) cf_malloc(sizeof(float) * nseconds);
+    if (det_flag || ids_flag) {
+	for (k = 0; k < nseconds; k++) tot_dtc[k] = 1.0;
+	mean_tot_dtc = 1.0;
+    }
+    else {
+	for (k = 0; k < nseconds; k++) {
+	    tot_dtc[k] = elec_dtc[k] * ids_dtc[k];
+            mean_tot_dtc += tot_dtc[k];
+	}
+        mean_tot_dtc /= nseconds;
+    }
+
+    /* In TTAG mode, scale weights by tot_dtc as a function of time. */
+    if (!strncmp(instmode, "TTAG", 4)) for (j=k=0; j<nevents; j++) {
+        while(timeline[k+1]-FRAME_TOLERANCE < time[j] && k+1 < nseconds)
+            k++;
+        weight[j] *= tot_dtc[k];
+    }
+
+    /* In HIST mode, scale all weights by mean dead-time correction. */
+    else if (mean_tot_dtc > 1.)
+	for (j = 0; j < nevents; j++) 
+            weight[j] *= mean_tot_dtc;
+    else mean_tot_dtc = 1.;
+
+    cf_verbose(2, "Mean total dead-time correction: %f", mean_tot_dtc);
+    FITS_update_key(header, TFLOAT, "TOT_DEAD", &mean_tot_dtc, NULL, &status);
+
+    if (det_flag || ids_flag) {
+        FITS_write_comment(header, "  ", &status);
+	if (ids_flag) {
+	    sprintf(comment,
+		"IDS_DEAD > 1.5.  Setting dead-time correction to unity.");
+            cf_if_warning(comment);
+            FITS_write_comment(header, comment, &status);
+	}
+	if (det_flag) {
+	    sprintf(comment,
+		"DET_DEAD > 1.5.  Setting dead-time correction to unity.");
+            cf_if_warning(comment);
+            FITS_write_comment(header, comment, &status);
+	}
+        fits_get_system_time(datestr, &timeref, &status);
+        sprintf(comment, "CalFUSE v%s   %.10s", CALFUSE_VERSION, datestr);
+        FITS_write_comment(header, comment, &status);
+        FITS_write_comment(header, "  ", &status);
+    }
+
+    free (tot_dtc);
+    cf_proc_update(header, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return 0;
+}
diff --git a/src/libcf/cf_apply_filters.c b/src/libcf/cf_apply_filters.c
new file mode 100644
index 0000000..ff47f21
--- /dev/null
+++ b/src/libcf/cf_apply_filters.c
@@ -0,0 +1,177 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_apply_filters(fitsfile *header, int tscreen, long nevents,
+ *                      unsigned char *timeflags, unsigned char *loc_flags,
+ *			long ntimes, unsigned char *gtiflags,
+ *			float *dtime, float *ntime, long *ngood, long **index)
+ *
+ * Description: Select photons that satisfy filter criteria
+ *
+ * Arguments:   fitsfile  *header       Pointer to FITS file containing the
+ *                                      header of the intermediate data file
+ *              int       tscreen       Flag indicating whether to screen on
+ *                                       time flags (yes if > 0)
+ *              long      nevents       The number of events
+ *              unsigned char *timeflags Photon event time flags
+ *              unsigned char *loc_flags Photon event location flags
+ *              long      ntimes        Number of entries in timeline table
+ *              unsigned char *gtiflags Status flags from timeline table
+ *              float     *dtime        Day time exposure length
+ *              float     *ntime        Night time exposure length
+ *              long      *ngood        Number of good photons
+ *              long      **index       List of good photon indexes
+ *
+ * Return:      status
+ *
+ * History:     02/19/03   1.1    peb   Begin work
+ *              03/20/03   1.2    peb   Fixed daytime and nighttime
+ *                                      calculation and fill header with
+ *                                      correct EXPTIME and EXPNIGHT value.
+ *              04/08/03   1.3    wvd   Get timeline-table arrays from 
+ *					calling routine.
+ *		05/10/03   1.4    wvd	Read DAYNIGHT from file header;
+ *					test only first character.
+ *              05/20/03   1.5    rdr   Move to top level HDU before reading
+ *                                      header keywords
+ *              06/09/03   1.6    rdr   Ignore timing flags in the screening
+ *                                      if tscreen is 0.
+ *              10/06/03   1.8    wvd	Properly deal with new format of
+ *					timeline table.
+ *              12/08/03   1.9    wvd	If tscreen is 0, ignore temporal
+ *					flags when calculating dtime & ntime.
+ *              02/11/04   1.10   wvd	Correct error in calculation of
+ *					dtime and ntime.
+ *              06/02/04   1.11   wvd	Mask BRST, SAA, and LIMB flags
+ *					when calculating exposure time
+ *					for HIST data.
+ *              06/10/04   1.12   wvd	Delete timeline times array from 
+ *					argument list.
+ *		01/27/05   1.13   wvd	Use TEMPORAL_MASK rather than
+ *					TEMPORAL_DAY to screen photon status
+ *					flags.  They differ only in HIST mode.
+ *		07/18/08   1.14   wvd	If EXP_STAT = 2, target is bright
+ *					earth or airglow.  Mask limb-angle flag.
+ *		08/22/08   1.15   wvd	Compare EXP_STAT with TEMPORAL_LIMB, 
+ *					rather than a particular value.
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include <stdlib.h>
+#include <math.h>
+#include "calfuse.h"
+
+int
+cf_apply_filters(fitsfile *header, int tscreen, long nevents, 
+	unsigned char *timeflags, unsigned char *loc_flags,
+	long ntimes, unsigned char *gtiflags,
+	long *dtime, long *ntime, long *ngood, long **index)
+{
+    char CF_PRGM_ID[] = "cf_apply_filters";
+    char CF_VER_NUM[] = "1.15";
+
+    char daynight[FLEN_VALUE], instmode[FLEN_VALUE];
+    int  day=0, expstat, night=0, status=0;
+    long j;
+    float exptime;
+    unsigned char TEMPORAL_MASK;
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    /* 
+     *  Read INSTMODE keyword.  If in HIST mode, mask out
+     *  LIMB, SAA, and BRST flags.  TEMPORAL_DAY is the default.
+     */
+    TEMPORAL_MASK = TEMPORAL_DAY;
+    FITS_read_key(header, TSTRING, "INSTMODE", instmode, NULL, &status);
+    if (!strncmp(instmode, "HIST", 4)) {
+	TEMPORAL_MASK |= TEMPORAL_LIMB;
+	TEMPORAL_MASK |= TEMPORAL_SAA;
+	TEMPORAL_MASK |= TEMPORAL_BRST;
+    }
+    /*
+     * If EXP_STAT = TEMPORAL_LIMB, target is bright earth or airglow.  
+     * Mask limb-angle flag.
+     */
+    FITS_read_key(header, TINT, "EXP_STAT", &expstat, NULL, &status);
+    if (expstat == (int) TEMPORAL_LIMB) TEMPORAL_MASK |= TEMPORAL_LIMB;
+
+    /*
+     *  Calculate day/night exposure time.
+     *  If tscreen is 0, ignore the temporal flags (other than day/night).
+     */
+    *dtime = *ntime = 0.;
+    for (j=0; j<ntimes-1; j++) {
+	if ( !(gtiflags[j] & ~TEMPORAL_MASK) || !tscreen ) {
+	   if (gtiflags[j] & TEMPORAL_DAY)
+		*dtime += 1;
+	   else
+		*ntime += 1;
+	}
+    }
+    cf_verbose(2, "Exposure time: day = %ld, night = %ld", *dtime, *ntime);
+    /*
+     *  Read EXPTIME and DAYNIGHT keywords from file header.
+     */
+    FITS_movabs_hdu(header, 1, NULL, &status) ;
+    FITS_read_key(header, TFLOAT, "EXPTIME", &exptime, NULL, &status);
+    FITS_read_key(header, TSTRING, "DAYNIGHT", daynight, NULL, &status);
+
+    /* Decode DAYNIGHT keyword */
+    if (!strncmp(daynight, "D", 1) || !strncmp(daynight, "d", 1)) {
+	day = 1;
+	*ntime = 0.;
+    }
+    else if (!strncmp(daynight, "N", 1) || !strncmp(daynight, "n", 1)) {
+	night = 1;
+	*dtime = 0.;
+    }
+    else if (!strncmp(daynight, "B", 1) || !strncmp(daynight, "b", 1)) {
+	day = night = 1;
+    }
+    else
+	cf_if_error("Unknown DAYNIGHT keyword value");
+    cf_verbose(3, "DAYNIGHT flag set to %s", daynight);
+
+    /* Quick test of internal consistency */
+    if (fabs(*dtime + *ntime - exptime) > exptime/10.)
+	cf_if_warning("Sum of day and night time differs from EXPTIME by > 10%%");
+
+    /*
+     *  Apply screening to each photon event.
+     *  First mask out airglow and day flags and test for zero
+     *  (good) values.  Next, see if the user wants daytime,
+     *  night time, or both and confirm that appropriate flag is set.
+     */
+
+    *index = (long *) cf_calloc(nevents, sizeof(long));
+
+    if (tscreen) {
+        for(*ngood=j=0; j<nevents; j++) {
+	    if (!(loc_flags[j] & ~LOCATION_AIR) && 
+	        !(timeflags[j] & ~TEMPORAL_MASK) &&
+	        ((day   && (timeflags[j] & TEMPORAL_DAY)) || 
+	         (night && (timeflags[j] ^ TEMPORAL_DAY)))) {
+	        (*index)[(*ngood)++] = j;
+	    }
+	}
+    }
+
+    /*  If tscreen is 0, then screen only on the location flags.  */
+    else {
+	cf_verbose(1, "Ignoring time flags in the screening") ;
+	for(*ngood=j=0; j<nevents; j++) 
+	    if (!(loc_flags[j] & ~LOCATION_AIR)) 
+	        (*index)[(*ngood)++] = j;
+    }
+
+    cf_verbose(2, "%ld good events", *ngood);
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return status;
+}
diff --git a/src/libcf/cf_astig_farf.c b/src/libcf/cf_astig_farf.c
new file mode 100644
index 0000000..aabcdae
--- /dev/null
+++ b/src/libcf/cf_astig_farf.c
@@ -0,0 +1,144 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Description: Correct XFARF array for instrumental astigmatism.
+ *
+ * Returns:    0 upon successful completion.
+ *
+ * History:       12/12/02   1.1   jch  Begin work
+ *                02/24/03   1.2   peb  Using calfusettag.h include file
+ *                03/04/03   1.3   peb  Removed math.h - unnecessary
+ *                03/11/03   1.4   wvd  Changed channel to type *char
+ *                04/04/03   1.5   wvd  Test for overflow of astig array.
+ *                05/20/03   1.6   rdr  Add call to cf_proc_check
+ *                09/16/03   1.7   wvd  Remove calls to astig_target_aperture
+ *					and astig_read_file.  Change sign of
+ *					astigmatism correction to match
+ *					the new astg**009.fit files.
+ *					Make yoff a float.
+ *                11/05/03   1.8   wvd  Change channel to unsigned char.
+ *                04/07/07   1.9   wvd  Clean up compiler warnings.
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include "calfuse.h"
+
+static char CF_PRGM_ID[] = "cf_astig_farf";
+static char CF_VER_NUM[] = "1.9";
+
+
+/* 
+ * Add astigmatism correction to XFARF for each photon within target
+ * aperture.  Note that spectrum centroid moves with time.
+ */
+static int
+farf_astig_shifts(fitsfile *header, long nevents, float *xfarf, 
+	float *yfarf, unsigned char *channel, float *photon_time, 
+	long nseconds, float *timeline_time, float *ycentl, float *ycents)
+{
+    char        astig_file[FLEN_VALUE];
+    int   	status=0;
+    int   	active_ap[2], ap, ast_cen, extno, overflow=0;
+    long	i, j, k;
+    long  	npix, nx, ny, ii, jj, kk;
+    float 	yoff;
+    float       *astig=NULL, *centroid=NULL;
+    fitsfile    *astigfits;
+
+    /* Read target apertures from the file header */
+    (void) cf_source_aper (header, active_ap);
+
+    /* Open the astigmatism file */
+    FITS_read_key(header, TSTRING, "ASTG_CAL", astig_file, NULL, &status);
+    FITS_open_file(&astigfits, cf_cal_file(astig_file), READONLY, &status);
+
+    /*   Since we presently have no astig correction for extended
+     *   sources, we apply correction only to target aperture.
+     */
+    for (i = 0; i < 2; i++) {
+
+        ap = active_ap[i];
+	if (i == 0) 
+	    centroid = ycentl;
+	else
+	    centroid = ycents;
+
+        /* Read astigmatism correction for this aperture */
+        extno = ap+1;
+        cf_verbose(3, "Reading extension %d of %s", extno, astig_file);
+        FITS_movabs_hdu(astigfits, extno, NULL, &status);
+        FITS_read_key(astigfits, TINT, "SLIT_CEN", &ast_cen, NULL, &status);
+        FITS_read_key(astigfits, TLONG, "NAXIS1", &nx, NULL, &status);
+        FITS_read_key(astigfits, TLONG, "NAXIS2", &ny, NULL, &status);
+
+        npix = nx * ny;
+        astig = (float *) cf_malloc(sizeof(float) * npix);
+        FITS_read_img(astigfits, TFLOAT, 1L, npix, 0, astig, NULL, &status);
+
+	/* Go through the photon list, find the astigmatism (delta(X)) 
+         * corresponding to the (xfarf, yfarf) position and channel,
+	 * and add it to xfarf[k].
+	 */
+	k = 0;
+        for (j = 0; j < nevents; j++) {
+            if (channel[j] == ap) {
+                while ((photon_time[j] > timeline_time[k+1] - FRAME_TOLERANCE)
+		    && (k < nseconds-1)) {
+                    k++;
+                }
+
+        	/* Determine offset between spectrum and astig correction file. */
+        	yoff = centroid[k] - ast_cen;
+
+		/* Find the astigmatism correction appropriate 
+		   to the photon's (xfarf, yfarf) position. */
+                if ((ii = (xfarf[j] + 0.5)) >= nx) {overflow = 1; continue;};
+                if ((jj = (yfarf[j] - yoff + 0.5)) >= ny) {overflow = 1; continue;}
+                if ((kk = jj * nx + ii) >= npix) {overflow = 1; continue;}
+                xfarf[j] += astig[kk];
+            }
+        }
+
+        /* If overflow flag is set, there is a problem with the ASTG_CAL file. */
+	if (overflow)
+    	    cf_if_warning("Overflow of ASTG_CAL file in aperture %d", ap);
+
+        /* Space for astig array is allocated in each loop. */
+        free(astig);
+    }
+
+    FITS_close_file(astigfits, &status);
+    return status;
+}
+
+int cf_astig_farf(fitsfile *header, long nevents, float *xfarf, float *yfarf, 
+		  unsigned char *channel, float *photon_time, long nseconds, 
+		  float *timeline_time, float *ycentl, float *ycents)
+{
+    int 	errflg=0, status=0;
+
+    /* Enter a timestamp into the log. */
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+    if ((errflg = cf_proc_check(header, CF_PRGM_ID))) return errflg;
+
+    /* Check that astigmatism correction is appropriate for input image */
+    if (astig_check_input_image(header) == 1) {
+
+        /* Read astigmatism corrections for each aperture, add to XFARF */
+        farf_astig_shifts(header, nevents, xfarf, yfarf, channel,
+		photon_time, nseconds, timeline_time, ycentl, ycents);
+    }
+
+    /* Update processing flags. */
+    cf_proc_update(header, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done Processing");
+    return (status);
+}
diff --git a/src/libcf/cf_astigmatism.c b/src/libcf/cf_astigmatism.c
new file mode 100644
index 0000000..e02f361
--- /dev/null
+++ b/src/libcf/cf_astigmatism.c
@@ -0,0 +1,198 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Description: Modifies X array to correct for instrumental astigmatism.
+ *
+ *		Since we have no astigmatism correction for extended 
+ *		sources, this program does not attempt to apply one.
+ *
+ *              In keeping with the CalFUSE standard, the astigmatism 
+ *		correction is added to the measured X position of each photon.
+ *		Versions of the ASTG_CAL file prior to v009 have the opposite 
+ *		sign and are incompatible with this version of the program.
+ *                    
+ * Returns:     0 upon successful completion.
+ *
+ * History:     12/02/02   1.1   jch	Adapt from cf_astig.c
+ *		12/20/02   1.2   wvd	Install
+ *		02/11/03   1.3   wvd	Apply astig correction only if 
+ *					YCENT# > O for target aperture.
+ *					Add ASTG_KEY keyword.  Comment field:
+ *					Performed? 1=LiF, 2=SiC, 3=Both
+ *		02/13/03   1.4   wvd	Change all indices to type long.
+ *              02/24/03   1.5   peb    Changed include file to calfusettag.h
+ *              03/04/03   1.6   peb    Removed unused variables and math.h.
+ *                                      Corrected sprintf:185 argument error.
+ *		03/11/03   1.7   wvd	Change channel to type char
+ *		03/12/03   1.8   wvd	If wavelength undefined, set
+ *					channel[k] = 0
+ *		04/04/03   1.9   wvd	Test for overflow of astig array.
+ *		04/07/03   1.10  wvd	Delete test for quality of YCENT.
+ *					Delete ASTG_KEY keyword.
+ *					Don't round yoff to nearest integer.
+ *		04/09/03   1.11  wvd	Write name of ASTG_CAL file to trailer.
+ *              05/20/03   1.12  rdr    Added call to cf_proc_check
+ *              09/16/03   1.13  wvd    Change sign of ASTG_CAL file so that
+ *					correction is additive.
+ *              09/22/03   1.14  wvd    Initialize overflow counter.
+ *					Print out number of overflows.
+ *              10/17/03   1.15  wvd    Discard photons that fall outside of 
+ *					the astigmatism-correction window.
+ *              10/31/03   1.16  wvd    Change channel to unsigned char.
+ *              11/11/03   1.17  wvd    Interpolate between tabulated
+ *					wavelength values.  Use cf_read_col
+ *					to read wavecal files.
+ *              02/17/04   1.18  wvd    Replace cf_nint() with cf_nlong()
+ *              03/02/04   1.19  wvd    Change name of assign_wavelengths
+ *					to cf_x2lambda and make it
+ *					generally accessible.
+ *              07/16/04   1.20  wvd    Must change ASTG_COR to COMPLETE or
+ *					SKIPPED by hand.
+ *              02/18/05   1.21  wvd    Add some diagnostic output.
+ *              11/30/05   1.22  wvd    Don't complain when photon events
+ *					fall outside of astig images.
+ *              05/15/06   1.23  wvd    Divide cf_astigmatism_and_dispersion
+ *					into two separate routines.
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include <math.h>
+#include "calfuse.h"
+
+static char CF_PRGM_ID[] = "cf_astigmatism";
+static char CF_VER_NUM[] = "1.23";
+
+
+/* 
+ * Loop over the apertures, read appropriate astigmatism correction,
+ * and add to the input X shifts of pixels within extraction window.
+ */
+static int
+add_astig_shifts(fitsfile *infits, long nevents, float *x, float *y,
+	unsigned char *channel)
+{
+    char  	astig_file[FLEN_VALUE], keyword[FLEN_VALUE];
+    int   	status=0;
+    int   	ap, active_ap[2], ast_cen, extno, i, overflow;
+    long  	k, ii, jj, kk, npix, nx, ny;
+    float 	centroid, yoff;
+    float 	*astig=NULL;
+    fitsfile 	*astigfits;
+
+    /* Read target apertures from the file header */
+    (void) cf_source_aper (infits, active_ap);
+
+    /* Open the astigmatism file */
+    FITS_read_key(infits, TSTRING, "ASTG_CAL", astig_file, NULL, &status);
+    FITS_open_file(&astigfits, cf_cal_file(astig_file), READONLY, &status);
+
+    /*   Since we presently have no astig correction for extended
+     *   sources, we apply correction only to target aperture.
+     */
+    for (i = 0; i < 2; i++) {
+	ap = active_ap[i];
+
+	/* Read the centroid of the aperture from the input file. */
+	sprintf(keyword, "YCENT%1d", ap); 
+    	FITS_read_key(infits, TFLOAT, keyword, &centroid, NULL, &status);
+        cf_verbose(3, "Target aperture: %d\t Y centroid: %f", ap, centroid);
+
+	/* Read astigmatism correction for this aperture */
+	extno = ap+1;
+	cf_verbose(3, "Reading extension %d of %s", extno, astig_file);
+	FITS_movabs_hdu(astigfits, extno, NULL, &status);
+	FITS_read_key(astigfits, TINT, "SLIT_CEN", &ast_cen, NULL, &status);
+	FITS_read_key(astigfits, TLONG, "NAXIS1", &nx, NULL, &status);
+	FITS_read_key(astigfits, TLONG, "NAXIS2", &ny, NULL, &status);
+
+	npix = nx * ny;
+	astig = (float *) cf_malloc(sizeof(float) * npix);
+	FITS_read_img(astigfits, TFLOAT, 1L, npix, 0, astig, NULL, &status);
+
+	/* Determine offset between spectrum and astig correction file */
+	yoff = centroid - ast_cen;
+	cf_verbose(3, "Offset between spectrum and astig correction: %f", yoff);
+
+	/*  Go through the event list and find the astigmatism correction
+	 *  appropriate for the photon's (x, y) position.
+	 */
+	overflow = 0;
+	for (k = 0; k < nevents; k++) {
+	    if (channel[k] == ap) {
+		if (((ii = cf_nlong(x[k])) < 0 || ii >= nx) ||
+		    ((jj = cf_nlong(y[k] - yoff)) < 0 || jj >= ny) ||
+		    ((kk = jj * nx + ii) >= npix)) {
+			channel[k] = 0;
+			overflow++;
+			cf_verbose(3, "Cannot correct pixel %05ld (%f, %f)",
+				k, x[k], y[k]);
+		}
+		else x[k] += astig[kk]; 
+	    } 
+	}
+	/* If overflow flag is set, there is a problem either with
+		the ASTG_CAL file or the input photon list.
+	if (overflow)
+    	    cf_if_warning("%d events fell outside of aperture %d ASTG_CAL window",
+		overflow, ap);
+	Comment this out, as it is always triggered by cf_bad_pixels. - wvd (11/30/05) */
+
+        /* Space for astig array is allocated in each loop. */
+	free(astig);
+    	cf_verbose(3, "End of loop for aperture %d", ap);
+    }
+
+    FITS_close_file(astigfits, &status);
+    return status;
+}
+
+
+/*
+ *  If APERTURE = RFPT or target is not a point source, exit without
+ *  applying an astigmatism correction.
+ */
+int cf_astigmatism(fitsfile *infits, long nevents, float *x,
+	float *y, unsigned char *channel)
+{
+    char 	aperture[FLEN_VALUE];
+    char	source_type[FLEN_VALUE];
+    int 	errflg=0, fileok=TRUE, status=0;
+
+    /* Enter a timestamp into the log. */
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    if ((errflg = cf_proc_check(infits, CF_PRGM_ID))) return errflg;
+
+    FITS_read_key(infits, TSTRING, "APERTURE", aperture, NULL, &status);
+    if (!strncmp(aperture, "RFPT", 4)) {
+        cf_verbose(1, "Aperture is RFPT. No astig correction applied.");
+	fileok = FALSE;
+    }
+
+    /* Check source type */
+    FITS_read_key(infits, TSTRING, "SRC_TYPE", source_type, NULL, &status);
+    if (strncmp(source_type, "P", 1)) {
+	cf_verbose(1, "Source type is %s. No astig correction applied.",
+	    source_type);
+	fileok = FALSE;
+    }
+
+    if (fileok) {
+        add_astig_shifts(infits, nevents, x, y, channel);
+	cf_proc_update(infits, CF_PRGM_ID, "COMPLETE");
+    }
+    else
+	cf_proc_update(infits, CF_PRGM_ID, "SKIPPED");
+
+    /* Update processing flags. */
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done Processing");
+
+    return fileok;
+}
diff --git a/src/libcf/cf_cal_file.c b/src/libcf/cf_cal_file.c
new file mode 100644
index 0000000..59c873d
--- /dev/null
+++ b/src/libcf/cf_cal_file.c
@@ -0,0 +1,84 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_cal_file(char *calfile)
+ *
+ * Description: Returns a pointer to a string with the full calibration 
+ *              path (from the CF_CALDIR environment variable) prepended 
+ *              to the given file name.
+ *
+ * Arguments:   char    *calfile        Name of the calibration file.
+ *
+ * Returns:     A pointer to a string which contains the full path filename.
+ *
+ * History:     02/26/99       emurphy  Begin and finish work.
+ *              03/01/99       emurphy  Added some error checking
+ *              03/02/99       emurphy  Added use of cf_if_warning
+ *              04/04/99       emurphy  removed cf_error_init
+ *              04/08/99       barrett  replaced fitsio.h with calfuse.h
+ *              05/18/99       emurphy  Added checks on strlen and ending "/"
+ *              06/04/99          peb   Removed 160 character string limit
+ *                                      Added cf_malloc function.
+ *              08/05/99       emurphy  Created cf_populate_file, to support
+ *                                      cf_cal_file and cf_hist_file.c
+ *              08/25/99       emurphy  Added cf_parm_file for parameter files.
+ *              12/18/03       bjg      Change calfusettag.h to calfuse.h
+ *
+ ****************************************************************************/
+
+#include <stdlib.h>
+#include <string.h>
+#include "calfuse.h"
+
+static char
+*cf_populate_file(char *calfile, char *enviro_name)
+{
+    char *enviro, *filen;
+    int strl, strt;
+
+    enviro = getenv(enviro_name);
+
+    if (enviro) {
+        strl = strlen(enviro);
+	strt = strl + strlen(calfile) + 16;
+
+	filen = cf_malloc(strt);
+        strcpy(filen, enviro);
+
+        /* Check to see if last character is a "/" */
+        if (strncmp(filen+strl-1, "/", 1)!=0)
+             strcat(filen, "/");
+
+        strcat(filen, calfile);
+        return filen;
+    }
+    else {
+        printf("Environment variable %-20.20s undefined.",enviro_name);
+        cf_if_warning("Environment variable undefined");
+        return calfile;
+    }
+}
+
+char *cf_cal_file(char *calfile)
+{
+
+     return cf_populate_file(calfile, "CF_CALDIR");
+
+}
+
+char *cf_hist_file(char *calfile)
+{
+
+     return cf_populate_file(calfile, "CF_HISTDIR");
+
+}
+
+char *cf_parm_file(char *calfile)
+{
+
+     return cf_populate_file(calfile, "CF_PARMDIR");
+
+}
diff --git a/src/libcf/cf_calculate_y_centroid.c b/src/libcf/cf_calculate_y_centroid.c
new file mode 100644
index 0000000..ebcd264
--- /dev/null
+++ b/src/libcf/cf_calculate_y_centroid.c
@@ -0,0 +1,289 @@
+/**************************************************************************
+ *           Johns Hopkins University
+ *           Center for Astrophysical Sciences
+ *           FUSE
+ **************************************************************************
+ *
+ * Synopsis:    cf_calculate_y_centroid(infits, nevents, weight, x, y,
+ *			channel, timeflags, locflags)
+ *
+ * Description: Determines the y centroid of the target and airglow spectra
+ *              in each aperture.  The value written to the header depends
+ *		on the quality flag for each channel in the IDF header.
+ *		If QUALITY = HIGH, the target centroid is used; if MEDIUM,
+ *		the airglow centroid is used; if LOW, the default centroid
+ *		(from the CHID_CAL file) is used.
+ *
+ * Arguments:   fitsfile infits   Pointer to the input Intermediate Data File
+ *              long     nevents  Number of photon events in the file
+ *		float	 weight   Scale factor for each photon
+ *              float    *x, *y   X and Y positions of the photon
+ *       unsigned char  *channel  Aperture associated with each photon
+ *       unsigned char *timeflags Time flags - used to identify photons
+ *                                  arriving during bursts, etc.
+ *       unsigned char *locflags  Location flags - used to identify photons
+ *                                  in geocoronal line regions
+ *
+ * Calibration files required: 
+ *
+ * Returns: 0 on success
+ *                                
+ * HISTORY:     10/16/02    v1.1   RDR  started work
+ *              12/02/02    v1.2   RDR  cleaned up variables
+ *		12/12/02    v1.3   wvd	added include files
+ *              12/26/02    v1.4   RDR  corrected error in calculating centroid
+ *              02/24/03    v1.5   peb  changed include file to calfitsio.h
+ *		03/11/03    v1.6   wvd  Changed screen to unsigned char
+ *              03/25/03    v1.7   rdr  ignore pinhole aperture
+ *		04/03/03    v1.9   wvd  Simplify calculation of centroid.
+ *					Include airglow in centroid
+ *					calculation of non-target apertures.
+ *					Replace printf() with cf_verbose().
+ *		04/17/03    v1.10  wvd  Fix bug in calculation of non-target
+ *					centroids.
+ *		04/18/03    v1.11  wvd  Call cf_proc_update only if final_call
+ *					is TRUE.  Scale YCENT by photon weight
+ *					for use with HIST data.  Changed
+ *					screen to locflags.
+ *              05/20/03    v1.12  rdr  Added call to cf_proc_check
+ *              05/22/03    v1.14  wvd	cf_error_init to stderr
+ *              08/21/03    v1.16  wvd	Change channel to unsigned char
+ *              09/02/03    v1.17  bjg  Now read user-specified centroid 
+ *                                      information from PARM_CAL and
+ *                                      expected centroids from CHID_CAL.
+ *              09/02/03    v1.18  wvd	Tidy up code.
+ *              09/17/03    v1.19  wvd	Return -1 if a target centroid
+ *					is too far from expected value.
+ *              10/28/03    v1.20  wvd	Rewrite program with new logic.
+ *					Delete use of final_call.
+ *              11/12/03    v1.21  wvd	If no photons in channel, don't
+ *					crash, just use default centroid.
+ *					If quality = LOW, ygeo = ycent.
+ *              04/09/04    v1.22  bjg  Include string.h and stdio.h
+ *              06/04/04    v1.23  wvd	Use photon time flags to exclude
+ *					bursts, etc. from calculation.
+ *              08/18/04    v1.24  wvd	Test all spectra to see whether
+ *					centroid is out of bounds.
+ *		03/11/05    v1.25  wvd  Tabulate centroids as doubles,
+ *					then convert to floats.
+ *					Write target centroid values
+ *					to trailer file if verbose >= 2.
+ *		04/15/05    v1.26  wvd  Clean up i/o.
+ *		04/26/05    v1.27  wvd  Don't populate YGEO keywords, as
+ *					they are wrong for point sources.
+ *					Consider only events with good
+ *					LOCATION flags.
+ *					Use the largest aperture with a valid
+ *					YGEO to determine offset from tabulated
+ *					position.  Use this shift to calculate 
+ *					ygeo for the smaller apertures. 
+ *		05/18/05    v1.28  wvd  Test both SPEX_LIF and SPEX_SIC.
+ *					Don't override user-specified centroid,
+ *					even if it's far from expected value.
+ *					Fix bug in tabulation of expected
+ *					Y centroids.
+ *		02/01/06    v1.29  wvd  If ycent is too far from default value,
+ *					use default value, not airglow centroid.
+ *					Allow computation of yshift from
+ *					airglow photons in target aperture.
+ *		11/25/08    1.30 wvd	In HIST mode, there are no spectra in
+ *					other apertures to cause confusion,
+ *					so we need not require that the target
+ *					centroid lie within X pixels of either
+ *					the airglow or tabulated centroid.
+ *
+ **************************************************************************/
+
+#include <math.h>
+#include <string.h>
+#include <stdio.h>
+#include "calfuse.h"
+
+int cf_calculate_y_centroid(fitsfile *infits, long nevents, float *weight,
+     float *x, float *y, unsigned char *channel, unsigned char *timeflags,
+     unsigned char *locflags)
+{
+
+     char CF_PRGM_ID[] = "cf_calculate_y_centroid";
+     char CF_VER_NUM[] = "1.30";
+ 
+     char aperture[FLEN_VALUE], instmode[FLEN_VALUE];
+     char ycentname[FLEN_KEYWORD], file_name[FLEN_VALUE];
+     char key[FLEN_KEYWORD], quality[8][FLEN_VALUE];
+     double dncent, dngeo, dycent, dygeo;
+     float ycent, ygeo, yshift, ycent_tab[8];
+     int chan_num, errflg=0, status=0, active_ap[2];
+     int got_shift, i, hdu, target_ap, user;
+     int spex_sic, spex_lif, emax_sic, emax_lif, emax, extended;
+     long n;
+     fitsfile *parm_cal, *chid_cal;
+
+  /* Initialize error checking */ 
+     cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+  /* Enter a time stamp into the log */
+     cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+  /* Check whether routine is appropriate for this data file. */
+     if ( (errflg = cf_proc_check(infits, CF_PRGM_ID)) ) return errflg;
+
+  /* Read the source aperture from the file header. */
+     FITS_read_key(infits, TSTRING, "APERTURE", aperture, NULL, &status);
+     extended=cf_source_aper(infits, active_ap) ;
+
+  /* Were data taken in HIST or TTAG mode? */
+     FITS_read_key(infits, TSTRING, "INSTMODE", instmode, NULL, &status);
+     
+  /* Read centroid quality keywords from file header. */
+     for (i = 1; i < 8; i++) {
+	if (i == 4) continue;
+	sprintf(key, "YQUAL%1d", i);
+	FITS_read_key(infits, TSTRING, key, &quality[i][0], NULL, &status);
+     }
+     
+  /* Read extraction parameters from PARM_CAL file. */
+     FITS_read_key(infits, TSTRING, "PARM_CAL", file_name, NULL, &status);
+     FITS_open_file(&parm_cal, cf_parm_file(file_name), READONLY, &status);
+     FITS_read_key(parm_cal,TINT,"SPEX_SIC",&spex_sic,NULL,&status);
+     FITS_read_key(parm_cal,TINT,"SPEX_LIF",&spex_lif,NULL,&status);
+     FITS_read_key(parm_cal,TINT,"EMAX_SIC",&emax_sic,NULL,&status);
+     FITS_read_key(parm_cal,TINT,"EMAX_LIF",&emax_lif,NULL,&status);
+     FITS_close_file(parm_cal,&status);
+     
+  /* Read expected centroids from CHID_CAL file.  Use extended-aperture
+     values except for apertures containing point-source targets.  */
+     FITS_read_key(infits, TSTRING, "CHID_CAL", file_name, NULL, &status);
+     FITS_open_file(&chid_cal, cf_cal_file(file_name), READONLY, &status);
+     for (i = 1; i < 8; i++) {
+     	if (i==4) continue;
+        if ((i == active_ap[0] || i == active_ap[1]) && !extended) hdu=i+1;
+	else hdu=i+9;
+     	FITS_movabs_hdu(chid_cal, hdu, NULL, &status);
+     	FITS_read_key(chid_cal,TFLOAT,"CENTROID",ycent_tab+i,NULL,&status);
+     }
+     FITS_close_file(chid_cal,&status);
+
+  /* Determine the centroids for each channel */
+     yshift = 0;
+     got_shift = FALSE;
+     for (chan_num = 7; chan_num > 0; chan_num--) {
+	if (chan_num == 4) {
+	    yshift = 0;
+	    got_shift = FALSE;
+	    continue;
+	}
+        dngeo = dncent = 0.;
+	dygeo = dycent = 0.;
+	sprintf (ycentname, "YCENT%d", chan_num);
+
+        /* Is this a target aperture? */
+        if (chan_num == active_ap[0] || chan_num == active_ap[1])
+            target_ap = TRUE;
+        else
+            target_ap = FALSE;
+
+	/* If not, and we're in histogram mode, skip to the next channel. */
+	if (!target_ap && !strncmp(instmode, "HIST", 4)) continue;
+
+	/* Calculate separate target and geocoronal centroids. */
+        for (n = 0; n < nevents; n++) {
+	    if (channel[n] == chan_num && !(timeflags[n] & ~TEMPORAL_DAY) &&
+		!(locflags[n] & ~LOCATION_AIR)) { 
+
+		if(locflags[n] & LOCATION_AIR) {  /* Airglow photon */
+		    dygeo += y[n] * weight[n];
+		    dngeo += weight[n];
+		}
+		else {				  /* Target photon */
+		    dycent += y[n] * weight[n];
+		    dncent += weight[n];
+		}
+	    }
+        }
+
+	/* If we can't find any photons but expect to, set quality to LOW. */
+	if ((quality[chan_num][0] == 'H' && dncent < 1) ||
+	    (quality[chan_num][0] == 'M' && dngeo  < 1)) {
+	    quality[chan_num][0] = 'L';
+	    sprintf(key, "YQUAL%1d", chan_num);
+	    FITS_update_key(infits, TSTRING, key, "LOW", NULL, &status) ;
+	    cf_verbose(1, "No photon events in channel %d", chan_num);
+	}
+
+        /* Compute centroids of target and airglow spectra */
+	ycent = ygeo = 0; 
+	if (dncent > 0) ycent = dycent / dncent; 
+	if (dngeo  > 0) ygeo  = dygeo / dngeo; 
+
+	/* If yshift is already known, use it to calculate ygeo.
+	 * If not, and ygeo is valid for this aperture, compute yshift.
+	 */
+	if (got_shift)
+	    ygeo = yshift + ycent_tab[chan_num];
+	else if (dngeo > 0) {
+	    yshift = ygeo - ycent_tab[chan_num];
+	    got_shift = TRUE;
+	}
+
+	/* Now decide which values to write to the header. */
+	  
+	/* If we are in the target aperture and the user has specified
+         * YCENT for this channel, use it.
+	 */
+        if (target_ap && ((chan_num<5 && spex_lif>=0 && spex_lif<1024) ||
+            (chan_num>4 && spex_sic>=0 && spex_sic<1024))) {
+            if (chan_num<5) ycent=spex_lif;
+            else ycent=spex_sic;
+	    cf_verbose(1, "Channel %d: User-specified Y centroid = %g",
+		chan_num, ycent);
+	    user = TRUE;
+	}
+	else
+	    user = FALSE;
+
+	/* If the centroid quality is HIGH, use the calculated target
+	 * value, regardless of whether we are in a target aperture.
+	 * (This happens by default, so we don't have to do anything.)
+	 */
+
+	/* If the centroid quality is MED, use the airglow centroid. */
+	if (quality[chan_num][0] == 'M')
+	    ycent = ygeo;
+
+	/* If the quality is LOW, use the default value. */
+	else if (quality[chan_num][0] == 'L')
+	    ycent = ycent_tab[chan_num];
+
+        /* 
+	 *  Test whether YCENT is too far from the expected value.
+	 *  If so, use the tabulated value and set the quality to LOW.
+	 *  Don't test HIST data. (wvd, 11/25/2008)
+	 */
+	if (chan_num<5) emax=emax_lif; else emax=emax_sic;
+	if (fabs(ycent-ycent_tab[chan_num]) > emax && !user && !strncmp(instmode, "TTAG", 4)) {
+	    if(target_ap) {
+        	cf_verbose(1, "Channel %d: computed centroid (%.1f) is too far "
+		    "from expected value.", chan_num, ycent);
+		cf_verbose(1, "Channel %d: using default centroid of %.1f",
+		    chan_num, ycent_tab[chan_num]);
+	    }
+	    else {
+		cf_verbose(2, "Channel %d: using default centroid of %.1f",
+		    chan_num, ycent_tab[chan_num]);
+	    }
+	    ycent = ycent_tab[chan_num];
+	    sprintf(key, "YQUAL%1d", chan_num);
+	    FITS_update_key(infits, TSTRING, key, "LOW", NULL, &status) ;
+	}
+	    
+        /* Write centroid of target spectrum to the header */
+        FITS_update_key(infits, TFLOAT, ycentname, &ycent, NULL, &status) ;
+        cf_verbose(2, "For channel %d, Y centroid = %.1f", chan_num, ycent) ;
+
+     }			/* End of loop over channels. */
+
+     cf_proc_update(infits, CF_PRGM_ID, "COMPLETE");
+     cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished processing"); 
+
+     return status;
+}
diff --git a/src/libcf/cf_calculate_ycent_motion.c b/src/libcf/cf_calculate_ycent_motion.c
new file mode 100644
index 0000000..8879213
--- /dev/null
+++ b/src/libcf/cf_calculate_ycent_motion.c
@@ -0,0 +1,152 @@
+/**************************************************************************
+ *           Johns Hopkins University
+ *          Center for Astrophysical Sciences
+ *           FUSE
+ *************************************************************************
+ *
+ * synopsis:    cf_calculate_ycent_motion(header, nevents, ptime, y, channel,
+ *              locflags, nsec, ttime, ycentl, ycents)
+ *
+ * Description: Determines the Y centroid of the emission as a function
+ *              of time within the target apertures
+ *
+ * Arguments:   fitsfile  *header :   pointer to Intermediate Data File
+ *              long      nevents :   number of photon events in the file
+ *              float     *ptime  :   detection time for each photon
+ *              float     *y      :   y position of each photon
+ *       unsigned char    *channel:   aperture associated with each photon
+ *       unsigned char   *locflags:   location flag array
+ *              long      nsec    :   number of seconds tabulated in timeline
+ *              float     *ttime  :   tabulated times in the timeline
+ *                                    geocoronal photons
+ *              float     *ycentl, *ycents : 
+ *                                    y centroids of the Lif and SiC apertures,
+ *                                    tabulated once per second throughout
+ *                                    the observation
+ *             
+ *
+ * Calibration files required:     None
+ *
+ * Returns:	0 on success
+ *
+ *                                
+ * HISTORY:     11/05/02   v1.1   RDR   started work
+ *              11/27/07   v1.2   RDR   corrected a bug in determining ycent
+ *                                        cleaned up variables
+ *              12/04/02   v1.3   RDR   locflags out geocoronal emission
+ *                                        before determining centroids
+ *              12/12/02   v1.4   wvd   change order of subroutine arguments
+ *		01/17/03   v1.5   wvd   call cf_update_proc()
+ *              01/20/03   v1.6   rdr   correct error in calculating ycent
+ *                                        during the last time interval
+ *              02/24/03   v1.7   peb   Changed include file to calfitsio.h
+ *		03/11/03   v1.8   wvd   Changed locflags to unsigned char
+ *              05/20/03   v1.9   rdr   Added call to cf_proc_check
+ *		05/22/03   v1.10  wvd   cf_error_init to stderr
+ *		06/04/03   v1.11  wvd   Implement cf_verbose throughout.
+ *		08/21/03   v1.12  wvd   Change channel to unsigned char.
+ *		10/06/03   v1.13  wvd   Change screen to locflags throughout.
+ *              10/21/04   v1.14  bjg   Corrected several bugs
+ *              04/07/07   v1.15  wvd	Clean up compiler warnings.
+ *              04/07/07   v1.16  wvd	Clean up compiler warnings.
+ *
+ **************************************************************************/
+
+#include "calfuse.h"
+
+
+int
+cf_calculate_ycent_motion(fitsfile *header, long nevents, float *ptime, 
+			  float *y, unsigned char *channel, unsigned char *locflags,
+			  long nsec, float *ttime, float *ycentl, float *ycents)
+{
+    char CF_PRGM_ID[] = "cf_calculate_ycent_motion";
+    char CF_VER_NUM[] = "1.16";
+ 
+    char ycentname[FLEN_CARD];
+    int chan_num, status=0, j, src_type, active_ap[2], nave=500;
+    int errflg=0;
+    long i, ndx, ndxs, nsam;
+    float ycent, ptst, dt, dt1;
+    float ycentdef[2];
+    float *ycentptr[2];
+
+    ycentptr[0]=ycentl;
+    ycentptr[1]=ycents;
+
+    /* Initialize error checking */ 
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+    /* Enter a time stamp into the log */
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    /* Check whether routine is appropriate for this data file. */
+    if ((errflg = cf_proc_check(header, CF_PRGM_ID))) return errflg;
+
+    /* nave = number of photons to average in determining the centroid.
+       Should eventually be read from a parameter file. */
+    nave = 500;
+
+    /* Determine the source aperture and type from the header data.
+       src_type = 0 for a point source and 1 for an extended source. */
+
+    src_type = cf_source_aper(header, active_ap);
+    cf_verbose(3, "active_ap = %d and %d,   src_type = %d",
+	   active_ap[0], active_ap[1], src_type);
+
+
+    /* Determine the centroids.  Do LiF and SiC apertures separately. */
+
+    for (j=0; j<2; j++) {
+
+ 
+      /* Select the channel number of the appropriate active aperture */
+      chan_num = active_ap[j];
+      sprintf(ycentname, "YCENT%1d", chan_num);
+      FITS_read_key(header, TFLOAT, ycentname, &ycentdef[j], NULL, &status);
+
+      nsam = 0;
+      ycent = 0.;
+      ptst = ptime[0];
+      ndxs = 0;
+
+      /* Go through all of the photons, determine the y centroids,
+	 and fill in the arrays.  Avoid airglow lines. */ 
+      for (i=1; i<nevents; i++) {
+	dt = ptime[i] - ptst;
+	dt1 = ptime[i] - ptime[i-1];
+	if (channel[i] == chan_num && !(locflags[i] & LOCATION_AIR)) {
+	  ycent += y[i];
+	  nsam += 1;
+	}
+	if ((nsam > nave && dt > 1.) || i == nevents-1 || dt1 > 10)  {
+	  
+	  if (nsam==0) ycent = ycentdef[j];
+	  else ycent = ycent / nsam;
+	  
+	  ndx = ndxs;
+	  
+	  while ( ndx < nsec && (ndx==0 || ttime[ndx-1] < ptime[i])) {
+	    
+	    if (nsam > nave) ycentptr[j][ndx] = ycent;
+	    else {
+	      if (ndx==0) ycentptr[j][ndx] = ycentdef[j];
+	      else ycentptr[j][ndx] = ycentptr[j][ndx-1]; 
+	    }
+	    
+	    
+	    ndx += 1; 
+	  }
+	  
+	  ndxs=ndx;
+	  if (ndxs > nsec-1) ndxs = nsec-1; 
+	  nsam = 0;
+	  ycent=0.;
+	  ptst=ptime[i];
+	}
+      }
+    }
+    cf_proc_update(header, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished processing"); 
+    return (status);
+}
diff --git a/src/libcf/cf_check_digitizer.c b/src/libcf/cf_check_digitizer.c
new file mode 100644
index 0000000..81e9702
--- /dev/null
+++ b/src/libcf/cf_check_digitizer.c
@@ -0,0 +1,101 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_check_digitizer(fitsfile *infits);
+ *
+ * Description: Check the digitizer values against a reference file.
+ *
+ * Arguments:   fitsfile  *infits       Input FITS file pointer
+ *
+ * Calls:       
+ *
+ * Returns:     0 on success
+ *
+ * History:     01/16/03   1.1   jch    Initial coding
+ *		01/28/03   1.2   wvd    Check only values for this detector.
+ *		02/29/03   1.3   rch    Correct error in making comparisons.
+ *              01/29/03   1.4   rdr    Include math.h
+ *              03/04/03   1.5   peb    Remove unused variables and header
+ *              05/20/03   1.6   rdr    Add call to cf_proc_check
+ *		07/29/03   1.8   wvd	If cf_proc_check fails, return errflg.
+ *		01/28/05   1.9   wvd	On error, set EXP_STAT flag to -999 and
+ *					issue a warning rather than an error.
+ *		03/11/05   1.10  wvd	On error, write a warning to the file
+ *					header using our standard format.
+ *		03/30/07   1.11  wvd	On error, set EXP_STAT flag to -2,
+ *					rather than -999.
+ *
+ ****************************************************************************/
+
+#include <stdio.h>
+#include <math.h>
+#include "calfuse.h"
+
+#define N 32
+
+int
+cf_check_digitizer(fitsfile *infits)
+{
+    char 	CF_PRGM_ID[] = "cf_check_digitizer";
+    char 	CF_VER_NUM[] = "1.11";
+
+    char  	comment[FLEN_COMMENT], datestr[FLEN_CARD], 
+		file_name[FLEN_VALUE], detector[FLEN_VALUE];
+    fitsfile	*digifits;
+    int   	errflg=0, status=0, i, first, last, exp_stat = -2;
+    int		timeref;
+    float	val, ref_val;
+
+    char    	key[N][9] = {"DET1ASCL", "DET1BSCL", "DET1AXOF", "DET1BXOF", "DET1AUCT", "DET1BUCT", "DET1ABWK", "DET1BBWK", "DET1AEWK", "DET1BEWK", "DET1ABSL", "DET1BBSL", "DET1ALCT", "DET1BLCT", "DET1ALTT", "DET1BLTT", "DET2ASCL", "DET2BSCL", "DET2AXOF", "DET2BXOF", "DET2AUCT", "DET2BUCT", "DET2ABWK", "DET2BBWK", "DET2AEWK", "DET2BEWK", "DET2ABSL", "DET2BBSL", "DET2ALCT", "DET2BLCT", "DET2ALTT", "DET2BLTT"};
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    if ((errflg = cf_proc_check(infits, CF_PRGM_ID))) return errflg;
+
+    /*
+     *  Determine which detector produced our data file.
+     */
+    FITS_read_key(infits, TSTRING, "DETECTOR", detector, 0, &status);
+    if (detector[0] == '1')
+	first = 0, last = N/2;
+    else
+	first = N/2, last = N;
+
+    /*
+     *  Read the digitizer reference file name and open it.
+     */
+    FITS_read_key(infits, TSTRING, "DIGI_CAL", file_name, 0, &status);
+    FITS_open_file(&digifits, cf_cal_file(file_name), READONLY, &status);
+
+    /*
+     *  Read keywords.  Compare with reference values.
+     */
+    for (i = first; i < last; i++) {
+        FITS_read_key(infits, TFLOAT, key[i], &val, NULL, &status);
+        FITS_read_key(digifits, TFLOAT, key[i], &ref_val, NULL, &status);
+
+        if (fabs(val - ref_val) > 2.0) {
+            cf_if_warning("Digitizer keyword %s is out of bounds.", key[i]);
+	    sprintf(comment, "Data suspect: keyword %s out of bounds", key[i]);
+	    FITS_update_key(infits, TINT, "EXP_STAT", &exp_stat, comment,
+		&status);    
+            FITS_write_comment(infits, " ", &status);
+	    sprintf(comment, "Data are suspect.  Keyword %s is out of bounds.",
+		key[i]);
+            FITS_write_comment(infits, comment, &status);
+            fits_get_system_time(datestr, &timeref, &status);
+            sprintf(comment, "CalFUSE v%s   %.10s", CALFUSE_VERSION, datestr);
+            FITS_write_comment(infits, comment, &status);
+            FITS_write_comment(infits, " ", &status);
+	}
+    }
+
+    FITS_close_file(digifits, &status);
+    cf_proc_update(infits, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return 0;
+}
diff --git a/src/libcf/cf_convert_to_ergs.c b/src/libcf/cf_convert_to_ergs.c
new file mode 100644
index 0000000..2eaaeef
--- /dev/null
+++ b/src/libcf/cf_convert_to_ergs.c
@@ -0,0 +1,182 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_convert_to_ergs(fitsfile *header, long nevents,
+ *              float *weight, float *ergcm2, unsigned char *channel,
+ *		float *lambda);
+ *
+ * Description: Convert counts to ergs.
+ *
+ * Arguments:   *header                 Input FITS file pointer
+ *              nevents                 number of points in the photon list
+ *              *weight			weight of each event
+ * 		*ergcm2			flux (returned)
+ *              *channel                channel number in the photon list
+ *              *lambda                 wavelength in the photon list
+ *
+ * Returns:    	0 (int) upon successful completion.
+ *
+ * History:    	01/02/03   1.0   jch    Initial coding
+ *		02/10/03   1.1   wvd    Install
+ *		02/10/03   1.2   wvd    Replace FLUX_CAL with AEFF_CAL
+ *                                      Define HC in calfusettag.h
+ *                                      Don't sort photons by wavelength
+ *              03/04/03   1.3   peb    Fixed sprintf argument formating,
+ *                                      deleted unused variable, localized
+ *                                      scope of some variables, made sure
+ *                                      that memory is allocated for aeff,
+ *                                      and fixed memory leak with aeff,
+ *                                      aeff1, and aeff2.
+ *		03/11/03   1.4   wvd    Changed channel to type char
+ *		03/12/03   1.5   wvd    Fixed bug in calculation of dl.
+ *					If unable to calculate flux,
+ *					set channel[k] = 0.
+ *					Made aeff, aeff1, aeff2 doubles
+ *					to match aeff*fit files.
+ *		05/07/03   1.6   wvd	Change ERGCM2S to ERGCM2 throughout.
+ *					Don't divide by EXPTIME.
+ *					Use cf_verbose throughout.
+ *		05/16/03   1.7   wvd	Update version number.
+ *              05/20/03   1.8   rdr    Add call to cf_proc_check
+ *              06/11/03   1.9   wvd    Pass datatype to cf_read_col.
+ *					Change calfusettag.h to calfuse.h
+ *              08/25/03   1.10  wvd    Change coltype from string to int
+ *					in cf_read_col.
+ *              09/17/03   1.11  wvd    Change aeff arrays to type float
+ *					to match AEFF_CAL files.
+ *              11/05/03   1.12  wvd    Change channel to unsigned char
+ *              04/27/04   1.13  wvd    Print out relative weighting of
+ *					the two effective-area files.
+ *              11/18/05   1.14  wvd    Change aeff arrays to type double
+ *					to match AEFF_CAL files.
+ *              04/07/07   1.15  wvd	Clean up compiler warnings.
+ *              04/07/07   1.16  wvd	Clean up compiler warnings.
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include "calfuse.h"
+
+static char CF_PRGM_ID[] = "cf_convert_to_ergs";
+static char CF_VER_NUM[] = "1.16";
+
+
+int
+cf_convert_to_ergs(fitsfile *header, long nevents, float *weight, 
+		   float *ergcm2, unsigned char *channel, float *lambda)
+{
+    char        aeff1file[FLEN_VALUE], aeff2file[FLEN_VALUE];
+    int		ap, errflg=0, interp=0, status=0;
+    float 	sig1=0, sig2=0;
+    fitsfile    *aeff1fits, *aeff2fits;
+
+    /* Enter a timestamp into the log. */
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+    if ((errflg = cf_proc_check(header, CF_PRGM_ID))) return errflg;
+
+    /* Read the AEFF1CAL and AEFF2CAL keywords. */
+    FITS_read_key(header, TSTRING, "AEFF1CAL", aeff1file, NULL, &status);
+    FITS_read_key(header, TSTRING, "AEFF2CAL", aeff2file, NULL, &status);
+
+    /* Open the calibration files. */
+    FITS_open_file(&aeff1fits, cf_cal_file(aeff1file), READONLY, &status);
+
+    /* Determine whether we need to interpolate getween AEFF_CAL files. */
+    if (strcmp(aeff1file, aeff2file)) {
+	float dt1, dt2, dt3, a1date, a2date, expstart, expend, expmjd;
+        interp = 1;
+        FITS_open_file(&aeff2fits, cf_cal_file(aeff2file), READONLY, &status);
+        FITS_read_key(aeff1fits, TFLOAT, "EFFMJD", &a1date, NULL, &status);
+        FITS_read_key(aeff2fits, TFLOAT, "EFFMJD", &a2date, NULL, &status);
+
+	/* Linearly interpolate the aeff according to exposure time */
+        FITS_read_key(header, TFLOAT, "EXPSTART", &expstart, NULL, &status);
+        FITS_read_key(header, TFLOAT, "EXPEND", &expend, NULL, &status);
+	expmjd = (expstart + expend) / 2.;
+        dt1=a2date-a1date;
+        dt2=a2date-expmjd;
+        dt3=expmjd-a1date;
+        if (dt1 < 0.01) {
+            cf_if_error("Calibration file dates are identical: "
+	    "cal1=%10.5f obs=%10.5f cal2=%10.5f", a1date, expmjd, a2date);
+        }
+        sig1=dt2/dt1;
+        sig2=dt3/dt1;
+	cf_verbose(3, "Interpolation: %0.2f x %s, %0.2f x %s", 
+		sig1, aeff1file, sig2, aeff2file);
+    }
+    else
+	cf_verbose(3, "No interpolation.  Using Aeff file %s", aeff1file);
+	
+    /* Step through the apertures, skipping aperture 4 (pinhole) */
+    for (ap = 1; ap < 8; ap++) {
+	long jmax=0,	/* size of wave and aeff arrays */
+    	    j,		/* index through wave and aeff */
+	    k;		/* index through photon array */
+
+	double *aeff;
+	float *wavelength, dl, w0;
+	
+        if (ap == 4)
+	    continue;
+
+	if (interp == 1) {
+	    /* Interpolate the calibrated aeff. */
+	    double *aeff1, *aeff2;
+
+            FITS_movabs_hdu(aeff1fits, ap+1, NULL, &status);
+	    jmax = cf_read_col(aeff1fits, TDOUBLE, "AREA", (void **) &aeff1);
+
+            FITS_movabs_hdu(aeff2fits, ap+1, NULL, &status);
+	    jmax = cf_read_col(aeff2fits, TDOUBLE, "AREA", (void **) &aeff2);
+
+	    aeff = (double *) cf_calloc(jmax, sizeof(double));
+
+	    for (j = 0; j < jmax; j++) {
+                aeff[j] = sig1 * aeff1[j] + sig2 * aeff2[j];
+	    }
+	    free(aeff1);
+	    free(aeff2);
+	} else {
+            FITS_movabs_hdu(aeff1fits, ap+1, NULL, &status);
+	    jmax = cf_read_col(aeff1fits, TDOUBLE, "AREA", (void **) &aeff);
+	}
+
+	/* Read wavelength array in AEFF_CAL file */
+	jmax = cf_read_col(aeff1fits, TFLOAT, "WAVE", (void **) &wavelength);
+
+	/* Compute translation from wavelength to pixel within AEFF_CAL file. */
+	w0 = wavelength[0];
+	dl = (wavelength[jmax-1] - wavelength[0]) / (jmax - 1);
+
+	/* Go through the photon list */
+        for (k = 0; k < nevents; k++) {
+            if (channel[k] == ap) {
+		long j = (lambda[k] - w0) / dl + 0.5;
+		if (j >= 0L && j < jmax)
+		    ergcm2[k] = weight[k]*HC/lambda[k]/aeff[j];
+		else
+		    channel[k] = 0;
+            }
+        }
+	free(wavelength);
+	free(aeff);
+    }
+
+    /* Clean up. */
+    FITS_close_file(aeff1fits, &status);
+    if (interp == 1)
+        FITS_close_file(aeff2fits, &status);
+
+    /* Update processing flags. */
+    cf_proc_update(header, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done Processing");
+    return (status);
+}
diff --git a/src/libcf/cf_count_rate_y_distort.c b/src/libcf/cf_count_rate_y_distort.c
new file mode 100644
index 0000000..a42a4ac
--- /dev/null
+++ b/src/libcf/cf_count_rate_y_distort.c
@@ -0,0 +1,157 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_count_rate_y_distort(fitsfile *header, long nevents,
+ *                                      float *time, float *yfarf,
+ *                                      unsigned char *locflags, long nseconds,
+ *                                      float *timeline, float *fec_rate)
+ *
+ * Description: Corrects the Y position of each event based on the
+ *              instantaneous count rate.
+ *
+ * Arguments:   fitsfile  *header       Pointer to FITS file containing the
+ *                                      header of the intermediate data file
+ *              long      nevents       The number of events
+ *              float     *time         An array of event times
+ *              float     *yfarf        An array of event Y positions
+ *              unsigned char *locflags Location flags for each event
+ *              long      nseconds      The number of seconds in the timeline
+ *              float     *timeline     The timeline in seconds
+ *              float     *fec_rate     Front End Counter rate
+ *
+ * Calls:
+ *
+ * Return:      0  on success
+ *
+ * History:     08/06/02   1.1   peb    Begin work
+ *              10/27/02   1.2   peb    Added a time-dependent correction
+ *                                      which uses the Front End Counter
+ *                                      (FEC) rates.
+ *              11/11/02   1.3   peb    Removed non-time-dependent correction.
+ *                                      (Code now expects timeline extension
+ *                                      data.)
+ *              11/11/02   1.4   peb    Fixed compile error - added buffer
+ *                                      variable.
+ *              11/12/02   1.5   peb    Added check to move only events in
+ *                                      active region.
+ *		03/11/03   1.6   wvd    Changed locflags to unsigned char
+ *              05/20/03   1.7   rdr    Added call to cf_proc_check
+ *		07/29/03   1.8   wvd    If cf_proc_check fails, return errflg.
+ *		08/04/03   1.9   wvd    Convert fec_rate to type short.
+ *		11/26/03   1.10  wvd    Convert fec_rate to type float.
+ *		08/18/04   1.11  wvd    Interpolate stretch correction among
+ *					tabulated Y values.
+ *		10/06/05   1.12  wvd    For HIST data, set each element of
+ *					fec_rate to weighted mean of array.
+ *		04/07/07   1.13  wvd    Clean up compiler warnings.
+ *
+ ****************************************************************************/
+
+#include <math.h>
+#include <string.h>
+#include <stdlib.h>
+#include "calfuse.h"
+
+int
+cf_count_rate_y_distort(fitsfile *header, long nevents, float *time,
+			float *yfarf, unsigned char *locflags, long nseconds,
+			float *timeline, float *fec_rate)
+{
+    char CF_PRGM_ID[] = "cf_count_rate_y_distort";
+    char CF_VER_NUM[] = "1.13";
+    
+    char  instmode[FLEN_VALUE], ystrfile[FLEN_VALUE];
+    short xlen, ylen;
+    int   errflg=0, hdutype, status=0, anynull=0;
+    int   i, ii, i_max, rndx, yndx;
+    long  j, k;
+    float *ystretch, ystr_1d[NYMAX], flt=0.;
+    fitsfile *ystrfits;
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    if ((errflg = cf_proc_check(header, CF_PRGM_ID))) return errflg;
+
+    /*
+     *  For HIST data, replace fec_rate with weighted mean value.
+     */
+    FITS_read_key(header, TSTRING, "INSTMODE", instmode, NULL, &status);
+    if (!strncmp(instmode, "HIST", 4)) {
+	float *mean_rate, ratio, numerator=0, denominator=0;
+	mean_rate = (float *) cf_malloc(sizeof(float) * nseconds);
+	for (i = 0; i < nseconds; i++) {
+	    numerator += fec_rate[i] * fec_rate[i];
+	    denominator += fec_rate[i];
+	}
+	ratio = numerator / denominator;
+	for (i = 0; i < nseconds; i++) mean_rate[i] = ratio;
+	fec_rate = mean_rate;
+	cf_verbose(2, "Weighted mean count rate = %f", ratio);
+    }
+
+    /*
+     *  Read the rate calibration file.
+     */
+    FITS_read_key(header, TSTRING, "RATE_CAL", ystrfile, NULL, &status);
+    FITS_open_file(&ystrfits, cf_cal_file(ystrfile), READONLY, &status);
+    FITS_movabs_hdu(ystrfits, 2, &hdutype, &status);
+    FITS_read_key(ystrfits, TSHORT, "NAXIS1", &xlen, 0, &status);
+    FITS_read_key(ystrfits, TSHORT, "NAXIS2", &ylen, 0, &status);
+    ystretch = (float *) cf_malloc(sizeof(float)*xlen*ylen);
+    FITS_read_img(ystrfits, TFLOAT, 1L, xlen*ylen, &flt, ystretch, &anynull,
+		  &status);
+    FITS_close_file(ystrfits, &status);
+
+    i_max = (xlen-1) * 10;
+    for(j=k=0; j<nevents; j++) {	/* Loop through all events. */
+	/*
+	 *  Move only events in active region.
+	 */
+	if (!(locflags[j] & LOCATION_SHLD)) {
+
+	    /* If time has changed, compute a new ystretch array. */
+	    while(timeline[k]-FRAME_TOLERANCE < time[j] && k < nseconds) {
+		k++;
+
+		/* This index reflects the count rate. */
+	        rndx = (int)((log10(fec_rate[k])-1.)*10.);
+	        if (rndx < 0)
+		    rndx = 0;
+	        else if (rndx >= ylen)
+		    rndx = ylen-1;
+
+		/* 
+		 *  This index reflects Y position on the detector.
+		 *  Shift information is provided for every 10 Y pixels.
+		 *  We interpolate to the nearest Y pixel.  Otherwise,
+		 *  counts pile up at the 10-pixel boundaries.
+		 */
+		for (i = 0; i < i_max; i++) {
+		    ii = (i/10) * 10;
+		    ystr_1d[i] = ((ii+10-i) * (ystretch+rndx*xlen)[i/10] +
+				  (i - ii)  * (ystretch+rndx*xlen)[i/10+1]) / 10.;
+		}
+		for ( ; i < NYMAX; i++) 
+		    ystr_1d[i] = (ystretch+rndx*xlen)[xlen-1];
+	    }
+
+	    /* Now apply the shift. */
+	    yndx = (int) yfarf[j];
+	    if (yndx < 0)
+		yndx = 0;
+	    else if (yndx >= NYMAX)
+		yndx = NYMAX-1;
+	    yfarf[j] -= ystr_1d[yndx];
+	}
+    }
+    free(ystretch);
+    if (!strncmp(instmode, "HIST", 4)) free(fec_rate);
+
+    cf_proc_update(header, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return 0;
+}
diff --git a/src/libcf/cf_dispersion.c b/src/libcf/cf_dispersion.c
new file mode 100644
index 0000000..19a47c1
--- /dev/null
+++ b/src/libcf/cf_dispersion.c
@@ -0,0 +1,85 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Description: Assigns wavelength to each photon in data stream.  
+ *                    
+ * Returns:     0 upon successful completion.
+ *
+ * History:     05/15/06   1.1   wvd	Adapt from cf_astigmatism_and_dispersion.c
+ *					Program incorporates cf_x2lambda.
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include <math.h>
+#include "calfuse.h"
+
+static char CF_PRGM_ID[] = "cf_dispersion";
+static char CF_VER_NUM[] = "1.1";
+
+
+int
+cf_dispersion(fitsfile *infits, long nevents, float *x,
+		   unsigned char *channel, float *lambda)
+{
+    char  	wave_file[FLEN_VALUE];
+    float	*wavelength=NULL;
+    float	x_lower, x_upper, weight_l, weight_u, wave_l, wave_u;
+    int	  	ap, errflg=0, nwave, xl_int, xu_int, status=0;
+    long	k;
+    fitsfile 	*wavefits;
+
+    /* Enter a timestamp into the log. */
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    if ((errflg = cf_proc_check(infits, CF_PRGM_ID))) return errflg;
+
+    FITS_read_key(infits, TSTRING, "WAVE_CAL", wave_file, NULL, &status);
+    FITS_open_file(&wavefits, cf_cal_file(wave_file), READONLY, &status);
+
+    /* Cycle through channels, skipping #4 (pinhole) */
+    for (ap = 1; ap < 8; ap++) {
+	if (ap == 4) continue;
+
+    	FITS_movabs_hdu(wavefits, ap+1, NULL, &status);
+	nwave = cf_read_col(wavefits, TFLOAT, "WAVELENGTH", (void **) &wavelength);
+
+	/* Compute wavelength for each event by interpolation. */
+        for (k = 0; k < nevents; k++) {
+	    if (channel[k] == ap) {
+		x_lower = floor(x[k]);
+		x_upper = ceil(x[k]);
+		xl_int	= (int) (x_lower + 0.5);
+		xu_int	= (int) (x_upper + 0.5);
+		if (xl_int >= 0 && xu_int < nwave) {
+		    if (xl_int == xu_int)
+			lambda[k] = wavelength[xl_int];
+		    else {
+		        weight_l = x_upper - x[k];
+		        weight_u = x[k] - x_lower;
+		        wave_l = wavelength[xl_int];
+		        wave_u = wavelength[xu_int];
+		        lambda[k] = wave_l * weight_l + wave_u * weight_u;
+		    }
+		}
+		else
+		    channel[k] = 0;
+	    }
+	}
+        /* Space for wavelength array is allocated in each loop. */
+	free(wavelength);
+    }
+    FITS_close_file(wavefits, &status);
+
+    /* Update processing flags. */
+    cf_proc_update(infits, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done Processing");
+
+    return status;
+}
diff --git a/src/libcf/cf_doppler_and_heliocentric.c b/src/libcf/cf_doppler_and_heliocentric.c
new file mode 100644
index 0000000..f95672d
--- /dev/null
+++ b/src/libcf/cf_doppler_and_heliocentric.c
@@ -0,0 +1,87 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:	cf_doppler_and_heliocentric(*infits, nevents, *photon_time, 
+ *		  	*channel, *lambda, nseconds, *timeline_time, 
+ *			*timeline_velocity);
+ *
+ * Description: Doppler-correct each photon for both heliocentric and orbital
+ *		motions.  Resulting wavelength scale is heliocentric.
+ *
+ * Arguments:	*infits			Input FITS file pointer
+ * 		nevents			number of points in the photon list
+ * 		*photon_time		time array of photon events
+ * 		*channel		channel number in the photon list
+ * 		*lambda			wavelength in the photon list
+ * 		nseconds		number of points in the timeline table
+ * 		*timeline_time		time array of timeline list
+ * 		*timeline_velocity	orbital velocity in km/s
+ *
+ * Returns:	O upon successful completion
+ *
+ * History:     12/09/2002   jch   1.1	Initial coding
+ *	        12/11/2002   wvd   1.2	Move Doppler calculation to separate
+ *					  loop.
+ *              12/11/2002   wvd   1.3  Change nevents and nseconds to long.
+ *              12/20/2002   wvd   1.4  Change channel to unsigned char.
+ *              02/24/03     peb   1.5  Change include file to calfusettag.h
+ *                                      and calfitsio.h
+ *              03/11/2003   wvd   1.6  Change channel to char.
+ *              05/20/2003   rdr   1.7  Added call to cf_proc_check
+ *              09/17/2003   wvd   1.8  Return errflg from cf_prock_check
+ *              10/21/2003   wvd   1.9  Change channel to unsigned char.
+ *              04/21/2004   bjg   1.10 Cosmetic change to prevent warning
+ *                                      with gcc -Wall
+ *              11/17/2005   wvd   1.11 Change velocity and doppler to doubles.
+ *
+ ****************************************************************************/
+
+#include <stdlib.h>
+#include "calfuse.h"
+
+char CF_PRGM_ID[] = "cf_doppler_and_heliocentric";
+char CF_VER_NUM[] = "1.11";
+
+
+int cf_doppler_and_heliocentric(fitsfile *infits, long nevents,
+	float *photon_time, unsigned char *channel, float *lambda,
+	long nseconds, float *timeline_time, float *timeline_velocity)
+{
+	int	errflg=0, status=0;
+	long	i, k;
+	float	v_helio;	/* heliocentric velocity in km/sec */
+	double	velocity, *doppler;
+
+	/* Enter a timestamp into the log. */
+    	cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+    	cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+        if ((errflg = cf_proc_check(infits, CF_PRGM_ID) )) return errflg;
+
+	FITS_read_key(infits, TFLOAT, "V_HELIO", &v_helio, NULL, &status);
+
+	/* Compute array of Doppler corrections. */
+	doppler = (double *) cf_malloc(sizeof(double) * nseconds);
+	for (k = 0; k < nseconds; k++) {
+		velocity = timeline_velocity[k] + v_helio;
+		doppler[k] = 1. + velocity / C;
+	}
+
+	/* Apply Doppler correction to each photon assigned to an aperture. */
+	k = 0;
+	for (i = 0; i < nevents; i++)
+	    if (channel[i] > 0) {
+	        while (photon_time[i] > timeline_time[k+1] - FRAME_TOLERANCE
+		    && k < nseconds-1) k++;
+	        lambda[i] *= doppler[k];
+	    }
+	free (doppler);
+
+	/* Update processing flags. */
+    	cf_proc_update(infits, CF_PRGM_ID, "COMPLETE");
+    	cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done Processing");
+    	return (status);
+}
diff --git a/src/libcf/cf_electronics_dead_time.c b/src/libcf/cf_electronics_dead_time.c
new file mode 100644
index 0000000..38c2219
--- /dev/null
+++ b/src/libcf/cf_electronics_dead_time.c
@@ -0,0 +1,104 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_electronics_dead_time(fitsfile *header, long nseconds,
+ *                                      float *fec_rate, float *elec_dtc)
+ *
+ * Description: Scales the weighting factor to correct for the electronics
+ *              dead time.
+ *
+ * Arguments:   fitsfile  *header       Pointer to FITS file containing the
+ *                                      header of the intermediate data file
+ *              long      nseconds      The number of timeline values
+ *              float     *fec_rate     An array of Front End Counter (FEC)
+ *                                      rates
+ *              float     *elec_dtc     Dead-time correction array (returned)
+ * Calls:
+ *
+ * Return:      0  on success
+ *
+ * History:     10/27/02   1.1    peb   Begin work
+ *              11/11/02   1.2    peb   Corrected function description and
+ *                                      added cf_timestamp after ELEC_COR
+ *                                      check.
+ *		12/06/02   1.4    wvd   Calculate DT correction for each time
+ *					step, then apply to photons.
+ *					Set keyword DET_DEAD.
+ *              05/20/03   1.5    rdr   Added proc_check call
+ *              08/01/03   1.7    wvd   Just calculate correction; don't
+ *                                      apply it.  Return elec_dtc array.
+ *              08/04/03   1.8    wvd   Convert fec_rate to type short.
+ *              11/26/03   1.9    wvd   Change fec_rate to type float.
+ *              02/12/04   1.10   wvd   In verbose mode, write mean DTC.
+ *              04/07/07   1.11   wvd   Clean up compiler warnings.
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include <math.h>
+#include "calfuse.h"
+
+int
+cf_electronics_dead_time(fitsfile *header, long nseconds, 
+			 float *fec_rate, float *elec_dtc)
+{
+    char CF_PRGM_ID[] = "cf_electronics_dead_time";
+    char CF_VER_NUM[] = "1.11";
+
+    char  elecfile[FLEN_VALUE]={"\0"}, detector[FLEN_VALUE]={"\0"};
+    char  keyword[FLEN_KEYWORD]={"\0"};
+    int   errflg=0, status=0;
+    long  k;
+    float abort, clock, state;
+    float mean_elec_dtc = 0.;
+    fitsfile *elecfits;
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    if ((errflg = cf_proc_check(header, CF_PRGM_ID))) return errflg;
+
+    FITS_read_key(header, TSTRING, "DETECTOR", detector, NULL, &status);
+    /*
+     *  Get the electronics dead-time constants.
+     */
+    FITS_read_key(header, TSTRING, "ELEC_CAL", elecfile, NULL, &status);
+    FITS_open_file(&elecfits, cf_cal_file(elecfile), READONLY, &status);
+    sprintf(keyword, "ABORT_%s", detector);
+    FITS_read_key(elecfits, TFLOAT, keyword, &abort, NULL, &status);
+    sprintf(keyword, "CLOCK_%s", detector);
+    FITS_read_key(elecfits, TFLOAT, keyword, &clock, NULL, &status);
+    sprintf(keyword, "STATE_%s", detector);
+    FITS_read_key(elecfits, TFLOAT, keyword, &state, NULL, &status);
+    FITS_close_file(elecfits, &status);
+    /*
+     *  Calculate dead-time correction.
+     */
+    for (k=0; k<nseconds; k++) {
+        float xa, x, x2, x4, x6, x10;
+
+        xa = exp(-fec_rate[k]*abort);
+        x  = exp(-fec_rate[k]*clock);
+        x2 = x*x;
+        x4 = x2*x2;
+        x6 = x4*x2;
+        x10 = x6*x4;
+
+        elec_dtc[k] = (1. + fec_rate[k]*state + 4.*(x2-x) + x6 - x10)/xa;
+        if (elec_dtc[k] < 1.0) elec_dtc[k] = 1.0;
+	mean_elec_dtc += elec_dtc[k];
+    }
+    /*
+     *  Calculate mean dead-time correction.  Write to file header.
+     */
+    mean_elec_dtc /= nseconds;
+    cf_verbose(2, "Mean detector electronics dead-time correction: %f", mean_elec_dtc);
+    FITS_update_key(header, TFLOAT, "DET_DEAD", &mean_elec_dtc, NULL, &status);
+
+    cf_proc_update(header, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return 0;
+}
diff --git a/src/libcf/cf_error_msg.c b/src/libcf/cf_error_msg.c
new file mode 100644
index 0000000..12fb7e5
--- /dev/null
+++ b/src/libcf/cf_error_msg.c
@@ -0,0 +1,263 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_error_init(char *prgmid, char *vernum, FILE *errfile)
+ *
+ * Description: Writes a timestamp, the calling program name, and an
+ *		error message to stdout for a cfitsio routine.
+ *
+ * Arguments:   char    *progid         Name of the calling program
+ *              char    *vernum         Version of the calling program
+ *                                      (should be version control number)
+ *              FILE    *errfile        Output file name (default is stderr)
+ *
+ * Returns:     none
+ *
+ * History:     02/22/99        peb     Some simple functions to make error
+ *                                      reporting easier.  Deficiencies in
+ *                                      cfitsio make printing comprehensive
+ *                                      messages difficult.
+ *              03/15/99        emm     Added cf_if_memory_error.
+ *              04/30/99        peb     Added cf_malloc and cf_calloc.
+ *              06/07/99        peb     Added reporting of version number 
+ *              09/01/99        emm     Added fflush to see if it helps print
+ *                                      out error messages on failure.
+ *              11/08/99        emm     Added !!!!!!!! to error reporting to
+ *                                      better delimit the error message and
+ *                                      to make them more obvious.
+ *              04/23/01  1.10  wvd     Make cf_malloc & cf_calloc print error
+ *					message returned by malloc & calloc
+ *              03/07/03  1.2   peb     Added cf_verbose and external variable
+ *                                      verbose_level
+ *              03/13/03  1.3   peb     Enabled cf_verbose, cf_if_warning, and
+ *                                      cf_if_error to accept a variable
+ *                                      number of parameters.  Changed the
+ *                                      output format to print month, day, time
+ *                                      hostname, function name and message.
+ *              03/25/03  1.4   peb     Changed output to print time, program,
+ *                                      and version number for warning and
+ *                                      error messages.
+ *                                      Changed output to use verbose_level
+ *                                      to modify output format:
+ *                                      level==1 prints program, version, and
+ *                                      message.
+ *                                      level>=2 prints only message.
+ *              10/30/03  1.5   peb     Replaced cftime function with strftime
+ *                                      for UNIX compatibility.
+ *                                      Removed unnecessary header files,
+ *                                      malloc.h and unistd.h
+ *              04/07/04  1.6   bjg     fflush stdout and error_file
+ *
+ ****************************************************************************/
+
+#include <errno.h>
+#include <stdarg.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include <string.h>
+#include <time.h>
+#include "fitsio.h"
+
+#define  N_STYM  40
+
+int   verbose_level=0;
+
+static char *program_name=NULL;
+static char *version_no=NULL;
+static FILE *error_file=NULL;
+
+void cf_error_init(const char *progid, const char *vernum, FILE *errfile)
+{
+    static char unknown[] = "unknown file";
+    static char version[] = "1.6";
+    if (progid) {
+        program_name = malloc(strlen(progid)+1);
+        strcpy(program_name, progid);
+    }
+    else {
+        program_name = malloc(strlen(unknown)+1);
+        strcpy(program_name, unknown);
+    }
+    if (vernum) {
+        version_no = malloc(strlen(vernum)+1);
+	strcpy(version_no, vernum);
+    }
+    else {
+        version_no = malloc(strlen(version)+1);
+	strcpy(version_no, version);
+    }
+    if (errfile)
+        error_file = errfile;
+    else
+        error_file = stderr;
+}
+
+void cf_verbose(int level, const char *format, ...)
+{
+    va_list args;
+    va_start(args, format);
+
+    if (verbose_level >= level) {
+	if (level == 1)
+	    printf("   %s-%s: ", program_name, version_no);
+	else if (level >= 2)
+	    printf("\t");
+	vprintf(format, args);
+	printf("\n");
+	fflush(stdout);
+    }
+
+    va_end(args);
+}
+
+void cf_if_warning(char *format, ...)
+{
+    char stym[N_STYM]={'\0'};
+    time_t tym;
+    va_list args;
+
+    va_start(args, format);
+    time(&tym);
+    strftime(stym, N_STYM, "%Y %b %e %T", localtime(&tym));
+
+    fprintf(error_file, "%s %s-%s: WARNING - ",
+	    stym, program_name, version_no);
+    vfprintf(error_file, format, args);
+    fprintf(error_file, "\n");
+    fflush(error_file);
+    va_end(args);
+}
+
+void cf_if_error(char *format, ...)
+{
+    char stym[N_STYM]={'\0'};
+    time_t tym;
+    va_list args;
+
+    va_start(args, format);
+    time(&tym);
+    strftime(stym, N_STYM, "%Y %b %e %T", localtime(&tym));
+
+    fprintf(error_file, "%s %s-%s: ERROR - ",
+	    stym, program_name, version_no);
+    vfprintf(error_file, format, args);
+    fprintf(error_file, "\n");
+
+    fflush(error_file);
+    va_end(args);
+    exit(1);
+}
+
+void cf_if_fits_warning(int status)
+{
+    if (status) {
+	char stym[N_STYM]={'\0'};
+	time_t tym;
+
+	time(&tym);
+	strftime(stym, N_STYM, "%Y %b %e %T", localtime(&tym));
+
+	fprintf(error_file, "%s %s-%s: FITS WARNING - ",
+		stym, program_name, version_no);
+        fits_report_error(error_file, status);
+        fflush(error_file);
+    }
+}
+
+void cf_if_fits_error(int status)
+{
+    if (status) {
+	char stym[N_STYM]={'\0'};
+	time_t tym;
+
+	time(&tym);
+	strftime(stym, N_STYM, "%Y %b %e %T", localtime(&tym));
+
+	fprintf(error_file, "%s %s-%s: FITS ERROR - ",
+		stym, program_name, version_no);
+        fits_report_error(error_file, status);
+        fflush(error_file);
+        exit(1);
+    }
+}
+
+void *cf_malloc(size_t size)
+{
+    void *ptr;
+
+    if (!(ptr = malloc(size))) {
+	char stym[N_STYM]={'\0'};
+	time_t tym;
+
+	time(&tym);
+	strftime(stym, N_STYM, "%Y %b %e %T", localtime(&tym));
+
+	fprintf(error_file, "%s %s-%s: ERROR - %s\n",
+		stym, "cf_malloc", "1.0", strerror(errno));
+
+        fflush(error_file);
+	exit(1);
+	/*
+	fprintf(error_file,
+		"     \n     malloc: Attemping to allocate %d bytes", size);
+	*/
+    }
+    return ptr;
+}
+
+void *cf_calloc(size_t nelem, size_t elsize)
+{
+    void *ptr;
+
+    if (!(ptr = calloc(nelem, elsize))) {
+	char stym[N_STYM]={'\0'};
+	time_t tym;
+
+	time(&tym);
+	strftime(stym, N_STYM, "%Y %b %e %T", localtime(&tym));
+
+	fprintf(error_file, "%s %s-%s: ERROR - %s\n",
+		stym, "cf_calloc", "1.0", strerror(errno));
+
+        fflush(error_file);
+	exit(1);
+	/*
+	fprintf(error_file,
+		"     \n     calloc: Attemping to allocate %d bytes",
+				nelem * elsize);
+	*/
+    }
+    return ptr;
+}
+
+void cf_if_memory_error(int status)
+{
+    time_t tym;
+
+    if (!status) {
+        time(&tym);
+        fprintf(error_file, "Memory allocation error in %s-%s: %s",
+                program_name, version_no, ctime(&tym));
+
+        /* Print out cfitsio error messages and continue */
+
+        fits_report_error(error_file, status);
+	fflush(error_file);
+    }
+}
+
+/*
+int main()
+{
+    int i;
+    cf_error_init("test program", "1.0", stdout);
+    cf_if_warning("Non-fatal error occurred");
+
+    for (i=0; i < 10; i++)
+        cf_if_fits_warning(i);
+    exit(0);
+}
+*/
diff --git a/src/libcf/cf_extraction_limits.c b/src/libcf/cf_extraction_limits.c
new file mode 100644
index 0000000..5567d14
--- /dev/null
+++ b/src/libcf/cf_extraction_limits.c
@@ -0,0 +1,137 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE 
+ *****************************************************************************
+ *
+ * Synopsis:    cf_extraction_limits(fitsfile *infits, int aperture,
+ *		int srctype, short **ylow, short **yhigh, short *xmin,
+ *		short *xmax)
+ *
+ * Description: Read the extraction limits for a given aperture and source
+ *		type (point or extended) from the CHID_CAL file.  Shift these
+ *		limits to match the centroid of the observed spectrum, if
+ *		that measurement has been performed.  For point sources
+ *		observed in HIST mode, pad YLOW and YHIGH by SPECBINY pixels.
+ *
+ * Arguments:   fitsfile  *infits       Pointer to the location of the FITS
+ *                                      header of the Intermediate Data File
+ *              int       aperture	aperture designation (1 through 8)
+ *		int	  srctype	0 = point source, 1 = extended
+ *              short     **ylow	lower Y bound for the extraction window
+ *              short     **yhigh	upper Y bound for the extraction window
+ *              short     *xmin 	lower X bound for the extraction window
+ *              short     *xmax  	upper X bound for the extraction window
+ *
+ * Calls:       None
+ *
+ * Return:      npts = length of arrays ylow and yhigh
+ *
+ * History:     08/22/03    1.1  BJG    Based on subroutine from v1.6 of
+ *					cf_bad_pixels.c by RDR.
+ *					Change coltype from char to int in
+ *					cf_read_col.
+ *		03/15/05    1.2  wvd	Read HIST_PAD from appropriate HDU
+ *					of CHID_CAL file and pad apertures
+ *					if data are in HIST mode.
+ *		03/16/05    1.3  wvd	For extended sources, return large
+ *					apertures.
+ *		10/06/05    1.4  wvd	Always pad apertures by 8 pixels
+ *					in HIST mode.
+ *		05/03/06    1.5  wvd	Always pad apertures by SPECBINY
+ *					pixels in HIST mode.
+ *
+ ****************************************************************************/
+
+#include <stdio.h>
+#include <stdlib.h>
+#include <string.h>
+#include "calfuse.h"
+
+long cf_extraction_limits(fitsfile *infits, int aperture, int srctype,
+	short **ylow, short **yhigh, short *xmin, short *xmax) { 
+
+    char CF_PRGM_ID[] = "cf_extraction_limits"; 
+    char CF_VER_NUM[] = "1.5";
+
+    fitsfile *chidfits ;
+    int status=0, hdutype;
+    int dcent, hdu ; 
+    short histpad=0, specbiny;
+    short xmint, xmaxt, *ylowt=NULL, *yhight=NULL;
+    float ycent_data, ycent_tab ;
+    long j, npts ;
+    char ycentname[FLEN_VALUE]={'\0'}, chidfile[FLEN_VALUE] ;
+    char instmode[FLEN_VALUE];
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    /* Read the measured centroid from the input file header. */
+    FITS_movabs_hdu(infits, 1, &hdutype, &status) ;
+    sprintf(ycentname,"YCENT%1d",aperture) ;
+    FITS_read_key(infits, TFLOAT, ycentname, &ycent_data, NULL, &status);
+    cf_verbose(3, "Reading extraction limits for aperture %d ", aperture) ;
+    cf_verbose(3, "ycent keyword = %s, value=%5.1f ", ycentname, ycent_data) ;
+
+    /* Read instrument mode and binning factor from file header. */
+    FITS_read_key(infits, TSTRING, "INSTMODE", instmode, NULL, &status);
+    FITS_read_key(infits, TSHORT, "SPECBINY", &specbiny, NULL, &status);
+
+    /* Which HDU to read depends on both channel and source type. */
+    hdu = aperture + 1;
+    if (srctype) hdu += 8;
+
+    /* Open the CHID_CAL file. */
+    FITS_read_key(infits, TSTRING, "CHID_CAL", chidfile, NULL, &status);
+    cf_verbose(3, "spectral extraction file = %s, HDU = %d", chidfile, hdu);
+    FITS_open_file(&chidfits, cf_cal_file(chidfile), READONLY, &status);
+    FITS_movabs_hdu(chidfits, hdu, &hdutype, &status);
+
+    /* Read X limits of extraction window. */
+    FITS_read_key(chidfits, TSHORT, "XMIN", &xmint, NULL, &status);
+    FITS_read_key(chidfits, TSHORT, "XMAX", &xmaxt, NULL, &status);
+
+    /* Read centroid of tabulated extraction window. */
+    FITS_read_key(chidfits,TFLOAT,"CENTROID",&ycent_tab,NULL,&status);
+
+    /* For point-source data taken in HIST mode, pad window. */
+    if ((!strncmp(instmode, "HIST", 4)) && !srctype) histpad = specbiny;
+	/* FITS_read_key(chidfits,TSHORT,"HIST_PAD",&histpad,NULL,&status); */
+
+    /* Read the upper and lower boundaries of the extraction slit. */
+    npts=cf_read_col(chidfits, TSHORT, "YLOW",  (void **) &ylowt);
+    npts=cf_read_col(chidfits, TSHORT, "YHIGH", (void **) &yhight);
+    FITS_close_file(chidfits, &status) ;
+
+    /* If the spectral centroid has been measured, shift the aperture
+       limits so that the tabulated centroid equals the measured value. */
+    if (ycent_data > 1 && ycent_data < NYMAX) {
+	dcent = (short) cf_nint(ycent_data - ycent_tab) ;
+        cf_verbose(3, "shifting extraction window: ycent_tab=%5.1f, delta=%d",
+            ycent_tab, dcent) ;
+        for (j = xmint; j <= xmaxt; j++) {
+	    ylowt[j]  += dcent ;
+            yhight[j] += dcent ; 
+	}
+    }
+
+    /* If HIST_PAD > 0, pad the extraction window, top and bottom. */
+    if (histpad > 0) {
+        cf_verbose(3, "HIST point source.  "
+	    "Padding extraction window by +/- %d pixels", histpad);
+        for (j = xmint; j <= xmaxt; j++) {
+	    ylowt[j]  -= histpad ;
+	    yhight[j] += histpad ; 
+	}
+    }
+
+    /* Return the extraction limits. */
+    *xmin = xmint;
+    *xmax = xmaxt;
+    *ylow = ylowt ;
+    *yhigh = yhight ;
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return npts ;
+}
diff --git a/src/libcf/cf_fes_proc_check.c b/src/libcf/cf_fes_proc_check.c
new file mode 100644
index 0000000..74a41b4
--- /dev/null
+++ b/src/libcf/cf_fes_proc_check.c
@@ -0,0 +1,94 @@
+/******************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ ******************************************************************************
+ *
+ * Synopsis:    cf_fes_proc_check(fitsfile *fptr, char *prog_id)
+ *
+ * Description: cf_fes_proc_check will determine if a given calibration
+ *              step is to be performed on the data.  It will also
+ *              determine whether all previous steps have been
+ *              completed successfully.
+ *
+ * Arguments:   fitsfile    *fptr	Pointer to input file
+ *              char        *prog_id 	Procedure name
+ *
+ * History:     06/21/98        emm     Begin work.
+ *		08/19/2004 1.1	wvd	Move to v3.0, add CF_VER_NUM,
+ *					change cf_errmsg to cf_if_error.
+ *		09/07/2007 1.2	bot	Removed unused CF_VER_NUM and CF_PRGM_ID
+ *
+ *****************************************************************************/
+
+#include <stdio.h>
+#include <string.h>
+#include "calfuse.h"
+#define  MAXCHARS 120
+
+int cf_fes_proc_check(fitsfile *fptr, char *prog_id) 
+{
+    int   i,j, status=0;
+    char  comment[FLEN_CARD], key_value[FLEN_CARD];
+    char  complete[19], skipped[19], perform[19];
+
+    /*
+     *  The calfuse.h file contains the definitions of fes_keyword_tab
+     *  NUM_PROC_STEPS, and CALIBRATION_STEP_KEYS.
+     */
+    struct fes_keyword_tab keytab[NUM_FES_PROC_STEPS]=FES_CALIBRATION_STEP_KEYS;
+    status=0;
+
+    strncpy(complete,"COMPLETE          ",19);
+    strncpy(skipped, "SKIPPED           ",19);
+    strncpy(perform, "PERFORM           ",19);
+
+    j=0;
+    /*
+     *  First, determine if this procedure is even supposed to be
+     *  run on this data.
+     */
+    while ((strncmp(keytab[j].proc,prog_id, strlen(keytab[j].proc)) != 0) &&
+	   (j < NUM_FES_PROC_STEPS)) j++;
+    if ((j >= NUM_FES_PROC_STEPS) || 
+	(strncmp(keytab[j].value,perform,7))) {
+	cf_if_error("Processing step does not "
+		  "need to be run on this type of data.");
+	fprintf(stderr,"     Step %18.18s does not need "
+		"to be run.\n",prog_id);
+	return 1;
+    }
+
+    status=0;
+    fits_read_key_str(fptr, keytab[j].name, key_value, comment, 
+		      &status);
+
+    /* Now check to see if the step has already been completed. */
+    if (strncmp(key_value,complete,7)==0) {
+	cf_if_error("Processing step has already been completed.\n");
+	fprintf(stderr,"     Step %18.18s does not need to be run.\n",
+		prog_id);
+	return 1;
+    }
+
+    /*  Now determine if the previous programs are all complete. */
+    for (i=0; i<j; i++) {
+	fits_read_key_str(fptr, keytab[i].name, key_value, comment, 
+			  &status);
+	if (strncmp(keytab[i].value,perform,7)==0) {
+	    if (strncmp(key_value,complete,8) &&
+		strncmp(key_value,skipped,7)) {
+		cf_if_error("Processing step not completed.");
+		fprintf(stderr,"     Step %8.8s has value "
+			"%8.8s.\n",keytab[i].name,key_value);
+		fprintf(stderr,"     It should be either "
+			"COMPLETE or SKIPPED before running "
+			"%18.18s\n",prog_id);
+		return 1;
+	    } /* End if check on key_value */
+	} /* End check on keytab[i].value */
+    } /* End for */
+   
+    /* If we got to here, it must be OK */
+    return 0;
+}
diff --git a/src/libcf/cf_fes_proc_update.c b/src/libcf/cf_fes_proc_update.c
new file mode 100644
index 0000000..14f1f78
--- /dev/null
+++ b/src/libcf/cf_fes_proc_update.c
@@ -0,0 +1,68 @@
+/******************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ ******************************************************************************
+ *
+ * Synopsis:    cf_fes_proc_update(fitsfile *fptr, char *prgm_id, 
+ *                                 char *key_value)
+ *
+ * Description: cf_fes_proc_update will update the FITS header keyword 
+ *              which corresponds to the given prgm_id in the file 
+ *              fptr to the value given in key_value.
+ *
+ * Arguments:   fitsfile    *fptr	Pointer to input file
+ *              char        *prgm_id 	Procedure name
+ *              char        *key_value 	Updated procedure status
+ *
+ * History:     07/21/98        emm     Begin work.
+ *              08/19/2004 1.1  wvd     Move to v3.0, add CF_VER_NUM,
+ *                                      change cf_errmsg to cf_if_error.
+ *					Delete fits_print_err.
+ *		09/07/2007 1.2	bot	Removed unused CF_VER_NUM and CF_PRGM_ID
+ *
+ *****************************************************************************/
+
+#include <stdio.h>
+#include <string.h>
+#include "calfuse.h"
+
+int cf_fes_proc_update(fitsfile *fptr, char *prgm_id, char *key_value) 
+{
+    int i=0, status=0;
+    /*
+     *  The calfuse.h file contains the definitions of fes_keyword_tab
+     *  NUM_FES_PROC_STEPS, and FES_CALIBRATION_STEP_KEYS.
+     */
+    struct fes_keyword_tab keytab[NUM_FES_PROC_STEPS]=FES_CALIBRATION_STEP_KEYS;
+    /*
+     *  Find the keyword associated with prgm_id by looping 
+     *  through keytab[i].proc
+     */
+    while ((strncmp(keytab[i].proc,prgm_id, strlen(keytab[i].proc)) != 0) &&
+	   (i < NUM_FES_PROC_STEPS)) i++;
+    if (i < NUM_FES_PROC_STEPS) {
+	/*
+	 *  We found a match to prgm_id, so change the associated
+	 *  keyword in the header.
+	 */
+	fits_modify_key_str(fptr,keytab[i].name,key_value,
+			    "&",&status);
+	if (status) {
+	    cf_if_error("Error updating keyword");
+	    return status;
+	}
+    }
+    else {
+	/*
+	 *  The given prgm_id did not match any of the known
+	 *  keytab[i].hist_proc, so return 1.
+	 */
+	cf_if_error("Program ID does not apply to this"
+		  "type of file, could not update");
+	fprintf(stderr,"Failed to update program id:%20.20s\n",
+		    prgm_id);
+	return 1;
+    }
+    return status;
+}
diff --git a/src/libcf/cf_fifo_dead_time.c b/src/libcf/cf_fifo_dead_time.c
new file mode 100644
index 0000000..67ac065
--- /dev/null
+++ b/src/libcf/cf_fifo_dead_time.c
@@ -0,0 +1,164 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_fifo_dead_time(fitsfile *header, long nevents,
+ *		float *ptime, long nseconds, float *ttime, float *aic_rate,
+ *		float *ids_dtc)
+ *
+ * Description: Searches high-count-rate observations for data drop-outs
+ *		due to FIFO overflows.  If found, calculates time-dependent
+ *		scale factor to correct for lost photon events.
+ *
+ * Arguments:   fitsfile  *header       Pointer to FITS file containing the
+ *                                      header of the intermediate data file
+ *              long      nevents       Number of photon events in the file
+ *              float     *ptime        Detection time for each photon
+ *              long      nseconds      The number of timeline values
+ *              float     *ttime        Tabulated times in the timeline
+ *              float     *aic_rate     Active Image Counter array
+ *              float     *ids_dtc      IDS dead-time correction array
+ *					(modified)
+ *
+ * Calls:
+ *
+ * Return:      0  on success
+ *
+ * History of cf_screen_fifo_overflow:
+ *
+ *		02/10/04   1.1    wvd   Begin work
+ *              02/17/05   1.2    wvd   Place parentheses around assignment
+ *                                      used as truth value.
+ *              11/09/05   1.3    wvd   In the current scheme, the rate_lif
+ *					and rate_sic arrays contain values
+ *					from the housekeeping file and do
+ *					not reflect data loss due to FIFO
+ *					overflows.  Now we calculate the
+ *					count-rate array directly from the
+ *					photon time array.
+ *              02/23/06   1.4    wvd   Change length of data_rate array
+ *					from nevents to nseconds.
+ *
+ * History:	12/29/06   1.1    wvd	Derived from cf_screen_fifo_overflow.
+ *              01/15/07   1.2    wvd   When count rate is zero, correct one
+ *					second before to two seconds after.
+ *              02/08/07   1.3    wvd   If TTPERIOD = 0, set it to 1.
+ *              04/07/07   1.4    wvd   Clean up compiler warnings.
+ *
+ ****************************************************************************/
+
+#include <stdlib.h>
+#include "calfuse.h"
+
+int
+compute_count_rate(long nevents, float *ptime, long nseconds,
+    float *ttime, long **data_rate)
+{
+    float delta_max = 1.0 + FRAME_TOLERANCE;
+    long j,k;
+
+    *data_rate = (long *) cf_calloc(nseconds, sizeof(long));
+    for (j=k=0; j<nevents; j++) {
+        while(ttime[k+1]-FRAME_TOLERANCE < ptime[j] && k+1 < nseconds) k++;
+        if ((ptime[j] - ttime[k]) < delta_max) (*data_rate)[k]++;
+    }
+    return 0;
+}
+
+int
+cf_fifo_dead_time(fitsfile *header, long nevents, float *ptime,
+    long nseconds, float *ttime, float *aic_rate, float *ids_dtc)
+{
+    char CF_PRGM_ID[] = "cf_fifo_dead_time";
+    char CF_VER_NUM[] = "1.4";
+
+    char elecfile[FLEN_VALUE];
+    int  errflg=0, status=0;
+    int  fifo_drain_rate;
+    int  *flag_array, found_drop_out = FALSE;
+    long *data_rate, k;
+    float mean_ids_rate, ttperiod;
+    float mean_ids_dtc;
+    fitsfile *elecfits;
+
+    /* Exit if data were obtained in HIST mode. */
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+    if ((errflg = cf_proc_check(header, CF_PRGM_ID))) return errflg;
+
+    /* Read IDS drain rate from calibration file. */
+    FITS_read_key(header, TSTRING, "ELEC_CAL", elecfile, NULL, &status);
+    FITS_open_file(&elecfits, cf_cal_file(elecfile), READONLY, &status);
+    FITS_read_key(elecfits, TINT, "FIFO_DRN", &fifo_drain_rate, NULL, &status);
+    FITS_close_file(elecfits, &status);
+    cf_verbose(4, "fifo_drain_rate = %d", fifo_drain_rate);
+
+    /* Read interval between time stamps. */
+    FITS_read_key(header, TFLOAT, "TTPERIOD", &ttperiod, NULL, &status);
+    if (ttperiod < 1E-6) ttperiod = 1.0;
+
+    /* Compute mean IDS count rate. */
+    mean_ids_rate = 0.;
+    for (k=0; k<nseconds; k++) 
+        mean_ids_rate += aic_rate[k];
+    mean_ids_rate /= nseconds;
+    mean_ids_rate += 1./ttperiod;
+    cf_verbose(4, "mean_ids_rate = %f", mean_ids_rate);
+
+    /* If mean IDS count rate > 3200, look for data drop-outs. */
+    if (mean_ids_rate > 3200 && nseconds > 4) {
+	compute_count_rate(nevents, ptime, nseconds, ttime, &data_rate);
+	flag_array = (int *) cf_calloc(nseconds, sizeof(int));
+
+        /* If count rate goes to zero, set flag_array.  Where possible,
+	   set flags from one second before to two seconds after. */
+	for (k=0; k<1; k++) if (data_rate[k] == 0) 
+	    flag_array[k] = flag_array[k+1] = flag_array[k+2] = TRUE;
+
+	for ( ; k<nseconds-2; k++) if (data_rate[k] == 0) 
+	    flag_array[k-1] = flag_array[k] = flag_array[k+1] = 
+		flag_array[k+2] = TRUE;
+
+	for ( ; k<nseconds-1; k++) if (data_rate[k] == 0) 
+	    flag_array[k-1] = flag_array[k] = flag_array[k+1] = TRUE;
+
+	for ( ; k<nseconds; k++) if (data_rate[k] == 0) 
+	    flag_array[k-1] = flag_array[k] = TRUE;
+
+	for (k=0; k<nseconds; k++) if (data_rate[k] == 0) {
+	   found_drop_out = TRUE;
+	   break;
+	}
+
+	/* If there are any drop-outs, modify IDS dead-time correction. */
+	if (found_drop_out)
+	     for ( ; k < nseconds; k++) if (flag_array[k])
+		ids_dtc[k] = (aic_rate[k] - 1./ttperiod) / fifo_drain_rate;
+
+	free(data_rate);
+	free(flag_array);
+    }
+
+    /*
+     *  Calculate mean dead-time correction.  Write to file header.
+     */
+    if (found_drop_out) {
+	mean_ids_dtc = 0;
+	for (k = 0; k < nseconds; k++) mean_ids_dtc += ids_dtc[k];
+	mean_ids_dtc /= nseconds;
+	cf_verbose(1, "IDS FIFO overflow detected.");
+        cf_verbose(2, "Modified mean IDS dead-time correction: %f",
+	    mean_ids_dtc);
+        FITS_update_key(header, TFLOAT, "IDS_DEAD", &mean_ids_dtc, NULL,
+	    &status);
+    }
+
+    /*
+     *  Clean up and go home.
+     */
+    cf_proc_update(header, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return 0;
+}
diff --git a/src/libcf/cf_find_spectra.c b/src/libcf/cf_find_spectra.c
new file mode 100644
index 0000000..412a1e4
--- /dev/null
+++ b/src/libcf/cf_find_spectra.c
@@ -0,0 +1,396 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE 
+ *****************************************************************************
+ *
+ * Synopsis:    cf_find_spectra(fitsfile *header, long nevents,
+ *		float *weight, float, *xfarf, float *yfarf, char *chan,
+ *		unsigned char *timeflags, unsigned char *locflags,
+ *		int airglow_centroid)
+ *
+ * Description: Determines the spectral centroid for each aperture.
+ *		First, we compute the airglow centroid for the LWRS
+ *		aperture and determine its offset relative to the
+ *		tabulated value.  For the MDRS and HIRS apertures, we
+ *		apply this offset to the tabulated centroid to get the
+ *		airglow centroid.  For each aperture, we search for a
+ *		target spectrum in a narrow range around the airglow
+ *		centroid.  If we find it, we use it; otherwise, we use
+ *		the airglow centroid.  If airglow_centroid = TRUE, use
+ *		airglow centroid for the target spectrum.
+ *
+ *
+ * Arguments:   fitsfile  *header       Pointer to the location of the FITS
+ *                                      header of the Intermediate Data File
+ *              long      nevents       Number of photons in the file
+ *              float     *weight       scale factor for each photon event
+ *              float     *xfarf        X position of each photon event
+ *              float     *yfarf        Y position of each photon event
+ *          unsigned char *chan         Pointer to the array containing
+ *                                      channel information for each event
+ *          unsigned char *timeflags    Pointer to the array containing
+ *					time flags for each event
+ *          unsigned char *locflags     Pointer to the array containing
+ *					location flags for each event
+ *		int  airglow_centroid	If TRUE, use airglow lines to compute
+ *					centroid of target spectrum.
+ *
+ * Calls:       
+ *
+ * Return:      0 on success
+ *
+ * History:     04/18/03    1.1  wvd    Initial work
+ *              05/20/03    1.2  rdr    Added call to cf_proc_check 
+ *              07/29/03    1.3  rdr    Deal with case where no source is
+ *                                      present (i.e. Aperture = RFPT)
+ *              08/21/03    1.6  wvd    Change channel to unsigned char.
+ *              09/08/03    1.7  wvd    Fix typo in verbose statement.
+ *              09/18/03    1.8  wvd    Stop iteration if
+ *					cf_calculate_y_centroid returns -1.
+ *              10/22/03    1.9  wvd    Rewrite program.
+ *              11/12/03    1.10 wvd    In HIST mode, use default centroid
+ *					for non-target channels.
+ *              04/09/04    1.11 bjg    Include stdlib.h and stdio.h
+ *                                      Change formats in printf to 
+ *                                      match arg types.
+ *              04/19/04    1.12 wvd    Sum background only over detector
+ *					active area.  Scale intrinsic count
+ *					rate by EXPTIME and detector width.
+ *              05/03/04    1.13 wvd    Move call to cf_identify_channel
+ *					from this routine to cf_remove_motions.
+ *              06/02/04    1.14 wvd    Don't need PHA array; can use locflags
+ *					instead.  Use time flags to exclude
+ *					bursts, etc.
+ *              04/21/05    1.15 wvd    Rewrite program using airglow lines
+ *					(if available) to constrain search
+ *					for target centroid.  Don't bother
+ *					reading model background files.
+ *              06/03/05    1.16 wvd    Fix bug in tabulation of exected Y
+ *					centroids. Remove unused variables.
+ *              02/01/06    1.17 wvd    Tighten region over which centroids
+ *					are computed.
+ *					If target centroid is too far from
+ *					airglow centroid, reject it.
+ *					If ycent is too far from default value,
+ *					use default, not airglow value.
+ *					Change ysum and norm to doubles.
+ *              08/30/06    1.18 wvd    Added airglow_centroid argument.
+ *		03/14/08    1.19 wvd	In HIST mode, there are no spectra in
+ *					other apertures to cause confusion,
+ *					so we need not require that the 
+ *					target centroid be within 30 pixels
+ *					of the airglow value.
+ *		11/25/08    1.20 wvd	Don't compare HIST centroids to
+ *					either airglow or tabulated centroid.
+ *
+ ****************************************************************************/
+#include <stdlib.h>
+#include <stdio.h>
+#include <math.h>
+#include <string.h>
+#include "calfuse.h"
+
+#define YLENGTH		NYMAX/16
+
+int
+cf_find_spectra(fitsfile *header, long nevents,
+	float *weight, float *xfarf, float *yfarf, unsigned char *channel,
+	unsigned char *timeflags, unsigned char *locflags, int airglow_centroid)
+{
+    char aper[FLEN_VALUE], instmode[FLEN_VALUE], quality[FLEN_VALUE];
+    char key[FLEN_KEYWORD], filename[FLEN_VALUE], detector[FLEN_VALUE];
+    double norm, ysum;
+    float bkgd, peak, ycent, yshift=0;
+    float yairg[NYMAX], ydist[NYMAX], ysigma[NYMAX];
+    float ybin[YLENGTH], sbin[YLENGTH], ycent_tab[8];
+    float dy, sigma, xmin, xmax, ycent_air;
+    int  active_ap[2], airglow=FALSE, target_ap, status=0;
+    int  bkgd_num, bkgd_min[8], bkgd_max[8];
+    int  chan_num, errflg = 0, lwrs;
+    int  chan_order[] = { 3, 2, 1, 7, 6, 5 };
+    int  center, high, low, npeak, hdu;
+    int  spex_sic, spex_lif, emax, emax_sic, emax_lif, extended;
+    long i, j, k;
+    fitsfile  *chidfits, *parmfits;
+
+    char CF_PRGM_ID[] = "cf_find_spectra";
+    char CF_VER_NUM[] = "1.20";
+
+    /* Initialize error checking */
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+    /* Enter a time stamp into the log */
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    /* Check whether routine is appropriate for this data file. */
+    if ( (errflg = cf_proc_check(header, CF_PRGM_ID)) ) return errflg;
+
+    /* Initialize Y-distribution arrays. */
+    for (i = 0; i < NYMAX; i++)
+	yairg[i] = ydist[i] = ysigma[i] = 0.;
+    for (i = 0; i < YLENGTH; i++)
+	ybin[i] = sbin[i] = 0.;
+
+    /* Read header keywords from IDF. */
+    FITS_read_key(header, TSTRING, "INSTMODE", instmode, NULL, &status);
+    FITS_read_key(header, TSTRING, "DETECTOR", detector, NULL, &status);
+    FITS_read_key(header, TSTRING, "APERTURE", aper, NULL, &status);
+    extended = cf_source_aper(header, active_ap);
+
+    FITS_read_key(header, TINT, "BKGD_NUM", &bkgd_num, NULL, &status);
+    for (i = 0; i < bkgd_num; i++) {
+	sprintf(key, "BKG_MIN%ld", i);
+        FITS_read_key(header, TINT, key, bkgd_min+i, NULL, &status);
+	sprintf(key, "BKG_MAX%ld", i);
+        FITS_read_key(header, TINT, key, bkgd_max+i, NULL, &status);
+    }
+
+    /* Read expected channel centroids from CHID_CAL file. */
+    FITS_read_key(header, TSTRING, "CHID_CAL", filename, NULL, &status);
+    FITS_open_file(&chidfits, cf_cal_file(filename), READONLY, &status);
+    for (i = 1; i < 8; i++) {
+	if (i==4) continue;
+        if ((i == active_ap[0] || i == active_ap[1]) && !extended) hdu=i+1;
+	else hdu=i+9;
+	FITS_movabs_hdu(chidfits, hdu, NULL, &status);
+	FITS_read_key(chidfits, TFLOAT, "CENTROID", ycent_tab+i, NULL, &status);
+    }
+    FITS_read_key(chidfits, TFLOAT, "XMIN", &xmin, NULL, &status);
+    FITS_read_key(chidfits, TFLOAT, "XMAX", &xmax, NULL, &status);
+    FITS_close_file(chidfits, &status);
+
+    /* 
+     * Generate photon and airglow arrays as a function of YFARF.
+     * Ignore events near the detector edge.
+     */
+    xmin += 250;
+    xmax -= 250;
+    for (i = 0; i < nevents; i++) {
+	if (!(timeflags[i] & ~TEMPORAL_DAY) &&
+	    (xfarf[i] > xmin) && (xfarf[i] < xmax)) {
+	    if (!locflags[i])
+	        ydist[cf_nint(yfarf[i])] += weight[i];
+	    else if (locflags[i] == LOCATION_AIR)
+	        yairg[cf_nint(yfarf[i])] += weight[i];
+	}
+    }
+    /* Set error array equal to photon counts (= variance). */
+    for (i = 0; i < NYMAX; i++)
+	ysigma[i] = ydist[i];
+
+    /* If exposure was taken in TTAG mode, estimate BKGD level */
+    bkgd = 0.;
+    if (!strcmp(instmode, "TTAG")) {
+	k = 0;
+	for (i = 0; i < bkgd_num; i++) {
+	    for (j = bkgd_min[i]; j <= bkgd_max[i]; j++) {
+		bkgd += ydist[j];
+		k++;
+	    }
+	}
+	bkgd /= k;
+	cf_verbose(3, "Mean background level: %.1f", bkgd);
+    }
+
+    /* Subtract mean background and bin data by 16 pixels. */
+    for (i = 0; i < NYMAX; i++) {
+	j = i / 16;
+	ybin[j] += ydist[i] - bkgd;
+	sbin[j] += ysigma[i];
+    }
+    for (i = 0; i < YLENGTH; i++) sbin[i] = sqrt(sbin[i]);
+
+    /* Read extraction parameters from PARM_CAL file. */
+    FITS_read_key(header, TSTRING, "PARM_CAL", filename, NULL, &status);
+    FITS_open_file(&parmfits, cf_parm_file(filename), READONLY, &status);
+    FITS_read_key(parmfits,TINT,"SPEX_SIC",&spex_sic,NULL,&status);
+    FITS_read_key(parmfits,TINT,"SPEX_LIF",&spex_lif,NULL,&status);
+    FITS_read_key(parmfits,TINT,"EMAX_SIC",&emax_sic,NULL,&status);
+    FITS_read_key(parmfits,TINT,"EMAX_LIF",&emax_lif,NULL,&status);
+    FITS_close_file(parmfits,&status);
+
+    /* Determine centroid for each channel. */
+    for (k = 0; k < 6; k++) {
+	chan_num = chan_order[k];
+
+	/* Is this the LWRS aperture? */
+	if (chan_num == 3 || chan_num == 7)
+	    lwrs = TRUE;
+	else 
+	    lwrs = FALSE;
+
+	/* Is it the target aperture? */
+	if (chan_num == active_ap[0] || chan_num == active_ap[1])
+	    target_ap = TRUE;
+	else
+	    target_ap = FALSE;
+
+        /* If we're in histogram mode, and this is not the target aperture,
+	   move to next aperture. */
+        if (!strncmp(instmode, "HIST", 4) && !target_ap) {
+	    if (lwrs) yshift = 0;
+	    continue;
+	}
+
+	/* First, we compute a centroid from the airglow lines.
+	   For the LWRS aperture, search within 70 pixels of
+	   the expected centroid.  Compute the offset between the
+	   measured and tabulated centroids.  For the MDRS and HIRS
+	   apertures, apply the offset computed from the LWRS aperture
+	   to the tabulated centroid.
+	   Disregard regions near the bottom and top of the detector. */
+
+	if (lwrs) {
+	    center = cf_nint(ycent_tab[chan_num]);
+	    dy = 70;
+            if ((low  = center-dy) < 16) low = 16;
+            if ((high = center+dy) > NYMAX-50) high = NYMAX-50;
+	    norm = ysum = 0.;
+	    for (i = low; i <= high; i++) {
+		ysum += i * yairg[i];
+		norm += yairg[i];
+	    }
+
+	    /* If the airglow lines contain at least 33 events, use their
+	       centroid.  If not, use the tabulated centroid. */
+	    if (norm > 33.) {
+		ycent = ysum / norm;
+		yshift = ycent - ycent_tab[chan_num];
+		airglow = TRUE;
+	    }
+	    else {
+		ycent = ycent_tab[chan_num];
+		yshift = 0;
+		airglow = FALSE;
+	    }
+	}
+ 		/* For MDRS and HIRS apertures */
+	else
+	    ycent = yshift + ycent_tab[chan_num];
+
+	/* Remember airglow centroid */
+	ycent_air = ycent;
+
+	/* Now we find the centroid for the target spectrum.  If we are
+	   in a target aperture and user has specified YCENT, use it. */
+
+	if (target_ap && ((chan_num<5 && spex_lif>=0 && spex_lif<1024) ||
+	    (chan_num>4 && spex_sic>=0 && spex_sic<1024))) {
+            if (chan_num<5) ycent=spex_lif;
+            else ycent=spex_sic;
+            sprintf(key, "YCENT%1d", chan_num);
+            FITS_update_key(header, TFLOAT, key, &ycent, NULL, &status);
+	    sprintf(quality, "HIGH");
+            sprintf(key, "YQUAL%1d", chan_num);
+            FITS_update_key(header, TSTRING, key, quality, NULL, &status);
+            cf_verbose(1, "Channel %d: User-specified Y centroid = %.2f",
+                chan_num, ycent);
+	    continue;
+        }
+
+	/* If we must find the target spectrum ourselves, use the binned
+	   data array to improve the S/N.  Search within 2 binned pixels
+	   of ycent, however it was computed. */
+
+	center = cf_nint(ycent / 16.);
+	dy = 2;
+	if ((low = center - dy) < 3) low = 3;
+	if ((high = center + dy) > YLENGTH-4) high = YLENGTH-4;
+
+	npeak = 0;
+	peak = -1.0E5;
+	for (i = low; i <= high; i++) {
+	    if (ybin[i] > peak) {
+		peak = ybin[i];
+		npeak = i;
+	    }
+	}
+
+	/* If peak is significant, compute Y centroid for events falling
+	   within 40 pixels of peak.  If this number is within 30 pixels
+	   of airglow centroid, use it.  If not, use airglow centroid.
+	   Note that we require a higher significance for the SiC LWRS
+	   channel on side 1, because it sits on an elevated background. */
+
+	if (!strncmp(detector, "1", 1) && chan_num == 7) sigma = 9.;
+	else sigma = 5.;
+
+	sprintf(quality, "UNKNOWN");
+
+	if (peak > sigma * sbin[npeak] && !airglow_centroid) {
+	    center = npeak * 16 + 8;
+	    dy = 40;
+	    if ((low = center - dy) < 32) low = 32;
+	    if ((high = center + dy) > NYMAX-50) high = NYMAX-50;
+	    norm = ysum = 0.;
+	    for (i = low; i <= high; i++) {
+		ysum += i * ydist[i];
+		norm += ydist[i];
+	    }
+	    ycent = ysum / norm;
+
+	    /* Don't test offset for HIST data. (wvd, 03/14/2008) */
+	    if (fabs(ycent - ycent_air) < 30 || !strncmp(instmode, "HIST", 4)) {
+	    	sprintf(quality, "HIGH");
+	    	cf_verbose(3, "Channel %d: default centroid: %.2f",
+			chan_num, ycent_tab[chan_num]);
+	    	if (airglow) cf_verbose(3, "Channel %d: airglow centroid: %.2f",
+			chan_num, ycent_air);
+	    	cf_verbose(3,"Channel %d: counts in peak = %.0f, limit = %.0f",
+			chan_num, peak, sigma * sbin[npeak]);
+	    	cf_verbose(2, "Channel %d: using target centroid = %.2lf",
+			chan_num, ycent);
+	    }
+	}
+	/* If peak is not significant or ycent differs too much from
+	   the airglow centroid, use the airglow centroid. */
+	if (!strncmp(quality, "UNKNOWN", 1)) {
+	    if (airglow) {
+		sprintf(quality, "MEDIUM");
+	        cf_verbose(3, "Channel %d: default centroid: %.2f",
+		    chan_num, ycent_tab[chan_num]);
+		cf_verbose(3,"Channel %d: peak = %.0f, limit = %.0f",
+		    chan_num, peak, sigma * sbin[npeak]);
+		cf_verbose(2, "Channel %d: using airglow centroid = %.2lf",
+		    chan_num, ycent);
+	    }
+	    else {
+	        sprintf(quality, "LOW");
+		cf_verbose(3,"Channel %d: peak = %f, limit = %f",
+		    chan_num, peak, sigma * sbin[npeak]);
+		cf_verbose(2, "Channel %d: using default centroid = %.2lf",
+		    chan_num, ycent);
+	    }
+	}
+
+	/* If centroid lies too far from the default value, use default. */
+        if (chan_num<5) emax=emax_lif; else emax=emax_sic;
+	    /* Don't test offset for HIST data. (wvd, 11/25/2008) */
+        if (fabs(ycent - ycent_tab[chan_num]) > emax && !strncmp(instmode, "TTAG", 4)) {
+	    if (target_ap) {
+        	cf_verbose(1, "Computed centroid (%.1lf) is too far from "
+		    "expected value.", ycent);
+	        cf_verbose(1, "Channel %d: using default centroid of %.1f",
+		    chan_num, ycent_tab[chan_num]);
+	    }
+	    else {
+	        cf_verbose(2, "Channel %d: using default centroid of %.1f",
+		    chan_num, ycent_tab[chan_num]);
+	    }
+            ycent = ycent_tab[chan_num];
+	    sprintf(quality, "LOW");
+        }
+
+	/* Write results to file header */
+        sprintf(key, "YCENT%1d", chan_num);
+        FITS_update_key(header, TFLOAT, key, &ycent, NULL, &status);
+        sprintf(key, "YQUAL%1d", chan_num);
+        FITS_update_key(header, TSTRING, key, quality, NULL, &status);
+    }
+
+    cf_proc_update(header, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done Processing");
+
+    return status;
+}
diff --git a/src/libcf/cf_fpa_position.c b/src/libcf/cf_fpa_position.c
new file mode 100644
index 0000000..fd7229c
--- /dev/null
+++ b/src/libcf/cf_fpa_position.c
@@ -0,0 +1,231 @@
+/****************************************************************************
+ *
+ * Synopsis:    cf_fpa_position(fitsfile *header, long nevents, float *x,
+ *                       unsigned char *channel)
+ *
+ * Description: Modify X position of photon events to account for an offset
+ *              of the focal plane assembly (FPA)
+ *
+ * Arguments:   fitsfile *header        Pointer to the FITS header
+ *                                      of the Intermediate Data File
+ *              long     npts           Number of photons in the file
+ *              float    *x             X positions for each photon event
+ *     unsigned char     *channel       Assigned channel of each photon
+ *
+ * Calls:       None
+ *
+ * Return:      0 on success 
+ *
+ * History:	09/04/02 v1.1	wvd	Based on cf_dpix by HSU
+ * 		01/14/03 v1.3	wvd	Rename cf_fpa_pos to cf_read_fpa_pos
+ *					Move spectrograph optical parameters
+ *					 to separate calibration file.
+ *					Abandon linear wavelength scale.
+ * 		02/13/03 v1.4	wvd	Write FPA shifts to file header.
+ * 		04/07/03 v1.5	wvd	Change keywords to FPADXLIF and
+ *					FPADXSIC.  Implement cf_verbose.
+ *					Comment out cf_proc_check.
+ *					Test channel[i] as int, not char.
+ *              05/20/03 v1.6   rdr     Added call to cf_proc_check.
+ * 		08/21/03 v1.7	wvd	Change channel to unsigned char.
+ * 		08/23/05 v1.8	wvd	If either FPA position is out of 
+ *					bounds, issue a warning and set
+ *					that FPA correction to zero.
+ * 		08/01/05 v1.9	wvd	Broaden FPA limits by +/- 1.
+ * 		09/06/05 v1.10  wvd	Correct for both X and Z motions
+ *					of FPA.
+ *					Delete call to cf_read_fpa_pos.c
+ * 		12/02/05 v1.11  wvd	Delete unused variables.
+ *              04/07/07 v1.12  wvd	Clean up compiler warnings.
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include <stdio.h>
+#include <math.h>
+#include "calfuse.h"
+
+#define PIX1 2500		/* PIX1,2 are just inside the non-linear */
+#define PIX2 13500		/*  regions of the detector 		 */
+
+int cf_fpa_position(fitsfile *header, long nevents, float *x,
+	unsigned char *channel)
+{
+    char CF_PRGM_ID[] = "cf_fpa_position";
+    char CF_VER_NUM[] = "1.12";
+
+    int   errflg=0, status=0, hdutype, hdunum;
+    int   nwave;     /* number of pixels in calibration file */
+    char  aperture[FLEN_VALUE];  /* aperture keyword from FITS header */
+    char  detector[FLEN_VALUE];  /* detector keyword from FITS header */
+    char  wave_file[FLEN_FILENAME]; /* name of wavelength calibration file */
+    char  spec_file[FLEN_FILENAME]; /* name of spectrograph calibration file */
+    long  i;
+			/* Spectrograph optical parameters */
+    float alpha, alpha_lif, alpha_sic, sigma_lif, sigma_sic, diam;
+    float *wavelength;  /* wavelengths read from calibration file */
+    float fpaxlifdata;	/* LiF FPA X position in microns for spectrum */
+    float fpaxsicdata;	/* SiC FPA X position in microns for spectrum */
+    float fpaxcal;	/* FPA X position in microns for calibration file */
+    float dxfpa;	/* fpax_data - fpaxcal */
+    float fpazlifdata;	/* LiF FPA Z position in microns for spectrum */
+    float fpazsicdata;	/* SiC FPA Z position in microns for spectrum */
+    float fpazcal;	/* FPA Z position in microns for calibration file */
+    float dzfpa;	/* fpaz_data - fpazcal */
+    float dpix, dpix_LiF, dpix_SiC; /* Spectral shift (in pixels)*/
+
+    double w1, w2;	/* wavelengths at which to sample calibration */
+    double beta1,beta2;	/* grating exit angle for w1, w2 */
+    double sinalpha;	/* sin (spectrograph entrance angle) */
+    double cosalpha;	/* cos (spectrograph entrance angle) */
+    double sigma;	/* grating groove spacing in Angstroms */
+    double cosbeta;	/* cos (mean grating exit angle) */
+    double pixscale;	/* mean effective microns/pixel for det segment */
+    fitsfile *specfits, *wavefits;
+
+    /* Initialize error checking */
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+    /* Enter a timestamp into the log. */
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    /* Check whether routine is appropriate for this data file. */
+    if ((errflg = cf_proc_check(header, CF_PRGM_ID))) return errflg;
+
+    /* Read keywords from data file header. */
+    FITS_read_key(header, TSTRING, "DETECTOR", detector, NULL, &status);
+    FITS_read_key(header, TSTRING, "APERTURE", aperture, NULL, &status);
+    FITS_read_key(header, TFLOAT,  "FPASXPOS", &fpaxsicdata, NULL, &status);
+    FITS_read_key(header, TFLOAT,  "FPALXPOS", &fpaxlifdata, NULL, &status);
+    FITS_read_key(header, TFLOAT,  "FPASZPOS", &fpazsicdata, NULL, &status);
+    FITS_read_key(header, TFLOAT,  "FPALZPOS", &fpazlifdata, NULL, &status);
+    FITS_read_key(header, TSTRING, "SPEC_CAL", spec_file, NULL, &status);
+    FITS_read_key(header, TSTRING, "WAVE_CAL", wave_file, NULL, &status);
+
+    /* Read spectrograph optical parameters from SPEC_CAL file. */
+    FITS_open_file(&specfits, cf_cal_file(spec_file), READONLY, &status);
+    FITS_read_key(specfits, TFLOAT, "ALPHALIF", &alpha_lif, NULL, &status);
+    FITS_read_key(specfits, TFLOAT, "ALPHASIC", &alpha_sic, NULL, &status);
+    FITS_read_key(specfits, TFLOAT, "SIGMALIF", &sigma_lif, NULL, &status);
+    FITS_read_key(specfits, TFLOAT, "SIGMASIC", &sigma_sic, NULL, &status);
+    FITS_read_key(specfits, TFLOAT, "DIAM", &diam, NULL, &status);
+    FITS_close_file(specfits, &status);
+
+    /* Determine the extension number (LiF) from aperture */
+    hdunum = 4;					/* Default is LWRS */
+    if (!strcmp(aperture, "HIRS")) hdunum = 2;
+    if (!strcmp(aperture, "MDRS")) hdunum = 3;
+
+    /* Open wavelength calibration file */
+    FITS_open_file(&wavefits, cf_cal_file(wave_file), READONLY, &status);
+
+    /* Loop over the two apertures; first (i==0) LiF, then SiC. */
+    /* Determine shifts for LiF and SiC channels.		*/
+    for(i=0; i<2; i++) {
+
+	/* Move to appropriate HDU in WAVECAL file. */
+	hdunum += i*4;
+	FITS_movabs_hdu(wavefits, hdunum, &hdutype, &status);
+
+	/* Get FPA position for which WAVECAL was derived */
+	FITS_read_key(wavefits, TFLOAT, "FPACXPOS", &fpaxcal, NULL, &status);
+	FITS_read_key(wavefits, TFLOAT, "FPACZPOS", &fpazcal, NULL, &status);
+
+        /* Read the wavelength array from the WAVECAL file. */
+	nwave=cf_read_col(wavefits, TFLOAT,"WAVELENGTH", (void **) &wavelength);
+
+	/* Set LiF/SIC-dependent quantities */
+	if (i == 1) { 			/* SiC data */
+	    dxfpa = fpaxsicdata - fpaxcal;
+	    dzfpa = fpazsicdata - fpazcal;
+	    sigma = sigma_sic;
+	    alpha = alpha_sic;
+	} else { 			/* LiF data */
+	    dxfpa = fpaxlifdata - fpaxcal;
+	    dzfpa = fpazlifdata - fpazcal;
+	    sigma = sigma_lif;
+	    alpha = alpha_lif;
+	}
+	/*
+	 * Compute mean pixel scale from points just inside the
+	 * highly-nonlinear regions at edges of detectors */
+        w1 = wavelength[PIX1];
+        w2 = wavelength[PIX2];
+	sinalpha = sin (alpha * RADIAN);
+	cosalpha = cos (alpha * RADIAN);
+	beta1 = asin (w1/sigma - sinalpha);
+	beta2 = asin (w2/sigma - sinalpha);
+	cosbeta = cos ((beta1 + beta2)/2.);  /* mean cosbeta for segment */
+	pixscale = diam * fabs(beta1 - beta2) * 1000. / (double)(PIX2-PIX1);
+
+	/* Compute shift of spectrum in pixels due to the FPA offset. */
+	if (i == 1)			/* SiC data */
+	    dpix = (dxfpa * cosalpha + dzfpa * sinalpha) / cosbeta / pixscale;
+
+	else				/* LiF data */
+	    dpix = (dxfpa * cosalpha - dzfpa * sinalpha) / cosbeta / pixscale;
+
+	/* For side 2, multiply the above expressions by -1. */
+	if (!strncmp(detector, "2", 1))
+	    dpix *= -1;
+
+	/* Write info to log file */
+	if (i == 1) {
+	   dpix_SiC = dpix;
+	   cf_verbose(3, "FPAX data: %8.3f   FPAX calib: %8.3f",
+		   fpaxsicdata, fpaxcal);
+	   cf_verbose(3, "FPAZ data: %8.3f   FPAZ calib: %8.3f",
+		   fpazsicdata, fpazcal);
+	   cf_verbose(2, "SiC spectra to be shifted by %8.3f pixels", dpix_SiC);
+	}
+	else {
+	   dpix_LiF = dpix;
+	   cf_verbose(3, "FPAX data: %8.3f   FPAX calib: %8.3f",
+		   fpaxlifdata, fpaxcal);
+	   cf_verbose(3, "FPAZ data: %8.3f   FPAZ calib: %8.3f",
+		   fpazlifdata, fpazcal);
+	   cf_verbose(2, "LiF spectra to be shifted by %8.3f pixels", dpix_LiF);
+	}
+  
+    } /* End of i loop */
+
+    /* Close the WAVECAL file */
+    FITS_close_file(wavefits, &status);
+
+    /* If tabulated FPA position is out of range, set the corresponding
+	dpix value to zero and issue a warning. */
+    if (fpaxlifdata < -1 || fpaxlifdata > 401) {
+	dpix_LiF = 0;
+	cf_if_warning("Keyword FPALXPOS is out of bounds.  Setting FPADXLIF = 0.");
+    }
+    if (fpaxsicdata < -1 || fpaxsicdata > 401) {
+	dpix_SiC = 0;
+	cf_if_warning("Keyword FPASXPOS is out of bounds.  Setting FPADXSIC = 0.");
+    }
+
+    /* Shift only photons with assigned apertures. */
+    for(i = 0; i < nevents; i++) {
+	switch(channel[i]) {
+	case 1: case 2: case 3: case 4:
+	    x[i] += dpix_LiF;
+	    break;
+	case 5: case 6: case 7: case 8:
+	    x[i] += dpix_SiC;
+	    break;
+	default:
+	    break;
+	}
+    }
+
+    /* Write shifts to IDF file header */
+    FITS_update_key(header, TFLOAT, "FPADXLIF", &dpix_LiF, NULL, &status);
+    FITS_update_key(header, TFLOAT, "FPADXSIC", &dpix_SiC, NULL, &status);
+
+    /* Update processing flags. */
+    cf_proc_update(header, CF_PRGM_ID, "COMPLETE");
+
+    /* Enter a timestamp into the log. */
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+
+    return status;
+}
diff --git a/src/libcf/cf_fuv_init.c b/src/libcf/cf_fuv_init.c
new file mode 100644
index 0000000..a2bb181
--- /dev/null
+++ b/src/libcf/cf_fuv_init.c
@@ -0,0 +1,592 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_fuv_init(fitsfile *fptr)
+ *
+ * Description: cf_fuv_init performs the following functions:
+ *              1.  Populates the data processing step keywords based upon
+ *                  the type of data (TTAG or HIST).  The processing steps
+ *                  and the associated keywords are defined in the 
+ *                  structure CALIBRATION_STEP_KEYS in calfuse.h.
+ *              2.  Populates the orbital parameters in the header by
+ *                  calling read_tle.  The orbital elements come from
+ *                  the file FUSE.TLE, which is in standard NORAD two-line
+ *                  element format.
+ *              3.  Populates the calibration file keywords based on the 
+ *                  time and date of observation, the detector segment, 
+ *                  and the interpolation status of the calibration file.
+ *                  The relation between processing steps and associated
+ *                  calibration file keywords is defined in the structure
+ *                  CALIBRATION_FILE_KEYS in calfuse.h.  The names and
+ *                  effective dates of the calibration files are found in
+ *                  the ASCII-format file master_calib_file.dat in the 
+ *                  CF_PARMDIR directory.
+ *
+ * Input:   fitsfile    *fptr	Pointer to input file
+ *
+ * History:     05/11/98        emm     Begin work.
+ *              05/15/98        emm     finished
+ *              06/04/98        emm     Modified keywords to reflect updated
+ *                                      calfuse design
+ *              11/12/98        emm     Added ability to read orbital elements
+ *                                      from file FUSE.TLE.
+ *              03/18/99        emm     Added call to cf_cal_file.  master_
+ *                                      calib_file.dat must now be in the
+ *                                      CF_CALDIR directory.  (on 08/25/99
+ *                                      this became CF_PARMDIR).
+ *              03/18/99        emm     Edited header only.
+ *              04/14/99        peb     Increased strings sizes to prevent
+ *                                        character overflow.
+ *                                      Implemented FITS wrapper functions.
+ *              05/19/99        peb     Implemented cf_error_msg functions.
+ *              06/07/99        peb     Added reporting of version number.
+ *              07/29/99        emm     Added CF_VERS keyword update.
+ *              08/25/99        emm     master_calib_file.dat now in CF_PARMDIR
+ *              12/06/99 v1.8   emm     Removed cf_if_error call when master
+ *                                      calib file keyword not found.
+ *		10/13/00 v1.9	jwk	change CF_VER_NUM from "1.5"
+ *		08/23/01 v1.10  wvd     Read PARM file; if requested, set
+ *					BRST_COR, ASTG_COR, PHAX_COR, 
+ *					MKBK_COR, or BKGD_COR to "OMIT"
+ *		10/23/01 v1.11  hsu     Check OPUS version
+ *		10/26/01 v1.12  wvd     Install subroutine.
+ *		02/11/02 v1.13  wvd     Check detector bias levels.
+ *		02/13/02 v1.14  wvd     Modified bias logic; write warning
+ *					to data header as COMMENT lines.
+ *		02/13/02 v1.15  wvd     Don't crash if bias keywords missing.
+ *		02/19/02 v1.16  wvd     Check whether voltage too high
+ *		02/20/02 v1.17  wvd     If keyword RAWTIME does not exist,
+ *					create with value of EXPTIME
+ *              10/30/02  1.18  peb     Converted header to calfusettag.h
+ *		03/26/03  1.4   wvd	Removed "Warning" from warnings.
+ *              04/16/03 v1.5   wvd     Test for corrupted bias values.
+ *                                      Update comment field for HV_FLAG.
+ *		04/28/03 v1.6   wvd	Change logic of assigning cal files
+ *                                      never to extrapolate forward in time.
+ *		07/23/03 v1.7   wvd	Write HSKP_CAL to file header.
+ *		07/23/03 v1.8   wvd	Change calfusettag.h to calfuse.h
+ *		09/09/03 v1.9   wvd	Read SAA_SCR and LIMB_SCR from
+ *					SCRN_CAL and set RUN_SAA and RUN_LIMB.
+ *		04/27/04 v1.10  wvd	Keywords MKBK_COR and BKGD_COR are
+ *					gone, so we don't populate them.
+ *		06/04/04 v1.11  wvd	Allow for the possibility that the
+ *					time associated with a calibration
+ *					file exactly equals EXPSTART.
+ *		06/14/04 v1.12  wvd	Check value of BRIT_OBJ keyword and
+ *					modify header accordingly.
+ *					Write CF_VERS to trailer file.
+ *		07/16/04 v1.13  wvd	Must set ASTG_COR to PERFORM, as
+ *					pipeline doesn't do it automatically.
+ *		11/26/04 v1.14  wvd	Check whether SAA_SCR and LIMB_SCR
+ *					are ON or OFF, not YES or NO.
+ *		12/02/04 v1.15  wvd	Read value of RUN_JITR from PARM file.
+ *		03/24/05 v1.16  wvd	Use HVGOODLM to determine whether
+ *					detector voltage is low.
+ *		06/12/06 v1.17  wvd	Call cf_verbose rather than
+ *					cf_if_warning for non-optimal voltage.
+ *              07/18/08 v1.18  wvd     For bright-earth and airglow exposures, 
+ *					change EXP_STAT to 2, 
+ *					change SRC_TYPE to EE, and
+ *					write warning to file header.
+ *
+ ****************************************************************************/
+
+#include <stdio.h>
+#include <stdlib.h>
+#include <string.h>
+#include "calfuse.h"
+
+#define  MAXCHARS 120
+#define  MASTER_CAL_FILE "master_calib_file.dat"
+
+int cf_fuv_init(fitsfile *fptr)
+{
+    char CF_PRGM_ID[] = "cf_fuv_init";
+    char CF_VER_NUM[] = "1.18";
+
+    int   i, status=0, expstat, interp_in, timeref;
+    int   n, hv_flag, lowv, highv, saav, fullv;
+    char  comment[FLEN_CARD], instmode[FLEN_CARD], detector[FLEN_CARD];
+    char  opus_str[FLEN_CARD], keyword_in[FLEN_CARD], segment_in[FLEN_CARD];
+    char  datestr[FLEN_CARD];
+    char  filename_in[]="                    ", rootname[FLEN_CARD];
+    char  hkexists[FLEN_CARD];
+    char  keyword_out1[FLEN_CARD], keyword_out2[FLEN_CARD];
+    char  linin[MAXCHARS];
+    char  run_limb[FLEN_VALUE], run_saa[FLEN_VALUE], src_type[FLEN_VALUE];
+    char  run_brst[FLEN_VALUE], run_walk[FLEN_VALUE], run_astg[FLEN_VALUE];
+    /* char  run_mkbk[FLEN_VALUE], run_bkgd[FLEN_VALUE], brit_obj[FLEN_VALUE]; */
+    char  run_jitr[FLEN_VALUE], brit_obj[FLEN_VALUE];
+    char  hv_str[FLEN_CARD], lv_str[FLEN_CARD], mjd_str[FLEN_CARD];
+    char  saa_str[FLEN_CARD], full_str[FLEN_CARD];
+    float hvgood, mjdv, expstart, aftermjd_in;
+    fitsfile *parmfits, *scrnfits;
+
+    struct keyword_tab  keytab[NUM_PROC_STEPS]=CALIBRATION_STEP_KEYS;
+    struct cal_file_tab calkey[NUMCALKEYS]=CALIBRATION_FILE_KEYS;
+    FILE  *fpin;
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin initializing headers");
+
+    /* Check the OPUS version number */
+    fits_read_key(fptr, TSTRING, "OPUSVERS", opus_str, NULL, &status);
+    if (status) {
+        status = 0;
+	cf_add_header_keywords(fptr);
+	cf_verbose(2, "Data file generated by old version of OPUS.");
+    }
+    else if (atof(opus_str) < OPUS_VERSION) {
+	cf_add_header_keywords(fptr);
+	cf_verbose(2, "Data file generated by old version (%s) of OPUS.", opus_str);
+    }
+    FITS_update_key(fptr, TSTRING, "CF_VERS", CALFUSE_VERSION, NULL, &status);
+    cf_verbose (1, "This is CalFUSE v%s", CALFUSE_VERSION);
+
+    /*
+     *  Populate data processing keywords based on observing mode found
+     *  in the INSTMODE keyword.  NOTE:  We check only the first 
+     *  letter of the INSTMODE keyword.
+     */
+    FITS_read_key(fptr, TSTRING, "INSTMODE", instmode, NULL, &status);
+
+    switch (instmode[0]) {
+    case 'H':
+	/*  Histogram mode */
+	for (i=0; i<NUM_PROC_STEPS; i++)
+	    FITS_update_key(fptr, TSTRING, keytab[i].name,
+			    keytab[i].hist_value, 0, &status);
+	break;
+    case 'T':
+	/*  Time tag mode */
+	for (i=0; i<NUM_PROC_STEPS; i++)
+	    FITS_update_key(fptr, TSTRING, keytab[i].name,
+			    keytab[i].ttag_value, 0, &status);
+	break;
+    default:
+	/*  Invalid mode */
+	cf_if_error("Invalid INSTMODE value");
+	FITS_update_key(fptr, TSTRING, "INIT_COR", "ERROR", 0, &status);
+	break;
+    } /* End switch (instmode[0]) */
+
+    /*  Populate the orbital parameters from a file of two-line elements. */
+    read_tle(fptr);
+
+    /*  Populate calibration file keywords based on the date of the
+     *  observation and the segment/channel number. */
+
+    FITS_read_key(fptr, TFLOAT, "EXPSTART", &expstart, NULL, &status);
+    FITS_read_key(fptr, TSTRING, "DETECTOR", detector, NULL, &status);
+
+    /*  Open the Master calibration database file. */
+
+    fpin = fopen(cf_parm_file(MASTER_CAL_FILE), "r");
+    if (fpin == NULL)
+	cf_if_error("Master calibration database file not found");
+
+    /*  Cycle through the master cal file until we run out of lines. */
+
+    /*  Here's how this section works.  We need to keep track of 3 calibration
+     *  files for each keyword: the cal file which immediately preceedes the 
+     *  date of observation, the cal file which immediately preceedes the cal
+     *  file which immediately preceedes the observation, and the cal file 
+     *  immediately after the observation.  These are stored in strut calkey
+     *  in:
+     *     calkey[i].filenames[0] => second cal file preceeding observation
+     *     calkey[i].filenames[1] => cal file immediately preceeding observa-
+     *                                 tion
+     *     calkey[i].filenames[2] => cal file immediately after observation
+     *
+     *  Here is the plan.  Cycle through the master cal file, reading each
+     *  line.  Determine the keyword for each line, and use that to determine
+     *  the appropriate index [i] for calkey.  Then, if the detector segment 
+     *  is correct, determine where the new file fits into the structure above.
+     *  If it is more recent than one or both of the preceeding cal files, 
+     *  but is older than the observation (expstart) replace either 
+     *  filenames[0] or filenames[1].  If filenames[1] is replaced, shift
+     *  the old value down into filenames[0].  If the file is more recent 
+     *  than the observation, and closer to the observation than the file 
+     *  in filenames[2], replace filenames[2].  The values 
+     *  calkey[i].aftermjd[] and calkey[i].interp[] store the date and 
+     *  interpolation status of the best files.  This organization allows
+     *  the master calibration database file to be written in any order.
+     */
+
+    while (fgets(linin, MAXCHARS, fpin) != NULL) {
+        /* Check for comment lines */
+
+	if ((linin[0] != '#') && (linin[0] != '\n')) {
+	    sscanf(linin, "%4c%*2c%2c%*2c%13c%*2c%9f%*2c%1d",keyword_in,
+		   segment_in,filename_in,&aftermjd_in,&interp_in);
+	    /*
+	     *  Determine which keyword we just read in.
+	     */
+	    i=0;
+	    while ((strncmp(calkey[i].name,keyword_in,4) != 0) &&
+		   (i < NUMCALKEYS)) i++;
+	    if (i >= NUMCALKEYS) {
+		cf_if_warning("Keyword %s in %s is unknown", keyword_in, MASTER_CAL_FILE);
+	    } else {
+		if ((strncmp(segment_in,"  ",2) == 0) ||
+		    (strncmp(segment_in,detector,2) == 0)) {
+		    if ((aftermjd_in <= expstart) &&
+			(aftermjd_in > calkey[i].aftermjd[0]) &&
+			(aftermjd_in > calkey[i].aftermjd[1])) {
+			strncpy(calkey[i].filenames[0],
+				calkey[i].filenames[1],18);
+			calkey[i].aftermjd[0]=calkey[i].aftermjd[1];
+			calkey[i].interp[0]=calkey[i].interp[1];
+			strncpy(calkey[i].filenames[1],
+				filename_in,18);
+			calkey[i].aftermjd[1]=aftermjd_in;
+			calkey[i].interp[1]=interp_in;
+		    } else if ((aftermjd_in < expstart) &&
+			       (aftermjd_in > calkey[i].aftermjd[0])) {
+			strncpy(calkey[i].filenames[0],
+				filename_in,18);
+			calkey[i].aftermjd[0]=aftermjd_in;
+			calkey[i].interp[0]=interp_in;
+		    }
+		    if ((aftermjd_in > expstart) &&
+			(aftermjd_in < calkey[i].aftermjd[2])) {
+			strncpy(calkey[i].filenames[2],
+				filename_in,18);
+			calkey[i].aftermjd[2]=aftermjd_in;
+			calkey[i].interp[2]=interp_in;
+		    }
+		} /* Endif segment match */
+	    } /* end else unrecognized keyword */		   
+	}  /* end while linin not comment */
+    } /* end while(linin != NULL) */
+
+    fclose(fpin);
+
+/*************************************************************************
+        I have changed Rule 3 so that we NEVER extrapolate calibration
+        files forward in time.  Instead, we just use the most recent file.
+        This reduces from 8 to 4 the number of possible cases, since we
+        no longer care about the value of interp[0].
+        This section and the previous one ought to be re-written,
+        but I will simply change 0 to 1 for Case 110 below.
+        WVD - 04/28/03
+*************************************************************************/
+
+    /*  OK, now that we have identified the closest two files before
+     *  the observation, and the file after the observation, we can
+     *  decide what to do with them.  First, the easy part:  if 
+     *  calkey[i].numfiles=1, no interpolation is possible, so we
+     *  write out calkey[i].filenames[1], which is the file immediately
+     *  preceeding the observation.  If calkey[i].numfiles=2, interpolation
+     *  is possible, and we will have to write two keywords into the header.
+     *  The decision as to which two keywords to write follows these rules:
+     *  Rule 1: If an observation occurs between two files which can be 
+     *          interpolated, then an interpolation must be done. 
+     *  Rule 2: If the calibration file immediately preceeding an 
+     *          observation is to be used in a stepwise manner, then said
+     *          file shall be used in stepwise manner. 
+     *  Rule 3: If the two calibration files immediately preceeding an 
+     *          observation can be interpolated, but the following file 
+     *          cannot, then the two previous files will be extrapolated 
+     *          forward in time. 
+     *  Rule 4: If the closest preceeding calibration file has an interpolation
+     *          flag, but the file preceeding it has a stepwise flag, the the 
+     *          closest preceeding file will be used in a sterpwise manner.
+     *  Rule 5: Never interpolate backward in time.
+     *
+     *  In fact, there are only 8 possible cases:
+     *
+     *  Remember, the files were sorted such that the observation 
+     *  always occurs between [1] and [2].  Also remember that 
+     *  interp[i]=0 => stepwise):
+     *
+     *    Case               Action
+     *
+     *  interp[0] = 0
+     *  interp[1] = 0    filenames[1] will be used in a stepwise manner
+     *  interp[2] = 0
+     *
+     *  interp[0] = 0
+     *  interp[1] = 0    filenames[1] will be used in a stepwise manner
+     *  interp[2] = 1
+     *
+     *  interp[0] = 0
+     *  interp[1] = 1    filenames[1] will be used in a stepwise manner
+     *  interp[2] = 0
+     *
+     *  interp[0] = 1
+     *  interp[1] = 0    filenames[1] will be used in a stepwise manner
+     *  interp[2] = 0
+     *
+     *  interp[0] = 1
+     *  interp[1] = 0    filenames[1] will be used in a stepwise manner
+     *  interp[2] = 1
+     *
+     *  interp[0] = 0
+     *  interp[1] = 1    filenames[1] and filenames[2] will be interpolated
+     *  interp[2] = 1
+     *
+     *  interp[0] = 1
+     *  interp[1] = 1    filenames[0] and filenames[1] will be extrapolated
+     *  interp[2] = 0
+     *
+     *  interp[0] = 1
+     *  interp[1] = 1    filenames[1] and filenames[2] will be interpolated
+     *  interp[2] = 1
+     *
+     */
+
+    /*  Write the calibration files into the header keywords. */
+    /*  Cycle through the keywords. */
+    for (i=0; i<NUMCALKEYS; i++) {
+	if (calkey[i].numfiles == 1) {
+	    /*  This is the easy case, no interpolation is possible. */
+
+	    sprintf(keyword_out1,"%4.4s%1.1s%3.3s",calkey[i].name,"_",
+		    calkey[i].extension);
+
+	    FITS_update_key(fptr, TSTRING, keyword_out1,
+			    calkey[i].filenames[1], 0, &status);
+	}
+	else {
+	    /*  OK, interpolation is possible, now decide which two files
+	     *  to write out. */
+
+	    /* Create the two output keywords */
+	    sprintf(keyword_out1,"%4.4s%1.1s%3.3s",calkey[i].name,"1",
+                    calkey[i].extension);
+	    sprintf(keyword_out2,"%4.4s%1.1s%3.3s",calkey[i].name,"2",
+                    calkey[i].extension);
+
+	    if (calkey[i].interp[1] == 0) {
+		/*  Easy, preceeding file is a 0, so write filenames[1] to
+		 *  both keywords.  Takes care of cases 000, 001, 100, 101.
+		 */
+		FITS_update_key(fptr, TSTRING, keyword_out1,
+				calkey[i].filenames[1], 0, &status);
+		FITS_update_key(fptr, TSTRING, keyword_out2,
+				calkey[i].filenames[1], 0, &status);
+	    }
+	    else if ((calkey[i].interp[1] == 1) &&
+		     (calkey[i].interp[2] == 1)) {
+		/* Case 011 and 111 */
+		FITS_update_key(fptr, TSTRING, keyword_out1,
+				calkey[i].filenames[1], 0, &status);
+		FITS_update_key(fptr, TSTRING, keyword_out2,
+				calkey[i].filenames[2], 0, &status);
+	    } else if ((calkey[i].interp[0] == 1) &&
+		       (calkey[i].interp[1] == 1) &&
+		       (calkey[i].interp[2] == 0)){
+		/* Case 110 */
+	    /* CHANGED 0 to 1 in the following line - wvd 04/28/03 */
+		FITS_update_key(fptr, TSTRING, keyword_out1,
+				calkey[i].filenames[1], 0, &status);
+		FITS_update_key(fptr, TSTRING, keyword_out2,
+				calkey[i].filenames[1], 0, &status);
+	    }
+	    else if ((calkey[i].interp[0] == 0) && (calkey[i].interp[1] == 1)
+		     && (calkey[i].interp[2] == 0)){
+		/* Case 010 */
+		FITS_update_key(fptr, TSTRING, keyword_out1,
+				calkey[i].filenames[1], 0, &status);
+		FITS_update_key(fptr, TSTRING, keyword_out2,
+				calkey[i].filenames[1], 0, &status);
+	    }
+	    else
+                cf_if_error("The interpolation/stepwise logic has"
+                            "failed.  I am confused.");
+	} /* end else calkey.numfiles == 1 */
+    } /* end for i=0; i<NUMCALKEYS */
+
+    /*
+     *  If housekeeping file exists,
+     *	add HSKP_CAL and JITR_CAL filenames to the header.
+     */
+    FITS_read_key(fptr, TSTRING, "HKEXISTS", hkexists, NULL, &status);
+    if(!strncasecmp(hkexists, "Y", 1)) {
+	FITS_read_key(fptr, TSTRING, "ROOTNAME", rootname, NULL, &status);
+	sprintf(keyword_out1, "%s%s", rootname, "hskpf.fit");
+	FITS_update_key(fptr, TSTRING, "HSKP_CAL", keyword_out1, 0, &status);
+	sprintf(keyword_out2, "%s%s", rootname, "jitrf.fit");
+	FITS_update_key(fptr, TSTRING, "JITR_CAL", keyword_out2, 0, &status);
+    }
+    /*
+     *  Check min and max voltage levels and set HV_FLAG accordingly.
+     */
+    sprintf(hv_str, "DET%cHV%cH", detector[0], detector[1]);
+    sprintf(lv_str, "DET%cHV%cL", detector[0], detector[1]);
+
+    fits_read_key(fptr, TINT, hv_str, &highv, NULL, &status);
+    if (status) {
+        status = 0;
+        hv_flag = -1;
+        sprintf(comment, "Detector bias keywords not found");
+        FITS_update_key(fptr, TINT, "HV_FLAG", &hv_flag, comment, &status);
+        cf_verbose(2, comment);
+    }
+    else {
+        FITS_read_key(fptr, TINT, lv_str, &lowv, NULL, &status);
+        FITS_read_key(fptr, TSTRING, "VOLT_CAL", filename_in, NULL, &status);
+        FITS_open_file(&parmfits, cf_cal_file(filename_in), READONLY, &status);
+        FITS_read_key(parmfits, TFLOAT, "HVGOODLM", &hvgood, NULL, &status);
+
+        n = 0;
+        do {
+            n++;
+            sprintf(mjd_str, "MJD%d", n);
+            FITS_read_key(parmfits, TFLOAT, mjd_str, &mjdv, NULL, &status);
+        } while (expstart > mjdv);
+        n--;
+
+        sprintf(saa_str, "SAA%d", n);
+        sprintf(full_str, "FULL%d", n);
+        FITS_read_key(parmfits, TINT, saa_str, &saav, NULL, &status);
+        FITS_read_key(parmfits, TINT, full_str, &fullv, NULL, &status);
+        FITS_close_file(parmfits, &status);
+
+             if (lowv > fullv + 3) {
+                hv_flag = 5;
+                sprintf(comment, "Detector voltage high throughout exposure");
+            }
+        else if ((float) lowv / fullv > hvgood) {
+                hv_flag = 4;
+                sprintf(comment, "Detector voltage full throughout exposure");
+            }
+        else if (lowv > saav  + 3) {
+                hv_flag = 3;
+                sprintf(comment, "Detector voltage low throughout exposure");
+            }
+        else if (lowv > saav  - 3) {
+                hv_flag = 2;   
+                sprintf(comment, "Detector at SAA voltage throughout exposure");
+            }
+        else {
+                hv_flag = 1;
+                sprintf(comment, "Detector below SAA voltage throughout exposure");
+            }
+
+             if (highv - lowv > 3) {
+                hv_flag = 0;
+                sprintf (comment, "Detector voltage changed during exposure");
+            }
+        else if (lowv > highv) {
+                hv_flag = -1;
+                sprintf(comment, "Detector bias keywords are corrupted");
+            }
+
+        FITS_update_key(fptr, TINT, "HV_FLAG", &hv_flag, comment, &status);
+
+        if (hv_flag != 4) {
+            if (hv_flag == -1) cf_if_warning(comment);
+            else cf_verbose(1, comment);
+            FITS_write_comment(fptr, "  ", &status);
+            FITS_write_comment(fptr, comment, &status);
+	    fits_get_system_time(datestr, &timeref, &status);
+	    sprintf(comment, "CalFUSE v%s   %.10s", CALFUSE_VERSION, datestr);
+            FITS_write_comment(fptr, comment, &status);
+            FITS_write_comment(fptr, "  ", &status);
+        }
+    }
+
+    /*  Read BRIT_OBS keyword and modify header accordingly. */
+
+    FITS_read_key(fptr, TSTRING, "SRC_TYPE", src_type, NULL, &status);
+    FITS_read_key(fptr, TSTRING, "BRIT_OBJ", brit_obj, NULL, &status);
+    if (!strcmp(brit_obj, "DEFOCUS") && !strncmp(src_type, "P", 1)) {
+	*src_type = 'E';
+	FITS_update_key(fptr, TSTRING, "SRC_TYPE", src_type,
+		"DEFOCUS OBS ==> Treat as extended source", &status);
+    }
+
+    /* Flag bright-earth and airglow (M106, S100, and 900+) exposures. */
+
+    FITS_read_key(fptr, TSTRING, "ROOTNAME", rootname, NULL, &status);
+    if (!strncmp(rootname, "M106", 4) || !strncmp(rootname, "S100", 4)) {
+
+        cf_verbose(1, "Bright-earth exposure.");
+
+	/* Set EXP_STAT to TEMPORAL_LIMB. */
+	expstat = (int) TEMPORAL_LIMB;
+	FITS_update_key(fptr, TINT, "EXP_STAT", &expstat, 
+		"Bright-earth exposure", &status);
+    }
+
+   if (!strncmp(rootname+8, "9", 1)) {
+
+        cf_verbose(1, "Airglow exposure.  Will treat as extended source.");
+
+	/* Set EXP_STAT to TEMPORAL_LIMB. */
+	expstat = (int) TEMPORAL_LIMB;
+	FITS_update_key(fptr, TINT, "EXP_STAT", &expstat, 
+		"Airglow exposure", &status);
+
+	/* Change SRC_TYPE to EE. */
+	(void) strcpy(src_type, "EE");
+	FITS_update_key(fptr, TSTRING, "SRC_TYPE", src_type,
+		"Airglow exposure ==> Treat as extended source", &status);
+
+        /* Write warning to trailer file and IDF header. */
+	FITS_write_comment(fptr, " ", &status);
+	sprintf(comment, "Airglow exposure. Not an astrophysical target.");
+	FITS_write_comment(fptr, comment, &status);
+	fits_get_system_time(datestr, &timeref, &status);
+	sprintf(comment, "CalFUSE v%s   %.10s", CALFUSE_VERSION, datestr);
+	FITS_write_comment(fptr, comment, &status);
+	FITS_write_comment(fptr, " ", &status);
+    }
+
+    /*  Read the SCRN file and see if user wants to skip any steps. */
+
+    FITS_read_key(fptr, TSTRING, "SCRN_CAL", filename_in, NULL, &status);
+    FITS_open_file(&scrnfits, cf_parm_file(filename_in), READONLY, &status);
+    FITS_read_key(scrnfits, TSTRING, "SAA_SCR", run_saa, NULL, &status);
+    FITS_read_key(scrnfits, TSTRING, "LIMB_SCR", run_limb, NULL, &status);
+    FITS_close_file(scrnfits, &status);
+
+    /*  Now read the PARM file and see if user wants to skip any steps. */
+
+    FITS_read_key(fptr, TSTRING, "PARM_CAL", filename_in, NULL, &status);
+    FITS_open_file(&parmfits, cf_parm_file(filename_in), READONLY, &status);
+    FITS_read_key(parmfits, TSTRING, "RUN_BRST", run_brst, NULL, &status);
+    FITS_read_key(parmfits, TSTRING, "RUN_PHAX", run_walk, NULL, &status);
+    /* FITS_read_key(parmfits, TSTRING, "RUN_MKBK", run_mkbk, NULL, &status); */
+    /* FITS_read_key(parmfits, TSTRING, "RUN_BKGD", run_bkgd, NULL, &status); */
+    FITS_read_key(parmfits, TSTRING, "RUN_ASTG", run_astg, NULL, &status);
+    FITS_read_key(parmfits, TSTRING, "RUN_JITR", run_jitr, NULL, &status);
+    FITS_close_file(parmfits, &status);
+
+    if (!strncmp(run_limb, "OFF", 3) || !strncmp(run_limb, "off", 3))
+	FITS_update_key(fptr, TSTRING, "LIMB_COR", "OMIT", NULL, &status);
+
+    if (!strncmp(run_saa, "OFF", 3) || !strncmp(run_saa, "off", 3))
+	FITS_update_key(fptr, TSTRING, "SAA__COR", "OMIT", NULL, &status);
+
+    if (!strncmp(run_brst, "N", 1) || !strncmp(run_brst, "n", 1))
+	FITS_update_key(fptr, TSTRING, "BRST_COR", "OMIT", NULL, &status);
+
+    if (!strncmp(run_walk, "N", 1) || !strncmp(run_walk, "n", 1))
+	FITS_update_key(fptr, TSTRING, "PHAX_COR", "OMIT", NULL, &status);
+
+    /*
+    if (!strncmp(run_mkbk, "N", 1) || !strncmp(run_mkbk, "n", 1)) 
+	FITS_update_key(fptr, TSTRING, "MKBK_COR", "OMIT", NULL, &status);
+
+    if (!strncmp(run_bkgd, "N", 1) || !strncmp(run_bkgd, "n", 1)) 
+	FITS_update_key(fptr, TSTRING, "BKGD_COR", "OMIT", NULL, &status);
+    */
+
+    if (!strncmp(run_astg, "N", 1) || !strncmp(run_astg, "n", 1))
+	FITS_update_key(fptr, TSTRING, "ASTG_COR", "OMIT", NULL, &status);
+    else
+	FITS_update_key(fptr, TSTRING, "ASTG_COR", "PERFORM", NULL, &status);
+
+    if (!strncmp(run_jitr, "N", 1) || !strncmp(run_jitr, "n", 1))
+	FITS_update_key(fptr, TSTRING, "JITR_COR", "OMIT", NULL, &status);
+    else
+	FITS_update_key(fptr, TSTRING, "JITR_COR", "PERFORM", NULL, &status);
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done initializing headers");
+    return status;
+}
diff --git a/src/libcf/cf_geometric_distort.c b/src/libcf/cf_geometric_distort.c
new file mode 100644
index 0000000..1164b5c
--- /dev/null
+++ b/src/libcf/cf_geometric_distort.c
@@ -0,0 +1,145 @@
+/****************************************************************************
+ *
+ * Synopsis:    cf_geometric_distort(fitsfile *header, long nevents,
+ *                                   float *xfarf, float *yfarf,
+ *                                   unsigned char *locflags)
+ *
+ * Description: Corrects the X and Y positions of the event for geometric
+ *              distortion.
+ *
+ * Arguments:   fitsfile  *header       Pointer to the location of the FITS
+ *                                      header of the Intermediate Data File
+ *              long      nevents       number of photons in the file
+ *              float     *xfarf        X positions for each photon event
+ *              float     *yfarf        Y positions for each photon event
+ *              unsigned char *locflags Location flags for each event
+ *
+ * Calls :      None
+ *
+ * Return:      0  on success
+ *
+ * History:     08/09/02   1.1   rdr    Begin work 
+ *              11/12/02   1.2   peb    Added check to move only events in
+ *                                      active region.  Added locflags to
+ *                                      function cal.
+ *		03/11/03   1.3   wvd    Changed locflags to unsigned char.
+ *              05/20/03   1.4   rdr    Added call to cf_proc_check
+ *              07/29/03   1.5   wvd    If cf_proc_check fails, return errflg.
+ *              03/26/04   1.6   rdr    Modify specbiny
+ *              04/05/04   1.7   wvd	Modify specbiny only if specbiny > 1.
+ *              04/07/07   1.8   wvd	Clean up compiler warnings.
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include <stdlib.h>
+#include "calfuse.h"
+
+int
+cf_geometric_distort(fitsfile *header, long nevents, float *xfarf,
+		     float *yfarf, unsigned char *locflags)
+{
+    char CF_PRGM_ID[] = "cf_geometric_distort";
+    char CF_VER_NUM[] = "1.8";
+
+    char geomfile[FLEN_VALUE]={'\0'};
+    short *geomx_img, *geomy_img;
+    int   errflg=0, status=0, hdutype, anynull, nullval;
+    int   specbiny ;
+    long  fpixel=1, j;
+    long  xdim_gx, ydim_gx, xdim_gy, ydim_gy, npix_gx, npix_gy;
+    float scale_gx=1., zero_gx=0., scale_gy=1., zero_gy=0.;
+    float yexp ;
+    fitsfile *geomfits=NULL;
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    if ((errflg = cf_proc_check(header, CF_PRGM_ID))) return errflg;
+
+    /*
+     *  Get the name of the calibration file and open it
+     */
+    FITS_read_key(header, TINT, "SPECBINY", &specbiny, NULL, &status);
+    cf_verbose(5,"Initial value of specbiny=%d",specbiny) ;
+    FITS_read_key(header, TSTRING, "GEOM_CAL", geomfile, NULL, &status);
+    cf_verbose(4, "Geometric correction file = %s", geomfile);
+    FITS_open_file(&geomfits, cf_cal_file(geomfile), READONLY, &status);
+
+    /* Read the y expansion factor from the calibration header */
+    FITS_movabs_hdu(geomfits, 1, &hdutype, &status);
+    FITS_read_key(geomfits, TFLOAT,  "YEXPAND", &yexp,  NULL, &status);
+    cf_verbose(3,"Y scale expansion factor = %f",yexp) ;
+
+    /* If SPECBINY > 1, scale by Y expansion factor */
+    if (specbiny > 1) {
+       specbiny = (int) (0.5 + (float) specbiny * yexp) ;
+       FITS_update_key(header, TINT, "SPECBINY", &specbiny, NULL, &status) ;
+       cf_verbose(5,"Corrected value of specbiny = %d",specbiny) ;
+    }
+
+    /*
+     *  Read in the X distortion calibration image
+     */
+    FITS_movabs_hdu(geomfits, 2, &hdutype, &status);
+    FITS_read_key(geomfits, TLONG,  "NAXIS1", &xdim_gx,  NULL, &status);
+    FITS_read_key(geomfits, TLONG,  "NAXIS2", &ydim_gx,  NULL, &status);
+    npix_gx = xdim_gx * ydim_gx;
+
+    FITS_read_key(geomfits, TFLOAT, "BSCALE", &scale_gx, NULL, &status);
+    FITS_read_key(geomfits, TFLOAT, "BZERO",  &zero_gx,  NULL, &status);
+    geomx_img = (short *) cf_malloc(sizeof(short) * npix_gx);
+    fits_set_bscale(geomfits, 1., 0., &status);
+    FITS_read_img(geomfits, TSHORT, fpixel, npix_gx, &nullval, geomx_img,
+		  &anynull, &status);
+    /*
+     *  Read the Y distortion calibration image
+     */
+    FITS_movabs_hdu(geomfits, 3, &hdutype, &status);
+    FITS_read_key(geomfits, TLONG,  "NAXIS1", &xdim_gy,  NULL, &status);
+    FITS_read_key(geomfits, TLONG,  "NAXIS2", &ydim_gy,  NULL, &status);
+    npix_gy = xdim_gy * ydim_gy;
+
+    FITS_read_key(geomfits, TFLOAT, "BSCALE", &scale_gy, NULL, &status);
+    FITS_read_key(geomfits, TFLOAT, "BZERO",  &zero_gy,  NULL, &status);
+    geomy_img = (short *) cf_malloc(sizeof(short) * npix_gy);
+    fits_set_bscale(geomfits, 1., 0., &status);
+    FITS_read_img(geomfits, TSHORT, fpixel, npix_gy, &nullval, geomy_img,
+		  &anynull, &status);
+    FITS_close_file(geomfits, &status);
+    /*
+     *  Make sure that the X and Y distortion images are the same size
+     */
+    if (xdim_gx != xdim_gy || ydim_gx != ydim_gy) 
+	cf_if_warning("X and Y distortion images not the same size.");
+    /*
+     *  Use the data in the geometric distortion calibration images to
+     *  correct XFARF and YFARF
+     */
+    for (j=0; j<nevents; j++) {
+	/*
+	 *  Move only events in active region.
+	 */
+	if (!(locflags[j] & LOCATION_SHLD)) {
+	    int xndx = (int) xfarf[j], yndx = (int) yfarf[j], ndx;
+	    /*
+	     *  Check that the y indices are within bounds
+	     */
+	    if (yndx < 0)
+		yndx = 0;
+	    else if (yndx > ydim_gy-1)
+		yndx = ydim_gy-1;
+
+	    ndx = yndx*xdim_gx + xndx;
+	    xfarf[j] += geomx_img[ndx]*scale_gx + zero_gx;
+	    yfarf[j] += geomy_img[ndx]*scale_gy + zero_gy;
+	}
+    }
+    free(geomx_img);
+    free(geomy_img);
+
+    cf_proc_update(header, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done Processing");
+
+    return 0;
+}
diff --git a/src/libcf/cf_grating_motion.c b/src/libcf/cf_grating_motion.c
new file mode 100644
index 0000000..fe50d63
--- /dev/null
+++ b/src/libcf/cf_grating_motion.c
@@ -0,0 +1,432 @@
+/****************************************************************************
+ *	        Johns Hopkins University
+ *	        Center For Astrophysical Sciences
+ *	        FUSE
+ *****************************************************************************
+ *
+ * Synopsis:	cf_grating_motion(header, nevents, time, x, y, channel,
+ *			ntimes, ttime, tsunrise)
+ *
+ * Description: Reads spectral shift caused by thermal grating motions
+ *              and corrects the X and Y locations of each photon event.
+ *
+ *              fitsfile  *header       Pointer to the FITS header of the
+ *                                      Intermediate Data File
+ *              long      nevents       Number of photons in the file
+ *              int       *time         Time (in seconds) since exposure start
+ *              float     *x            Position of the photon (in pixels)
+ *              float     *y            Position of the photon (in pixels)
+ *     unsigned char      channel       Channel ID of each photon
+ *		long	  ntimes	Number of entries in timeline table
+ *		float	  ttime		Time array of timeline table
+ *		short	  tsunrise	Time since last sunrise
+ *
+ * Returns:     0 on success
+ *
+ * History:	09/05/02    1.0  RDR    Begin work; adapted from cf_make_shift
+ *		04/21/03    1.3  wvd	Use tsunrise array from timeline table.
+ *					Do not assume that ttime is continuous.
+ *              05/20/03    1.4  rdr    Added call to cf_proc_check
+ *              08/21/03    1.5  wvd    Change channel to unsigned char.
+ *              06/25/04    1.6  wvd    Estimate time between sunrises using
+ *                                      orbit period in file header.
+ *              03/22/05    1.7  wvd    Change tsunrise from float to short.
+ *                                      Read orbital period from file header.
+ *              04/15/05    1.8  wvd    Close GRAT_CAL file before exiting.
+ *					If ORBPERID keyword is not found,
+ *					assume that orbit period is 6000 s.
+ *		12/30/05    1.9  wvd	Current algorithm corrects for orbital
+ *					drift of spectrum, but wavelength zero
+ *					point still varies with beta angle and
+ *					observation date.  New subroutine
+ *					corrects LiF 1 data for these effects.
+ *		07/06/06    2.0  wvd	Rewrite to use Dave Sahnow's new
+ *					grating-correction file (version 003).
+ *		07/12/06    2.1  wvd	Modify to read an arbitrary number of
+ *					extensions, each with phase information
+ *					in file header keywords.
+ *		10/20/06    2.2  wvd	Grating motion also depends on APER_PA.
+ *					Now we read it from the file header
+ *					and select appropriate coefficients.
+ *					If no correction is defined for a 
+ *					particular set of parameters, set
+ *		11/28/06    2.3  wvd	Grating motion includes a long-term,
+ *					non-periodic drift.  Read it from the
+ *					first four extensions of GRAT_CAL file.
+ *              04/07/07    2.4  wvd	Clean up compiler warnings.
+ *
+ ****************************************************************************/
+
+#include <math.h>
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include "calfuse.h"
+
+static int
+read_nonperiodic_shifts(fitsfile *header, fitsfile *shiftfits, 
+    long ntimes, float *dxlif, float *dylif, float *dxsic, float *dysic)
+{
+    char  channel[FLEN_VALUE], comment[FLEN_CARD], detector[FLEN_VALUE];
+    int   nrows, tndx;
+    int   status=0, hdutype=0, hdunum=0;
+    long  i;
+    float *mjd, *xshift, *yshift;
+    double expstart;
+    
+    /* Read header keywords from data file. */
+    fits_read_key(header, TDOUBLE, "EXPSTART", &expstart, NULL, &status);
+    FITS_read_key(header, TSTRING, "DETECTOR", detector, NULL, &status);
+
+    /* First do the LiF channels */
+    if (!strncmp(detector,"1",1)) {
+         hdunum=2;
+    } else if (!strncmp(detector,"2",1)) {
+         hdunum=4;
+    } else {
+         cf_if_error("Cannot parse DETECTOR keyword in data file.");
+    }
+    cf_verbose(3, "Reading HDU %d of GRAT_CAL file.", hdunum);
+
+    FITS_movabs_hdu(shiftfits, hdunum, &hdutype, &status);
+    FITS_read_key(shiftfits, TSTRING, "CHANNEL", channel, NULL, &status);
+    sprintf(comment, "LiF%c", detector[0]);
+    if (strncmp(channel, comment, 4))
+        cf_if_error("Cannot find %s correction info in extension %d",
+	comment, hdunum);
+
+    /* Read X and Y corrections as a function of time. */
+    nrows = cf_read_col(shiftfits, TFLOAT, "MJD", (void *) &mjd);
+    nrows = cf_read_col(shiftfits, TFLOAT, "XSHIFT", (void *) &xshift);
+    nrows = cf_read_col(shiftfits, TFLOAT, "YSHIFT", (void *) &yshift);
+
+    /* Select appropriate MJD for this exposure. */
+    i = 0;
+    while (expstart > mjd[i] && i < nrows) i++;
+    tndx = i-1;
+    if (tndx < 0) tndx = 0;
+    cf_verbose(3,"EXPSTART = %g", expstart);
+    cf_verbose(3,"Using LiF corrections for MJD >= %g", mjd[tndx]);
+    if (tndx < nrows-1)
+        cf_verbose(3,"                      and MJD <  %g", mjd[tndx+1]);
+    cf_verbose(3,"xshift = %f, yshift = %f", xshift[tndx], yshift[tndx]);
+
+    /* Copy X and Y corrections to output arrays. */
+    for (i = 0; i < ntimes; i++) {
+	dxlif[i] = xshift[tndx];
+	dylif[i] = yshift[tndx];
+    }
+
+    /* Now do the SiC channels */
+    hdunum += 1;
+    cf_verbose(3, "Reading HDU %d of GRAT_CAL file.", hdunum);
+    FITS_movabs_hdu(shiftfits, hdunum, &hdutype, &status);
+    FITS_read_key(shiftfits, TSTRING, "CHANNEL", channel, NULL, &status);
+    sprintf(comment, "SiC%c", detector[0]);
+    if (strncmp(channel, comment, 4))
+        cf_if_error("Cannot find %s correction info in extension %d",
+	comment, hdunum);
+
+    /* Read X and Y corrections as a function of time. */
+    nrows = cf_read_col(shiftfits, TFLOAT, "MJD", (void *) &mjd);
+    nrows = cf_read_col(shiftfits, TFLOAT, "XSHIFT", (void *) &xshift);
+    nrows = cf_read_col(shiftfits, TFLOAT, "YSHIFT", (void *) &yshift);
+
+    /* Select appropriate MJD for this exposure. */
+    i = 0;
+    while (expstart > mjd[i] && i < nrows) i++;
+    tndx = i-1;
+    if (tndx < 0) tndx = 0;
+    cf_verbose(3,"Using SiC corrections for MJD >= %g", mjd[tndx]);
+    if (tndx < nrows-1)
+        cf_verbose(3,"                      and MJD <  %g", mjd[tndx+1]);
+    cf_verbose(3,"xshift = %f, yshift = %f", xshift[tndx], yshift[tndx]);
+
+    /* Copy X and Y corrections to output arrays. */
+    for (i = 0; i < ntimes; i++) {
+	dxsic[i] = xshift[tndx];
+	dysic[i] = yshift[tndx];
+    }
+
+    return 0;
+}
+
+
+static int
+read_periodic_shifts(fitsfile *header, fitsfile *shiftfits, int ncorrection,
+    double *lif_mjd0, double *lif_period, double *sic_mjd0, double *sic_period,
+    double *lif_x_coef, double *lif_y_coef, double *sic_x_coef, double *sic_y_coef)
+{
+    char  detector[FLEN_CARD], channel[FLEN_CARD], comment[FLEN_CARD];
+    int   status=0, hdutype=0, hdunum=0, anynul=0;
+    int   i, nregions, region, typecode;
+    long  max_coeff, ncoeff, width;
+    float aper_pa, *aperpalo, *aperpahi;
+    float *betalo, *betahi, *polelo, *polehi;
+    double beta, pole, sunang;
+    
+    /* Initialize variables. */
+    *lif_mjd0 = *lif_period = *sic_mjd0 = *sic_period = 0.;
+    for (i = 0; i < 11; i++) {
+	lif_x_coef[i] = 0.;
+	lif_y_coef[i] = 0.;
+	sic_x_coef[i] = 0.;
+	sic_y_coef[i] = 0.;
+    }
+
+    FITS_read_key(header, TFLOAT,  "APER_PA", &aper_pa, NULL, &status);
+    FITS_read_key(header, TDOUBLE, "SUNANGLE", &sunang, NULL, &status);
+    FITS_read_key(header, TDOUBLE, "POLEANGL", &pole, NULL, &status);
+    FITS_read_key(header, TSTRING, "DETECTOR", detector, NULL, &status);
+    while (999.9 > aper_pa && aper_pa > 360.) aper_pa -= 360.;
+    while (aper_pa < 0.) aper_pa += 360.;
+    beta = 180.0 - sunang;
+
+    cf_verbose(3, "S/C orientation: beta = %5.1f, pole = %5.1f, aper_pa = %5.1f",
+	beta, pole, aper_pa);
+
+    /* First do the LiF channels */
+    if (!strncmp(detector,"1",1)) {
+         hdunum=2;
+    } else if (!strncmp(detector,"2",1)) {
+         hdunum=4;
+    } else {
+         cf_if_error("Cannot parse DETECTOR keyword in read_shift_file");
+    }
+    hdunum += ncorrection * 4;
+    cf_verbose(3, "Reading HDU %d of GRAT_CAL file.", hdunum);
+
+    FITS_movabs_hdu(shiftfits, hdunum, &hdutype, &status);
+    FITS_read_key(shiftfits, TSTRING, "CHANNEL", channel, NULL, &status);
+    sprintf(comment, "LiF%c", detector[0]);
+    if (strncmp(channel, comment, 4))
+        cf_if_error("Cannot find %s correction info in extension %d",
+	comment, hdunum);
+
+    if (ncorrection > 1) {
+	FITS_read_key(shiftfits, TDOUBLE, "PERIOD", lif_period, NULL, &status);
+	FITS_read_key(shiftfits, TDOUBLE, "MJD_ZERO", lif_mjd0, NULL, &status);
+	cf_verbose(3, "%s: period = %g, mjd_zero = %g",
+		channel, *lif_period, *lif_mjd0);
+    }
+    
+    nregions = cf_read_col(shiftfits, TFLOAT, "BETALO", (void *) &betalo);
+    nregions = cf_read_col(shiftfits, TFLOAT, "BETAHI", (void *) &betahi);
+    nregions = cf_read_col(shiftfits, TFLOAT, "POLELO", (void *) &polelo);
+    nregions = cf_read_col(shiftfits, TFLOAT, "POLEHI", (void *) &polehi);
+    nregions = cf_read_col(shiftfits, TFLOAT, "APERPALO", (void *) &aperpalo);
+    nregions = cf_read_col(shiftfits, TFLOAT, "APERPAHI", (void *) &aperpahi);
+    FITS_get_coltype(shiftfits, 7, &typecode, &ncoeff, &width, &status);
+    max_coeff = ncoeff;
+
+    for (i = 0; i < nregions; i++) 
+	if (betalo[i] <= beta && beta < betahi[i] &&
+	    polelo[i] <= pole && pole < polehi[i] &&
+	    aperpalo[i] <= aper_pa && aper_pa < aperpahi[i]) break;
+
+    if (i == nregions) 
+	cf_verbose(3, "LiF correction not defined for beta = %g, pole = %g, "
+	"aper_pa = %g", beta, pole, aper_pa);
+    else {
+	cf_verbose(3, "LIF REGION %2d: beta = %g - %g, pole = %g - %g,", 
+	i, betalo[i], betahi[i], polelo[i], polehi[i]);
+	cf_verbose(3, "                aper_pa = %g - %g, %d coefficients",
+	aperpalo[i], aperpahi[i], ncoeff);
+
+	region = i+1; 		/* CFITSIO counts from 1, not 0. */
+	FITS_read_col(shiftfits, TDOUBLE, 7, region, 1, ncoeff, NULL, lif_x_coef,
+	&anynul, &status);
+	FITS_read_col(shiftfits, TDOUBLE, 8, region, 1, ncoeff, NULL, lif_y_coef,
+	&anynul, &status);
+    }
+
+    /* Now the SiC channels */
+    hdunum += 1;
+    cf_verbose(3, "Reading HDU %d of GRAT_CAL file.", hdunum);
+    FITS_movabs_hdu(shiftfits, hdunum, &hdutype, &status);
+    FITS_read_key(shiftfits, TSTRING, "CHANNEL", channel, NULL, &status);
+    sprintf(comment, "SiC%c", detector[0]);
+    if (strncmp(channel, comment, 4))
+        cf_if_error("Cannot find %s correction info in extension %d", 
+	comment, hdunum);
+
+    if (ncorrection > 1) {
+	FITS_read_key(shiftfits, TDOUBLE, "PERIOD", sic_period, NULL, &status);
+	FITS_read_key(shiftfits, TDOUBLE, "MJD_ZERO", sic_mjd0, NULL, &status);
+	cf_verbose(3, "%s: period = %g, mjd_zero = %g",
+		channel, *sic_period, *sic_mjd0);
+    }
+    
+    nregions = cf_read_col(shiftfits, TFLOAT, "BETALO", (void *) &betalo);
+    nregions = cf_read_col(shiftfits, TFLOAT, "BETAHI", (void *) &betahi);
+    nregions = cf_read_col(shiftfits, TFLOAT, "POLELO", (void *) &polelo);
+    nregions = cf_read_col(shiftfits, TFLOAT, "POLEHI", (void *) &polehi);
+    nregions = cf_read_col(shiftfits, TFLOAT, "APERPALO", (void *) &aperpalo);
+    nregions = cf_read_col(shiftfits, TFLOAT, "APERPAHI", (void *) &aperpahi);
+    FITS_get_coltype(shiftfits, 7, &typecode, &ncoeff, &width, &status);
+    if (max_coeff < ncoeff) max_coeff = ncoeff;
+
+    for (i = 0; i < nregions; i++)
+        if (betalo[i] <= beta && beta < betahi[i] &&
+            polelo[i] <= pole && pole < polehi[i] &&
+	    aperpalo[i] <= aper_pa && aper_pa < aperpahi[i]) break;
+
+    if (i == nregions) 
+	cf_verbose(3, "SiC correction not defined for beta = %g, pole = %g, "
+	"aper_pa = %g", beta, pole, aper_pa);
+    else {
+	cf_verbose(3, "SIC REGION %2d: beta = %g - %g, pole = %g - %g,",
+	i, betalo[i], betahi[i], polelo[i], polehi[i]);
+	cf_verbose(3, "                aper_pa = %g - %g, %d coefficients",
+	aperpalo[i], aperpahi[i], ncoeff);
+
+	region = i+1; 		/* CFITSIO counts from 1, not 0. */
+	FITS_read_col(shiftfits, TDOUBLE, 7, region, 1, ncoeff, NULL, sic_x_coef,
+	    &anynul, &status);
+	FITS_read_col(shiftfits, TDOUBLE, 8, region, 1, ncoeff, NULL, sic_y_coef,
+	    &anynul, &status);
+    }
+
+    cf_verbose(2, "Fourier coefficients of grating-motion correction:");
+    cf_verbose(2,"    LiF X      LiF Y      SiC X      SiC Y");
+    for (i=0; i<max_coeff; i++) {
+	cf_verbose(2, "%10.5f %10.5f %10.5f %10.5f",lif_x_coef[i],
+	       lif_y_coef[i], sic_x_coef[i], sic_y_coef[i]);
+    }
+
+    return 0;
+}
+
+
+static double
+thermal_shift(double theta, double *a)
+{
+    theta *= 2.0 * PI;
+    return      (a[0]+
+		 a[1]*sin(1.0*theta)+a[2]*cos(1.0*theta)+
+		 a[3]*sin(2.0*theta)+a[4]*cos(2.0*theta)+
+		 a[5]*sin(3.0*theta)+a[6]*cos(3.0*theta)+
+		 a[7]*sin(4.0*theta)+a[8]*cos(4.0*theta)+
+		 a[9]*sin(5.0*theta)+a[10]*cos(5.0*theta));
+}
+
+
+int
+cf_grating_motion(fitsfile *header, long nevents, float *time, float *x,
+	float *y, unsigned char *channel, long ntimes, float *ttime,
+	short *tsunrise)
+{
+    char CF_PRGM_ID[] = "cf_grating_motion";
+    char CF_VER_NUM[] = "2.4";
+
+    char     shift_file[FLEN_CARD];
+    int      errflg=0, status=0;
+    int      calfvers, num_hdus, ncorrections;
+    long     i, j, k;
+    float    *dxlif, *dylif, *dxsic, *dysic, period;
+    double   lif_mjd0, lif_period, sic_mjd0, sic_period;
+    double   expstart, phase, lif_phase, sic_phase;
+    double   lif_x_coef[11], lif_y_coef[11], sic_x_coef[11], sic_y_coef[11];
+    fitsfile *shiftfits;
+
+    /* Initialize error checking. */
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+    /* Enter a time stamp into the log */
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    /* Check whether routine is appropriate for this data file. */
+    if ((errflg = cf_proc_check(header, CF_PRGM_ID))) return errflg;
+
+    /* Read exposure start time from IDF header. */
+    fits_read_key(header, TDOUBLE, "EXPSTART", &expstart, NULL, &status);
+
+    /* Read orbital period from IDF header. If not found, estimate. */
+    fits_read_key(header, TFLOAT, "ORBPERID", &period, NULL, &status);
+    if (status) {
+	status = 0;
+	period = 6000;
+	cf_verbose(1, "Keyword ORBPERID not found; assuming 6000 seconds.");
+    }
+    else
+	cf_verbose(2, "Estimated orbital period is %d seconds", cf_nint(period));
+
+    /* Allocate space for shift arrays. */
+    dxlif = (float *) cf_calloc(ntimes, sizeof(float));
+    dylif = (float *) cf_calloc(ntimes, sizeof(float));
+    dxsic = (float *) cf_calloc(ntimes, sizeof(float));
+    dysic = (float *) cf_calloc(ntimes, sizeof(float));
+
+    /* Open the GRAT_CAL file, check version number, and count extensions. */
+    FITS_read_key(header, TSTRING, "GRAT_CAL", shift_file, NULL, &status);
+    FITS_open_file(&shiftfits, cf_cal_file(shift_file), READONLY, &status);
+    FITS_get_num_hdus(shiftfits, &num_hdus, &status);
+    cf_verbose(3, "GRAT_CAL file %s contains %d HDUs.", shift_file, num_hdus);
+    ncorrections = num_hdus / 4;
+
+    /* Exit if the CALFVERS keyword is less than 4. */
+    FITS_read_key(shiftfits, TINT, "CALFVERS", &calfvers, NULL, &status);
+    if (calfvers < 4) 
+        cf_if_error("Grating-calibration file format is out of date.");
+
+    /* First correct for the long-term, non-periodic grating motions. */
+    read_nonperiodic_shifts(header, shiftfits, ntimes, dxlif, dylif, dxsic, dysic);
+
+    /* Next correct for periodic motions. */
+    for (i = 1; i < ncorrections; i++) {
+
+	/* Read the calibration file.  If there's no correction for this spacecraft
+	orientation, the coefficients will be set to zero. */
+	read_periodic_shifts(header, shiftfits, i, &lif_mjd0, &lif_period, &sic_mjd0,
+	    &sic_period, lif_x_coef, lif_y_coef, sic_x_coef, sic_y_coef);
+
+	/* For orbital motions, the period is just the orbit period. */
+	if (i == 1) {
+	    for (k=0; k<ntimes; k++) {
+		phase = tsunrise[k]/period;
+		dxlif[k] += thermal_shift(phase, lif_x_coef);
+		dylif[k] += thermal_shift(phase, lif_y_coef);
+		dxsic[k] += thermal_shift(phase, sic_x_coef);
+		dysic[k] += thermal_shift(phase, sic_y_coef);
+	    }
+	}
+	/* For longer-term motions, read the period and zero point from the file header. */
+	else {
+	    for (k=0; k<ntimes; k++) {
+		lif_phase = ((expstart - lif_mjd0) + ttime[k]/(24.*3600.))/lif_period;
+		sic_phase = ((expstart - sic_mjd0) + ttime[k]/(24.*3600.))/sic_period;
+		dxlif[k] += thermal_shift(lif_phase, lif_x_coef);
+		dylif[k] += thermal_shift(lif_phase, lif_y_coef);
+		dxsic[k] += thermal_shift(sic_phase, sic_x_coef);
+		dysic[k] += thermal_shift(sic_phase, sic_y_coef);
+	    }
+	}
+    }
+
+    /* Close the GRAT_CAL file. */
+    FITS_close_file(shiftfits, &status);
+
+    /* Apply grating-motion correction. */
+    for (j=k=0; j<nevents; j++) {
+        while(ttime[k+1] - FRAME_TOLERANCE < time[j] && k+1 < ntimes) k++;
+	if (channel[j] > 0 && channel[j] < 4) {
+	    x[j] += dxlif[k];
+	    y[j] += dylif[k];
+	}
+	else if (channel[j] > 4) {
+	    x[j] += dxsic[k];
+	    y[j] += dysic[k];
+	} 
+    }
+    
+    /* Release memory. */
+    free(dxlif);
+    free(dylif);
+    free(dxsic);
+    free(dysic);
+
+    cf_proc_update(header, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished execution.");
+
+    return status;
+}
diff --git a/src/libcf/cf_header_io.c b/src/libcf/cf_header_io.c
new file mode 100644
index 0000000..d534ac2
--- /dev/null
+++ b/src/libcf/cf_header_io.c
@@ -0,0 +1,110 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_copy_to_memory(*infile, **memp);
+ *
+ * Description: Returns an in-memory FITS file pointer
+ *
+ *
+ * Arguments:   char     *infile        Input data file name
+ *	        fitsfile **memp         In memory FITS file pointer
+ *
+ * Returns:     None
+ *
+ * History:     08/15/2002  1.0   jch   Initial coding
+ *              12/18/03          bjg   Change calfusettag.h to calfuse.h
+ *
+ ****************************************************************************/
+
+
+#include <string.h>
+#include <stdio.h>
+#include "calfitsio.h"
+#include "calfuse.h"
+
+void
+cf_read_header(char *infile, fitsfile **memp)
+{
+    fitsfile *ip;       /* input file pointer */
+    int	status=0;       /* status used in CFITSIO */
+
+    /* open the input file */
+    FITS_open_file(&ip, infile, READONLY, &status);
+
+    /* create the temp file in memory */
+    FITS_create_file(memp, "mem://", &status);
+
+    /* copy the input primary HDU to the temp file */
+    FITS_copy_hdu(ip, *memp, 0, &status);
+
+    /* close the input file */
+    FITS_close_file(ip, &status);
+}
+
+
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_copy_to_file(*memp, *outfile);
+ *
+ * Description: Copy the header in the in-memory FITS file to an output FITS
+ *              file's primary HDU.
+ *
+ *
+ * Arguments:   fitsfile *memp          In memory FITS file pointer
+ *              char     *outfile       Output data file name
+ *
+ * Returns:     None
+ *
+ * History:     08/15/2002  jch   1.0   Initial coding
+ *
+ ****************************************************************************/
+
+void
+cf_write_header(fitsfile *memp, char *outfile)
+{
+    fitsfile *op;       /* output file pointer */
+    int	status=0;       /* status used in CFITSIO */
+
+    int	ncards_memp, ncards_op, morekeys=0;
+    char card[FLEN_CARD];
+
+    /* Open the output FITS file. */
+    FITS_open_file(&op, outfile, READWRITE, &status);
+
+    fits_get_hdrspace(memp, &ncards_memp, &morekeys, &status);
+    fits_get_hdrspace(op,   &ncards_op,   &morekeys, &status);
+	
+    /* overwrite output file's primary HDU card by card */
+    if (ncards_op >= ncards_memp) {
+	int i;
+	for (i=1; i<=ncards_memp; i++) {
+	    FITS_read_record(memp, i, card, &status);
+	    FITS_modify_record(op, i, card, &status);
+	}
+	/* delete from the bottom */
+	for (i=ncards_op; i>=ncards_memp+1; i--) {
+	    FITS_delete_record(op, i, &status);
+	}
+    }
+    else {
+	int i;
+	for (i=1; i<=ncards_op; i++) {
+	    FITS_read_record(memp, i, card, &status);
+	    FITS_modify_record(op, i, card, &status);
+	}
+	for (i=ncards_op+1; i<=ncards_memp; i++) {
+	    FITS_read_record(memp, i, card, &status);
+	    FITS_write_record(op, card, &status);
+	}
+    }
+
+    /* close output file. */
+    FITS_close_file(op, &status);
+}
diff --git a/src/libcf/cf_identify_channel.c b/src/libcf/cf_identify_channel.c
new file mode 100644
index 0000000..7d6a8e3
--- /dev/null
+++ b/src/libcf/cf_identify_channel.c
@@ -0,0 +1,201 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE 
+ *****************************************************************************
+ *
+ * Synopsis:    cf_identify_channel(fitsfile *header, long nevents,
+ *              float *xfarf, float *yfarf, unsigned char *chan, 
+ *		unsigned char *locflags, int pad, int final_call)
+ *
+ * Description: Assigns an aperture to each photon in the IDF.
+ *
+ *		Change of logic in v1.11: This routine may be called
+ *		multiple times.  All photons are examined and assigned to
+ *		a channel unless final_call = TRUE.  On the final call, only
+ *		photons with channel > 0 are considered.  Because only photons
+ *		assigned to a channel are motion corrected, the spectrum can
+ *		move on top of previously-rejected photons.  We don't want
+ *		to include them in the final spectrum, so leave their channel
+ *		values unchanged.
+ *
+ *		Change of logic in v1.16: We've decided to use extended-
+ *		source apertures for the non-target channels.  These
+ *		apertures can overlap, so we assign disputed photons to
+ *		their most likely source.  In decreasing order, these are
+ *		the target aperture, the larger non-target aperture, and
+ *		the smaller non-target aperture.
+ *		
+ * Arguments:   fitsfile  *header       Pointer to the location of the FITS
+ *                                      header of the Intermediate Data File
+ *              long      nevents       Number of photons in the file
+ *              float     *xfarf        X positions for each photon event
+ *              float     *yfarf        Y positions for each photon event
+ *     unsigned char      *chan         Pointer to pointer to the array 
+ *                                      containing the channel information
+ *     unsigned char      *locflags     Location flags for each photon 
+ *              int       pad           Switch saying whether to expand the
+ *                                      width of the tabulated extraction
+ *                                      window (yes if > 0). The number refers
+ *                                      to the amount of padding (e.g. pad=5
+ *                                      will add 5 pixels to each side of the
+ *                                      extraction window.
+ *		int	  final_call	This subroutine may be called
+ *					many times.  The last time, set
+ *					final_call = TRUE.
+ *
+ * Return:      0 on success
+ *
+ * History:     08/09/02    1.0  RDR    Begin work 
+ *              09/04/02    1.1  rdr    Change program so that it just fills
+ *                                      the channel array rather than creating
+ *                                      and filling it.  Decreased the size of
+ *                                      the mask.  Use the value of pad to
+ *                                      specify degree of window padding.
+ *                                      Check for extended source.
+ *              12/11/02    1.2  RDR    Adjust aperture limits by measured
+ *                                      y centroid (if available)
+ *              02/11/03    1.3  rdr    changed test for ycent values
+ *              02/12/03    1.6  wvd    Don't crash if YCENT# is undefined
+ *              03/25/03    1.7  rdr    Ignore pinhole aperture 
+ *		03/31/03    1.10 wvd    Ignore regions where YMAX = YMIN + 1.
+ *					They are not valid channel regions.
+ *		04/07/03    1.11 wvd    Shift channel boundaries to match FPA
+ *					positions.  Implement use of cf_verbose.
+ *					Update CHID_COR if final_call = TRUE.
+ *              05/20/03    1.12 rdr    Added call to cf_proc_check
+ *              07/23/03    1.14 rdr    Correct procedure which reads CHID
+ *                                      calibration file
+ *		08/21/03    1.15 wvd    Change channel to unsigned char.
+ *		08/25/03    1.16 wvd    Use extended windows for non-target
+ *					apertures.  Replace aperture mask
+ *					with a grid of aperture limits.
+ *					Use cf_nint() to round floats.
+ *              08/25/03    1.17 wvd    Change coltype from string to int
+ *					in cf_read_col.
+ *              09/08/03    1.18 wvd    Default value is channel[i] = 0.
+ *					Identify low and high values of x 
+ *					by setting y limits to -NYMAX.
+ *              09/18/03    1.19 wvd    Consider only photons falling on the
+ *					active area of the detector.
+ *              11/12/03    1.20 wvd    Don't bother with non-target channels
+ *					in HIST mode.
+ *              06/14/04    1.21 wvd    Don't bother shifting extraction
+ *					windows to correct for FPA position.
+ *					If known, shift is not needed.
+ *              06/17/04    1.22 wvd    Because the extraction windows don't
+ *					quite match the WGTS arrays, we pad
+ *					windows by XPAD pixels in X.
+ *              07/21/04    1.23 wvd    Change i from long to int.
+ *              03/15/05    1.24 wvd    Call cf_extraction_limits to get limits
+ *					of extraction windows, rather than
+ *					reading CHID_CAL file directly.
+ *					Do not pad windows in X.
+ *              03/16/05    1.25 wvd    Pass srctype to cf_extraction_limits.
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include "calfuse.h"
+
+int
+cf_identify_channel(fitsfile* header, long npts, float* x, float* y,
+	unsigned char* channel, unsigned char* locflags, int pad,
+	int final_call)
+{
+    char CF_PRGM_ID[] = "cf_identify_channel";
+    char CF_VER_NUM[] = "1.25";
+
+    char  instmode[FLEN_VALUE], zero=0;
+    int   errflg=0, extended, n_chan=6, status=0;
+    int   active_ap[2], chan, srctype[8];
+    int   i;	/* Always steps through targ_ap */
+    int   *targ_ap,
+	  lwrs[]={3,7,2,6,1,5},	/* LWRS, MDRS, HIRS (LiF & SiC) */
+	  mdrs[]={2,6,3,7,1,5},	/* MDRS, LWRS, HIRS (LiF & SiC) */
+	  hirs[]={1,5,3,7,2,6};	/* HIRS, LWRS, MDRS (LiF & SiC) */
+    long  j,	/* Always steps through extraction window arrays */
+	  k;	/* Always steps through photon list */
+    short xint, yint, xmin, xmax, *ymin[6], *ymax[6];
+
+    /* Initialize error checking */ 
+     cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+    /* Enter a time stamp into the log */
+     cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    /* Check whether routine is appropriate for this data file. */
+     if ((errflg = cf_proc_check(header, CF_PRGM_ID))) return errflg;
+
+    /* If data were taken in HIST mode, ignore non-target channels. */
+     FITS_read_key(header, TSTRING, "INSTMODE", instmode, NULL, &status);
+     if (!strncmp(instmode, "HIST", 4)) n_chan = 2;
+
+    /* Determine source type and active apertures */
+     extended = cf_source_aper(header, active_ap);
+
+    /* Set the order in which we will assign photons to channels. */
+     switch (active_ap[0]) {
+	case 1: targ_ap = hirs;
+		break;
+	case 2: targ_ap = mdrs;
+		break;
+	default: targ_ap = lwrs;
+		break;
+     }
+
+    /* For target apertures, srctype reflects target.
+	Use extended apertures for the rest. */
+     for (i = 0; i < 2;  i++) srctype[i] = extended;
+     for ( ; i < n_chan; i++) srctype[i] = 1;
+
+    /* While we're at it, here's one more bit of i/o. */
+     if (pad > 0)
+        cf_verbose(3, "Padding extraction windows by %d Y pixels", pad);
+ 
+    /* 
+     * Loop through all channels, read extraction limits,
+     * and apply any requested padding.
+     */
+     for (i = 0; i < n_chan; i++) {
+	chan = targ_ap[i];
+
+       /* Read the extraction limits for this aperture. */
+	(void) cf_extraction_limits(header, chan, srctype[i],
+	    (ymin+i), (ymax+i), &xmin, &xmax);
+ 
+	/* Add any padding requested by the user.  */
+	if (pad > 0) {
+	    for (j = xmin; j <= xmax; j++) {
+		ymin[i][j] -= pad;
+		ymax[i][j] += pad;
+	    }
+	}
+    }
+
+    /* Loop through photon list.  Assign a channel ID to each. */
+    cf_verbose(3, "Entering loop to assign channel ID's.");
+    for (k = 0; k < npts; k++) {
+	if (final_call && channel[k] == zero) continue;
+	channel[k] = zero;
+	if (!(locflags[k] & LOCATION_SHLD)) {
+	    xint = (short) cf_nint(x[k]);
+	    yint = (short) cf_nint(y[k]);
+	    if (xint < xmin || xint > xmax) continue;
+	    for (i = 0; i < n_chan; i++) {
+	        if (yint >= ymin[i][xint] && yint <= ymax[i][xint]) {
+		    channel[k] = (char) targ_ap[i];
+		    break;
+		}
+	    }
+	}
+    } 
+
+  /* If final_call = TRUE, update IDF header keyword for this subroutine. */
+     if (final_call) 
+	cf_proc_update(header, CF_PRGM_ID, "COMPLETE");
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done Processing");
+
+    return status;
+}
diff --git a/src/libcf/cf_idf_io.c b/src/libcf/cf_idf_io.c
new file mode 100644
index 0000000..8d8d43a
--- /dev/null
+++ b/src/libcf/cf_idf_io.c
@@ -0,0 +1,161 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    npts = cf_read_col(fitsfile, coltype, colname, colval) 
+ *
+ * Description: Procedure to read the values from a column in a FUSE
+ *              Intermediate Data File (IDF).
+ *		Because floating-point data may be stored as shorts,
+ *		must convert data to type expected by calling routine.
+ *
+ * Variables:   fitsfile  *fileptr      Pointer to the input file
+ *              int       coltype       Data type of the column
+ *					  (TBYTE, TDOUBLE, TSHORT, or TFLOAT)
+ *              char      *colname      Name of the column to re read
+ *                                        (e.g. TIME or XFARF)
+ *              void      **colval      Address of the array containing
+ *                                      the data (must be cast to void)
+ *
+ * Return:      long      npts          Number of points in the array
+ *
+ * Example:
+ *              fitsfile *infits ;
+ *              long npts ;
+ *              float *xfarf ;
+ *       
+ *              FITS_open_file(&infits, argv[1], READWRITE, &status); 
+ *              npts = cf_read_col(infits, TFLOAT, "XFARF", (void **) &xfarf); 
+ *
+ * History:     08/08/02    rdr		Begin work
+ *		06/11/03    wvd  v1.4  	Pass coltype from calling routine.
+ *		08/25/03    wvd  v1.5  	Change coltype from string to int.
+ *		08/28/03    wvd  v1.6  	Use CASEINSEN in calls to
+ *					fits_get_colnum
+ *              12/18/03    bjg  v1.7   Change calfusettag.h to calfuse.h
+ *              04/28/05    wvd  v1.8   Allow arrays to be read as doubles.
+ *              08/24/07    wvd  v1.9   Read nrows as type TLONG.
+ *
+ *************************************************************************/
+
+#include <string.h>
+#include "calfuse.h"
+
+long
+cf_read_col(fitsfile *infits, int coltype, char *colname, void **colval)
+{
+    int  colnum, tcode, intnull=0, anynull, status=0;
+    long nrows, width, repeat, nentries;
+
+    /* Get the column number of the column to be extracted. */
+    FITS_get_colnum(infits, CASEINSEN, colname, &colnum, &status);
+
+    /* Determine the properties of the column. */
+    fits_get_coltype(infits, colnum, &tcode, &repeat, &width, &status);
+
+    /* Read the number of rows in the table. */
+    FITS_read_key(infits, TLONG, "NAXIS2", &nrows, NULL, &status);
+
+    /* Calculate the number of entries in the table. */
+    nentries = nrows * repeat;
+
+    /* Set tcode and width to values expected by calling routine. */
+    if (coltype == TFLOAT) {
+        tcode = TFLOAT;        
+        width = (long) sizeof (float);
+    }
+    if (coltype == TDOUBLE) {
+        tcode = TDOUBLE;        
+        width = (long) sizeof (double);
+    }
+
+    /* Allocate space for the file. */
+    *colval = (void *) cf_malloc(nentries * width);
+    
+    /* Read the data from the file. */
+    FITS_read_col(infits, tcode, colnum, 1, 1, nentries, &intnull, *colval,
+		  &anynull, &status); 
+
+    return nentries;
+}
+
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_write_col(fitsfile, colname, colval, npts) 
+ *
+ * Description: Procedure to write an array into a specified column of a
+ *              FUSE Intermediate Data File (IDF).
+ *		Because floating-point data may be stored as shorts,
+ *		data type of array may not match that of output file header.
+ *
+ * Variables:   fitsfile  *fileptr      Pointer to the input file
+ *              int       coltype       Data type of the column
+ *					  (TBYTE, TDOUBLE, TSHORT, or TFLOAT)
+ *              char      *colname      Name of the column to re read
+ *                                        (e.g. TIME or XFARF)
+ *              void      **colval      Address of the array containing
+ *                                      the data (must be cast to void)
+ *              long      npts          Number of points in the array
+ *
+ * Reture:	status
+ *
+ * Example:
+ *              fitsfile *infits ;
+ *              long npts=100 ;
+ *              float *xfarf ;
+ *       
+ *              FITS_open_file(&infits, argv[1], READWRITE, &status);
+ *              npts = cf_read_col(infits, TFLOAT, "XFARF", (void **) &xfarf);
+ *
+ * History:     08/08/02    rdr         Begin work
+ *		06/11/03    wvd  v1.4  	Pass coltype from calling routine.
+ *					Check for overflow in X arrays.
+ *		08/25/03    wvd  v1.5  	Change coltype from string to int.
+ *		08/28/03    wvd  v1.6  	Use CASEINSEN in calls to
+ *					fits_get_colnum
+ *
+ *************************************************************************/
+
+int
+cf_write_col(fitsfile *infits, int coltype, char *colname, void *colval,
+	long npts)
+{
+    int  colnum, tcode, status=0;
+    long i, width, nevents;
+
+    /* Get the column number of the column to be written. */
+    FITS_get_colnum(infits, CASEINSEN, colname, &colnum, &status);
+
+    /* Determine the properties of the column. */
+    fits_get_coltype(infits, colnum, &tcode, &nevents, &width, &status);
+
+    /* 
+     * If the calling routine and the IDF differ on the data type of this
+     * array, use the data type from the calling routine.
+     */
+    if (coltype == TFLOAT) {
+        tcode = TFLOAT;        
+        width = (long) sizeof (float);
+    }
+
+    /* Check for overflow in X arrays. */
+    if (!strncmp(colname, "X", 1)) {
+	float *x;
+	x = (float *) colval;
+	for (i = 0; i < nevents; i++) {
+            if (x[i] < 0) x[i] = 0.;
+            if (x[i] > NXMAX - 1) x[i] = NXMAX - 1;
+	}
+    }
+
+    /* Write the data to the relevant column. */
+    FITS_write_col(infits, tcode, colnum, 1, 1, npts, colval, &status);
+
+    return status;
+}
diff --git a/src/libcf/cf_ids_dead_time.c b/src/libcf/cf_ids_dead_time.c
new file mode 100644
index 0000000..656222e
--- /dev/null
+++ b/src/libcf/cf_ids_dead_time.c
@@ -0,0 +1,109 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_ids_dead_time(fitsfile *header, long nseconds,
+ *                               float *aic_rate, float *ids_dtc)
+ *
+ * Description: Computes the weighting factor needed to correct
+ *		for the IDS dead time.
+ *
+ * Arguments:   fitsfile  *header       Pointer to FITS file containing the
+ *                                      header of the intermediate data file
+ *              long      nseconds      The number of timeline values
+ *              float     *aic_rate     An array of Active Image Counter
+ *                                      values
+ *              float     *ids_dtc      Dead-time correction array (returned)
+ *
+ * Calls:
+ *
+ * Return:      0  on success
+ *
+ * History:     10/27/02   1.1    peb   Begin work
+ *              11/11/02   1.2    peb   Correct function description and add
+ *                                      cf_timestamp after IDS__COR check.
+ *              12/09/02   1.4    wvd   Calculate DT correction for each time
+ *                                      step, then apply to photons.
+ *                                      Set keyword IDS_DEAD.
+ *              05/20/03   1.5    rdr   Add proc_check call.
+ *		08/01/03   1.8    wvd   Just calculate correction; don't
+ *					apply it.  Return ids_dtc array.
+ *		08/04/03   1.9    wvd   Convert aic_rate to type short.
+ *		11/26/03   1.10   wvd   Convert aic_rate to type float.
+ *		02/09/04   1.11   wvd   max_ids_rate depends on instrument
+ *					mode. For TTAG data, include time
+ *					stamps in aic_rate.
+ *		04/07/07   1.12   wvd   Clean up compiler warnings.
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include "calfuse.h"
+
+int
+cf_ids_dead_time(fitsfile *header, long nseconds, float *aic_rate,
+	float *ids_dtc)
+{
+    char CF_PRGM_ID[] = "cf_ids_dead_time";
+    char CF_VER_NUM[] = "1.12";
+
+    char elecfile[FLEN_VALUE], instmode[FLEN_VALUE];
+    int  errflg=0, status=0;
+    long  k;
+    float ids_rate, tstamps, ttperiod;
+    float mean_ids_dtc = 0.;
+    float max_ids_rate = 1.;
+    fitsfile *elecfits;
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+    if ((errflg = cf_proc_check(header, CF_PRGM_ID))) return errflg;
+    /*
+     *  Read observing mode and interval between time stamps.
+     */
+    FITS_read_key(header, TSTRING, "INSTMODE", instmode, NULL, &status);
+    FITS_read_key(header, TFLOAT, "TTPERIOD", &ttperiod, NULL, &status);
+    /*
+     *  Compute number of time stamps per second (0 for HIST data).
+     */
+    if (!strncmp(instmode, "TTAG", 4)) 		/* TTAG MODE */
+	if (ttperiod > 1e-8) tstamps = 1./ttperiod;
+	else tstamps = 1.;
+    else					/* HIST MODE */
+	tstamps = 0.;
+    /*
+     *  Maximum IDS rate depends on instrument mode.
+     */
+    FITS_read_key(header, TSTRING, "ELEC_CAL", elecfile, NULL, &status);
+    FITS_open_file(&elecfits, cf_cal_file(elecfile), READONLY, &status);
+    if (!strncmp(instmode, "TTAG", 4)) 
+        FITS_read_key(elecfits, TFLOAT, "TTAG_BUS", &max_ids_rate, NULL, &status);
+    else
+        FITS_read_key(elecfits, TFLOAT, "HIST_BUS", &max_ids_rate, NULL, &status);
+    FITS_close_file(elecfits, &status);
+    cf_verbose(4, "max_ids_rate = %f", max_ids_rate);
+    /*
+     *  Calculate the IDS dead-time correction.
+     */
+    for (k=0; k<nseconds; k++) {
+        ids_rate = aic_rate[k] + tstamps;
+
+	if (ids_rate > max_ids_rate)
+	    ids_dtc[k] = ids_rate/max_ids_rate;
+	else
+	    ids_dtc[k] = 1.0;
+        mean_ids_dtc += ids_dtc[k];
+    }
+    /*
+     *  Write mean IDS dead-time correction to file header.
+     */
+    mean_ids_dtc /= nseconds;
+    cf_verbose(2, "Mean IDS dead-time correction: %f", mean_ids_dtc);
+    FITS_update_key(header, TFLOAT, "IDS_DEAD", &mean_ids_dtc, NULL, &status);
+
+    cf_proc_update(header, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return 0;
+}
diff --git a/src/libcf/cf_init_support.c b/src/libcf/cf_init_support.c
new file mode 100644
index 0000000..68db0f6
--- /dev/null
+++ b/src/libcf/cf_init_support.c
@@ -0,0 +1,1344 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Description: Routines used by cf_ttag_init and cf_hist_init.
+ *              
+ * History:     07/15/03  v1.1	wvd   Move routines from cf_ttag_init
+ *		07/24/03   1.2  wvd   If tsunrise and tsunset get huge, 
+ *					store them as floats, not integers.
+ *		07/30/03   1.5  wvd   Omit TZERO and TSCALE for these 
+ *					timeline table entries:
+ *					HIGH_VOLTAGE
+ *					LIF_CNT_RATE
+ *					SIC_CNT_RATE
+ *					FEC_CNT_RATE
+ *					AIC_CNT_RATE
+ *					BKGD_CNT_RATE
+ *					This will effectively convert them
+ *					to arrays of shorts.
+ *					Add 0.5 to all count rates in 
+ *					anticipation of truncation.
+ *		08/22/03   1.7  wvd   Populate MIN_LIMB keyword.
+ *		09/03/03   1.8  wvd   Implement cf_verbose throughout.
+ *				      Add EXP_JITR and EXPNIGHT to IDF header.
+ *		09/22/03   1.9  wvd   Correct comment field for YCENT1
+ *		10/02/03   1.10 wvd   Modify timeline table:
+ *				      - no time gaps
+ *				      - set TEMPORAL_OPUS for times outside
+ *					of OPUS good-time intervals.
+ *				      Delete cf_get_times.
+ *				      Use cf_read_col in cf_get_gti
+ *					and cf_get_geocorona.
+ *				      Don't modify gtis[0] for HIST data.
+ *		10/13/03   1.11 wvd   Add 1s to end of timeline table for
+ *					TTAG data.
+ *		10/15/03   1.12 wvd   Swap voltages for detectors 2A and 2B
+ *					if housekeeping file was written
+ *					before April of 2003.
+ *		10/22/03   1.13 wvd   Compute EXPNIGHT for raw data file
+ *					and write to output file header.
+ *					Add YQUALLIF & YQUALSIC keywords.
+ *		11/25/03   1.14 wvd   Raise upper limits on LIF_CNT_RATE and
+ *					SIC_CNT_RATE to 32000.  Raise limits
+ *					on FEC_CNT_RATE and AIC_CNT_RATE
+ *					to 64000.  Use TZERO = 32768 for
+ *					FEC_CNT_RATE and AIC_CNT_RATE. 
+ *					They must be read as floats.
+ *              01/15/04   1.15 bjg   Now performs cnt0 -= 16777216 when
+ *                                      cnt0 < cnt before computing 
+ *                                      cnt_rate for the first cnt and 
+ *                                      cnt0 in function 
+ *                                      fill_cntrate_array
+ *                                    cf_timeline 1.6 -> 1.7
+ *                                      free the arrays only at the end
+ *                                      version 1.6 tries to read tflag
+ *                                      array after it has been freed
+ *		02/06/04   1.16 wvd   Modify fill_cntrate_array() so
+ *					that the output array no longer runs
+ *					16 seconds behind the HSKP data.
+ *		02/18/04   1.17 wvd   Voltages for detectors 2A and 2B
+ *					are still swapped.  Set HKERR_ENDS
+ *					to 20100000.
+ *              03/04/04   1.18 bjg   Read begin and end counters as float
+ *                                    Set countrate to zero when cntb is more
+ *                                    than 16777216.
+ *              03/19/04        bjg   FITS data types (TFLOAT, TSTRING, TBYTE)
+ *                                    now match type of C containers (float, 
+ *                                    char *, char) when reading and writing 
+ *                                    in FITS header.
+ *              04/06/04   1.19 bjg   Include ctype.h
+ *                                    Functions now return EXIT_SUCCESS
+ *                                    Remove unused variables
+ *                                    Remove static keyword in struct key 
+ *                                    definition
+ *                                    If cnt_rate>32000 set cnt_rate=0
+ *		05/07/04   1.20 wvd   Delete HKERR_ENDS.  If HSKPVERS keyword
+ *				      is not present in HSKP file, test to
+ *				      determine whether high-voltage arrays
+ *				      for 2A and 2B are swapped.
+ *		05/27/04   1.21 bjg   Test counter keywords. If bad, use
+ *				      cnt_rate=NEVENTS/exptime or 0
+ *		06/14/04   1.22 wvd   Add BRIT_OBJ keyword to header.
+ *				      Rewrite fill_hv_array() to make it more
+ *					robust.
+ *				      If HV values in header are good, use
+ *					them to determine whether HV 
+ *                                    	arrays for 2A and 2B are swapped.
+ *              10/17/04        bjg   Replaced lots of
+ *                                    "while (val<array[i] && i<nmax)"
+ *                                    with
+ *                                    "while (i<nmax && val<array[i])"
+ *              11/09/04   1.23 bjg   Fixed Timeline AIC countrate. 
+ *                                    Sum of AIC countrates 
+ *                                    for all 4 detectors
+ *		02/09/05   1.24 wvd   Use count rates, rather than counts,
+ *					when testing header keywords.
+ *		02/15/05   1.25 wvd   If the count-rate arrays get too big,
+ *					truncate and issue a warning.
+ *		02/28/05   1.26 wvd   Fix bug in AIC count-rate test.
+ *				      Lower AIC and FEC thresholds to
+ *					0.8 * NEVENTS/EXPTIME.
+ *				      If GTI values span more than 25 ks,
+ *					make timeline table entries only for
+ *					times in the GTI's.
+ *				      Set OPUS flag for timeline-table 
+ *					entries whose values exceed 25 ks.
+ *				      Rewrite fill_hv_array() to make it more
+ *					robust.
+ *				      Set overflow count-rate values to zero.
+ *				      Treat HV as array of shorts throughout.
+ *		03/03/05   1.27 wvd   Raise exposure-length limit to 55 ksec.
+ *		03/14/05   1.28 wvd   Modify gtis[0] only if TTPERIOD = 1.0
+ *		03/17/05   1.29 wvd   Issue a warning if bigtime = TRUE.
+ *		03/21/05   1.30 wvd   If there's a break in the timeline
+ *					array, recalculate times of sunrise
+ *					and sunset.  Delete bigtime and the
+ *					mechanism for storing tsunrise and
+ *					tsunset as floats.  Define lastsunrise
+ *					and lastsunset relative to ptime[0],
+ *					rather than mjd_start.  Write time
+ *					between sunsets to header in ORBPERID.
+ *		08/30/05   1.31 wvd   Allow for the possibility that some of
+ *					the photons have absurd arrival times
+ *					AND others are not included in the
+ *					OPUS good-time intervals.
+ *		08/31/05   1.32 wvd   In cf_set_background_limits, use LWRS
+ *					limits for RFPT observations.
+ *		11/03/05   1.33 wvd   When housekeeping file is missing and
+ *					engineering snapshot times are
+ *					corrupted, use EXPSTART and EXPEND
+ *					to estimate eng_time. If EXPEND
+ *					is corrupted, use EXPTIME.
+ *		04/09/06   1.34 wvd   Flag as bad times after final OPUS GTI.
+ *		08/21/06   1.35 wvd   Treat housekeeping time array as double.
+ *					Don't add 0.5 to arrays in subroutine
+ *					fill_cntrate_array.
+ *		12/29/06   1.36 wvd   Correct bug in construction of AIC
+ *					count-rate array.
+ *		02/13/07   1.37 wvd   If TTPERIOD = 0, set to 1.
+ *		03/07/07   1.38 wvd   Remove pos from call to space_vel.
+ *		03/23/07   1.39 wvd   Give more detailed error message if
+ *					housekeeping file is not usable.
+ *		04/07/07   1.40 wvd   Clean up compiler warnings.
+ *		05/18/07   1.41 wvd   If HV array in HSKP file consists of a 
+ *					single 0 followed by all -1's, use 
+ *					header info to populate timeline table.
+ *					Rename fill_hv_array to hv_from_hskp
+ *					and add hv_from_header.
+ *
+ ****************************************************************************/
+ 
+#include <unistd.h>
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include <math.h>
+#include <ctype.h>
+#include "calfuse.h" 
+#include "sgp4.h"
+
+
+struct key {
+        char keyword[FLEN_KEYWORD];
+        float value;
+        };
+
+
+/***********************************************************************
+ *
+ *  procedure to get the GTI values from the input file
+ *
+ **********************************************************************/
+
+int cf_get_gti(fitsfile *infits, double **gtis, double **gtie) {
+
+    char	instmode[FLEN_VALUE];
+    int		ngti, status=0;
+    float	ttperiod;
+
+    cf_verbose(3, "Entering cf_get_gti.");
+
+   /* Read header keywords. */
+    FITS_movabs_hdu(infits, 1, NULL, &status);
+    FITS_read_key(infits, TSTRING, "INSTMODE", instmode, NULL, &status);
+    FITS_read_key(infits, TFLOAT, "TTPERIOD", &ttperiod, NULL, &status);
+    if (ttperiod < 1E-6) ttperiod = 1.0;
+
+   /* Move to the second extension and read the GTI's */
+    FITS_movabs_hdu(infits, 3, NULL, &status);
+    ngti = cf_read_col(infits, TDOUBLE, "START", (void **) gtis);
+    ngti = cf_read_col(infits, TDOUBLE, "STOP",  (void **) gtie);
+
+   /* 
+    *  If gtis[0] = 0.000, then it is probably wrong.
+    *  Set it equal to the fractional part of gtie[0].
+    *  In HIST mode, gtis[0] is always 0., so don't change it.
+    *  This trick only works if TTPERIOD = 1.0.
+    */
+    if (**gtis < FRAME_TOLERANCE && !strncmp(instmode, "TTAG", 4)
+	&& fabs(ttperiod - 1.0) < FRAME_TOLERANCE)
+	**gtis = fmod(*gtie[0], 1.);
+
+    cf_verbose(3, "Exiting cf_get_gti.");
+    return ngti;
+}
+
+/***********************************************************************
+ *
+ * procedure to get a list of geocoronal line locations from the AIRG 
+ *   calibration file
+ *
+ ***********************************************************************/
+
+int
+cf_get_geocorona(fitsfile *outfits, short **gxmin, short **gxmax,
+	short **gymin, short **gymax)
+{
+   char airgfile[FLEN_VALUE]; 
+   int nrow, status=0; 
+   fitsfile *airgfits;
+
+   cf_verbose(3, "Entering cf_get_geocorona.");
+
+  /* Read the name of the AIRG calibration file to use and open it */
+   FITS_movabs_hdu(outfits, 1, NULL, &status);
+   FITS_read_key(outfits, TSTRING, "AIRG_CAL", airgfile, NULL, &status);
+   FITS_open_file(&airgfits, cf_cal_file(airgfile), READONLY, &status); 
+   cf_verbose(3, "AIRG_CAL = %s", airgfile);
+
+  /* 
+   *  Move to the first extension and read the positions of the
+   *  geocoronal lines.
+   */  
+   FITS_movabs_hdu(airgfits, 2, NULL, &status);
+   nrow = cf_read_col(airgfits, TSHORT, "XMIN", (void **) gxmin); 
+   nrow = cf_read_col(airgfits, TSHORT, "XMAX", (void **) gxmax);
+   nrow = cf_read_col(airgfits, TSHORT, "YMIN", (void **) gymin);
+   nrow = cf_read_col(airgfits, TSHORT, "YMAX", (void **) gymax);
+
+   FITS_close_file(airgfits, &status);
+   cf_verbose(3, "Exiting cf_get_geocorona.");
+   return nrow;
+}
+
+
+/***********************************************************************
+ *
+ * Procedures to compute times of most recent sunrise and sunset
+ *
+ ***********************************************************************/
+
+SGP4   set_orbit_parms(fitsfile *);
+
+static double
+sunrise(double mjd_start, SGP4 sgp4)
+{
+    double ang_sep, mjd, ptime, pos[3], vel[3];
+    int    i, dn_flag, dn_flag_last;
+
+    dn_flag_last = 1; /* Assume that we begin in night. */
+
+    for (i=1; i>-8000; i--) {
+        ptime = (double) i;
+        mjd = mjd_start + ptime/86400.0;
+
+        /* Get the state vector at time mjd */
+        SGP4_getStateVector(sgp4, mjd, pos, vel);
+        SGP4_precess(pos, mjd, MJD2000);
+
+        dn_flag = eclipse(pos, mjd, &ang_sep); /* 0=day, 1=night */
+
+	/* We're going backward in time, so sunrise is day into night. */
+        if ((dn_flag == 1) && (dn_flag_last == 0)) break;
+
+        dn_flag_last=dn_flag;
+    }
+    /* Historically, we've defined sunrise as the time increment after
+	the change, so add 1 to the number we've just calculated. */
+    return (ptime + 1.);
+}
+
+
+static double
+sunset(double mjd_start, SGP4 sgp4)
+{
+    double ang_sep, mjd, ptime, pos[3], vel[3];
+    int    i, dn_flag, dn_flag_last;
+
+    dn_flag_last = 0; /* Assume that we begin in day. */
+
+    for (i=1; i>-8000; i--) {
+	ptime = (double) i;
+	mjd = mjd_start + ptime/86400.0;
+
+	/* Get the state vector at time mjd */
+	SGP4_getStateVector(sgp4, mjd, pos, vel);
+	SGP4_precess(pos, mjd, MJD2000);
+
+	dn_flag = eclipse(pos, mjd, &ang_sep);  /* 0=day, 1=night */
+
+	/* We're going backward in time, so sunset is night into day. */
+	if ((dn_flag == 0) && (dn_flag_last == 1)) break;
+
+	dn_flag_last = dn_flag;
+    }
+    /* Historically, we've defined sunset as the time increment after
+	the change, so add 1 to the number we've just calculated. */
+    return (ptime + 1.);
+}
+
+/****************************************************************************/
+
+static void
+fill_cntrate_array(long nsam_hk, long *hk_colval, double *time_hk,
+		   long ntime, double *ttime, float *tarray)
+{
+    /*
+     *  Procedure to fill an array with count rate housekeeping (HK)
+     *  information, which is tabulated on an approx 16s time interval.
+     *
+     *  nsam_hk   = number of time samples in the housekeeping file
+     *  hk_colval = array containing the housekeeping data
+     *  time_hk   = time from the exposure start for each second in the
+     *              houskeeping file
+     *  ntime     = number of tabulated rows in the timeline array
+     *  ttime     = tabulated times in the timeline array
+     *  tarray    = timeline array to be filled, one sample per second
+     *              starting at the start of the exposure
+     */
+
+    double hk_time, hk_time0;
+    long hk_cnt, hk_cnt0;
+    long i;	/* index through timeline table */
+    long k;	/* index through housekeeping array */
+    float cnt_rate = 0.;
+
+    i = k = 0;	/* Initialize indices */
+
+    /*
+     *  Find the first non-negative value in the HK array
+     */
+    while(k < nsam_hk && hk_colval[k] < 0) k++;
+    hk_cnt0  = hk_colval[k];
+    hk_time0 = time_hk[k];
+
+    /*
+     *  Begin big loop through the timeline table
+     */
+    while (i < ntime) {
+
+	/* Find the next non-negative value in the HK array. */
+	k++;
+	while(k < nsam_hk && hk_colval[k] < 0) k++;
+
+	/* If we've run out of HK entries,
+		fill in the rest of the timeline and quit. */
+	if (k == nsam_hk) {
+	    for ( ; i < ntime; i++)
+		tarray[i] = cnt_rate;
+	    break;
+	}
+
+	/* Otherwise, calculate the count rate between
+		times hk_time0 and hk_time. */
+	hk_cnt = hk_colval[k];
+	hk_time = time_hk[k];
+	if (hk_cnt < hk_cnt0)
+	    hk_cnt0 -= 16777216;
+	cnt_rate = (hk_cnt - hk_cnt0) / (hk_time - hk_time0);
+
+	/* Populate the timeline table for times less than hk_time */
+	while (i < ntime && cf_nlong(ttime[i]) < hk_time) 
+	    tarray[i++] = cnt_rate;
+
+	/* Save latest HK time and count values. */
+	hk_cnt0  = hk_cnt;
+	hk_time0 = hk_time;
+    }
+}
+
+
+/****************************************************************************/
+
+static void
+hv_from_header(fitsfile *outfits, char *det, char *side, long ntime, short *hv)
+{
+
+	char  hv_key[FLEN_CARD];
+	int   det_hv, hv_flag, status=0;
+	long  i;
+
+        fits_read_key(outfits, TINT, "HV_FLAG", &hv_flag, NULL, &status);
+	if (hv_flag == -1) {
+           det_hv = -999;
+           cf_verbose(1, "Bad HV keywords: setting HV to -999 in timeline table.");
+	}
+	else {
+           sprintf(hv_key, "DET%.1sHV%.1sH", det, side);
+           FITS_read_key(outfits, TINT, hv_key, &det_hv, NULL, &status);
+	}
+	if (hv_flag == 0)
+	   cf_verbose(1, "Applying max voltage value to whole exposure.");
+
+        cf_verbose(2, "High voltage = %d", det_hv);
+	for (i=0; i<ntime; i++)
+	    hv[i] = det_hv;
+}
+
+
+/****************************************************************************/
+
+int
+hv_from_hskp(long nsam_hk, long *hk_colval, double *time_hk,
+	      long ntime, double *ttime, short *tarray)
+{
+    /*
+     *  Procedure to fill an array with high voltage housekeeping (HK)
+     *  information, which is tabulated on an approx 16s time interval.
+     *
+     *  nsam_hk   = number of time samples in the housekeeping file
+     *  hk_colval = array containing the housekeeping data
+     *  time_hk   = time from the exposure start for each second in the
+     *              housekeeping file
+     *  ntime     = number of tabulated rows in the timeline array
+     *  ttime     = tabulated times in the timeline array
+     *  tarray    = timeline array to be filled, one sample per second
+     *              starting at the start of the exposure
+     */
+
+    long i;     /* index through timeline table */
+    long k;     /* index through housekeeping array */
+    short hv = 0; 
+    
+    i = k = 0;  /* Initialize indices */
+
+    /* 
+     *  Scan the input HK array.  If it consists of a zero followed by
+     *  all -1's, exit with an error.
+     */
+
+    if (hk_colval[0] == 0) {
+	for (i = 1; i < nsam_hk; i++) if (hk_colval[i] != -1) break;
+	if (i == nsam_hk) return (-1);
+    }
+
+    /* 
+     *  Find the first non-negative value in the HK array
+     */
+
+    while(k < nsam_hk && hk_colval[k] < 0) k++;
+    hv = hk_colval[k];
+
+    /*
+     *  Begin big loop through the timeline table
+     */
+
+    while (i < ntime) {
+
+	/* Find the next non-negative value in the HK array */
+	k++;
+	while(k < nsam_hk && hk_colval[k] < 0) k++;
+
+	/* If we've run out of HK entries, fill in the rest of the
+	   timeline and quit. */
+	if (k == nsam_hk) {
+	    for ( ; i < ntime; i++)
+		tarray[i] = hv;
+	    break;
+	}
+
+	/* Otherwise, populate the timeline table for times less than hk_time */
+	while (i < ntime && ttime[i] < time_hk[k])
+	    tarray[i++] = hv;
+
+	/* Save latest HV value from HK array */
+	hv = hk_colval[k];
+    }
+
+    return (0);
+}
+
+
+/****************************************************************************/
+
+int cf_timeline(fitsfile *outfits)
+{
+  /*************************************************************
+   *
+   *   Procedure to fill in the third extension of the IDF,
+   *   which contains information about orbital parameters,
+   *   count rates, high voltage info, and Y centroids as
+   *   a function of time during the observation. The data
+   *   are tabulated once each second.
+   *
+   **************************************************************/
+
+    char  hkexists[FLEN_VALUE], det[FLEN_VALUE], side[2];
+    char  fmt_byte[FLEN_CARD], fmt_float[FLEN_CARD], fmt_short[FLEN_CARD];
+    char  instmode[FLEN_VALUE], keyword[FLEN_KEYWORD], card[FLEN_CARD];
+    char  volt_cal[FLEN_VALUE];
+    unsigned char *tflag;
+    int   hv_flag, ngti, n_bad_times, TIMES_TOO_BIG = FALSE;
+    int   status=0, anynull, intnull=0, dn_flag_last=0;
+    int   biglif = FALSE, bigsic = FALSE, bigfec = FALSE, bigaic = FALSE; 
+    long  i, j, k, expnight, nevents, ntime, vmax;
+    short *hv;
+    float *lifcr, *siccr, *feccr, *aiccr, *bkgdcr;
+    float first_time, last_time, bad_times[1024], *time=NULL;
+    float *ycentl, *ycents;
+    float max_lif, max_sic, max_fec, max_aic;
+    double *gtis, *gtie, min_limb=999., period;
+    double mjd_start, mjd_end, mjd, *ptime, *lon, *lat, *limbang;
+    double *vorb, *tsunrise, lastsunrise=0, *tsunset, lastsunset=0;
+    orbital orb;
+    SGP4  sgp4;
+    struct key tscal[16], tzero[16];
+    long nevts;
+
+    char * dets[]={"1A","1B","2A","2B"};
+
+    char extname[]="TIMELINE";
+    int tfields=16;  /* output table will have 16 columns */
+    char *ttype[]={"TIME", "STATUS_FLAGS", "TIME_SUNRISE", "TIME_SUNSET",
+		   "LIMB_ANGLE", "LONGITUDE", "LATITUDE", "ORBITAL_VEL",
+		   "HIGH_VOLTAGE", "LIF_CNT_RATE", "SIC_CNT_RATE",
+		   "FEC_CNT_RATE", "AIC_CNT_RATE", "BKGD_CNT_RATE",
+                   "YCENT_LIF","YCENT_SIC"};
+
+    char *tform[16]; /* we will define tform later, when the number
+			of photons is known */
+
+    char *tunit[]={"seconds", "unitless", "seconds", "seconds", "degrees",
+                   "degrees", "degrees",  "km/s", "unitless", "counts/sec",
+                   "counts/sec", "counts/sec", "counts/sec", "counts/sec",
+                   "pixels","pixels" };
+
+    char CF_PRGM_ID[] = "cf_timeline";
+    char CF_VER_NUM[] = "1.41";
+
+    /* Initialize error checking. */
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Started execution.");
+
+    /*  Set the orbital parameters keywords. */
+    FITS_movabs_hdu(outfits, 1, NULL, &status);
+    FITS_read_key(outfits, TDOUBLE, "EXPSTART", &mjd_start, NULL, &status);
+    FITS_read_key(outfits, TDOUBLE, "EXPEND",   &mjd_end, NULL, &status);
+    FITS_read_key(outfits, TDOUBLE, "RA_TARG",  &orb.ra_ap, NULL, &status);
+    FITS_read_key(outfits, TDOUBLE, "DEC_TARG", &orb.dec_ap, NULL, &status);
+    FITS_read_key(outfits, TSTRING, "INSTMODE", instmode, NULL, &status);
+    FITS_read_key(outfits, TSTRING, "VOLT_CAL", volt_cal, NULL, &status);
+
+    cf_velang(outfits, (mjd_end+mjd_start)/2.0);
+
+    sgp4 = set_orbit_parms(outfits);
+
+    /* Read the good time intervals */
+    ngti = cf_get_gti(outfits, &gtis, &gtie);
+    for (i=0; i<ngti; i++)
+	cf_verbose(3, "GTI start = %0.1f, end= %0.1f", gtis[i], gtie[i]);
+
+    /* 
+     * An exposure should never span more than 55 ks.  If it appears to
+     * do so, include only the good-time intervals in the timeline table.
+     * Otherwise, include all times between EXPSTART and EXPEND, whether
+     * or not there are any associated photons.
+     */
+    if (gtie[ngti-1] - gtis[0] > MAX_EXPTIME) {
+	TIMES_TOO_BIG = TRUE;
+	cf_if_warning("Exposure appears to span %0.0f ks.  Truncating "
+		"timeline table.", (gtie[ngti-1] - gtis[0])/1000.);
+    }
+
+    /* For HIST data, use the good-time intervals
+	to set the times in the timeline table. */ 
+    if (!strncmp(instmode, "HIST", 4)) {
+        if (TIMES_TOO_BIG) {
+	    ntime = 0;
+	    for (i = 0; i < ngti; i++) 
+		ntime += (long) (gtie[i] - gtis[i] + 1.5);
+	    ptime = (double *) cf_malloc(sizeof(double) * ntime);
+	    k = 0;
+	    for (i = 0; i < ngti; i++) {
+		ntime = (long) (gtie[i] - gtis[i] + 1.5);
+		for (j = 0; j < ntime; j++)
+		    ptime[k++] = gtis[i] + j;
+	    }
+	    ntime = k;
+	}
+	else {
+	    ntime = (long) (gtie[ngti-1] - gtis[0] + 1.5);
+	    ptime = (double *) cf_malloc(sizeof(double) * ntime);
+	    for (i = 0; i < ntime; i++)
+		ptime[i] = gtis[0] + i;
+	}
+    }
+
+    /* For TTAG data, use the photon times themselves. */
+    else {
+	FITS_movabs_hdu(outfits, 2, NULL, &status);
+	nevents = cf_read_col(outfits, TFLOAT, "TIME", (void **) &time);
+	FITS_movabs_hdu(outfits, 1, NULL, &status);
+	n_bad_times = 0;
+        if (TIMES_TOO_BIG) {
+	    last_time = 0;
+	    i = nevents - 1;
+	    while (time[i] > MAX_EXPTIME && i > 0) {
+		if (fabs(time[i] - last_time) > FRAME_TOLERANCE && n_bad_times < 1024) {
+		    bad_times[n_bad_times++] = time[i];
+		    last_time = time[i];
+		}
+		i--;
+	    }
+	    last_time = time[i] + 1.;
+	}
+	else
+	    last_time = time[nevents-1] + 1.;
+	first_time = time[0];
+	if (first_time < fmod(last_time, 1.))
+		first_time = fmod(last_time, 1.) - 1.;
+	ntime = (long) (last_time - first_time + 1.5) + n_bad_times;
+	ptime = (double *) cf_malloc(sizeof(double) * ntime);
+	for (i = 0; i < ntime - n_bad_times; i++)
+	    ptime[i] = first_time + i;
+	for (j = n_bad_times-1; i < ntime; i++, j--)
+	    ptime[i] = bad_times[j];
+	free(time);
+    }
+    cf_verbose(2, "Timeline table will contain %ld entries", ntime);
+
+    /* Now generate all of the other arrays in the timeline table. */
+
+    lon   = (double *) cf_calloc(ntime, sizeof(double));
+    lat   = (double *) cf_calloc(ntime, sizeof(double));
+    limbang  = (double *) cf_calloc(ntime, sizeof(double));
+    vorb  = (double *) cf_calloc(ntime, sizeof(double));
+    tsunrise = (double *) cf_calloc(ntime, sizeof(double));
+    tsunset = (double *) cf_calloc(ntime, sizeof(double));
+    hv    = (short *) cf_calloc(ntime, sizeof(short));
+    lifcr = (float *) cf_calloc(ntime, sizeof(float));
+    siccr = (float *) cf_calloc(ntime, sizeof(float));
+    feccr = (float *) cf_calloc(ntime, sizeof(float));
+    aiccr = (float *) cf_calloc(ntime, sizeof(float));  
+    bkgdcr = (float *) cf_calloc(ntime, sizeof(float));
+    tflag = (unsigned char *) cf_calloc(ntime, sizeof(unsigned char));
+    ycentl = (float *)cf_calloc(ntime, sizeof(float));
+    ycents = (float *)cf_calloc(ntime, sizeof(float));
+
+    for (i=0; i<ntime; i++) {
+	int   dn_flag, day_limb;
+	float dx;
+	double geo_lon, geo_lat, gmst, pos[3], vel[3], zdist, ang_sep;
+
+	mjd = mjd_start + ptime[i]/86400.0;
+
+	/* get the state vector at time mjd */
+	SGP4_getStateVector(sgp4, mjd, pos, vel);
+	SGP4_precess(pos, mjd, MJD2000);
+	SGP4_precess(vel, mjd, MJD2000);
+
+	dx = space_vel(vel, orb.ra_ap, orb.dec_ap);
+
+	state_geod(pos, mjd, &geo_lon, &geo_lat, &gmst);
+	limbang[i] = (double) state_limb(pos, mjd, orb.ra_ap, orb.dec_ap, 
+					 &zdist, &day_limb);
+	if (min_limb > limbang[i]) min_limb = limbang[i];
+
+	dn_flag = eclipse(pos, mjd, &ang_sep);  /* 0=day, 1=night */
+
+	/* The first time through, and after any breaks in the timeline,
+	 * compute times of most recent sunrise and sunset. */
+	if ((i == 0) || (ptime[i] - ptime[i-1] - 1. > FRAME_TOLERANCE)) {
+	    lastsunrise = ptime[i] + sunrise(mjd, sgp4);
+	    lastsunset  = ptime[i] + sunset(mjd, sgp4);
+	    if (lastsunset > lastsunrise) dn_flag_last = 1 ;
+	    else dn_flag_last = 0 ;
+            /*  The first time through, compute the orbital period and
+	     *	write it to file header.  */
+	    if (i == 0) {
+		mjd += (lastsunset - ptime[i] + 7000.)/86400.0;
+		period = 7000. + sunset(mjd, sgp4);
+		FITS_movabs_hdu(outfits, 1, NULL, &status);
+		FITS_update_key(outfits, TDOUBLE, "ORBPERID", &period,
+		"[s] Estimate of orbital period", &status);
+	    }
+	}
+	/* If we've moved from day into night (or night into day), update
+	   last sunrise/sunset times. */
+	else if ((dn_flag == 0) && (dn_flag_last == 1))
+	    lastsunrise = ptime[i];
+	else if ((dn_flag == 1) && (dn_flag_last == 0)) 
+      	    lastsunset = ptime[i]; 
+
+	/* If this is daytime, set the day bit in TFLAG array. */
+	if (dn_flag == 0)
+	    tflag[i] |= TEMPORAL_DAY;
+
+	lon[i] = geo_lon;
+	lat[i] = geo_lat;
+	vorb[i] = dx;
+	tsunrise[i] = ptime[i] - lastsunrise;
+	tsunset[i]  = ptime[i] - lastsunset;
+	dn_flag_last = dn_flag;
+    }
+
+
+    /* 
+     * Set the OPUS flag for times outside of the OPUS good-time
+     * intervals.  Since there are no photons associated with the
+     * last second of a GTI, we make sure that it is flagged as
+     * bad.  The first second of a good-time interval is good.
+     */
+    j = 0;
+    for (i = 0; i < ntime; i++) {
+	while (j < ngti-1 && ptime[i] > gtie[j] - 0.5)
+	    j++;
+	if (ptime[i] < gtis[j] - FRAME_TOLERANCE ||
+	    ptime[i] > gtie[j] + FRAME_TOLERANCE)
+	    tflag[i] |= TEMPORAL_OPUS;
+    }
+    tflag[ntime-1] |= TEMPORAL_OPUS;
+
+    /*
+     * No exposure should be longer than 55 ks.  For HIST data, we'll just
+     * put up with it, but for TTAG data, we'll flag as bad any timeline
+     * table entries with absurd arrival times.  We use the OPUS flag for
+     * this.  What we're really saying is that we don't believe that the 
+     * times associated with these photons are correct.
+     */
+    for (i = 0; i < ntime; i++)
+	if (ptime[i] > MAX_EXPTIME)
+	    tflag[i] |= TEMPORAL_OPUS;
+
+    /* Fill housekeeping columns (count rates and high voltage). */
+    FITS_movabs_hdu(outfits, 1, NULL, &status);
+    FITS_read_key(outfits, TSTRING, "HKEXISTS", hkexists, NULL, &status);
+    FITS_read_key(outfits, TSTRING, "DETECTOR", det, NULL, &status);
+    strncpy(side, det+1, 1);
+
+    /* Populate MIN_LIMB keyword. */
+    FITS_update_key(outfits, TDOUBLE, "MIN_LIMB", &min_limb, NULL, &status);
+
+    /* If no housekeeping file exists, use header info to fill timeline. */
+ loop:
+    if(!strncasecmp(hkexists, "N", 1)) {
+	char  cntb_key[FLEN_CARD], cnte_key[FLEN_CARD];
+	float  cntb, cnte;
+	float cnt_rate, cnt_rate2, eng_time, exp_time;
+	double ctimeb, ctimee;
+
+        cf_verbose(1, "No housekeeping file: filling timeline with header info.");
+
+	/* move to the top level header to read the relevant keywords */ 
+        FITS_movabs_hdu(outfits, 1, NULL, &status);
+	FITS_read_key(outfits, TFLOAT, "EXPTIME", &exp_time, NULL, &status);
+	FITS_read_key(outfits, TLONG, "NEVENTS", &nevts, NULL, &status);
+
+	/* calculate engineering count rates */ 
+	FITS_read_key(outfits, TDOUBLE, "CTIME_B", &ctimeb, NULL, &status);
+	FITS_read_key(outfits, TDOUBLE, "CTIME_E", &ctimee, NULL, &status);
+	eng_time = (ctimee-ctimeb) * 86400.;
+
+        /* If eng_time is unreasonable, use the EXPTIME keyword */
+	if (eng_time < 1) {
+	  cf_if_warning("Engineering snapshot time less than or equal to zero.");
+	  if ((eng_time = (mjd_end-mjd_start) * 86400.) < MAX_EXPTIME)
+	     cf_if_warning("Estimating LiF, SiC, FEC and AIC count rates from EXPSTART and EXPEND.");
+	  else {
+	     eng_time = exp_time;
+	     cf_if_warning("Estimating LiF, SiC, FEC and AIC count rates from EXPTIME.");
+	  }
+	}
+
+	/* SiC count rate timeline */
+        sprintf(cntb_key, "C%.2sSIC_B", det);
+        FITS_read_key(outfits, TFLOAT, cntb_key, &cntb, NULL, &status);
+        sprintf(cnte_key, "C%.2sSIC_E", det);
+        FITS_read_key(outfits, TFLOAT, cnte_key, &cnte, NULL, &status); 
+				
+	if ((cnte<0) || (cntb<0) || (cntb>cnte) || eng_time < 1. ||
+	    (cnte==0xEB90EB90) || (cnte==0xDEADDEAD) ||
+	    (cntb==0xEB90EB90) || (cntb==0xDEADDEAD) ||
+	    ((cnt_rate = (cnte - cntb) / eng_time) > 32000)) {
+	    cf_if_warning("Bad SiC counter.  SiC count rate will be set to zero.");
+	    cnt_rate=0;
+	}
+	
+	cf_verbose(2, "SiC count rate = %d", (int) cnt_rate);
+	for (i=0; i<ntime; i++)
+	    siccr[i] = cnt_rate;
+
+	/* LiF count rate timeline */
+        sprintf(cntb_key, "C%.2sLIF_B", det);
+        FITS_read_key(outfits, TFLOAT, cntb_key, &cntb, NULL, &status);
+        sprintf(cnte_key, "C%.2sLIF_E", det);
+        FITS_read_key(outfits, TFLOAT, cnte_key, &cnte, NULL, &status);
+      
+        if ((cnte<0) || (cntb<0) || (cntb>cnte) || eng_time < 1. ||
+            (cnte==0xEB90EB90) || (cnte==0xDEADDEAD) ||
+            (cntb==0xEB90EB90) || (cntb==0xDEADDEAD) ||
+            ((cnt_rate = (cnte - cntb) / eng_time) > 32000)) {
+            cf_if_warning("Bad LiF counter.  LiF count rate will be set to zero.");
+            cnt_rate=0;
+        }
+
+	cf_verbose(2, "LiF count rate = %d", (int) cnt_rate);
+	for (i=0; i<ntime; i++)
+	    lifcr[i] = cnt_rate;
+
+	/* FEC count rate timeline */
+        sprintf(cntb_key, "C%.2sFE_B", det);
+        FITS_read_key(outfits, TFLOAT, cntb_key, &cntb, NULL, &status);
+        sprintf(cnte_key, "C%.2sFE_E", det);
+        FITS_read_key(outfits, TFLOAT, cnte_key, &cnte, NULL, &status);
+      
+	if ((cnte<0) || (cntb<0) || (cntb>cnte) || eng_time<1 ||
+	    (cnte==0xEB90EB90) || (cnte==0xDEADDEAD) ||
+	    (cntb==0xEB90EB90) || (cntb==0xDEADDEAD) ||
+	    ((cnt_rate = (cnte - cntb) / eng_time) > 64000) ||
+	    (cnt_rate < 0.8*nevts/exp_time)) {
+	    cf_if_warning("Bad FEC counter"); 
+	    cf_if_warning("-- FEC count rate will be computed from NEVENTS and EXPTIME.");
+	    cf_if_warning("-- Electronic deadtime correction will be underestimated.");
+	    cf_if_warning("-- Y stretch will be underestimated.");
+	    cnt_rate=nevts/exp_time;
+	}			
+				
+	cf_verbose(2, "FEC count rate = %d", (int) cnt_rate);
+	for (i=0; i<ntime; i++)
+	    feccr[i] = cnt_rate;
+
+	/* AIC count rate timeline */
+	cnt_rate=0;
+	for (i=0;i<4;i++){
+	  sprintf(cntb_key, "C%.2sAI_B", dets[i]);
+	  FITS_read_key(outfits, TFLOAT, cntb_key, &cntb, NULL, &status);
+	  sprintf(cnte_key, "C%.2sAI_E", dets[i]);
+	  FITS_read_key(outfits, TFLOAT, cnte_key, &cnte, NULL, &status);			
+
+	  if (((cnte<0) || (cntb<0) || (cntb>cnte) || (eng_time<1) ||
+	    (cnte==0xEB90EB90) || (cnte==0xDEADDEAD) ||
+	    (cntb==0xEB90EB90) || (cntb==0xDEADDEAD) ||
+	    ((cnt_rate2 = (cnte - cntb)/ eng_time) > 64000)) ||
+	    ((!(strncasecmp(dets[i],det,2))) && (cnt_rate2<0.8*nevts/exp_time))) {
+	      cf_if_warning("Bad AIC counter %s",dets[i]); 
+	      cf_if_warning("-- AIC count rate will be computed from NEVENTS and EXPTIME.");
+	      cf_if_warning("-- IDS deadtime correction will be underestimated.");
+	      cnt_rate=nevts/exp_time;
+	      break;
+	  }	
+	  cnt_rate+=cnt_rate2;
+	}
+       
+	cf_verbose(2, "AIC count rate = %d", (int) cnt_rate);
+	for (i=0; i<ntime; i++)
+	    aiccr[i] = cnt_rate;
+
+	/* High voltage timeline */
+	hv_from_header(outfits, det, side, ntime, hv);
+    }
+    else {
+	/*
+	 *  Housekeeping file exists.  Use it to calculate timeline values.
+	 */
+	char  cntb_key[FLEN_VALUE], hk_file_name[FLEN_VALUE];
+	int   hk_colnum, hskpvers, MUST_TEST_HV=FALSE, swap_HV=FALSE;
+	long  nsam_hk, *hk_colval;
+	double *hk_mjd, *time_hk;
+	fitsfile *hskpfits;
+	float * aiccr2;
+
+	FITS_read_key(outfits, TSTRING, "HSKP_CAL", hk_file_name, NULL, &status);
+	/* If you can't open the housekeeping file, try a lower-case filename.*/
+	if (fits_open_file(&hskpfits, hk_file_name, READONLY, &status)) {
+            status = 0;
+            cf_verbose(3, "Can't find housekeeping file %s", hk_file_name);
+            hk_file_name[0] = (char) tolower(hk_file_name[0]);
+            cf_verbose(3, "Will look for file named %s", hk_file_name);
+
+	    /* If you still can't open the housekeeping file, use header keywords. */
+            if (fits_open_file(&hskpfits, hk_file_name, READONLY, &status)) {
+		status = 0;
+                cf_verbose(3, "Can't find housekeeping file %s", hk_file_name);
+		strncpy(hkexists, "N", 1);
+		goto loop;
+	    }
+	    /* If lower-case filename works, write it to the file header. */
+            FITS_update_key(outfits, TSTRING, "HSKP_CAL", hk_file_name, NULL, &status);
+        }
+	cf_verbose(1, "Housekeeping file exists: using it to fill timeline.");
+
+	/* If we're on side 2 and the HSKPVERS keyword does not exist, then we'll
+		need to check whether the HV arrays are swapped. */
+        if (*det == '2' &&
+	    fits_read_key(hskpfits, TINT, "HSKPVERS", &hskpvers, NULL, &status)) {
+	    status = 0;
+	    MUST_TEST_HV = TRUE;
+	}
+
+        FITS_movabs_hdu(hskpfits, 2, NULL, &status);
+        FITS_read_key(hskpfits, TLONG, "NAXIS2", &nsam_hk, NULL, &status);
+	cf_verbose(3, "Number of samples in the HK file = %ld", nsam_hk);
+
+	/*  Allocate space to hold the column contents */
+	hk_colval = (long *) cf_calloc(nsam_hk, sizeof(long));
+        hk_mjd    = (double *) cf_calloc(nsam_hk, sizeof(double));
+	time_hk   = (double *) cf_calloc(nsam_hk, sizeof(double));
+
+	/* Read in the various columns */
+        
+	/* First the MJD values - convert to time from start in seconds  */
+	FITS_get_colnum(hskpfits, TRUE, "MJD", &hk_colnum, &status);
+        FITS_read_col(hskpfits, TDOUBLE, hk_colnum, 1L, 1L, nsam_hk, &intnull,
+		      hk_mjd, &anynull, &status);
+        for (i=0; i<nsam_hk; i++)
+	    time_hk[i] = (hk_mjd[i]-mjd_start) * 86400.;
+
+	/* SiC count rate timeline */
+        sprintf(cntb_key, "I_DET%.1sCSIC%.1s", det, side);
+
+	/* Check to see whether the column exists. If not, then 
+           reset the housekeeping flag and do the analysis using 
+           keyword values in the input file header. If so, then check
+           whether it contains real values. If not, then use the 
+           keywords */
+	if(!fits_get_colnum(hskpfits, TRUE, cntb_key, &hk_colnum, &status)) {
+           FITS_read_col(hskpfits, TLONG, hk_colnum, 1L, 1L, nsam_hk, &intnull,
+		      hk_colval, &anynull, &status);
+           vmax = 0;
+           for (j=0; j< nsam_hk; j++)
+	       if (hk_colval[j] > vmax)
+		   vmax = hk_colval[j];
+	   if (vmax <= 0) {
+              cf_if_warning("Data missing from housekeeping column.  "
+		"Will treat file as missing.");
+              strncpy(hkexists, "N", 1);
+              status=0;
+              goto loop; }
+            else fill_cntrate_array(nsam_hk, hk_colval, time_hk, ntime,
+				    ptime, siccr);}
+	 else {
+	      cf_if_warning("Data column missing from housekeeping file.  "
+		"Will treat file as missing.");
+              strncpy(hkexists, "N", 1);
+              status=0;
+              goto loop;
+	    }
+	cf_verbose(3,"SiC count-rate info read from housekeeping file.");
+
+	/* LiF count rate timeline */
+        sprintf(cntb_key, "I_DET%.1sCLIF%.1s", det, side);
+	FITS_get_colnum(hskpfits, TRUE, cntb_key, &hk_colnum, &status);
+        FITS_read_col(hskpfits, TLONG, hk_colnum, 1L, 1L, nsam_hk, &intnull,
+		      hk_colval, &anynull, &status);
+        fill_cntrate_array(nsam_hk, hk_colval, time_hk, ntime, ptime, lifcr);
+	cf_verbose(3,"LiF count-rate info read from housekeeping file.");
+
+	/* FEC count rate timeline */
+	sprintf(cntb_key, "I_DET%.1sCFE%.1s", det, side);
+	FITS_get_colnum(hskpfits, TRUE, cntb_key, &hk_colnum, &status);
+	FITS_read_col(hskpfits, TLONG, hk_colnum, 1L, 1L, nsam_hk, &intnull,
+		      hk_colval, &anynull, &status);
+        fill_cntrate_array(nsam_hk, hk_colval, time_hk, ntime, ptime, feccr);
+	cf_verbose(3,"FEC count-rate info read from housekeeping file.");
+
+ 	/* AIC count rate timeline */ 
+	aiccr2 = (float *) cf_calloc(ntime, sizeof(float));
+	for (j=0;j<ntime;j++) aiccr[j]=0;
+	for (i=0;i<4;i++){
+	  sprintf(cntb_key, "I_DET%.1sCAI%.1s", dets[i], dets[i]+1);
+	  FITS_get_colnum(hskpfits, TRUE, cntb_key, &hk_colnum, &status);
+	  FITS_read_col(hskpfits, TLONG, hk_colnum, 1L, 1L, nsam_hk, &intnull,
+			hk_colval, &anynull, &status); 
+	  fill_cntrate_array(nsam_hk, hk_colval, time_hk, ntime, ptime, aiccr2); 
+	  for (j=0;j<ntime;j++) aiccr[j]+=aiccr2[j];
+	}
+	cf_verbose(3,"AIC count-rate info read from housekeeping file.");
+
+	/* If MUST_TEST_HV = TRUE, determine whether HV for 2A and 2B are swapped. */
+	if (MUST_TEST_HV) {
+	    char  mjd_str[FLEN_VALUE], full_str[FLEN_VALUE], saa_str[FLEN_VALUE];
+	    double mjd_volt;
+	    int full, hdr_max2a, max2a = 0, saa;
+	    long n, nhk, *hv2a;
+	    fitsfile *voltfits;
+
+	    cf_verbose(3, "Testing whether HV arrays are swapped.");
+
+	    /* Read HV array for 2A from HSKP file; find max value. */
+	    nhk = cf_read_col(hskpfits, TLONG, "I_DET2HVBIASAST", (void **) &hv2a);
+	    for (n = 0L; n < nhk; n++) if (max2a < hv2a[n]) max2a = hv2a[n];
+	    free (hv2a);
+	    
+	    /*
+	     *  If HV values in file header are good, read 2A max.
+	     *	Compare with value from HSKP file.
+	     */
+	    fits_read_key(outfits, TINT, "HV_FLAG", &hv_flag, NULL, &status);
+	    if (hv_flag > -1) {
+		FITS_read_key(outfits, TINT, "DET2HVAH", &hdr_max2a, NULL, &status);
+		cf_verbose(3, "   Max for 2A: header says %d, housekeeping file says %d.",
+		    hdr_max2a, max2a);
+		if (abs(max2a - hdr_max2a) < 5)
+		    cf_verbose(3, "   HV arrays are OK.  No need to swap.");
+		else
+		    swap_HV = TRUE;
+	    }
+
+	    /*
+	     *  If HV values in file header are bad, compare with expected
+	     *  values from VOLT_CAL file.
+	     */
+	    else {
+		FITS_open_file(&voltfits, cf_cal_file(volt_cal), READONLY, &status);
+	        n = 0L;
+	        do {
+	            n++;
+	            sprintf(mjd_str, "MJD%ld", n);
+	            FITS_read_key(voltfits, TDOUBLE, mjd_str, &mjd_volt, NULL, &status);
+	        } while (mjd_start > mjd_volt);
+	        n--;
+
+	        sprintf(full_str, "FULL%ld", n);
+	        sprintf(saa_str, "SAA%ld", n);
+	        FITS_read_key(voltfits, TINT, full_str, &full, NULL, &status);
+	        FITS_read_key(voltfits, TINT, saa_str, &saa, NULL, &status);
+	        FITS_close_file(voltfits, &status);
+
+	        /* If max for 2A matches expected full or SAA voltage -- and
+		    we're on side 2A -- then we're OK.  Otherwise, must swap. */
+	        cf_verbose(3, "   2A max = %d; Expected values for %s: full = %d, SAA = %d",
+		    max2a, det, full, saa);
+	        if ((abs(max2a - full) < 10 || abs(max2a - saa) < 5) &&
+		    (*side == 'A'))
+		    cf_verbose(3, "   HV arrays are OK.  No need to swap.");
+	        else swap_HV = TRUE;
+	    }
+	}
+
+ 	/* High voltage timeline */
+	if (swap_HV) {
+	    if (*side == 'A') sprintf(cntb_key, "I_DET2HVBIASBST");
+	    else              sprintf(cntb_key, "I_DET2HVBIASAST");
+	    cf_verbose(3, "   Swapping HV values for detectors 2A and 2B");
+	}
+        else sprintf(cntb_key, "I_DET%.1sHVBIAS%.1sST", det, side);
+	FITS_get_colnum(hskpfits, TRUE, cntb_key, &hk_colnum, &status);
+        FITS_read_col(hskpfits, TLONG, hk_colnum, 1L, 1L, nsam_hk, &intnull,
+		      hk_colval, &anynull, &status);
+        if (!hv_from_hskp(nsam_hk, hk_colval, time_hk, ntime, ptime, hv))
+	    cf_verbose(3,"HV info read from housekeeping file.");
+        else {
+	    cf_verbose(1,"Housekeeping file corrupted: reading HV info from file header.");
+	    hv_from_header(outfits, det, side, ntime, hv);
+	}
+
+	free(time_hk);
+	free(hk_mjd);
+	free(hk_colval);
+	FITS_close_file(hskpfits, &status);
+    }
+
+    /*
+     * Set TFORM, TSCALE, and TZERO values for output table.
+     */
+    sprintf(fmt_byte,  "%ldB", ntime);
+    sprintf(fmt_float, "%ldE", ntime);
+    sprintf(fmt_short, "%ldI", ntime);
+
+    /* First set default values. */
+    tform[0] = fmt_float;
+    tform[1] = fmt_byte;
+    for (i=2; i<tfields; i++)
+	tform[i] = fmt_short;
+
+    /* For most arrays, we keep one decimal place. */
+    for (i=2; i<tfields; i++) {
+	sprintf(tscal[i].keyword, "TSCAL%ld", i+1);
+	tscal[i].value = 0.1;
+	sprintf(tzero[i].keyword, "TZERO%ld", i+1);
+	tzero[i].value = 0.;
+    }
+
+    /* Now we start tinkering. */
+
+    /* The orbital velocity is small, so we can keep two decimal places. */
+    tscal[7].value = 0.01;
+
+    /* FEC_CNT_RATE and AIC_CNT_RATE can get big, so we
+        use TZERO AND TSCALE to compress them. */
+    tscal[11].value = 1;
+    tscal[12].value = 2;
+    tzero[11].value = 32768;
+    tzero[12].value = 65536;
+
+    /* If a count rate is high, set to zero. */
+    max_lif = max_sic = 32767.;
+    max_fec = 65535.;
+    max_aic = 131070.;
+
+    for (i = 0; i < ntime; i++) {
+	if (lifcr[i] > max_lif) {
+		lifcr[i] = 0.;
+		biglif = TRUE;
+	}
+	if (siccr[i] > max_sic) {
+		siccr[i] = 0.;
+		bigsic = TRUE;
+	}
+	if (feccr[i] > max_fec) {
+		feccr[i] = 0.;
+		bigfec = TRUE;
+	}
+	if (aiccr[i] > max_aic) {
+		aiccr[i] = 0.;
+		bigaic = TRUE;
+	}
+    }
+
+	if (biglif) cf_if_warning("LIF_CNT_RATE out of bounds.  Setting bad values to zero.");
+	if (bigsic) cf_if_warning("SIC_CNT_RATE out of bounds.  Setting bad values to zero.");
+	if (bigfec) cf_if_warning("FEC_CNT_RATE out of bounds.  Setting bad values to zero.");
+	if (bigaic) cf_if_warning("AIC_CNT_RATE out of bounds.  Setting bad values to zero.");
+
+    /*
+     * Write the timeline table to the output file.
+     */
+    FITS_movabs_hdu(outfits, 3, NULL, &status);
+    FITS_create_hdu(outfits, &status);
+
+    FITS_create_tbl(outfits, BINARY_TBL, 1L, tfields, ttype, 
+                    tform, tunit, extname, &status);
+
+    /* Write TSCALE and TZERO entries to header */
+    for (i=2; i<tfields; i++) {
+
+        /* Omit TSCALE and TZERO for these six arrays. */
+        if (i ==  2) continue;  /* TIME_SUNRISE */
+        if (i ==  3) continue;  /* TIME_SUNSET  */
+        if (i ==  8) continue;  /* HIGH_VOLTAGE */
+        if (i ==  9) continue;  /* LIF_CNT_RATE */
+        if (i == 10) continue;  /* SIC_CNT_RATE */
+        if (i == 13) continue;  /* BKGD_CNT_RATE */
+
+	sprintf(keyword, "TUNIT%ld", i+1);
+	if (fits_read_keyword(outfits, keyword, card, NULL, &status))
+		cf_if_fits_error(status);
+	FITS_insert_key_flt(outfits, tscal[i].keyword, tscal[i].value,
+		-1, NULL, &status);
+	FITS_insert_key_flt(outfits, tzero[i].keyword, tzero[i].value,
+		-5, NULL, &status);
+    }
+
+    FITS_write_col(outfits, TDOUBLE, 1, 1L, 1L, ntime, ptime, &status);
+	cf_verbose(3, "ptime array written to timeline table");
+    FITS_write_col(outfits, TBYTE,   2, 1L, 1L, ntime, tflag, &status);
+	cf_verbose(3, "tflag array written to timeline table");
+    FITS_write_col(outfits, TDOUBLE, 3, 1L, 1L, ntime, tsunrise, &status);
+	cf_verbose(3, "tsunrise array written to timeline table");
+    FITS_write_col(outfits, TDOUBLE, 4, 1L, 1L, ntime, tsunset, &status);
+	cf_verbose(3, "tsunset array written to timeline table");
+    FITS_write_col(outfits, TDOUBLE, 5, 1L, 1L, ntime, limbang, &status);
+	cf_verbose(3, "limbang array written to timeline table");
+    FITS_write_col(outfits, TDOUBLE, 6, 1L, 1L, ntime, lon, &status);
+	cf_verbose(3, "lon array written to timeline table");
+    FITS_write_col(outfits, TDOUBLE, 7, 1L, 1L, ntime, lat, &status);
+	cf_verbose(3, "lat array written to timeline table");
+    FITS_write_col(outfits, TDOUBLE, 8, 1L, 1L, ntime, vorb, &status);
+	cf_verbose(3, "vorb array written to timeline table");
+    FITS_write_col(outfits, TSHORT,  9, 1L, 1L, ntime, hv, &status);
+	cf_verbose(3, "hv array written to timeline table");
+    FITS_write_col(outfits, TFLOAT, 10, 1L, 1L, ntime, lifcr, &status);
+	cf_verbose(3, "lifcr array written to timeline table");
+    FITS_write_col(outfits, TFLOAT, 11, 1L, 1L, ntime, siccr, &status);
+	cf_verbose(3, "siccr array written to timeline table");
+    FITS_write_col(outfits, TFLOAT, 12, 1L, 1L, ntime, feccr, &status);
+	cf_verbose(3, "feccr array written to timeline table");
+    FITS_write_col(outfits, TFLOAT, 13, 1L, 1L, ntime, aiccr, &status);
+	cf_verbose(3, "aiccr array written to timeline table");
+    FITS_write_col(outfits, TFLOAT, 14, 1L, 1L, ntime, bkgdcr, &status);
+	cf_verbose(3, "bkgdcr array written to timeline table");
+    FITS_write_col(outfits, TFLOAT, 15, 1L, 1L, ntime, ycentl, &status);
+	cf_verbose(3, "ycentl array written to timeline table");
+    FITS_write_col(outfits, TFLOAT, 16, 1L, 1L, ntime, ycents, &status);
+	cf_verbose(3, "ycents array written to timeline table");
+
+    /* Compute EXPNIGHT for raw data file and write to output header. */
+    expnight = 0;
+    for (i=0; i<ntime; i++)
+	if (!tflag[i]) expnight++;
+    FITS_movabs_hdu(outfits, 1, NULL, &status);
+    FITS_update_key(outfits, TLONG, "EXPNIGHT", &expnight, NULL, &status);
+    cf_verbose(3, "For raw data, EXPNIGHT = %d", expnight);
+
+    free(ptime);
+    free(lon);
+    free(lat);
+    free(limbang);
+    free(vorb);
+    free(tsunrise);
+    free(tsunset);
+    free(hv);
+    free(lifcr);
+    free(siccr);
+    free(feccr);
+    free(aiccr);
+    free(bkgdcr);
+    free(tflag);
+    free(ycentl);
+    free(ycents);
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished execution.");
+    return EXIT_SUCCESS; 
+}
+
+
+/* Add new header keywords - needed only for old versions of OPUS */
+
+int cf_add_header_keywords(fitsfile *outfits)
+{
+    char  hkexists[FLEN_CARD];
+    int status=0;
+    float dum=0., rawtime;
+    short sdum=0;
+    long  ldum=0;
+    short bkgd_num=0;
+
+    cf_verbose(3, "Entering cf_add_header_keywords");
+
+    /* If keyword RAWTIME does not exist, create with value of EXPTIME */
+    fits_read_key(outfits, TFLOAT, "RAWTIME", &rawtime, NULL, &status);
+    if (status) {
+	status = 0;
+        FITS_read_key(outfits, TFLOAT, "EXPTIME", &rawtime, NULL, &status);
+        FITS_update_key(outfits, TFLOAT, "RAWTIME", &rawtime,
+		"[s] Exposure duration of raw data file", &status);
+    }
+
+    /* If keyword HKEXISTS is missing, create with value of "NO" */
+    fits_read_key(outfits, TSTRING, "HKEXISTS", hkexists, NULL, &status);
+    if (status != 0) {
+	status=0;
+	cf_verbose(1, "HKEXISTS keyword missing: assume no housekeeping file.");
+	FITS_update_key(outfits, TSTRING, "HKEXISTS", "NO",
+	    "Housekeeping data file exists", &status);
+    }
+
+    FITS_update_key(outfits, TSTRING, "BRIT_OBJ", "NO", "Not an over-bright observation", &status);
+    FITS_update_key(outfits, TSTRING, "HSKP_CAL", "        ", "Housekeeping data file", &status);
+    FITS_update_key(outfits, TSTRING, "DAYNIGHT", "BOTH", "Use only DAY, NIGHT or BOTH", &status);
+    FITS_update_key(outfits, TLONG,  "EXP_HV", &ldum, "[s] Integration time lost to low voltage", &status);
+    FITS_update_key(outfits, TLONG,  "EXP_JITR", &ldum, "[s] Integration time lost to jitter", &status);
+    FITS_update_key(outfits, TLONG,  "EXPNIGHT", &ldum, "[s] Integration time during night after screening", &status);
+    FITS_update_key(outfits, TFLOAT, "FPADXLIF", &dum, "[pixels] Correction for FPA position",&status);
+    FITS_update_key(outfits, TFLOAT, "FPADXSIC", &dum, "[pixels] Correction for FPA position",&status);
+    FITS_update_key(outfits, TFLOAT, "YCENT1", &dum, "[pixels] Y centroid of LIF HIRS aperture",&status);
+    FITS_update_key(outfits, TFLOAT, "YCENT2", &dum, "[pixels] Y centroid of LIF MDRS aperture",&status);
+    FITS_update_key(outfits, TFLOAT, "YCENT3", &dum, "[pixels] Y centroid of LIF LWRS aperture",&status);
+    FITS_update_key(outfits, TFLOAT, "YCENT5", &dum, "[pixels] Y centroid of SIC HIRS aperture",&status);
+    FITS_update_key(outfits, TFLOAT, "YCENT6", &dum, "[pixels] Y centroid of SIC MDRS aperture",&status);
+    FITS_update_key(outfits, TFLOAT, "YCENT7", &dum, "[pixels] Y centroid of SIC LWRS aperture",&status);
+    FITS_update_key(outfits, TSTRING, "YQUAL1", "        ", "Quality of Y centroid value (LIF HIRS)",&status);
+    FITS_update_key(outfits, TSTRING, "YQUAL2", "        ", "Quality of Y centroid value (LIF MDRS)",&status);
+    FITS_update_key(outfits, TSTRING, "YQUAL3", "        ", "Quality of Y centroid value (LIF LWRS)",&status);
+    FITS_update_key(outfits, TSTRING, "YQUAL5", "        ", "Quality of Y centroid value (SIC HIRS)",&status);
+    FITS_update_key(outfits, TSTRING, "YQUAL6", "        ", "Quality of Y centroid value (SIC MDRS)",&status);
+    FITS_update_key(outfits, TSTRING, "YQUAL7", "        ", "Quality of Y centroid value (SIC LWRS)",&status);
+    FITS_update_key(outfits, TFLOAT, "YGEO_LIF", &dum, "Y centroid of geocoronal lines in target spectrum", &status);
+    FITS_update_key(outfits, TFLOAT, "YGEO_SIC", &dum, "Y centroid of geocoronal lines in target spectrum", &status);
+    FITS_update_key(outfits, TSHORT, "BKGD_NUM", &bkgd_num, "Number of background regions defined", &status);
+    FITS_update_key(outfits, TSHORT, "BKG_MIN0", &sdum, "[pixels] bkgd sample region 0 - lower limit",&status);
+    FITS_update_key(outfits, TSHORT, "BKG_MIN1", &sdum, "[pixels] bkgd sample region 1 - lower limit",&status);
+    FITS_update_key(outfits, TSHORT, "BKG_MIN2", &sdum, "[pixels] bkgd sample region 2 - lower limit",&status);
+    FITS_update_key(outfits, TSHORT, "BKG_MIN3", &sdum, "[pixels] bkgd sample region 3 - lower limit",&status);
+    FITS_update_key(outfits, TSHORT, "BKG_MIN4", &sdum, "[pixels] bkgd sample region 4 - lower limit",&status);
+    FITS_update_key(outfits, TSHORT, "BKG_MIN5", &sdum, "[pixels] bkgd sample region 5 - lower limit",&status);
+    FITS_update_key(outfits, TSHORT, "BKG_MIN6", &sdum, "[pixels] bkgd sample region 6 - lower limit",&status);
+    FITS_update_key(outfits, TSHORT, "BKG_MIN7", &sdum, "[pixels] bkgd sample region 7 - lower limit",&status);
+    FITS_update_key(outfits, TSHORT, "BKG_MAX0", &sdum, "[pixels] bkgd sample region 0 - upper limit",&status);
+    FITS_update_key(outfits, TSHORT, "BKG_MAX1", &sdum, "[pixels] bkgd sample region 1 - upper limit",&status);
+    FITS_update_key(outfits, TSHORT, "BKG_MAX2", &sdum, "[pixels] bkgd sample region 2 - upper limit",&status);
+    FITS_update_key(outfits, TSHORT, "BKG_MAX3", &sdum, "[pixels] bkgd sample region 3 - upper limit",&status);
+    FITS_update_key(outfits, TSHORT, "BKG_MAX4", &sdum, "[pixels] bkgd sample region 4 - upper limit",&status);
+    FITS_update_key(outfits, TSHORT, "BKG_MAX5", &sdum, "[pixels] bkgd sample region 5 - upper limit",&status);
+    FITS_update_key(outfits, TSHORT, "BKG_MAX6", &sdum, "[pixels] bkgd sample region 6 - upper limit",&status);
+    FITS_update_key(outfits, TSHORT, "BKG_MAX7", &sdum, "[pixels] bkgd sample region 7 - upper limit",&status);
+
+    cf_verbose(3, "Exiting cf_add_header_keywords");
+    return EXIT_SUCCESS;
+}
+ 
+/* Set limits to the background sample regions */
+
+int cf_set_background_limits(fitsfile *outfits) {
+
+    char aper[FLEN_VALUE];
+    char bchrfile[FLEN_FILENAME];
+    int status=0;
+    long npts;
+    short bkgd_num=3, *ylim;
+    fitsfile *bchrfits;
+
+    cf_verbose(3, "Entering cf_set_background_limits");
+
+/*  Read the target aperture from the input file header. */
+    FITS_read_key(outfits,TSTRING,"APERTURE",aper, NULL, &status);
+    cf_verbose(3, "aperture = %s", aper); 
+
+/*  If APERTURE = RFPT, use same background region as for LWRS. */
+    if (!strncmp (aper, "RFPT", 4)) {
+	strncpy(aper, "LWRS", 4);
+	cf_verbose(1, "APERTURE = RFPT.  Will treat as LWRS observation.");
+    }
+
+/*  Read the name of the BCHR parameter file and open it. */
+    FITS_read_key(outfits, TSTRING, "BCHR_CAL",bchrfile, NULL, &status);
+    cf_verbose(3,"BCHR parameter file = %s ",bchrfile);
+    FITS_open_file(&bchrfits,cf_parm_file(bchrfile), READONLY, &status); 
+
+/*  From the first extension of the BCHR_CAL file, read the limits
+    to the background regions.  Close the file */
+    FITS_movabs_hdu(bchrfits, 2, NULL, &status);
+    npts = cf_read_col(bchrfits, TSHORT, aper, (void **) &ylim);
+    FITS_close_file(bchrfits, &status);
+
+    cf_verbose(3, "Number of background regions: %d", bkgd_num);
+    cf_verbose(3, "Limits of background regions: %d, %d, %d, %d, %d, %d",
+      ylim[0],ylim[1],ylim[2],ylim[3],ylim[4],ylim[5]);
+
+/*  Update the header keywords */
+    FITS_update_key(outfits, TSHORT, "BKGD_NUM", &bkgd_num, NULL, &status);
+    FITS_update_key(outfits, TSHORT, "BKG_MIN0", &ylim[0], NULL, &status);
+    FITS_update_key(outfits, TSHORT, "BKG_MIN1", &ylim[2], NULL, &status);
+    FITS_update_key(outfits, TSHORT, "BKG_MIN2", &ylim[4], NULL, &status);
+    FITS_update_key(outfits, TSHORT, "BKG_MAX0", &ylim[1], NULL, &status);
+    FITS_update_key(outfits, TSHORT, "BKG_MAX1", &ylim[3], NULL, &status);
+    FITS_update_key(outfits, TSHORT, "BKG_MAX2", &ylim[5], NULL, &status);
+
+    free (ylim);
+    cf_verbose(3, "Exiting cf_set_background_limits");
+    return EXIT_SUCCESS ;
+}
diff --git a/src/libcf/cf_make_mask.c b/src/libcf/cf_make_mask.c
new file mode 100644
index 0000000..090222c
--- /dev/null
+++ b/src/libcf/cf_make_mask.c
@@ -0,0 +1,175 @@
+/***********************************************************************
+ *
+ *                  CF_MAKE_MASK
+ *
+ *    Procedure to create a mask of the bad pixels from the pixel list
+ *    generated by cf_bad_pixels
+ *
+ *    CALL: cf_make_mask(header, ap, nout, wave_out, bny, bymin, bpmask)
+ *
+ *    Arguments: fitsfile    header   name of the input IDF 
+ *               int         ap       Aperture designation
+ *               long        nout     number of points in wavelength array
+ *               float       wave_out wavelength array
+ *               int         bny      Y dimension of the output image -
+ *                                    should be same as background
+ *               int         bymin    Y coordinate of first element in 
+ *                                    output array. Should match background
+ *               float       bpmask   Output bad pixel mask - dimensions
+ *                                    are nout * bny 
+ *
+ *    History:	04/29/03  rdr  v1.0	Begin work 
+ *		04/30/03  wvd  v1.1	Install
+ *		09/30/03  wvd  v1.2	Use cf_read_col to read BPM_CAL
+ *					file.
+ *		11/11/03  wvd  v1.3	Fix bug in normalization of
+ *					pothole map.
+ *		07/21/04  wvd  v1.4	Fix bug in construction of
+ *					pothole mask: change & to && 
+ *		11/25/05  wvd  v1.5	Fill gaps in the mask that
+ *					open when the bad-pixel map
+ *					is converted from pixels to
+ *					wavelengths.
+ *
+ ***********************************************************************/
+
+#include "calfuse.h"
+
+int cf_make_mask(fitsfile *header, int ap, long nout, float *wave_out, 
+int bny, int bymin, float **bpmask){
+
+    char CF_PRGM_ID[] = "cf_make_mask";
+    char CF_VER_NUM[] = "1.5";
+
+    char bpm_file[FLEN_VALUE], *chan;
+    int *bphist, nhist, status=0;
+    long bpsum, i, j, k, ndx, nsam, npix, npts;
+    float *bpmaskt, w0, wpc, pnorm=1;
+    float *x, *y, *wt, *lam ;
+    float bpmax ;
+    fitsfile *bpmfits ;
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    cf_verbose(3, "Entering routine cf_make_mask") ;
+
+    /* Generate an array (nout * bny) to contain the map. */
+    npix = nout * bny;
+    bpmaskt = cf_calloc(npix, sizeof(float)) ;
+
+    /* Read wavelength information from input file header. */
+    FITS_movabs_hdu(header, 1, NULL, &status);
+    FITS_read_key(header, TFLOAT, "WPC", &wpc, NULL, &status);
+    w0 = wave_out[0];
+    cf_verbose(3, "Wavelengths: w0=%g, dw=%g", w0, wpc);
+
+    /* Open the bad-pixel file. */
+    if (fits_read_key(header, TSTRING, "BPM_CAL", bpm_file, NULL, &status)) {
+	cf_verbose(0,
+	    "No bad pixel (BPM_CAL) file specified.  Assuming no potholes.") ;
+	for (i=0; i<npix; i++) bpmaskt[i] = 1.;
+	*bpmask = bpmaskt;
+	return 0;
+    }
+    cf_verbose(3, "Bad Pixel file = %s ", bpm_file) ;
+    if (fits_open_file(&bpmfits, bpm_file, READONLY, &status) ) {
+	cf_verbose(0,
+	    "No bad pixel (BPM_CAL) file found.  Assuming no potholes.");
+	for (i=0; i<npix; i++) bpmaskt[i] = 1.;
+	*bpmask = bpmaskt;
+	return 0;
+    };
+
+    /* Read the BPM file. */
+    FITS_movabs_hdu(bpmfits, 2, NULL, &status);
+    npts = cf_read_col(bpmfits, TFLOAT, "X",       (void **) &x);
+    npts = cf_read_col(bpmfits, TFLOAT, "Y",       (void **) &y);
+    npts = cf_read_col(bpmfits, TFLOAT, "WEIGHT",  (void **) &wt);
+    npts = cf_read_col(bpmfits, TFLOAT, "LAMBDA",  (void **) &lam);
+    npts = cf_read_col(bpmfits, TBYTE,  "CHANNEL", (void **) &chan);
+
+    /* Fill the map with pothole information. */
+    nsam = 0;
+    for (i=0; i<npts; i++) {
+	if (chan[i] == ap) {
+	    j = (long) ( (lam[i] - w0)/wpc + 0.5 ) ;
+	    k = (long) ( (y[i] - bymin) + 0.5 ) ;
+	    if (j < nout && k < bny) {
+		nsam++ ;
+		ndx = k*nout + j ;
+		if (ndx > 0 && ndx < npix) bpmaskt[ndx] += wt[i] ;
+	    }
+	}
+    }
+    cf_verbose(3, "Channel %d contains %d bad pixels.", ap, nsam) ;
+
+    /* If any potholes are present, generate the pothole map. */
+    if(nsam > 0) {
+
+	/* Determine a normalization for the potholes. This is done by
+	creating a histogram of the weights between 0 and the maximum
+	and then selecting the 95% level as the normalization factor.
+	We use 95%, rather than the maximum, to avoid the possibility
+	of having a few spurious points define the normalization. */
+
+	/* Determine the maximum value. */
+	bpmax = 0.;
+	for (i=0; i<npix; i++)
+	    if (bpmaskt[i] > bpmax) bpmax = bpmaskt[i] ;
+
+	/* Generate the histogram. */
+	nhist = (int) (bpmax * 10.) + 1 ;
+	bphist = (int *) cf_calloc(nhist, sizeof(int)) ;
+	bpsum = 0;
+	for (i=0; i < npix; i++) {
+	    ndx = (int) (bpmaskt[i] * 10.) ;
+	    if (ndx > 0 && ndx < nhist) {
+		bphist[ndx]++;
+		bpsum++;
+	    }
+	}
+
+	/* Now select the 95% level. */
+	nsam = 0;
+	i = nhist-1 ;
+	while (nsam < bpsum/20 && i >= 0) {
+	    nsam += bphist[i] ;
+	    pnorm = bpmax - (nhist-1-i) / 10. ;
+	    i--;
+	}
+
+	cf_verbose(3, "bpmax = %.1f, normalizing factor = %.2f", bpmax, pnorm) ;      
+
+	/* Normalize and invert the mask so that the center of the
+	pothole is zero and the region outside is 1. */
+
+	for (i=0; i<npix; i++) {
+	    bpmaskt[i] = 1. - (bpmaskt[i] / pnorm) ;
+	    if (bpmaskt[i] < 0.) bpmaskt[i] = 0. ;
+	}
+
+	/* If a pixel in the mask is higher than both of its neighbors,
+	it probably represents a gap that opened when converting from
+	pixels to wavelengths.  Fill it. */
+
+	for (j = 1; j < nout-1; j++) {
+	    for (k = 0; k < bny; k++) {
+		ndx = k*nout + j ;
+		if (bpmaskt[ndx-1] < bpmaskt[ndx] && bpmaskt[ndx] > bpmaskt[ndx+1])
+			bpmaskt[ndx] = (bpmaskt[ndx-1] + bpmaskt[ndx+1]) / 2.;
+	    }
+	}
+    }
+
+    /* If there are no potholes, generate an array with all ones. */
+    else 
+	for (i=0; i<npix; i++) bpmaskt[i] = 1. ;
+
+    /* Redirect the pointer. */
+    *bpmask = bpmaskt;
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+
+    return status ;
+}
diff --git a/src/libcf/cf_make_wave_array.c b/src/libcf/cf_make_wave_array.c
new file mode 100644
index 0000000..bbbefcd
--- /dev/null
+++ b/src/libcf/cf_make_wave_array.c
@@ -0,0 +1,147 @@
+/*****************************************************************************
+ *            Johns Hopkins University
+ *            Center For Astrophysical Sciences
+ *            FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_make_wave_array(fitsfile *header, int aperture, long *nout,
+ *		float **wave_out)
+ *
+ * Description: Reads W0, WMAX, and WPC from the scrn*.fit file and returns
+ *		output wavelength array and its size.  If not supplied by
+ *		user, values are taken from the WAVE_CAL file.
+ *
+ *              The FITS wavelength-calibration file has 8 extensions in the
+ *              following order:
+ *              Ext# HDU# Channel Aperture
+ *                1   2     LiF     HIRS
+ *                2   3     LiF     MDRS
+ *                3   4     LiF     LWRS
+ *                4   5     LiF     PINH
+ *                5   6     SiC     HIRS
+ *                6   7     SiC     MDRS
+ *                7   8     SiC     LWRS
+ *                8   9     SiC     PINH
+ *
+ * Arguments:   fitsfile  *header       Pointer to IDF FITS file header
+ *              int       aperture      Target aperture (values 1-8)
+ *              long      *nout         Length of output arrays
+ *              float     **wave_out    Pointer to output wavelength array
+ *
+ * Returns:     0 on success
+ *
+ * History:     02/24/03  1.1   wvd	Initial coding.
+ *		03/02/03  1.2   wvd	Write W0 and WPC to IDF header.
+ *		09/29/03  1.3   wvd	Change calfusettag.h to calfuse.h
+ *		10/15/03  1.4   wvd	Read either LIF or SIC wavelength
+ *					parameters from PARM_CAL file,
+ *					depending upon aperture.
+ *		03/16/04  1.5   wvd	Cast wave_out array as type float.
+ *
+ ****************************************************************************/
+
+#include <stdio.h>
+#include "calfuse.h"
+
+static char CF_PRGM_ID[] = "cf_make_wave_array";
+static char CF_VER_NUM[] = "1.5";
+
+int
+cf_make_wave_array(fitsfile *header, int aperture, long *nout,
+	float **wave_out)
+{
+    char  parm_file[FLEN_VALUE];	/* Name of parameter file */
+    char  wave_file[FLEN_VALUE]; 	/* Name of WAVE_CAL file */
+    char  w0_key[FLEN_KEYWORD];		/* Depends on aperture */
+    char  wmax_key[FLEN_KEYWORD];	/* Depends on aperture */
+    char  wpc_key[FLEN_KEYWORD];	/* Depends on aperture */
+
+    int   status=0, hdunum;
+    long  i;
+
+    float default_w0, default_wmax, default_wpc; /* Default values */
+    float w0, wmax, wpc;			 /* Requested values */
+
+    fitsfile *parmfits, *wavefits;
+
+    /* Initialize error checking */
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin processing");
+
+    /* 
+     *  Set keywords to read either LIF or SIC parameters, depending on
+     *	the aperture number.
+     */
+    if (aperture < 5) {
+	sprintf(w0_key,   "LIF_W0");
+	sprintf(wmax_key, "LIF_WMAX");
+	sprintf(wpc_key,  "LIF_WPC");
+    } else {
+	sprintf(w0_key,   "SIC_W0");
+	sprintf(wmax_key, "SIC_WMAX");
+	sprintf(wpc_key,  "SIC_WPC");
+    }
+
+    /* Read recommended values of W0, WMAX, and WPC from WAVE_CAL header */
+    hdunum = aperture + 1;
+    FITS_read_key(header, TSTRING, "WAVE_CAL", wave_file, NULL, &status);
+    FITS_open_file(&wavefits, cf_cal_file(wave_file), READONLY, &status);
+    FITS_movabs_hdu(wavefits, hdunum, NULL, &status);
+    FITS_read_key(wavefits, TFLOAT, "W0", &default_w0, NULL, &status);
+    FITS_read_key(wavefits, TFLOAT, "WMAX", &default_wmax, NULL, &status);
+    FITS_read_key(wavefits, TFLOAT, "WPC", &default_wpc, NULL, &status);
+    FITS_close_file(wavefits, &status);
+    cf_verbose(3, "Recommended wavelength parameters:");
+    cf_verbose(3, "\tW0 = %g, WMAX = %g, WPC = %g",
+	default_w0, default_wmax, default_wpc);
+
+    /* 
+     * Read requested values of W0, WMAX, and WPC from PARM_CAL.
+     * If no value requested, use default values.
+     * Compare requested values with default; complain if weird.
+     */
+    FITS_read_key(header, TSTRING, "PARM_CAL", parm_file, NULL, &status);
+    FITS_open_file(&parmfits, cf_parm_file(parm_file), READONLY, &status);
+    if (fits_read_key(parmfits, TFLOAT, w0_key, &w0, NULL, &status)) {
+	w0 = default_w0;
+	status = 0;
+    }
+    else if (w0 < default_w0)
+	cf_if_warning("Requested value of W0 is less than recommended value.");
+
+    if (fits_read_key(parmfits, TFLOAT, wmax_key, &wmax, NULL, &status)) {
+        wmax = default_wmax;
+        status = 0;
+    }   
+    else if (wmax > default_wmax)
+        cf_if_warning("Requested value of WMAX is greater than "
+		      "recommended value.");
+
+    if (fits_read_key(parmfits, TFLOAT, wpc_key, &wpc, NULL, &status)) {
+        wpc = default_wpc;
+        status = 0;
+    }   
+    else if (wpc < default_wpc)
+        cf_if_warning("Requested value of WPC is less than "
+		      "recommended value.");
+    FITS_close_file(parmfits, &status);
+    cf_verbose(3, "Using these wavelength parameters:");
+    cf_verbose(3, "\tW0 = %g, WMAX = %g, WPC = %g", w0, wmax, wpc);
+
+    /*  Compute length of output wavelength array, allocate memory,
+     *  and fill array.
+     */
+    *nout = (long) ((wmax - w0)/wpc + 0.5) + 1L;
+    *wave_out  = (float *) cf_calloc(*nout, sizeof(float));
+    for (i = 0; i < *nout; i++)
+	(*wave_out)[i] = w0 + wpc * (float) i;
+
+    /*
+     *  Write WO and WPC to output file header.
+     */
+    FITS_update_key(header, TFLOAT, "WPC", &wpc, NULL, &status);
+    FITS_update_key(header, TFLOAT, "W0", &w0, NULL, &status);
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return status;
+}
diff --git a/src/libcf/cf_mirror_motion.c b/src/libcf/cf_mirror_motion.c
new file mode 100644
index 0000000..d5dd3b3
--- /dev/null
+++ b/src/libcf/cf_mirror_motion.c
@@ -0,0 +1,189 @@
+/*****************************************************************************
+ *	        Johns Hopkins University
+ *	        Center For Astrophysical Sciences
+ *	        FUSE
+ *****************************************************************************
+ *
+ * Synopsis:	cf_mirror_motion(header, nevents, time, x, y, channel,
+ *			ntimes, ttime, tsunset)
+ *
+ * Description: Calculates the shift of the spectrum in both X and Y caused
+ *              by thermal changes in the mirror position and corrects
+ *              the X and Y coordinates of each photon event. 
+ *
+ *              fitsfile  *header       Pointer to the location of the FITS
+ *                                      header of the Intermediate data File
+ *              long      nevents       Number of photons in the file
+ *              int       *time         Time stamp (in seconds) since the
+ *                                      start of the exposure
+ *              float     *x            Position of the photon (in pixels)
+ *              float     *y            Position of the photon (in pixels)
+ *     unsigned char      channel       Channel id of each photon
+ *              long      ntimes        Number of entries in timeline table
+ *              float     ttime         Time array of timeline table
+ *              short     tsunset       Time since last sunset
+ *
+ * Returns:     0 on success
+ *
+ * History:	09/06/02   1.1  RDR     Begin work, adapted from cf_make_shift
+ *		03/01/03   1.3  wvd	Correct use of pointer in FITS_read_key()
+ *              04/21/03   1.4  wvd	Use tsunset array from timeline table.
+ *					Do not assume that ttime is continuous.
+ *					Interpolate between tabulated shifts.
+ *              05/20/03   1.5  rdr     Added call to cf_proc_check
+ *              08/21/03   1.6  wvd     Change channel to unsigned char.
+ *              06/22/04   1.7  wvd     Estimate time between sunsets using
+ *					orbit period in file header.
+ *              07/14/04   1.8  rdr     Correct line which selects calibration
+ *              03/22/05   1.9  wvd     Change tsunset from float to short.
+ *					Read orbital period from file header.
+ *              04/15/05   1.10 wvd     If ORBPERID keyword is not present,
+ *					assume that it is 6000 s.
+ *              12/20/05   1.11 wvd     Omit correction for an extended
+ *					source.
+ *              04/07/07   1.12 wvd	Clean up compiler warnings.
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include "calfuse.h"
+
+int
+cf_mirror_motion(fitsfile *header, long nevents, float *time, float *x,
+		 float *y, unsigned char *channel, long ntimes, float *ttime,
+                 short *tsunset) {
+
+    char CF_PRGM_ID[] = "cf_mirror_motion";
+    char CF_VER_NUM[] = "1.12";
+
+    fitsfile *mmfits;
+    int    errflg=0, status=0, anynull=0, hdutype, nullval=0;
+    int    active_ap[2], extended;
+    long   j, k, ndx;
+    char   det[FLEN_VALUE], mmcal[FLEN_VALUE];
+    float  *tdxlif, *tdxsic, *dxlif, *dylif, *dxsic, *dysic;
+    float  frac, period, w0, w1, w99;
+
+    /* Initialize error checking. */
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+    /* Enter a time stamp into the log */
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    /* Check whether routine is appropriate for this data file. */
+    if ((errflg = cf_proc_check(header, CF_PRGM_ID))) return errflg;
+
+    /* Read detector keyword from header. */
+    FITS_read_key(header, TSTRING, "DETECTOR", det, NULL, &status);
+
+    /* Determine the channel numbers of the active apertures */
+    extended = cf_source_aper(header, active_ap);
+    
+    /* If source is extended, exit now. */
+    if (extended) {
+	cf_verbose(1, "Extended source.  Omitting photon shift.");
+        cf_proc_update(header, CF_PRGM_ID, "SKIPPED");
+	return (status);
+    }
+
+    /* 
+     *  Read orbital period from file header.
+     */
+    fits_read_key(header, TFLOAT, "ORBPERID", &period, NULL, &status);
+    if (status) {
+	status = 0;
+	period = 6000;
+        cf_verbose(1, "Keyword ORBPERID not found; assuming 6000 seconds");
+    }
+    else
+	cf_verbose(2, "Estimated orbital period is %.2f seconds", period);
+
+    /* Allocate space for shift arrays. */
+    dxlif = (float *) cf_calloc(ntimes, sizeof(float));
+    dylif = (float *) cf_calloc(ntimes, sizeof(float));
+    dxsic = (float *) cf_calloc(ntimes, sizeof(float));
+    dysic = (float *) cf_calloc(ntimes, sizeof(float));
+
+    /* Read the name of the mirror-motion calibration file */
+    FITS_read_key(header, TSTRING, "MIRR_CAL", mmcal, NULL, &status); 
+    cf_verbose(3, "Mirror motion calibration file = %s", mmcal);
+
+    /*  Open the calibration file and read in the information relating 
+     *  x shifts as a function of time (in minutes) from sunset for one orbit
+     *  (100 minutes)
+     */
+    FITS_open_file(&mmfits, cf_cal_file(mmcal), READONLY, &status);
+    tdxsic = (float *) cf_calloc(100, sizeof(float)); 
+    tdxlif = (float *) cf_calloc(100, sizeof(float)); 
+    cf_verbose(3,"detector= %s",det) ;
+    if (!strncmp(det, "1", 1) ) {
+      cf_verbose(3,"Correcting detector 1") ;
+	/*
+	 *  NOTE: LiF 1 is used as reference and so, by definition, has no
+	 *  mirror motions. Thus, on side 1 only the SiC spectrum will move.
+	 */
+	FITS_movabs_hdu(mmfits,2, &hdutype, &status);
+	FITS_read_img(mmfits, TFLOAT, 1,100, &nullval, tdxsic, &anynull,
+		      &status);
+    }
+    else {
+      cf_verbose(3,"Correcting detector 2") ;
+	FITS_movabs_hdu(mmfits,3, &hdutype, &status);
+	FITS_read_img(mmfits, TFLOAT, 1,100, &nullval, tdxlif, &anynull,
+		      &status);
+	FITS_movabs_hdu(mmfits,4, &hdutype, &status);
+	FITS_read_img(mmfits, TFLOAT, 1,100, &nullval, tdxsic, &anynull,
+		      &status);
+    }
+    FITS_close_file(mmfits, &status);
+    /* Determine the shifts for each second of the observation. */
+    for (k=0; k<ntimes; k++) {
+	frac = tsunset[k] / period * 100.;
+	ndx = (long) frac;
+	if (ndx >= 99) {
+	    w99 = 100. - frac;
+	    w0 = frac - 99.;
+	    dxlif[k] = w0 * tdxlif[0] + w99 * tdxlif[99];
+	    dxsic[k] = w0 * tdxsic[0] + w99 * tdxsic[99];
+	}
+	else {
+	    w0 = (float) (ndx + 1) - frac;
+	    w1 = frac - (float) (ndx);
+	    dxlif[k] = w0 * tdxlif[ndx] + w1 * tdxlif[ndx + 1];
+	    dxsic[k] = w0 * tdxsic[ndx] + w1 * tdxsic[ndx + 1];
+	}
+    }
+    
+    /* Apply the calculated shifts to the data. */
+    for (j=k=0; j<nevents; j++) {
+        while(ttime[k+1] - FRAME_TOLERANCE < time[j] && k+1 < ntimes) k++;
+	/*
+	 *  Shift only photons in the active aperture.
+	 *  active_ap[0] = lif, active_ap[1] = sic 
+	 */
+	if (channel[j] == active_ap[0]) {
+            x[j] += dxlif[k];
+            y[j] += dylif[k];
+
+        }
+	if (channel[j] == active_ap[1]) {
+            x[j] += dxsic[k];
+            y[j] += dysic[k];
+        }
+    }
+
+    /* Release array storage */
+    free(tdxlif);
+    free(tdxsic);
+    free(dxlif);
+    free(dylif);
+    free(dxsic);
+    free(dysic);
+
+    cf_proc_update(header, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished execution.");
+
+    return status;
+}
diff --git a/src/libcf/cf_modify_hist_pha.c b/src/libcf/cf_modify_hist_pha.c
new file mode 100644
index 0000000..a842b5d
--- /dev/null
+++ b/src/libcf/cf_modify_hist_pha.c
@@ -0,0 +1,91 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_modify_hist_pha (fitsfile *header, long nevents,
+ *                          unsigned char *pha, unsigned char *channel)
+ *
+ * Description: For histogram data, set pulse heights of all photons to the
+ *              most likely value, a function of aperture and obs date.
+ *
+ * Arguments:   fitsfile       *header      Input FITS file pointer
+ *              long           nevents      Number of photon events
+ *              unsigned char  *pha	    Pulse-height array (output)
+ *              unsigned char  *channel     Channel assignment (input)
+ *
+ * Calls:
+ *
+ * Returns:     0 on success
+ *
+ * History:     03/01/05   1.1   wvd    Initial coding
+ *		03/16/05   1.2   wvd	Read PHA array as type TBYTE, not TINT.
+ *		04/28/05   1.3   wvd	Fix bug in loop through MJD array.
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include "calfuse.h"
+
+int
+cf_modify_hist_pha (fitsfile *header, long nevents, unsigned char *pha,
+	unsigned char *channel)
+{
+    char CF_PRGM_ID[] = "cf_modify_hist_pha";
+    char CF_VER_NUM[] = "1.3";
+
+    char		phahfile[FLEN_FILENAME];
+    unsigned char	pha_chan[8], *pha_mjd=NULL;
+    int			errflg=0, status=0;
+    long		i, j, jmax;
+    double		expstart, *mjd=NULL;
+    fitsfile		*phahfits;
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    /* If data were not taken in HIST mode, exit now. */
+    if ((errflg = cf_proc_check(header, CF_PRGM_ID))) return errflg;
+
+    /* Read header keywords. */
+    FITS_read_key(header, TDOUBLE, "EXPSTART", &expstart, NULL, &status);
+
+    /* Open the pulse-height calibration file. */
+    FITS_read_key(header, TSTRING, "PHAH_CAL", phahfile, NULL, &status);
+    cf_verbose(3, "Pulse-height calibration file = %s", phahfile);
+    FITS_open_file(&phahfits, cf_cal_file(phahfile), READONLY, &status);
+
+    /*
+     * Loop through all channels, reading expected pulse heights from PHAH_CAL.
+     * Use the values appropriate for the date of this exposure.
+     */
+    pha_chan[0] = 20;		/* Default for events not in a channel */
+    for (i = 1; i < 8; i++) {
+	if (i == 4) continue;
+        FITS_movabs_hdu(phahfits, i+1, NULL, &status);
+        jmax = cf_read_col(phahfits, TDOUBLE, "MJD", (void *) &mjd);
+        jmax = cf_read_col(phahfits, TBYTE,   "PHA", (void *) &pha_mjd);
+	j = 0;
+	while (j < jmax-1 && mjd[j+1] < expstart) j++;
+	pha_chan[i] = pha_mjd[j];
+	cf_verbose(3, "channel = %d, j = %d, pha = %d", i, j, pha_chan[i]);
+    }
+
+    /* Close the pulse-height calibration file. */
+    FITS_close_file(phahfits, &status);
+
+    /* Set pulse height for each photon according to its channel number. */
+    for (j = 0; j < nevents; j++)
+	pha[j] = pha_chan[(int) channel[j]];
+
+    free(mjd);
+    free(pha_mjd);
+
+    cf_proc_update(header, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+
+    return status;
+}
diff --git a/src/libcf/cf_modify_hist_times.c b/src/libcf/cf_modify_hist_times.c
new file mode 100644
index 0000000..ba1b5d0
--- /dev/null
+++ b/src/libcf/cf_modify_hist_times.c
@@ -0,0 +1,83 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_modify_hist_times (fitsfile *infits, long nevents,
+ *                          float *time, GTI *gti);
+ *
+ * Description: For histogram data, set photon-arrival times to the midpoint
+ *              of the longest good-time interval.
+ *
+ * Arguments:   fitsfile   *infits        	Input FITS file pointer
+ *              long       nevents       	Number of photon events
+ *              float      *time 		Time array for photon list
+ *              GIT        *gti           	Good time interval(s)
+ *
+ * Calls:
+ *
+ * Returns:     TRUE if time array is changed.
+ *              FALSE if time array is not changed.
+ *
+ * History:     06/02/04   1.1   wvd    Initial coding
+ *		06/07/04   1.2   wvd	Use standard return values.
+ *		02/17/05   1.3   wvd	Initalize jmax to 0.
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include "calfuse.h"
+
+int
+cf_modify_hist_times (fitsfile *infits, long nevents, float *time, GTI *gti)
+{
+    char CF_PRGM_ID[] = "cf_modify_hist_times";
+    char CF_VER_NUM[] = "1.3";
+
+    int    errflg=0, status=0;
+    long   j, jmax=0;
+    float  exptime, gti_time, max_time, photon_time, rawtime;
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    /* If data were not taken in HIST mode, exit now. */
+    if ((errflg = cf_proc_check(infits, CF_PRGM_ID))) return errflg;
+
+    /* Read header keywords. */
+    FITS_read_key(infits, TFLOAT, "EXPTIME", &exptime, NULL, &status);
+    FITS_read_key(infits, TFLOAT, "RAWTIME", &rawtime, NULL, &status);
+
+    /* 
+     *  If the entire exposure was rejected by the screening routines,
+     *	we don't bother changing photon-arrival times.  If no time was
+     *	lost to screening, the default arrival times are OK.  Exit now.
+     */
+    if (exptime < 1. || exptime > rawtime - 1.) {
+	cf_proc_update(infits, CF_PRGM_ID, "COMPLETE");
+	cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+	return -1;
+    }
+
+    /* Determine which is the longest good-time interval. */
+    max_time = 0.;
+    for (j = 0; j < gti->ntimes; j++) {
+	if ((gti_time = gti->stop[j] - gti->start[j]) > max_time) {
+	    max_time = gti_time;
+	    jmax = j;
+	}
+    }
+
+    /* Set all photon-arrival times to midpoint of longest GTI. */
+    photon_time = (gti->start[jmax] + gti->stop[jmax]) / 2.;
+    for (j = 0; j < nevents; j++)
+	time[j] = photon_time;
+    cf_verbose(1, "Setting photon-arrival times to %.1f", photon_time);
+
+    cf_proc_update(infits, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return status;
+}
diff --git a/src/libcf/cf_nint.c b/src/libcf/cf_nint.c
new file mode 100644
index 0000000..8488911
--- /dev/null
+++ b/src/libcf/cf_nint.c
@@ -0,0 +1,47 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    n = cf_nint(x)
+ *
+ * Description: Converts double to nearest integer.
+ *
+ * Variables:   double    x	A double
+ *
+ * Return:      int       n	Nearest integer
+ *
+ * History:     08/25/03    wvd  v1.1   Begin work
+ *              02/09/04    wvd  v1.2   Add cf_nlong()
+ *              02/17/04    wvd  v1.3   Test for overflow of int, long
+ *              02/18/04    wvd  v1.4   Change format of error message.
+ *					Change from values.h to limits.h
+ *
+ *************************************************************************/
+
+#include <limits.h>
+#include "calfuse.h"
+
+int
+cf_nint(double x)
+
+{
+	if (x > INT_MAX || x < INT_MIN)
+	    cf_if_error("Cannot convert %10.4e to an integer", x);
+
+	if (x < 0.)	return (int) (x - 0.5);
+	else		return (int) (x + 0.5);
+}
+
+
+long
+cf_nlong(double x)
+
+{
+	if (x > LONG_MAX || x < LONG_MIN)
+	    cf_if_error("Cannot convert %10.4e to a long", x);
+
+        if (x < 0.)     return (long) (x - 0.5);
+        else            return (long) (x + 0.5);
+}
diff --git a/src/libcf/cf_optimal_extraction.c b/src/libcf/cf_optimal_extraction.c
new file mode 100644
index 0000000..4bbca9f
--- /dev/null
+++ b/src/libcf/cf_optimal_extraction.c
@@ -0,0 +1,551 @@
+/*****************************************************************************
+ *              Johns Hopkins University 
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_optimal_extraction(fitsfile *header, int optimal, 
+ *              int aperture, float *weight, float *y, unsigned char *channel,
+ *              float *lambda, long ngood, long *good_index,
+ *		float *barray, float *bpmask, int pny, float pycent,
+ *		float *parray, long nout, float *wave_out, float **flux_out,
+ *		float **sigma_out, long **counts_out, float **weights_out, 
+ *		float **bkgd_out, short **bpix_out)
+ *
+ * Description: Perform standard or optimal extraction of target spectrum.
+ *
+ * Note:	We use a modified version of the optimal-extraction
+ *		algorithm described by Keith Horne (PASP, 98, 609, 1986).
+ *
+ * Arguments:   fitsfile  *header       Pointer to IDF FITS file header
+ *		int	  optimal	TRUE if optimal extraction requested.
+ *		int	  aperture	Target aperture (values 1-8)
+ *		float	  *weight       Scale factor for each photon
+ *		float	  *y            Final y position of each photon
+ *		unsigned char *channel	Channel ID of each photon
+ *		float 	  *lambda       Wavelength for each photon
+ *		long	  ngood		Length of array good_index 
+ *		long	  *good_index	Indices of screened photon events
+ *		float     *barray       2-D background array
+ *                                       (flux-calibrated and binned)
+ *              float     *bpmask       2-D array containing bad pixel locations
+ *                                      Same size and location as the background array
+ *	        int       pny           Size in Y of weights array
+ *	        float     pycent        Y centroid of weights array
+ *	        float     parray        2-D weights array (binned)
+ *	        long      nout          Length of output arrays
+ *	        float     *wave_out	Output wavelength array
+ *	        float     **flux_out    Output flux array
+ *	        float     **sigma_out   Output error array
+ *	        long      **counts_out  Output counts array
+ *	        float     **weights_out Output weights array
+ *	        float     **bkgd_out 	Output background array
+ *              short     **bpix_out    Output bad pixel spectrum
+ *
+ * Returns:     0 on success
+ *
+ * History:     01/28/03   1.1   wvd    Initial coding
+ *              02/28/03   1.2   peb    Changed flux_out, var_out, counts_out
+ *                                      and weight_out argument variables to
+ *                                      pointer-to-pointers, so the arrays can
+ *                                      be returned to the calling routine.
+ *                                      Also tidied the code using lint.
+ *		03/11/03   1.3   wvd    Update documentation regarding use of
+ *					unsigned char
+ *		03/12/03   1.4   wvd    Change weights_out to sum of weights
+ *		03/19/03   1.5   wvd    Divide flux_out and var_out by WPC
+ *              04/04/03   1.6   rdr    - correct bugs in optimum extraction
+ *                                      - adjust criterion for redetermining
+ *                                        y centroid
+ *		05/07/03   1.7   wvd	Change ergcm2s to ergcm2 throughout. 
+ *					Divide by EXPTIME.  Use cf_verbose.
+ *		05/22/03   1.8   wvd	If EXPTIME = 0, set flux and error to 0.
+ *              05/28/03   1.9   rdr    - For HIST data, spread counts
+ *					  along the y dimension of
+ *                                        the data and variance arrays
+ *                                      - Incorporate the bad pixel mask into
+ *                                        optimal extraction algorithm
+ *                                      - Return bad-pixel spectrum
+ *              09/30/03   1.10  wvd    Negative values of YCENT are 
+ *					meaningless.  Use S/N of data to 
+ *					determine significance of YCENT.
+ *					Exclude airglow lines from S/N.
+ *              10/08/03   1.11  wvd    Change counts_out array to type long.
+ *					Add 0.5 to it before rounding.
+ *					Limit Y coordinates of probability
+ *					array before comparing with bkgd.
+ *              10/31/03   1.12  wvd    Read centroid quality flags from IDF
+ *					header.  Do not attempt to calculate
+ *					spectral centroid.
+ *              11/03/03   1.13  wvd    Modify calculation of variance estimate.
+ *					Modify scheme for smoothing HIST data.
+ *					Iterate only to 20% accuracy.
+ *              12/05/03   1.14  wvd    Check value of SPECBINY before
+ *					smoothing HIST data in the Y dimension.
+ *              03/16/04   1.15  wvd    In HIST mode, assume counts are
+ *					distributed across one X pixel.
+ *					Delete wave_out -- not used.
+ *					After 50 iterations, abandon optimal
+ *					extraction and use boxcar extraction
+ *					instead.
+ *					Don't test size of barray,
+ *					as it is now the same as parray.
+ *					Change pycent from int to float.
+ *              04/06/04   1.16  bjg    Include string.h
+ *                                      Remove unused variables
+ *              04/21/04   1.17  wvd	Set dispapix = fabs(dispapix).
+ *					Iterate to 5% accuracy.
+ *					In boxcar extraction, use parray to
+ *					set extraction limits.
+ *					For TTAG data, compute counts_out
+ *					directly from photon list.
+ *              04/26/04   1.18  wvd	Perform all calculations with
+ *					weights array, rather than ergcm2.
+ *					Return counts spectrum.
+ *					Convert from variance to sigma here,
+ *					rather than in cf_write_spectra.
+ *					Iterate to 10% accuracy.
+ *              05/17/04   1.19  wvd	If weights_out[j] = 0, set variance
+ *					= bkgd.  Iterate optimal extraction
+ *					to accuracy of 0.01 counts. In boxcar
+ *					extraction, reduce parray limit to
+ *					1E-4 to better match fluxes from 
+ *					optimal extraction for bright stars.
+ *              08/13/04   1.20  wvd	Use QUALITY array to set X limits 
+ *					of extraction region.  Insure that
+ *					sigma_out array is non-zero.
+ *              11/22/05   1.21  wvd	Scale variance estimate by bad-pixel
+ *					mask to better approximate observed
+ *					counts.
+ *              06/12/06   1.22  wvd	Call cf_verbose rather than
+ *					cf_if_warning.
+ *
+ ****************************************************************************/
+
+#include <unistd.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include <math.h>
+#include <string.h>
+
+#include "calfuse.h"
+
+static char 	CF_PRGM_ID[] = "cf_optimal_extraction";
+static char 	CF_VER_NUM[] = "1.22";
+
+int
+cf_optimal_extraction(fitsfile *header, int optimal, int aperture, 
+	float *weight, float *y, unsigned char *channel,
+	float *lambda, long ngood, long *good_index,
+	float *barray, float *bpmask, 
+	int pny, float pycent, float *parray, long nout, float *wave_out,
+	float **flux_out, float **sigma_out, long **counts_out,
+	float **weights_out, float **bkgd_out, short **bpix_out)
+
+{
+    char	instmode[FLEN_VALUE], yquality_str[FLEN_KEYWORD], 
+		ycent_str[FLEN_KEYWORD], yquality[FLEN_VALUE];
+    int   	status=0;
+    int		nloop;			/* Iterations of optimal
+						extraction loop */
+    int		ycent_uncertain = FALSE;/* TRUE if centroid quality
+						less than HIGH */
+
+    long	i, 			/* index through photon list */
+		ii,			/* ii = good_index[i] */
+		j, 			/* X index through 2-D arrays */
+		jmin, jmax,		/* limits of output spectrum */
+		k; 			/* Y index through 2-D arrays */
+    
+		 
+    float	exptime,		/* exposure time */
+		tdead,			/* mean dead-time correction */
+		w0,			/* minimum value of output wave array */
+		wpc,			/* wavelength increment per output bin */
+		*flux_old,		/* flux values from previous iteration */
+		*flux_box,		/* flux values from boxcar extraction */
+		*var_out,		/* 1-D variance array */
+		*var_box,		/* variance values from boxcar extraction */
+
+		ycent;			/* Y centroid of target spectrum */
+
+    double      numerator, denominator, /* Used in optimal-extraction calculations */
+		var_num, weights_num,
+		bkgd_num,
+		*data,			/* 2-D data array */
+		*variance,		/* 2-D variance array */
+		*w;			/* weights array for variance calculation */
+
+    int		l, lmin, lmax,		/* These variables are	*/
+    		specbiny, specbiny2;	/* are used to smooth	*/
+    float 	psum, pval;		/* HIST data in the	*/
+    double	vval;			/* Y dimension.		*/
+
+    long	jj, jjj, m, m_min, n;	/* These variables are used to smooth */
+    double	edge[2], frac[2], x; 	/* HIST data in the X dimension.      */
+    double	dispapix;		/* Mean dispersion per pixel */
+    char	wave_file[FLEN_VALUE];  /* Name of WAVE_CAL file */
+    int		hdunum;			/* HDU number of WAVE_CAL file */
+    fitsfile	*wavefits;		/* Pointer to WAVE_CAL file */
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    cf_verbose(3, "Entering cf_optimal_extraction");
+
+    /* 
+     *  Check type of observation (HIST or TTAG) and binning factor.
+     */
+    FITS_movabs_hdu(header, 1, NULL, &status) ;
+    FITS_read_key(header, TSTRING, "INSTMODE", instmode, NULL, &status);
+    FITS_read_key(header, TINT, "SPECBINY", &specbiny, NULL, &status);
+    specbiny2 = specbiny/2 ;
+    if (specbiny2 < 1) specbiny2 = 1 ;
+    cf_verbose(3, "Aperture = %d, instrument mode = %s, binning in Y = %d",
+	aperture, instmode, specbiny) ;
+
+    /*
+     *  Read EXPTIME and TOT_DEAD from file header.
+     */
+    FITS_read_key(header, TFLOAT, "EXPTIME", &exptime, NULL, &status);
+    FITS_read_key(header, TFLOAT, "TOT_DEAD", &tdead, NULL, &status);
+    if (tdead < 1.0) tdead = 1.0;
+    cf_verbose (3, "EXPTIME = %.0f, TOT_DEAD=%g", exptime, tdead);
+
+    /*
+     *  Read wavelength parameters W0 and WPC from file header.
+     */
+    FITS_read_key(header, TFLOAT, "WPC", &wpc, NULL, &status);
+    FITS_read_key(header, TFLOAT, "W0", &w0, NULL, &status);
+    cf_verbose (3, "Wavelength info: w0=%g, dw=%g", w0, wpc) ;
+
+    /*
+     *  Read spectral centroid YCENT and YQUAL from file header.
+     */
+    sprintf(ycent_str, "YCENT%1d", aperture);
+    FITS_read_key(header, TFLOAT, ycent_str, &ycent, NULL, &status);
+    sprintf(yquality_str, "YQUAL%1d", aperture);
+    FITS_read_key(header, TSTRING, yquality_str, yquality, NULL, &status);
+    if (*yquality != 'H') ycent_uncertain = TRUE;
+    cf_verbose (3, "%s = %g, quality = %s", ycent_str, ycent, yquality);
+
+    /*
+     * If HIST data, read DISPAPIX from header of WAVE_CAL file.
+     */
+    if (!strncmp(instmode,"H",1)) {
+	hdunum = aperture + 1;
+	FITS_read_key(header, TSTRING, "WAVE_CAL", wave_file, NULL, &status);
+	FITS_open_file(&wavefits, cf_cal_file(wave_file), READONLY, &status);
+	FITS_movabs_hdu(wavefits, hdunum, NULL, &status);
+	FITS_read_key(wavefits, TDOUBLE, "DISPAPIX", &dispapix, NULL, &status);
+	dispapix = fabs(dispapix);
+	FITS_close_file(wavefits, &status);
+    }
+
+    /*
+     *  Allocate space for all arrays.
+     */
+     data = (double *) cf_calloc(pny*nout, sizeof(double));
+     variance = (double *) cf_calloc(pny*nout, sizeof(double));
+     w = (double *) cf_calloc(nout, sizeof(double));
+
+     flux_old = (float *) cf_calloc(nout, sizeof(float));
+     flux_box = (float *) cf_calloc(nout, sizeof(float));
+     var_box  = (float *) cf_calloc(nout, sizeof(float));
+
+     *flux_out = (float *) cf_calloc(nout, sizeof(float));
+     var_out = (float *) cf_calloc(nout, sizeof(float));
+     *counts_out = (long *) cf_calloc(nout, sizeof(long));
+     *weights_out = (float *) cf_calloc(nout, sizeof(float));
+     *bkgd_out = (float *) cf_calloc(nout, sizeof(float));
+     *bpix_out = (short *) cf_calloc(nout, sizeof(short)) ;
+
+    /* 
+     *  The quality array (bpix_out) is the product of the probability
+     *  array and the bad-pixel mask.  We use it to set the limits of
+     *  the extraction region.
+     */
+     cf_verbose(3, "Generating bad-pixel spectrum.") ;
+     for (j=0; j<nout; j++) {
+         float bpix=0. ;
+         for (k=0; k<pny; k++)
+	   bpix += (parray[k*nout + j] * bpmask[k*nout + j]);
+         (*bpix_out)[j] = (short) (100. * bpix + 0.5) ;
+     }
+     jmin = 0L; jmax = nout;
+     for (j=0; j<nout; j++) {
+	if ((*bpix_out)[j] > 0) {
+	    jmin = j;
+	    break;
+	}
+     }
+     for (j = nout-1; j >= 0; j--) {
+	if ((*bpix_out)[j] > 0) {
+	    jmax = j+1;
+	    break;
+	}
+     }
+
+    /*
+     *  Construct data and variance arrays from photon lists.
+     *  Arrays are pny pixels in Y (to match probability array) 
+     *  and nout pixels in X (to match output wavelength array).  
+     *  We must thus shift individual photons by PYCENT - YCENT
+     *  pixels in Y.
+     */
+
+     cf_verbose(3, "Filling the data array") ;
+     for (i = 0; i < ngood; i++) {
+	ii = good_index[i];
+
+	if (channel[ii] != aperture) continue;
+
+	j = (long) ((lambda[ii] - w0)/wpc + 0.5);
+	if (j < jmin || j >= jmax) continue;
+
+	k = (long) (y[ii] - ycent + pycent + 0.5);
+	if (k < 0 || k >= pny) continue;
+
+        if (!strncmp(instmode,"T",1)) {
+	   /* TTAG data */
+	    (*counts_out)[j]++;
+	    data[k*nout + j] += weight[ii];
+	    variance[k*nout + j] += weight[ii] * weight[ii];
+	}
+	else { 
+	   /* If HIST data are already smoothed in Y, it's easy: */
+	   if (specbiny == 1) {
+	       data[k*nout + j] += weight[ii];
+	       variance[k*nout + j] += weight[ii] * tdead;
+	   }
+	   /* If HIST data are binned, smooth in both X and Y dimensions. */
+	    else {
+		m_min = 0;
+		edge[0] = ((double) j - 0.5) * wpc + w0;
+		edge[1] = ((double) j + 0.5) * wpc + w0;
+		if ((x = (lambda[ii] - edge[0]) / dispapix) < 0.5) {
+		   frac[0] = 0.5 - x;
+		   frac[1] = 0.5 + x;
+		   jj = j - 1;
+		   n = 2;
+		   if (jj == -1) m_min = 1;
+		}
+		else if ((x = (edge[1] - lambda[ii]) / dispapix) < 0.5) {
+		   frac[0] = 0.5 + x;
+		   frac[1] = 0.5 - x;
+		   jj = j;
+		   n = 2;
+		   if (jj + 1 == nout) n = 1;
+		}
+		else {
+		   frac[0] = 1.0;
+		   jj = j;
+		   n = 1;
+		}
+
+		psum = 0.;
+		vval = weight[ii] * tdead;
+		lmin = k - specbiny2;
+		lmax = lmin + specbiny;
+		if (lmin < 0) lmin = 0;
+		if (lmax > pny) lmax = pny;
+		pval = 1. / (lmax - lmin);
+		for (l = lmin; l < lmax; l++)
+		    psum += parray[l*nout + j];
+		for (l = lmin; l < lmax; l++) {
+		    if (psum > 0) pval = parray[l*nout + j] / psum;
+		    for (m = m_min; m < n; m++) {
+			jjj = jj + m;
+			data[l*nout + jjj] += pval * frac[m] * weight[ii];
+			variance[l*nout + jjj] += pval * frac[m] * vval;
+		    }
+		}
+	    }
+	}
+     }
+
+    /*
+     *  Boxcar extraction.  Use parray to set extraction limits in Y.
+     */
+     cf_verbose(3, "Doing the boxcar extraction.") ;
+     nloop = 0;
+     for (j = jmin; j < jmax; j++) {
+	for (k = 0; k < pny; k++) {
+	   if (parray[k*nout + j] > 1E-4) {
+	         (*bkgd_out)[j] += barray[k*nout + j];
+	             var_out[j] += variance[k*nout + j];
+	      (*weights_out)[j] += data[k*nout + j];
+	   }
+	}
+	(*flux_out)[j] = (*weights_out)[j] - (*bkgd_out)[j];
+     }
+
+    /*
+     *  Has the user requested optimal extraction?
+     */
+     cf_verbose(3,"Optimal keyword = %d ", optimal) ;
+     if (optimal) {
+
+       /*
+	*  If Y centroid is uncertain, abandon optimal extraction.
+	*/
+	if (ycent_uncertain)
+	   cf_verbose(1, "%s uncertain.  Cannot perform optimal extraction.",
+		ycent_str);
+
+	else {		/* Proceed with optimal extraction */
+
+ 	    cf_verbose(3, "Attempting optimal extraction");
+
+	/*
+	 *  Save boxcar versions of flux and variance arrays.
+	 */
+	for (j = jmin; j < jmax; j++) {
+	    flux_box[j] = (*flux_out)[j];
+	    var_box[j] = var_out[j];
+	}
+
+	/*
+	 *  Need array w[j] to scale the variance estimate.
+	 *  w[j] is mean scale factor from counts to weights at each wavelength.
+	 *  Must calculate for TTAG data; can use TOT_DEAD for HIST data.
+	 */
+	if (!strncmp(instmode,"T",1)) for (j = jmin; j < jmax; j++) {
+	    if ((*counts_out)[j] > 0) {
+		for (k = 0; k < pny; k++) w[j] += data[k*nout + j];
+		w[j] /= (*counts_out)[j];
+	    }
+	    else w[j] = tdead;
+	}
+	else for (j = jmin; j < jmax; j++) w[j] = tdead;
+
+	/*
+	 *  Begin big loop.
+	 */
+	do {
+	    /*
+	     *  Revise variance estimate
+	     *  We can omit w[j] here, as it appears in both the numerator
+	     *  and denominator of the flux estimate (below).
+	     *  05/17/02 wvd:  If weights_out[j] = 0, set variance = bkgd.
+	     *  11/22/05 wvd:  Scale variance estimate by bpmask.
+	     */
+	     for (j = jmin; j < jmax; j++) {
+		if ((*weights_out)[j] > 0)
+		   for (k = 0; k < pny; k++)
+			variance[k*nout + j] = bpmask[k*nout + j] *
+			fabs(parray[k*nout + j] * (*flux_out)[j] + barray[k*nout + j]);
+		else
+		   for (k = 0; k < pny; k++)
+			variance[k*nout + j] = bpmask[k*nout + j] * barray[k*nout + j];
+	     }
+
+	    /*
+	     *  Optimal extraction
+	     */
+	     nloop++;
+	     for (j = jmin; j < jmax; j++) {
+		numerator = denominator = 0.;
+		for (k = 0; k < pny; k++) if (variance[k*nout+j] > 0) {
+		    numerator += bpmask[k*nout+j] * parray[k*nout + j] * 
+                      (data[k*nout + j] - barray[k*nout + j]) / variance[k*nout + j];
+		    denominator += bpmask[k*nout+j] * parray[k*nout + j] * 
+                       parray[k*nout + j] / variance[k*nout + j];
+		}
+		flux_old[j] = (*flux_out)[j];
+		if (denominator > 0) (*flux_out)[j] = numerator / denominator;
+                else (*flux_out)[j] = flux_old[j] = 0. ;
+	     }
+
+	    /*
+	     *  Repeat loop if any element of flux_out has changed by > 0.01 counts.
+	     */
+	     for (j = jmin; j < jmax; j++) {
+		if (fabs((*flux_out)[j]-flux_old[j]) > 0.01) {
+		    cf_verbose(3, "%d\t%d\t%g", nloop, j, (*flux_out)[j]);
+		    break;
+		}
+	     }
+
+	} while (j < jmax && nloop < 50);	/* End of do loop */
+
+	/*
+	 *  If nloop < 50, calculate var_out, weights_out, and bkgd_out.
+	 *  Note that we must scale var_out by w[j] here.
+	 */
+	if (nloop < 50) {
+
+	    memset (*bkgd_out, 0, nout*sizeof(float));
+	    memset (*weights_out, 0, nout*sizeof(float));
+	    memset (var_out, 0, nout*sizeof(float));
+
+	    for (j = jmin; j < jmax; j++) {
+		bkgd_num = weights_num = var_num = denominator = 0.;
+		for (k = 0; k < pny; k++) if (variance[k*nout+j] > 0) {
+		   bkgd_num += bpmask[k*nout+j] * parray[k*nout + j] *
+                      barray[k*nout + j] / variance[k*nout + j];
+		   weights_num += bpmask[k*nout+j] * parray[k*nout + j] *
+                      data[k*nout + j] / variance[k*nout + j];
+		   var_num += bpmask[k*nout+j] * parray[k*nout + j];
+		   denominator += bpmask[k*nout+j] * parray[k*nout + j] * 
+                        parray[k*nout + j] / variance[k*nout + j];
+		}
+		if (denominator > 0) {
+		    (*bkgd_out)[j] = bkgd_num / denominator;
+		    (*weights_out)[j] = weights_num / denominator;
+		    var_out[j] = var_num / denominator * w[j];
+		}
+		else {
+		    (*bkgd_out)[j] = (*weights_out)[j] = var_out[j] = 0.;
+		}
+	    }
+	}
+	/*
+	 *  If nloop = 50, use boxcar extraction instead.
+	 */
+	else {
+	    cf_verbose(1, "Optimal extraction failed to converge for aperture %d."
+		"  Using boxcar extraction.", aperture);
+	    nloop = 0;
+	    for (j = jmin; j < jmax; j++) {
+		(*flux_out)[j] = flux_box[j];
+		var_out[j] = var_box[j];
+            }
+	}
+
+	}			/* End of if/else test of YCENT */
+     }				/* End of optimal extraction block */
+
+    /*
+     *  Write number of iterations to file header.
+     */
+     FITS_update_key(header, TINT, "OPT_EXTR", &nloop, NULL, &status);
+     cf_verbose(2, "Number of iterations in optimal extraction = %d", nloop) ;
+
+    /* Convert error array from variance to sigma. */
+    for (j = jmin; j < jmax; j ++) {
+	if (var_out[j] > 0.) var_out[j] = sqrt(var_out[j]);
+	else if ((*bkgd_out)[j] > 0.) var_out[j] = sqrt((*bkgd_out)[j]);
+	else var_out[j] = 0.;
+    }
+    *sigma_out = var_out;
+
+    /*
+     *  For HIST data, counts array = weights "uncorrected" for dead time.
+     */
+     if (!strncmp(instmode,"H",1)) for (j = jmin; j < jmax; j++)
+	(*counts_out)[j] = (long) ((*weights_out)[j] / tdead + 0.5);
+
+    /*
+     *  Clean up
+     */
+    free(data);
+    free(flux_old);
+    free(flux_box);
+    free(var_box);
+    free(variance);
+    free(w);
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return status;
+}
diff --git a/src/libcf/cf_pha_x_distort.c b/src/libcf/cf_pha_x_distort.c
new file mode 100644
index 0000000..5f58824
--- /dev/null
+++ b/src/libcf/cf_pha_x_distort.c
@@ -0,0 +1,107 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_pha_x_distort(fitsfile *header, long nevents, 
+ *			unsigned char *pha, float *xfarf,
+ *			unsigned char *locflags)
+ *
+ * Description: Corrects the X position of low-pulse-height events.
+ *
+ *		Note: To conform with the CalFUSE standard, the PHAX
+ *		correction is now ADDED to the input photon X coordinate.
+ *		This change from previous versions of the code requires
+ *		a new set of calibration files.  The program now checks the
+ *		version number of the PHAX_CAL file and returns an error if
+ *		it is less than 4.
+ *
+ * Arguments:   fitsfile  *header       Pointer to FITS file containing the
+ *                                      header of the intermediate data file
+ *              long      nevents       The number of events
+ *              unsigned  char *pha     An array of PHA values
+ *              float     *xfarf        An array of event X positions
+ *              unsigned char *locflags Location flags of each event
+ *
+ * Calls:
+ *
+ * Return:      0  on success
+ *
+ * History:     11/11/02   1.1    peb   Begin work
+ *              11/12/02   1.3    peb   Added check to move only events in
+ *                                      active region.
+ *		03/11/03   1.4    wvd   Changed pha and locflags to unsigned
+ *					char
+ *              05/20/03   1.5    rdr   Added call to cf_proc_check
+ *		07/29/03   1.6    wvd	If cf_proc_check fails, return errflg.
+ *		10/14/03   1.7    wvd	Add, rather than subtract, PHAX
+ *					correction.  Check cal file version.
+ *		10/17/03   1.8    wvd	Don't crash if CALFVERS keyword 
+ *					is missing.
+ *              04/07/07   1.9   wvd	Clean up compiler warnings.
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include <stdlib.h>
+#include "calfuse.h"
+
+int
+cf_pha_x_distort(fitsfile *header, long nevents, unsigned char *pha,
+		float *xfarf, unsigned char *locflags)
+{
+    char CF_PRGM_ID[] = "cf_pha_x_distort";
+    char CF_VER_NUM[] = "1.9";
+
+    char  phaxfile[FLEN_VALUE]={'\0'};
+    int   anynull=0, calfvers, errflg=0, status=0, xlen, ylen;
+    long  j;
+    float *phax, flt=0.;
+    fitsfile *phaxfits=NULL;
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    if ((errflg = cf_proc_check(header, CF_PRGM_ID))) return errflg;
+
+    /*
+     *  Read PHA correction (Walk) file
+     */
+    FITS_read_key(header, TSTRING, "PHAX_CAL", phaxfile, NULL, &status);
+    FITS_open_file(&phaxfits, cf_cal_file(phaxfile), READONLY, &status);
+    FITS_read_key(phaxfits, TINT, "NAXIS1", &xlen, NULL, &status);
+    FITS_read_key(phaxfits, TINT, "NAXIS2", &ylen, NULL, &status);
+
+    /* If CALFVERS keyword missing or less than 4, abort pipeline. */
+    fits_read_key(phaxfits, TINT, "CALFVERS", &calfvers, NULL, &status);
+    if (status || calfvers < 4) {
+	status = 0;
+	FITS_close_file(phaxfits, &status);
+	cf_if_error("Old versions of PHAX_CAL have wrong sign.  Aborting.");
+    }
+
+    /* Otherwise, read walk correction as an image. */
+    phax = (float *) cf_malloc(sizeof(float)*xlen*ylen);
+    FITS_read_img(phaxfits, TFLOAT, 1L, xlen*ylen, &flt, phax, &anynull, &status);
+    FITS_close_file(phaxfits, &status);
+
+    if (xlen != NXMAX)
+	cf_if_warning("NAXIS1 of %s != 16384", phaxfile);
+    /*
+     *  Apply PHA X correction to each event.
+     */
+    for(j=0; j<nevents; j++) {
+	/*
+	 *  Move only events in active region.
+	 */
+	if (!(locflags[j] & LOCATION_SHLD)) {
+	    xfarf[j] += phax[(int)(pha[j]*xlen + xfarf[j])];
+	}
+    }
+    free(phax);
+
+    cf_proc_update(header, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return 0;
+}
diff --git a/src/libcf/cf_proc_check.c b/src/libcf/cf_proc_check.c
new file mode 100644
index 0000000..0dd2c72
--- /dev/null
+++ b/src/libcf/cf_proc_check.c
@@ -0,0 +1,124 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_proc_check(fitsfile *fptr, char *prog_id)
+ *
+ * Description: cf_proc_check will determine whether a given calibration
+ *              step is to be performed on the data.
+ *
+ * Arguments:   fitsfile    *fptr	Pointer to input file
+ *              char        *prog_id 	Procedure name
+ *
+ * History:     05/21/98        emm     Begin work.
+ *              05/21/98        emm     finished
+ *              06/17/98        emm     Modified so that the keyword_tab
+ *                                      structure is read from ed_calfuse.h
+ *                                      file, which simplifies revisions in
+ *                                      the order of processing.
+ *              03/04/99        emm     I added use of errflg instead of
+ *                                      return so that it checks all parms.
+ *		04/01/03	wvd	Change fits_read_key_str to 
+ *					FITS_read_key, delete fits_print_err
+ *              05/20/03        rdr     remove part which checks previous steps
+ *              05/22/03 v1.6   wvd     Modify i/o; implement cf_verbose
+ *              07/23/03 v1.7   wvd     Modify i/o
+ *              09/10/03 v1.8   wvd     Bug fix: was printing HIST values
+ *					whenever called with verbose option.
+ *					Now returns TTAG when appropriate.
+ *              03/17/04 v1.9   wvd     Call cf_verbose rather than
+ *					cf_if_warning when program not
+ *					appropriate for HIST data.
+ *              06/02/04 v1.10  wvd     Call cf_verbose rather than
+ *					cf_if_warning when program not
+ *					appropriate for TTAG data.
+ *              11/26/04 v1.11  wvd     If header keyword is set to OMIT, skip
+ *					this step and set keyword to SKIPPED.
+ *              03/30/05 v1.12  wvd     If header keyword is set to SKIPPED,
+ *					skip this step.
+ *
+ ****************************************************************************/
+
+#include <stdio.h>
+#include <string.h>
+#include "calfuse.h"
+
+
+int cf_proc_check(fitsfile *fptr, char *prog_id) 
+{
+    char  comment[FLEN_CARD], instmode[FLEN_CARD];
+    char  key_value[FLEN_CARD];
+    int   j=0, errflg=0, status=0;
+
+    /*  The calfuse.h file contains the definitions of keyword_tab,
+     *  NUM_PROC_STEPS, and CALIBRATION_STEP_KEYS.
+     */
+    struct keyword_tab keytab[NUM_PROC_STEPS]=CALIBRATION_STEP_KEYS;
+
+    FITS_read_key(fptr, TSTRING, "INSTMODE", instmode, comment, &status);
+   
+    switch (instmode[0]) {
+    case 'H':
+	/*  Histogram mode */
+	/*  First, determine if this procedure is even supposed to be
+	 *  run on this data. */
+
+	while ((strncmp(keytab[j].hist_proc,prog_id,
+			strlen(keytab[j].hist_proc)) != 0) &&
+	       (j < NUM_PROC_STEPS)) j++;
+	if (j < NUM_PROC_STEPS) 
+	    cf_verbose(3, "cf_proc_check: prog_id=%s, key=%s, j=%d, value=%s",
+               prog_id, keytab[j].hist_proc, j, keytab[j].hist_value) ;
+	if ((j >= NUM_PROC_STEPS) || 
+	    (strncmp(keytab[j].hist_value, "PERFORM", 7))) {
+	    cf_verbose(1, "Not appropriate for HIST data.  Exiting.");
+	    errflg=1;
+	}
+
+	break;
+
+    case 'T':
+	/*  Time-tag mode */
+	/*  First, determine if this procedure is even supposed to be
+	 *  run on this data. */
+	while ((strncmp(keytab[j].ttag_proc,prog_id,
+			strlen(keytab[j].ttag_proc)) != 0) &&
+	       (j < NUM_PROC_STEPS)) j++;
+	if (j < NUM_PROC_STEPS) 
+	    cf_verbose(3, "cf_proc_check: prog_id=%s, key=%s, j=%d, value=%s",
+               prog_id, keytab[j].ttag_proc, j, keytab[j].ttag_value) ;
+	if ((j >= NUM_PROC_STEPS) || 
+	    (strncmp(keytab[j].ttag_value, "PERFORM", 7))) {
+	    cf_verbose(1, "Not appropriate for TTAG data.  Exiting.");
+	    errflg=1;
+	}
+
+	break;
+
+    default:
+	errflg = 1;
+    }
+
+    if (!errflg) {
+	/* Check to see whether user wants to skip this step. */
+	FITS_read_key(fptr, TSTRING, keytab[j].name, key_value, comment,
+		&status);
+	if (!strncmp(key_value, "OMIT", 4) || !strncmp(key_value, "SKIPPED", 7)) {
+	    cf_verbose(1, "Header keyword %s = %s.  Exiting.",
+		keytab[j].name, key_value);
+	    FITS_update_key(fptr, TSTRING, keytab[j].name, "SKIPPED", NULL,
+		&status);
+	    errflg=1;
+	}
+
+	/* Now check to see if the step has already been completed. */
+	if (!strncmp(key_value, "COMPLETE", 7)) {
+	    cf_if_warning("Exiting.\n\t%s has already been run on this file.", 
+		prog_id);
+	    errflg=1;
+	}
+    }
+    return errflg;
+}
diff --git a/src/libcf/cf_proc_update.c b/src/libcf/cf_proc_update.c
new file mode 100644
index 0000000..2e15d29
--- /dev/null
+++ b/src/libcf/cf_proc_update.c
@@ -0,0 +1,97 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_proc_update(fitsfile *fptr, char *prgm_id, char *key_value)
+ *
+ * Description: cf_proc_update will update the FITS header keyword 
+ *              which corresponds to the given prgm_id in the file 
+ *              fptr to the value given in key_value.
+ *
+ * Arguments:   fitsfile    *fptr	Pointer to input file
+ *              char        *prgm_id 	Procedure name
+ *              char        *key_value 	Updated procedure status
+ *
+ * History:     05/21/98        emm     Begin work.
+ *              05/21/98        emm     finished
+ *              06/17/98        emm     Modified so that the keyword_tab
+ *                                      structure is read from ed_calfuse.h
+ *                                      file, which simplifies revisions in
+ *                                      the order of processing.
+ *              09/08/99        peb     Added lines to update NEXTEND keyword
+ *              01/31/00        emm     Added update to DATE keyword.
+ *		04/01/03	wvd	Changed cf_errmsg to cf_if_warning,
+ *					fits_modify_key_str to FITS_update_key,
+ *					fits_read_key_str to FITS_read_key
+ *              12/18/03        bjg     Change calfusettag.h to calfuse.h
+ *              04/07/07  1.5   wvd     Delete CF_PRGM_ID, as it is not used.
+ *
+ ****************************************************************************/
+
+#include <stdio.h>
+#include <string.h>
+#include "calfuse.h"
+
+int cf_proc_update(fitsfile *fptr, char *prgm_id, char *key_value) 
+{
+
+    char  comment[FLEN_CARD], instmode[FLEN_CARD];
+    int i, status=0, hdutype=0, nextend;
+    /*
+     *  The calfuse.h file contains the definitions of keyword_tab
+     *  NUM_PROC_STEPS, and CALIBRATION_STEP_KEYS.
+     */
+    struct keyword_tab keytab[NUM_PROC_STEPS]=CALIBRATION_STEP_KEYS;
+
+    FITS_movabs_hdu(fptr, 1, &hdutype, &status);
+    FITS_get_num_hdus(fptr, &nextend, &status);
+    nextend -= 1;
+    FITS_update_key(fptr, TINT, "NEXTEND", &nextend, NULL, &status);
+    
+    FITS_read_key(fptr, TSTRING, "INSTMODE", instmode, comment, &status);
+
+    FITS_write_date(fptr, &status);
+
+    switch (instmode[0]) {
+    case 'H':
+	/*  Find the keyword associated with prgm_id by looping 
+	 *  through keytab[i].hist_proc */
+	i=0;
+	while ((strncmp(keytab[i].hist_proc,prgm_id,
+			strlen(keytab[i].hist_proc)) != 0) &&
+	       (i < NUM_PROC_STEPS)) i++;
+	if (i < NUM_PROC_STEPS) {
+	    /* We found a match to prgm_id, so change the associated
+	     * keyword in the header. */
+	    FITS_update_key(fptr, TSTRING,keytab[i].name,key_value, NULL, &status);
+	} else {
+	    /* The given prgm_id did not match any of the known
+	     * keytab[i].hist_proc, so return 1. */
+	    cf_if_warning("No PROCESSING STEP keyword is defined for %s", prgm_id);
+	    return 1;
+	}
+	break;
+    case 'T':
+	/*  Timetag mode */
+	/*  Find the keyword associated with prgm_id by looping 
+	 *  through keytab[i].ttag_proc */
+	i=0;
+	while ((strncmp(keytab[i].ttag_proc,prgm_id,
+			strlen(keytab[i].ttag_proc)) != 0) &&
+	       (i < NUM_PROC_STEPS)) i++;
+	if (i < NUM_PROC_STEPS) {
+	    /* We found a match to prgm_id, so change the associated
+	     * keyword in the header. */
+	    FITS_update_key(fptr, TSTRING,keytab[i].name,key_value, NULL, &status);
+	} else {
+	    /* The given prgm_id did not match any of the known
+	     * keytab[i].ttag_proc, so return 1. */
+	    cf_if_warning("No PROCESSING STEP keyword is defined for %s", prgm_id);
+	    return 1;
+	}
+	break;
+    }
+    return status;
+}
diff --git a/src/libcf/cf_read_fpa_pos.c b/src/libcf/cf_read_fpa_pos.c
new file mode 100644
index 0000000..87e8099
--- /dev/null
+++ b/src/libcf/cf_read_fpa_pos.c
@@ -0,0 +1,82 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_read_fpa_pos (fitsfile *infits, float *fpaxsic, float *fpaxlif)
+ *
+ * Description: Returns SiC and LiF FPA positions in microns.  Can read both
+ *              old and new FPA position keywords.
+ *
+ * Arguments:   fitsfile    *infile       Input data file name
+ *              float       *fpaxsic      FPA SiC position (returned)
+ *              float       *fpaxlif      FPA LiF position (returned)
+ *
+ * Returns:     int	     status	  CFITSIO status value
+ *
+ * History:     08/21/01   v1.1   wvd     Subroutine taken from cf_wfits.c
+ * 		01/14/03   v1.3   wvd     Change name to cf_read_fpa_pos.
+ *              12/18/03   v1.4   bjg     Change calfusettag.h to calfuse.h
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include "calfuse.h"
+
+/* for all FPA's an increase in "data number" moves the FPA towards +Xipcs */
+#define FPALIF1DN2X0 -69.949	/* DN to microns conversion, zero-point */
+#define FPALIF1DN2X1 .14144	/* DN to microns conversion, linear term  */
+#define FPALIF2DN2X0 -73.189	/* DN to microns conversion, zero-point */
+#define FPALIF2DN2X1 .14487	/* DN to microns conversion, linear term  */
+#define FPASIC1DN2X0 -132.507	/* DN to microns conversion, zero-point */
+#define FPASIC1DN2X1 .14156	/* DN to microns conversion, linear term  */
+#define FPASIC2DN2X0 -89.116	/* DN to microns conversion, zero-point */
+#define FPASIC2DN2X1 .14206	/* DN to microns conversion, linear term  */
+
+int cf_read_fpa_pos (fitsfile *infits, float *fpaxsic, float *fpaxlif)
+{
+    char  detector[FLEN_VALUE]; /* detector keyword from FITS header */
+    int	status=0;
+    float tmpxsic, tmpxlif;
+
+    FITS_read_key(infits, TSTRING, "DETECTOR", detector, NULL, &status);
+
+    /* Get FPA positions */
+    /* Use ffgky instead of FITS_read_key so we can read either the old
+     * or new FPA position keywords */
+    ffgky (infits, TFLOAT, "FPASXPOS", fpaxsic, NULL, &status);
+    if (status != 0) {
+	/* New keywords are not present; must be the old ones.
+	 * Determine which detector provided current spectrum
+	 * and convert raw FPA position to microns.
+	 */
+	status = 0;
+	if (strncmp(detector,"1", 1)==0) {
+	    FITS_read_key (infits, TFLOAT, "FP1SXPOS", &tmpxsic, NULL, 
+			   &status);
+	    FITS_read_key (infits, TFLOAT, "FP1LXPOS", &tmpxlif, NULL, 
+			   &status);
+	    *fpaxsic = FPASIC1DN2X0 + FPASIC1DN2X1 * tmpxsic;
+	    *fpaxlif = FPALIF1DN2X0 + FPALIF1DN2X1 * tmpxlif;
+	}
+	else if (strncmp(detector,"2", 1)==0) {
+	    FITS_read_key (infits, TFLOAT, "FP2SXPOS", &tmpxsic, NULL, 
+			   &status);
+	    FITS_read_key (infits, TFLOAT, "FP2LXPOS", &tmpxlif, NULL, 
+			   &status);
+	    *fpaxsic = FPASIC2DN2X0 + FPASIC2DN2X1 * tmpxsic;
+	    *fpaxlif = FPALIF2DN2X0 + FPALIF2DN2X1 * tmpxlif;
+	}
+	else {
+	    cf_if_error("Could not parse DETECTOR keyword, cannot "
+			"convert raw FPA positions.");
+	}
+    }
+    else {
+	/* New SiC FPA keyword present. Assume new LiF FPA keyword
+	 * is also present */
+	FITS_read_key(infits, TFLOAT, "FPALXPOS", fpaxlif, NULL, &status);
+    }
+    return status;
+}
diff --git a/src/libcf/cf_rebin_background.c b/src/libcf/cf_rebin_background.c
new file mode 100644
index 0000000..23e15f3
--- /dev/null
+++ b/src/libcf/cf_rebin_background.c
@@ -0,0 +1,211 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences 
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:   cf_rebin_background(infits, aperture, nout, wave_out,
+ *		  binx, biny, bnx, bny, bimage, barray) 
+ *
+ * Arguments:   *fitsfile  infits     :  Input IDF file
+ *              int       aperture    :  Aperture ID for the analysis
+ *              long      nout        :  Length of wave_out array
+ *              float     wave_out    :  Wavelength vector
+ *              int       binx, biny  :  Binning factors of the background array
+ *              int       bnx, bny    :  X and Y dimension of the background array
+ *              float     bimage      :  2-D background image (original) 
+ *              float     barray      :  (OUTPUT) Binned background image.
+ *
+ * Description:
+ *
+ *	The input background image is binned in X.
+ *	We need an image binned in wavelength.   
+ *	To get it, we use the WAVE_CAL file (shifted to account
+ *	for the FPA position) to derive a wavelength array for the
+ *	background image.  For each row in the background image (bimage),
+ *	we build a second image (barray) scaled to the size of the output 
+ *	wavelength bins.
+ *
+ *  History     02/21/03   v1.1   rdr   Started work
+ *              04/01/03   v1.2   rdr   Made aeff arrays double precision in 
+ *                                      the cf_read_fluxcal routine to be 
+ *                                      compatible with data in calfiles
+ *		05/07/03   v1.4   wvd	Don't divide by EXPTIME.
+ *					Read WPC from file header.
+ *					Use cf_verbose.
+ *              06/02/03   v1.5   rdr   Correct bug in filling output arrays
+ *              06/11/03   v1.7   wvd	Pass datatype to cf_read_col.
+ *					Change calfusettag.h to calfuse.h
+ *              08/22/03   v1.8   bjg	Move get_extraction_limits to external
+ *					subroutine.  Free orphan arrays.
+ *					Change coltype from char to int in
+ *					cf_read_col.
+ *              08/28/03   v1.9   wvd	Debug
+ *              09/29/03   v1.10  wvd	Shift background model to match
+ *					position of FPA.
+ *              03/16/04   v1.11  wvd	Correct error in calculation of dw_ave
+ *					and dweff.
+ *              04/05/04   v1.12  wvd	Modify i/o.
+ *              04/26/04   v1.13  wvd	Do not flux-calibrate 2-D background
+ *					model.  Do not extract 1-D background
+ *					spectrum.
+ *              05/13/04   v1.14  wvd	Correct value of CF_PRGM_ID.
+ *              07/21/04   v1.16  wvd	Delete unused variables.
+ *
+ *****************************************************************************/
+
+#include <math.h>
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include "calfuse.h"
+
+
+int cf_rebin_background(fitsfile *infits, int aperture, long nout,
+	float *wave_out, int binx, int biny, int bnx, int bny,
+	float *bimage, float **barray) {
+
+    char CF_PRGM_ID[] = "cf_rebin_background";
+    char CF_VER_NUM[] = "1.16";
+
+    fitsfile  *wavefits ;
+    int       status=0;
+    int       dndx, dpix, nyout;
+    long      npix, npix_out, nwave, ndx, ndx1, ndx2;
+    long      i, j, k;
+    float     dwb, dw_out, mf, ctot, dw_ave;
+    float     dpix_fpa;
+    float     *wave, *wavet, *outarr;
+    char      wavefile[FLEN_VALUE], det[FLEN_VALUE] ;
+
+    /* Initialize error checking */
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Started execution.");
+
+    /* Read wavelength spacing of the output array */
+    FITS_read_key(infits, TFLOAT, "WPC", &dw_out, NULL, &status) ;
+    cf_verbose(3, "Bin size of the output wavelength array = %5.3f A",
+	dw_out) ;
+    FITS_read_key(infits, TSTRING, "DETECTOR", det, NULL, &status) ;
+    cf_verbose(3,"Detector = %s, aperture = %d", det, aperture) ;
+
+    /* Read wavelength-calibration file */
+    FITS_read_key(infits, TSTRING, "WAVE_CAL", wavefile, NULL, &status) ;
+    cf_verbose(3, "Wavelength calibration file = %s",wavefile) ;
+    FITS_open_file(&wavefits, cf_cal_file(wavefile), READONLY, &status) ;
+    cf_verbose(3, "HDU to read = %d",aperture+1) ;
+    FITS_movabs_hdu(wavefits, aperture +1, NULL, &status) ;
+    nwave=cf_read_col(wavefits,TFLOAT,"WAVELENGTH",(void **) &wave);
+    cf_verbose(3, "Points read = %d, min & max: %4.2f, %4.2f",
+	nwave, wave[0], wave[nwave-1]);
+
+    /* Read pixel shifts due to FPA positions */
+    if (aperture < 5) 
+	FITS_read_key(infits, TFLOAT, "FPADXLIF", &dpix_fpa, NULL, &status);
+    else 
+	FITS_read_key(infits, TFLOAT, "FPADXSIC", &dpix_fpa, NULL, &status);
+    dpix = cf_nint(dpix_fpa);
+
+    /* To correct for the position of the FPA, each photon has been shifted
+	in X by dpix pixels.  Rather than shifting the background to match,
+	we modify the wavelength array that maps the background onto the
+	output spectrum. */
+    cf_verbose(2, "Shifting aperture %d background by %d X pixels "
+	"to match the FPA shift.", aperture, cf_nint(dpix_fpa));
+
+    /*  Generate a new wavelength array binned to match the background array */
+    cf_verbose(3, "X and Y binning factors for background array = %d, %d",
+	binx, biny) ;
+
+        wavet = (float *) cf_calloc(bnx, sizeof(float));
+	for (i = 0; i < bnx; i++) {
+          ndx=i * binx + (binx/2) + dpix;
+	  if (ndx > nwave-1) ndx = nwave-1 ;
+	  if (ndx < 0) ndx = 0;
+	  wavet[i] = wave[ndx];
+	 }
+
+      /* Error check: average wavelength spacing */
+      dw_ave = fabs(wavet[bnx-1]-wavet[0])/(bnx-1);
+      cf_verbose(3,"Average wavelength spacing of background array = %f", dw_ave) ;
+
+      if ((aperture < 4 && strncmp(det,"1",1) == 0) ||
+	  (aperture > 4 && strncmp(det,"2",1) == 0)) {
+           cf_verbose(3, "Maximum tabulated wavelength = %.2f", wavet[bnx-1]);
+           cf_verbose(3, "Maximum of wave_out = %.2f", wave_out[nout-1] );
+      }
+      else {
+           cf_verbose(3, "Maximum tabulated wavelength = %.2f", wave_out[nout-1] );
+           cf_verbose(3, "Maximum of wave_out = %.2f", wave_out[nout-1] );
+      }
+
+  /* Define some sizes and allocate space for the output arrays */
+  nyout = bny * biny ;		/* Y dimension of output 2-D bkgd array */
+  npix_out = nout * nyout ;	/* Size of output 2-D bkgd array */
+  npix = bnx * bny ;		/* Size of input 2-D bkgd array */
+  outarr = (float *) cf_calloc(npix_out, sizeof(float) ); /* 2-D output array */
+
+    /* Error check: total counts in the background image */
+    ctot=0.;
+    for (i=0; i<npix; i++) ctot+=bimage[i] ;
+    cf_verbose(3, "Number of counts in the input bkgd image = %f",ctot) ;
+
+  /* For each wavelength in the output array, find the nearest point
+     in the input background array.  Scale its value by the relative
+     sizes of the background and output wavelength bins.
+
+     Remember: wavelengths for the Lif channels and the SiC channels run
+               in opposite directions.  For side one, wavelengths increase 
+               with index for Lif but decrease for SiC. The opposite is true
+	       for side two. */
+  ndx=0 ;
+  dndx = 1 ; 
+  if ((aperture < 4 && strncmp(det,"2",1) == 0)  ||
+      (aperture > 4 && strncmp(det,"1",1) == 0 ) ) {
+    ndx = bnx - 1 ;
+    dndx = -1 ;
+  }
+
+  cf_verbose(3,"Filling output: starting ndx=%d, increment =%d ", ndx, dndx) ;
+
+  dwb = dw_ave;
+  for (i=0; i<nout; i++) {
+    /* Locate the element of the bkgd array corresponding to this wavelength */
+        while (wavet[ndx] < wave_out[i] && ndx < bnx && ndx >= 0) ndx += dndx ;
+
+	/* compute the relative
+           wavelength coverage of the background and output arrays */
+        if (ndx < bnx-2) dwb = fabs((double) (wavet[ndx+1]-wavet[ndx])) ;
+	   mf = dw_out/dwb ;
+	/* correct the scale factor for binning in y */
+           mf /= biny ;
+	/* populate the column of the array */
+	for (j=0; j< nyout ; j++) {
+          k = j/biny ;
+          ndx1 = j*nout + i ;
+	  if (ndx1 > npix_out-1) ndx1 = npix_out-1 ;
+	  ndx2 = k*bnx + ndx ;
+	    if (ndx2 > npix-1) ndx2=npix-1 ;
+	  outarr[ndx1] = mf * bimage[ndx2] ; 
+	}
+  }
+
+
+    /* Error checking: total counts in the background image */
+    ctot=0.;
+    for (i=0; i<npix_out; i++) ctot+=outarr[i] ;
+    cf_verbose(3, "Number of counts in the output bkgd image = %f", ctot) ;
+
+
+ /* Return output arrays */
+    *barray = outarr ;
+     
+ /* Close wavelength calibration file */
+      FITS_close_file(wavefits, &status) ;
+
+   free(wave);
+   free(wavet);
+
+   cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished execution.");
+   return status;
+}
diff --git a/src/libcf/cf_rebin_probability_array.c b/src/libcf/cf_rebin_probability_array.c
new file mode 100644
index 0000000..285441e
--- /dev/null
+++ b/src/libcf/cf_rebin_probability_array.c
@@ -0,0 +1,180 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences  
+ *              FUSE  
+ *****************************************************************************
+ *
+ * Synopsis: cf_rebin_probability_array(infits, extended, aperture, nout,
+ *		wave_out, pny, pycent, parray)
+ *
+ * Arguments:     *fitsfile  infits     :  Input IDF file
+ *                int        extended   :  TRUE if target is extended
+ *                int        aperture   :  Aperture ID for the analysis
+ *                long       nout       :  number of output wavelength bins
+ *                float      wave_out   :  output wavelength vector
+ *                int        pny        :  y dimension of probability array
+ *                float      pycent     :  y position of the peak of the 
+ *                                           probability array
+ *                float      parray     :  probability array
+ *
+ * History:       02/20/03   v1.1   rdr    Started work
+ *                04/03/03   v1.2   rdr    Normalize so that integral along y
+ *                                         at each sample point is 1
+ *                06/02/03   v1.3   rdr    Correct error in filling output array
+ *                09/30/03   v1.5   wvd    Use cf_read_col to read WAVE_CAL.
+ *                03/22/04   v1.6   wvd    Change pycent from int to float.
+ *                03/23/04   v1.7   wvd    Shift weights array to account for
+ *					   FPA shifts.
+ *                06/14/04   v1.8   wvd    Because the weights array is defined
+ *					   wrt the FARF, we need not correct
+ *					   for FPA shifts here.
+ *                05/17/05   v1.9   wvd    Don't normalize regions where the
+ *					   total probability is less than 0.1.
+ *					   Set them to zero.
+ *		  06/15/05   v1.10  wvd	   BUG FIX: Program always read the
+ *					   probability arrays for point-source 
+ *					   targets from the WGTS_CAL file.  Now
+ *					   it distinguishes between point-source
+ *					   and extended targets.
+ *
+ *****************************************************************************/
+
+#include <math.h>
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include "calfuse.h"
+
+int cf_rebin_probability_array(fitsfile *infits, int extended, int aperture,
+	long nout, float *wave_out, int *pny, float *pycent, float **parray)
+{
+
+  char CF_PRGM_ID[] = "cf_rebin_probability_array";
+  char CF_VER_NUM[] = "1.10";
+
+  fitsfile *wgtsfits, *wavefits ;
+  int status=0, fpixel=1, nullval=0, anynull=0 ;
+  int hdu, nxwt, nywt, dndx, wtbin;
+  long npix, npix_out, nwave, ndx, ndx1, ndx2, i, j ; 
+  float *wave, *wavet, *wgts_arr, *ynorm, *outarr ;
+  float total, wgt_cent ;
+  char wgtsfile[FLEN_VALUE]={'\0'}, wavefile[FLEN_VALUE]={'\0'} ;
+  char buffer[FLEN_CARD], det[FLEN_CARD] ;
+
+    /* Initialize error checking */
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Started execution.");
+
+  /* Read calibration file names from the IDF file header. */
+  FITS_movabs_hdu(infits, 1, NULL, &status) ;
+  FITS_read_key(infits, TSTRING, "WGTS_CAL", wgtsfile, NULL, &status) ;
+    cf_verbose(3,"weights cal file = %s ",wgtsfile) ;
+  FITS_read_key(infits, TSTRING, "WAVE_CAL", wavefile, NULL, &status) ;
+    cf_verbose(3, "wavelength cal file = %s ",wavefile) ;
+  FITS_read_key(infits, TSTRING, "DETECTOR", det, NULL, &status) ;
+    cf_verbose(3,"Detector = %s ",det) ;
+
+  /* Open the weights file and read the array */
+  FITS_open_file(&wgtsfits, cf_cal_file(wgtsfile), READONLY, &status) ;
+  hdu = extended * 8 + aperture + 1;
+  cf_verbose(3, "WGTS_CAL: extended = %d, aperture = %d, hdu = %d",
+	extended, aperture, hdu);
+  FITS_movabs_hdu(wgtsfits, hdu, NULL, &status) ;
+  FITS_read_key(wgtsfits, TINT, "NAXIS1", &nxwt, buffer, &status) ;
+  FITS_read_key(wgtsfits, TINT, "NAXIS2", &nywt, buffer, &status) ;
+  FITS_read_key(wgtsfits, TFLOAT, "WGT_CENT", &wgt_cent, buffer, &status) ;
+  npix=nxwt * nywt ;
+  cf_verbose(3, "prob array: nx=%d, ny=%d, wgt_cent=%f ",nxwt, nywt, wgt_cent);
+  wgts_arr = (float *) calloc(npix, sizeof(float)) ;
+  FITS_read_img(wgtsfits, TFLOAT, fpixel, npix, &nullval, wgts_arr, 
+		 &anynull, &status) ;
+  FITS_close_file(wgtsfits, &status) ;
+
+  /* Read the wavelength array */
+  FITS_open_file(&wavefits, cf_cal_file(wavefile), READONLY, &status) ;
+  FITS_movabs_hdu(wavefits, aperture +1, NULL, &status) ;
+  nwave=cf_read_col(wavefits,TFLOAT,"WAVELENGTH", (void **) &wave);
+  FITS_close_file(wavefits, &status) ;
+
+  /* Determine the binning factor for the weights and generate a new
+     wavelength array that corresponds to the binning factor used. */
+	wtbin = NXMAX / nxwt ;
+	cf_verbose(3, "Binning factor for weights array = %d ", wtbin) ;
+	wavet = (float *) cf_calloc(nxwt, sizeof(float) ) ;
+	for (i=0; i<nxwt; i++) {
+	    ndx=i * wtbin + (wtbin/2);
+	    if (ndx > nwave-1) ndx = nwave-1 ;
+	    if (ndx < 0) ndx = 0 ;
+	    wavet[i] = wave[ndx] ;
+	}
+
+  /* Allocate space for the output array */
+  npix_out = nout * nywt ;
+  if ((aperture < 4 && strncmp(det,"1",1) == 1) ||
+      (aperture > 4 && strncmp(det,"2",1) == 1)) 
+      cf_verbose(3, "maximum tabulated wavelength = %g, "
+	"maximum of wave_out=%g", wavet[nxwt-1],wave_out[nout-1] );
+  else
+      cf_verbose(3, "maximum tabulated wavelength = %g, "
+	"maximum of wave_out=%g", wavet[0],wave_out[nout-1] );
+  outarr = (float *) cf_calloc(npix_out, sizeof(float)) ;
+
+  /* Fill in the output array - use the weight profile which is closest
+     to the individual wavelengths in the output wavelength array. 
+     Remember : the Lif channels and the SiC channels have wavelengths
+     that run in opposite directions, e.g. for side 1 wavelengths
+     increase with index for Lif but decrease for SiC. The opposite is
+     true for side 2. */
+
+  ndx=0 ;
+  dndx = 1 ; 
+  if ((aperture < 4 && strncmp(det,"2",1) == 0) ||
+      (aperture > 4 && strncmp(det,"1",1) == 0 ) ) {
+    ndx = nxwt - 1 ;
+    dndx = -1 ;
+  }
+
+  cf_verbose(3, "filling output: starting index = %d, increment = %d ",
+	ndx, dndx) ;
+
+  for (i=0; i<nout; i++) {
+    /* locate the wavelength corresponding to this entry */
+        while (wavet[ndx] < wave_out[i] && ndx <= nxwt-1 && ndx >= 0 )
+		ndx += dndx ;
+	/* populate the column of the array */
+	for (j=0; j<nywt ; j++) {
+          ndx1 = j*nout + i ;
+	  if (ndx1 > npix_out-1) ndx1 = npix_out-1 ;
+	  ndx2 = j*nxwt + ndx ;
+	    if (ndx2 > npix-1) ndx2=npix-1 ;
+	  outarr[ndx1] = wgts_arr[ndx2] ; 
+	}
+  }
+
+  /* Adjust the probabilities so that the integral along y at every 
+     wavelength position is 1 */
+
+  /* First sum the points along y (ynorm) at each point */
+  ynorm= (float *) cf_calloc(nout, sizeof(float)) ;
+  for (i=0; i<nout; i++) {
+    total=0. ;
+    for (j=0; j<nywt; j++) total += outarr[j*nout+i] ;
+    ynorm[i]=total ;
+  }
+
+  /* Normalize all points by dividing by the total */
+  for (i=0; i<nout; i++) {
+     if (ynorm[i] > 0.1)
+	for (j=0; j<nywt; j++) outarr[j*nout+i] /= ynorm[i] ;
+     else
+	for (j=0; j<nywt; j++) outarr[j*nout+i] = 0. ;
+  }
+          
+  /* Redirect the output pointers. */
+  *pny = nywt ; 
+  *pycent = wgt_cent ;
+  *parray = outarr ; 
+
+  cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished execution.");
+  return status;
+}
diff --git a/src/libcf/cf_satellite_jitter.c b/src/libcf/cf_satellite_jitter.c
new file mode 100644
index 0000000..9f3a5d9
--- /dev/null
+++ b/src/libcf/cf_satellite_jitter.c
@@ -0,0 +1,245 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center for Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_satellite_jitter infile, nevents, time, x, y, channel,
+ *              	nsec, ttime, status_flag)
+ *
+ * Description: Correct photon coordinates for spacecraft motion.
+ *
+ *		Operates only on point-source observations made in TTAG mode.
+ *		Only photon events in the target aperture are corrected.
+ *		Minimum trustworthy TRKFLG value is read from parameter file.
+ *
+ *              Key to new TRKFLG values:
+ *      	5 = dx, dy from known FPDs and q_cmd from telemetry
+ *      	4 = good dx, dy from ACS q_est and q_cmd from telemetry
+ *      	3 = maybe good dx, dy from ACS q_est
+ *      	2 = dx, dy from known FPDs, but q_cmd from FITS header coords
+ *      	1 = dx, dy from ACS q_est, but q_cmd from FITS header coordis
+ *      	0 = no pointing information (missing telemetry)
+ *             -1 = pointing is assumed to be bad (never achieved known track)
+ *
+ * Arguments:   fitsfile  infile        Pointer to the IDF
+ *              long      nevents       The number of events
+ *              float     *time         An array of event times
+ *              float     *x            An array of event X positions
+ *              float     *y            An array of event Y positions
+ *     unsigned char      *channel      Channel assignment for each photon
+ *              long      nsec          Number of seconds in the timeline
+ *              long      *ttime        time (sec) of each point in the timeline
+ *     unsigned char      *status_flag  Timeline status flags
+ *
+ * Returns:	0 upon success
+ *
+ * History:     09/12/02   v1.1   RDR   Adapted from cf_ttag_jitter
+ *              10/02/02   v1.2   RDR   Modified to be compatable with
+ *                                      new IDF file format
+ *              12/10/02   v1.3   RDR   Adjusted method of populating the 
+ *                                      timeline jitter status flag. 
+ *              12/13/02   v1.4   RDR   Exit gracefully if there is no jitr file 
+ *              03/01/03   v1.6   wvd   Correct use of pointer in FITS_read_key
+ *              04/07/03   v1.7   wvd   Confirm that TRKFLG <= 5.
+ *					Replace printf with cf_verbose.
+ *              04/14/03   v1.8   rdr   Changed flag from char to unsigned char
+ *              04/22/03   v1.9   wvd   Move only photons in target aperture.
+ *					Do not assume that ttime is continuous.
+ *              04/29/03   v1.10  wvd   Allow possiblity that jitter
+ *                                      filename is in lower-case letters.
+ *              05/20/03   v1.11  rdr   Added call to cf_proc_check
+ *              05/22/03   v1.12  wvd   Direct cf_error_init to stderr
+ *              07/11/03   v1.13  rdr   Set all points as bad if JIT_STAT=1
+ *                                       (no reference position found)
+ *              08/06/03   v1.14  wvd   Improve documentation, delete
+ *					comparison with GTI's, change channel
+ *					array to unsigned char.
+ *              08/29/03   v1.15  wvd   Set all points as bad if JIT_STAT != 0
+ *              09/18/03   v1.16  wvd   Print name of jitter file only if
+ *					the file exists.
+ *              10/03/03   v1.17  wvd   Check HKEXISTS before looking for 
+ *					jitter file.
+ *              02/12/04   v1.18  wvd   Make interpolation immune
+ *					to errors in jitter time array.
+ *              02/24/04   v1.19  rdr   Change limits of acceptable jitter
+ *					values
+ *              03/01/04   v1.20  rdr   Populate the PLATESC keyword in the
+ *					input file header
+ *              06/01/04   v1.21  bjg   Exit when keyword JIT_STAT not found.
+ *              06/07/04   v1.22  wvd   Return EXP_JITR to calling routine.
+ *		01/26/05   v1.23  wvd   Fix tiny bug in a verbose stmt.
+ *		04/05/05   v1.24  wvd   If JIT_STAT != 0, APERTURE = RFPT,
+ *					or target = airglow, exit without 
+ *					flagging any times as bad.
+ *					Use new TRKFLG values (see above).
+ *					Delete adjust_trkflg subroutine and
+ *					the J_TRKFLG and JTIMEGAP keywords.
+ *					Use cf_read_col to read jitter file.
+ *		07/06/05   v1.25  wvd   If JIT_VERS < 2.0, issue a warning.
+ *		11/29/05   v1.26  wvd	Move screening functions into 
+ *					cf_screen_jitter.
+ *              08/21/06   v1.27  wvd   Use EXPSTART in jitter and data
+ *                                      headers to correct jitter time array.
+ *              08/25/06   v1.28  wvd   Change meaning of TRKFLG values.
+ *                                      TRKFLG = 3 is only used internally.
+ *              11/06/06   v1.29  wvd   Change meaning of TRKFLG values.
+ *					Read APER_COR keyword in file header.
+ *					Read min TRKFLG value from parmfile.
+ *					Don't have to test observing mode.
+ *              03/23/07   v1.30  wvd   Store offset between the jitter and 
+ *					data values of EXPSTART in variable
+ *					time_diff.
+ *              04/07/07   v1.31  wvd   Clean up compiler warnings.
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include <ctype.h>
+#include "calfuse.h"
+
+int
+cf_satellite_jitter(fitsfile *infits, long nevents, float *time,
+	float *x, float *y, unsigned char *channel, long nsec,
+	float *ttime, unsigned char *status_flag)
+{
+    char CF_PRGM_ID[] = "cf_satellite_jitter"; 
+    char CF_VER_NUM[] = "1.31";
+
+    fitsfile  *jitfits, *parmfits;
+    char  det[FLEN_VALUE];
+    char  jitr_cal[FLEN_VALUE], parmfile[FLEN_VALUE];
+    char  comment[FLEN_COMMENT];
+    short c, *trkflg, trkflg_min;
+    int   active_ap[2], extended, status=0, hdutype;
+    long  j, k, njitr, nrej, *time_jit, time_diff;
+    double data_expstart, jitr_expstart;
+    float *dx_jit, *dy_jit, x_factor, y_factor;
+    float *dx_tt, *dy_tt;
+    float factor[2][4] = {{1.743,1.743,-1.743, -1.743},
+			  {1.154,1.163,-0.6335,-0.581}};
+
+    /* Initialize error checking */ 
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+    /* Enter a time stamp into the log */
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    /* Read exposure start time from IDF header */
+    FITS_read_key(infits, TDOUBLE, "EXPSTART", &data_expstart, NULL, &status);
+
+    /* If APER_COR is not set to "COMPLETE", exit now. */
+    FITS_read_key(infits, TSTRING, "APER_COR", comment, NULL, &status);
+    if (strncmp(comment, "COMPLETE", 8)) {
+        cf_verbose(1, "APER_COR = %s.  Omitting photon shift.", comment);
+	cf_proc_update(infits, CF_PRGM_ID, "SKIPPED");
+	return (status);
+    }
+
+    /* If target is an extended source, exit now. */
+    extended = cf_source_aper(infits, active_ap);
+    if (extended) {
+	cf_verbose(1, "Extended source.  Omitting photon shift.");
+	cf_proc_update(infits, CF_PRGM_ID, "SKIPPED");
+	return (status);
+    }
+
+    /* Determine the scale factor to convert arcseconds to pixels. */
+    FITS_read_key(infits, TSTRING, "DETECTOR", det, NULL, &status);
+    c = det[0] =='2'? 2: 0;
+    if (det[1] == 'B')
+	c++;
+    x_factor=factor[0][c];
+    y_factor=factor[1][c];
+
+    /* Update the PLATESC (plate scale) keyword in the header */
+    FITS_update_key(infits, TFLOAT, "PLATESC", &y_factor, NULL, &status);
+
+    cf_verbose(3, "Arcsec to pixels: X = %5.3f\tY = %5.3f",
+	x_factor, y_factor);
+
+    /* Try to open the jitter file. */
+    FITS_read_key(infits, TSTRING, "JITR_CAL", jitr_cal, NULL, &status);
+    fits_open_file(&jitfits, jitr_cal, READONLY, &status);
+
+    /* If the jitter file is not found, try a lower-case filename. */
+    if (status != 0) {
+        status = 0;
+        jitr_cal[0] = (char) tolower(jitr_cal[0]);
+        fits_open_file(&jitfits, jitr_cal, READONLY, &status);
+    }
+
+    /* Read exposure start time from jitter file header */
+    FITS_read_key(jitfits, TDOUBLE, "EXPSTART", &jitr_expstart, NULL, &status);
+
+    /* Allocate space for correction arrays */
+    dx_tt = (float *) cf_calloc(nsec, sizeof(float));
+    dy_tt = (float *) cf_calloc(nsec, sizeof(float));
+
+    /* Read the jitter file. */
+    FITS_movabs_hdu(jitfits, 2, &hdutype, &status);
+    njitr=cf_read_col(jitfits, TLONG, "TIME", (void **) &time_jit);
+    njitr=cf_read_col(jitfits, TFLOAT, "DX", (void **) &dx_jit);
+    njitr=cf_read_col(jitfits, TFLOAT, "DY", (void **) &dy_jit);
+    njitr=cf_read_col(jitfits, TSHORT, "TRKFLG", (void **) &trkflg);
+    FITS_close_file(jitfits, &status);
+
+    /* Read minimum acceptable TRKFLG value from PARM_CAL file */
+    FITS_read_key(infits, TSTRING, "PARM_CAL", parmfile, NULL, &status);
+    FITS_open_file(&parmfits, cf_parm_file(parmfile), READONLY, &status);
+    FITS_read_key(parmfits, TSHORT, "TRKFLG", &trkflg_min, NULL, &status);
+    FITS_close_file(parmfits, &status);
+
+    /* Correct for difference in data and jitter EXPSTART times */
+    time_diff = cf_nlong((data_expstart - jitr_expstart) * 86400.);
+    for (j=0; j< njitr; j++) time_jit[j] -= time_diff;
+
+    /*
+     * Map times in the jitter file to times in the timeline table
+     * and calculate the jitter offsets.
+     */
+    for (j=k=0; k < nsec; k++) {
+	while ((float) time_jit[j+1] < ttime[k] && j+1 < njitr) j++;
+	if (trkflg[j] >= trkflg_min) {
+	    dx_tt[k] = x_factor * dx_jit[j];
+	    dy_tt[k] = y_factor * dy_jit[j];
+	}
+    }
+    /*
+     *  Map times in the timeline table to the times associated
+     *  with individual photons and apply the appropriate shifts.
+     *  Move only photons in the active aperture and for which the
+     *  timeline status jitter flag has not been set.
+     *  Record number of rejected events.
+     *  Note: active_ap[0] = lif, active_ap[1] = sic
+     */
+    nrej = 0;
+    for (j=k=0; j<nevents; j++) {
+	while (ttime[k+1] - FRAME_TOLERANCE < time[j] && k+1 < nsec) k++;
+	    if (channel[j] == active_ap[0] || channel[j] == active_ap[1]) {
+		if (status_flag[k] & TEMPORAL_JITR) nrej++;
+		else {
+		   x[j] += dx_tt[k];
+		   y[j] += dy_tt[k];
+		}
+	    }
+    }
+
+    /* Write to trailer file */
+    cf_verbose(2, "Rejected %ld photons from target aperture", nrej);
+
+    /* Deallocate storage space */
+    free(time_jit);
+    free(dx_jit);
+    free(dy_jit);
+    free(trkflg);
+    free(dx_tt);
+    free(dy_tt);
+   
+    cf_proc_update(infits, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished processing");
+
+    return (status);
+}
diff --git a/src/libcf/cf_scale_bkgd.c b/src/libcf/cf_scale_bkgd.c
new file mode 100644
index 0000000..556c0c7
--- /dev/null
+++ b/src/libcf/cf_scale_bkgd.c
@@ -0,0 +1,956 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences  
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis: cf_scale_bkgd(infits, nevents, x_in, y_in, w_in, channel,
+ *		timeflags, locflags, ngood, good_index, dtime, ntime, 
+ *		&binx, &biny, &nx_lif, &ny_lif,
+ *              &ymin_lif, img_lif, &nx_sic, &ny_sic, &ymin_sic, &img_sic)
+ *
+ * Arguments:  *fitsfile     infits      Input IDF file
+ *             long          nevents     Number of photon events recorded
+ *             float         x_in, y_in  Coordinates of each photon
+ *	       float	     w_in	 Weighting factor for each photon
+ *             unsigned char channel     Aperture ID for each photon
+ *             unsigned char timeflags   Photon status flags regarding time
+ *             unsigned char locflags    Photon status flags regarding location
+ *             long          ngood       Number of good photons
+ *             long          good_index  List of indices for the good photons
+ *             long          dtime       Length of the daytime exposure
+ *             long          ntime       Length of the night time exposure
+ *             int           binx, biny  Binning factors of the background
+ *                                         array along the X and Y axes
+ *             int         nx_lif, nx_sic X Size of background array
+ *             int         ny_lif, ny_sic Y Size of background array
+ *             int     ymin_lif, ymin_sic Y value corresponding to the
+ *                                          first row of the bkgd image
+ *             float   *img_lif, *img_sic 2D background image (binned)
+ *
+ * Description:
+ *  (a) Determine the total counts in a background sample region for data
+ *      taken during the night and during the day. Use the data in the
+ *      IDF event list, after screening out the geocoronal lines.
+ *  (b) Read estimated intrinsic count rates from the background characterization
+ *      file and estimate the intrinsic counts in the background region from
+ *      the exposure times and number of pixels in the region.
+ *  (c) Subtract the estimated intrinsic counts from the measured total to 
+ *      get an estimate of the scattered light contribution for both day
+ *      and night portions of the observation
+ *  (d) Use the scattered light counts to scale daytime and night background 
+ *      images obtained from the background calibration files
+ *  (e) Combine the two background images to obtain the final background model
+ *
+ * A previous assumption that the intrinsic background is constant was
+ * found to be incorrect. The program now iterates the assumed intrinsic 
+ * background count rate (assumed constant in day and night) and checks the
+ * calculated model against the observations by comparing the intensity 
+ * variations along the x direction. In this comparison, we mask out regions
+ * that are affected by geocoronal contamination.
+ *
+ * Caveats: The "intrinsic" component of the background is neither intrinsic
+ * nor constant in day and night.  It is better called the "spatially uniform"
+ * component and should be computed independently for day and night portions
+ * of the exposure.  wvd 01/24/2006
+ *
+ * History:     01/11/03   v1.1   rdr   Started work - adapted program
+ *                                              from cf_make_ttag_bkgd
+ *              03/01/03   v1.3   wvd   Correct use of pointer in FITS_read_key
+ *		03/11/03   v1.4   wvd   Update documentation regarding use of 
+ *					unsigned char.
+ *              03/28/03   v1.5   rdr   corrected error in freeing storage
+ *              03/31/03   v1.6   rdr   corrected error in assigning subarrays
+ *                                      for lif and sic apertures
+ *              05/08/03   v1.7   rdr   read limits to the background region
+ *                                      from the header of the IDF. Also 
+ *                                      changed print statements to cf_verbose.
+ *              05/20/03   v1.8   rdr   - Make a model using only exposure time
+ *                                      if no background sample regions have
+ *                                      been specified (generally for HIST data)
+ *                                      - Look into parm file to determine
+*                                       whether to generate a background model
+ *              05/22/03   v1.9    rdr  Correct problems occuring when exptime=0
+ *              06/04/03   v1.10   rdr  Change method for determining limits of 
+ *                                      output arrays
+ *              09/08/03   v1.12   wvd  Use cf_read_col in get_limits()
+ *              09/29/03   v1.13   wvd  Fix bug in population of 2-D bkgd
+ *					array; clean up i/o.
+ *              10/07/03   v1.14   wvd  Reject airglow photons using a
+ *					bit-wise comparison of locflags.
+ *              10/31/03   v1.15   wvd  Increase aperture pad from 10 to 15.
+ *					Change channel to unsigned char.
+ *              10/31/03   v1.16   wvd  Use cf_read_col in get_geocoronal_mask()
+ *              03/22/04   v1.17   wvd  Change get_limits so that sizes of
+ *					bkgd and probability arrays are equal.
+ *              04/08/04   v1.18   bjg  Replace NXMAX by nx
+ *                                      Remove unused variables
+ *                                      Change format in printf to match 
+ *                                      arg type.
+ *		04/27/04   v1.19   wvd	Replace RUN_MKBK with RUN_BKGD
+ *					throughout.
+ *		07/01/04   v1.20   wvd	Fix bug: nxb was undefined for
+ *					RUN_BKGD = NO.
+ *		03/08/05   v1.21   wvd	Convert to cf_scale_bkgd.
+ *					Treat data and models the same way.
+ *					Modify get_xvar_img.  Add
+ *					make_bad_pixel_mask and sum_good_pixels.
+ *		06/15/05   v1.22   wvd	BUG FIX: get_limits always read the
+ *					probability arrays for point-source 
+ *					targets from the WGTS_CAL file.  Now
+ *					it distinguishes between point-source
+ *					and extended targets.
+ *		01/20/06   v1.23   wvd	BUG FIX: Apply uniform X limits to
+ *					data and background models.
+ *					BUG FIX: Allow output bkgd images
+ *					to fall off the detector if target 
+ *					centroid requires it.
+ *		01/24/06   v1.24   wvd	BUG FIX: Test y coordinate of photon
+ *					before adding it to the data image.
+ *		02/01/06   v1.25   wvd	BUG FIX: Make npix a long in 
+ *					sum_good_pixels.  Correct error in
+ *					extraction of sub-arrays.
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include <math.h>
+#include "calfuse.h"
+
+
+/*********************************************************************
+ *
+ *    GET_XVAR_IMG
+ *
+ *   Subroutine to compute the intensity variation along the X direction
+ *   of a background image.  Pixels flagged as bad are excluded.
+ *     bkgimg = image from which to extract the data
+ *     maskimg = mask for data image (1 = good pixel)
+ *     nxb = size of bkgimg in x
+ *     nxsam = number of elements in the xvars array
+ *     xvars = array of x variations
+ *
+ ***********************************************************************/
+
+
+int
+get_xvar_img(float *bkgimg, float *maskimg, int nxb, int nxsam, float *xvars)
+{
+    int     nbin;
+    long    i, j;
+
+    nbin = nxb/nxsam ;
+    for (i = 0; i < NYMAX; i++) 
+	for (j = 0; j < nxb; j++)
+	    xvars[j/nbin] += bkgimg[i*nxb+j] * maskimg[i*nxb+j];
+
+    return 0 ;
+}
+
+/*********************************************************************
+ *
+ *       MAKE_MODEL
+ *
+ *  Subroutine to combine a day and night calibration image to generate the 
+ *    final background model:
+ *       npix = number of pixels in the full background image
+ *       nsam = number of pixels in the background regions of the detector
+ *       nxb = size of the x dimension of the background images
+ *       intcr = assumed intrinsic count rate
+ *       expnight, expday = exposure times during the night and day
+ *       data_sum_night, data_sum_day = sum of weights within the background
+ *             sample regions for night and day exposures
+ *       model_sum_night, model_sum_day = number of counts in the unscaled
+ *              night and day background calibration images
+ *		- background regions only
+ *       bkgimgn = image containing the night calibration image.
+ *       bkgimgd = image containing the daytime calibration image 
+ *       bkgimg = final background image 
+ *	 maskimg = mask defining good background regions
+ *
+ *****************************************************************************/
+
+int
+make_model(long npix, long nsam, int nxb, float intcr, float expnight,
+    float expday, double data_sum_night, double data_sum_day,
+    double model_sum_night, double model_sum_day,
+    float *bkgimgn, float *bkgimgd, float *bkgimg, float *maskimg)
+{
+    int   bin_size ;
+    long  i;
+    float int_counts;
+    float sfd, sfn, intnight, intday, scatnight, scatday ;
+
+    /* bin_size = binning factor of the background image */
+    bin_size = NXMAX / nxb ;
+
+    cf_verbose(3, "\n\tConstructing the background model\n") ;
+    cf_verbose(3, "total counts in the data: night= %.1f, day = %.1f",
+        data_sum_night, data_sum_day);
+    cf_verbose(3, "intrinsic count rate = %.2f x 10^-7 ",intcr ) ;
+    cf_verbose(3, "exptime night = %.1f, exptime day = %.1f ",
+        expnight, expday );
+
+    /* Sum the intrinsic background counts */
+    intnight = nsam * bin_size * intcr * expnight * 1.e-7 ;
+    intday = nsam * bin_size * intcr * expday * 1.e-7 ;
+    cf_verbose(3, "total intrinsic counts: night= %.1f , day= %.1f ",
+        intnight, intday) ;
+
+    /* Sum of scattered light in data (measured - intrinsic) */
+    scatnight = data_sum_night - intnight ;
+        if (scatnight <= 0.) scatnight = 0. ;
+    scatday = data_sum_day - intday ;
+        if (scatday <= 0.) scatday = 0. ;
+    cf_verbose(3, "total scattered light count: night = %.1f, day = %.1f",
+        scatnight, scatday);
+    cf_verbose(3, "total counts in unscaled background model: "
+        "night = %.2f, day = %.2f", model_sum_night, model_sum_day);
+
+    /* Calculate the scale factor for the night scattered light image */
+    sfn = 0. ;
+    if (model_sum_night > 0)  sfn = scatnight / model_sum_night ;
+
+    /* Calculate the scale factor for the day scattered light image */
+    sfd = 0. ;
+    if (model_sum_day > 0) sfd = scatday / model_sum_day ;
+    cf_verbose(3, "scale factors for background images: "
+        "night = %.1f, day = %.1f ", sfn, sfd) ;
+
+    /* Calculate the intrinsic counts per binned pixel */
+    int_counts = bin_size * intcr * (expnight + expday) * 1.e-7 ;
+    cf_verbose(3, "intrinsic counts per binned pixel = %.6f ", int_counts ) ;
+
+    /* Use the scattered light scaling factors and the tabulated intrinsic
+       count rate to model the final background image */
+
+    for (i = 0; i < npix; i++)
+        bkgimg[i] = (sfn * bkgimgn[i]) + (sfd * bkgimgd[i]) + int_counts;
+
+    return 0 ;
+}
+
+
+/*********************************************************************
+ *
+ *     MAKE_MODEL_EXPTIME  : 
+ *
+ *  Subroutine to combine a day and night calibration image based on
+ *    exposure times only to generate the final background model:
+ *      npix = total number of pixels in the image
+ *      nxb = length of the x axis in the background images
+ *     intcr = assumed intrinsic count rate
+ *     expnight, expday = exposure times during the night and day
+ *     bkging = image containing the night calibration image.
+ *     bkgimgd = image containing the daytime calibration image 
+ *     bkgimg = final background model    
+ *
+ *********************************************************************/
+ 
+
+int
+make_model_exptime(long npix, int nxb, float intcr, float expnight,
+    float expday, float *bkgimgn, float *bkgimgd, float *bkgimg)
+{
+
+    int i, bin_size ;
+    float intnight, intday ;
+
+    /* Compute the binning factor in x */
+    bin_size = NXMAX/nxb ;
+
+    /* Calculate the expected intrinsic counts in the background */ 
+    intnight = bin_size * intcr * expnight * 1.e-7 ;
+    intday = bin_size * intcr * expday * 1.e-7 ;
+
+    /* Combine the day and night images based on exposure times */
+    for (i=0 ; i<npix ; i++)
+    bkgimg[i] = intnight + intday + bkgimgn[i]*expnight + bkgimgd[i]*expday ;
+
+   return 0 ;
+}
+
+/*****************************************************************************
+ *
+ *    MAKE_BAD_PIXEL_MASK :
+ *
+ *  Produces a mask the same size as the background image. 
+ *  Good pixels are flagged with 1 and bad pixels with 0.  Bad pixels are
+ *  - all pixels that are NOT in the user-selected background regions;
+ *  - all pixels containing airglow lines (from AIRG_CAL); and
+ *  - all pixels lying outside of the active area of the detector.
+ *	bkgd_num = number of background regions
+ *	ylim - limits of background regions
+ *      npix = number of pixels in the background array
+ *      nxb = dimension of the x axis of the array
+ *      maskimg = array to contain the mask (must be initialized to zero)
+ *      nsam = number of good pixels in the mask
+ *
+ ****************************************************************************/
+
+int
+make_bad_pixel_mask (fitsfile *infits, int bkgd_num, short *ylim,
+	long npix, int nxb, float *maskimg, long *nsam)
+{
+
+    int nbin;
+    int xmin,xmax,ymin,ymax ;
+    long nrow, ndx, i, j, k, n_air, n_good;
+    short *gxmin, *gxmax, *gymin, *gymax ;
+
+    /* Compute the binning factor in x */
+    nbin = NXMAX/nxb;
+
+    /* Ignore regions near the detector edges. */
+    xmin =  2048 / nbin;
+    xmax = 14336 / nbin;
+
+    /* Flag all pixels in the user-defined background regions as good (1). */
+    for (i = 0; i < bkgd_num; i++)
+	for (j = ylim[2*i]; j <= ylim[2*i+1]; j++)
+	    for (k = xmin; k < xmax; k++) {
+		ndx = (long) (j*nxb+k) ;
+		maskimg[ndx] = 1.;
+	    }
+
+    /* Read the positions of the geocoronal lines. */  
+    nrow = cf_get_geocorona(infits, &gxmin, &gxmax, &gymin, &gymax);
+    cf_verbose(3, "Number of geocoronal lines = %ld", nrow) ;
+
+    /* Flag pixels affected by geocoronal lines as bad (0). */
+    n_air = 0;
+    for (i=0; i<nrow; i++) {
+	xmin = gxmin[i] / nbin ;
+	xmax = gxmax[i] / nbin ;
+	ymin = gymin[i] ;
+	ymax = gymax[i] ;
+	for (j=ymin; j<ymax; j++) 
+	    for (k=xmin; k<xmax; k++) {
+		ndx = j * nxb + k ;
+		if (maskimg[ndx] > 0) {
+		    maskimg[ndx] = 0. ;
+		    n_air++ ;
+		}
+	    }
+	}
+
+    free(gxmin);
+    free(gxmax);
+    free(gymin);
+    free(gymax);
+
+    cf_verbose(3, "Number of bkgd pixels affected by geocoronal lines = %ld",
+	n_air) ;
+
+    /* Count up and return the number of good pixels. */
+    n_good = 0;
+    for (i = 0; i < npix; i++) if(maskimg[i] > 0) n_good++;
+    cf_verbose(3, "Number of bkgd pixels flagged as good = %ld", n_good) ;
+
+    *nsam = n_good;
+    return 0 ;
+}
+
+
+/******************************************************************************
+ *
+ *             GET_LIMITS
+ *
+ *  Set limits of background subimage to match those of probability array.
+ *
+ *
+ ******************************************************************************/
+
+int get_limits(fitsfile *infits, int extended, int aperture,
+	int *ymin, int *ymax)
+{
+
+	char wgtsfile[FLEN_VALUE], ycentname[FLEN_KEYWORD];
+	int hdu, nywt, status=0;
+	float ycentv, wgt_cent;
+	fitsfile *wgtsfits;
+
+	cf_verbose(3, "Determining Y limits for aperture %d background array.",
+		aperture);
+
+	/* Read the measured centroid of the target spectrum. */
+	sprintf(ycentname,"YCENT%1d", aperture);
+	FITS_movabs_hdu(infits, 1, NULL, &status);
+	FITS_read_key(infits, TFLOAT, ycentname, &ycentv, NULL, &status);
+
+	/* Read the centroid and size of the probability array. */ 
+	FITS_read_key(infits, TSTRING, "WGTS_CAL", wgtsfile, NULL, &status);
+	FITS_open_file(&wgtsfits, cf_cal_file(wgtsfile), READONLY, &status);
+	hdu = extended * 8 + aperture + 1;
+	cf_verbose(3, "WGTS_CAL: extended = %d, aperture = %d, hdu = %d",
+		extended, aperture, hdu);
+	FITS_movabs_hdu(wgtsfits, hdu, NULL, &status);
+	FITS_read_key(wgtsfits, TINT, "NAXIS2", &nywt, NULL, &status);
+	FITS_read_key(wgtsfits, TFLOAT, "WGT_CENT", &wgt_cent, NULL, &status);
+	FITS_close_file(wgtsfits, &status);
+
+        cf_verbose(3, "Spectrum centroid=%6.2f, weights centroid=%5.2f, "
+	   "weights ny=%4d", ycentv, wgt_cent, nywt) ;
+
+	/* Note that we allow these values to exceed the limits of the 
+	 * detector.  This is required if the bkgd arrays are to cover
+	 * the same area as the 2-D probability and data arrays. */
+
+	*ymin = cf_nint (ycentv - wgt_cent);
+        *ymax = *ymin + nywt - 1;
+
+	return status ; 
+}
+
+
+/*********************************************************************
+ *
+ *    SUM_GOOD_PIXELS
+ *
+ *    Subroutine multiplies image and mask arrays, then sums the result.
+ *     image = image from which to extract the data
+ *     mask = mask for data image (1 = good pixels)
+ *     npix = size of image and mask arrays
+ *
+ ***********************************************************************/
+
+
+int
+sum_good_pixels(float *image, float *mask, long npix, double *image_sum)
+{
+    
+    long    i;
+
+    *image_sum = 0;
+
+    for (i = 0; i < npix; i++) 
+            *image_sum += image[i] * mask[i];
+
+    return 0 ;
+}
+
+
+/******************************************************************************
+ *
+ *             MAIN PROGRAM BEGINS HERE
+ *
+ ******************************************************************************/
+
+
+int cf_scale_bkgd(fitsfile *infits, long nevents, float *x_in, float *y_in,
+    float *w_in, unsigned char *channel, unsigned char *timeflags,
+    unsigned char *locflags, long ngood, long *good_index, long dtime,
+    long ntime, int *binx, int *biny, int *nx_lif, int *ny_lif,
+    int *ymin_lif, float **img_lif, int *nx_sic, int *ny_sic, int *ymin_sic,
+    float **img_sic)
+{
+
+   char CF_PRGM_ID[] = "cf_scale_bkgd";
+   char CF_VER_NUM[] = "1.25";
+
+    fitsfile  *bkgdfits, *scrnfits, *bchrfits, *parmfits ;
+    char     buffer[FLEN_CARD], bkgdfile[FLEN_CARD], scrnfile[FLEN_CARD];
+    char     bchrfile[FLEN_CARD], keyname[FLEN_CARD], parmfile[FLEN_CARD] ;
+    char     run_bkgd[FLEN_VALUE]; 
+    char     comment[FLEN_CARD], datestr[FLEN_CARD];
+    int      nx, nxb, ny, status, hdutype, frow, felem, niter;
+    int      src_ap[2], nullval, anynull, bkgd_num;
+    int      ymin, ymax, phalow, nbinx, nxsam, bkgdtype ;
+    int      bin_size, extended, keyval, timeref;
+    double   data_sum_day, data_sum_night, data_sum;
+    double   model_sum_night, model_sum_day, model_sum ;
+    float    *xvarg, *bkgarr, *xvars0, *xvarm0 ;
+    float    *bkgimg, *bkgimgd, *bkgimgn, *xvars, *xvarm;
+    float    floatnull, exptime, expnight, expday, xvars_ave ;
+    float    intcrarray[9], intcr, scattot, rms, rms0, dcr ;
+    float    intcnt, scat_int_ratio, zero, mf, numtot, xvars_tot, xvarm_tot ;
+    float    *dataimg, *maskimg;
+    short    *ylim ;
+    long     fpixel, npix, i, j, k, nsam;
+    long     nbgood, npts, ndx, ndx1, ndx2, bkgd_ndx;
+
+    /* Initialize error checking */
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Started execution.");
+
+    /* Initialize CFITSIO variables */
+    anynull = 0 ;
+    hdutype = 0 ;
+    frow = 1 ;
+    felem = 1 ;
+    floatnull = 0. ;
+    fpixel = 1 ;
+    status = 0 ;
+
+    /* Initialize other variables */
+    data_sum_day=0.;
+    data_sum_night=0.;
+    zero = 0.;
+
+    /* Open parameter file and check whether user wants a background model. */
+    FITS_movabs_hdu(infits, 1, &hdutype, &status) ;
+    FITS_read_key(infits, TSTRING, "PARM_CAL", parmfile, NULL, &status) ;
+    cf_verbose(3, "parameter file is %s ", parmfile) ;
+    FITS_open_file(&parmfits,cf_parm_file(parmfile), READONLY, &status) ;
+    FITS_read_key(parmfits, TSTRING, "RUN_BKGD", run_bkgd, NULL, &status) ;
+    FITS_close_file(parmfits, &status) ;
+    cf_verbose(3, "RUN_BKGD = %s", run_bkgd) ;
+
+    /* If the RUN_BKGD = NO, then fill background array with zeros. */ 
+    if (!strncmp(run_bkgd, "N", 1) || !strncmp(run_bkgd, "n", 1)) {
+        cf_verbose(1, "RUN_BKGD = NO.  No background subtraction.") ;
+	FITS_write_comment(infits, " ", &status);
+	FITS_write_comment(infits, "RUN_BKGD = NO.  No background subtraction.",
+	     &status);
+	fits_get_system_time(datestr, &timeref, &status);
+        sprintf(comment, "CalFUSE v%s   %.10s", CALFUSE_VERSION, datestr);
+        FITS_write_comment(infits, comment, &status);
+	FITS_write_comment(infits, " ", &status);
+
+        bin_size = 1 ;
+        nx=nxb=NXMAX ;
+        ny=NYMAX ;
+        npix=nx * ny ;
+        bkgimg = (float *) cf_calloc(npix, sizeof(float)) ;
+        goto fin ;
+    }
+
+/***********************************************************************
+ *
+ *      Set up the parameters for the analysis 
+ *
+ ***********************************************************************/
+
+    /* Set day and night exposure times */
+    expday = (float) dtime ;
+    expnight = (float) ntime ;
+    exptime = expday + expnight ;
+
+    /* Get name of background characterization file */
+    FITS_read_key(infits, TSTRING, "BCHR_CAL",bchrfile, NULL, &status) ;
+    cf_verbose(3, "BCHR parameter file is %s ",bchrfile) ;
+
+    /* Get name of background calibration file */
+    FITS_read_key(infits, TSTRING, "BKGD_CAL", bkgdfile, buffer, &status);
+    cf_verbose(3,"Background calibration file = %s ",bkgdfile ) ;
+
+    /* Get name of screening file */
+    FITS_read_key(infits, TSTRING, "SCRN_CAL",scrnfile, NULL, &status) ;
+    cf_verbose(4, "screening file is %s ",scrnfile) ; 
+
+    /* Read pha screening limit from the input file header */
+    FITS_read_key(infits,TINT,"PHALOW",&phalow, NULL, &status) ; 
+    if (phalow > 8) phalow=8 ;
+    cf_verbose(2, "pha screening limit = %d", phalow) ;
+
+    /* Determine the type of background model to make by checking the
+       BKGDTYPE flag in the screening file. If BKGDTYPE > 0, do a full
+       model. If BKGDTYPE < 0, calculate a model based on exposure time. */
+    FITS_open_file(&scrnfits,cf_parm_file(scrnfile), READONLY, &status) ;
+    FITS_read_key(scrnfits, TINT, "BKGDTYPE",&bkgdtype, NULL, &status) ;
+    FITS_close_file(scrnfits, &status) ;
+
+    /* Read the intrinsic count rate from the BCHR file */
+    FITS_open_file(&bchrfits,cf_parm_file(bchrfile), READONLY, &status) ; 
+    FITS_movabs_hdu(bchrfits, 3, &hdutype, &status) ;
+    FITS_read_img(bchrfits, TFLOAT, fpixel, 9, &nullval, intcrarray,
+      &anynull, &status) ;
+    FITS_close_file(bchrfits, &status) ;
+    intcr=intcrarray[phalow] ;
+    cf_verbose(2,"Initial guess for the intrinsic count rate = "
+	"%.1f x 10^-7 c/s/pixel ", intcr) ;
+
+    /* Read the limits of the background sample regions from the header
+	of the input file */
+    FITS_read_key(infits, TINT, "BKGD_NUM", &bkgd_num, NULL, &status) ;
+    cf_verbose(3, "Number of background sample regions = %d ", bkgd_num) ;
+
+    ylim = (short *) cf_calloc(bkgd_num*2, sizeof(short) ) ;
+    for (i=0; i<bkgd_num; i++) {
+	sprintf(keyname,"BKG_MIN%ld",i) ;
+	FITS_read_key(infits, TINT, keyname,&keyval, NULL, &status) ; 
+	ylim[2*i] = keyval ;
+	sprintf(keyname,"BKG_MAX%ld",i) ;
+	FITS_read_key(infits, TINT, keyname,&keyval, NULL, &status) ; 
+	ylim[2*i+1] = keyval ;
+    }
+    cf_verbose(3, "Limits of background regions") ;
+    for (i=0; i<bkgd_num; i++) cf_verbose(3,
+	"region %d = %d to %d ", i, ylim[2*i], ylim[2*i+1] ) ;
+
+    /* If no background sample regions have been specified (as is usual for
+       HIST data), then generate a model based only on exposure time */
+    if (bkgd_num == 0) {
+	bkgdtype = -1 ;
+	cf_verbose(1, "No background sample regions specified "
+	    "- probably HIST") ;
+    }
+
+
+/*************************************************************************
+ *    
+ *   Read in the background calibration information
+ *
+ *************************************************************************/
+ 
+    /* Open background image file and go to the night image hdu */
+    FITS_open_file(&bkgdfits, cf_cal_file(bkgdfile), READONLY, &status);
+    FITS_movabs_hdu(bkgdfits, 2, &hdutype, &status);
+    FITS_read_key(bkgdfits, TINT, "NAXIS1", &nx, buffer, &status);
+    FITS_read_key(bkgdfits, TINT, "NAXIS2", &ny, buffer, &status);
+    cf_verbose(3, "Reading background calibration file:",
+	"naxis1=%d,  naxis2 = %d ",nx,ny) ;
+       
+    /* Background image files are binned in X, but not Y.
+	Determine the degree of compression. */
+    bin_size= NXMAX/nx ; 
+    cf_verbose(3, "Background images are binned by %d pixels", bin_size) ;
+            
+    /* Allocate space to hold the background, data, and mask images */
+    npix = nx * ny ;
+    nxb = nx ;
+    bkgimgn = (float *) cf_calloc(npix, sizeof(float)) ;
+    bkgimgd = (float *) cf_calloc(npix, sizeof(float)) ;
+    bkgimg  = (float *) cf_calloc(npix, sizeof(float)) ;
+    dataimg = (float *) cf_calloc(npix, sizeof(float)) ;
+    maskimg = (float *) cf_calloc(npix, sizeof(float)) ;
+    
+    /* Read the night and day scattered-light images */
+    FITS_read_img(bkgdfits, TFLOAT, fpixel, npix, &nullval, bkgimgn,
+	&anynull, &status) ;
+    FITS_movabs_hdu(bkgdfits, 3, &hdutype, &status);
+    FITS_read_img(bkgdfits, TFLOAT, fpixel, npix, &nullval, bkgimgd,
+	&anynull, &status) ;
+    FITS_close_file(bkgdfits, &status) ;
+
+    /* Rescale the background images if they have been compressed. */
+    if (bin_size > 1) for (i=0; i<npix; i++) {
+	bkgimgn[i] *= bin_size ;
+	bkgimgd[i] *= bin_size ;
+    }
+
+    /* Generate a mask of the same dimensions as the background image.
+	It is 1 in the user-defined background regions, but 0 around
+	airglow lines and near the edges of the detector. */
+    make_bad_pixel_mask (infits, bkgd_num, ylim, npix, nxb, maskimg, &nsam);
+
+
+/****************************************************************************
+ *
+ *      Read the photon list.
+ *	Store in an array the same size as the the background image. 
+ *	Populate only regions flagged as good in the background mask.
+ *	Omit photons flagged as airglow.
+ *	This scheme rejects non-airglow photons that drift into airglow
+ *	regions due to mirror or spacecraft motion.  We thus under-estimate
+ *	the background, but assume that the resulting error is small.
+ *
+ ****************************************************************************/
+
+    /* If the background model is to be calculated only by exposure time,
+       then skip the IDF file analysis */
+    if (bkgdtype < 0) {
+      cf_verbose(3, "Skipping the analysis of the IDF file") ;
+    }
+    else {	/* Analysis of the data begins here. */
+      cf_verbose(3, "Beginning the analysis of the IDF file") ;
+
+    nbgood=0;
+    for (i=0; i<ngood; i++) {
+	ndx=good_index[i] ;
+	if (locflags[ndx] & LOCATION_AIR) continue;
+	if ((j = cf_nint(y_in[ndx])) < 0 || j >= NYMAX) continue;
+	bkgd_ndx = j*nxb + cf_nint(x_in[ndx])/bin_size;
+	if (maskimg[bkgd_ndx] > 0) {
+		dataimg[bkgd_ndx] += w_in[ndx];
+      		if (timeflags[ndx] & TEMPORAL_DAY) data_sum_day += w_in[ndx] ;
+       		else data_sum_night += w_in[ndx]; 
+	  	nbgood++ ;
+	}
+    }
+
+    cf_verbose(3, "Number of photons events in the background region = %ld",
+	nbgood); 
+    cf_verbose(3, "Sum of daytime weights  = %.1lf ", data_sum_day) ;
+    cf_verbose(3, "Sum of nighttime weights  = %.1lf ", data_sum_night) ;
+
+    /* If the background scattered light contribution is too large, the
+	background may be contaminated, perhaps by a source in one of the
+	other apertures.  This is common in crowded fields or with nebulocity.
+	In this case, we calculate the background model based on the 
+	exposure times, as done for the histogram data */
+
+    /* Check the level of the scattered-light background */
+    intcnt = intcr * nsam * bin_size * exptime * 1.e-7 ;
+    scattot = data_sum_day + data_sum_night - intcnt ;
+    scat_int_ratio = 0. ;
+    if (intcnt > 0) scat_int_ratio = scattot / intcnt ;
+    cf_verbose(3, "int cnt = %.1f, scat cnt = %.1f , scat/int = %f ",
+	intcnt, scattot, scat_int_ratio) ;
+
+    if (scat_int_ratio > 10) {
+	cf_verbose(1, "The scattered light background is too large.");
+	bkgdtype = -1;
+    }
+    else {
+	cf_verbose(2,
+	    "Scattered light appears reasonable. Proceeding with analysis.") ;
+    }
+
+    }	/* Analysis of the data ends here. */
+
+    /* If the background model is to be calculated using only the exposure
+	time, then do it now. */
+    if (bkgdtype < 0) {
+        cf_verbose(1, "Constructing background based only on exposure time.") ;
+	make_model_exptime( npix, nxb, intcr, expnight, expday,
+	    bkgimgn, bkgimgd, bkgimg) ;
+        goto fin ; 
+    }
+
+/****************************************************************************
+ *
+ *      In this section, we attempt to determine the intrinsic count rate.
+ *      The scattered light shows little structure in the Y dimension, so
+ *	we project all of the arrays onto the X axis.  Only good pixels
+ *	in the user-specified background regions are included in the sum.
+ *
+ ****************************************************************************/
+
+    /* Make a scattered light reference image assuming an intrinsic count
+       rate of zero. */
+    make_model_exptime(npix, nxb, zero, expnight, expday,
+	bkgimgn, bkgimgd, bkgimg) ;
+
+    /* We bin the data by another factor of 8 in X      */
+    /*   nbinx = number of detector pixels in one bin	*/
+    /*   nxsam = number of samples in the array		*/
+    nbinx=128 ;
+    nxsam = NXMAX/nbinx ;
+    cf_verbose(3, "X variation array information: "
+                  "nbinx = %d, nxsam= %d ", nbinx, nxsam) ; 
+
+    xvars  = (float *) cf_calloc(nxsam,sizeof(float)) ;
+    xvarm  = (float *) cf_calloc(nxsam,sizeof(float)) ;
+    xvars0 = (float *) cf_calloc(nxsam,sizeof(float)) ;
+    xvarm0 = (float *) cf_calloc(nxsam,sizeof(float)) ;
+    xvarg  = (float *) cf_calloc(nxsam,sizeof(float)) ;
+
+    /* Project each image onto the X axis */
+    get_xvar_img(bkgimg,  maskimg, nxb, nxsam, xvarm0) ;
+    get_xvar_img(dataimg, maskimg, nxb, nxsam, xvars0) ;
+    get_xvar_img(maskimg, maskimg, nxb, nxsam, xvarg) ;
+
+    /* Calculate the average counts per "good" bin in the data array. */
+    xvars_ave = 0;
+    for (i = j = 0; i < nxsam; i++)
+	if (xvarg[i] > 0) {
+	    xvars_ave += xvars0[i];
+	    j++;
+	}
+    xvars_ave /= j;
+    cf_verbose (3, "xvars_ave = %.1f (should be > 100)", xvars_ave);
+
+    /* If the average number of counts in the xvars0 array (which holds 
+    the observed intensity variation along the x direction) is small,
+    then we can't determine an intrinsic count rate from the data and
+    we use the tabulated rate.  If the count is large enough, then we
+    can do a more detailed fit of the model to the observations. */
+
+    if (xvars_ave > 100) {	/* Begin fit to intrinsic background */
+
+    cf_verbose(1, "Calculating a full background model.") ;
+    cf_verbose(3, "\n\tInterpolating to derive intrinsic count rate\n") ;
+
+    /* Sum the counts in the data and model arrays. */
+    sum_good_pixels(dataimg, maskimg, npix, &data_sum);
+    sum_good_pixels(bkgimg, maskimg, npix, &model_sum);
+
+    cf_verbose(3, "Total counts in initial scattered-light model = %7.0lf",
+	model_sum);
+    cf_verbose(3, "Intrinsic counts summed over good regions =     %7.0f",
+	(intcnt = intcr * nsam * bin_size * exptime * 1.e-7));
+    cf_verbose(3, "Sum of above                                  = %7.0lf",
+	model_sum + intcnt);
+    cf_verbose(3, "Total counts in good regions of data array =    %7.0lf",
+	data_sum);
+
+    /* Sum the counts in the data and model x variation arrays */
+    xvarm_tot = 0.;
+    xvars_tot = 0.;
+    for (i = j = 0; i < nxsam; i++) if (xvarg[i] > 0) {
+	xvarm_tot += xvarm0[i];
+	xvars_tot += xvars0[i];
+    }
+    cf_verbose(3, "Total counts in scattered-light xvar array =    %7.0f",
+	xvarm_tot);
+    cf_verbose(3, "Total counts in data x variation array =        %7.0f",
+	xvars_tot);
+
+    /* Convert the x variation arrays from total counts to units of
+	1.e-7 c/s/pix, the units of the intrinsic count rate. */
+    mf = bin_size * exptime * 1.e-7 ;
+    for (i=0 ; i<nxsam ; i++) if (xvarg[i] > 0) {
+	xvars0[i] /= xvarg[i] * mf ;
+	xvarm0[i] /= xvarg[i] * mf ;
+    }
+
+    /* Sum the counts in the rescaled xvar arrays */
+    xvarm_tot = 0.;
+    xvars_tot = 0.;
+    for (i = j = 0; i < nxsam; i++) if (xvarg[i] > 0) {
+	xvars_tot += xvars0[i];
+	xvarm_tot += xvarm0[i];
+	j++;
+    }
+    cf_verbose(3, "Mean xvar count rates in units of 10^-7 c/s/pixel:");
+    cf_verbose(3, "     Initial model = %.1f", xvarm_tot/j);
+    cf_verbose(3, "  Intrinsic counts = %.1f", intcr);
+    cf_verbose(3, "        Data array = %.1f", xvars_tot/j);
+
+    /* Determine the value of the intrinsic background by comparing the X
+	variations of the data (after removing a guess for the intrinsic
+	background) with the model scattered light variations, making sure
+	that the final average count rate is the same for both.  Iterate
+	until the intrinsic background changes by less than 0.1 units. */
+
+    dcr = 1. ;
+    niter = 0 ;
+    rms0 = 1.e10 ;
+    while ( fabs(dcr) > 0.1) { 
+
+        /* Subtract intrinsic counts from the data array and sum it. */
+	xvars_tot = 0. ;
+	for (i=0; i<nxsam; i++) if (xvarg[i] > 0) {
+	    xvars[i] = xvars0[i] - intcr ;
+	    xvars_tot += xvars[i] ;
+	}
+
+    	/* Scale the model array to match the data.  Sum it. */
+	numtot = 0. ;
+	for (i=0 ; i<nxsam ; i++) if (xvarg[i] > 0) {
+	    xvarm[i] = xvarm0[i] * (xvars_tot / xvarm_tot) ;
+	    numtot += xvarm[i] ;
+	}
+        
+	/* Sum the absolute difference between the data and model arrays. */
+	rms = 0. ;
+	for (i=0 ; i<nxsam ; i++) if (xvarg[i] > 0)  
+	    rms += (fabs(xvars[i]-xvarm[i])) ; 
+	cf_verbose(3, "intr cr= %5.2f, data-model = %6.2f, "
+	    "dat cnts = %5.0f, mod cnts=%5.0f", intcr,rms,xvars_tot,numtot) ;
+
+	niter++ ;
+	if (niter > 20) break ;
+
+	/* if the current rsm value is greater than the preceeding one,
+	   reverse direction and reduce the step size by 50% */
+	if ( rms > rms0 )  dcr = -0.5*dcr ;
+	    intcr += dcr ;
+ 
+	/* initialize the next iteration */
+	rms0 = rms ;
+    }
+    }		/* End of fit to intrinsic background */
+
+    else { 
+    cf_verbose(1, "Background count too small for a detailed fit.");
+    cf_verbose(1, "Assuming an intrinsic count rate of %.1f cts/s", intcr ) ;
+    }
+
+    /* Sum the good pixels in the unscaled day and night background images. */
+    sum_good_pixels(bkgimgn, maskimg, npix, &model_sum_night);
+    sum_good_pixels(bkgimgd, maskimg, npix, &model_sum_day);
+
+    /* Make the final background model */
+    make_model(npix, nsam, nxb, intcr, expnight, expday,
+	data_sum_night, data_sum_day, model_sum_night, model_sum_day, 
+	bkgimgn, bkgimgd, bkgimg, maskimg) ;
+
+    /* Sum the counts in the final background image. */
+    sum_good_pixels(bkgimg, maskimg, npix, &model_sum);
+
+    cf_verbose(3, "Total counts in final background model = %.0lf", model_sum);
+    cf_verbose(3, "                       measured counts = %.0lf",
+	data_sum_day+data_sum_night);
+
+    free(bkgimgn) ;
+    free(bkgimgd) ;
+    free(dataimg) ;
+    free(maskimg) ;
+    free(xvars) ;
+    free(xvars0) ;
+    free(xvarm) ;
+    free(xvarm0) ;
+    free(xvarg) ;
+
+    fin:
+
+  /**************************************************************************
+   *
+   *     Extract the subarrays covering the active LiF and SiC apertures 
+   *
+   ***************************************************************************/
+
+    extended = cf_source_aper(infits, src_ap) ;
+    cf_verbose(3, "\n\tSelecting subarrays\n") ;
+    cf_verbose(3, "source apertures: lif=%d,  sic=%d ",src_ap[0], src_ap[1]) ; 
+
+    /* Populate some output values */
+    *binx=bin_size ;
+    *biny=1 ;
+
+    for (k=0; k<2 ; k++) {	/* Loop over LiF and SiC channels */
+
+    /* Read the y limits for the output array */
+    get_limits(infits, extended, src_ap[k], &ymin, &ymax) ;
+  
+    /* Set up array to contain the image */ 
+    npts = nxb * (ymax-ymin+1) ;
+    bkgarr = (float *) cf_calloc(npts, sizeof(float)) ;
+				   
+    /* Fill the array */
+    ndx1 = -1 ;
+    model_sum = 0 ;
+    for (i=ymin; i<=ymax ; i++) {
+	if (i < 0 || i >= ny)
+	    ndx1 += nxb ;
+	else {
+	    for (j=0; j<nxb; j++) {
+	        ndx2 = i*nxb + j ;
+	        if (ndx2 >= npix) break ;
+	        ndx1++;
+	        if (ndx1 >= npts) break ;
+	        bkgarr[ndx1]=bkgimg[ndx2] ;
+		model_sum += bkgarr[ndx1] ;
+	    }
+	}
+    }
+
+    /* Populate the output arrays and values */
+    if (k == 0) {
+	*nx_lif = nxb ;
+	*ny_lif = (ymax - ymin + 1) ;
+	*ymin_lif = ymin ;
+	*img_lif = bkgarr ;
+    }
+    else {
+	*nx_sic = nxb ;
+	*ny_sic = (ymax - ymin + 1) ;
+	*ymin_sic = ymin ;
+	*img_sic = bkgarr ;
+    }
+
+    cf_verbose(2, "for aperture %d, nx=%d, ny=%d, ymin=%d, model_sum=%.0f",
+	src_ap[k], nxb, (ymax-ymin+1), ymin, model_sum) ; 
+
+    }	/* End loop over LiF and SiC channels */
+
+    /* release memory for the background image */
+    free(bkgimg) ;
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished execution.");
+    return 0;
+}
diff --git a/src/libcf/cf_screen_airglow.c b/src/libcf/cf_screen_airglow.c
new file mode 100644
index 0000000..5a7b2b3
--- /dev/null
+++ b/src/libcf/cf_screen_airglow.c
@@ -0,0 +1,70 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_screen_airglow (fitsfile *header, long nevents,
+ *			      float *x, float *y, unsigned char *location)
+ *
+ * Description: Flag photon events in airglow regions.
+ *
+ * Arguments:   fitsfile  *header	Input FITS file pointer
+ *              long      nevents	Number of photon events
+ *              float     *x		X coordinate array
+ *              float     *y		Y coordinate array
+ *              unsigned char *location Photon location flag array
+ *
+ * Calls:	cf_get_geocorona
+ *
+ * Returns:	0 on success
+ *
+ * History:	03/10/05   1.1   wvd    Initial coding
+ *
+ ****************************************************************************/
+
+#include <stdlib.h>
+#include "calfuse.h"
+
+int
+cf_screen_airglow (fitsfile *header, long nevents, float *x, float *y,
+	unsigned char *location)
+{
+    char CF_PRGM_ID[] = "cf_screen_airglow";
+    char CF_VER_NUM[] = "1.1";
+
+    int   errflg=0, ngeo;
+    long  i, j;
+    short *gxmin, *gxmax, *gymin, *gymax;
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+    if ((errflg = cf_proc_check(header, CF_PRGM_ID))) return errflg;
+
+    /*
+     *  Read limits of airglow regions from AIRG_CAL file.
+     */
+    ngeo = cf_get_geocorona(header, &gxmin, &gxmax, &gymin, &gymax);
+
+    /*
+     *  Set the airglow bit of photons in the airglow regions.
+     */
+    for (i = 0; i < nevents; i++) {
+	for (j=0; j<ngeo; j++) {
+            if (x[i] > gxmin[j] && x[i] < gxmax[j] &&
+		y[i] > gymin[j] && y[i] < gymax[j] ) {
+		location[i] = location[i] | LOCATION_AIR;
+		break;
+	    }
+        }
+    }
+
+    free(gxmin);
+    free(gxmax);
+    free(gymin);
+    free(gymax);
+
+    cf_proc_update(header, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return 0;
+}
diff --git a/src/libcf/cf_screen_bad_pixels.c b/src/libcf/cf_screen_bad_pixels.c
new file mode 100644
index 0000000..99884a5
--- /dev/null
+++ b/src/libcf/cf_screen_bad_pixels.c
@@ -0,0 +1,122 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_screen_bad_pixels (fitsfile *header, long nevents,
+ *			      float *x, float *y, unsigned char *location)
+ *
+ * Description: Flag photon events in bad-pixel regions.
+ *
+ * Arguments:   fitsfile  *header	Input FITS file pointer
+ *              long      nevents	Number of photon events
+ *              float     *x		X coordinate array
+ *              float     *y		Y coordinate array
+ *              unsigned char *location Photon location flag array
+ *
+ * Calls:	cf_get_potholes
+ *
+ * Returns:	0 on success
+ *
+ * History:	11/22/05   1.1   wvd    Initial coding
+ *
+ ****************************************************************************/
+
+#include <stdlib.h>
+#include "calfuse.h"
+
+/***********************************************************************
+ *
+ * Procedure to read pothole locations from the QUAL_CAL file
+ *
+ ***********************************************************************/
+
+int
+cf_get_potholes(fitsfile *header, float **xbad, float **ybad,
+        float **rxbad, float **rybad)
+{
+    char qualfile[FLEN_VALUE];
+    int nbad, status=0;
+    fitsfile *qualfits;
+
+    cf_verbose(3, "Entering cf_get_potholes.");
+
+    /*
+     *  Read limits of bad-pixel regions from the first extension 
+     *  of the QUAL_CAL file.
+     */
+    FITS_movabs_hdu(header, 1, NULL, &status);
+    FITS_read_key(header, TSTRING, "QUAL_CAL", qualfile, NULL, &status);
+    cf_verbose(3, "QUAL_CAL = %s", qualfile);
+
+    FITS_open_file(&qualfits, cf_cal_file(qualfile), READONLY, &status);
+    FITS_movabs_hdu(qualfits, 2, NULL, &status);
+    nbad = cf_read_col(qualfits, TFLOAT, "X",  (void **) xbad);
+    nbad = cf_read_col(qualfits, TFLOAT, "Y",  (void **) ybad);
+    nbad = cf_read_col(qualfits, TFLOAT, "RX", (void **) rxbad);
+    nbad = cf_read_col(qualfits, TFLOAT, "RY", (void **) rybad);
+    FITS_close_file(qualfits, &status);
+
+    cf_verbose(3, "Exiting cf_get_potholes.");
+    return nbad;
+}
+
+
+int
+cf_screen_bad_pixels (fitsfile *header, long nevents, float *x, float *y,
+	unsigned char *location)
+{
+    char CF_PRGM_ID[] = "cf_screen_bad_pixels";
+    char CF_VER_NUM[] = "1.1";
+
+    int   errflg=0, nbad;
+    long  counter=0, i, j;
+    float *xbad, *ybad, *rxbad, *rybad, *rx2, *ry2;
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+    if ((errflg = cf_proc_check(header, CF_PRGM_ID))) return errflg;
+
+    /*
+     *  Read limits of bad-pixel regions from QUAL_CAL file.
+     */
+    nbad = cf_get_potholes(header, &xbad, &ybad, &rxbad, &rybad);
+    cf_verbose(2, "For first pothole: x = %.0f, y = %.0f, rx = %.0f, ry = %.0f",
+	xbad[0], ybad[0], rxbad[0], rybad[0]);
+
+    /*
+     *  Square the semi-major axes.
+     */
+    for (j = 0; j < nbad; j++) {
+	rxbad[j] *= rxbad[j];
+	rybad[j] *= rybad[j];
+    }
+    rx2 = rxbad;
+    ry2 = rybad;
+    cf_verbose(2, "For first pothole: rx2 = %.0f, ry2 = %.0f", rx2[0], ry2[0]);
+
+    /*
+     *  Flag photons in the bad-pixel regions.
+     */
+    for (i = 0; i < nevents; i++) {
+	for (j = 0; j < nbad; j++) {
+            if ((x[i] - xbad[j]) * (x[i] - xbad[j]) / rx2[j] +
+		(y[i] - ybad[j]) * (y[i] - ybad[j]) / ry2[j] < 1.0) {
+		location[i] = location[i] | LOCATION_BADPX;
+		counter++;
+		break;
+	    }
+        }
+    }
+    cf_verbose(2, "Flagged %d pixels as bad", counter);
+
+    free(xbad);
+    free(ybad);
+    free(rxbad);
+    free(rybad);
+
+    cf_proc_update(header, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return 0;
+}
diff --git a/src/libcf/cf_screen_burst.c b/src/libcf/cf_screen_burst.c
new file mode 100644
index 0000000..f80374e
--- /dev/null
+++ b/src/libcf/cf_screen_burst.c
@@ -0,0 +1,758 @@
+/****************************************************************************
+ *              Johns Hopkins University
+ *              Center for Astrophysical Sciences
+ *              FUSE
+ ****************************************************************************
+ *
+ * Synopsis:    cf_screen_burst(infits, nevents, ptime, x, y, locflags,
+ *                              gti, nsec, ttime, sflag, aic_rate, bkgd) 
+ *
+ * Description: Determines the times for bursts and sets the burst
+ *              flag in the timeline status array so that the busts
+ *              can be removed later.
+ *
+ * Arguments:   fitsfile  infile        Pointer to Intermediate Data File 
+ *              long      nevents       Number of photons
+ *              float     ptime         Time of event
+ *              float     *x, *y        X and Y positions of the photon
+ *              byte      locflags       flags on photon location 
+ *                                        (LOC_FLGS column in IDF)
+ *              GTI       gti           Structure with Good Time Intervals
+ *              long      nsec          Length of timeline array
+ *              float     ttime         Timeline array
+ *              byte      sflag         Status flags in timeline table
+ *		float	  aic_rate	AIC count rate
+ *              short     bkgd          Count rate for the background 
+ *                                      sample region 
+ *
+ * Algorithm used:
+ *
+ *     1. Generate an array (flgarr) with 1 second intervals that 
+ *        contains flags indicating whether that time interval is good 
+ *        or not. All elements of this array are originally set to negative
+ *        numbers, indicating bad times.
+ *     2. Read in the good time intervals from the initial screening
+ *        analysis and set all good time elements in flgarr to positive 
+ *        values
+ *     3. Determine the median count per binned element in the entire time 
+ *        sequence (ignoring times with no data) and set all elements with
+ *        a count > 5 times this median value to negative values (indicating
+ *        a burst at that time).
+ *     4. Do a median filter of the modified time sequence (ignoring the neg
+ *        numbers) and identify all times where the count per bin is greater
+ *        than a specified value or is more than a specified number of 
+ *        standard deviations from the median. These points are flagged with
+ *        negative numbers to indicate bursts. The screening parameters used
+ *        are specified in the screening parameter file.
+ *     5. Iterate time-sequence analysis until no more points are removed.
+ *     6. Transfer the burst times from the cnt array to flgarr
+ *     7. Go through all detected photons. If the time of arrival for that 
+ *        photon has been flagged as bad in FLGARR then ignore it,  
+ *        otherwise copy the information to the output file.   
+ *
+ *
+ * Calibration files:
+ *	BCHR_CAL: location of the background sample regions
+ *	SCRN_CAL: burst screening params
+ *
+ * Parameter file keywords used to control the burst screening process
+ *
+ *    MNCNT : minimum enhancement of the background (in counts) needed to 
+ *            flag a burst (currently = 5)
+ *    STDRE : minimum number of standard deviations from the local mean 
+ *            for a burst to be detected (currently=5)
+ *    NBIN  : binning factor (in seconds) for the tiome sequence before 
+ *            analysis. (currently=15 seconds)
+ *    NSMED : Interval (in seconds) used in determining the median filter 
+ *            (currently=600)
+ *    SRCFRAC :  Fraction of the source intensity required for a 
+ *               burst to be removed. SCRFRAC=0.01 requires that a burst 
+ *               exceed 1% of the integrated source intensity before being 
+ *               removed (default 0.001)
+ *
+ * Returns:     0 on success
+ *
+ * History:    10/29/02   v1.1   RDR    Adapted from cf_ttag_burst
+ *             11/14/02   v1.2   peb    Tidied code and made it compatible 
+ *                                      with cf_screen_burst
+ *             12/09/02   v1.3   RDR    - Adjusted procedure for filling
+ *                                      burst flags in the timeline
+ *                                      - Corrected error in the procedure
+ *                                      that tabulates bursts properties.
+ *                                      - Used LOCATION flags to exclude
+ *                                      geocoronal emission and photons
+ *                                      off the active detector.
+ *             12/20/02   v1.4   rdr    changed status flag arrays to 
+ *                                      unsigned char
+ *             01/24/03   v1.5   rdr    corrected problem with high 
+ *                                      count rates
+ *             03/01/03   v1.6   wvd    Correct use of pointer in FITS_read_key
+ *             05/20/03   v1.7   rdr    Add cf_proc_check
+ *             05/22/03   v1.8   wvd    Exit if EXPTIME !> 0.
+ *					Change cf_error_init to stderr.
+ *					Implement cf_verbose throughout.
+ *             04/06/03   v1.9   rdr    Exclude times which have previously 
+ *                                      had a screening bit set
+ *             09/03/03   v1.10  wvd    Delete extraneous print statements
+ *             09/10/03   v1.11  wvd    Change background array to type short
+ *					Set burst flag only when flgarr[i]
+ *					< -1, not 0, to prevent bursts 
+ *					from echoing LIMB/SAA/HV flags.
+ *             09/15/03   v1.12  wvd    Use ttime[i] to populate bkgd array.
+ *					Old scheme didn't work.
+ *             10/06/03   v1.13  wvd    Change locflgs to locflags throughout.
+ *					Use bit-wise logic to test sflag array.
+ *             06/04/04   v1.14  wvd    Clean up i/o.
+ *             02/02/05   v1.15  wvd	Read AIC count rate from timeline table
+ *					rather than file header keywords.
+ *             02/02/05   v1.16  wvd	Generate bkgd array for the entire
+ *					exposure, not just good times.
+ *             08/30/05   v1.17  wvd	Ignore photons with arrival times
+ *					greater than MAX_EXPTIME.
+ *             04/09/06   v1.18  wvd	In subroutine median_filter, require
+ *					that nwin >= 1.
+ *             06/12/06   v1.19  wvd	Call cf_verbose rather than 
+ *					cf_if_warning.
+ *
+ ***************************************************************************/
+
+#include <math.h>
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include <ctype.h>
+#include "calfuse.h"
+
+/*
+ *  Function to determine the median value of an array.  
+ *  Arguments are the array,
+ *  the number of points in the array (npt) and the maximum count to
+ *  use in the histogram analysis (nmax). The median value is returned.
+ *
+ *  The analysis uses a histogram approach to determine the median
+ *  value.  Negative values of the array have been flagged as bursts
+ *  and should be ignored in determining the median value.  If all of
+ *  the points in the array have been flagged, returns zero.
+ */
+
+static int
+median(int *array, int npts, int nmax)
+{
+    int i, ngood=0, *hist, medval;
+
+    /*
+     * Set up an array to contain the histogram of the data.
+     */
+    hist = (int *) cf_calloc((nmax+1), sizeof(int));
+    /*
+     *  Fill the histogram with the data.  
+     *  Negative points are not counted.
+     */
+    for (i=0; i< npts; i++) {
+	int ndx = array[i];
+	if (ndx > nmax-1)
+	    ndx = nmax-1;
+	if (ndx >= 0 ) {
+	    ngood ++;
+	    hist[ndx]++;
+	}
+    }
+
+    /*
+     *  Determine the median value.  Set the data to 0 if there
+     *  are fewer than 2 points.
+     */
+    if (ngood > 2 ) {
+	int hnum= (int) ngood/2, atot=0;
+	i=-1;
+	while ((atot <= hnum) && (i < nmax) )
+	    atot += hist[++i];
+	medval = (int) i;
+    }
+    else
+	medval = 0;
+
+    free(hist) ;
+
+    return medval;
+}
+
+/* 
+ *  Function to construct a median filter for an array:
+ *  array  = array for which the median filter is to be constructed
+ *  npts   = number of points in the array
+ *  nflt   = number of points over which to determine the median value
+ *  medflt = array containing the median filter.
+ */
+
+static void
+median_filter(int *array, int npts, int nflt, int *medflt)
+{
+    int cntmax=0, i, hwidth, nwin, *win, medval, nsam ;
+    /*
+     *  Determine the maximum value of the array.
+     */
+    for (i = 0; i < npts; i++)
+	if (array[i] > cntmax)
+	    cntmax=array[i];
+
+    cf_verbose(3,"Constructing median filter - max cnt = %d",cntmax) ;
+    
+    /*
+     *  Determine the properties of the window over which to calculate
+     *  the median values. Make sure that the window is not larger
+     *  than the width of the data.
+     */
+    if (nflt > npts)
+	hwidth = (int) ( npts/2. ) - 1;
+    else
+	hwidth = (int) (0.5 + nflt/2. );
+    nwin = (int) 2*hwidth+1;
+    if (nwin < 1) nwin = 1;
+    win = (int *) cf_calloc(nwin, sizeof(int));
+    /*
+     *  Construct the median filter.
+     */
+    for (i = 0; i < npts; i++) {
+	int j, nmin, nmax;
+	/*
+	 *  Determine the limits to the sample.
+	 */
+	nmin = i - hwidth;
+	if (nmin < 0)
+	    nmin=0;
+	nmax = nmin+nwin;
+	if (nmax > npts-1 )
+	    nmin = npts-nwin-1;
+
+	/* Fill the sample array */
+        nsam=0 ;
+	for (j=0; j<=2*hwidth; j++) {  
+	    int ndx = nmin+j;
+	    if (ndx > npts-1)
+		ndx = npts-1;
+	    win[j] = array[ndx];
+            if (array[ndx] > 0) nsam++ ;
+	}
+
+	/* Get the median value for the sample array */
+	medval = median(win, nwin, cntmax);
+
+	/*
+        cf_verbose(6,"at point %d, nmin=%d, nmax=%d, nsam=%d, medval=%d",
+		   i, nmin, nmax, nsam, medval) ;
+	*/
+
+	/* Update the median filter */
+	medflt[i] =  medval;
+    }
+
+    free(win) ;
+
+}
+
+/*
+ *  Function to take an array marked with the times and intensities of
+ *  the bursts and identify individual bursts events and output these
+ *  to an ASCII file for later analysis.
+ */
+
+static void
+tab_burst(int *bursts, int npts, int nbin, int mjd, long tst, char *outfile)
+{
+    FILE *output;
+    int i, bflg=-1, bdur=0, bcnts=0, bst=0;
+    /*
+     *  Go through the bursts array and determine the times and
+     *  properties of the bursts.
+     */
+    output = fopen(outfile, "w");
+
+    cf_verbose(2, "BURST SUMMARY") ;
+    for (i=0; i<npts; i++) {
+	if (bursts[i] > 0 && bflg < 0) {
+	    bflg=1;
+	    bst= i*nbin;
+	}
+	if (bursts[i] > 0 && bflg > 0) {
+	    bdur++;
+	    bcnts = bcnts + bursts[i];
+	}
+	if (bursts[i] < 0 && bflg > 0) {
+	  cf_verbose(2, "start=%d,  duration=%ld seconds,  counts=%d",
+		 bst, bdur*nbin, bcnts) ; 
+ 	   fprintf(output, " %d   %ld    %d   %d \n",
+	       mjd, bst+tst, bdur*nbin, bcnts);
+  	    bflg=-1;
+	    bdur=0;
+	    bcnts=0;
+	}
+    }
+
+    /* Check to see whether a burst is in progress at the end of the obs */
+    if (bflg > 0) {
+       	  cf_verbose(2, "start=%d,  duration=%ld seconds,  counts=%d",
+		 bst, bdur*nbin, bcnts) ; 
+	  fprintf(output, " %d   %ld    %d   %d\n",
+		    mjd, bst+tst, bdur*nbin, bcnts);
+    }
+
+}
+
+
+int
+cf_screen_burst(fitsfile *infits, long nevents, float *ptime, float *x, 
+		float *y, unsigned char *locflags, GTI *gti, long nsec, 
+                float *ttime, unsigned char *sflag, float *aic_rate,
+		short *bkgd)
+{
+    char CF_PRGM_ID[] = "cf_screen_burst";
+    char CF_VER_NUM[] = "1.19";
+
+    short ylim[8], k;
+    int   anynull, errflg=0, intnull=0, cflg=-1, nrowbkg=0, ngood;
+    int   npts, nmax, nflt, iflg, numflg, ndxs, ndxe, ndx, ndxb;
+    int   *bcnts, *cnts, *gcnts, *medflt, *flgarr, *bursts, lim_col;
+    int   nflg, niter, mjd , status=0, medval;
+    long  frow=1, felem=1, tst , i, j;
+    long  stdrej, mncnt, nsmed, mnburst, nbin, nflgarr;
+    float exptime, max_aic_rate, bkgsf, bkgsft, srcfrac, mxtime;
+    double expstrt;
+    char  burst_tab[FLEN_CARD];
+    char  expid[FLEN_CARD], progid[FLEN_CARD], targid[FLEN_CARD];
+    char  scobsid[FLEN_CARD], scrnfile[FLEN_CARD], aperf[FLEN_CARD];
+    char  det[FLEN_CARD], bchrfile[FLEN_CARD], aper[5];
+    fitsfile *scrnfits, *bchrfits;
+
+    /*
+     *  Initialize error checking
+     */ 
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+    if ((errflg = cf_proc_check(infits, CF_PRGM_ID))) return errflg;
+
+    /*
+     *  Read header keywords.
+     */
+    FITS_read_key(infits, TFLOAT, "EXPTIME", &exptime, NULL, &status);
+    FITS_read_key(infits, TDOUBLE, "EXPSTART", &expstrt, NULL, &status);
+    FITS_read_key(infits, TSTRING, "PRGRM_ID", progid, NULL, &status);
+    FITS_read_key(infits, TSTRING, "TARG_ID", targid, NULL, &status);
+    FITS_read_key(infits, TSTRING, "SCOBS_ID", scobsid, NULL, &status);
+    FITS_read_key(infits, TSTRING, "EXP_ID", expid, NULL, &status);
+    FITS_read_key(infits, TSTRING, "DETECTOR", det, NULL, &status);
+
+    /*
+     * Exit if EXPTIME is 0.
+     */ 
+    if (exptime < 1) {
+	cf_verbose(1, "EXPTIME = %f.  Exiting.", exptime);
+	return status;
+    }
+
+    /*
+     *  Determine the Julian date and start time from expstrt.
+     */
+    mjd = (int) expstrt;
+    tst = (int) ((expstrt - mjd)*86400.);
+    det[1] = tolower(det[1]);
+
+    /*  Ignore events with arrival times greater than MAX_EXPTIME. */
+    i = nevents - 1;
+    while (ptime[i] > MAX_EXPTIME && i > 0) i--;
+    nevents = i + 1;
+    i = nsec - 1;
+    while (ttime[i] > MAX_EXPTIME && i > 0) i--;
+    nsec = i + 1;
+  
+    /*
+     *  Determine the maximum count rate for the exposure.
+     *  If the count rate is too high, there is the possibility of
+     *  losing counts and of dropouts - Check the count rate and set
+     *  a flag if it is too high.
+     */
+    max_aic_rate = -999.;
+    for (i = 0; i < nsec; i++)
+	if (aic_rate[i] > max_aic_rate) max_aic_rate = aic_rate[i];
+    cf_verbose(2, "Max AIC count rate = %d", cf_nint(max_aic_rate));
+    if(max_aic_rate > 4000) cflg=1;
+
+    /*
+     *  Read the screening parameter file.
+     */
+    FITS_read_key(infits, TSTRING, "SCRN_CAL", scrnfile, NULL, &status);
+    cf_verbose(3, "Screening parameters from %s\n", scrnfile);
+    FITS_open_file(&scrnfits, cf_parm_file(scrnfile), READONLY, &status);
+    FITS_read_key(scrnfits, TLONG, "MNCNT", &mncnt, NULL, &status);
+    FITS_read_key(scrnfits, TLONG, "STDREJ", &stdrej, NULL, &status);
+    FITS_read_key(scrnfits, TLONG, "NBIN", &nbin, NULL, &status);
+    /*
+     *  Set the binning factor to 1 for high count rate data.
+     */
+    if (cflg > 0) {
+        nbin=1;
+        cf_verbose(1, "High count-rate observation: using 1 sec time bins") ;
+    }
+    FITS_read_key(scrnfits,TLONG,"NSMED",&nsmed, NULL, &status);
+    /*
+     *  srcfrac=required fraction of the source intensity for a
+     *  burst to be counted, i.e. the burst must exceed this fraction
+     *  before it is deemed to be significant.
+     */
+    FITS_read_key(scrnfits, TFLOAT, "SRCFRAC", &srcfrac, NULL, &status);
+    FITS_read_key(infits, TSTRING, "APERTURE", aperf, NULL, &status);
+    FITS_close_file(scrnfits, &status);
+
+    cf_verbose(3, "Screening parameters used:");
+    cf_verbose(3, "Minimum count rate = %ld", mncnt);
+    cf_verbose(3, "Detection criterion (num sigma) = %ld", stdrej);
+    cf_verbose(3, "Number of seconds to bin the time sequence = %ld", nbin);
+    cf_verbose(3, "Interval (seconds) used in median filter = %ld", nsmed);
+    cf_verbose(3, "Fraction of source intensity for burst = %f\n", srcfrac);
+    /*
+     *  Select the background extraction regions - RFPT implies
+     *  that there is no source, so the entire detector can be used.
+     */
+    strncpy(aper, aperf, 5);
+    cf_verbose(3, "Aperture designation = %s", aper);
+    if (strcmp ( aper , "RFPT") == 0 ) {
+	cf_verbose(3, "APERTURE = RFPT.  No source in aperture.");
+	ylim[0] = 0;
+	ylim[1] = 1;
+	ylim[2] = 2;
+	ylim[3] = 1020;
+	ylim[4] = 1021;
+	ylim[5] = 1022;
+	ylim[6] = 1022;
+	ylim[7] = 1022;
+    }
+    else {
+	/*
+	 *  open the bchr parameter file
+	 */
+	FITS_read_key(infits, TSTRING, "BCHR_CAL", bchrfile, NULL, &status);
+	cf_verbose(3, "BCHR parameter file: %s", bchrfile);
+	FITS_open_file(&bchrfits, cf_parm_file(bchrfile), READONLY, &status);
+
+	/* Move to the first extension of the BCHR file, which contains
+	   the limits to the background regions */
+	FITS_movabs_hdu(bchrfits, 2, NULL, &status);
+
+	/* Get the column number for the data to be extracted */
+	FITS_get_colnum(bchrfits, CASEINSEN, aper, &lim_col, &status);
+	
+	/* Read the data from the table */
+	FITS_read_col(bchrfits, TSHORT, lim_col, frow, felem, 8, &intnull, 
+		      ylim, &anynull, &status);
+
+	/* Close the bchr file */
+	FITS_close_file(bchrfits, &status);
+    }
+    cf_verbose(3, "Y limits of background region: %d-%d, %d-%d, %d-%d\n",
+	   ylim[0], ylim[1], ylim[2], ylim[3], ylim[4], ylim[5]);
+    /*
+     *  Now get the time sequence and a good time interval flag array.
+     */
+    cf_verbose(3, "nevents = %ld", nevents);
+    mxtime=ptime[nevents-1];
+    nflgarr = cf_nint(mxtime);
+    npts= (int) mxtime/nbin;
+    cf_verbose(3, "Number of points in the (binned) time sequence = %d", npts);
+    cf_verbose(3, "Number of points in the good time flag array = %ld", nflgarr);
+    /*
+     *  Generate arrays to contain the time sequence in the
+     *  background sample regions (cnts) as well as the entire
+     *  detector (gcnts). Also generate an array to contain only
+     *  the bursts (bursts).
+     *  Array bcnts will contain the background count rate.
+     */
+    bcnts  = (int *) cf_calloc(npts, sizeof(int));
+    cnts   = (int *) cf_calloc(npts, sizeof(int));
+    gcnts  = (int *) cf_calloc(npts, sizeof(int));
+    bursts = (int *) cf_calloc(npts, sizeof(int));
+    /* Generate an array to contain the good time flags - this is an array 
+       with 1s time intervals. Each interval is set to a negative number (-1)
+       if it contains a bad time interval or a positive number (1) if it 
+       contains a good time interval. The contents of this array are used to
+       screen the photons and to determine the good time intervals */
+    flgarr = (int*) cf_calloc(nflgarr, sizeof(int) );
+    /* Generate an array with 1s time intervals to contain the day/night
+       information - this will be 1 for night and 0 for day */
+
+    /* Initially flag all of the points with a negative number.
+       The good time intervals will be determined later */
+    for (i=0; i<npts; i++) {
+      cnts[i] = -10 ;
+      gcnts[i] = 0 ;
+      bursts[i] = -10 ;
+    }
+    for (i=0; i<nflgarr; i++) flgarr[i] = -1 ;
+    /*
+     *  Set the counts array to zero (i.e. unflag the point) for all
+     *  good time points.
+     */
+    ngood = 0 ;
+    for (i=0; i < gti->ntimes;  i++) {
+	 ndxs= (int) gti->start[i]/nbin;
+	   if (ndxs < 0 ) ndxs = 0 ;
+	 ndxe = (int) (0.5 + gti->stop[i]/nbin);
+           if (ndxe > npts-1) ndxe = npts-1;
+	for (j=ndxs; j<= ndxe; j++) {
+	    ngood++;
+	    cnts[j]=0;
+	}
+    }
+    cf_verbose(2, "Number of good time points = %d\n", ngood);
+
+    /* Set the good time flags array to a positive value for all good 
+       time points  */
+
+    for (i=0; i < gti->ntimes;  i++) {
+	ndxs= (int) gti->start[i];
+	    if (ndxs < 0) ndxs = 0 ;
+	ndxe = (int) gti->stop[i];
+	   if (ndxe > nflgarr-1) ndxe=nflgarr-1;
+	for (j=ndxs; j<= ndxe; j++)
+	    flgarr[j]=1;
+    }
+
+    /* Check the timeline-table screening flag and mark all times that have
+       a screening bit set (except for day/night) */
+     for (i=0; i<nsec; i++) {
+       ndx = (int) (0.5+ttime[i]) ;
+	if( ndx > nflgarr-1) ndx = nflgarr-1;
+        if( ndx < 0) ndx = 0 ;
+       ndxb = (int) (0.5 + (float) ndx/ (float) nbin) ;
+        if(ndxb > npts-1) ndxb = npts-1 ;
+        if (ndxb < 0) ndxb=0 ;
+       if (sflag[i] & ~TEMPORAL_DAY) {
+	  flgarr[ndx] = -1 ;
+          cnts[ndxb] = -10 ;
+	}
+    }
+
+    /* Generate the time sequence for the total counts from the detector. 
+       Use only the active area and ignore geocoronal emission. */
+
+    for (i=0; i < nevents; i+=1)
+    if( (locflags[i] & LOCATION_SHLD) == 0 && 
+        (locflags[i] & LOCATION_AIR) == 0 ) {
+	    int ndx = (int) ptime[i]/nbin;
+	    if (ndx > npts-1)
+		ndx=npts-1;
+	    if (ndx < 0)
+		ndx=0;
+	    gcnts[ndx] += 1;
+	}
+    
+    /* Determine the number of rows in the background sample region */
+    for (k=0; k < 3; k++)
+	nrowbkg += ylim[2*k+1] - ylim[2*k];
+    /*  
+     *  Determine the scaling factor needed to convert the measured
+     *  counts in the background regions to an estimate of the
+     *  background counts over the active aperture.
+     */
+    bkgsf= (float) ylim[6]/nrowbkg;
+    bkgsft = (float) ylim[7]/nrowbkg;
+
+    cf_verbose(2, "Rows in target aperture = %d", ylim[6]);
+    cf_verbose(2, "Rows on the detector = %d", ylim[7]);
+    cf_verbose(2, "Rows in background region = %d", nrowbkg);
+    cf_verbose(2, "Scale factor to aperture = %f ", bkgsf);
+    cf_verbose(2, "Scale factor to entire detector = %f", bkgsft);
+        
+    /* Generate the time sequence using only the counts from the three
+       selected background regions - ignore geocoronal lines and times 
+       that have been flagged as bad (with negative count values) */ 
+    for (k=0; k<3; k++) {  
+	short ylow=ylim[2*k];
+	short yhigh=ylim[2*k+1];
+	for (i=0; i < nevents; i+=1) {
+	  if( (locflags[i] & LOCATION_SHLD) == 0 && 
+              (locflags[i] & LOCATION_AIR) == 0 && 
+              (y[i] > ylow) && (y[i] < yhigh) ) {
+		int ndx = (int) ptime[i]/nbin;
+		if (ndx > npts-1)
+		    ndx=npts-1;
+		if (ndx < 0)
+		    ndx=0;
+		if (cnts[ndx] >= 0) cnts[ndx] += 1;
+		bcnts[ndx] ++;
+	    }
+	}
+    }
+    
+    /* Fill background count rate array with cnts array, and divide by nbin
+       to give count rate */
+/*	THIS SCHEME WORKS ONLY IF THERE ARE NO TIME BREAKS IN THE TIMELINE
+ *	TABLE.  SINCE TIME BREAKS ARE COMMON, MUST USE TTIME ARRAY TO MAP
+ *	CNTS ARRAY TO BKGD ARRAY.	WVD 09/15/03
+ *   for (i=0; i<npts; i++) {
+ *	int ndxs= i*nbin;
+ *	int ndxe= ndxs + nbin;
+ *	if (ndxe > nsec-1)
+ *	    ndxe=nsec-1;
+ *	for (j=ndxs;j<ndxe; j++)
+ *	    bkgd[j] = (short) ((float) cnts[i] / nbin + 0.5);
+ *   }
+ */
+    for (i=0; i<nsec; i++) {
+       ndx = cf_nint(ttime[i]/nbin) ;
+	if( ndx > nflgarr-1)
+	    ndx = nflgarr-1;
+/*	if (cnts[ndx] > 0.)
+  	    bkgd[i] = (short) ((float) cnts[ndx] / nbin + 0.5);
+	else
+	    bkgd[i] = 0;
+*/
+	bkgd[i] = bcnts[ndx] / nbin;
+    }
+    free (bcnts);
+
+    /* Remove the background counts (scaled to the entire detector) from the 
+       measured gross count rate  */
+    for (i=0; i < npts; i++) if (cnts[i] > 0) {
+	gcnts[i] = gcnts[i] - bkgsft*cnts[i];
+	if (gcnts[i] < 0)
+	    gcnts[i] = 0;
+    }
+
+    /* Check for zeros in the count array for high count rate data - these
+       indicate dropouts. If one is found, flag it with a negative number so
+       that the program will ignore it in future analysis */
+    numflg=0;
+     if (cflg > 0) {
+	for (i=0; i < npts; i++) {
+	    if (cnts[i] <= 0.1 ) {
+		numflg += 1;
+		cnts[i]=-10;
+	    }
+	}
+    }
+    cf_verbose(2, "Number of dropouts found = %d", numflg);
+
+    /* Determine the median value of the array */
+    nmax=2000;
+    medval = median(cnts, npts, nmax);
+    cf_verbose(2, "Median value of the entire original array = %d ", medval);
+
+    /* Screen the time series for very large count rates (> 3 x median) */
+    cf_verbose(2, "Searching for large bursts ") ;
+    for ( i=0; i<npts; i++)
+	if (cnts[i] > 4*medval) {
+	  cf_verbose(2,"point rej: time=%d, cnts=%d, 4*medval=%d ",
+		     i*nbin, cnts[i], 4*medval) ;
+	    bursts[i] = cnts[i]-medval;
+	    cnts[i] = -100;
+	}
+
+    /* Do a median filter on the pre-filtered array */
+
+    /* Generate the array to contain the median filter */
+    medflt = (int *) cf_calloc(npts, sizeof(int) );
+
+    /*
+     *  Now specify the parameters of the filter - 
+     *  nsmed = number of seconds over which to determine median values
+     *  nflt = number of points in the cnts array over which to
+     *  determine the median value
+     */
+    nflt = nsmed / nbin;
+    niter=0;
+ 
+    cf_verbose(3,"Searching for small bursts - nflt = %d", nflt) ;
+
+    do {
+	median_filter(cnts, npts, nflt, medflt);
+
+	/* Throw out all points which are more than (stdrej) standard
+	   deviations above the median. Also require that the counts exceed
+	   a certain minimum value. */
+	nflg=0;
+	mnburst=mncnt*nbin;
+	for (i=0; i<npts; i++) {
+	    int dcnt=cnts[i]-medflt[i];
+	    if ( (dcnt > mnburst) && 
+		 (dcnt > stdrej*sqrt((double) cnts[i])) && 
+		 (dcnt*bkgsf > srcfrac*gcnts[i]) ) {
+		nflg++;
+		cf_verbose(2, "point rej: time=%ld, cnts=%d, medflt=%d, "
+		       "dif=%d, gcnts= %d",
+		       i*nbin, cnts[i], medflt[i], dcnt, gcnts[i]);
+		cnts[i] = -100;
+		bursts[i] = dcnt;
+	    }
+	}
+	niter++;
+	cf_verbose(3,"After iteration %d, we found %d times affected by bursts",
+                   niter, nflg) ;
+	/*  Iterate the median filter if any additional points have
+	 *  been modified*/ 
+    } while(nflg > 0 && niter < 10);
+
+    /* Print out the results of the screening 
+       cf_verbose(5, " "); 
+       for (i=0; i<npts; i++) 
+           cf_verbose(5, "At time %4d, cnts= %4d, medflt= %4d, dif= %4d, gcnts= %4d",
+		i*nbin, cnts[i],medflt[i], cnts[i]-medflt[i], gcnts[i]);
+       cf_verbose(3, " "); 
+    */
+
+    /* Use the regions of the cnts array equal to -100 to specify
+       the burst times in the flgarr array */
+    for (i=0; i<npts; i++ ) {
+	if (cnts[i] < -20) {
+	    int ndxs = i*nbin, ndxe;
+	    if (ndxs > nflgarr-nbin-2) 
+		ndxs=nflgarr-nbin-2;
+	    ndxe = ndxs + nbin - 1;
+	    for (j=ndxs; j<=ndxe; j++)
+		flgarr[j] = -10;
+	}
+    }
+
+    /* tabulate the burst times */
+    sprintf(burst_tab, "%4s%2s%2s%3s%2s_bursts.dat", progid, targid, scobsid, expid, det);
+    tab_burst(bursts, npts, nbin, mjd, tst, burst_tab);
+    cf_verbose(3, "Burst properties written to file: %s", burst_tab);
+
+    /* Check the last 2*nbin elements of flgarr. If any of these are set as
+       bad, then set all the end points as bad. The binned count time sequence 
+       will not sample the end of the ovarall time sequence if there is not an 
+       integral number of bins present. We also do not need the last bin if the
+       second-to-last is bad. */
+
+    i=nflgarr-2*nbin;
+    iflg=10;
+    do{ 
+	if (flgarr[i] < -1) {		/* 09/12/03 - wvd - Change from 0 */
+	    for (j=i; j<nflgarr; j++)
+		flgarr[j]=-10;
+	    iflg = -10;
+	};
+	i++;
+    } while (iflg > 0 && i < nflgarr);
+
+    /* set the timeline status flag (sflag - TEMPORAL_BRST) for all 
+       times containing bursts */
+    for (i=0; i<nsec; i++) {
+       ndx = (int) (0.5+ttime[i]) ;
+	if( ndx > nflgarr-1)
+	    ndx = nflgarr-1;
+	if (flgarr[ndx] < -1)		/* 09/12/03 - wvd - Change from 0 */
+	    sflag[i] = sflag[i] | TEMPORAL_BRST;
+    }
+    /* deallocate storage space */
+    free(cnts) ;
+    free(gcnts) ;
+    free(flgarr) ;
+    free(medflt) ;
+    free(bursts) ;
+
+    /* Enter a time stamp into the log */
+    cf_proc_update(infits, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished processing");
+
+    return (status);
+} 
diff --git a/src/libcf/cf_screen_high_voltage.c b/src/libcf/cf_screen_high_voltage.c
new file mode 100644
index 0000000..57a9716
--- /dev/null
+++ b/src/libcf/cf_screen_high_voltage.c
@@ -0,0 +1,146 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:	cf_screen_high_voltage(fitsfile *infits, long nseconds,
+ *              unsigned char *timeline_status, short *timeline_hv);
+ *
+ * Description: Set the screening bit if detector voltage is low.
+ *
+ * Arguments:   fitsfile  *infits       Input FITS file pointer
+ * 		long      nseconds      Number of points in the timeline table
+ * 		unsigned char  *timeline_status   The status flag array
+ * 		short     *timeline_hv  The high voltage array
+ *
+ * Calls:
+ *
+ * Returns:	0 on success
+ *
+ * History:	10/23/02   1.1   jch    Initial coding
+ * 		12/20/02   1.3   jch    Make sure the flags are "unsigned" char
+ *              01/24/03   1.4   rdr    Lower the voltage threshold required 
+ *                                      to flag a time to 95% of the full 
+ *                                      voltage
+ * 		02/11/03   1.6   jch    Skip HV which is negative
+ *              05/20/03   1.7   rdr    Add call to cf_proc_check
+ *              05/22/03   1.8   wvd    Implement cf_verbose
+ *              06/11/03   1.9   wvd    Change HV array to type short.
+ *              06/13/03   1.10  wvd    Change calfusettag.h to calfuse.h
+ *              09/10/03   1.11  wvd    Return errflg from cf_proc_check.
+ *              07/21/04   1.12  wvd    Delete unused variable volt_cor.
+ *              02/17/05   1.13  wvd    Place parentheses around assignment
+ *					used as truth value.
+ *              03/18/05   1.14  wvd    HV can be 0, so test for HV > -1
+ *              03/24/05   1.15  wvd    Read HVGOODLM and HVBADLIM from 
+ *					VOLT_CAL file.  If HV/FULLV drops
+ *					below HVGOODLM, issue warning.
+ *					If it falls below HVBADLM, set
+ *					TEMPORAL_HV flag.
+ *              06/22/06   1.16  wvd    Don't set EXP_STAT keyword.
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include <stdio.h>
+#include "calfuse.h"
+
+int
+cf_screen_high_voltage(fitsfile *infits, long nseconds,
+	       unsigned char *timeline_status, short *timeline_hv)
+{
+    char CF_PRGM_ID[] = "cf_screen_high_voltage";
+    char CF_VER_NUM[] = "1.16";
+
+    char  file_name[FLEN_VALUE], mjd_str[FLEN_VALUE], full_str[FLEN_VALUE];
+    char  datestr[FLEN_VALUE], comment[FLEN_COMMENT], instmode[FLEN_VALUE];
+    int	  errflg=0, status=0, timeref, hvflag=FALSE, n, fullv;
+    long  i;
+    float expstart, hvfrac, hvgood, hvbad, mjdv;
+    fitsfile *scrnfits;
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+    if ((errflg = cf_proc_check(infits, CF_PRGM_ID))) return errflg;
+
+    /* Read exposure start time and instrument mode. */
+    FITS_read_key(infits, TFLOAT, "EXPSTART", &expstart, NULL, &status);
+    FITS_read_key(infits, TSTRING, "INSTMODE", instmode, NULL, &status);
+    /*
+     *  Open the high-voltage calibration file.
+     */
+    FITS_read_key(infits, TSTRING, "VOLT_CAL", file_name, NULL, &status);
+    FITS_open_file(&scrnfits, cf_cal_file(file_name), READONLY, &status);
+    /*
+     *  Read the limits of the good and questionable voltage regimes.
+     */
+    FITS_read_key(scrnfits, TFLOAT, "HVGOODLM", &hvgood, NULL, &status);
+    FITS_read_key(scrnfits, TFLOAT, "HVBADLIM", &hvbad,  NULL, &status);
+    /*
+     *  Read full-voltage level in use at time of observation.
+     */
+    n = 0;
+    do {
+	n++;
+	sprintf(mjd_str, "MJD%d", n);
+	FITS_read_key(scrnfits, TFLOAT, mjd_str, &mjdv, NULL, &status);
+    } while (expstart > mjdv);
+    n--;
+
+    sprintf(full_str, "FULL%d", n);
+    FITS_read_key(scrnfits, TINT, full_str, &fullv, NULL, &status);
+    FITS_close_file(scrnfits, &status);
+
+    /*
+     *  Check for low values of the detector voltage.
+     *  Set the high voltage bit if timeline_hv/fullv < hvbad.
+     */
+        cf_verbose(2, "Threshold voltage = %d", cf_nint(hvbad * fullv)) ; 
+
+    for (i = 0; i < nseconds; i++) if (timeline_hv[i] > -1) {
+	hvfrac = timeline_hv[i] / (float) fullv;
+	if (hvfrac < hvgood) {
+	    if (hvfrac < hvbad) timeline_status[i] |= TEMPORAL_HV; 
+	    else hvflag = TRUE;
+	}
+    }
+
+    /*
+     *  If the detector voltage ever falls between the good and bad
+     *  levels, issue a stern warning to the user.
+     */
+    if (hvflag) {
+	/* Write warning to trailer file. */
+	if (!strncmp(instmode, "HIST", 4))
+	cf_if_warning("Detector voltage is < 90%% of optimal value.  "
+	"Check photometry and wavelength scale.");
+	else
+	cf_if_warning("Detector voltage is < 90%% of optimal value.  "
+	"Check pulse-height distribution.");
+
+	/* Write warning to IDF file header. */
+	FITS_write_comment(infits, " ", &status);
+	FITS_write_comment(infits,
+	"Detector voltage is less than 90%% of optimal value.", &status);
+	if (!strncmp(instmode, "HIST", 4)) {
+	FITS_write_comment(infits,
+	"Carefully examine these data for photometric errors", &status);
+	FITS_write_comment(infits, "and walk effects.", &status);
+	}
+	else {
+	FITS_write_comment(infits,
+	"Carefully examine the pulse height distribution of photons", &status);
+	FITS_write_comment(infits,
+	"in the target aperture before accepting these data.", &status);
+	}
+	fits_get_system_time(datestr, &timeref, &status);
+	sprintf(comment, "CalFUSE v%s   %.10s", CALFUSE_VERSION, datestr);
+	FITS_write_comment(infits, comment, &status);
+	FITS_write_comment(infits, "  ", &status);
+    }
+
+    cf_proc_update(infits, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return status;
+}
diff --git a/src/libcf/cf_screen_jitter.c b/src/libcf/cf_screen_jitter.c
new file mode 100644
index 0000000..68327a0
--- /dev/null
+++ b/src/libcf/cf_screen_jitter.c
@@ -0,0 +1,246 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center for Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_screen_jitter (infile, nsec, ttime, status_flag)
+ *
+ * Description: Flag times when target is out of the aperture or pointing
+ *		is known to be bad.  Read the minimum trustworthy TRKFLG 
+ *		value and aperture limits from the parameter file.
+ *		
+ *              Key to new TRKFLG values:
+ *      	5 = dx, dy from known FPDs and q_cmd from telemetry
+ *      	4 = good dx, dy from ACS q_est and q_cmd from telemetry
+ *      	3 = maybe good dx, dy from ACS q_est
+ *      	2 = dx, dy from known FPDs, q_cmd from FITS header coordinates
+ *      	1 = dx, dy from ACS q_est, q_cmd from FITS header coordinates
+ *      	0 = no pointing information (missing telemetry)
+ *             -1 = Pointing is assumed to be bad (never achieved known track)
+ *
+ * Arguments:   fitsfile  infile        Pointer to the IDF
+ *              long      nsec          Number of seconds in the timeline
+ *              long      *ttime        time (sec) of each point in the timeline
+ *     unsigned char      *status_flag  Timeline status flags
+ *
+ * Returns:	0 upon success
+ *
+ * History:     11/29/05   v1.1   wvd   Adapted from cf_satellite_jitter
+ *		03/28/06    1.2   wvd	Test both dx and dy.
+ *		05/09/06    1.3   wvd	Apply jitter screening to RFPT obs.
+ *		06/12/06    1.4   wvd	Call cf_verbose when jitter file not
+ *					found.
+ *		08/21/06    1.5   wvd	Use EXPSTART in jitter and data
+ *					headers to correct jitter time array.
+ *		08/25/06    1.6   wvd	Change meaning of TRKFLG values.
+ *					TRKFLG = 3 is only used internally.
+ *		11/06/06    1.7   wvd	Change meaning of TRKFLG values.
+ *					Read minimum TRKFLG value and
+ *					aperture limits from parmfile.
+ *					Require jitter file version >= 3.0.
+ *					Don't screen moving targets.
+ *					Bail out only if JIT_STAT = 1.
+ *		12/29/06    1.8   wvd	Exit if JIT_VERS < 3.0.
+ *              03/23/07    1.9   wvd   Store offset between the jitter and 
+ *					data values of EXPSTART in variable
+ *					time_diff.
+ *              04/07/07    1.10  wvd   Clean up compiler warnings.
+ *              08/16/07    1.11  wvd   Don't apply jitter correction to
+ *					observations taken after the 
+ *					spacecraft lost pointing control.
+ *              07/25/08    1.12  wvd   Use EXP_STAT keyword, rather than
+ *					file name, to check for bright-earth
+ *					or airglow observations.
+ *              11/21/08    1.13  wvd   Don't apply jitter correction to
+ *					ERO observations of Jupiter.
+ *					
+ ****************************************************************************/
+
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include <ctype.h>
+#include "calfuse.h"
+
+#define	JIT_VERS_MIN	3.0
+#define	BAD_TRKFLG	-1
+#define LAST_MJD	54300.
+
+int
+cf_screen_jitter(fitsfile *infits, long nsec, float *ttime,
+	unsigned char *status_flag)
+{
+    char CF_PRGM_ID[] = "cf_screen_jitter"; 
+    char CF_VER_NUM[] = "1.13";
+
+    char  jitr_cal[FLEN_VALUE], parmfile[FLEN_VALUE];
+    char  comment[FLEN_COMMENT], hkexists[FLEN_VALUE], jit_vers[FLEN_VALUE];
+    char  mov_targ[FLEN_VALUE], program[FLEN_VALUE];
+    int   errflg=0, status=0, expstat, jitter_status, hdutype;
+    long  j, k, njitr, *time_jit, time_diff;
+    short *trkflg, trkflg_min;
+    double data_expstart, jitr_expstart;
+    float *dx_jit, *dy_jit, dx_max, dy_max;
+    fitsfile  *jitfits, *parmfits;
+
+    /* Initialize error checking */ 
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+    /* Enter a time stamp into the log */
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    /* Read exposure start time from IDF header */
+    FITS_read_key(infits, TDOUBLE, "EXPSTART", &data_expstart, NULL, &status);
+
+    /* Check whether program is appropriate for this data set. */
+    if ((errflg = cf_proc_check(infits, CF_PRGM_ID))) return errflg;
+
+    /* Don't apply jitter screening to bright-earth or airglow observations. */
+    FITS_read_key(infits, TINT, "EXP_STAT", &expstat, NULL, &status);
+    if (expstat == (int) TEMPORAL_LIMB) {
+        cf_verbose(1, "Bright-earth or airglow observation.  ",
+	"No jitter correction.");
+        cf_proc_update(infits, CF_PRGM_ID, "SKIPPED");
+        cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished processing");
+        return 0;
+    }
+
+    /* Don't apply jitter screening to moving targets. */
+    FITS_read_key(infits, TSTRING, "MOV_TARG", mov_targ, NULL, &status);
+    if (!strncmp(mov_targ, "M", 1)) {
+        cf_verbose(1, "Moving-target observation.  No jitter correction.");
+        cf_proc_update(infits, CF_PRGM_ID, "SKIPPED");
+        cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished processing");
+        return 0;
+    }
+
+    /* Don't apply jitter screening to ERO observations of Jupiter. */
+    FITS_read_key(infits, TSTRING, "PRGRM_ID", program, NULL, &status);
+    if (!strncmp(program, "X006", 4)) {
+        cf_verbose(1, "Moving-target observation.  No jitter correction.");
+        cf_proc_update(infits, CF_PRGM_ID, "SKIPPED");
+        cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished processing");
+        return 0;
+    }
+
+    /* Don't apply jitter screening after pointing control is lost. */
+    if (data_expstart > LAST_MJD) {
+        cf_verbose(1, "No pointing control.  No jitter correction.");
+        cf_proc_update(infits, CF_PRGM_ID, "SKIPPED");
+        cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished processing");
+        return 0;
+    }
+
+    /* Check HKEXISTS before looking for jitter file. */
+    FITS_read_key(infits, TSTRING, "HKEXISTS", hkexists, NULL, &status);
+    if(!strncasecmp(hkexists, "N", 1) || !strncasecmp(hkexists, "n", 1)) {
+        cf_verbose(1, "HKEXISTS = %s.  No jitter correction.", hkexists);
+        cf_proc_update(infits, CF_PRGM_ID, "SKIPPED");
+        cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished processing");
+        return 0;
+    }
+
+    /* Try to open the jitter file. */
+    FITS_read_key(infits, TSTRING, "JITR_CAL", jitr_cal, NULL, &status);
+    fits_open_file(&jitfits, jitr_cal, READONLY, &status);
+
+    /* If the jitter file is not found, try a lower-case filename. */
+    if (status != 0) {
+        status = 0;
+        jitr_cal[0] = (char) tolower(jitr_cal[0]);
+        fits_open_file(&jitfits, jitr_cal, READONLY, &status);
+    }
+
+    /* If the jitter file is still not found, exit the program */
+    if (status != 0) {
+        cf_verbose(1, "Jitter file not found.  No jitter correction.");
+        cf_proc_update(infits, CF_PRGM_ID, "SKIPPED");
+        cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished processing");
+        return 0;
+    }
+    cf_verbose(3, "Jitter calibration file = %s", jitr_cal);
+
+    /* Check status keyword in jitter file.  Exit if missing or non-zero. */
+    fits_read_key(jitfits, TINT, "JIT_STAT", &jitter_status, comment, &status);
+    if (status != 0) {
+	status = 0;
+	cf_verbose(1, "Keyword JIT_STAT not found. No jitter correction.");
+	cf_proc_update(infits, CF_PRGM_ID, "SKIPPED");
+	cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished processing");
+	return 0;
+    }
+    if (jitter_status == 1) {
+	cf_verbose(1, "Keyword JIT_STAT = %d.  No jitter correction.",
+	jitter_status) ;
+	cf_proc_update(infits, CF_PRGM_ID, "SKIPPED");
+	cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished processing");
+	return 0;
+    }
+
+    /* Read exposure start time from jitter file header */
+    FITS_read_key(jitfits, TDOUBLE, "EXPSTART", &jitr_expstart, NULL, &status);
+
+    /* Check JIT_VERS keyword.  Exit if missing or value too low. */
+    fits_read_key(jitfits, TSTRING, "JIT_VERS", jit_vers, NULL, &status);
+    if (status != 0 || atof(jit_vers) < JIT_VERS_MIN) {
+	status = 0;
+	cf_verbose(1, "Jitter file format is out of date. No jitter correction.");
+	cf_proc_update(infits, CF_PRGM_ID, "SKIPPED");
+	cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished processing");
+	return 0;
+    }
+
+    /* Read the jitter file. */
+    FITS_movabs_hdu(jitfits, 2, &hdutype, &status);
+    njitr=cf_read_col(jitfits, TLONG, "TIME", (void **) &time_jit);
+    njitr=cf_read_col(jitfits, TFLOAT, "DX", (void **) &dx_jit);
+    njitr=cf_read_col(jitfits, TFLOAT, "DY", (void **) &dy_jit);
+    njitr=cf_read_col(jitfits, TSHORT, "TRKFLG", (void **) &trkflg);
+    FITS_close_file(jitfits, &status);
+
+    /* Correct for difference in data and jitter EXPSTART times */
+    time_diff = cf_nlong((data_expstart - jitr_expstart) * 86400.);
+    cf_verbose(2, "Offset between IDF and jitter EXPSTART values: %d sec",
+	time_diff);
+    for (j=0; j< njitr; j++) time_jit[j] -= time_diff;
+
+    /* Read minimum TRKFLG value and aperture boundaries from PARM_CAL file */
+    FITS_read_key(infits, TSTRING, "PARM_CAL", parmfile, NULL, &status);
+    FITS_open_file(&parmfits, cf_parm_file(parmfile), READONLY, &status);
+    FITS_read_key(parmfits, TSHORT, "TRKFLG", &trkflg_min, NULL, &status);
+    FITS_read_key(parmfits, TFLOAT, "DX_MAX", &dx_max, NULL, &status);
+    FITS_read_key(parmfits, TFLOAT, "DY_MAX", &dy_max, NULL, &status);
+    FITS_close_file(parmfits, &status);
+
+    /* Reject times when tracking is good, but target is out of aperture. */
+    for (j=0; j< njitr; j++) {
+	if (trkflg[j] >= trkflg_min  && 
+		(dx_jit[j] < -dx_max || dx_jit[j] > dx_max ||
+		 dy_jit[j] < -dy_max || dy_jit[j] > dy_max)) {
+	    trkflg[j] = BAD_TRKFLG;
+	}
+    }
+
+    /*
+     * Map times in the jitter file to times in the timeline table.
+     * If trkflg[j] = BAD_TRKFLG, set the jitter flag in the timeline
+     * status array.
+     */
+    for (j=k=0; k < nsec; k++) {
+	while ((float) time_jit[j+1] < ttime[k] && j+1 < njitr) j++;
+	if (trkflg[j] == BAD_TRKFLG) {
+	    status_flag[k] |= TEMPORAL_JITR;
+	}
+    }
+
+    /* Deallocate storage space */
+    free(time_jit);
+    free(dy_jit);
+    free(trkflg);
+   
+    cf_proc_update(infits, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished processing");
+
+    return (status);
+}
diff --git a/src/libcf/cf_screen_limb_angle.c b/src/libcf/cf_screen_limb_angle.c
new file mode 100644
index 0000000..5e2f54b
--- /dev/null
+++ b/src/libcf/cf_screen_limb_angle.c
@@ -0,0 +1,87 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_screen_limb_angle(fitsfile *infits, long nseconds,
+ *                                   unsigned char *timeline_status,
+ *                                   float *timeline_limb);
+ *
+ * Description: Set the screening bit due to limb angle constraint.
+ *
+ * Arguments:   fitsfile  *infits       Input FITS file pointer
+ *              long      nseconds      Number of points in the timeline table
+ *              unsigned char  *timeline_status   The status flag array
+ * 		float     *timeline_limb The limb angle distance array
+ *
+ * Calls:
+ *
+ * Returns:	0 on success
+ *
+ * History:	10/21/02   1.1   jch    Initial coding
+ * 		12/20/02   1.3   jch    Make sure the flags are unsigned char
+ *              05/20/03   1.4   rdr    Added call to cf_proc_check
+ *              09/10/03   1.5   wvd    Move test of LIMB_SCR to cf_fuv_init.
+ *              07/21/04   1.7   wvd    Delete unused variable limb_cor.
+ *              02/17/05   1.8   wvd    Place parentheses around assignment
+ *                                      used as truth value.
+ *              03/30/05   1.9   wvd    Write BRITLIMB and DARKLIMB keywords
+ *					to IDF file header.
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include <stdio.h>
+#include "calfuse.h"
+
+int
+cf_screen_limb_angle(fitsfile *infits, long nseconds, 
+		unsigned char *timeline_status, float *timeline_limb)
+{
+    char CF_PRGM_ID[] = "cf_screen_limb_angle";
+    char CF_VER_NUM[] = "1.9";
+
+    int	  errflg=0, status=0;
+    long  i;
+    char  file_name[FLEN_VALUE];
+    double angle, britlimb, darklimb;
+    fitsfile  *scrnfits;
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    if ((errflg = cf_proc_check(infits, CF_PRGM_ID))) return errflg;
+
+    /*
+     *  Open the screening parameters file and read the parameters.
+     */
+    FITS_read_key(infits, TSTRING, "SCRN_CAL", file_name, NULL, &status);
+    FITS_open_file(&scrnfits, cf_parm_file(file_name), READONLY, &status);
+
+    FITS_read_key(scrnfits, TDOUBLE, "BRITLIMB", &britlimb, NULL, &status);
+    FITS_read_key(scrnfits, TDOUBLE, "DARKLIMB", &darklimb, NULL, &status);
+    /*
+     *  Write BRITLIMB and DARKLIMB keywords to IDF file header.
+     */
+    FITS_update_key(infits, TDOUBLE, "BRITLIMB", &britlimb, NULL, &status);
+    FITS_update_key(infits, TDOUBLE, "DARKLIMB", &darklimb, NULL, &status);
+    /*
+     *  If the limb angle is less than the limit, set the limb-angle bit.
+     *  Use day or night limit as appropriate.
+     */
+    for (i = 0; i < nseconds; i++) {
+        angle = darklimb;
+        if ((timeline_status[i] & TEMPORAL_DAY) == TEMPORAL_DAY) {
+	    angle = britlimb;
+        }
+        if (timeline_limb[i] < angle) {
+	     timeline_status[i] |= TEMPORAL_LIMB; 
+        }
+    }
+    FITS_close_file(scrnfits, &status);
+    
+    cf_proc_update(infits, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return status;
+}
diff --git a/src/libcf/cf_screen_pulse_height.c b/src/libcf/cf_screen_pulse_height.c
new file mode 100644
index 0000000..3b2c43e
--- /dev/null
+++ b/src/libcf/cf_screen_pulse_height.c
@@ -0,0 +1,79 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_screen_pulse_height(fitsfile *infits, long nevents,
+ *                              unsigned char *photon_ph, 
+ *				unsigned char *photon_locflag);
+ *
+ * Description: Set the screening bit according to PHA limits.
+ *
+ * Arguments:   fitfile  *infits        Input FITS file pointer
+ *              long     nevents        Number of points in the photon list
+ *              unsigned char     *photon_ph     The photon pulse height array
+ *              unsigned char     *photon_locflag The photon location array
+ *
+ * Returns:	0 on success
+ *
+ * History:	11/01/02   1.1   jch    Initial coding
+ * 		12/20/02   1.3   jch    Make sure the flags are "unsigned" char
+ *              02/14/03   1.4   rdr    Update phalow and phahigh keywords
+ *                                       in the IDF
+ *              05/20/03   1.5   rdr    Add call to cf_proc_check
+ *              09/10/03   1.6   wvd    Write NBADPHA as type LONG.
+ *              10/02/03   1.7   wvd    Move PHA bit from TEMPORAL to 
+ *					LOCATION flags.
+ *              05/04/04   1.9   bjg    Cosmetic change to prevent 
+ *                                      compiler warning with gcc -Wall
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include <stdio.h>
+#include "calfuse.h"
+
+int
+cf_screen_pulse_height(fitsfile *infits, long nevents, unsigned char *photon_ph,
+		       unsigned char *photon_locflag)
+{
+    char CF_PRGM_ID[] = "cf_screen_pulse_height";
+    char CF_VER_NUM[] = "1.9";
+
+    char  scrnfile[FLEN_VALUE];
+    unsigned char  phalow, phahigh;
+    int	  errflg=0, status=0;
+    long  i, nbadpha=0;
+    fitsfile *scrnfits;
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    if ((errflg = cf_proc_check(infits, CF_PRGM_ID))) return errflg;
+
+     /*
+     *  Open the screening parameters file and read the parameters.
+     */
+    FITS_read_key(infits, TSTRING, "SCRN_CAL", scrnfile, NULL, &status);
+    FITS_open_file(&scrnfits, cf_parm_file(scrnfile), READONLY, &status);
+    FITS_read_key(scrnfits, TBYTE, "PHALOW", &phalow, NULL, &status);
+    FITS_read_key(scrnfits, TBYTE, "PHAHIGH", &phahigh, NULL, &status);
+    FITS_close_file(scrnfits, &status);
+    /*
+     *  Set the pulse-height bit if pulse height is outside limits.
+     */
+    for (i = 0; i < nevents; i++) {
+	if (photon_ph[i] < phalow || photon_ph[i] > phahigh) {
+	    photon_locflag[i] |= LOCATION_PHA; 
+	    nbadpha++;
+	}
+    }
+    FITS_update_key(infits, TLONG, "NBADPHA", &nbadpha, NULL, &status);
+    FITS_update_key(infits, TBYTE, "PHALOW",  &phalow,  NULL, &status);
+    FITS_update_key(infits, TBYTE, "PHAHIGH", &phahigh, NULL, &status);
+    
+    cf_proc_update(infits, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return status;
+}
diff --git a/src/libcf/cf_screen_saa.c b/src/libcf/cf_screen_saa.c
new file mode 100644
index 0000000..c79dc6e
--- /dev/null
+++ b/src/libcf/cf_screen_saa.c
@@ -0,0 +1,83 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_screen_saa(fitsfile *infits, long nseconds,
+ *                            unsigned char *timeline_status, 
+ *			      float *timeline_long, float *timeline_lat);
+ *
+ * Description: Set the screening bit due to SAA boundary.
+ *
+ * Arguments:   fitsfile  *infits       Input FITS file pointer
+ *              long      nseconds      Number of points in the timeline table
+ *              unsigned char  *timeline_status The status flag array
+ *              float     *timeline_long The longitude array
+ *              float     *timeline_lat  The latitude array
+ *
+ * Calls:	saa
+ *
+ * Returns:	0 on success
+ *
+ * History:	10/29/02   1.1   jch    Initial coding
+ * 		12/20/02   1.3   jch    Include reading SAA table here
+ * 		12/20/02   1.4   wvd    Delete call to calfuse.h 
+ *              05/20/03   1.5   rdr    Add call to cf_proc_check
+ *              08/28/03   1.6   bjg    New definition of structure saareg
+ * 		09/02/03   1.7   wvd    Change calfusettag.h to calfuse.h
+ * 		09/10/03   1.8   wvd    Tidy up code.
+ *              02/17/05   1.9   wvd    Place parentheses around assignment
+ *                                      used as truth value.
+ *
+ ****************************************************************************/
+
+#include <stdlib.h>
+
+#include "calfuse.h"
+
+int
+cf_screen_saa(fitsfile *infits, long nseconds, unsigned char *timeline_status,
+	      float *timeline_long, float *timeline_lat)
+{
+    char CF_PRGM_ID[] = "cf_screen_saa";
+    char CF_VER_NUM[] = "1.9";
+
+    char  saa_cal[FLEN_VALUE];
+    int   errflg=0, status=0, hdutype;
+    long  i;
+    saareg saa_bounds;
+    fitsfile *saafits;
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+    if ((errflg = cf_proc_check(infits, CF_PRGM_ID))) return errflg;
+
+    /*
+     *  Read SAA boundaries from the specified calibration file.
+     */
+    FITS_read_key(infits, TSTRING, "SAAC_CAL", saa_cal, NULL, &status);
+    FITS_open_file(&saafits, cf_cal_file(saa_cal), READONLY, &status);
+    FITS_movabs_hdu(saafits, 2, &hdutype, &status);
+
+    saa_bounds.n_points =
+	   cf_read_col(saafits, TFLOAT, "LATITUDE",  (void **) &(saa_bounds.lat));
+    (void) cf_read_col(saafits, TFLOAT, "LONGITUDE", (void **) &(saa_bounds.lon));
+    
+    fits_close_file(saafits, &status);
+
+    /*
+     *  Set the SAA boundary bit if in SAA
+     */
+    for (i = 0; i < nseconds; i++) {
+	if (saa(&saa_bounds, (double)timeline_long[i], (double)timeline_lat[i])) {
+	    timeline_status[i] |= TEMPORAL_SAA; 
+	}
+    }
+    free(saa_bounds.lon);
+    free(saa_bounds.lat);
+
+    cf_proc_update(infits, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return status;
+}
diff --git a/src/libcf/cf_set_good_time_intervals.c b/src/libcf/cf_set_good_time_intervals.c
new file mode 100644
index 0000000..2ed0d54
--- /dev/null
+++ b/src/libcf/cf_set_good_time_intervals.c
@@ -0,0 +1,157 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_set_good_time_intervals(fitsfile *infits, long nseconds,
+ *                          float *timeline_time, 
+ *			    unsigned char *timeline_status, GTI *gti);
+ *
+ * Description: Compute the new good time intervals based on the timeline 
+ *              status flag.
+ *
+ * Arguments:   fitsfile   *infits        	Input FITS file pointer
+ *              long       nseconds       	Length of timeline table
+ *              float      *timeline_time 	Time array of timeline list
+ *     	   unsigned char   *timeline_status    	Status array of timeline list
+ *              GIT        *gti           	Good time interval(s)
+ *
+ * Calls:
+ *
+ * Returns:     0 on success
+ *              -1 on error
+ *
+ * History:     11/01/02   1.1   jch    Initial coding
+ * 		12/20/02   1.3   jch    Make sure that flags are unsigned char
+ *		05/09/03   1.4   wvd	Include D/N screening in GTI's.
+ *					Calculate EXPTIME as SUM (GTI's).
+ *					Update header keyword EXPTIME.
+ *              05/20/03   1.5   rdr    Add call to cf_proc_check
+ *              05/29/03   1.6   wvd    Allow lower-case value of DAYNIGHT.
+ *					Correct bug in calculation of gti.stop 
+ *					If in HIST mode, ignore LIMB, SAA,
+ *					and BRST flags.
+ *              09/10/03   1.7   wvd    Change calfusettag.h to calfuse.h
+ *              10/13/03   1.8   wvd    Modify for new timeline table format.
+ *					No time skips.
+ *              04/20/04   1.9   bjg    Remove unused variables
+ *              12/01/04   1.10  bjg    Set gti start and stop to zero 
+ *                                      for the single GTI when there are no
+ *                                      Good Times.
+ *              08/23/07   1.11  wvd    Change malloc to cf_malloc.
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include "calfuse.h"
+
+int
+cf_set_good_time_intervals(fitsfile *infits, long nseconds,
+	float *timeline_time, unsigned char *timeline_status, GTI *gti)
+{
+    char CF_PRGM_ID[] = "cf_set_good_time_intervals";
+    char CF_VER_NUM[] = "1.11";
+
+    char   daynight[FLEN_VALUE], instmode[FLEN_VALUE];
+    int	   in_bad;  		   /* True between good-time intervals */
+    int    day=FALSE, night=FALSE, errflg=0, status=0;
+    long   j, jj;
+    float  exptime=0.;
+    double last_good_time=-99;
+    unsigned char TEMPORAL_MASK;
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    if ((errflg = cf_proc_check(infits, CF_PRGM_ID) )) return errflg;
+
+    /* Read and interpret DAYNIGHT keyword. */
+
+    FITS_read_key(infits, TSTRING, "DAYNIGHT", daynight, NULL, &status);
+    if (!strncmp(daynight, "D", 1) || !strncmp(daynight, "d", 1)) {
+        day = TRUE;
+    }
+    else if (!strncmp(daynight, "N", 1) || !strncmp(daynight, "n", 1)) {
+        night = TRUE;
+    }
+    else if (!strncmp(daynight, "B", 1) || !strncmp(daynight, "b", 1)) {
+        day = night = TRUE;
+    }
+    else
+        cf_if_error("Unknown DAYNIGHT keyword value: %s", daynight);
+    cf_verbose(3, "DAYNIGHT flag set to %s", daynight);
+
+    /* 
+     *  Read INSTMODE keyword.  If in HIST mode, mask out
+     *  LIMB, SAA, and BRST flags.  TEMPORAL_DAY is the default.
+     */
+    TEMPORAL_MASK = TEMPORAL_DAY;
+    FITS_read_key(infits, TSTRING, "INSTMODE", instmode, NULL, &status);
+    if (!strncmp(instmode, "HIST", 4)) {
+	TEMPORAL_MASK |= TEMPORAL_LIMB;
+	TEMPORAL_MASK |= TEMPORAL_SAA;
+	TEMPORAL_MASK |= TEMPORAL_BRST;
+    }
+
+    /*
+     *  Determine limits of good-time intervals.
+     */
+    gti->start = (double *) cf_malloc(sizeof(double)*nseconds);
+    gti->stop  = (double *) cf_malloc(sizeof(double)*nseconds);
+
+    in_bad = TRUE;
+    jj = -1;
+    for (j = 0; j < nseconds; j++) {
+        /*
+         *  If we are in a good time interval and were in a bad one,
+	 *  increment jj and set gti->start.
+         */
+        if (!(timeline_status[j] & ~TEMPORAL_MASK) &&
+            ((day   && (timeline_status[j] & TEMPORAL_DAY)) ||
+             (night && (timeline_status[j] ^ TEMPORAL_DAY)))) {
+	    if (in_bad) {
+		jj++;
+		gti->start[jj] = timeline_time[j];
+		in_bad = FALSE;
+	    }
+        /*
+         *  If we are in a good time interval and were in a good one,
+	 *  update last_good_time.
+         */
+	    last_good_time = timeline_time[j];
+	}
+        /*
+         *  If we are in a bad time interval and were in a good one,
+	 *  set in_bad to TRUE and update gti->stop.
+         */
+	else if (in_bad == FALSE) {
+	    gti->stop[jj] = timeline_time[j];
+	    in_bad = TRUE;
+	}
+    }
+    gti->ntimes = jj + 1;
+
+    /* If the entire exposure is bad, return a zero-length GTI. */
+    if (gti->ntimes == 0) {
+	gti->ntimes = 1;
+	gti->start[0] = gti->stop[0] = 0;
+    }
+
+    /* Calculate total exposure time and write it to file header */
+    for (j = 0; j < gti->ntimes; j++)
+	exptime += gti->stop[j] - gti->start[j];
+    FITS_update_key(infits, TFLOAT, "EXPTIME", &exptime, NULL, &status);
+
+    /* Results to trailer file. */
+    cf_verbose(2, "GTI's:\t START\t  STOP");
+    for (j = 0; j < gti->ntimes; j++)
+        cf_verbose(2, "%3d\t%6.0f\t%6.0f", j, gti->start[j], gti->stop[j]);
+    cf_verbose(2, "Total EXPTIME = %6.0f", exptime);
+
+    cf_proc_update(infits, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return status;
+}
diff --git a/src/libcf/cf_set_photon_flags.c b/src/libcf/cf_set_photon_flags.c
new file mode 100644
index 0000000..de2b623
--- /dev/null
+++ b/src/libcf/cf_set_photon_flags.c
@@ -0,0 +1,425 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_set_photon_flags(fitsfile *infits, long nevents,
+ *                                  float *photon_time, 
+ *				    float *photon_weight,
+ *				    unsigned char *photon_status,
+ *				    unsigned char *photon_locflag,
+ *                                  long nseconds, float *timeline_time,
+ *                                  unsigned char *timeline_status);
+ *
+ * Description: Copy status flags from the timeline table to the photon list.
+ *		Update header keywords.
+ *
+ *		For histogram data, we set only the DAY flag.
+ *		Other situations are treated as follows:
+ *
+ *		DAY      All photons flagged if exposure >10% day
+ *
+ *		LIMB     True for all if true for one.
+ *		SAA      Do not flag photons or modify EXPTIME.
+ *		BRST     Instead, set header keyword EXP_STAT.
+ *			 Ignore all violations during the 
+ *			 first and last 20 seconds of an exposure.
+ *
+ *		HV	 Modify EXPTIME, but do not flag photons.
+ *		JITR     Ditto.
+ *
+ *		OPUS     Ignore for now.
+ *		USER	 Ignore for now.
+ *
+ * Arguments:   fitsfile *infits        Input FITS file pointer
+ *              long     nevents        Number of points in the photon list
+ *              float    *photon_time	Time array of photon events
+ *              float    *photon_weight Scale factor for each photon
+ *              unsigned char  *photon_status	Status flags for photon events
+ *              unsigned char  *photon_locflag  Location flags for photon events
+ *              long     nseconds       Number of points in the timeline table
+ *              float    *timeline_time Time array of timeline list
+ *              unsigned char  *timeline_status Status flags for timeline list
+ *
+ * Calls:
+ *
+ * Returns:	0 on success
+ *
+ * History:	10/31/02   1.1   jch    Initial coding
+ * 		12/20/02   1.3   jch    Make sure the flags are "unsigned" char
+ *		05/09/03   1.4   wvd	Change EXP* keywords to type long.
+ *					Consider DAYNIGHT keyword in evaluation
+ *					of NBADEVNT and EXP_BAD.
+ *					Use frame_tolerance in time comparison.
+ *					Use photon_locflag in counting NBADEVNT
+ *               05/20/03  1.5   rdr    Add call to cf_proc_check
+ *               05/29/03  1.6   wvd    Modify to handle HIST data:
+ *					Use single flag for all photon events.
+ *					Ignore LIMB, SAA, and BRST flags when
+ *					counting EXP_BAD.  Scale NBADEVNT by
+ *					photon_weight[i]/TOT_DEAD.
+ *               06/02/03  1.7   wvd    Properly deal with GTI's.
+ *               07/14/03  1.8   wvd    Read DAYNIGHT from SCRN_CAL and 
+ *					populate IDF header keyword.
+ *					Use FRAME_TOLERANCE from calfuse.h.
+ *               09/15/03  1.9   wvd    Copy flags only to photons whose times
+ *					are within 1s of timeline table time.
+ *               10/02/03  1.10  wvd    Change timeline table: no breaks in
+ *					time; add TEMPORAL_OPUS flag.
+ *               10/13/03  1.11  wvd    Use same scheme for calculating
+ *					EXP_BAD and exp_screen.
+ *               04/20/04  1.12  bjg    Cosmetic change to prevent 
+ *                                      compiler warning with gcc -Wall 
+ *               05/20/04  1.13  wvd	Don't flag HIST photons as bad
+ *					when HV or JITR are bad.
+ *					We'll reduce EXPTIME instead.
+ *               06/01/04  1.14  wvd	For HIST data, set only DAY flag.
+ *					Write other flags to EXP_STAT keyword.
+ *               06/28/04  1.15  wvd	If > 90% of exposure is lost to a
+ *					burst, jitter, etc., write cause to
+ *					trailer file.
+ *               03/24/05  1.16  wvd	If EXP_STAT != 0, don't change it.
+ *               01/01/07  1.17  wvd	Remove mention of FIFO flag.
+ *               07/18/08  1.18  wvd	If EXP_STAT = 2, target is bright
+ *					earth or airglow. Set limb-angle 
+ *					flags to zero.
+ *               08/22/08  1.19  wvd	Compare EXP_STAT to TEMPORAL_LIMB, 
+ *					rather than a particular value.
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include <stdio.h>
+#include "calfuse.h"
+
+#define HIST_PAD 20	/* Ignore first and last 20 s of each exposure. */
+
+/*
+ *  Compute integration time lost to a particular screening step.
+ *  Ignore times outside of OPUS-defined good-time intervals.
+ */
+static long
+time_loss(long nseconds, unsigned char *timeline_status,
+	unsigned char criterion)
+{
+    long exp_screen = 0, j;
+
+    for (j = 0; j < nseconds; j++) {
+	if (timeline_status[j] & TEMPORAL_OPUS) continue;
+	if (timeline_status[j] & criterion) exp_screen++;
+    }
+
+    return(exp_screen);
+}
+
+
+/*
+ *  Compute integration time lost to a particular screening step,
+ *  but ignore first and last HIST_PAD seconds of exposure.
+ */
+static long
+time_loss_pad(long nseconds, unsigned char *timeline_status,
+	unsigned char criterion)
+{
+    long exp_screen = 0, j;
+
+    for (j = HIST_PAD; j < nseconds - HIST_PAD; j++) {
+	if (timeline_status[j] & TEMPORAL_OPUS) continue;
+	if (timeline_status[j] & criterion) exp_screen++;
+    }
+    return (exp_screen);
+}
+
+
+/*
+ *  In HIST mode, generate a status flag good for all photons.
+ *  Except for D/N flag, we ignore first and last 20 seconds of exposure.
+ *  D/N flag is written to TEMPORAL_MASK.
+ *  LIMB/SAA/BRST flags are written to EXP_STAT.
+ */
+static void
+generate_temporal_mask(float rawtime, long nseconds, float *timeline_time,
+	unsigned char *timeline_status, unsigned char *TEMPORAL_MASK,
+	unsigned char *EXP_STAT, char *comment)
+{
+    long exp_day;
+
+    *EXP_STAT = *TEMPORAL_MASK = 0;
+
+   /*
+    *  Day if exp_day > 10% of total exposure time.
+    */
+    exp_day=time_loss(nseconds, timeline_status, TEMPORAL_DAY);
+    if (exp_day * 10 > rawtime) {
+	*TEMPORAL_MASK = TEMPORAL_DAY;
+	sprintf(comment, "Exposure more than 10 percent day");
+	cf_verbose(1, comment);
+    }
+   /*
+    * If exposure is less than 40 seconds long, we're done.
+    */
+    if (rawtime < 2. * HIST_PAD) return;
+
+   /*
+    * Are there limb-angle violations?
+    */
+    if (time_loss_pad(nseconds, timeline_status, TEMPORAL_LIMB)) {
+    	*EXP_STAT |= TEMPORAL_LIMB;
+	sprintf(comment, "Data suspect: Limb-angle violation");
+	cf_verbose(1, comment);
+    }
+   /*
+    * Do we ever enter the SAA?
+    */
+    if (time_loss_pad(nseconds, timeline_status, TEMPORAL_SAA)) {
+	*EXP_STAT |= TEMPORAL_SAA;
+	sprintf(comment, "Data suspect: SAA violation");
+	cf_verbose(1, comment);
+    }
+   /*
+    * Are there any bursts?
+    */
+    if (time_loss_pad(nseconds, timeline_status, TEMPORAL_BRST)) {
+	*EXP_STAT |= TEMPORAL_BRST;
+	sprintf(comment, "Data suspect: Burst detected");
+	cf_verbose(1, comment);
+    }
+
+   /*
+    * Is the detector voltage ever too low?
+    * If so, just issue a warning; we'll modify the exposure time later.
+    */
+    if (time_loss_pad(nseconds, timeline_status, TEMPORAL_HV))
+        cf_verbose(1, "EXPTIME modified: Detector voltage low.");
+   /*
+    * Was any time rejected by the jitter routine?
+    * If so, just issue a warning; we'll modify the exposure time later.
+    */
+    if (time_loss_pad(nseconds, timeline_status, TEMPORAL_JITR))
+        cf_verbose(1, "EXPTIME modified: Target out of aperture.");
+
+    return;
+}
+
+
+int
+cf_set_photon_flags(fitsfile *infits, long nevents, float *photon_time,
+	    float *photon_weight, unsigned char *photon_status,
+	    unsigned char *photon_locflag, long nseconds,
+	    float *timeline_time, unsigned char *timeline_status)
+{
+    char CF_PRGM_ID[] = "cf_set_photon_flags";
+    char CF_VER_NUM[] = "1.19";
+
+    char  comment[FLEN_COMMENT], daynight[FLEN_KEYWORD]; 
+    char  instmode[FLEN_KEYWORD], scrnfile[FLEN_KEYWORD];
+    long  i, j, k;
+
+    long nbadevnt=0;	/* number of events deleted in screening */
+    long exp_bad=0;	/* integration time lost to screening */
+    long exp_brst=0;	/* integration time lost to event bursts */
+    long exp_hv=0;	/* integration time lost to low detector voltage */
+    long exp_jitr=0;	/* integration time lost to jitter */
+    long exp_limb=0;	/* integration time with low limb angle */
+    long exp_saa=0;	/* integration time while in SAA */
+    long exp_day=0;	/* integration time during day after screening */
+    long expnight=0;	/* integration time during night after screening */
+    int  day = FALSE, night = FALSE;
+    int  errflg = 0;	/* value returned by cf_proc_check */
+    int	 status = 0;	/* CFITSIO status */
+    int  expstat;	/* initial value of EXP_STAT keyword */
+    float deadtime, rawtime;
+    fitsfile *scrnfits;
+    unsigned char EXP_STAT, TEMPORAL_MASK;
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    if ((errflg = cf_proc_check(infits, CF_PRGM_ID) )) return errflg;
+
+    /* Read and interpret DAYNIGHT keyword. Copy to IDF header. */
+
+    FITS_read_key(infits, TSTRING, "SCRN_CAL", scrnfile, NULL, &status);
+    FITS_open_file(&scrnfits, cf_parm_file(scrnfile), READONLY, &status);
+    FITS_read_key(scrnfits, TSTRING, "DAYNIGHT", daynight, NULL, &status);
+    FITS_close_file(scrnfits, &status);
+
+    if (!strncmp(daynight, "D", 1) || !strncmp(daynight, "d", 1)) {
+        day = TRUE;
+    }
+    else if (!strncmp(daynight, "N", 1) || !strncmp(daynight, "n", 1)) {
+        night = TRUE;
+    }
+    else if (!strncmp(daynight, "B", 1) || !strncmp(daynight, "b", 1)) {
+        day = night = TRUE;
+    }
+    else
+        cf_if_error("Unknown DAYNIGHT keyword value: %s", daynight);
+
+    /*
+     *  Read EXP_STAT, RAWTIME, INSTMODE and TOT_DEAD keywords.
+     */
+    FITS_read_key(infits, TINT, "EXP_STAT", &expstat, NULL, &status);
+    FITS_read_key(infits, TFLOAT, "RAWTIME", &rawtime, NULL, &status);
+    FITS_read_key(infits, TSTRING, "INSTMODE", instmode, NULL, &status);
+    FITS_read_key(infits, TFLOAT, "TOT_DEAD", &deadtime, NULL, &status);
+
+    /*
+     *  If EXP_STAT = TEMPORAL_LIMB, target is bright earth or airglow.  
+     *  Compute EXP_LIMB, then set limb-angle flags to 0.
+     */
+    exp_limb=time_loss(nseconds, timeline_status, TEMPORAL_LIMB);
+    if (expstat == (int) TEMPORAL_LIMB) 
+	for (i = 0; i < nseconds-1; i++) 
+	    timeline_status[i] &= ~TEMPORAL_LIMB;
+
+    /*
+     *  If in HIST mode:
+     *  Generate TEMPORAL_MASK
+     *  Copy status flags from TEMPORAL_MASK to photon list.
+     *  Count bad photons.
+     */
+    if (!strncmp(instmode, "HIST", 4)) {
+	generate_temporal_mask(rawtime, nseconds, timeline_time,
+		timeline_status, &TEMPORAL_MASK, &EXP_STAT, comment);
+	for (i = 0; i < nevents; i++) {
+            photon_status[i] = TEMPORAL_MASK;
+           /*
+            *  A bad photon is one for which
+            *  - something other than AIRGLOW is wrong; or
+            *  - you don't want day, but this one is; or
+            *  - you don't want night, but this one is.
+            */
+            if ((photon_locflag[i] & ~LOCATION_AIR) ||
+                (!day   && (photon_status[i] & TEMPORAL_DAY)) ||
+                (!night && (photon_status[i] ^ TEMPORAL_DAY)))
+                nbadevnt += (long)(photon_weight[i]/deadtime + 0.5);
+        }
+	if (EXP_STAT && !expstat)
+	    FITS_update_key(infits, TBYTE, "EXP_STAT", &EXP_STAT,
+	    comment, &status);
+    }
+
+    /* 
+     *  If in TTAG mode:
+     *  Copy status flags from timeline table to photon list.
+     *  Confirm that photon time is included in timeline table.
+     *  Count bad photons.
+     */
+     else {
+	for (i = k = 0; i < nevents; i++) {
+            while (photon_time[i] > timeline_time[k+1]-FRAME_TOLERANCE &&
+		k < nseconds-1) { k++; }
+
+            if (photon_time[i] - timeline_time[k] < 2.0)
+            	photon_status[i] = timeline_status[k];
+	    else
+		cf_if_warning("Time %g not included in timeline table",
+		    photon_time[i]);
+
+           /*
+            *  A bad photon is one for which 
+	    *  - something other than DAYNIGHT is wrong; or
+	    *  - something other than AIRGLOW is wrong; or
+	    *  - you don't want day, but this one is; or
+	    *  - you don't want night, but this one is.
+            */
+            if ((photon_status[i] & ~TEMPORAL_DAY) ||
+	        (photon_locflag[i] & ~LOCATION_AIR) ||
+                (!day   && (photon_status[i] & TEMPORAL_DAY)) ||
+                (!night && (photon_status[i] ^ TEMPORAL_DAY)))
+	        nbadevnt++;
+	}
+     }
+
+    /*
+     *  Now count day, night, and bad seconds.
+     *  If in HIST mode, mask out LIMB, SAA, and BRST flags.
+     *  Exclude OPUS-defined bad times.
+     */
+    TEMPORAL_MASK = TEMPORAL_DAY;
+
+    if (!strncmp(instmode, "HIST", 4)) {
+        TEMPORAL_MASK |= TEMPORAL_LIMB;
+        TEMPORAL_MASK |= TEMPORAL_SAA;
+        TEMPORAL_MASK |= TEMPORAL_BRST;
+    }
+
+    for (j = 0; j < nseconds; j++) {
+	if (timeline_status[j] & TEMPORAL_OPUS)
+		continue;
+	if (timeline_status[j] & ~TEMPORAL_MASK)
+		exp_bad++;
+	else if (timeline_status[j] & TEMPORAL_DAY)
+		exp_day++;
+	else
+		expnight++;
+    }
+    /* 
+     *  If user rejects either day or night data, add to EXP_BAD.
+     *  If user rejects night data, set EXPNIGHT = 0.
+     */
+     if (!day) {
+	exp_bad += exp_day;
+     }
+     if (!night) {
+	exp_bad += expnight;
+	expnight = 0;
+     }
+
+    /* 
+     *  Compute EXP_BRST 
+     */
+    exp_brst=time_loss(nseconds, timeline_status, TEMPORAL_BRST);
+    /* 
+     *  Compute EXP_HV
+     */
+    exp_hv=time_loss(nseconds, timeline_status, TEMPORAL_HV);
+    /* 
+     *  Compute EXP_JITR 
+     */
+    exp_jitr=time_loss(nseconds, timeline_status, TEMPORAL_JITR);
+    /* 
+     *  Compute EXP_LIMB	(already done)
+	exp_limb=time_loss(nseconds, timeline_status, TEMPORAL_LIMB);
+     */
+    /*
+     *  Compute EXP_SAA 
+     */
+    exp_saa=time_loss(nseconds, timeline_status, TEMPORAL_SAA);
+
+    /*
+     *  If data are in time-tag mode and more than 90% of time was
+     *  was rejected by screening, say why. 
+     */
+    if (!strncmp(instmode, "TTAG", 4)) {
+	if (exp_brst > 0.9 * rawtime)
+	    cf_verbose(1, "%d sec lost to bursts.", exp_brst);
+	if (exp_hv > 0.9 * rawtime)
+	    cf_verbose(1, "%d sec lost to low voltage.", exp_hv);
+	if (exp_jitr > 0.9 * rawtime)
+	    cf_verbose(1, "%d sec lost to jitter.", exp_jitr);
+	if (exp_limb > 0.9 * rawtime)
+	    cf_verbose(1, "%d sec lost to low limb angle.", exp_limb);
+	if (exp_saa > 0.9 * rawtime)
+	    cf_verbose(1, "%d sec lost to SAA.", exp_saa);
+    }
+
+    /* 
+     *  Update the header keywords 
+     */
+    FITS_update_key(infits, TLONG, "NBADEVNT", &nbadevnt, NULL, &status);
+    FITS_update_key(infits, TLONG, "EXP_BAD",  &exp_bad,  NULL, &status);
+    FITS_update_key(infits, TLONG, "EXP_BRST", &exp_brst, NULL, &status);
+    FITS_update_key(infits, TLONG, "EXP_HV",   &exp_hv,   NULL, &status);
+    FITS_update_key(infits, TLONG, "EXP_JITR", &exp_jitr, NULL, &status);
+    FITS_update_key(infits, TLONG, "EXP_LIM",  &exp_limb, NULL, &status);
+    FITS_update_key(infits, TLONG, "EXP_SAA",  &exp_saa,  NULL, &status);
+    FITS_update_key(infits, TLONG, "EXPNIGHT", &expnight, NULL, &status);
+    FITS_update_key(infits, TSTRING, "DAYNIGHT", &daynight, NULL, &status);
+
+    cf_proc_update(infits, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return status;
+}
diff --git a/src/libcf/cf_set_user_gtis.c b/src/libcf/cf_set_user_gtis.c
new file mode 100644
index 0000000..54a88d5
--- /dev/null
+++ b/src/libcf/cf_set_user_gtis.c
@@ -0,0 +1,100 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_set_user_gtis(fitsfile *infits, long nseconds,
+ *                                  float *timeline_times,
+ *                                  unsigned char *timeline_status);
+ *
+ * Description: Apply user-defined good time intervals to timeline table.
+ *
+ * Arguments:   fitsfile  *infits       Input FITS file pointer
+ *              long      nseconds      Number of points in the timeline table
+ * 		float     *timeline_times Array of times
+ *              unsigned char  *timeline_status   The status flag array
+ *
+ * Calls:
+ *
+ * Returns:	0 on success
+ *
+ * History:	09.10.03   1.1   bjg    Initial coding
+ * 		
+ *              09.12.03   1.2   bjg    Bug fix. When nusergti was zero or less
+ *                                      this function set all the photons to 
+ *                                      bad. Now it doesn't change anything.
+ *              04.20.04   1.3   bjg    Remove unused variables
+ *                                      Change format to match arg type in
+ *                                      sprintf.
+ *
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include <stdio.h>
+#include "calfuse.h"
+
+int
+cf_set_user_gtis(fitsfile *infits, long nseconds, 
+	 float *timeline_times,	unsigned char *timeline_status)
+{
+    char CF_PRGM_ID[] = "cf_set_user_gtis";
+    char CF_VER_NUM[] = "1.3";
+
+    int	  errflg=0, status=0, nusergti;
+    long  i,n;
+    char  file_name[FLEN_VALUE];
+    float limit1,limit2;
+    char keywd1[FLEN_KEYWORD],keywd2[FLEN_KEYWORD];
+    fitsfile  *scrnfits;
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    if ((errflg = cf_proc_check(infits, CF_PRGM_ID) )) return errflg;
+
+    /*
+     *  Open the screening parameters file and read the good time intervals.
+     */
+    FITS_read_key(infits, TSTRING, "SCRN_CAL", file_name, NULL, &status);
+    FITS_open_file(&scrnfits, cf_parm_file(file_name), READONLY, &status);
+
+    FITS_read_key(scrnfits, TINT, "NUSERGTI", &nusergti, NULL, &status);
+    
+    if (nusergti>0){
+    
+        i=0;
+    
+        for (n=1;n<=nusergti;n++){
+           sprintf(keywd1, "GTIBEG%02ld",n);
+           FITS_read_key(scrnfits, TFLOAT, keywd1, &limit1, NULL, &status);
+           sprintf(keywd2, "GTIEND%02ld",n);
+           FITS_read_key(scrnfits, TFLOAT, keywd2, &limit2, NULL, &status);
+        
+        
+           while ((i<nseconds)&&(timeline_times[i]<limit1)) {
+              timeline_status[i] |= TEMPORAL_USER;
+              i++;
+           }
+        
+           while ((i<nseconds)&&(timeline_times[i]<limit2)) {
+              i++;
+           }
+    
+        }
+
+
+        while (i<nseconds){
+             timeline_status[i] |= TEMPORAL_USER;
+             i++;
+        }
+    
+    }
+    
+    FITS_close_file(scrnfits, &status);
+    
+    cf_proc_update(infits, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return status;
+}
diff --git a/src/libcf/cf_source_aper.c b/src/libcf/cf_source_aper.c
new file mode 100644
index 0000000..3b1cb60
--- /dev/null
+++ b/src/libcf/cf_source_aper.c
@@ -0,0 +1,67 @@
+/**************************************************************************
+ *           Johns Hopkins University
+ *           Center for Astrophysical Sciences
+ *           FUSE
+ *************************************************************************
+ *
+ * Synopsis:    cf_source_aper(infits, ap)
+ *
+ * Description: Procedure to determine which aperture contains the source
+ *
+ * Arguments :  fitsfile     infits     Pointer to Integmediate Data File
+ *              int          *ap        Array containing the two active
+ *                                      apertures
+ *
+ * Returns      int          srctype    Type of source in aperture
+ *
+ * HISTORY      12/12/02  v1.1   rdr    First delivery
+ *              12/13/02  v1.3   wvd    Changed file name
+ *              02/24/03  v1.4   peb    Changed include file to calfitsio.h
+ *		04/17/03  v1.5   wvd	Change to cf_source_aper throughout.
+ *              07/11/03  v1.6   rdr    Change so that src_type returns
+ *                                      1 rather than 3 for extended source
+ *		08/21/03  v1.7   wvd	If APERTURE=RFPT, treat as LWRS.
+ *              04/09/04  v1.8   bjg    Include string.h
+ *                                      Remove unused variables
+ *
+ ************************************************************************/
+
+#include "calfuse.h"
+#include <string.h>
+
+int
+cf_source_aper(fitsfile *infits, int *active_ap )
+{
+     /* char CF_PRGM_ID[] = "cf_source_aper";         */
+     /* char CF_VER_NUM[] = "1.8";                    */
+
+    char aper[FLEN_CARD], src[FLEN_CARD];
+    int status=0, hdutype, src_type;
+
+    /* Determine the active aperture */
+    FITS_movabs_hdu(infits, 1, &hdutype, &status); 
+    FITS_read_key(infits, TSTRING, "APERTURE", aper, NULL, &status);
+ 
+    /* Specify the channels of the active aperture */
+    if (!strncmp(aper,"HIRS",4)) {
+	active_ap[0] = 1;
+	active_ap[1] = 5; }
+    else if (!strncmp(aper,"MDRS",4)) {
+	active_ap[0] = 2;
+	active_ap[1] = 6; }
+    else if (!strncmp(aper,"LWRS",4) || !strncmp(aper,"RFPT",4)) {
+	active_ap[0] = 3;
+	active_ap[1] = 7;
+    }
+    else
+	cf_if_error("APERTURE keyword corrupted.");
+    cf_verbose(3, "APERTURE = %s, channels are %d and %d",
+		aper, active_ap[0], active_ap[1]);
+
+    FITS_read_key(infits, TSTRING,"SRC_TYPE", src, NULL, &status);
+    src_type = 0;
+    if (!strncmp(src,"E",1) || !strncmp(src,"e",1) ) src_type = 1;
+
+    cf_verbose(3, "SRC_TYPE = %s, source type = %d", src, src_type);
+    return src_type;
+}
diff --git a/src/libcf/cf_standard_or_optimal_extraction.c b/src/libcf/cf_standard_or_optimal_extraction.c
new file mode 100644
index 0000000..2b2a6fa
--- /dev/null
+++ b/src/libcf/cf_standard_or_optimal_extraction.c
@@ -0,0 +1,75 @@
+/*****************************************************************************
+ *            Johns Hopkins University
+ *            Center For Astrophysical Sciences
+ *            FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_standard_or_optimal_extraction (fitsfile *header,
+ *			int *optimal)
+ *
+ * Description: Sets optimal to TRUE if optimal extraction is desired.
+ *		FALSE if RUN_OPTI = 'NO' in parm*.fit file.
+ *		FALSE if SRC_TYPE[0] = 'E' in file header.
+ *
+ * Arguments:   fitsfile  *header       Pointer to IDF FITS file header
+ *              int       *optimal      TRUE if optimal extraction desired
+ *
+ * Calls:
+ *
+ * Returns:     0 on success
+ *
+ * History:     03/02/03  1.1   wvd	Initial coding.
+ *		03/12/03  1.2   wvd	Write value of optimal to trailer file.
+ *		03/19/03  1.3   wvd	Read SRC_TYPE, not SP_TYPE.
+ *		03/19/03  1.4   wvd	Add call to cf_timestamp at start.	
+ *					Change printf to cf_verbose
+ *		09/30/03  1.5   wvd	Check for lower-case value of
+ *					RUN_OPTI.
+ *		03/15/05  1.6   wvd	No optimal extraction for HIST targets
+ *					unless try_optimal = TRUE;
+ *		03/18/05  1.7   wvd	v1.6 was a bad idea.  Returning to v1.5
+ *
+ ****************************************************************************/
+
+#include <stdio.h>
+#include "calfuse.h"
+
+static char CF_PRGM_ID[] = "cf_standard_or_optimal_extraction";
+static char CF_VER_NUM[] = "1.7";
+
+int
+cf_standard_or_optimal_extraction(fitsfile *header, int *optimal)
+{
+    char  parm_file[FLEN_VALUE], instmode[FLEN_VALUE];
+    char  run_opti[FLEN_VALUE], src_type[FLEN_VALUE];
+    int   status=0;
+    fitsfile *parmfits;
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin processing");
+
+    /* Read SRC_TYPE from IDF header. */
+    FITS_read_key(header, TSTRING, "SRC_TYPE", src_type, NULL, &status);
+    FITS_read_key(header, TSTRING, "INSTMODE", instmode, NULL, &status);
+
+    /* Read RUN_OPTI from PARM_CAL. */
+    FITS_read_key(header, TSTRING, "PARM_CAL", parm_file, NULL, &status);
+    FITS_open_file(&parmfits, cf_parm_file(parm_file), READONLY, &status);
+    FITS_read_key(parmfits, TSTRING, "RUN_OPTI", run_opti, NULL, &status);
+    FITS_close_file(parmfits, &status);
+
+    /* Determine value of optimal. */
+    *optimal = TRUE;
+    if (*run_opti != 'Y' && *run_opti != 'y') {
+	cf_verbose (1, "RUN_OPTI = %s.  No optimal extraction.", run_opti);
+	*optimal = FALSE;
+    }
+    if (*src_type != 'P') {
+	cf_verbose (1, "SRC_TYPE = %s.  No optimal extraction.", src_type);
+	*optimal = FALSE;
+    }
+    if (*optimal) cf_verbose (1, "Attempting optimal extraction.");
+
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return status;
+}
diff --git a/src/libcf/cf_target_count_rate.c b/src/libcf/cf_target_count_rate.c
new file mode 100644
index 0000000..eab5b26
--- /dev/null
+++ b/src/libcf/cf_target_count_rate.c
@@ -0,0 +1,112 @@
+/**************************************************************************
+ *           Johns Hopkins University
+ *           Center for Astrophysical Sciences
+ *           FUSE
+ *************************************************************************
+ *
+ * Synopsis:    cf_target_count_rate(header, nevents, ptime, weight,
+ *              channel, locflags, ntimes, ttime, rate_lif, rate_sic)
+ *
+ * Description: Determines the count rate in the target aperture for both
+ *		LiF and SiC channels.  Excludes airglow lines.
+ *
+ * Arguments:   fitsfile  *header :   pointer to IDF header
+ *              long      nevents :   number of photon events in the file
+ *              float     *ptime  :   detection time for each photon
+ *              float     *weight :   weight associated with each photon
+ *     unsigned char      *channel:   aperture associated with each photon
+ *     unsigned char     *locflags:   location flag array - flags the 
+ *                                    geocoronal photons
+ *              long      ntimes    :   number of seconds tabulated in timeline
+ *              float     *ttime  :   tabulated times in the timeline
+ *              float	*rate_lif, *rate_sic :
+ *                                    count rates through the Lif and SiC
+ *				      apertures, excluding geocoronal emission
+ *
+ * Calibration files required:     None
+ *
+ * Returns:	0 on success
+ *
+ *                                
+ * HISTORY:     03/03/03    v1.1   RDR    started work
+ *		03/05/03    v1.2   wvd    change name of subroutine & install
+ *              03/10/03    v1.21  rdr    changed specification of locflags
+ *                                        from char to unsigned char
+ *              05/20/03    v1.3   rdr    Added call to cf_proc_check
+ *              05/22/03    v1.5   wvd    Direct cf_error_init to stderr
+ *              06/02/03    v1.6   wvd    Implement cf_verbose throughout.
+ *              06/04/03    v1.7   wvd    Revise scheme for summing counts.
+ *              08/20/03    v1.8   wvd    Use FRAME_TOLERANCE from calfuse.h,
+ *					  change channel to unsigned char.
+ *              09/15/03    v1.9   wvd    Test that photon times match
+ *					  timeline times to within 1 sec.
+ *              10/06/03    v1.10  wvd    Changed screen to locflags throughout.
+ *              12/29/06    v1.11  wvd    Sum weights rather than counts.
+ *					  Convert output arrays to type float.
+ *					  Scale HIST count rate by DET_DEAD.
+ *              04/07/07    v1.12  wvd	  Clean up compiler warnings.
+ *              04/07/07    v1.13  wvd	  Clean up compiler warnings.
+ *
+ **************************************************************************/
+
+#include <string.h>
+#include "calfuse.h"
+
+int
+cf_target_count_rate(fitsfile *header, long nevents, float *ptime, 
+	float *weight, unsigned char *channel, unsigned char *locflags,
+	long ntimes, float *ttime, float *rate_lif, float *rate_sic) {
+
+    char CF_PRGM_ID[] = "cf_target_count_rate" ;
+    char CF_VER_NUM[] = "1.13" ;
+ 
+    char instmode[FLEN_VALUE];
+    int errflg=0, status=0, active_ap[2] ;
+    float delta_max = 1.0 + FRAME_TOLERANCE;
+    float det_dead;
+    long j, k ;
+ 
+    /* Initialize error checking. */ 
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+    /* Enter a time stamp into the log. */
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    /* Confirm that this subroutine should be run. */
+    if ((errflg = cf_proc_check(header, CF_PRGM_ID))) return errflg;
+
+    /* Determine the source aperture from the header data. */
+    FITS_read_key(header, TSTRING, "INSTMODE", instmode, NULL, &status);
+    (void) cf_source_aper(header, active_ap) ;
+
+    /*
+     * For histogram data, scale the LiF and SiC count rates, which come
+     * from the housekeeping data file, by DET_DEAD.
+     */
+    if (!strncmp(instmode, "HIST", 4)) {
+	FITS_read_key(header, TFLOAT, "DET_DEAD", &det_dead, NULL, &status);
+	for (k = 0; k < ntimes; k++) rate_lif[k] *= det_dead;
+	for (k = 0; k < ntimes; k++) rate_sic[k] *= det_dead;
+    }
+
+    /* 
+     * For time-tag data, count the photons arriving during each second
+     * of the exposure.  Exclude events near airglow regions.
+     */
+    else {
+	for (k = 0; k < ntimes; k++) rate_lif[k] = rate_sic[k] = 0.; 
+	for (j=k=0; j<nevents; j++) {
+            while(ttime[k+1]-FRAME_TOLERANCE < ptime[j] && k+1 < ntimes)
+		k++;
+            if (!(locflags[j] & LOCATION_AIR) &&
+		(ptime[j] - ttime[k] < delta_max)) {
+		if (channel[j] == active_ap[0]) rate_lif[k] += weight[j] ;
+		if (channel[j] == active_ap[1]) rate_sic[k] += weight[j] ;
+	    }
+	}
+    }
+
+    cf_proc_update(header, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished processing"); 
+    return (status);
+}
diff --git a/src/libcf/cf_thermal_distort.c b/src/libcf/cf_thermal_distort.c
new file mode 100644
index 0000000..fcfb2e6
--- /dev/null
+++ b/src/libcf/cf_thermal_distort.c
@@ -0,0 +1,258 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_thermal_distort(fitsfile *header, long nevents, 
+ *				   float *xfarf, float *yfarf, float *weight,
+ *				   unsigned char *locflags)
+ *
+ * Description: Corrects the X position of the event for thermal distortion
+ *              using the locations of the stim pulses.  The correction is
+ *              made only to stim pulses and events in the detector active 
+ *		region.
+ *
+ * Arguments:   fitsfile  *header       Pointer to FITS file containing the
+ *                                      header of the intermediate data file
+ *              long      nevents       The number of events
+ *              float     *xfarf        An array of event X positions
+ *              float     *yfarf        An array of event Y positions
+ *              float     *weight       Number of photons per pixel
+ *              unsigned char *locflags Location flags for each event
+ *
+ * Calls:       cf_estimate_drift_coefficients
+ *              cf_get_stim_positions   These are static functions.
+ *
+ * Return:      0  on success
+ *
+ * History:     08/06/02   1.1    peb   Begin work
+ *              11/11/02   1.2    peb   Corrected function description and
+ *                                      added cf_timestamp after ELEC_COR
+ *                                      check.
+ *              11/12/02   1.3    peb   Sets left and right stim pulse flags.
+ *              11/12/02   1.4    peb   Added check to move only events in
+ *                                      stim-pulse and active region.
+ *		03/11/03   1.5    wvd   Changed locflags to unsigned char
+ *              05/20/03   1.6    rdr   Added cf_proc_check call
+ *		07/29/03   1.8    wvd	If cf_proc_check fails, return errflg.
+ *              02/27/04   1.9    rdr   Added weights to the calculation - 
+ *                                      needed for histogram mode
+ *              03/01/04   1.10   rdr   Corrected bug in procedure for finding
+ *                                       stim pulses
+ *              07/21/04   1.13   wvd	Delete variable i; unused.
+ *              03/03/05   1.14   wvd	Read thermal coefficients from STIM_CAL
+ *					file if STIM pulses are unavailable.
+ *              04/06/05   1.15   wvd	Require at least 500 counts in a stim
+ *					pulse to compute a centroid.
+ *		10/05/07   1.16   bot	Corrected jmax in estimate_drift
+ *
+ ****************************************************************************/
+
+#include <math.h>
+#include <stdlib.h>
+#include <string.h>
+#include "calfuse.h"
+
+#define STIMS (LOCATION_STIML|LOCATION_STIMR)
+
+static int
+cf_estimate_drift_coefficients (fitsfile *header, float *x0, float *x1,
+	float *y0, float *y1)
+{
+    char	stimfile[FLEN_FILENAME];
+    int		status=0;
+    long	j, jmax;
+    float	*x0_array=NULL, *x1_array=NULL, *y0_array=NULL, *y1_array=NULL;
+    double	expstart, *mjd=NULL;
+    fitsfile	*stimfits;
+
+    /* Read header keywords. */
+    FITS_read_key(header, TDOUBLE, "EXPSTART", &expstart, NULL, &status);
+    FITS_read_key(header, TSTRING, "STIM_CAL", stimfile, NULL, &status);
+    cf_verbose(3, "Drift-coefficient calibration file = %s", stimfile);
+
+    /* Read drift-coefficients from the calibration file. */
+    FITS_open_file(&stimfits, cf_cal_file(stimfile), READONLY, &status);
+    FITS_movabs_hdu(stimfits, 2, NULL, &status);
+    jmax = cf_read_col(stimfits, TDOUBLE, "MJD", (void *) &mjd);
+    jmax = cf_read_col(stimfits, TFLOAT,  "X0", (void *) &x0_array);
+    jmax = cf_read_col(stimfits, TFLOAT,  "X1", (void *) &x1_array);
+    jmax = cf_read_col(stimfits, TFLOAT,  "Y0", (void *) &y0_array);
+    jmax = cf_read_col(stimfits, TFLOAT,  "Y1", (void *) &y1_array);
+    FITS_close_file(stimfits, &status);
+
+    /* Find the coefficients appropriate for this exposure. */
+    j = 0;
+    while (j < jmax-1 && mjd[j+1] < expstart) j++;
+    *x0 = x0_array[j];
+    *x1 = x1_array[j];
+    *y0 = y0_array[j];
+    *y1 = y1_array[j];
+
+    free(mjd);
+    free(x0_array);
+    free(x1_array);
+    free(y0_array);
+    free(y1_array);
+
+    return status;
+}
+
+
+static int
+cf_get_stim_positions(long nevents, float *xfarf, float *yfarf, float *weight, 
+                   unsigned char *loc, float width, float *stimlx, float *stimly,
+		   float *stimrx, float *stimry)
+{
+    int   stim_status=0;
+    long  j;
+    double lx=0., ly=0., rx=0., ry=0., nl=0., nr=0.;
+
+    cf_verbose(3,"initial: stimlx = %0.1f, stimly=%0.1f, width=%0.1f ",
+               *stimlx, *stimly, width) ;
+    cf_verbose(3,"initial: stimrx = %0.1f, stimry=%0.1f, width=%0.1f ",
+		*stimrx, *stimry, width) ;
+
+    for (j=0; j<nevents; j++) {
+	if      (xfarf[j] >= *stimlx-width && xfarf[j] <= *stimlx+width &&
+		 yfarf[j] >= *stimly-width && yfarf[j] <= *stimly+width) {
+	    lx += xfarf[j] * weight[j];
+	    ly += yfarf[j] * weight[j];
+	    nl += weight[j];
+	    loc[j] |= LOCATION_STIML;
+	}
+	else if (xfarf[j] >= *stimrx-width && xfarf[j] <= *stimrx+width &&
+		 yfarf[j] >= *stimry-width && yfarf[j] <= *stimry+width) {
+	    rx += xfarf[j] * weight[j];
+	    ry += yfarf[j] * weight[j];
+	    nr +=  weight[j];
+	    loc[j] |= LOCATION_STIMR;
+	}
+	else {
+	    loc[j] &= ~STIMS;
+	}
+    }
+
+    cf_verbose(3,"nl=%0.1f,  nr=%0.1f ",nl,nr) ;
+
+    if (nl > 500) {
+	*stimlx = lx/nl;
+	*stimly = ly/nl;
+    } else {
+	cf_if_warning("Cannot determine left STIM position.  Estimating.");
+	stim_status = 1;
+    }
+    if (nr > 500) {
+	*stimrx = rx/nr;
+	*stimry = ry/nr;
+    } else {
+	cf_if_warning("Cannot determine right STIM position.  Estimating.");
+	stim_status = 1;
+    }
+
+    if (!stim_status) {
+	cf_verbose(3,"after iteration: stimlx = %0.1f, stimly=%0.1f ", *stimlx, *stimly);
+	cf_verbose(3,"after iteration: stimrx = %0.1f, stimry=%0.1f ", *stimrx, *stimry);
+    }
+
+    return stim_status;
+}
+
+int
+cf_thermal_distort(fitsfile *header, long nevents, float *xfarf, 
+		   float *yfarf, float *weight, unsigned char *locflags)
+{
+    char CF_PRGM_ID[] = "cf_thermal_distort";
+    char CF_VER_NUM[] = "1.16";
+
+    char  elecfile[FLEN_VALUE], detector[FLEN_VALUE];
+    char  keyword[FLEN_KEYWORD];
+    int   errflg=0, status=0, stim_status=0;
+    long  j;
+    float farflx, farfly, farfrx, farfry, x0, x1, y0, y1;
+    float stimlx, stimly, stimrx, stimry, oldlx, oldly, oldrx, oldry;
+    float width=128., tol=0.01;
+    fitsfile *elecfits;
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    if ((errflg = cf_proc_check(header, CF_PRGM_ID))) return errflg;
+
+    FITS_read_key(header, TSTRING, "DETECTOR", detector, NULL, &status);
+    /*
+     *  Get the name of the calibration file and open it
+     */
+    FITS_read_key(header, TSTRING, "ELEC_CAL", elecfile, NULL, &status);
+    FITS_open_file(&elecfits, cf_cal_file(elecfile), READONLY, &status);
+    /*
+     *  Read stim locations in FARF frame.
+     */
+    FITS_read_key(elecfits, TFLOAT, "STIMWDTH", &width, NULL, &status);
+    FITS_read_key(elecfits, TFLOAT, "STIMTOLR", &tol, NULL, &status);
+    sprintf(keyword, "STIMLX%s", detector);
+    FITS_read_key(elecfits, TFLOAT, keyword, &farflx, NULL, &status);
+    sprintf(keyword, "STIMLY%s", detector);
+    FITS_read_key(elecfits, TFLOAT, keyword, &farfly, NULL, &status);
+    sprintf(keyword, "STIMRX%s", detector);
+    FITS_read_key(elecfits, TFLOAT, keyword, &farfrx, NULL, &status);
+    sprintf(keyword, "STIMRY%s", detector);
+    FITS_read_key(elecfits, TFLOAT, keyword, &farfry, NULL, &status);
+    FITS_close_file(elecfits, &status);
+    /*
+     *  Get stim positions (iteratively).
+     */
+    stimlx = farflx; stimly = farfly;
+    stimrx = farfrx; stimry = farfry;
+    do {
+	oldlx = stimlx;	oldly = stimly;
+	oldrx = stimrx;	oldry = stimry;
+	width /= 2.;
+	stim_status = cf_get_stim_positions(nevents, xfarf, yfarf, weight,
+		locflags, width, &stimlx, &stimly, &stimrx, &stimry);
+	if (!stim_status)
+	    cf_verbose(3,"dstimlx=%.1f,  dstimly=%.1f, dstimrx=%.1f,"
+	    "dstimry=%.1f ", fabs(oldlx-stimlx), fabs(oldly-stimly),
+	    fabs(oldrx-stimrx), fabs(oldry-stimry) ) ;
+    } while (fabs(oldlx-stimlx) > tol && fabs(oldly-stimly) > tol && 
+	     fabs(oldrx-stimrx) > tol && fabs(oldry-stimry) > tol &&
+	     !stim_status);
+    /*
+     *  Write stim pulse positions to file header.
+     */
+    if (!stim_status) {
+	FITS_update_key(header, TFLOAT, "STIM_L_X", &stimlx, NULL, &status);
+	FITS_update_key(header, TFLOAT, "STIM_L_Y", &stimly, NULL, &status);
+	FITS_update_key(header, TFLOAT, "STIM_R_X", &stimrx, NULL, &status);
+	FITS_update_key(header, TFLOAT, "STIM_R_Y", &stimry, NULL, &status);
+    }
+    /*
+     *  Calculate drift coefficients from stim pulse positions
+     */
+    if (!stim_status) {
+	x0 = (stimlx*farfrx - stimrx*farflx)/(stimlx - stimrx);
+	x1 = (farflx - farfrx)/(stimlx - stimrx);
+	y0 = 0.5*((farfly + farfry) - (stimly + stimry));
+	y1 = 1.0;
+    }
+    /* 
+     *  ...or estimate them from date of exposure.
+     */
+    else
+	cf_estimate_drift_coefficients (header, &x0, &x1, &y0, &y1);
+    cf_verbose(2, "Drift coefficients: %f %f, %f %f", x0, x1, y0, y1);
+    /*
+     *  Apply thermal correction to events in active area and
+     *  stim-pulse regions.
+     */
+    for (j=0; j<nevents; j++) {
+	if (!(locflags[j] & LOCATION_SHLD) || (locflags[j] & STIMS)) {
+	    xfarf[j] = x1*xfarf[j] + x0;
+	    yfarf[j] = y1*yfarf[j] + y0;
+	}
+    }
+    cf_proc_update(header, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return 0;
+}
diff --git a/src/libcf/cf_time_xy_distort.c b/src/libcf/cf_time_xy_distort.c
new file mode 100644
index 0000000..bcb8af0
--- /dev/null
+++ b/src/libcf/cf_time_xy_distort.c
@@ -0,0 +1,171 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_time_xy_distort(fitsfile *header, long nevents,
+ *		float *xfarf, float *yfarf, unsigned char *locflags)
+ *
+ * Description: Corrects each photon event in the active area for long-term
+ *		drifts in the X and Y coordinate scales.
+ *
+ * Arguments:   fitsfile  *header       Pointer to FITS file containing the
+ *                                      header of the intermediate data file
+ *              long      nevents       The number of events
+ *              float     *xfarf        An array of event X positions
+ *              float     *yfarf        An array of event Y positions
+ *              unsigned char *locflags Location flags for each event
+ *
+ * Calls:
+ *
+ * Return:      0  on success
+ *
+ * History:     11/01/06   1.1   wvd    Based on cf_count_rate_y_distort.c
+ *		11/22/06   1.2   wvd	Read BIN_FACT from file header.
+ *					Make X correction a function of X.
+ *		01/19/07   1.3   wvd	Clean up i/o.
+ *		04/07/07   1.4   wvd	Clean up compiler warnings.
+ *
+ ****************************************************************************/
+
+#include <math.h>
+#include <string.h>
+#include <stdlib.h>
+#include "calfuse.h"
+
+int
+cf_time_xy_distort(fitsfile *header, long nevents,
+	float *xfarf, float *yfarf, unsigned char *locflags)
+{
+    char CF_PRGM_ID[] = "cf_time_xy_distort";
+    char CF_VER_NUM[] = "1.4";
+    
+    char  tmxyfile[FLEN_VALUE];
+    int   errflg=0, hdutype, status=0, anynull=0;
+    int   binfact, i, ii, i_max, tndx, xndx, yndx;
+    long  j, xlen, ylen;
+    double expstart;
+    float *xstretch2d, *ystretch2d, xstretch1d[NXMAX], ystretch1d[NYMAX];
+    fitsfile *tmxyfits;
+
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    if ((errflg = cf_proc_check(header, CF_PRGM_ID))) return errflg;
+
+    /*
+     *  Read MJD of exposure start.
+     */
+    FITS_read_key(header, TDOUBLE, "EXPSTART", &expstart, NULL, &status);
+
+    /*
+     *  Read the X correction array.
+     *  Note: the first column of the calibration array contains MJD.
+     */
+    FITS_read_key(header, TSTRING, "TMXY_CAL", tmxyfile, NULL, &status);
+    cf_verbose(3, "Reading TMXY_CAL file %s", tmxyfile);
+    FITS_open_file(&tmxyfits, cf_cal_file(tmxyfile), READONLY, &status);
+    FITS_movabs_hdu(tmxyfits, 2, &hdutype, &status);
+    FITS_read_key(tmxyfits, TLONG, "NAXIS1", &xlen, NULL, &status);
+    FITS_read_key(tmxyfits, TLONG, "NAXIS2", &ylen, NULL, &status);
+    FITS_read_key(tmxyfits, TINT, "BIN_FACT", &binfact, NULL, &status);
+    xstretch2d = (float *) cf_malloc(sizeof(float)*xlen*ylen);
+    FITS_read_img(tmxyfits, TFLOAT, 1L, xlen*ylen, NULL, xstretch2d,
+    	&anynull, &status);
+
+    /* 
+     * Find the row in the calibration array that corresponds to the 
+     * exposure start time.
+     */
+    i = 0;
+    while (expstart > *(xstretch2d+i*xlen) && i < ylen) i++;
+    tndx = i-1;
+    if (tndx < 0) tndx = 0;
+    cf_verbose(2,"EXPSTART = %g.", expstart);
+    cf_verbose(2,"Using X corrections for MJD >= %g", *(xstretch2d+tndx*xlen));
+    if (tndx < ylen-1)
+	cf_verbose(2,"                    and MJD <  %g",
+	*(xstretch2d+(tndx+1)*xlen));
+
+    /* 
+     *  Now compute a 1-D array containing corrections to X
+     *  coordinate as a function of X position on the detector.
+     *  Shift information binned by BIN_FACT pixels.
+     *  We interpolate to the nearest X pixel.  Otherwise,
+     *  counts pile up at the boundaries.
+     */
+    i_max = (xlen-2) * binfact;
+    for (i = 0; i < i_max; i++) {
+	ii = (i/binfact) * binfact;
+	xstretch1d[i] = ((ii+binfact-i) * (xstretch2d+tndx*xlen)[1+i/binfact] +
+	                (i-ii) * (xstretch2d+tndx*xlen)[2+i/binfact]) / binfact;
+    }
+    for ( ; i < NXMAX; i++) 
+	xstretch1d[i] = (xstretch2d+tndx*xlen)[xlen-1];
+
+    /*
+     *  Read the Y correction array.
+     */
+    FITS_movabs_hdu(tmxyfits, 3, &hdutype, &status);
+    FITS_read_key(tmxyfits, TLONG, "NAXIS1", &xlen, NULL, &status);
+    FITS_read_key(tmxyfits, TLONG, "NAXIS2", &ylen, NULL, &status);
+    FITS_read_key(tmxyfits, TINT, "BIN_FACT", &binfact, NULL, &status);
+    ystretch2d = (float *) cf_malloc(sizeof(float)*xlen*ylen);
+    FITS_read_img(tmxyfits, TFLOAT, 1L, xlen*ylen, NULL, ystretch2d,
+    	&anynull, &status);
+    FITS_close_file(tmxyfits, &status);
+
+    /* 
+     * Find the row in the calibration array that corresponds to the 
+     * exposure start time.
+     */
+    i = 0;
+    while (expstart > *(ystretch2d+i*xlen) && i < ylen) i++;
+    tndx = i-1;
+    if (tndx < 0) tndx = 0;
+    cf_verbose(3,"Using Y corrections for MJD >= %g", *(ystretch2d+tndx*xlen));
+    if (tndx < ylen-1)
+	cf_verbose(3,"                    and MJD <  %g",
+	*(ystretch2d+(tndx+1)*xlen));
+
+    /* 
+     *  Now compute a 1-D array containing corrections to Y 
+     *  coordinate as a function of Y position on the detector.
+     */
+    i_max = (xlen-2) * binfact;
+    for (i = 0; i < i_max; i++) {
+	ii = (i/binfact) * binfact;
+	ystretch1d[i] = ((ii+binfact-i) * (ystretch2d+tndx*xlen)[1+i/binfact] +
+	                (i-ii) * (ystretch2d+tndx*xlen)[2+i/binfact]) / binfact;
+    }
+    for ( ; i < NYMAX; i++) 
+	ystretch1d[i] = (ystretch2d+tndx*xlen)[xlen-1];
+    cf_verbose(3, "For y = 430, ystretch = %f\n", ystretch1d[430]);
+    cf_verbose(3, "For y = 810, ystretch = %f\n", ystretch1d[810]);
+
+    /* 
+     * Loop through all events. Move only events in active region.
+     */
+    for (j = 0; j < nevents; j++) {
+	if (!(locflags[j] & LOCATION_SHLD)) {
+	    xndx = (int) xfarf[j];
+	    if (xndx < 0) xndx = 0;
+	    else if (xndx >= NXMAX) xndx = NXMAX-1;
+
+	    yndx = (int) yfarf[j];
+	    if (yndx < 0) yndx = 0;
+	    else if (yndx >= NYMAX) yndx = NYMAX-1;
+
+	    xfarf[j] += xstretch1d[xndx];
+	    yfarf[j] += ystretch1d[yndx];
+	}
+    }
+
+    free(xstretch2d);
+    free(ystretch2d);
+
+    cf_proc_update(header, CF_PRGM_ID, "COMPLETE");
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done processing");
+    return 0;
+}
diff --git a/src/libcf/cf_timestamp.c b/src/libcf/cf_timestamp.c
new file mode 100644
index 0000000..52ef311
--- /dev/null
+++ b/src/libcf/cf_timestamp.c
@@ -0,0 +1,78 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_timestamp(const char *prgmid, const char *vernum, char *msg)
+ *
+ * Description: Writes a timestamp and the calling program name to stdout.
+ *
+ * Arguments:   char    *prgmid         Name of the calling program
+ *              char	*msg		Optional additional message string
+ *
+ * Returns:     none
+ *
+ * History:     01/04/91        mlr     Original "warn_str.c" for libhut
+ *		03/03/98	gak	Adapted for placing timestamps in
+ *					FUSE pipeline programs.
+ *              06/07/99        peb     Added reporting of version number.
+ *              10/27/99        emm     Added fflush(stdout)
+ *              04/23/01        wvd     Change declaration of tim from
+ *                                      long to time_t
+ *              03/19/03        peb     Made this function a wrapper for
+ *                                      cf_verbose.
+ *              03/25/03        peb     Changed output to print time, program,
+ *                                      version number and to use verbose_level
+ *                                      when printing output
+ *                                      level>=1 prints "Finished processing"
+ *                                      level>=2 prints "Begin processing"
+ *              09/15/03  v1.5  wvd     To reduce size of the trailer file,
+ *					if verbose level = 1, print "Finished"
+ *					only for top-level routines.
+ *              10/17/03  v1.6  wvd     Use strcmp, rather than strncmp, to
+ *					set this_is_a_top_level_routine.
+ *              10/30/03  1.7   peb     Replaced cftime function with strftime
+ *                                      for UNIX compatibility.
+ *
+ ****************************************************************************/
+
+#include <string.h>
+#include <time.h>
+#include "calfuse.h"
+
+#define  N_STYM  80
+
+void cf_timestamp(const char *prgmid, const char *vernum, char *msg)
+{
+    char stym[N_STYM]={'\0'};
+    char *top_level_routines[]=TOP_LEVEL_ROUTINES;
+    int  i, this_is_a_top_level_routine = FALSE;
+    time_t tym;
+
+    time(&tym);
+    strftime(stym, N_STYM, "%Y %b %e %T", localtime(&tym));
+
+    /* Compare program ID with list of top-level routines. */
+    for (i = 0; i < NTOP_LEVEL_ROUTINES; i++) {
+	if (!strcmp(prgmid, top_level_routines[i])) {
+	    this_is_a_top_level_routine = TRUE;
+	    break;
+	}
+    }
+
+    /*
+     *  The following test should get most "Finished" or "Done" type of
+     *  timestamps.  For those not caught if might be best to change them to
+     *  one of these two.
+     */
+    if (((verbose_level == 1 && this_is_a_top_level_routine) ||
+	(verbose_level > 1)) &&
+	(strncmp(msg, "Finish", 6) == 0 || strncmp(msg, "Done", 4) == 0))
+	printf("%s %s-%s: %s\n", stym, prgmid, vernum, "Finished processing");
+    else if (verbose_level >= 2 &&
+	     (strncmp(msg, "Start", 5) == 0 || strncmp(msg, "Begin", 5) == 0))
+	printf("%s %s-%s: %s\n", stym, prgmid, vernum, "Begin processing");
+
+    fflush(stdout);
+}
diff --git a/src/libcf/cf_velang.c b/src/libcf/cf_velang.c
new file mode 100644
index 0000000..8395738
--- /dev/null
+++ b/src/libcf/cf_velang.c
@@ -0,0 +1,147 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    cf_velang(fitsfile *outfits, double mjd)
+ *
+ * Description: Calculates the sun angle, moon angle, and conversions to
+ *              heliocentric and LSR velocities at given mjd, which should be
+ *              the middle of the exposure.  For FUV images, the needed
+ *              data is in the primary header, so we have to go back
+ *              up to the top.  For FES images, the data should be in
+ *              each HDU, so you should call cf_velang_calc instead.
+ *
+ * Arguments:   fitsfile  *outfits       Pointer to FITS file containing the
+ *                                      input data and orbital elements
+ *              double    mjd           The Modified Julian Date of the 
+ *                                      photon arrival time.
+ *
+ * Calls:       slaDsep         dsep.f
+ *              slaRdplan       rdplan.f
+ *
+ * History:     07/13/98        emm     Begin work
+ *              06/10/99        emm     Added keyword header update, added
+ *                                      calculation of MOONANG.
+ *              06/11/99        emm     Fixed some bugs that Jayant found.
+ *              06/21/99         jm     Corrected name
+ *              07/16/99        emm     Changed GEO_LON to GEO_LONG
+ *              07/21/99        peb     RA and Dec now use RA_TARG and DEC_TARG
+ *              07/22/99	emm     Added V_GEOCEN update.
+ *              07/23/99	emm     Added cf_velang_calc for FES images.
+ *              05/31/00        peb	Implemented cfortran.h calls for slalib
+ *                                 	functions.
+ *		04/01/03  v1.3	wvd	Replaced printf with cf_verbose
+ *		04/04/03  v1.4	wvd	Modifed calls to cf_verbose.
+ *              12/18/03  v1.5  bjg     Change calfusettag.h to calfuse.h
+ *              07/06/06  v1.6  wvd     Add call to pole_ang and populate 
+ *					header keyword POLEANGL.
+ *              03/07/07  v1.7  wvd     Remove pos from call to space_vel. 
+ *
+ ****************************************************************************/
+
+#include <stdio.h>
+
+#ifdef CFORTRAN
+#include "cfortran.h"
+PROTOCCALLSFFUN4(DOUBLE, SLA_DSEP, sla_dsep, DOUBLE, DOUBLE, DOUBLE, \
+		 DOUBLE)
+#define slaDsep(A1, B1, A2, B2) \
+     CCALLSFFUN4(SLA_DSEP, sla_dsep, DOUBLE, DOUBLE, DOUBLE, DOUBLE, \
+		 A1, B1, A2, B2)
+PROTOCCALLSFSUB7(SLA_RDPLAN, sla_rdplan, DOUBLE, INT, DOUBLE, DOUBLE, \
+		 PDOUBLE, PDOUBLE, PDOUBLE)
+#define slaRdplan(DATE, NP, ELONG, PHI, RA, DEC, DIAM) \
+     CCALLSFSUB7(SLA_RDPLAN, sla_rdplan, DOUBLE, INT, DOUBLE, DOUBLE, \
+		 PDOUBLE, PDOUBLE, PDOUBLE, \
+		 DATE, NP, ELONG, PHI, RA, DEC, DIAM)
+#else
+#include "slalib.h"
+#include "slamac.h"
+#endif
+
+#include "calfuse.h"
+#include "sgp4.h"
+
+SGP4 set_orbit_parms(fitsfile *);
+
+static void
+cf_velang_calc(fitsfile *outfits, double mjd)
+{
+    int    status=0;
+    char   comment[FLEN_CARD];
+    double ra, dec, geo_lon, geo_lat, mag_lat, pos[3], vel[3], gmst, helvel;
+    double ra_moon, dec_moon, moon_ang, dia_moon, vlsr1, vlsr2, sun_ang;
+    double geo_vel, pole_angle;
+    SGP4   sgp4;
+
+    /* get the state vector at time mjd */
+    sgp4 = set_orbit_parms(outfits);
+    SGP4_getStateVector(sgp4, mjd, pos, vel);
+    SGP4_precess(pos, mjd, MJD2000); SGP4_precess(vel, mjd, MJD2000);
+
+    cf_verbose(2,"State vector at MJD=%14.6f days", mjd);
+    cf_verbose(2,"x=%14.6f y=%14.6f z=%14.6f km", pos[0], pos[1], pos[2]);
+    cf_verbose(2,"vx=%14.6f vy=%14.6f vz=%14.6f km/s",vel[0], vel[1], vel[2]);
+
+    state_geod(pos, mjd, &geo_lon, &geo_lat, &gmst);
+
+    mag_lat = geod_mag(geo_lon, geo_lat);
+    /*
+     *  Note: this function has been changed to use RA_TARG and DEC_TARG
+     *  keywords, because the RA_APER and DEC_APER keywords are currently
+     *  not being set.
+     */
+    FITS_read_key(outfits, TDOUBLE, "RA_TARG", &ra, comment, &status);
+    FITS_read_key(outfits, TDOUBLE, "DEC_TARG", &dec, comment, &status);
+
+    geo_vel= space_vel(vel, ra, dec);
+    helvel = helio_vel(mjd, ra, dec);
+    vlsr1  = lsrk_vel(ra, dec);
+    vlsr2  = lsrd_vel(ra, dec);
+
+    /* Calculate sun angle */
+    sun_ang = solar_ang(mjd, ra, dec);
+
+    /* Calculate moon angle */
+#ifdef CFORTRAN
+    slaRdplan(mjd, 3, geo_lon, geo_lat, ra_moon, dec_moon, dia_moon);
+#else
+    slaRdplan(mjd, 3, geo_lon, geo_lat, &ra_moon, &dec_moon, &dia_moon);
+#endif
+    moon_ang = slaDsep(ra*RADIAN, dec*RADIAN, ra_moon, dec_moon)/RADIAN;
+
+    /* Calculate sun angle */
+    pole_angle = pole_ang(pos, vel, ra, dec);
+
+    FITS_update_key(outfits, TDOUBLE, "SUNANGLE", &sun_ang, NULL, &status);
+    FITS_update_key(outfits, TDOUBLE, "MOONANGL", &moon_ang, NULL, &status);
+    FITS_update_key(outfits, TDOUBLE, "POLEANGL", &pole_angle, NULL, &status);
+    FITS_update_key(outfits, TDOUBLE, "GEO_LONG", &geo_lon, NULL, &status);
+    FITS_update_key(outfits, TDOUBLE, "GEO_LAT",  &geo_lat, NULL, &status);
+    FITS_update_key(outfits, TDOUBLE, "MAG_LAT",  &mag_lat, NULL, &status);
+    FITS_update_key(outfits, TDOUBLE, "V_GEOCEN", &geo_vel, NULL, &status);
+    FITS_update_key(outfits, TDOUBLE, "V_HELIO",  &helvel, NULL, &status);
+    FITS_update_key(outfits, TDOUBLE, "V_LSRDYN", &vlsr2, NULL, &status);
+    FITS_update_key(outfits, TDOUBLE, "V_LSRSTD", &vlsr1, NULL, &status);
+}
+
+
+void cf_velang(fitsfile *outfits, double mjd)
+{
+    int    status=0, hdunum=0, hdutype;
+    /*
+     *  The outfits file pointer may be down in one of the extensions
+     *  whereas the orbital info is in the primary hdu.  Therefore,
+     *  record the current position, move to the primary header, 
+     *  read the orbital data, and return to the previous hdu.
+     */
+    FITS_get_hdu_num(outfits, &hdunum);
+    FITS_movabs_hdu(outfits, 1, &hdutype, &status);
+
+    cf_velang_calc(outfits, mjd);
+
+    FITS_movabs_hdu(outfits, hdunum, &hdutype, &status);
+
+}
diff --git a/src/libcf/cf_write_extracted_spectrum.c b/src/libcf/cf_write_extracted_spectrum.c
new file mode 100644
index 0000000..90831c2
--- /dev/null
+++ b/src/libcf/cf_write_extracted_spectrum.c
@@ -0,0 +1,226 @@
+/**************************************************************************
+ *              Johns Hopkins University
+ *              Center for Astrophysical Sciences
+ *              FUSE
+ *************************************************************************
+ *
+ * synopsis:    cf_write_extracted_spectrum(infile, aperture, nout, wave_out,
+ *                    flux_out, var_out, counts_out, weights_out, bkgd_out,
+ *                    bpix_out, outrootname)
+ *
+ * Description: Write the results of the data reduction to a file.
+ *              Information from the header is used to generate the name
+ *              of the output file.  Aperture coding is as follows:
+ *
+ *              1-8 -> LiF[HIRS,MDRS,LWRS,PINH], SiC[HIRS,MDRS,LWRS,PINH]
+ *
+ * Arguments:   fitsfile  infile   :   pointer to Intermediate Data File
+ *              int       aperture :   Target aperture (values are 1 to 8)
+ *		int  valid_spectrum:   True if spectrum contains photons.
+ *              long      nout     :   number of tabulated points
+ *              float     wave_out :   Output wavelength array
+ *              float     flux_out :   Output flux array
+ *              float     var_out  :   Output variance array
+ *              long    counts_out :   Output counts array (in counts)
+ *              float  weights_out :   Output weights array (in counts)
+ *              float     bkgd_out :   Output background array (in counts)
+ *              short     bpix_out :   Output bad pixel spectrum
+ *              char    outrootname:   Optional output file name
+ *
+ * Returns:	0 if successful
+ *                                
+ * HISTORY:     02/10/03   1.1   RDR    started work
+ *              02/28/03   1.2   peb    Added header files to file and tidied
+ *                                      code using lint.
+ *		03/12/03   1.3   wvd    Output ERROR = sqrt(var_out)
+ *		03/31/03   1.4   wvd	Update keywords FILENAME, FILETYPE,
+ *                                      and APER_ACT.
+ *		05/22/03   1.5   wvd	Direct cf_error_init to stderr.
+ *              05/29/03   1.6   rdr    Added bad pixel column
+ *              06/03/03   1.7   rdr    Change naming convention to allow
+ *					hist data
+ *              07/17/03   1.9   wvd    Test var_out before taking sqrt.
+ *					Change calfusettag.h to calfuse.h
+ *              10/01/03   1.10  wvd    Modify verbose levels.
+ *              11/10/03   1.11  wvd    Correct numbering scheme for HIRS
+ *					and MDRS apertures.
+ *              02/13/04   1.12  wvd    Correct error in COMMENT lines.
+ *              03/03/04   1.13  rdr    Populate archive search keywords
+ *              03/05/04   1.14  wvd    Change name of POTHOLE column 
+ *					to QUALITY.
+ *              03/24/04   1.15  wvd    If valid_spectrum=FALSE, write
+ *					warning message to file header.
+ *              04/06/04   1.16  bjg    Include string.h and ctype.h
+ *              04/09/04   1.17  wvd    If valid_spectrum=FALSE, set
+ *					EXPTIME = 0 in file header.
+ *              04/27/04   1.18  wvd    Move conversion from variance
+ *					to sigma from this routine to
+ *					cf_optimal_extraction.
+ *              06/11/04   1.19  peb    Added the -r option to override the
+ *                                      default rootname
+ *		02/01/05   1.20  wvd	Revert to standard FITS binary
+ *					table format for output file.
+ *		04/11/05   1.21  wvd	In HIST mode, don't write SIA
+ *					table to output spectral file.
+ *		06/03/05   1.22  wvd	Return status from cf_copy_hist_header.
+ *		06/03/05   1.23  wvd	Change cf_copy_hist_header to type void.
+ *		08/11/05   1.24  wvd	Delete FITS_write_date from 
+ *					cf_copy_hist_header.
+ *
+ **************************************************************************/
+
+#include <string.h>
+#include <ctype.h>
+#include <stdio.h>
+#include "calfuse.h"
+
+static char *ap_code[] = {"", "lif3", "lif2", "lif4", "lif1",
+                              "sic3", "sic2", "sic4", "sic1"};
+
+static void
+cf_copy_hist_header(fitsfile *infits, fitsfile *outfits, int *status)
+{
+	char	card[FLEN_CARD];
+	int	i, nkeys, naxis=0, nextend=1;
+	long	naxes[2];
+
+	naxes[0] = naxes[1] = 0;
+
+	FITS_create_img(outfits, SHORT_IMG, naxis, naxes, status);
+	FITS_delete_key(outfits, "COMMENT", status);
+	FITS_delete_key(outfits, "COMMENT", status);
+	FITS_write_key(outfits, TINT, "NEXTEND", &nextend,
+		"Number of standard extensions", status);
+	fits_get_hdrspace(infits, &nkeys, NULL, status);
+	cf_if_fits_error(*status);
+	for (i = 9; i <= nkeys; i++) {
+	    FITS_read_record(infits, i, card, status);
+	    FITS_write_record(outfits, card, status);
+	}
+}
+
+int
+cf_write_extracted_spectrum(fitsfile *infits, int aperture,
+	int valid_spectrum, long nout, float *wave_out,
+	float *flux_out, float *var_out, long *counts_out,
+	float *weights_out, float *bkgd_out, short *bpix_out,
+	char *outrootname)
+{
+    char CF_PRGM_ID[] = "cf_write_extracted_spectrum";
+    char CF_VER_NUM[] = "1.24";
+
+    fitsfile *outfits;
+    int nextend=1, status=0, tfields=7, timeref;
+    long i, frow=1, felem=1;
+    float bw=0., center=0., wmin=1200., wmax=0. ;
+    char comment[FLEN_CARD], datestr[FLEN_CARD];
+    char rootname[FLEN_VALUE]={'\0'}, instmode[FLEN_VALUE] ;
+    char det[FLEN_VALUE]={'\0'}, outfile[FLEN_VALUE]={'\0'};
+    char extname[]="SPECTRUM";
+    char *aperact[] = {"HIRS_LIF", "MDRS_LIF", "LWRS_LIF", "PINH_LIF",
+                      "HIRS_SIC", "MDRS_SIC", "LWRS_SIC", "PINH_SIC"};
+    char *ttype[]={"WAVE","FLUX","ERROR","COUNTS","WEIGHTS","BKGD","QUALITY"};
+    char *tform[]={"1E", "1E", "1E", "1J", "1E", "1E", "1I"};
+    char *tunit[]={"ANGSTROMS","ERG CM^-2 S^-1 ANG^-1","ERG CM^-2 S^-1 ANG^-1",
+		"COUNTS", "COUNTS", "COUNTS","UNITLESS"};
+
+    /* Initialize error checking */ 
+    cf_error_init(CF_PRGM_ID, CF_VER_NUM, stderr);
+
+    /* Enter a time stamp into the log */
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin Processing");
+
+    /*
+     *  Read the observation ID from the input file and create an
+     *  output file name.
+    */
+    FITS_movabs_hdu(infits, 1, NULL, &status);
+    FITS_read_key(infits, TSTRING, "ROOTNAME", rootname, NULL, &status);
+    FITS_read_key(infits, TSTRING, "DETECTOR", det, NULL, &status);
+    FITS_read_key(infits, TSTRING, "INSTMODE", instmode, NULL, &status);
+
+    /* Override the default rootname if the -r option is given. */
+    if (outrootname != NULL)
+        strcpy(rootname, outrootname);
+
+    /* Convert detector name to lower case */
+    det[1] = tolower(det[1]);
+    
+    if (!strncmp(instmode,"T",1))
+        sprintf(outfile, "%11s%2s%4sttagfcal.fit",
+                rootname, det, ap_code[aperture]);
+    else if (!strncmp(instmode,"H",1))
+        sprintf(outfile, "%11s%2s%4shistfcal.fit",
+                rootname, det, ap_code[aperture]);
+    else {
+      cf_if_error("Cannot create name for the output files.") ;
+      return 1;
+    }
+    cf_verbose(3, "Output file name = %s", outfile);
+
+    /* Open the output file and copy the header info from the input file */
+    FITS_create_file(&outfits, outfile, &status);
+    if (!strncmp(instmode,"T",1))
+        FITS_copy_header(infits, outfits, &status);
+    else
+	cf_copy_hist_header(infits, outfits, &status);
+    FITS_update_key(outfits, TINT, "NEXTEND", &nextend, NULL, &status);
+    FITS_update_key(outfits, TSTRING, "FILENAME", outfile, NULL, &status);
+    FITS_update_key(outfits, TSTRING, "FILETYPE",
+                 "CALIBRATED EXTRACTED SPECTRUM", NULL, &status);
+    FITS_update_key(outfits, TSTRING, "APER_ACT", aperact[aperture-1],
+                 NULL, &status);
+
+    /* If valid_spectrum = FALSE, write warning to file header. */
+    if (valid_spectrum == FALSE) {
+	float exptime = 0.;
+	FITS_update_key(outfits, TFLOAT, "EXPTIME", &exptime, NULL, &status);
+        FITS_write_comment(outfits, "  ", &status);
+        FITS_write_comment(outfits,
+		"No good data.  Output arrays set to zero.", &status);
+        fits_get_system_time(datestr, &timeref, &status);
+        sprintf(comment, "CalFUSE v%s   %.10s", CALFUSE_VERSION, datestr);
+        FITS_write_comment(outfits, comment, &status);
+        FITS_write_comment(outfits, "  ", &status);
+    }
+
+    /* Populate archive search keywords */
+    for (i=0 ; i<nout ; i++) {
+      if (wave_out[i] < wmin) wmin=wave_out[i] ;
+      if (wave_out[i] > wmax) wmax=wave_out[i] ;
+    }
+       bw = wmax-wmin ;
+       center = (wmax + wmin) / 2. ;
+    FITS_update_key(outfits, TFLOAT, "BANDWID", &bw, NULL, &status);
+    FITS_update_key(outfits, TFLOAT, "CENTRWV", &center, NULL, &status);
+    FITS_update_key(outfits, TFLOAT, "WAVEMIN", &wmin, NULL, &status);
+    FITS_update_key(outfits, TFLOAT, "WAVEMAX", &wmax, NULL, &status);
+
+    /* Put the data into the table */
+    FITS_create_tbl(outfits, BINARY_TBL, nout, tfields, ttype, tform,
+		    tunit, extname, &status);
+    FITS_write_col(outfits, TFLOAT, 1, frow, felem, nout, wave_out, &status);
+    FITS_write_col(outfits, TFLOAT, 2, frow, felem, nout, flux_out, &status);
+    FITS_write_col(outfits, TFLOAT, 3, frow, felem, nout, var_out, &status);
+    FITS_write_col(outfits, TLONG,  4, frow, felem, nout, counts_out, &status);
+    FITS_write_col(outfits, TFLOAT, 5, frow, felem, nout, weights_out, &status);
+    FITS_write_col(outfits, TFLOAT, 6, frow, felem, nout, bkgd_out, &status);
+    FITS_write_col(outfits, TSHORT, 7, frow, felem, nout, bpix_out, &status);
+    
+    /* Write some comments into the header */
+    FITS_write_comment(outfits, " ", &status);
+    FITS_write_comment(outfits, "RAW COUNTS = COUNTS ",
+		       &status);
+    FITS_write_comment(outfits, "TARGET COUNTS = WEIGHTS - BKGD ",
+		       &status);
+    FITS_write_comment(outfits, "TARGET FLUX = TARGET COUNTS * HC / LAMBDA / "
+		       "AEFF / EXPTIME / WPC", &status);
+    FITS_write_comment(outfits, " ", &status);
+
+    FITS_close_file(outfits, &status);
+
+    /* Enter a time stamp into the log */
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Finished processing");
+
+    return (status);
+}
diff --git a/src/libcf/eclipse.c b/src/libcf/eclipse.c
new file mode 100644
index 0000000..a1e0b44
--- /dev/null
+++ b/src/libcf/eclipse.c
@@ -0,0 +1,148 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    int eclipse(double pos[3], double mjdate)
+ *
+ * Description: Determines if FUSE is in the day or night portion of the orbit.
+ *              
+ *
+ * Arguments:   double pos            Cartesian vector xyz coord of satellite.
+ *              double mjdate          Julian date of observation
+ *
+ * Returns:     int                   0 if day portion of orbit
+ *                                    1 if night portion of orbit
+ *                    
+ * Calls:       slaDcc2s              dcc2s.f
+ *              slaDranrm             dranrm.f
+ *              slaDsep               dsep.f
+ *              slaEvp                evp.f
+ *              slaPreces             preces.f
+ *
+ * History:     03/10/98  E. Murphy   Begin work.
+ *              03/10/98  E. Murphy   Initial version working
+ *              07/07/99  E. Murphy   Replaced x,y,z in call with pos
+ *              07/20/99  jm          Removed duplicate define statements
+ *              08/26/99  E. Murphy   ang_sep now returned.
+ *              05/31/00        peb   Implemented cfortran.h calls for slalib
+ *                                    functions.
+ *              12/18/03  bjg       Change calfusettag.h to calfuse.h
+ *              06/17/04  bjg  1.4  Corrected cfortran call to sla_preces   
+ *
+ * References:  This routine makes use of the Starlink set of astronomical
+ *              subroutines (SLALIB).  More information can be found at
+ *              http://star-www.rl.ac.uk.
+ ****************************************************************************/
+ 
+#include <stdio.h>
+#include <math.h>
+
+#ifdef CFORTRAN
+#include "cfortran.h"
+PROTOCCALLSFSUB3(SLA_DCC2S, sla_dcc2s, DOUBLEV, PDOUBLE, PDOUBLE)
+#define slaDcc2s(V, A, B) \
+     CCALLSFSUB3(SLA_DCC2S, sla_dcc2s, DOUBLEV, PDOUBLE, PDOUBLE, V, A, B)
+PROTOCCALLSFFUN1(DOUBLE, SLA_DRANRM, sla_dranrm, DOUBLE)
+#define slaDranrm(ANGLE) \
+     CCALLSFFUN1(SLA_DRANRM, sla_dranrm, DOUBLE, ANGLE)
+PROTOCCALLSFFUN4(DOUBLE, SLA_DSEP, sla_dsep, DOUBLE, DOUBLE, DOUBLE, \
+		 DOUBLE)
+#define slaDsep(A1, B1, A2, B2) \
+     CCALLSFFUN4(SLA_DSEP, sla_dsep, DOUBLE, DOUBLE, DOUBLE, DOUBLE, \
+		 A1, B1, A2, B2)
+PROTOCCALLSFSUB6(SLA_EVP, sla_evp, DOUBLE, DOUBLE, DOUBLEV, DOUBLEV, \
+		 DOUBLEV, DOUBLEV)
+#define slaEvp(DATE, DEQX, DVB, DPB, DVH, DPH) \
+     CCALLSFSUB6(SLA_EVP, sla_evp, DOUBLE, DOUBLE, DOUBLEV, DOUBLEV, \
+		 DOUBLEV, DOUBLEV, DATE, DEQX, DVB, DPB, DVH, DPH)
+PROTOCCALLSFSUB5(SLA_PRECES, sla_preces, STRING, DOUBLE, DOUBLE, PDOUBLE, \
+		 PDOUBLE)
+#define slaPreces(SYSTEM, EP0, EP1, RA, DC) \
+     CCALLSFSUB5(SLA_PRECES, sla_preces, STRING, DOUBLE, DOUBLE, PDOUBLE, \
+		 PDOUBLE, SYSTEM, EP0, EP1, RA, DC)
+#else
+#include "slalib.h"
+#include "slamac.h"
+#endif
+
+#include "calfuse.h"
+
+int eclipse(double *pos, double mjdate, double *ang_sep)
+{
+    /* Define variables. */
+    int    i, retcode;
+    double dvb[3], dpb[3], dvh[3], dph[3], epoch2;
+    double r, ra_earth, dec_earth, ra_sun, dec_sun, ang_earth, ang_sun;
+    char fk5_st[10]="FK5";
+
+    /* Calculate the J2000.0 apparent RA and DEC of the Earth */
+    r=sqrt(pos[0]*pos[0]+pos[1]*pos[1]+pos[2]*pos[2]);
+    ra_earth=atan2(-pos[1],-pos[0]);
+    dec_earth=asin(-pos[2]/r);
+
+    /*  We must precess the J2000 RA and DEC to date of observation. This
+     *  is a very small correction, and could probably be ignored.
+     */
+
+    epoch2=2000.0-((51544.0-mjdate)/365.25);
+
+#ifdef CFORTRAN
+    slaPreces(fk5_st, 2000.0, epoch2, ra_earth, dec_earth);
+#else
+    slaPreces(fk5_st, 2000.0, epoch2, &ra_earth, &dec_earth);
+#endif
+
+    /*  Evp returns four 3-vectors containing the barycentric velocity and
+     *  position (dvb,dpv) and the heliocentric velocity and position 
+     *  (dvh,dph) of the Earth on the date mjdate.  It requires a modified 
+     *  Julian date as input.  Output has units of AU for positions and 
+     *  AU/s for velocities.
+     */
+
+    slaEvp(mjdate, 2000.0, dvb, dpb, dvh, dph);
+
+    /*  Convert the 3-vector position of the Sun into a J2000.0 RA and DEC */
+
+    for (i=0; i<3; i++) dph[i]*=-1.0;
+
+ 
+#ifdef CFORTRAN
+    slaDcc2s(dph, ra_sun, dec_sun);
+#else
+    slaDcc2s(dph, &ra_sun, &dec_sun);
+#endif
+
+    ra_sun=slaDranrm(ra_sun);
+
+    /*  We must precess the J2000 RA and DEC to date of observation. This
+     *  is a very small correction, and could probably be ignored.
+     */
+
+    epoch2=2000.0-((51544.0-mjdate)/365.25);
+
+#ifdef CFORTRAN
+    slaPreces(fk5_st, 2000.0, epoch2, ra_sun, dec_sun);
+#else
+    slaPreces(fk5_st, 2000.0, epoch2, &ra_sun, &dec_sun);
+#endif
+
+    /* Compute the angular sizes of the Earth and the Sun. */
+
+    ang_earth=asin(RE/r);
+
+    ang_sun=asin(RS/(sqrt(dph[0]*dph[0]+dph[1]*dph[1]+dph[2]*dph[2])*AU));
+
+    /* Compute the angular separation of the Earth and the Sun. */
+
+    *ang_sep=slaDsep(ra_earth, dec_earth, ra_sun, dec_sun);
+
+    retcode=0;
+    if (*ang_sep < ang_earth+ang_sun) retcode=1;
+
+    /* Convert ang_sep into degrees. */
+    *ang_sep /= RADIAN;
+
+    return retcode;
+}
diff --git a/src/libcf/geod_mag.c b/src/libcf/geod_mag.c
new file mode 100644
index 0000000..6750f9d
--- /dev/null
+++ b/src/libcf/geod_mag.c
@@ -0,0 +1,40 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    double geod_mag(double lon, double lat)
+ *
+ * Description: Computes the magnetic latitude of FUSE from the
+ *              given geocentric longitude and latitude.
+ *
+ * Arguments:   double lon,lat        (deg) Geocentric longitude and latitude
+ *
+ * Returns:     double                Geomagnetic latitude.
+ *                    
+ * History:     03/11/98  E. Murphy   Begin work.
+ *              03/11/98  E. Murphy   Initial version working
+ *              04/13/99  E. Murphy   Moved PI and RADIAN to calfuse.h
+ *              12/18/03  bjg         Change calfusettag.h to calfuse.h
+ *
+ *              Ake, T. 1998 in The Scientific Impact of the Goddard
+ *                   High Resolution Spectrograph, ed. J. C. Brandt et al.,
+ *                   ASP Conference Series, in preparation.
+ ****************************************************************************/
+ 
+#include <stdio.h>
+#include <math.h>
+#include "calfuse.h"
+ 
+double geod_mag(double lon, double lat)
+{
+    double lat_rad, c1;
+
+    lat_rad=lat*RADIAN;
+
+    c1=sin(lat_rad)*cos(11.4*RADIAN)-
+        cos(lat_rad)*cos((lon+69.8)*RADIAN)*sin(11.4*RADIAN);
+
+    return asin(c1)/RADIAN;
+}
diff --git a/src/libcf/helio_vel.c b/src/libcf/helio_vel.c
new file mode 100644
index 0000000..bc069b6
--- /dev/null
+++ b/src/libcf/helio_vel.c
@@ -0,0 +1,82 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    double helio_vel(double mjdate, double ra, double dec)
+ *
+ * Description: Computes the Earth's orbital velocity in the direction 
+ *              of ra,dec to convert to heliocentric velocity.
+ *
+ * Arguments:   double mjdate         Mod. Julian date of observation
+ *              double ra             (deg) J2000.0 right ascension
+ *              double dec            (deg) J2000.0 declination 
+ *
+ * Returns:     double                (km/s) velocity in direction of source
+ *                    
+ * Calls:       slaEvp                evp.f
+ *              slaDcs2c              dcs2c.f
+ *              slaDvdv               dvdv.f
+ *
+ * History:     03/05/98  E. Murphy   Begin work.
+ *              03/05/98  E. Murphy   Initial version working
+ *              05/31/00        peb   Implemented cfortran.h calls for slalib
+ *                                    functions.
+ *              06/15/01  V. Dixon    Correct sign of return value to agree
+ *				      with astronomical convention.
+ *              12/18/03  bjg         Change calfusettag.h to calfuse.h
+ *
+ * References:  This routine makes use of the Starlink set of astronomical
+ *              subroutines (SLALIB).  More information can be found at
+ *              http://star-www.rl.ac.uk.
+ ****************************************************************************/
+ 
+#include <stdio.h>
+
+#ifdef CFORTRAN
+#include "cfortran.h"
+
+PROTOCCALLSFSUB3(SLA_DCS2C, sla_dcs2c, DOUBLE, DOUBLE, DOUBLEV)
+#define slaDcs2c(A, B, V) \
+     CCALLSFSUB3(SLA_DCS2C, sla_dcs2c, DOUBLE, DOUBLE, DOUBLEV, A, B, V)
+
+PROTOCCALLSFFUN2(DOUBLE, SLA_DVDV, sla_dvdv, DOUBLEV, DOUBLEV)
+#define slaDvdv(VA, VB) \
+     CCALLSFFUN2(SLA_DVDV, sla_dvdv, DOUBLEV, DOUBLEV, VA, VB)
+
+PROTOCCALLSFSUB6(SLA_EVP, sla_evp, DOUBLE, DOUBLE, DOUBLEV, DOUBLEV, \
+		 DOUBLEV, DOUBLEV)
+#define slaEvp(DATE, DEQX, DVB, DPB, DVH, DPH) \
+     CCALLSFSUB6(SLA_EVP, sla_evp, DOUBLE, DOUBLE, DOUBLEV, DOUBLEV, \
+		 DOUBLEV, DOUBLEV, DATE, DEQX, DVB, DPB, DVH, DPH)
+#else
+#include "slalib.h"
+#include "slamac.h"
+#endif
+
+#include "calfuse.h"
+ 
+double helio_vel(double mjdate, double ra, double dec)
+{
+    /* Define variables. */
+    double dvb[3], dpb[3], dvh[3], dph[3], vect[3];
+    /*
+     *  Evp returns four 3-vectors containing the barycentric velocity and
+     *  position (dvb,dpb) and the heliocentric velocity and position 
+     *  (dvh,dph) of the Earth on the date mjdate.  It requires a modified 
+     *  Julian date as input.  Output has units of AU for positions and 
+     *  AU/s for velocities.
+     */
+    slaEvp(mjdate, 2000.0, dvb, dpb, dvh, dph);
+
+    /*  Convert the J2000.0 RA and DEC into a 3-vector position */
+
+    slaDcs2c(RADIAN*ra, RADIAN*dec, vect);
+    /*
+     *  Compute the dot product of the RA DEC position vector and the 
+     *  heliocentric velocity vector.  Mutliply by km/AU to get velocity 
+     *  in km/s.
+     */
+    return slaDvdv(vect, dvh)*149.5978707E6;
+}
diff --git a/src/libcf/lsrd_vel.c b/src/libcf/lsrd_vel.c
new file mode 100644
index 0000000..a90c22b
--- /dev/null
+++ b/src/libcf/lsrd_vel.c
@@ -0,0 +1,51 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    double lsrd_vel(double ra, double dec)
+ *
+ * Description: Computes the Sun's velocity in the direction 
+ *              of ra,dec to convert to a LSR.  In this case we
+ *              are using the dynamical solar motion of 
+ *              16.6 km/s towards l=53, b=+25.
+ *
+ * Arguments:   double ra             (deg) J2000.0 right ascension
+ *              double dec            (deg) J2000.0 declination 
+ *
+ * Returns:     double                (km/s) velocity in direction of source
+ *                    
+ * Calls:       slaRvlsrd             rvslrd.f
+ *
+ * History:     03/05/98  E. Murphy   Begin work.
+ *              03/05/98  E. Murphy   Initial version working
+ *              05/31/00        peb   Implemented cfortran.h calls for slalib
+ *                                    functions.
+ *              06/15/01  V. Dixon    Multiply return value by -1.0 to agree
+ *				      with astronomical convention.
+ *              12/18/03    bjg       Change calfusettag.h to calfuse.h
+ *
+ * References:  This routine makes use of the Starlink set of astronomical
+ *              subroutines (SLALIB).  More information can be found at
+ *              http://star-www.rl.ac.uk.
+ ****************************************************************************/
+ 
+#include <stdio.h>
+
+#ifdef CFORTRAN
+#include "cfortran.h"
+PROTOCCALLSFFUN2(FLOAT, SLA_RVLSRD, sla_rvlsrd, FLOAT, FLOAT)
+#define slaRvlsrd(R2000, D2000) \
+     CCALLSFFUN2(SLA_RVLSRD, sla_rvlsrd, FLOAT, FLOAT, R2000, D2000)
+#else
+#include "slalib.h"
+#include "slamac.h"
+#endif
+
+#include "calfuse.h"
+ 
+double lsrd_vel(double ra, double dec)
+{
+    return -1.0 * slaRvlsrd((float) ra*RADIAN, (float) dec*RADIAN);
+}
diff --git a/src/libcf/lsrk_vel.c b/src/libcf/lsrk_vel.c
new file mode 100644
index 0000000..15f5a6c
--- /dev/null
+++ b/src/libcf/lsrk_vel.c
@@ -0,0 +1,52 @@
+/****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ ****************************************************************************
+ *
+ * Synopsis:    double lsrk_vel(double ra, double dec)
+ *
+ * Description: Computes the Sun's velocity in the direction 
+ *              of ra,dec to convert to a LSR.  In this case we
+ *              are using standard solar motion of 
+ *              20 km/s towards RA 18h Dec +30d (1900).
+ *
+ * Arguments:   double ra             (deg) J2000.0 right ascension
+ *              double dec            (deg) J2000.0 declination 
+ *
+ * Returns:     double                (km/s) velocity in direction of source
+ *                    
+ * Calls:       slaRvlsrk             rvlsrk.f
+ *
+ * History:     03/05/98  E. Murphy   Begin work.
+ *              03/05/98  E. Murphy   Initial version working
+ *              04/13/99  E. Murphy   Clean up a bit
+ *              05/31/00        peb   Implemented cfortran.h calls for slalib
+ *                                    functions.
+ *              06/15/01  V. Dixon    Multiply return value by -1.0 to agree
+ *                                    with astronomical convention.
+ *              12/18/03    bjg       Change calfusettag.h to calfuse.h
+ *
+ * References:  This routine makes use of the Starlink set of astronomical
+ *              subroutines (SLALIB).  More information can be found at
+ *              http://star-www.rl.ac.uk.
+ ****************************************************************************/
+ 
+#include <stdio.h>
+
+#ifdef CFORTRAN
+#include "cfortran.h"
+PROTOCCALLSFFUN2(FLOAT, SLA_RVLSRK, sla_rvlsrk, FLOAT, FLOAT)
+#define slaRvlsrk(R2000, D2000) \
+     CCALLSFFUN2(SLA_RVLSRK, sla_rvlsrK, FLOAT, FLOAT, R2000, D2000)
+#else
+#include "slalib.h"
+#include "slamac.h"
+#endif
+
+#include "calfuse.h"
+
+double lsrk_vel(double ra, double dec)
+{
+    return -1.0 * slaRvlsrk((float) ra*RADIAN, (float) dec*RADIAN);
+}
diff --git a/src/libcf/month_day.c b/src/libcf/month_day.c
new file mode 100644
index 0000000..1ecfae1
--- /dev/null
+++ b/src/libcf/month_day.c
@@ -0,0 +1,19 @@
+/* month_day: return month,day from day of year */
+/*	07/21/04    1.4   wvd	Add () to defn of leap */
+
+#include "calfuse.h"
+
+void month_day(int year, int yearday, int *pmonth, int *pday)
+{
+    static char daytab[2][13]={
+	{0,31,28,31,30,31,30,31,31,30,31,30,31},
+	{0,31,29,31,30,31,30,31,31,30,31,30,31}
+    };
+    int i, leap;
+
+    leap = ((year%4 == 0 && year%100 != 0) || year%400 == 0);
+    for (i=1; yearday>daytab[leap][i]; i++)
+	yearday-=daytab[leap][i];
+    *pmonth=i;
+    *pday=yearday;
+}
diff --git a/src/libcf/pole_ang.c b/src/libcf/pole_ang.c
new file mode 100644
index 0000000..ae90cc2
--- /dev/null
+++ b/src/libcf/pole_ang.c
@@ -0,0 +1,64 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    double pole_ang(double *pos, double *vel, double ra, double dec)
+ *
+ * Description: Computes the position of the orbit pole from the given state 
+ *		6-vector.  Returns the angle between the pole and the given
+ *		RA and DEC.
+ *
+ * Arguments:   double *pos           (km) 3-vector position of satellite
+ *              double *vel           (km/s) 3-vector velocity of satellite
+ *              double ra,dec         (deg) position of source
+ *
+ * Returns:     double                (deg) angle from orbit pole to source
+ *
+ * History:     07/06/06  wvd   1.1   Adapted from space_vel and sun_ang
+ *		04/08/07  wvd	1.2   Cast SGP4_getPole as a void.
+ *
+ * References:  This routine makes use of the Starlink set of astronomical
+ *              subroutines (SLALIB).  More information can be found at
+ *              http://star-www.rl.ac.uk.
+ *****************************************************************************/
+ 
+#include <stdio.h>
+
+#ifdef CFORTRAN
+#include "cfortran.h"
+PROTOCCALLSFSUB3(SLA_DCC2S, sla_dcc2s, DOUBLEV, PDOUBLE, PDOUBLE)
+#define slaDcc2s(V, A, B) \
+     CCALLSFSUB3(SLA_DCC2S, sla_dcc2s, DOUBLEV, PDOUBLE, PDOUBLE, V, A, B)
+PROTOCCALLSFFUN1(DOUBLE, SLA_DRANRM, sla_dranrm, DOUBLE)
+#define slaDranrm(ANGLE) \
+     CCALLSFFUN1(SLA_DRANRM, sla_dranrm, DOUBLE, ANGLE)
+PROTOCCALLSFFUN4(DOUBLE, SLA_DSEP, sla_dsep, DOUBLE, DOUBLE, DOUBLE, DOUBLE)
+#define slaDsep(A1, B1, A2, B2) \
+     CCALLSFFUN4(SLA_DSEP, sla_dsep, DOUBLE, DOUBLE, DOUBLE, DOUBLE, \
+                 A1, B1, A2, B2)
+#else
+#include "slalib.h"
+#include "slamac.h"
+#endif
+
+#include "calfuse.h"
+ 
+double pole_ang(double pos[3], double vel[3], double ra, double dec)
+{
+    double pole[3], ra_pole, dec_pole;
+
+    /* Get 3-vector containing the orbit pole. */
+    (void) SGP4_getPole(pos, vel, pole);
+
+    /* Convert 3-vector into J2000.0 RA and DEC */
+#ifdef CFORTRAN
+    slaDcc2s(pole, ra_pole, dec_pole);
+#else
+    slaDcc2s(pole, &ra_pole, &dec_pole);
+#endif
+
+    /*  Compute the angular separation of RA, DEC and RA_POLE, DEC_POLE */
+    return slaDsep(ra*RADIAN, dec*RADIAN, slaDranrm(ra_pole), dec_pole)/RADIAN;
+}
diff --git a/src/libcf/read_tle.c b/src/libcf/read_tle.c
new file mode 100644
index 0000000..38db069
--- /dev/null
+++ b/src/libcf/read_tle.c
@@ -0,0 +1,303 @@
+/******************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ ******************************************************************************
+ *
+ * Synopsis:    read_tle(fitsfile *fptr)
+ *
+ * Description: read_tle will read the standard tle format file FUSE.TLE 
+ *              and place the orbital elements into the header of the
+ *              fitsfile.  The FUSE.TLE file will contain multiple orbital 
+ *              element sets, so the set closest in time to the observation
+ *              will be used.
+ *
+ * Arguments:   fitsfile    *fptr    Pointer to input file
+ *
+ * History:     11/11/98   emurphy   Begin work.
+ *              03/18/98   emurphy   Added To do list.
+ *              04/08/99       peb   Tidied code and added necessary
+ *                                   include files
+ *              06/07/99       peb   Added reporting of version control.
+ *              06/22/99       peb   Added FITS_ wrappers.
+ *              08/05/99       emm   Added statements to print date
+ *                                   of obs and TLE if dtime > 5.
+ *                                   Also modified program to work with
+ *                                   FES keywords TEXPSTRT and TEXPEND
+ *              05/31/00       peb   Implemented cfortran.h calls for slalib
+ *                                   functions.
+ *		02/13/03 v1.4  wvd   Change 0 to NULL in FITS_update_key
+ *              03/01/03 v1.5  wvd   Correct use of pointer in FITS_read_key
+ *              04/01/03 v1.6  wvd   Replace cf_errmsg with cf_if_warning,
+ *					printf with cf_verbose
+ *              12/18/03 v1.7  bjg   Change calfusettag.h to calfuse.h
+ *              04/07/07 v1.8  wvd   Initialize min_mjd to zero to silence
+ *					compiler warnings.
+ *
+ *****************************************************************************/
+
+#include <math.h>
+#include <stdio.h>
+#include <stdlib.h>
+#include <string.h>
+
+#ifdef CFORTRAN
+#include "cfortran.h"
+PROTOCCALLSFSUB5(SLA_CLDJ, sla_cldj, INT, INT, INT, PDOUBLE, PINT)
+#define slaCldj(IY, IM, ID, DJM, J) \
+     CCALLSFSUB5(SLA_CLDJ, sla_cldj, INT, INT, INT, PDOUBLE, PINT, \
+		 IY, IM, ID, DJM, J)
+#else
+#include "slalib.h"
+#include "slamac.h"
+#endif
+
+#include "calfuse.h"
+
+#define  MAXCHARS 120
+static char CF_PRGM_ID[] = "read_tle";
+static char CF_VER_NUM[] = "1.8";
+
+void read_tle(fitsfile *fptr)
+{
+    char   line1[MAXCHARS], line2[MAXCHARS], line3[MAXCHARS];
+    char   sat_num[10], security_class[10], international_num[10];
+    char   inchar[15][15], sp[15][2], sgn[4][2];
+    char   comment[FLEN_CARD], eccen_str[20];
+    char   n6_mant_str[20], drag_mant_str[20], instrument[FLEN_CARD];
+    int    status=0, hdutype=0, card_num, epoch_year, n6_exponent;
+    int    drag_exponent, ephemeris, elset_num, checksum1, checksum2; 
+    int    rev_num, e_month, e_day;
+    double n6_mantissa, drag_mantissa, epoch_day, n2, inclin, raan;
+    double aop, mean_anom, mean_mot, n6, drag, semimaj, revspersec;
+    double expstart, expend, expmiddle, eccentr, dtime=1.0e9;
+    double i_day, f_day, mjd, mjd_f, mjd_d, min_mjd=0;
+    FILE   *ftle;
+
+    /* Enter a timestamp into the log. */
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Begin reading TLE file");
+
+    /*  Open the file with the standard two-line elements. */
+    ftle = NULL;
+    ftle = fopen(cf_cal_file("FUSE.TLE"),"r");
+    if (ftle == NULL)
+	cf_if_error("Cannot find file FUSE.TLE, which contains the"
+		  " orbital elements.");
+
+    /*  Rewind the fits file and get the start time of the exposure */
+    FITS_movabs_hdu(fptr, 1, &hdutype, &status);
+    FITS_read_key(fptr, TSTRING, "INSTRUME", instrument, comment, &status);
+
+    /* In the primary header, the FES files use keywords with a different
+       name.  This is because the FES may have many exposures in a file.
+       The TEXPSTRT is the start of the first exposure and TEXPEND is the
+       end of the last exposure. */
+    if (!strncmp(instrument,"FES",3)) {
+         /* Read in FES keywords */
+         FITS_read_key(fptr, TDOUBLE, "TEXPSTRT", &expstart, comment, &status);
+         FITS_read_key(fptr, TDOUBLE, "TEXPEND", &expend, comment, &status);
+    } else {
+         /* Read in FUV keywords */
+         FITS_read_key(fptr, TDOUBLE, "EXPSTART", &expstart, comment, &status);
+         FITS_read_key(fptr, TDOUBLE, "EXPEND", &expend, comment, &status);
+    }
+
+    /* expmiddle is in mjd */
+    expmiddle = (expstart+expend)/2.0;
+
+    /*  Read in FUSE.TLE file by getting one line at a time  */
+    while (fgets(line1, MAXCHARS,ftle) != NULL) {
+	fgets(line2, MAXCHARS, ftle);
+	fgets(line3, MAXCHARS, ftle);
+
+#ifdef DEBUG
+	printf("\n\n%-80.80s\n",line1);
+	printf("%-80.80s\n",line2);
+	printf("%-80.80s\n",line3);
+#endif
+	/*
+	 *  This may look like a stupid way to do this, but it has to be
+	 *  done this way.  You see, the fields can contain leading blanks
+	 *  which should be interpreted as zeros.  However, c skips over
+	 *  leading blanks when reading %f and %d.
+	 */
+	sscanf(line2,"%1c%1c%5c%1c%1c%8c%1c%2c%12c%1c%1c%9c%1c%1c%5c%2c%1c"
+	       "%1c%5c%2c%1c%1c%1c%4c%1c",
+	       inchar[1],sp[1],inchar[2],inchar[3],sp[2],inchar[4],sp[3],
+	       inchar[5],inchar[6],sp[4],sgn[1],inchar[7],sp[5],sgn[2],
+	       inchar[8],inchar[9],sp[6],sgn[3],inchar[10],inchar[11],
+	       sp[7],inchar[12], sp[8],inchar[13],inchar[14]);
+
+	inchar[1][1]='\0';
+	card_num=atoi(inchar[1]);
+
+	inchar[2][5]='\0';
+	strncpy(sat_num,inchar[2],5);
+
+	inchar[3][1]='\0';
+	strncpy(security_class,inchar[3],1);
+
+	inchar[4][8]='\0';
+	strncpy(international_num,inchar[4],8);
+
+	inchar[5][2]='\0';
+	epoch_year=atoi(inchar[5]);
+	if (epoch_year < 50)
+	    epoch_year+=2000;
+	else
+	    epoch_year+=1900;
+
+	inchar[6][12]='\0';
+	epoch_day=atof(inchar[6]);
+
+	inchar[7][9]='\0';
+	n2=atof(inchar[7]);
+	if (sgn[1][0] == '-')
+	    n2*=-1.0;
+
+	inchar[8][5]='\0';
+	strcpy(n6_mant_str,"0.");
+	strncat(n6_mant_str,inchar[8],7);
+#ifdef DEBUG
+	printf("n6=%-10.10s\n",n6_mant_str);
+#endif
+	n6_mantissa=atof(n6_mant_str);
+	if (sgn[2][0] == '-')
+	    n6_mantissa*=-1.0;
+
+	inchar[9][2]='\0';
+	n6_exponent=atoi(inchar[9]);
+
+	inchar[10][5]='\0';
+	strcpy(drag_mant_str,"0.");
+	strncat(drag_mant_str,inchar[10],7);
+#ifdef DEBUG
+	printf("Drag=%-10.10s\n",drag_mant_str);
+#endif
+	drag_mantissa=atof(drag_mant_str);
+	if (sgn[3][0] == '-')
+	    drag_mantissa*=-1.0;
+
+	inchar[11][2]='\0';
+	drag_exponent=atoi(inchar[11]);
+
+	inchar[12][1]='\0';
+	ephemeris=atoi(inchar[12]);
+
+	inchar[13][4]='\0';
+	elset_num=atoi(inchar[13]);
+
+	inchar[14][1]='\0';
+	checksum1=atoi(inchar[14]);
+
+	n6=n6_mantissa*pow(10.0,(double) n6_exponent);
+	drag=drag_mantissa*pow(10.0,(double) drag_exponent);
+
+#ifdef DEBUG
+	printf("n6=>%10.5f %5d %15.6E\n", n6_mantissa, n6_exponent, n6);
+	printf("drag=>%10.5f %5d %15.6E\n", drag_mantissa,
+	       drag_exponent, drag);
+	for(i=1; i<=14; i++)
+	    printf("%2d %-15.15s\n",i,inchar[i]);
+	for(i=1; i<=3; i++)
+	    printf("%2d %-5.5s\n",i,sgn[i]);
+#endif
+	sscanf(line3,"%1c%1c%5c%1c%8c%1c%8c%1c%7c%1c%8c%1c%8c%1c%11c%5c%1c",
+	       inchar[1],sp[1],inchar[2],sp[2],inchar[3],sp[3],inchar[4],
+	       sp[4],inchar[5],sp[5],inchar[6],sp[6],inchar[7],sp[7],
+	       inchar[8],inchar[9],inchar[10]);
+	inchar[1][1]='\0';
+	card_num=atoi(inchar[1]);
+
+	inchar[2][5]='\0';
+	strncpy(sat_num,inchar[2],5);
+
+	inchar[3][8]='\0';
+	inclin=atof(inchar[3]);
+
+	inchar[4][8]='\0';
+	raan=atof(inchar[4]);
+
+	inchar[5][7]='\0';
+	/* 
+	 *  strcpy(eccen_str,"0.");
+	 *  strncat(eccen_str,inchar[5],8);
+	 */
+	sprintf(eccen_str,"0.%-8s",inchar[5]);
+#ifdef DEBUG
+	printf("Ecstr=%-20.20s\n",eccen_str);
+#endif
+	eccentr=atof(eccen_str);
+
+	inchar[6][8]='\0';
+	aop=atof(inchar[6]);
+
+	inchar[7][8]='\0';
+	mean_anom=atof(inchar[7]);
+
+	inchar[8][11]='\0';
+	mean_mot=atof(inchar[8]);
+
+	inchar[9][5]='\0';
+	rev_num=atof(inchar[9]);
+
+	inchar[10][1]='\0';
+	checksum2=atoi(inchar[10]);
+
+#ifdef DEBUG
+	for(i=1; i<=10; i++)
+	    printf("%2d %-15.15s\n",i,inchar[i]);
+	printf("%4d\n%12.8f\n%10.8f\n%10.5E\n%10.5E%5d%5d%5d\n",
+	       epoch_year, epoch_day, n2, n6, drag, ephemeris,
+	       elset_num, checksum1);
+	printf("\n%8.4f\n%8.4f\n%10.8f\n%8.4f\n%8.4f\n%11.8f\n%5d\n%1d\n",
+	       inclin, raan, (float) eccentr, aop, mean_anom,
+	       mean_mot, rev_num, checksum2);  
+#endif
+	/* Convert the year and day of year into a year month day */
+
+	f_day = modf(epoch_day, &i_day);
+
+	month_day(epoch_year, (int) i_day, &e_month, &e_day);
+
+	/* Convert year month day into a Julian date. */
+#ifdef CFORTRAN
+	slaCldj(epoch_year, e_month, e_day, mjd, status);
+#else
+	slaCldj(epoch_year, e_month, e_day, &mjd, &status);
+#endif
+
+	mjd += f_day;
+
+	if (fabs(expmiddle-mjd) < dtime) {
+	    dtime = fabs(expmiddle-mjd);
+            min_mjd=mjd;
+	    revspersec = mean_mot/(24.0*60.0*60.0);
+	    semimaj = pow(MU/(4.0*PI*PI*revspersec*revspersec),1.0/3.0);
+            mjd_f=modf(mjd, &mjd_d);
+            FITS_update_key(fptr, TDOUBLE, "EPCHTIMD", &mjd_d, NULL, &status);
+            FITS_update_key(fptr, TDOUBLE, "EPCHTIMF", &mjd_f, NULL, &status);
+	    FITS_update_key(fptr, TDOUBLE, "INCLINAT", &inclin, NULL, &status);
+	    FITS_update_key(fptr, TDOUBLE, "ECCENTRY", &eccentr, NULL, &status);
+	    FITS_update_key(fptr, TDOUBLE, "MEANANOM", &mean_anom, NULL,&status);
+	    FITS_update_key(fptr, TDOUBLE, "ARGPERIG", &aop, NULL, &status);
+	    FITS_update_key(fptr, TDOUBLE, "RASCASCN", &raan, NULL, &status);
+	    FITS_update_key(fptr, TDOUBLE, "SEMIMAJR", &semimaj, NULL, &status);
+	    FITS_update_key(fptr, TDOUBLE, "MEANMOTN", &mean_mot, NULL, &status);
+	    FITS_update_key(fptr, TDOUBLE, "FDM2COEF", &n2, NULL, &status);
+	    FITS_update_key(fptr, TDOUBLE, "SDM6COEF", &n6, NULL, &status);
+	    FITS_update_key(fptr, TDOUBLE, "DRAGCOEF", &drag, NULL, &status);
+	    FITS_update_key(fptr, TSTRING, "PROPMODL", "SGP4", NULL, &status);
+	}
+    }  /* endwhile */
+
+    if (dtime > 5.0) {
+        cf_verbose(2, "MJD OBS=%12.5f MJD TLE=%12.5f DT=%12.5f\n", 
+                     expmiddle, min_mjd, dtime);
+	cf_if_warning("Orbital elements are more than 5 days old.");
+        }
+
+    /* Enter a timestamp into the log. */
+    cf_timestamp(CF_PRGM_ID, CF_VER_NUM, "Done reading TLE file");
+}
+
diff --git a/src/libcf/saa.c b/src/libcf/saa.c
new file mode 100644
index 0000000..0d2d0e3
--- /dev/null
+++ b/src/libcf/saa.c
@@ -0,0 +1,74 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    int saa(saareg *saa, double lon, double lat)
+ *
+ * Description: Determines if FUSE is in the SAA for given models of the SAA
+ *              
+ *
+ * Arguments:   saareg *saa           A structure containing data that roughly
+ *                                    outlines the SAA region.
+ *                                    (n_points: number of points
+ *                                     lat:    the latitude array
+ *                                     lon: the longitude array)
+ *                                    (currently we have only one model).
+ *              double lon,lat        Geocentric longitude and latitude of FUSE
+ *
+ * Returns:     int                   0 if not in SAA
+ *                                    1 if in SAA
+ *                    
+ * History:     07/17/98  E. Murphy   Begin work.
+ *              06/22/99        peb   Tidied code, added FITS_ wrappers,
+ *                                    removed hardcoded variables.
+ *              07/02/99        peb   Moved SAA data to a structure.
+ *              08/25/99        emm   Fixed bug in setting maxlon
+ *              08/28/03 v1.3   bjg   Adopt Bryce's algorithm for determining
+ *					when FUSE is in the SAA.
+ *              08/28/03 v1.4   bjg   v1.3 didn't compile but v1.4 does
+ *              08/29/03 v1.5   bjg   slightly modified getDir
+ *
+ ****************************************************************************/
+ 
+#include "calfuse.h"
+
+int getDir(double lon0,double lat0,double lon1,double lat1,double lon2,double lat2)
+{
+
+double dx1, dx2, dy1, dy2, t1, t2;
+    
+  dx1=lon1-lon0; dy1=lat1-lat0;
+  dx2=lon2-lon0; dy2=lat2-lat0;
+
+  t1=dx1*dy2; t2=dy1*dx2;
+
+  if (t1>t2) 
+    return(-1);
+  if (t1<t2) 
+    return(1);
+  
+
+  return(1);
+
+}
+
+
+int
+saa(saareg *saa, double lon, double lat)
+{
+int i;
+int dir=0;
+int oldDir=0;
+
+for (i=0; i<saa->n_points-1; i++) {
+    dir=getDir(lon,lat,(double)(saa->lon[i]),(double)(saa->lat[i]),(double)(saa->lon[i+1]),(double)(saa->lat[i+1]));
+    if (dir*oldDir<0)
+      return(0);
+    else
+      oldDir=dir;
+    }
+    
+  return(1);
+}
diff --git a/src/libcf/set_orbit_parms.c b/src/libcf/set_orbit_parms.c
new file mode 100644
index 0000000..65baca6
--- /dev/null
+++ b/src/libcf/set_orbit_parms.c
@@ -0,0 +1,86 @@
+/*****************************************************************************
+ *	      Johns Hopkins University
+ *	      Center For Astrophysical Sciences
+ *	      FUSE
+ *****************************************************************************
+ *
+ * Synopsis:	SGP4 set_orbit_parms(fitsfile *infits)
+ *
+ * Description: Initialized the sgp4 structure and reads the orbital 
+ *              paramaters from the infits header and places the data 
+ *              in the sgp4 structure.  It also calculates a number of
+ *              time invariant quantities in the sgp4 structure.
+ *
+ * Arguments:	fitsfile   *infits        Input FITS file.
+ *
+ * Return:      SGP4       sgp4	          Structure with orb parms.
+ *
+ * History:	07/07/99	emurphy	 Begin and finished work
+ *              07/14/99        emurphy  Fixed minor bugs
+ *              07/21/99        peb      Changed function to return SGP4
+ *                                       pointer. (This fixes a bug.)
+ *              08/05/99        emurphy  Converted to use set_orbit_parms_calc
+ *                                       so that FES pipeline can use these 
+ *                                       routines.
+ *              12/18/03        bjg      Change calfusettag.h to calfuse.h
+ *              04/07/07  1.4	wvd	 Delete CF_PRGM_ID and CF_VER_NUM, 
+ *					 as they are not used.
+ *
+ ****************************************************************************/
+
+#include <stdio.h>
+#include "calfuse.h"
+#include "sgp4.h"
+
+SGP4 set_orbit_parms_calc(fitsfile *infits)
+{
+    int    status=0;
+    char   comment[FLEN_CARD];
+    double epchtime, td, tf, inclinat, eccentry, meananom, argperig, rascascn;
+    double n0dt, n0dt2, bstar, mean_motion;
+    SGP4   sgp4;
+             
+    /*  Get the orbital data from the header of the infits file. */
+    FITS_read_key(infits, TDOUBLE, "EPCHTIMD", &td, comment, &status);
+    FITS_read_key(infits, TDOUBLE, "EPCHTIMF", &tf, comment, &status);
+    epchtime=td+tf;    
+    FITS_read_key(infits, TDOUBLE, "INCLINAT", &inclinat, comment, &status);
+    FITS_read_key(infits, TDOUBLE, "ECCENTRY", &eccentry, comment, &status);
+    FITS_read_key(infits, TDOUBLE, "MEANANOM", &meananom, comment, &status);
+    FITS_read_key(infits, TDOUBLE, "ARGPERIG", &argperig, comment, &status);
+    FITS_read_key(infits, TDOUBLE, "RASCASCN", &rascascn, comment, &status);
+    FITS_read_key(infits, TDOUBLE, "FDM2COEF", &n0dt, comment, &status);
+    FITS_read_key(infits, TDOUBLE, "SDM6COEF", &n0dt2, comment, &status);
+    FITS_read_key(infits, TDOUBLE, "DRAGCOEF", &bstar, comment, &status);
+    FITS_read_key(infits, TDOUBLE, "MEANMOTN", &mean_motion, comment, &status);
+
+    sgp4 = SGP4_create();
+
+    SGP4_set(sgp4, epchtime, n0dt, n0dt2,  bstar, inclinat,
+	     rascascn, eccentry, argperig, meananom, mean_motion);
+
+    /* do time invariant initializations */
+    SGP4_init(sgp4);
+    return sgp4;
+}
+
+SGP4 set_orbit_parms(fitsfile *infits)
+{
+    int    status=0, hdunum=0, hdutype;
+    SGP4   sgp4;
+    /*
+     *  The infits file pointer may be down in one of the extensions
+     *  whereas the orbital info is in the primary hdu.  Therefore,
+     *  record the current position, move to the primary header, 
+     *  set the orbital data, and return to the previous hdu.
+     */
+    FITS_get_hdu_num(infits, &hdunum);
+    FITS_movabs_hdu(infits, 1, &hdutype, &status);
+
+    sgp4=set_orbit_parms_calc(infits);
+
+    FITS_movabs_hdu(infits, hdunum, &hdutype, &status);
+
+    return sgp4;
+
+}
diff --git a/src/libcf/sgp4.c b/src/libcf/sgp4.c
new file mode 100644
index 0000000..b14dc45
--- /dev/null
+++ b/src/libcf/sgp4.c
@@ -0,0 +1,426 @@
+/* H+
+ *      Title     : sgp4.c
+ *      Author    : Bryce A. Roberts
+ *      Date      : 23 February 1999
+ *      Synopsis  : implementation of SGP4 propagation routines
+ *      SCCS      : @(#)sgp4.c	1.6 05/14/00
+ *      Revisions :
+ *      mm/dd/yy name   description
+ *      01/14/00 ma     get rid of unused function get_time (May 14 2000)
+ *      12/18/03 bjg    Change calfusettag.h to calfuse.h 
+* H-
+ */
+
+#include <string.h>
+#include <time.h>
+#include "calfuse.h"
+#include "sgp4.h"
+
+/* define some absolute constants used by SGP4 */
+#define MIN_PER_DAY  (1440.0)
+#define KM_PER_EARTH (6378.135)
+#define TWOBYTHREE   (2.0/3.0)
+#define Q0           (120.0)
+#define S0           (78.0)
+#define THREEPIBYTWO (PIBY2*3.0)
+#define KE           (0.074366916)
+#define AE           (1.0)
+#define S            (AE*(1.0+S0/KM_PER_EARTH))
+#define Q0MS4        pow((Q0-S0)*AE/KM_PER_EARTH, 4)
+#define CK2          (0.5*J2*AE*AE)
+#define CK4          (-0.375*J4*AE*AE*AE*AE)
+#define A30          (-J3/AE*AE*AE)
+
+#ifndef J2
+#define J2           (1.082616E-3)
+#endif
+
+#ifndef J3
+#define J3           (-0.253881E-5)
+#endif
+
+#ifndef J4
+#define J4           (-1.65597E-6)
+#endif
+
+#ifndef PI
+#define PI (3.141592653589793)
+#endif
+
+#ifndef TWOPI
+#define TWOPI (2.0*PI)
+#endif
+
+#define RAD2DEG(x) (((x)*180.0)/PI)
+#define DEG2RAD(x) ((PI/180.0)*(x))
+
+#ifndef false
+#define false (0)
+#endif
+
+#ifndef true
+#define true (1)
+#endif
+
+
+/*
+ * Name:     SGP4_isLeap
+ * Purpose:  determine if a given year is a leap year 
+ * Input:    int year (e.g. 1999)
+ * Output:   returns 1 if leap year, 0 if not
+ */
+static int SGP4_isLeap(int year) {
+  return(((year%4==0 && year%100!=0) || year%400==0));
+  }
+
+
+/*
+ * Name:     SGP4_doy2cal
+ * Purpose:  convert year/day-of-year to Gregorian calendar month and day
+ * Input:    int year, doy
+ * Output:   int *month, int *day, returns 0 for fail, 1 for success
+ */
+static int SGP4_doy2cal(int year, int doy, int *month, int *day) {
+  /* number of days in leap and non-leap year months */
+  static int daytab[2][13]={{0,31,28,31,30,31,30,31,31,30,31,30,31},
+                            {0,31,29,31,30,31,30,31,31,30,31,30,31}};
+  int leap;
+
+  /* do range checking */
+  if (doy<1 || doy>366)
+    return(false);
+  
+  leap=SGP4_isLeap(year) ? 1 : 0;
+  *day=doy;
+  for (*month=1; *day>daytab[leap][*month]; (*month)++)
+    *day-=daytab[leap][*month];
+  
+  return(true);
+  }
+
+
+/*
+ * Name:     SGP4_create
+ * Purpose:  creates an instance of SGP4
+ * Input:    none
+ * Output:   SGP4 
+ */
+SGP4 SGP4_create(void) {
+  return((SGP4)calloc(1, sizeof(struct sgp4_st)));
+  }
+
+
+/*
+ * Name:     SGP4_destroy
+ * Purpose:  destroys an instance of SGP4
+ * Input:    SGP4 sgp4
+ * Output:   none
+ */
+void SGP4_destroy(SGP4 sgp4) {
+  if (sgp4)
+    free(sgp4);
+  }
+
+
+/*
+ * Name:     SGP4_init
+ * Purpose:  initializes time-invariant SGP4 variables
+ * Input:    SGP4 sgp4
+ * Output:   none
+ */
+void SGP4_init(SGP4 sgp4) {
+  double a1, del1, a0, del0, perigee, sStar, eta_2, eta_3, eta_4, pinvsq, 
+    temp1, temp2, temp3, x3thetam1, x1m5th, xhdot1, theta_4, zeta, zeta_2, 
+    zeta_3, zeta_5, beta0, beta0_3, beta0_4, C2;
+
+  /* recover original mean motion and semimajor axis from the elements */
+  a1=pow(KE/sgp4->n0, TWOBYTHREE);
+  del1=1.5 * (CK2/(a1*a1))*((3*cos(sgp4->i0)*cos(sgp4->i0)-1.0)/
+    pow(1-sgp4->e0*sgp4->e0, 1.5));
+  a0=a1*(1-del1/3.0-del1*del1-(134.0/81.0)*del1*del1*del1);
+  del0=(del1*a1*a1)/(a0*a0);
+
+  /* find original mean motion, n0dp (n0'') */
+  sgp4->n0dp=sgp4->n0/(1+del0); 
+
+  /* find semimajor axis, a0dp (a0'') */
+  sgp4->a0dp=a0/(1-del0);
+
+  /* find the perigee (in km) */
+  perigee=(sgp4->a0dp*(1.0-sgp4->e0)-AE)*KM_PER_EARTH;
+  
+  /* make decisions on what value of s to use based on perigee */
+  if (perigee<=156.0 && perigee>=98.0) {
+    sStar=sgp4->a0dp*(1.0-sgp4->e0)-S-AE;
+    sgp4->q0ms4=pow(pow(Q0MS4, 0.25) + S - sStar, 4);
+    }
+  else if (perigee<98.0) {
+    sStar=20/KM_PER_EARTH + AE;
+    sgp4->q0ms4=pow(pow(Q0MS4, 0.25) + S - sStar, 4);
+    }
+  else {
+    sStar=S;
+    sgp4->q0ms4=Q0MS4;
+    }
+
+  sgp4->theta=cos(sgp4->i0); sgp4->theta_2=sgp4->theta*sgp4->theta; 
+  theta_4=sgp4->theta_2*sgp4->theta_2;
+  zeta=1/(sgp4->a0dp-sStar);
+  
+  zeta_2=zeta*zeta, zeta_3=zeta_2*zeta; 
+  sgp4->zeta_4=zeta_3*zeta;
+  zeta_5=sgp4->zeta_4*zeta;
+
+  sgp4->beta0_2=1-sgp4->e0*sgp4->e0;
+  beta0=sqrt(sgp4->beta0_2); beta0_3=sgp4->beta0_2*beta0; 
+  beta0_4=beta0_3*beta0;
+
+  sgp4->eta=sgp4->a0dp*sgp4->e0*zeta;
+  eta_2=sgp4->eta*sgp4->eta, eta_3=eta_2*sgp4->eta, eta_4=eta_3*sgp4->eta;
+  
+  C2=sgp4->q0ms4*(sgp4->zeta_4)*sgp4->n0dp*pow(1-eta_2, -7.0/2.0)*
+    (sgp4->a0dp*(1+ ((3.0/2.0)*eta_2) + 4*sgp4->e0*sgp4->eta + 
+    sgp4->e0*eta_3) + (3.0/2.0)*(CK2*zeta/(1-eta_2))*(-0.5 + 
+    1.5*sgp4->theta_2)*(8.0+24*eta_2 + 3*eta_4));
+  sgp4->C1=sgp4->bstar*C2; sgp4->C1_2=sgp4->C1*sgp4->C1; 
+  sgp4->C1_3=sgp4->C1_2*sgp4->C1; sgp4->C1_4=sgp4->C1_3*sgp4->C1;
+  sgp4->C3=(sgp4->q0ms4*(zeta_5)*A30*sgp4->n0dp*AE*sin(sgp4->i0))/
+    (CK2*sgp4->e0);
+  sgp4->C4=2*sgp4->n0dp*sgp4->q0ms4*(sgp4->zeta_4)*sgp4->a0dp*(sgp4->beta0_2)*
+    pow(1-eta_2, -7.0/2.0)*( (2*sgp4->eta*(1+sgp4->e0*sgp4->eta)+
+    0.5*sgp4->e0+0.5*eta_3)-2*CK2*zeta/(sgp4->a0dp*(1-eta_2))*
+   (3*(1-3*sgp4->theta_2)*(1 + 1.5*eta_2 -2*sgp4->e0*sgp4->eta - 
+   0.5*sgp4->e0*eta_3) + 0.75*(1-sgp4->theta_2)*(2*eta_2 - 
+   sgp4->e0*sgp4->eta - sgp4->e0*eta_3)*cos(2*sgp4->w0)));
+  sgp4->C5=2*sgp4->q0ms4*(sgp4->zeta_4)*sgp4->a0dp*(sgp4->beta0_2)*
+    pow(1-eta_2, -7.0/2.0)*(1 + (11.0/4.0)*sgp4->eta*(sgp4->eta+sgp4->e0)+
+    sgp4->e0*eta_3);
+
+  sgp4->D2=4*sgp4->a0dp*zeta*sgp4->C1_2;
+  sgp4->D3=(4.0/3.0)*sgp4->a0dp*zeta_2*(17*sgp4->a0dp + 
+    sStar)*sgp4->C1_3;
+  sgp4->D4=TWOBYTHREE*sgp4->a0dp*zeta_3*(221*sgp4->a0dp+
+    31*sStar)*sgp4->C1_4;
+
+  /* constants for secular effects calculation */
+  pinvsq=1.0/(sgp4->a0dp*sgp4->a0dp*beta0_4);
+  temp1=3.0*CK2*pinvsq*sgp4->n0dp;
+  temp2=temp1*CK2*pinvsq;
+  temp3=1.25*CK4*pinvsq*pinvsq*sgp4->n0dp;
+  x3thetam1=3.0*sgp4->theta_2 - 1.0;
+  x1m5th=1.0 - 5.0*sgp4->theta_2;
+  xhdot1=-temp1*sgp4->theta;
+
+  sgp4->mdot=sgp4->n0dp+0.5*temp1*beta0*x3thetam1+
+    0.0625*temp2*beta0*(13.0 - 78.0*sgp4->theta_2+137.0*theta_4);
+
+  sgp4->wdot=-0.5*temp1*x1m5th+0.0625*temp2*(7.0-114.0*sgp4->theta_2+
+    395.0*theta_4)+temp3*(3.0-36.0*sgp4->theta_2+49.0*theta_4);
+  
+  sgp4->raandot=xhdot1+(0.5*temp2*(4.0-19.0*sgp4->theta_2)+2.0*temp3*
+    (3.0-7.0*sgp4->theta_2))*sgp4->theta;
+  }
+
+
+/*
+ * Name:     SGP4_getStateVector
+ * Purpose:  finds position, velocity at a time
+ * Input:    SGP4 sgp4, double t
+ * Output:   double pos[3], double vel[3]
+ */
+void SGP4_getStateVector(SGP4 sgp4, double t, double pos[3], double vel[3]) {
+  double mdf, wdf, raandf, del_w, del_m, mp, w, RAAN, e, a, IL,
+    beta_2, n, axn, ILl, aynl, ILt, ayn, U, initial, eCosE,
+    eSinE, eL_2, pL, r, rDot, rfDot, cosu, sinu, u, rk, uk, RAANk, ik,
+    rDotk, rfDotk, mx, my, ux, uy, uz, vx, vy, vz, tsince;
+  int i;
+
+  /* find the time since the epoch, in minutes */
+  tsince=(t-sgp4->epochTime)*1440;
+
+  /* secular effects of atmospheric drag and gravitation */
+  mdf=sgp4->M0+(sgp4->mdot*tsince);
+  wdf=sgp4->w0+(sgp4->wdot*tsince);
+  raandf=sgp4->raan+(sgp4->raandot*tsince);
+  
+  del_w=sgp4->bstar*sgp4->C3*(cos(sgp4->w0))*tsince;
+  del_m=-TWOBYTHREE*sgp4->q0ms4*sgp4->bstar*sgp4->zeta_4*
+    (AE/(sgp4->e0*sgp4->eta))*(pow(1+sgp4->eta*cos(mdf), 3)-
+    pow(1+sgp4->eta*cos(sgp4->M0), 3));
+  
+  mp=mdf+del_w+del_m;
+  w=wdf-del_w-del_m;
+  
+  RAAN=raandf-(21.0/2.0)*((sgp4->n0dp*CK2*sgp4->theta)/(sgp4->a0dp*
+    sgp4->a0dp*sgp4->beta0_2))* sgp4->C1*tsince*tsince;
+  e=sgp4->e0-sgp4->bstar*sgp4->C4*tsince-sgp4->bstar*sgp4->C5*
+    (sin(mp)-sin(sgp4->M0));
+  
+  a=sgp4->a0dp*pow((1+tsince*(-sgp4->C1+tsince*(-sgp4->D2+tsince*
+    (-sgp4->D3-sgp4->D4*tsince)))), 2);
+  
+  IL=mp+w+RAAN+sgp4->n0dp*tsince*tsince*(1.5*sgp4->C1+tsince*
+    ((sgp4->D2+2*sgp4->C1_2) + tsince*(0.25*(3*sgp4->D3 + 
+    12*sgp4->C1*sgp4->D2 + 10*sgp4->C1_3)+tsince*(0.2*(3*sgp4->D4+12*
+    sgp4->C1*sgp4->D3+6*sgp4->D2*sgp4->D2+30*sgp4->C1_2*sgp4->D2+
+    15*sgp4->C1_4)))));
+
+  beta_2=1-e*e;
+  n=KE/pow(a, 3.0/2.0);
+
+  /* find the long-period periodic terms */
+  axn=e*cos(w);
+  ILl=(A30*sin(sgp4->i0))/(8*CK2*a*beta_2)*(e*cos(w))*((3+5*sgp4->theta)/
+    (1+sgp4->theta));
+  aynl=(A30*sin(sgp4->i0))/(4*CK2*a*beta_2);
+  ILt=IL+ILl;
+  ayn=e*sin(w)+aynl;
+    
+  /* iteratively solve Kepler's equation */
+  U=fmod(ILt-RAAN, TWOPI);
+
+  initial=U;
+  for (i=0; i<10; i++) {
+    U=(initial-ayn*cos(U)+axn*sin(U)-U)/(1.0-ayn*sin(U)-axn*cos(U))+U;
+    }
+
+  /* preliminary quantities for short period periodics */
+  eCosE=axn*cos(U)+ayn*sin(U); 
+  eSinE=axn*sin(U)-ayn*cos(U);
+  eL_2=axn*axn+ayn*ayn;
+  pL=a*(1-eL_2);
+  r=a*(1-eCosE);
+  rDot=KE*(sqrt(a)/r)*eSinE;
+  rfDot=KE*sqrt(pL)/r;
+  cosu=(a/r)*(cos(U)-axn+(ayn*eSinE)/(1+sqrt(1-eL_2)));
+  sinu=(a/r)*(sin(U)-ayn-(axn*eSinE)/(1+sqrt(1-eL_2)));
+  u=fmod(atan2(sinu, cosu)+TWOPI, TWOPI);
+
+  /* update for short-period periodics */
+  rk=r*(1-1.5*CK2*sqrt(1-eL_2)/(pL*pL)*(3*sgp4->theta_2-1))+
+    (CK2/(2*pL))*(1-sgp4->theta_2)*cos(2*u);
+  uk=u+-(CK2/(4*pL*pL))*(7*sgp4->theta_2-1.0)*sin(2*u);;
+  RAANk=RAAN+((3*CK2*sgp4->theta)/(2*pL*pL))*sin(2*u);
+  ik=sgp4->i0+((3*CK2*sgp4->theta)/(2*pL*pL))*sin(sgp4->i0)*cos(2*u);
+  rDotk=rDot-((CK2*n)/pL)*(1-sgp4->theta_2)*sin(2*u);
+  rfDotk=rfDot+((CK2*n)/pL)*((1-sgp4->theta_2)*cos(2*u)-
+  1.5*(1-3*sgp4->theta_2));
+  
+  /* find the position and velocity components */
+  mx=-sin(RAANk)*cos(ik);
+  my=cos(RAANk)*cos(ik);
+  
+  ux=mx*sin(uk)+cos(RAANk)*cos(uk);
+  uy=my*sin(uk)+sin(RAANk)*cos(uk);
+  uz=sin(ik)*sin(uk);
+  
+  vx=mx*cos(uk)-cos(RAANk)*sin(uk);
+  vy=my*cos(uk)-sin(RAANk)*sin(uk);
+  vz=sin(ik)*cos(uk);
+
+  pos[0]=KM_PER_EARTH*rk*ux;
+  pos[1]=KM_PER_EARTH*rk*uy;
+  pos[2]=KM_PER_EARTH*rk*uz;
+
+  vel[0]=MIN_PER_DAY*KM_PER_EARTH*(rDotk*ux+rfDotk*vx)/(AE*86400.0);
+  vel[1]=MIN_PER_DAY*KM_PER_EARTH*(rDotk*uy+rfDotk*vy)/(AE*86400.0);
+  vel[2]=MIN_PER_DAY*KM_PER_EARTH*(rDotk*uz+rfDotk*vz)/(AE*86400.0);
+  }
+
+
+/*
+ * Name:     SGP4_set
+ * Purpose:  sets the elements of an instance of SGP4
+ * Input:    SGP4 sgp4, double epochTime, double n0dt, double n0dt2,
+ *             double bstar, double i0, double raan, double e0,
+ *             double w0, double M0, double n0
+ * Output:   none
+ */
+void SGP4_set(SGP4 sgp4, double epochTime, double n0dt, double n0dt2,
+	      double bstar, double i0, double raan, double e0,
+	      double w0, double M0, double n0) {
+
+  /* set the epoch time */
+  sgp4->epochTime=epochTime;
+
+  /* set the first time derivative of mean motion */
+  sgp4->n0dt=n0dt*(TWOPI/(MIN_PER_DAY*MIN_PER_DAY));
+
+  /* set the second time derivative of mean motion */
+  sgp4->n0dt2=n0dt2*(TWOPI/(MIN_PER_DAY*MIN_PER_DAY));
+      
+  /* bstar drag term */
+  sgp4->bstar=bstar;
+
+  /* inclination */
+  sgp4->i0=DEG2RAD(i0);
+      
+  /* right ascension of the ascending node */
+  sgp4->raan=DEG2RAD(raan);
+
+  /* eccentricity */
+  sgp4->e0=e0;
+
+  /* argument of perigee  */
+  sgp4->w0=DEG2RAD(w0);
+
+  /* mean anomaly */
+  sgp4->M0=DEG2RAD(M0);
+
+  /* mean motion */
+  sgp4->n0=n0*(TWOPI/MIN_PER_DAY);
+  }
+
+
+/*
+ * Name:     SGP4_getPole
+ * Purpose:  finds the pole (orbit plane normal)
+ * Input:    double pos[3], double vel[3]
+ * Output:   double pole[3]
+ */
+void SGP4_getPole(double pos[3], double vel[3], double pole[3]) {
+  register double pNorm;
+
+  /* find the cross product between position and velocity */
+  pole[0]=pos[1]*vel[2] - vel[1]*pos[2];
+  pole[1]=pos[2]*vel[0] - vel[2]*pos[0];
+  pole[2]=pos[0]*vel[1] - vel[0]*pos[1];
+
+  /* normalize the resulting pole vector */
+  pNorm=sqrt(pole[0]*pole[0]+pole[1]*pole[1]+pole[2]*pole[2]);
+  pole[0]/=pNorm; pole[1]/=pNorm; pole[2]/=pNorm;
+  }
+
+
+/*
+ * Name:     SGP4_precess
+ * Purpose:  precesses a direction vector from t1 to t2
+ * Input:    double v[3], double t1, double t2
+ * Output:   double v[3]
+ */
+void SGP4_precess(double v[3], double t1, double t2) {
+  double t, st, a, b, c, temp[3], sina, sinb, sinc, cosa, cosb, cosc;
+
+  /* convert times to years */
+  t=0.001*(t2-t1)/365.25;
+  st=0.001*(t1-MJD2000)/365.25;
+
+  /* find the Euler angles */
+  a=DEG2RAD(t*(23062.181+st*(139.656+0.0139*st)+
+	       +t*(30.188-0.344*st+17.998*t)))/3600.0;
+  b=DEG2RAD(t*t*(79.280+0.410*st+0.205*t)/3600.0)+a;
+  c=DEG2RAD(t*(20043.109-st*(85.33+0.217*st)+
+	       +t*(-42.665-0.217*st-41.833*t)))/3600.0;
+  
+  /* do the precession rotation */
+  sina=sin(a); sinb=sin(b); sinc=sin(c);
+  cosa=cos(a); cosb=cos(b); cosc=cos(c);
+  temp[0]=(cosa*cosb*cosc-sina*sinb)*v[0]+(-cosa*sinb-sina*cosb*cosc)*v[1]+
+    -cosb*sinc*v[2];
+  temp[1]=(sina*cosb+cosa*sinb*cosc)*v[0]+(cosa*cosb-sina*sinb*cosc)*v[1]+
+    -sinb*sinc*v[2];
+  temp[2]=cosa*sinc*v[0]-sina*sinc*v[1]+cosc*v[2];
+  
+  /* replace existing direction vector */
+  v[0]=temp[0]; v[1]=temp[1]; v[2]=temp[2];
+  }
diff --git a/src/libcf/solar_ang.c b/src/libcf/solar_ang.c
new file mode 100644
index 0000000..421d460
--- /dev/null
+++ b/src/libcf/solar_ang.c
@@ -0,0 +1,90 @@
+/******************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ ******************************************************************************
+ *
+ * Synopsis:    double solar_ang(double mjdate, double ra, double dec)
+ *
+ * Description: Computes the angle between the Sun and J2000.0 RA and DEC
+ *              for a given date.
+ *
+ * Arguments:   double mjdate         Modified Julian date of observation
+ *              double ra             (deg) J2000.0 right ascension
+ *              double dec            (deg) J2000.0 declination 
+ *
+ * Returns:     double                (deg) angle between Sun and RA,DEC
+ *                    
+ * Calls:       slaDcc2s              dcc2s.f
+ *              slaDsep               dsep.f
+ *              slaDranrm             dranrm.f
+ *              slaEvp                evp.f
+ *
+ * History:     03/10/98  E. Murphy   Begin work.
+ *              03/10/98  E. Murphy   Initial version working
+ *              05/31/00        peb   Implemented cfortran.h calls for slalib
+ *                                    functions.
+ *              12/18/03    bjg       Change calfusettag.h to calfuse.h
+ *		07/21/04  1.4   wvd   Comment out variable vect; unused.
+ *
+ * References:  This routine makes use of the Starlink set of astronomical
+ *              subroutines (SLALIB).  More information can be found at
+ *              http://star-www.rl.ac.uk.
+ *****************************************************************************/
+ 
+#include <stdio.h>
+#include <math.h>
+
+#ifdef CFORTRAN
+#include "cfortran.h"
+PROTOCCALLSFSUB3(SLA_DCC2S, sla_dcc2s, DOUBLEV, PDOUBLE, PDOUBLE)
+#define slaDcc2s(V, A, B) \
+     CCALLSFSUB3(SLA_DCC2S, sla_dcc2s, DOUBLEV, PDOUBLE, PDOUBLE, V, A, B)
+PROTOCCALLSFFUN1(DOUBLE, SLA_DRANRM, sla_dranrm, DOUBLE)
+#define slaDranrm(ANGLE) \
+     CCALLSFFUN1(SLA_DRANRM, sla_dranrm, DOUBLE, ANGLE)
+PROTOCCALLSFFUN4(DOUBLE, SLA_DSEP, sla_dsep, DOUBLE, DOUBLE, DOUBLE, DOUBLE)
+#define slaDsep(A1, B1, A2, B2) \
+     CCALLSFFUN4(SLA_DSEP, sla_dsep, DOUBLE, DOUBLE, DOUBLE, DOUBLE, \
+		 A1, B1, A2, B2)
+PROTOCCALLSFSUB6(SLA_EVP, sla_evp, DOUBLE, DOUBLE, DOUBLEV, DOUBLEV, DOUBLEV, \
+		 DOUBLEV)
+#define slaEvp(DATE, DEQX, DVB, DPB, DVH, DPH) \
+     CCALLSFSUB6(SLA_EVP, sla_evp, DOUBLE, DOUBLE, DOUBLEV, DOUBLEV, DOUBLEV, \
+		 DOUBLEV, DATE, DEQX, DVB, DPB, DVH, DPH)
+#else
+#include "slalib.h"
+#include "slamac.h"
+#endif
+
+#include "calfuse.h"
+ 
+double solar_ang(double mjdate, double ra, double dec)
+{
+    /* Define variables. */
+    int i;
+    /* double dvb[3], dpb[3], dvh[3], dph[3], vect[3], ra_sun, dec_sun; */
+    double dvb[3], dpb[3], dvh[3], dph[3], ra_sun, dec_sun;
+    /*
+     *  Evp returns four 3-vectors containing the barycentric velocity and
+     *  position (dvb,dpv) and the heliocentric velocity and position 
+     *  (dvh,dph) of the Earth on the date mjdate.  It requires a modified 
+     *  Julian date as input.  Output has units of AU for positions and 
+     *  AU/s for velocities.
+     */
+    slaEvp(mjdate, 2000.0, dvb, dpb, dvh, dph);
+
+    /*  Convert the 3-vector position of the Sun into a J2000.0 RA and DEC */
+
+    for (i=0; i<3; i++) dph[i]*=-1.0;
+
+#ifdef CFORTRAN
+    slaDcc2s(dph, ra_sun, dec_sun);
+#else
+    slaDcc2s(dph, &ra_sun, &dec_sun);
+#endif
+
+    /*  Compute the angular separation of RA,DEC and RA_SUN and DEC_SUN */
+
+    return slaDsep(ra*RADIAN, dec*RADIAN, slaDranrm(ra_sun), dec_sun)/RADIAN;
+}
diff --git a/src/libcf/space_vel.c b/src/libcf/space_vel.c
new file mode 100644
index 0000000..e472961
--- /dev/null
+++ b/src/libcf/space_vel.c
@@ -0,0 +1,46 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    double space_vel(double *vel, double ra, double dec)
+ *
+ * Description: Computes the projection of the spacecraft orbital velocity 
+ *		vector onto a unit vector in the direction ra, dec.
+ *
+ * Arguments:   double *vel           (km/s) 3-vector velocity of satellite
+ *              double ra,dec         (deg) position of target
+ *
+ * Returns:     double                (km/s) velocity in direction of target
+ *                    
+ * History:     03/04/98  E. Murphy   Begin work.
+ *              03/04/98  E. Murphy   Initial version working
+ *              07/07/99  E. Murphy   Converted x,y,z and vx,vy,vz to pos,vel
+ *              06/15/01  V. Dixon    Comment out calculation of r, not used.
+ *              12/18/03  bjg         Change calfusettag.h to calfuse.h
+ *		07/21/04  1.4  wvd    Delete defn of r, as it is not used.
+ *		03/04/07  1.5  wvd    Rewrite program to compute dot product
+ *				      of target and velocity vectors.
+ *
+ ****************************************************************************/
+ 
+#include <math.h>
+#include "calfuse.h"
+ 
+double space_vel(double vel[3], double ra, double dec)
+{
+
+    double x, y, z, phi;
+
+    ra  *= RADIAN;
+    dec *= RADIAN;
+
+    z = sin(dec);
+    phi = cos(dec);
+    y = phi * sin(ra);
+    x = phi * cos(ra);
+
+    return x*vel[0] + y*vel[1] + z*vel[2];
+
+}
diff --git a/src/libcf/state_geod.c b/src/libcf/state_geod.c
new file mode 100644
index 0000000..4e0c161
--- /dev/null
+++ b/src/libcf/state_geod.c
@@ -0,0 +1,107 @@
+/******************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ ******************************************************************************
+ *
+ * Synopsis:    void state_geod(double pos,
+ *              double mjdate, double lon, double lat)
+ *
+ * Description: Computes the geocentric longitude and latitude of FUSE
+ *              from the given state 6-vector.
+ *
+ * Arguments:   double pos            (km) 3-vector xyz position of satellite
+ *              double mjdate         Modified Julian date of observation
+ *
+ * Returns:     double lon, lat       (deg) Geocentric longitude and latitude
+ *
+ * Calls:       slaPreces             preces.f
+ *
+ * History:     03/04/98  E. Murphy   Begin work.
+ *              03/04/98  E. Murphy   Initial version working
+ *              03/15/99  E. murphy   Changed function definition to void 
+ *                                    (was double)
+ *              07/07/99  E. Murphy   Changed call to use pos instead of x,y,z
+ *              05/31/00        peb   Implemented cfortran.h calls for slalib
+ *                                    functions.
+ *              12/18/03    bjg       Change calfusettag.h to calfuse.h
+ *              06/17/04  bjg  1.4  Corrected cfortran call to sla_preces  
+ *
+ *              Ake, T. 1998 in The Scientific Impact of the Goddard
+ *                   High Resolution Spectrograph, ed. J. C. Brandt et al.,
+ *                   ASP Conference Series, in preparation.
+ *****************************************************************************/
+ 
+#include <stdio.h>
+#include <math.h>
+
+#ifdef CFORTRAN
+#include "cfortran.h"
+PROTOCCALLSFSUB5(SLA_PRECES, sla_preces, STRING, DOUBLE, DOUBLE, PDOUBLE, \
+		 PDOUBLE)
+#define slaPreces(SYSTEM, EP0, EP1, RA, DC) \
+     CCALLSFSUB5(SLA_PRECES, sla_preces, STRING, DOUBLE, DOUBLE, PDOUBLE, \
+		 PDOUBLE, SYSTEM, EP0, EP1, RA, DC)
+#else
+#include "slalib.h"
+#include "slamac.h"
+#endif
+
+#include "calfuse.h"
+
+void state_geod(double pos[3], double mjdate, 
+		double *lon, double *lat, double *gmst)
+{
+    double ra, dec, epoch2, c1, r, intmjd, frcmjd;
+    char fk5_st[10]="FK5";
+
+    /* pos[0]=x
+       pos[1]=y
+       pos[2]=z
+       */
+
+    r=sqrt(pos[0]*pos[0]+pos[1]*pos[1]+pos[2]*pos[2]);
+    ra=atan2(pos[1],pos[0]);
+    dec=asin(pos[2]/r);
+
+    /*  We must precess the J2000 RA and DEC to date of observation. This
+     *  is a very small correction, and could probably be ignored.
+     */
+
+    epoch2=2000.0-((51544.0-mjdate)/365.25);
+
+#ifdef CFORTRAN
+    slaPreces(fk5_st, 2000.0, epoch2, ra, dec);
+#else
+    slaPreces(fk5_st, 2000.0, epoch2, &ra, &dec);
+#endif
+
+    /*  Calculate the Greenwich Mean Sidereal Time in seconds 
+     *  Astronomical Almanac, 1998, p. B6. 
+     */
+
+    frcmjd=modf(mjdate, &intmjd);
+
+    c1=(intmjd-51544.5)/36525.0;
+
+    /* The following line gives the GMST at 0 hr UT */
+    *gmst=24110.54841 + 8640184.812866*c1+0.093104*c1*c1-6.2E-6*c1*c1*c1;
+    /* The following adds on the number of seconds since the UT above */
+    *gmst+=frcmjd*1.00273791*86400.0;
+
+    *gmst*=(2*M_PI)/86400.0;
+
+    while (*gmst < 0.0) *gmst+=2*M_PI;
+
+    while (*gmst > 2*M_PI) *gmst-=2*M_PI;
+
+    *lon=(ra-*gmst)/RADIAN;
+
+    while (*lon > 180.0) *lon-=360.0;
+
+    while (*lon < -180.0) *lon+=360.0;
+
+    *lat=dec/RADIAN;
+
+    *gmst*=24.0/(2*M_PI);
+}
diff --git a/src/libcf/state_limb.c b/src/libcf/state_limb.c
new file mode 100644
index 0000000..9aacfb6
--- /dev/null
+++ b/src/libcf/state_limb.c
@@ -0,0 +1,159 @@
+/*****************************************************************************
+ *              Johns Hopkins University
+ *              Center For Astrophysical Sciences
+ *              FUSE
+ *****************************************************************************
+ *
+ * Synopsis:    double state_limb(double pos[3], double mjdate,
+ *              double ra, double dec, double *zdis,tint day_limb)
+ *
+ * Description: Computes the earth limb angle from J2000 RA and DEC given
+ *              the 3-vector position of FUSE.
+ *
+ * Arguments:   double pos            (km) 3-vector position of satellite
+ *              double mjdate         (days) Modified Julian date 
+ *              double ra,dec         (deg) J2000.0 RA and DEC
+ *              double zdist          (deg) zenith angle
+ *              integer day_limb      output : 1 if bright limb, 0 if dark limb
+ *
+ * Returns:     double                (deg) Earth limb angle
+ *              integer               day_limb will have the value 1 or 0 when
+ *                                    returning in the main program.
+ *                    
+ * Calls:       slaPreces             preces.f
+ *		slaDcc2s
+ *		slaDranrm
+ *		slaEvp
+ *
+ * History:     03/10/98  E. Murphy   Begin work.
+ *              03/10/98  E. Murphy   Initial version working
+ *              07/07/99  E. Murphy   Changed call to use pos instead of x,y,z
+ *              08/26/99  E. Murphy   Added zenith distance.
+ *              05/31/00        peb   Implemented cfortran.h calls for slalib
+ *                                    functions.
+ *              Ake, T. 1998 in The Scientific Impact of the Goddard
+ *                   High Resolution Spectrograph, ed. J. C. Brandt et al.,
+ *                   ASP Conference Series, in preparation.
+ *
+ *              09/23/00   v1.5  ma   Now this function determine bright or
+ *                                    dark limb
+ *                                    To do so, the procedure has a new
+ *                                    input argument: day_limb.
+ *                                    day_limb = 1 if bright, 0 if dark.
+ *              09/24/00   v1.6  ma   Fixed a bug in the input argument
+ *              09/27/00   v1.7  ma   Fixed bug in limbvec calc.
+ *		10/02/00   v1.8  jwk  Add fortran wrappers for slaDcc2s,
+ *                                    slaEvp, and slaDranrm
+ *              12/18/03  bjg  1.3    Change calfusettag.h to calfuse.h
+ *              06/17/04  bjg         Corrected cfortran call to sla_preces
+ *              07/22/04  bjg  1.4    Remove unused variables  
+ ****************************************************************************/
+ 
+#include <math.h>
+
+#ifdef CFORTRAN
+#include "cfortran.h"
+PROTOCCALLSFSUB5(SLA_PRECES, sla_preces, STRING, DOUBLE, DOUBLE, PDOUBLE, \
+		 PDOUBLE)
+#define slaPreces(SYSTEM, EP0, EP1, RA, DC) \
+     CCALLSFSUB5(SLA_PRECES, sla_preces, STRING, DOUBLE, DOUBLE, PDOUBLE, \
+		 PDOUBLE, SYSTEM, EP0, EP1, RA, DC)
+PROTOCCALLSFSUB3(SLA_DCC2S, sla_dcc2s, DOUBLEV, PDOUBLE, PDOUBLE)
+#define slaDcc2s(V, A, B) \
+     CCALLSFSUB3(SLA_DCC2S, sla_dcc2s, DOUBLEV, PDOUBLE, PDOUBLE, V, A, B)
+PROTOCCALLSFFUN1(DOUBLE, SLA_DRANRM, sla_dranrm, DOUBLE)
+#define slaDranrm(ANGLE) \
+     CCALLSFFUN1(SLA_DRANRM, sla_dranrm, DOUBLE, ANGLE)
+PROTOCCALLSFSUB6(SLA_EVP, sla_evp, DOUBLE, DOUBLE, DOUBLEV, DOUBLEV, DOUBLEV, \
+                 DOUBLEV)
+#define slaEvp(DATE, DEQX, DVB, DPB, DVH, DPH) \
+     CCALLSFSUB6(SLA_EVP, sla_evp, DOUBLE, DOUBLE, DOUBLEV, DOUBLEV, DOUBLEV, \
+                 DOUBLEV, DATE, DEQX, DVB, DPB, DVH, DPH)
+#else
+#include "slalib.h"
+#include "slamac.h"
+#endif
+
+#include "calfuse.h"
+
+double state_limb(double pos[3], double mjdate, 
+                  double ra, double dec, double *zdist,int *day_limb)
+{
+    double dvb[3], dpb[3], dvh[3], dph[3], limbvec[3], epoch2;
+    double ra_earth, dec_earth, r, ndist; 
+    double ra_sun, dec_sun;
+    int    i;    
+    char fk5_st[10]="FK5";
+
+    ra*=RADIAN;
+    dec*=RADIAN;
+
+    r=sqrt(pos[0]*pos[0]+pos[1]*pos[1]+pos[2]*pos[2]);
+    ra_earth=atan2(-pos[1],-pos[0]);
+    dec_earth=asin(-pos[2]/r);
+    /*  
+     *  We must precess the J2000 RA and DEC to date of observation. This
+     *  is a very small correction, and could probably be ignored.
+     */
+    epoch2=2000.0-((51544.0-mjdate)/365.25);
+
+#ifdef CFORTRAN
+    slaPreces(fk5_st, 2000.0, epoch2, ra_earth, dec_earth);
+#else
+    slaPreces(fk5_st, 2000.0, epoch2, &ra_earth, &dec_earth);
+#endif
+
+    /* Now we need the position of the sun (same code as in eclipse.c) */
+
+    slaEvp(mjdate, 2000.0, dvb, dpb, dvh, dph); 
+
+    /*  Convert the 3-vector position of the Sun into a J2000.0 RA and DEC */ 
+
+    for (i=0; i<3; i++) dph[i]*=-1.0; 
+
+ 
+#ifdef CFORTRAN 
+    slaDcc2s(dph, ra_sun, dec_sun);
+#else 
+    slaDcc2s(dph, &ra_sun, &dec_sun);
+#endif 
+
+    ra_sun=slaDranrm(ra_sun); 
+
+    /*  We must precess the J2000 RA and DEC to date of observation. This 
+     *  is a very small correction, and could probably be ignored. 
+     */
+
+    epoch2=2000.0-((51544.0-mjdate)/365.25); 
+
+#ifdef CFORTRAN 
+    slaPreces(fk5_st, 2000.0, epoch2, ra_sun, dec_sun);
+#else 
+    slaPreces(fk5_st, 2000.0, epoch2, &ra_sun, &dec_sun);
+#endif 
+
+    /* ndist is the angular distance (RADIAN) from the nadir to the target */
+    ndist = (acos(sin(dec)*sin(dec_earth)+
+                  cos(dec)*cos(dec_earth)*cos(ra-ra_earth)));
+
+    /* Now we want to calculate the limb vector (originating at the center
+       of Earth and crossing the target-FUSE line perpendicularily)*/
+
+    limbvec[2]=pos[2]+r*cos(ndist)*sin(dec);
+    limbvec[1]=pos[1]+r*cos(ndist)*cos(dec)*sin(ra);
+    limbvec[0]=pos[0]+r*cos(ndist)*cos(dec)*cos(ra);
+
+    /* Now we do the scalar product with the sun vector; then
+       if the result is <0 the limb is in the day zone (less
+       than 90 degrees between sun vector and limb vector)*/
+
+    if ((limbvec[0]*cos(dec_sun)*cos(ra_sun) + 
+	 limbvec[1]*cos(dec_sun)*sin(ra_sun)+limbvec[2]*sin(dec_sun)) >0) {
+	*day_limb=1;
+    } else {
+	*day_limb=0;
+    }
+    *zdist = 180.0 - ndist/RADIAN;
+
+    return  ndist/RADIAN-(asin(RE/r)/RADIAN);
+}
diff --git a/src/slalib/Makefile.am b/src/slalib/Makefile.am
new file mode 100644
index 0000000..895eea9
--- /dev/null
+++ b/src/slalib/Makefile.am
@@ -0,0 +1,187 @@
+lib_LTLIBRARIES = libsla.la
+libsla_la_SOURCES = \
+        addet.f  \
+        afin.f   \
+        airmas.f \
+        altaz.f  \
+        amp.f    \
+        ampqk.f  \
+        aop.f    \
+        aoppa.f  \
+        aoppat.f \
+        aopqk.f  \
+        atmdsp.f \
+        atms.f   \
+        atmt.f   \
+        av2m.f   \
+        bear.f   \
+        caf2r.f  \
+        caldj.f  \
+        calyd.f  \
+        cc2s.f   \
+        cc62s.f  \
+        cd2tf.f  \
+        cldj.f   \
+        clyd.f   \
+        combn.f  \
+        cr2af.f  \
+        cr2tf.f  \
+        cs2c.f   \
+        cs2c6.f  \
+        ctf2d.f  \
+        ctf2r.f  \
+        daf2r.f  \
+        dafin.f  \
+        dat.f    \
+        dav2m.f  \
+        dbear.f  \
+        dbjin.f  \
+        dc62s.f  \
+        dcc2s.f  \
+        dcmpf.f  \
+        dcs2c.f  \
+        dd2tf.f  \
+        de2h.f   \
+        deuler.f \
+        dfltin.f \
+        dh2e.f   \
+        dimxv.f  \
+        djcal.f  \
+        djcl.f   \
+        dm2av.f  \
+        dmat.f   \
+        dmoon.f  \
+        dmxm.f   \
+        dmxv.f   \
+        dpav.f   \
+        dr2af.f  \
+        dr2tf.f  \
+        drange.f \
+        dranrm.f \
+        ds2c6.f  \
+        ds2tp.f  \
+        dsep.f   \
+        dt.f     \
+        dtf2d.f  \
+        dtf2r.f  \
+        dtp2s.f  \
+        dtp2v.f  \
+        dtps2c.f \
+        dtpv2c.f \
+        dtt.f    \
+        dv2tp.f  \
+        dvdv.f   \
+        dvn.f    \
+        dvxv.f   \
+        e2h.f    \
+        earth.f  \
+        ecleq.f  \
+        ecmat.f  \
+        ecor.f   \
+        eg50.f   \
+        el2ue.f  \
+        epb.f    \
+        epb2d.f  \
+        epco.f   \
+        epj.f    \
+        epj2d.f  \
+        eqecl.f  \
+        eqeqx.f  \
+        eqgal.f  \
+        etrms.f  \
+        euler.f  \
+        evp.f    \
+        fitxy.f  \
+        fk425.f  \
+        fk45z.f  \
+        fk524.f  \
+        fk52h.f  \
+        fk54z.f  \
+        fk5hz.f  \
+        flotin.f \
+        galeq.f  \
+        galsup.f \
+        ge50.f   \
+        geoc.f   \
+        gmst.f   \
+        gmsta.f  \
+        h2e.f    \
+        h2fk5.f  \
+        hfk5z.f  \
+        idchf.f  \
+        idchi.f  \
+        imxv.f   \
+        intin.f  \
+        invf.f   \
+        kbj.f    \
+        m2av.f   \
+        map.f    \
+        mappa.f  \
+        mapqk.f  \
+        mapqkz.f \
+        moon.f   \
+        mxm.f    \
+        mxv.f    \
+        nut.f    \
+        nutc.f   \
+        oap.f    \
+        oapqk.f  \
+        obs.f    \
+        pa.f     \
+        pav.f    \
+        pcd.f    \
+        pda2h.f  \
+        pdq2h.f  \
+        permut.f \
+        pertel.f \
+        pertue.f \
+        planel.f \
+        planet.f \
+        plante.f \
+        pm.f     \
+        polmo.f  \
+        prebn.f  \
+        prec.f   \
+        precl.f  \
+        preces.f \
+        prenut.f \
+        pv2el.f  \
+        pv2ue.f  \
+        pvobs.f  \
+        pxy.f    \
+        range.f  \
+        ranorm.f \
+        rcc.f    \
+        rdplan.f \
+        refco.f  \
+        refro.f  \
+        refv.f   \
+        refz.f   \
+        rverot.f \
+        rvgalc.f \
+        rvlg.f   \
+        rvlsrd.f \
+        rvlsrk.f \
+        s2tp.f   \
+        sep.f    \
+        smat.f   \
+        subet.f  \
+        supgal.f \
+        svd.f    \
+        svdcov.f \
+        svdsol.f \
+        tp2s.f   \
+        tp2v.f   \
+        tps2c.f  \
+        tpv2c.f  \
+        ue2el.f  \
+        ue2pv.f  \
+        unpcd.f  \
+        v2tp.f   \
+        vdv.f    \
+        vn.f     \
+        vxv.f    \
+        xy2xy.f  \
+        zd.f
+
+AM_CFLAGS = -I../include -I./
diff --git a/src/slalib/Makefile.in b/src/slalib/Makefile.in
new file mode 100644
index 0000000..718fd59
--- /dev/null
+++ b/src/slalib/Makefile.in
@@ -0,0 +1,830 @@
+# Makefile.in generated by automake 1.15 from Makefile.am.
+# @configure_input@
+
+# Copyright (C) 1994-2014 Free Software Foundation, Inc.
+
+# This Makefile.in is free software; the Free Software Foundation
+# gives unlimited permission to copy and/or distribute it,
+# with or without modifications, as long as this notice is preserved.
+
+# This program is distributed in the hope that it will be useful,
+# but WITHOUT ANY WARRANTY, to the extent permitted by law; without
+# even the implied warranty of MERCHANTABILITY or FITNESS FOR A
+# PARTICULAR PURPOSE.
+
+@SET_MAKE@
+
+VPATH = @srcdir@
+am__is_gnu_make = { \
+  if test -z '$(MAKELEVEL)'; then \
+    false; \
+  elif test -n '$(MAKE_HOST)'; then \
+    true; \
+  elif test -n '$(MAKE_VERSION)' && test -n '$(CURDIR)'; then \
+    true; \
+  else \
+    false; \
+  fi; \
+}
+am__make_running_with_option = \
+  case $${target_option-} in \
+      ?) ;; \
+      *) echo "am__make_running_with_option: internal error: invalid" \
+              "target option '$${target_option-}' specified" >&2; \
+         exit 1;; \
+  esac; \
+  has_opt=no; \
+  sane_makeflags=$$MAKEFLAGS; \
+  if $(am__is_gnu_make); then \
+    sane_makeflags=$$MFLAGS; \
+  else \
+    case $$MAKEFLAGS in \
+      *\\[\ \	]*) \
+        bs=\\; \
+        sane_makeflags=`printf '%s\n' "$$MAKEFLAGS" \
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+	  echo " $(LIBTOOL) $(AM_LIBTOOLFLAGS) $(LIBTOOLFLAGS) --mode=uninstall rm -f '$(DESTDIR)$(libdir)/$$f'"; \
+	  $(LIBTOOL) $(AM_LIBTOOLFLAGS) $(LIBTOOLFLAGS) --mode=uninstall rm -f "$(DESTDIR)$(libdir)/$$f"; \
+	done
+
+clean-libLTLIBRARIES:
+	-test -z "$(lib_LTLIBRARIES)" || rm -f $(lib_LTLIBRARIES)
+	@list='$(lib_LTLIBRARIES)'; \
+	locs=`for p in $$list; do echo $$p; done | \
+	      sed 's|^[^/]*$$|.|; s|/[^/]*$$||; s|$$|/so_locations|' | \
+	      sort -u`; \
+	test -z "$$locs" || { \
+	  echo rm -f $${locs}; \
+	  rm -f $${locs}; \
+	}
+
+libsla.la: $(libsla_la_OBJECTS) $(libsla_la_DEPENDENCIES) $(EXTRA_libsla_la_DEPENDENCIES) 
+	$(AM_V_F77LD)$(F77LINK) -rpath $(libdir) $(libsla_la_OBJECTS) $(libsla_la_LIBADD) $(LIBS)
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+mostlyclean-compile:
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+distclean-compile:
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+
+.f.o:
+	$(AM_V_F77)$(F77COMPILE) -c -o $@ $<
+
+.f.obj:
+	$(AM_V_F77)$(F77COMPILE) -c -o $@ `$(CYGPATH_W) '$<'`
+
+.f.lo:
+	$(AM_V_F77)$(LTF77COMPILE) -c -o $@ $<
+
+mostlyclean-libtool:
+	-rm -f *.lo
+
+clean-libtool:
+	-rm -rf .libs _libs
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+ID: $(am__tagged_files)
+	$(am__define_uniq_tagged_files); mkid -fID $$unique
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+	here=`pwd`; \
+	$(am__define_uniq_tagged_files); \
+	shift; \
+	if test -z "$(ETAGS_ARGS)$$*$$unique"; then :; else \
+	  test -n "$$unique" || unique=$$empty_fix; \
+	  if test $$# -gt 0; then \
+	    $(ETAGS) $(ETAGSFLAGS) $(AM_ETAGSFLAGS) $(ETAGS_ARGS) \
+	      "$$@" $$unique; \
+	  else \
+	    $(ETAGS) $(ETAGSFLAGS) $(AM_ETAGSFLAGS) $(ETAGS_ARGS) \
+	      $$unique; \
+	  fi; \
+	fi
+ctags: ctags-am
+
+CTAGS: ctags
+ctags-am: $(TAGS_DEPENDENCIES) $(am__tagged_files)
+	$(am__define_uniq_tagged_files); \
+	test -z "$(CTAGS_ARGS)$$unique" \
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+	     $$unique
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+GTAGS:
+	here=`$(am__cd) $(top_builddir) && pwd` \
+	  && $(am__cd) $(top_srcdir) \
+	  && gtags -i $(GTAGS_ARGS) "$$here"
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+cscopelist-am: $(am__tagged_files)
+	list='$(am__tagged_files)'; \
+	case "$(srcdir)" in \
+	  [\\/]* | ?:[\\/]*) sdir="$(srcdir)" ;; \
+	  *) sdir=$(subdir)/$(srcdir) ;; \
+	esac; \
+	for i in $$list; do \
+	  if test -f "$$i"; then \
+	    echo "$(subdir)/$$i"; \
+	  else \
+	    echo "$$sdir/$$i"; \
+	  fi; \
+	done >> $(top_builddir)/cscope.files
+
+distclean-tags:
+	-rm -f TAGS ID GTAGS GRTAGS GSYMS GPATH tags
+
+distdir: $(DISTFILES)
+	@srcdirstrip=`echo "$(srcdir)" | sed 's/[].[^$$\\*]/\\\\&/g'`; \
+	topsrcdirstrip=`echo "$(top_srcdir)" | sed 's/[].[^$$\\*]/\\\\&/g'`; \
+	list='$(DISTFILES)'; \
+	  dist_files=`for file in $$list; do echo $$file; done | \
+	  sed -e "s|^$$srcdirstrip/||;t" \
+	      -e "s|^$$topsrcdirstrip/|$(top_builddir)/|;t"`; \
+	case $$dist_files in \
+	  */*) $(MKDIR_P) `echo "$$dist_files" | \
+			   sed '/\//!d;s|^|$(distdir)/|;s,/[^/]*$$,,' | \
+			   sort -u` ;; \
+	esac; \
+	for file in $$dist_files; do \
+	  if test -f $$file || test -d $$file; then d=.; else d=$(srcdir); fi; \
+	  if test -d $$d/$$file; then \
+	    dir=`echo "/$$file" | sed -e 's,/[^/]*$$,,'`; \
+	    if test -d "$(distdir)/$$file"; then \
+	      find "$(distdir)/$$file" -type d ! -perm -700 -exec chmod u+rwx {} \;; \
+	    fi; \
+	    if test -d $(srcdir)/$$file && test $$d != $(srcdir); then \
+	      cp -fpR $(srcdir)/$$file "$(distdir)$$dir" || exit 1; \
+	      find "$(distdir)/$$file" -type d ! -perm -700 -exec chmod u+rwx {} \;; \
+	    fi; \
+	    cp -fpR $$d/$$file "$(distdir)$$dir" || exit 1; \
+	  else \
+	    test -f "$(distdir)/$$file" \
+	    || cp -p $$d/$$file "$(distdir)/$$file" \
+	    || exit 1; \
+	  fi; \
+	done
+check-am: all-am
+check: check-am
+all-am: Makefile $(LTLIBRARIES)
+installdirs:
+	for dir in "$(DESTDIR)$(libdir)"; do \
+	  test -z "$$dir" || $(MKDIR_P) "$$dir"; \
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+	    install_sh_PROGRAM="$(INSTALL_STRIP_PROGRAM)" INSTALL_STRIP_FLAG=-s \
+	      install; \
+	else \
+	  $(MAKE) $(AM_MAKEFLAGS) INSTALL_PROGRAM="$(INSTALL_STRIP_PROGRAM)" \
+	    install_sh_PROGRAM="$(INSTALL_STRIP_PROGRAM)" INSTALL_STRIP_FLAG=-s \
+	    "INSTALL_PROGRAM_ENV=STRIPPROG='$(STRIP)'" install; \
+	fi
+mostlyclean-generic:
+
+clean-generic:
+
+distclean-generic:
+	-test -z "$(CONFIG_CLEAN_FILES)" || rm -f $(CONFIG_CLEAN_FILES)
+	-test . = "$(srcdir)" || test -z "$(CONFIG_CLEAN_VPATH_FILES)" || rm -f $(CONFIG_CLEAN_VPATH_FILES)
+
+maintainer-clean-generic:
+	@echo "This command is intended for maintainers to use"
+	@echo "it deletes files that may require special tools to rebuild."
+clean: clean-am
+
+clean-am: clean-generic clean-libLTLIBRARIES clean-libtool \
+	mostlyclean-am
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+	-rm -f Makefile
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+.MAKE: install-am install-strip
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+.PHONY: CTAGS GTAGS TAGS all all-am check check-am clean clean-generic \
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+.PRECIOUS: Makefile
+
+
+# Tell versions [3.59,3.63) of GNU make to not export all variables.
+# Otherwise a system limit (for SysV at least) may be exceeded.
+.NOEXPORT:
diff --git a/src/slalib/addet.f b/src/slalib/addet.f
new file mode 100644
index 0000000..c039aff
--- /dev/null
+++ b/src/slalib/addet.f
@@ -0,0 +1,67 @@
+      SUBROUTINE sla_ADDET (RM, DM, EQ, RC, DC)
+*+
+*     - - - - - -
+*      A D D E T
+*     - - - - - -
+*
+*  Add the E-terms (elliptic component of annual aberration)
+*  to a pre IAU 1976 mean place to conform to the old
+*  catalogue convention (double precision)
+*
+*  Given:
+*     RM,DM     dp     RA,Dec (radians) without E-terms
+*     EQ        dp     Besselian epoch of mean equator and equinox
+*
+*  Returned:
+*     RC,DC     dp     RA,Dec (radians) with E-terms included
+*
+*  Note:
+*
+*     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.
+*
+*  Reference:
+*     Explanatory Supplement to the Astronomical Ephemeris,
+*     section 2D, page 48.
+*
+*  Called:  sla_ETRMS, sla_DCS2C, sla_DCC2S, sla_DRANRM, sla_DRANGE
+*
+*  P.T.Wallace   Starlink   18 March 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION RM,DM,EQ,RC,DC
+
+      DOUBLE PRECISION sla_DRANRM
+
+      DOUBLE PRECISION A(3),V(3)
+
+      INTEGER I
+
+
+
+*  E-terms vector
+      CALL sla_ETRMS(EQ,A)
+
+*  Spherical to Cartesian
+      CALL sla_DCS2C(RM,DM,V)
+
+*  Include the E-terms
+      DO I=1,3
+         V(I)=V(I)+A(I)
+      END DO
+
+*  Cartesian to spherical
+      CALL sla_DCC2S(V,RC,DC)
+
+*  Bring RA into conventional range
+      RC=sla_DRANRM(RC)
+
+      END
diff --git a/src/slalib/afin.f b/src/slalib/afin.f
new file mode 100644
index 0000000..2308c74
--- /dev/null
+++ b/src/slalib/afin.f
@@ -0,0 +1,102 @@
+      SUBROUTINE sla_AFIN (STRING, IPTR, A, J)
+*+
+*     - - - - -
+*      A F I N
+*     - - - - -
+*
+*  Sexagesimal character string to angle (single precision)
+*
+*  Given:
+*     STRING  c*(*)   string containing deg, arcmin, arcsec fields
+*     IPTR      i     pointer to start of decode (1st = 1)
+*
+*  Returned:
+*     IPTR      i     advanced past the decoded angle
+*     A         r     angle in radians
+*     J         i     status:  0 = OK
+*                             +1 = default, A unchanged
+*                             -1 = bad degrees      )
+*                             -2 = bad arcminutes   )  (note 3)
+*                             -3 = bad arcseconds   )
+*
+*  Example:
+*
+*    argument    before                           after
+*
+*    STRING      '-57 17 44.806  12 34 56.7'      unchanged
+*    IPTR        1                                16 (points to 12...)
+*    A           ?                                -1.00000
+*    J           ?                                0
+*
+*    A further call to sla_AFIN, without adjustment of IPTR, will
+*    decode the second angle, 12deg 34min 56.7sec.
+*
+*  Notes:
+*
+*     1)  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 DFLTIN routine and is free-format.
+*
+*     2)  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.
+*
+*     3)  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...
+*
+*     4)  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.
+*
+*     5)  Further fields after the three expected ones are not treated
+*         as an error.  The pointer IPTR is left in the correct state
+*         for further decoding with the present routine or with DFLTIN
+*         etc.  See the example, above.
+*
+*     6)  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
+*
+*  Called:  sla_DAFIN
+*
+*  P.T.Wallace   Starlink   13 September 1990
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      CHARACTER*(*) STRING
+      INTEGER IPTR
+      REAL A
+      INTEGER J
+
+      DOUBLE PRECISION AD
+
+
+
+*  Call the double precision version
+      CALL sla_DAFIN(STRING,IPTR,AD,J)
+      IF (J.LE.0) A=REAL(AD)
+
+      END
diff --git a/src/slalib/airmas.f b/src/slalib/airmas.f
new file mode 100644
index 0000000..12431c8
--- /dev/null
+++ b/src/slalib/airmas.f
@@ -0,0 +1,58 @@
+      DOUBLE PRECISION FUNCTION sla_AIRMAS (ZD)
+*+
+*     - - - - - - -
+*      A I R M A S
+*     - - - - - - -
+*
+*  Air mass at given zenith distance (double precision)
+*
+*  Given:
+*     ZD     d     Observed zenith distance (radians)
+*
+*  The result is an estimate of the air mass, in units of that
+*  at the zenith.
+*
+*  Notes:
+*
+*  1)  The "observed" zenith distance referred to above means "as
+*      affected by refraction".
+*
+*  2)  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.
+*
+*  3)  The sign of the ZD is ignored.
+*
+*  4)  At zenith distances greater than about ZD = 87 degrees the
+*      air mass is held constant to avoid arithmetic overflows.
+*
+*  References:
+*     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.
+*
+*  Original code by P.W.Hill, St Andrews
+*
+*  P.T.Wallace   Starlink   18 March 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION ZD
+
+      DOUBLE PRECISION SECZM1
+
+
+      SECZM1 = 1D0/(COS(MIN(1.52D0,ABS(ZD))))-1D0
+      sla_AIRMAS = 1D0 + SECZM1*(0.9981833D0
+     :             - SECZM1*(0.002875D0 + 0.0008083D0*SECZM1))
+
+      END
diff --git a/src/slalib/altaz.f b/src/slalib/altaz.f
new file mode 100644
index 0000000..3a7124b
--- /dev/null
+++ b/src/slalib/altaz.f
@@ -0,0 +1,145 @@
+      SUBROUTINE sla_ALTAZ (HA, DEC, PHI,
+     :                      AZ, AZD, AZDD, EL, ELD, ELDD, PA, PAD, PADD)
+*+
+*     - - - - - -
+*      A L T A Z
+*     - - - - - -
+*
+*  Positions, velocities and accelerations for an altazimuth
+*  telescope mount.
+*
+*  (double precision)
+*
+*  Given:
+*     HA      d     hour angle
+*     DEC     d     declination
+*     PHI     d     observatory latitude
+*
+*  Returned:
+*     AZ      d     azimuth
+*     AZD     d        "    velocity
+*     AZDD    d        "    acceleration
+*     EL      d     elevation
+*     ELD     d         "     velocity
+*     ELDD    d         "     acceleration
+*     PA      d     parallactic angle
+*     PAD     d         "      "   velocity
+*     PADD    d         "      "   acceleration
+*
+*  Notes:
+*
+*  1)  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.
+*
+*  2)  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/2.  Position angle is +ve
+*      for a star west of the meridian and is the angle NP-star-zenith.
+*
+*  3)  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.
+*
+*  4)  No range checking of arguments is carried out.
+*
+*  5)  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.
+*
+*  P.T.Wallace   Starlink   14 March 1997
+*
+*  Copyright (C) 1997 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION HA,DEC,PHI,AZ,AZD,AZDD,EL,ELD,ELDD,PA,PAD,PADD
+
+      DOUBLE PRECISION DPI,D2PI,TINY
+      PARAMETER (DPI=3.1415926535897932384626433832795D0,
+     :           D2PI=6.283185307179586476925286766559D0,
+     :           TINY=1D-30)
+
+      DOUBLE PRECISION 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.EQ.0D0) THEN
+         A=0D0
+      ELSE
+         A=ATAN2(Y,X)
+      END IF
+      IF (A.LT.0D0) A=A+D2PI
+      E=ATAN2(Z,R)
+
+*  Parallactic angle
+      C=CD*SP-CH*SDCP
+      S=SH*CP
+      IF (C*C+S*S.GT.0) THEN
+         Q=ATAN2(S,C)
+      ELSE
+         Q=DPI-HA
+      END IF
+
+*  Velocities and accelerations (clamped at zenith/nadir)
+      IF (RSQ.LT.TINY) THEN
+         RSQ=TINY
+         R=SQRT(RSQ)
+      END IF
+      QD=-X*CP/RSQ
+      AD=SP+Z*QD
+      ED=CP*Y/R
+      EDR=ED/R
+      ADD=EDR*(Z*SP+(2D0-RSQ)*QD)
+      EDD=-R*QD*AD
+      QDD=EDR*(SP+2D0*Z*QD)
+
+*  Results
+      AZ=A
+      AZD=AD
+      AZDD=ADD
+      EL=E
+      ELD=ED
+      ELDD=EDD
+      PA=Q
+      PAD=QD
+      PADD=QDD
+
+      END
diff --git a/src/slalib/amp.f b/src/slalib/amp.f
new file mode 100644
index 0000000..6feb570
--- /dev/null
+++ b/src/slalib/amp.f
@@ -0,0 +1,68 @@
+      SUBROUTINE sla_AMP (RA, DA, DATE, EQ, RM, DM)
+*+
+*     - - - -
+*      A M P
+*     - - - -
+*
+*  Convert star RA,Dec from geocentric apparent to mean place
+*
+*  The mean coordinate system is the post IAU 1976 system,
+*  loosely called FK5.
+*
+*  Given:
+*     RA       d      apparent RA (radians)
+*     DA       d      apparent Dec (radians)
+*     DATE     d      TDB for apparent place (JD-2400000.5)
+*     EQ       d      equinox:  Julian epoch of mean place
+*
+*  Returned:
+*     RM       d      mean RA (radians)
+*     DM       d      mean Dec (radians)
+*
+*  References:
+*     1984 Astronomical Almanac, pp B39-B41.
+*     (also Lederle & Schwan, Astron. Astrophys. 134,
+*      1-6, 1984)
+*
+*  Notes:
+*
+*  1)  The distinction between the required TDB and TT is
+*      always negligible.  Moreover, for all but the most
+*      critical applications UTC is adequate.
+*
+*  2)  The accuracy is limited by the routine sla_EVP, called
+*      by sla_MAPPA, which computes the Earth position and
+*      velocity using the methods of Stumpff.  The maximum
+*      error is about 0.3 milliarcsecond.
+*
+*  3)  Iterative techniques are used for the aberration and
+*      light deflection corrections so that the routines
+*      sla_AMP (or sla_AMPQK) and sla_MAP (or sla_MAPQK) are
+*      accurate inverses;  even at the edge of the Sun's disc
+*      the discrepancy is only about 1 nanoarcsecond.
+*
+*  4)  Where multiple apparent places are to be converted to
+*      mean places, for a fixed date and equinox, it is more
+*      efficient to use the sla_MAPPA routine to compute the
+*      required parameters once, followed by one call to
+*      sla_AMPQK per star.
+*
+*  Called:  sla_MAPPA, sla_AMPQK
+*
+*  P.T.Wallace   Starlink   19 January 1993
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION RA,DA,DATE,EQ,RM,DM
+
+      DOUBLE PRECISION AMPRMS(21)
+
+
+
+      CALL sla_MAPPA(EQ,DATE,AMPRMS)
+      CALL sla_AMPQK(RA,DA,AMPRMS,RM,DM)
+
+      END
diff --git a/src/slalib/ampqk.f b/src/slalib/ampqk.f
new file mode 100644
index 0000000..6b94db1
--- /dev/null
+++ b/src/slalib/ampqk.f
@@ -0,0 +1,127 @@
+      SUBROUTINE sla_AMPQK (RA, DA, AMPRMS, RM, DM)
+*+
+*     - - - - - -
+*      A M P Q K
+*     - - - - - -
+*
+*  Convert star RA,Dec from geocentric apparent to mean place
+*
+*  The mean coordinate system is the post IAU 1976 system,
+*  loosely called FK5.
+*
+*  Use of this routine 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 sla_MAPPA routine.
+*
+*  Given:
+*     RA       d      apparent RA (radians)
+*     DA       d      apparent Dec (radians)
+*
+*     AMPRMS   d(21)  star-independent mean-to-apparent parameters:
+*
+*       (1)      time interval for proper motion (Julian years)
+*       (2-4)    barycentric position of the Earth (AU)
+*       (5-7)    heliocentric direction of the Earth (unit vector)
+*       (8)      (grav rad Sun)*2/(Sun-Earth distance)
+*       (9-11)   ABV: barycentric Earth velocity in units of c
+*       (12)     sqrt(1-v**2) where v=modulus(ABV)
+*       (13-21)  precession/nutation (3,3) matrix
+*
+*  Returned:
+*     RM       d      mean RA (radians)
+*     DM       d      mean Dec (radians)
+*
+*  References:
+*     1984 Astronomical Almanac, pp B39-B41.
+*     (also Lederle & Schwan, Astron. Astrophys. 134,
+*      1-6, 1984)
+*
+*  Notes:
+*
+*  1)  The accuracy is limited by the routine sla_EVP, called
+*      by sla_MAPPA, which computes the Earth position and
+*      velocity using the methods of Stumpff.  The maximum
+*      error is about 0.3 milliarcsecond.
+*
+*  2)  Iterative techniques are used for the aberration and
+*      light deflection corrections so that the routines
+*      sla_AMP (or sla_AMPQK) and sla_MAP (or sla_MAPQK) are
+*      accurate inverses;  even at the edge of the Sun's disc
+*      the discrepancy is only about 1 nanoarcsecond.
+*
+*  Called:  sla_DCS2C, sla_DIMXV, sla_DVDV, sla_DVN, sla_DCC2S,
+*           sla_DRANRM
+*
+*  P.T.Wallace   Starlink   21 June 1993
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION RA,DA,AMPRMS(21),RM,DM
+
+      INTEGER I,J
+
+      DOUBLE PRECISION GR2E,AB1,EHN(3),ABV(3),P3(3),P2(3),
+     :                 AB1P1,P1DV,P1DVP1,P1(3),W,PDE,PDEP1,P(3)
+
+      DOUBLE PRECISION sla_DVDV,sla_DRANRM
+
+
+
+*  Unpack scalar and vector parameters
+      GR2E = AMPRMS(8)
+      AB1 = AMPRMS(12)
+      DO I=1,3
+         EHN(I) = AMPRMS(I+4)
+         ABV(I) = AMPRMS(I+8)
+      END DO
+
+*  Apparent RA,Dec to Cartesian
+      CALL sla_DCS2C(RA,DA,P3)
+
+*  Precession and nutation
+      CALL sla_DIMXV(AMPRMS(13),P3,P2)
+
+*  Aberration
+      AB1P1 = AB1+1D0
+      DO I=1,3
+         P1(I) = P2(I)
+      END DO
+      DO J=1,2
+         P1DV = sla_DVDV(P1,ABV)
+         P1DVP1 = 1D0+P1DV
+         W = 1D0+P1DV/AB1P1
+         DO I=1,3
+            P1(I) = (P1DVP1*P2(I)-W*ABV(I))/AB1
+         END DO
+         CALL sla_DVN(P1,P3,W)
+         DO I=1,3
+            P1(I) = P3(I)
+         END DO
+      END DO
+
+*  Light deflection
+      DO I=1,3
+         P(I) = P1(I)
+      END DO
+      DO J=1,5
+         PDE = sla_DVDV(P,EHN)
+         PDEP1 = 1D0+PDE
+         W = PDEP1-GR2E*PDE
+         DO I=1,3
+            P(I) = (PDEP1*P1(I)-GR2E*EHN(I))/W
+         END DO
+         CALL sla_DVN(P,P2,W)
+         DO I=1,3
+            P(I) = P2(I)
+         END DO
+      END DO
+
+*  Mean RA,Dec
+      CALL sla_DCC2S(P,RM,DM)
+      RM = sla_DRANRM(RM)
+
+      END
diff --git a/src/slalib/aop.f b/src/slalib/aop.f
new file mode 100644
index 0000000..66ef9c4
--- /dev/null
+++ b/src/slalib/aop.f
@@ -0,0 +1,174 @@
+      SUBROUTINE sla_AOP (RAP, DAP, DATE, DUT, ELONGM, PHIM, HM,
+     :                    XP, YP, TDK, PMB, RH, WL, TLR,
+     :                    AOB, ZOB, HOB, DOB, ROB)
+*+
+*     - - - -
+*      A O P
+*     - - - -
+*
+*  Apparent to observed place, for optical sources distant from
+*  the solar system.
+*
+*  Given:
+*     RAP    d      geocentric apparent right ascension
+*     DAP    d      geocentric apparent declination
+*     DATE   d      UTC date/time (Modified Julian Date, JD-2400000.5)
+*     DUT    d      delta UT:  UT1-UTC (UTC seconds)
+*     ELONGM d      mean longitude of the observer (radians, east +ve)
+*     PHIM   d      mean geodetic latitude of the observer (radians)
+*     HM     d      observer's height above sea level (metres)
+*     XP     d      polar motion x-coordinate (radians)
+*     YP     d      polar motion y-coordinate (radians)
+*     TDK    d      local ambient temperature (DegK; std=273.155D0)
+*     PMB    d      local atmospheric pressure (mB; std=1013.25D0)
+*     RH     d      local relative humidity (in the range 0D0-1D0)
+*     WL     d      effective wavelength (micron, e.g. 0.55D0)
+*     TLR    d      tropospheric lapse rate (DegK/metre, e.g. 0.0065D0)
+*
+*  Returned:
+*     AOB    d      observed azimuth (radians: N=0,E=90)
+*     ZOB    d      observed zenith distance (radians)
+*     HOB    d      observed Hour Angle (radians)
+*     DOB    d      observed Declination (radians)
+*     ROB    d      observed Right Ascension (radians)
+*
+*  Notes:
+*
+*   1)  This routine returns zenith distance rather than elevation
+*       in order to reflect the fact that no allowance is made for
+*       depression of the horizon.
+*
+*   2)  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
+*       sla_REFRO routine returns a fixed value of the refraction.
+*       The complementary routines sla_AOP (or sla_AOPQK) and sla_OAP
+*       (or sla_OAPQK) are self-consistent to better than 1 micro-
+*       arcsecond all over the celestial sphere.
+*
+*   3)  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.
+*
+*   4)  "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 sla_MAP 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
+*       sla_FK425 etc routines.
+*
+*   5)  "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.
+*
+*   6)  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.
+*
+*   7)  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 sla_AOPPA once followed by one call per star to sla_AOPQK.
+*       Where a range of times within a limited period of a few hours
+*       is involved, and the highest precision is not required, call
+*       sla_AOPPA once, followed by a call to sla_AOPPAT each time the
+*       time changes, followed by one call per star to sla_AOPQK.
+*
+*   8)  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.
+*
+*   9)  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.
+*
+*  10)  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
+*       sla_OBS routine are west-positive, following astronomical
+*       usage, and must be reversed in sign before use in the present
+*       routine.
+*
+*  11)  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.
+*
+*  12)  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 sla_OBS.  If P,
+*       the pressure in millibars, is available, an adequate
+*       estimate of HM can be obtained from the expression
+*
+*             HM ~ -29.3D0*TSL*LOG(P/1013.25D0).
+*
+*       where TSL is the approximate sea-level air temperature in
+*       deg 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 ~ 1013.25D0*EXP(-HM/(29.3D0*TSL)).
+*
+*       Note, however, that the refraction is proportional to the
+*       pressure and that an accurate P value is important for
+*       precise work.
+*
+*  13)  The azimuths etc produced by the present routine are with
+*       respect to the celestial pole.  Corrections to the terrestrial
+*       pole can be computed using sla_POLMO.
+*
+*  Called:  sla_AOPPA, sla_AOPQK
+*
+*  P.T.Wallace   Starlink   6 September 1999
+*
+*  Copyright (C) 1999 P.T.Wallace and CCLRC
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION RAP,DAP,DATE,DUT,ELONGM,PHIM,HM,
+     :                 XP,YP,TDK,PMB,RH,WL,TLR,AOB,ZOB,HOB,DOB,ROB
+
+      DOUBLE PRECISION AOPRMS(14)
+
+
+      CALL sla_AOPPA(DATE,DUT,ELONGM,PHIM,HM,XP,YP,TDK,PMB,RH,WL,TLR,
+     :               AOPRMS)
+      CALL sla_AOPQK(RAP,DAP,AOPRMS,AOB,ZOB,HOB,DOB,ROB)
+
+      END
diff --git a/src/slalib/aoppa.f b/src/slalib/aoppa.f
new file mode 100644
index 0000000..b497fdb
--- /dev/null
+++ b/src/slalib/aoppa.f
@@ -0,0 +1,176 @@
+      SUBROUTINE sla_AOPPA (DATE, DUT, ELONGM, PHIM, HM,
+     :                      XP, YP, TDK, PMB, RH, WL, TLR, AOPRMS)
+*+
+*     - - - - - -
+*      A O P P A
+*     - - - - - -
+*
+*  Precompute apparent to observed place parameters required by
+*  sla_AOPQK and sla_OAPQK.
+*
+*  Given:
+*     DATE   d      UTC date/time (modified Julian Date, JD-2400000.5)
+*     DUT    d      delta UT:  UT1-UTC (UTC seconds)
+*     ELONGM d      mean longitude of the observer (radians, east +ve)
+*     PHIM   d      mean geodetic latitude of the observer (radians)
+*     HM     d      observer's height above sea level (metres)
+*     XP     d      polar motion x-coordinate (radians)
+*     YP     d      polar motion y-coordinate (radians)
+*     TDK    d      local ambient temperature (DegK; std=273.155D0)
+*     PMB    d      local atmospheric pressure (mB; std=1013.25D0)
+*     RH     d      local relative humidity (in the range 0D0-1D0)
+*     WL     d      effective wavelength (micron, e.g. 0.55D0)
+*     TLR    d      tropospheric lapse rate (DegK/metre, e.g. 0.0065D0)
+*
+*  Returned:
+*     AOPRMS d(14)  star-independent apparent-to-observed parameters:
+*
+*       (1)      geodetic latitude (radians)
+*       (2,3)    sine and cosine of geodetic latitude
+*       (4)      magnitude of diurnal aberration vector
+*       (5)      height (HM)
+*       (6)      ambient temperature (TDK)
+*       (7)      pressure (PMB)
+*       (8)      relative humidity (RH)
+*       (9)      wavelength (WL)
+*       (10)     lapse rate (TLR)
+*       (11,12)  refraction constants A and B (radians)
+*       (13)     longitude + eqn of equinoxes + sidereal DUT (radians)
+*       (14)     local apparent sidereal time (radians)
+*
+*  Notes:
+*
+*   1)  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.
+*
+*   2)  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.
+*
+*   3)  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.
+*
+*   4)  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
+*       sla_OBS routine are west-positive, following astronomical
+*       usage, and must be reversed in sign before use in the present
+*       routine.
+*
+*   5)  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.
+*
+*   6)  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 sla_OBS.  If P,
+*       the pressure in millibars, is available, an adequate
+*       estimate of HM can be obtained from the expression
+*
+*             HM ~ -29.3D0*TSL*LOG(P/1013.25D0).
+*
+*       where TSL is the approximate sea-level air temperature in
+*       deg 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 ~ 1013.25D0*EXP(-HM/(29.3D0*TSL)).
+*
+*       Note, however, that the refraction is proportional to the
+*       pressure and that an accurate P value is important for
+*       precise work.
+*
+*   7)  Repeated, computationally-expensive, calls to sla_AOPPA for
+*       times that are very close together can be avoided by calling
+*       sla_AOPPA just once and then using sla_AOPPAT for the subsequent
+*       times.  Fresh calls to sla_AOPPA will be needed only when changes
+*       in the precession have grown to unacceptable levels or when
+*       anything affecting the refraction has changed.
+*
+*  Called:  sla_GEOC, sla_REFCO, sla_EQEQX, sla_AOPPAT
+*
+*  P.T.Wallace   Starlink   6 September 1999
+*
+*  Copyright (C) 1999 P.T.Wallace and CCLRC
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DATE,DUT,ELONGM,PHIM,HM,XP,YP,TDK,PMB,
+     :                 RH,WL,TLR,AOPRMS(14)
+
+      DOUBLE PRECISION sla_EQEQX
+
+*  2Pi
+      DOUBLE PRECISION D2PI
+      PARAMETER (D2PI=6.283185307179586476925287D0)
+
+*  Seconds of time to radians
+      DOUBLE PRECISION S2R
+      PARAMETER (S2R=7.272205216643039903848712D-5)
+
+*  Speed of light (AU per day)
+      DOUBLE PRECISION C
+      PARAMETER (C=173.14463331D0)
+
+*  Ratio between solar and sidereal time
+      DOUBLE PRECISION SOLSID
+      PARAMETER (SOLSID=1.00273790935D0)
+
+      DOUBLE PRECISION 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.EQ.0D0.AND.YC.EQ.0D0) THEN
+         ELONG = 0D0
+      ELSE
+         ELONG = ATAN2(YC,XC)
+      END IF
+      PHI = ATAN2(ZC,SQRT(XC*XC+YC*YC))
+      AOPRMS(1) = PHI
+      AOPRMS(2) = SIN(PHI)
+      AOPRMS(3) = COS(PHI)
+
+*  Magnitude of the diurnal aberration vector
+      CALL sla_GEOC(PHI,HM,UAU,VAU)
+      AOPRMS(4) = D2PI*UAU*SOLSID/C
+
+*  Copy the refraction parameters and compute the A & B constants
+      AOPRMS(5) = HM
+      AOPRMS(6) = TDK
+      AOPRMS(7) = PMB
+      AOPRMS(8) = RH
+      AOPRMS(9) = WL
+      AOPRMS(10) = TLR
+      CALL sla_REFCO(HM,TDK,PMB,RH,WL,PHI,TLR,1D-10,
+     :               AOPRMS(11),AOPRMS(12))
+
+*  Longitude + equation of the equinoxes + sidereal equivalent of DUT
+*  (ignoring change in equation of the equinoxes between UTC and TDB)
+      AOPRMS(13) = ELONG+sla_EQEQX(DATE)+DUT*SOLSID*S2R
+
+*  Sidereal time
+      CALL sla_AOPPAT(DATE,AOPRMS)
+
+      END
diff --git a/src/slalib/aoppat.f b/src/slalib/aoppat.f
new file mode 100644
index 0000000..1342024
--- /dev/null
+++ b/src/slalib/aoppat.f
@@ -0,0 +1,45 @@
+      SUBROUTINE sla_AOPPAT (DATE, AOPRMS)
+*+
+*     - - - - - - -
+*      A O P P A T
+*     - - - - - - -
+*
+*  Recompute the sidereal time in the apparent to observed place
+*  star-independent parameter block.
+*
+*  Given:
+*     DATE   d      UTC date/time (modified Julian Date, JD-2400000.5)
+*                   (see AOPPA source for comments on leap seconds)
+*
+*     AOPRMS d(14)  star-independent apparent-to-observed parameters
+*
+*       (1-12)   not required
+*       (13)     longitude + eqn of equinoxes + sidereal DUT
+*       (14)     not required
+*
+*  Returned:
+*     AOPRMS d(14)  star-independent apparent-to-observed parameters:
+*
+*       (1-13)   not changed
+*       (14)     local apparent sidereal time (radians)
+*
+*  For more information, see sla_AOPPA.
+*
+*  Called:  sla_GMST
+*
+*  P.T.Wallace   Starlink   1 July 1993
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DATE,AOPRMS(14)
+
+      DOUBLE PRECISION sla_GMST
+
+
+
+      AOPRMS(14) = sla_GMST(DATE)+AOPRMS(13)
+
+      END
diff --git a/src/slalib/aopqk.f b/src/slalib/aopqk.f
new file mode 100644
index 0000000..9f8a45c
--- /dev/null
+++ b/src/slalib/aopqk.f
@@ -0,0 +1,242 @@
+      SUBROUTINE sla_AOPQK (RAP, DAP, AOPRMS, AOB, ZOB, HOB, DOB, ROB)
+*+
+*     - - - - - -
+*      A O P Q K
+*     - - - - - -
+*
+*  Quick apparent to observed place (but see note 8, below, for
+*  remarks about speed).
+*
+*  Given:
+*     RAP    d      geocentric apparent right ascension
+*     DAP    d      geocentric apparent declination
+*     AOPRMS d(14)  star-independent apparent-to-observed parameters:
+*
+*       (1)      geodetic latitude (radians)
+*       (2,3)    sine and cosine of geodetic latitude
+*       (4)      magnitude of diurnal aberration vector
+*       (5)      height (HM)
+*       (6)      ambient temperature (T)
+*       (7)      pressure (P)
+*       (8)      relative humidity (RH)
+*       (9)      wavelength (WL)
+*       (10)     lapse rate (TLR)
+*       (11,12)  refraction constants A and B (radians)
+*       (13)     longitude + eqn of equinoxes + sidereal DUT (radians)
+*       (14)     local apparent sidereal time (radians)
+*
+*  Returned:
+*     AOB    d      observed azimuth (radians: N=0,E=90)
+*     ZOB    d      observed zenith distance (radians)
+*     HOB    d      observed Hour Angle (radians)
+*     DOB    d      observed Declination (radians)
+*     ROB    d      observed Right Ascension (radians)
+*
+*  Notes:
+*
+*   1)  This routine returns zenith distance rather than elevation
+*       in order to reflect the fact that no allowance is made for
+*       depression of the horizon.
+*
+*   2)  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 slaRefro routine returns a fixed value of the refraction.
+*       The complementary routines slaAop (or slaAopqk) and slaOap
+*       (or slaOapqk) are self-consistent to better than 1 micro-
+*       arcsecond all over the celestial sphere.
+*
+*   3)  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.
+*
+*   4)  "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 sla_MAP 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
+*       sla_FK425 etc routines.
+*
+*   5)  "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.
+*
+*   6)  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.
+*
+*   7)  The star-independent apparent-to-observed-place parameters
+*       in AOPRMS may be computed by means of the sla_AOPPA routine.
+*       If nothing has changed significantly except the time, the
+*       sla_AOPPAT routine may be used to perform the requisite
+*       partial recomputation of AOPRMS.
+*
+*   8)  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.
+*
+*  9)   The azimuths etc produced by the present routine are with
+*       respect to the celestial pole.  Corrections to the terrestrial
+*       pole can be computed using sla_POLMO.
+*
+*  Called:  sla_DCS2C, sla_REFZ, sla_REFRO, sla_DCC2S, sla_DRANRM
+*
+*  P.T.Wallace   Starlink   22 February 1996
+*
+*  Copyright (C) 1996 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION RAP,DAP,AOPRMS(14),AOB,ZOB,HOB,DOB,ROB
+
+*  Breakpoint for fast/slow refraction algorithm:
+*  ZD greater than arctan(4), (see sla_REFCO routine)
+*  or vector Z less than cosine(arctan(Z)) = 1/sqrt(17)
+      DOUBLE PRECISION ZBREAK
+      PARAMETER (ZBREAK=0.242535625D0)
+
+      INTEGER I
+
+      DOUBLE PRECISION 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
+
+      DOUBLE PRECISION sla_DRANRM
+
+
+
+*  Sin, cos of latitude
+      SPHI = AOPRMS(2)
+      CPHI = AOPRMS(3)
+
+*  Local apparent sidereal time
+      ST = AOPRMS(14)
+
+*  Apparent RA,Dec to Cartesian -HA,Dec
+      CALL sla_DCS2C(RAP-ST,DAP,V)
+      XHD = V(1)
+      YHD = V(2)
+      ZHD = V(3)
+
+*  Diurnal aberration
+      DIURAB = AOPRMS(4)
+      F = (1D0-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.EQ.0D0.AND.YAET.EQ.0D0) THEN
+         AZOBS = 0D0
+      ELSE
+         AZOBS = ATAN2(YAET,-XAET)
+      END IF
+
+*  Topocentric zenith distance
+      ZDT = ATAN2(SQRT(XAET*XAET+YAET*YAET),ZAET)
+
+*
+*  Refraction
+*  ----------
+
+*  Fast algorithm using two constant model
+      REFA = AOPRMS(11)
+      REFB = AOPRMS(12)
+      CALL sla_REFZ(ZDT,REFA,REFB,ZDOBS)
+
+*  Large zenith distance?
+      IF (COS(ZDOBS).LT.ZBREAK) THEN
+
+*     Yes: use rigorous algorithm
+
+*     Initialize loop (maximum of 10 iterations)
+         I = 1
+         DZD = 1D1
+         DO WHILE (ABS(DZD).GT.1D-10.AND.I.LE.10)
+
+*        Compute refraction using current estimate of observed ZD
+            CALL sla_REFRO(ZDOBS,AOPRMS(5),AOPRMS(6),AOPRMS(7),
+     :                     AOPRMS(8),AOPRMS(9),AOPRMS(1),
+     :                     AOPRMS(10),1D-8,DREF)
+
+*        Remaining discrepancy
+            DZD = ZDOBS+DREF-ZDT
+
+*        Update the estimate
+            ZDOBS = ZDOBS-DZD
+
+*        Increment the iteration counter
+            I = I+1
+         END DO
+      END IF
+
+*  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(1) = SPHI*XAEO+CPHI*ZAEO
+      V(2) = YAEO
+      V(3) = -CPHI*XAEO+SPHI*ZAEO
+
+*  To spherical -HA,Dec
+      CALL sla_DCC2S(V,HMOBS,DCOBS)
+
+*  Right Ascension
+      RAOBS = sla_DRANRM(ST+HMOBS)
+
+*  Return the results
+      AOB = AZOBS
+      ZOB = ZDOBS
+      HOB = -HMOBS
+      DOB = DCOBS
+      ROB = RAOBS
+
+      END
diff --git a/src/slalib/atmdsp.f b/src/slalib/atmdsp.f
new file mode 100644
index 0000000..62869aa
--- /dev/null
+++ b/src/slalib/atmdsp.f
@@ -0,0 +1,121 @@
+      SUBROUTINE sla_ATMDSP (TDK, PMB, RH, WL1, A1, B1, WL2, A2, B2)
+*+
+*     - - - - - - -
+*      A T M D S P
+*     - - - - - - -
+*
+*  Apply atmospheric-dispersion adjustments to refraction coefficients.
+*
+*  Given:
+*     TDK       d       ambient temperature, degrees K
+*     PMB       d       ambient pressure, millibars
+*     RH        d       ambient relative humidity, 0-1
+*     WL1       d       reference wavelength, micrometre (0.4D0 recommended)
+*     A1        d       refraction coefficient A for wavelength WL1 (radians)
+*     B1        d       refraction coefficient B for wavelength WL1 (radians)
+*     WL2       d       wavelength for which adjusted A,B required
+*
+*  Returned:
+*     A2        d       refraction coefficient A for wavelength WL2 (radians)
+*     B2        d       refraction coefficient B for wavelength WL2 (radians)
+*
+*  Notes:
+*
+*  1  To use this routine, first call sla_REFCO specifying WL1 as the
+*     wavelength.  This yields refraction coefficients A1,B1, correct
+*     for that wavelength.  Subsequently, calls to sla_ATMDSP specifying
+*     different wavelengths will produce new, slightly adjusted
+*     refraction coefficients which apply to the specified wavelength.
+*
+*  2  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.
+*
+*  3  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.
+*
+*  4  If either wavelength exceeds 100 micrometres, the radio case
+*     is assumed and the returned refraction coefficients are the
+*     same as the given ones.
+*
+*  5  The algorithm consists of calculation of the refractivity of the
+*     air at the observer for the two wavelengths, using the methods
+*     of the sla_REFRO 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).
+*
+*  P.T.Wallace   Starlink   6 October 1995
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION TDK,PMB,RH,WL1,A1,B1,WL2,A2,B2
+
+      DOUBLE PRECISION F,TDKOK,PMBOK,RHOK,
+     :                 PSAT,PWO,W1,WLOK,WLSQ,W2,DN1,DN2
+
+
+*  Check for radio wavelengths
+      IF (WL1.GT.100D0.OR.WL2.GT.100D0) THEN
+
+*     Radio: no dispersion
+         A2 = A1
+         B2 = B1
+      ELSE
+
+*     Optical: keep arguments within safe bounds
+         TDKOK = MIN(MAX(TDK,100D0),500D0)
+         PMBOK = MIN(MAX(PMB,0D0),10000D0)
+         RHOK = MIN(MAX(RH,0D0),1D0)
+
+*     Atmosphere parameters at the observer
+         PSAT = 10D0**(-8.7115D0+0.03477D0*TDKOK)
+         PWO = RHOK*PSAT
+         W1 = 11.2684D-6*PWO
+
+*     Refractivity at the observer for first wavelength
+         WLOK = MAX(WL1,0.1D0)
+         WLSQ = WLOK*WLOK
+         W2 = 77.5317D-6+(0.43909D-6+0.00367D-6/WLSQ)/WLSQ
+         DN1 = (W2*PMBOK-W1)/TDKOK
+
+*     Refractivity at the observer for second wavelength
+         WLOK = MAX(WL2,0.1D0)
+         WLSQ = WLOK*WLOK
+         W2 = 77.5317D-6+(0.43909D-6+0.00367D-6/WLSQ)/WLSQ
+         DN2 = (W2*PMBOK-W1)/TDKOK
+
+*     Scale the refraction coefficients (see Green 4.31, p93)
+         IF (DN1.NE.0D0) THEN
+            F = DN2/DN1
+            A2 = A1*F
+            B2 = B1*F
+            IF (DN1.NE.A1) B2=B2*(1D0+DN1*(DN1-DN2)/(2D0*(DN1-A1)))
+         ELSE
+            A2 = A1
+            B2 = B1
+         END IF
+      END IF
+
+      END
diff --git a/src/slalib/atms.f b/src/slalib/atms.f
new file mode 100644
index 0000000..3b991f4
--- /dev/null
+++ b/src/slalib/atms.f
@@ -0,0 +1,40 @@
+      SUBROUTINE sla__ATMS (RT, TT, DNT, GAMAL, R, DN, RDNDR)
+*+
+*     - - - - -
+*      A T M S
+*     - - - - -
+*
+*  Internal routine used by REFRO
+*
+*  Refractive index and derivative with respect to height for the
+*  stratosphere.
+*
+*  Given:
+*    RT      d    height of tropopause from centre of the Earth (metre)
+*    TT      d    temperature at the tropopause (deg K)
+*    DNT     d    refractive index at the tropopause
+*    GAMAL   d    constant of the atmospheric model = G*MD/R
+*    R       d    current distance from the centre of the Earth (metre)
+*
+*  Returned:
+*    DN      d    refractive index at R
+*    RDNDR   d    R * rate the refractive index is changing at R
+*
+*  P.T.Wallace   Starlink   14 July 1995
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION RT,TT,DNT,GAMAL,R,DN,RDNDR
+
+      DOUBLE PRECISION B,W
+
+
+      B = GAMAL/TT
+      W = (DNT-1D0)*EXP(-B*(R-RT))
+      DN = 1D0+W
+      RDNDR = -R*B*W
+
+      END
diff --git a/src/slalib/atmt.f b/src/slalib/atmt.f
new file mode 100644
index 0000000..82d0ecd
--- /dev/null
+++ b/src/slalib/atmt.f
@@ -0,0 +1,54 @@
+      SUBROUTINE sla__ATMT (R0, T0, ALPHA, GAMM2, DELM2,
+     :                      C1, C2, C3, C4, C5, C6, R, T, DN, RDNDR)
+*+
+*     - - - - -
+*      A T M T
+*     - - - - -
+*
+*  Internal routine used by REFRO
+*
+*  Refractive index and derivative with respect to height for the
+*  troposphere.
+*
+*  Given:
+*    R0      d    height of observer from centre of the Earth (metre)
+*    T0      d    temperature at the observer (deg K)
+*    ALPHA   d    alpha          )
+*    GAMM2   d    gamma minus 2  ) see HMNAO paper
+*    DELM2   d    delta minus 2  )
+*    C1      d    useful term  )
+*    C2      d    useful term  )
+*    C3      d    useful term  ) see source
+*    C4      d    useful term  ) of sla_REFRO
+*    C5      d    useful term  )
+*    C6      d    useful term  )
+*    R       d    current distance from the centre of the Earth (metre)
+*
+*  Returned:
+*    T       d    temperature at R (deg K)
+*    DN      d    refractive index at R
+*    RDNDR   d    R * rate the refractive index is changing at R
+*
+*  Note that in the optical case C5 and C6 are zero.
+*
+*  P.T.Wallace   Starlink   30 May 1997
+*
+*  Copyright (C) 1997 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION R0,T0,ALPHA,GAMM2,DELM2,C1,C2,C3,C4,C5,C6,
+     :                 R,T,DN,RDNDR
+
+      DOUBLE PRECISION TT0,TT0GM2,TT0DM2
+
+
+      T = MAX(MIN(T0-ALPHA*(R-R0),320D0),100D0)
+      TT0 = T/T0
+      TT0GM2 = TT0**GAMM2
+      TT0DM2 = TT0**DELM2
+      DN = 1D0+(C1*TT0GM2-(C2-C5/T)*TT0DM2)*TT0
+      RDNDR = R*(-C3*TT0GM2+(C4-C6/TT0)*TT0DM2)
+
+      END
diff --git a/src/slalib/av2m.f b/src/slalib/av2m.f
new file mode 100644
index 0000000..ec1967c
--- /dev/null
+++ b/src/slalib/av2m.f
@@ -0,0 +1,68 @@
+      SUBROUTINE sla_AV2M (AXVEC, RMAT)
+*+
+*     - - - - -
+*      A V 2 M
+*     - - - - -
+*
+*  Form the rotation matrix corresponding to a given axial vector.
+*
+*  (single precision)
+*
+*  A rotation matrix describes a rotation about some arbitrary axis.
+*  The axis is called the Euler axis, and the angle through which the
+*  reference frame rotates is called the Euler angle.  The axial
+*  vector supplied to this routine has the same direction as the
+*  Euler axis, and its magnitude is the Euler angle in radians.
+*
+*  Given:
+*    AXVEC  r(3)     axial vector (radians)
+*
+*  Returned:
+*    RMAT   r(3,3)   rotation matrix
+*
+*  If AXVEC is null, the unit matrix is returned.
+*
+*  The reference frame rotates clockwise as seen looking along
+*  the axial vector from the origin.
+*
+*  P.T.Wallace   Starlink   June 1989
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL AXVEC(3),RMAT(3,3)
+
+      REAL X,Y,Z,PHI,S,C,W
+
+
+
+*  Euler angle - magnitude of axial vector - and functions
+      X = AXVEC(1)
+      Y = AXVEC(2)
+      Z = AXVEC(3)
+      PHI = SQRT(X*X+Y*Y+Z*Z)
+      S = SIN(PHI)
+      C = COS(PHI)
+      W = 1.0-C
+
+*  Euler axis - direction of axial vector (perhaps null)
+      IF (PHI.NE.0.0) THEN
+         X = X/PHI
+         Y = Y/PHI
+         Z = Z/PHI
+      END IF
+
+*  Compute the rotation matrix
+      RMAT(1,1) = X*X*W+C
+      RMAT(1,2) = X*Y*W+Z*S
+      RMAT(1,3) = X*Z*W-Y*S
+      RMAT(2,1) = X*Y*W-Z*S
+      RMAT(2,2) = Y*Y*W+C
+      RMAT(2,3) = Y*Z*W+X*S
+      RMAT(3,1) = X*Z*W+Y*S
+      RMAT(3,2) = Y*Z*W-X*S
+      RMAT(3,3) = Z*Z*W+C
+
+      END
diff --git a/src/slalib/bear.f b/src/slalib/bear.f
new file mode 100644
index 0000000..11238ff
--- /dev/null
+++ b/src/slalib/bear.f
@@ -0,0 +1,42 @@
+      REAL FUNCTION sla_BEAR (A1, B1, A2, B2)
+*+
+*     - - - - -
+*      B E A R
+*     - - - - -
+*
+*  Bearing (position angle) of one point on a sphere relative to another
+*  (single precision)
+*
+*  Given:
+*     A1,B1    r    spherical coordinates of one point
+*     A2,B2    r    spherical coordinates of the other point
+*
+*  (The spherical coordinates are RA,Dec, Long,Lat etc, in radians.)
+*
+*  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.
+*
+*  P.T.Wallace   Starlink   23 March 1991
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL A1,B1,A2,B2
+
+      REAL DA,X,Y
+
+
+      DA=A2-A1
+      Y=SIN(DA)*COS(B2)
+      X=SIN(B2)*COS(B1)-COS(B2)*SIN(B1)*COS(DA)
+      IF (X.NE.0.0.OR.Y.NE.0.0) THEN
+         sla_BEAR=ATAN2(Y,X)
+      ELSE
+         sla_BEAR=0.0
+      END IF
+
+      END
diff --git a/src/slalib/caf2r.f b/src/slalib/caf2r.f
new file mode 100644
index 0000000..5e5b616
--- /dev/null
+++ b/src/slalib/caf2r.f
@@ -0,0 +1,57 @@
+      SUBROUTINE sla_CAF2R (IDEG, IAMIN, ASEC, RAD, J)
+*+
+*     - - - - - -
+*      C A F 2 R
+*     - - - - - -
+*
+*  Convert degrees, arcminutes, arcseconds to radians
+*  (single precision)
+*
+*  Given:
+*     IDEG        int       degrees
+*     IAMIN       int       arcminutes
+*     ASEC        real      arcseconds
+*
+*  Returned:
+*     RAD         real      angle in radians
+*     J           int       status:  0 = OK
+*                                    1 = IDEG outside range 0-359
+*                                    2 = IAMIN outside range 0-59
+*                                    3 = ASEC outside range 0-59.999...
+*
+*  Notes:
+*
+*  1)  The result is computed even if any of the range checks
+*      fail.
+*
+*  2)  The sign must be dealt with outside this routine.
+*
+*  P.T.Wallace   Starlink   23 August 1996
+*
+*  Copyright (C) 1996 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER IDEG,IAMIN
+      REAL ASEC,RAD
+      INTEGER J
+
+*  Arc seconds to radians
+      REAL AS2R
+      PARAMETER (AS2R=0.484813681109535994E-5)
+
+
+
+*  Preset status
+      J=0
+
+*  Validate arcsec, arcmin, deg
+      IF (ASEC.LT.0.0.OR.ASEC.GE.60.0) J=3
+      IF (IAMIN.LT.0.OR.IAMIN.GT.59) J=2
+      IF (IDEG.LT.0.OR.IDEG.GT.359) J=1
+
+*  Compute angle
+      RAD=AS2R*(60.0*(60.0*REAL(IDEG)+REAL(IAMIN))+ASEC)
+
+      END
diff --git a/src/slalib/caldj.f b/src/slalib/caldj.f
new file mode 100644
index 0000000..c2d9a6d
--- /dev/null
+++ b/src/slalib/caldj.f
@@ -0,0 +1,57 @@
+      SUBROUTINE sla_CALDJ (IY, IM, ID, DJM, J)
+*+
+*     - - - - - -
+*      C A L D J
+*     - - - - - -
+*
+*  Gregorian Calendar to Modified Julian Date
+*
+*  (Includes century default feature:  use sla_CLDJ for years
+*   before 100AD.)
+*
+*  Given:
+*     IY,IM,ID     int    year, month, day in Gregorian calendar
+*
+*  Returned:
+*     DJM          dp     modified Julian Date (JD-2400000.5) for 0 hrs
+*     J            int    status:
+*                           0 = OK
+*                           1 = bad year   (MJD not computed)
+*                           2 = bad month  (MJD not computed)
+*                           3 = bad day    (MJD computed)
+*
+*  Acceptable years are 00-49, interpreted as 2000-2049,
+*                       50-99,     "       "  1950-1999,
+*                       100 upwards, interpreted literally.
+*
+*  Called:  sla_CLDJ
+*
+*  P.T.Wallace   Starlink   November 1985
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER IY,IM,ID
+      DOUBLE PRECISION DJM
+      INTEGER J
+
+      INTEGER NY
+
+
+
+
+*  Default century if appropriate
+      IF (IY.GE.0.AND.IY.LE.49) THEN
+         NY=IY+2000
+      ELSE IF (IY.GE.50.AND.IY.LE.99) THEN
+         NY=IY+1900
+      ELSE
+         NY=IY
+      END IF
+
+*  Modified Julian Date
+      CALL sla_CLDJ(NY,IM,ID,DJM,J)
+
+      END
diff --git a/src/slalib/calyd.f b/src/slalib/calyd.f
new file mode 100644
index 0000000..240a887
--- /dev/null
+++ b/src/slalib/calyd.f
@@ -0,0 +1,65 @@
+      SUBROUTINE sla_CALYD (IY, IM, ID, NY, ND, J)
+*+
+*     - - - - - -
+*      C A L Y D
+*     - - - - - -
+*
+*  Gregorian calendar date to year and day in year (in a Julian
+*  calendar aligned to the 20th/21st century Gregorian calendar).
+*
+*  (Includes century default feature:  use sla_CLYD for years
+*   before 100AD.)
+*
+*  Given:
+*     IY,IM,ID   int    year, month, day in Gregorian calendar
+*                       (year may optionally omit the century)
+*  Returned:
+*     NY         int    year (re-aligned Julian calendar)
+*     ND         int    day in year (1 = January 1st)
+*     J          int    status:
+*                         0 = OK
+*                         1 = bad year (before -4711)
+*                         2 = bad month
+*                         3 = bad day (but conversion performed)
+*
+*  Notes:
+*
+*  1  This routine exists to support the low-precision routines
+*     sla_EARTH, sla_MOON and sla_ECOR.
+*
+*  2  Between 1900 March 1 and 2100 February 28 it returns answers
+*     which are consistent with the ordinary Gregorian calendar.
+*     Outside this range there will be a discrepancy which increases
+*     by one day for every non-leap century year.
+*
+*  3  Years in the range 50-99 are interpreted as 1950-1999, and
+*     years in the range 00-49 are interpreted as 2000-2049.
+*
+*  Called:  sla_CLYD
+*
+*  P.T.Wallace   Starlink   23 November 1994
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER IY,IM,ID,NY,ND,J
+
+      INTEGER I
+
+
+
+*  Default century if appropriate
+      IF (IY.GE.0.AND.IY.LE.49) THEN
+         I=IY+2000
+      ELSE IF (IY.GE.50.AND.IY.LE.99) THEN
+         I=IY+1900
+      ELSE
+         I=IY
+      END IF
+
+*  Perform the conversion
+      CALL sla_CLYD(I,IM,ID,NY,ND,J)
+
+      END
diff --git a/src/slalib/cc2s.f b/src/slalib/cc2s.f
new file mode 100644
index 0000000..2e24b9d
--- /dev/null
+++ b/src/slalib/cc2s.f
@@ -0,0 +1,53 @@
+      SUBROUTINE sla_CC2S (V, A, B)
+*+
+*     - - - - -
+*      C C 2 S
+*     - - - - -
+*
+*  Direction cosines to spherical coordinates (single precision)
+*
+*  Given:
+*     V     r(3)   x,y,z vector
+*
+*  Returned:
+*     A,B   r      spherical coordinates in radians
+*
+*  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.
+*
+*  If V is null, zero A and B are returned.
+*  At either pole, zero A is returned.
+*
+*  P.T.Wallace   Starlink   July 1989
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL V(3),A,B
+
+      REAL X,Y,Z,R
+
+
+      X = V(1)
+      Y = V(2)
+      Z = V(3)
+      R = SQRT(X*X+Y*Y)
+
+      IF (R.EQ.0.0) THEN
+         A = 0.0
+      ELSE
+         A = ATAN2(Y,X)
+      END IF
+
+      IF (Z.EQ.0.0) THEN
+         B = 0.0
+      ELSE
+         B = ATAN2(Z,R)
+      END IF
+
+      END
diff --git a/src/slalib/cc62s.f b/src/slalib/cc62s.f
new file mode 100644
index 0000000..c2ccd8d
--- /dev/null
+++ b/src/slalib/cc62s.f
@@ -0,0 +1,82 @@
+      SUBROUTINE sla_CC62S (V, A, B, R, AD, BD, RD)
+*+
+*     - - - - - -
+*      C C 6 2 S
+*     - - - - - -
+*
+*  Conversion of position & velocity in Cartesian coordinates
+*  to spherical coordinates (single precision)
+*
+*  Given:
+*     V      r(6)   Cartesian position & velocity vector
+*
+*  Returned:
+*     A      r      longitude (radians)
+*     B      r      latitude (radians)
+*     R      r      radial coordinate
+*     AD     r      longitude derivative (radians per unit time)
+*     BD     r      latitude derivative (radians per unit time)
+*     RD     r      radial derivative
+*
+*  P.T.Wallace   Starlink   28 April 1996
+*
+*  Copyright (C) 1996 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL V(6),A,B,R,AD,BD,RD
+
+      REAL X,Y,Z,XD,YD,ZD,RXY2,RXY,R2,XYP
+
+
+
+*  Components of position/velocity vector
+      X=V(1)
+      Y=V(2)
+      Z=V(3)
+      XD=V(4)
+      YD=V(5)
+      ZD=V(6)
+
+*  Component of R in XY plane squared
+      RXY2=X*X+Y*Y
+
+*  Modulus squared
+      R2=RXY2+Z*Z
+
+*  Protection against null vector
+      IF (R2.EQ.0.0) THEN
+         X=XD
+         Y=YD
+         Z=ZD
+         RXY2=X*X+Y*Y
+         R2=RXY2+Z*Z
+      END IF
+
+*  Position and velocity in spherical coordinates
+      RXY=SQRT(RXY2)
+      XYP=X*XD+Y*YD
+      IF (RXY2.NE.0.0) THEN
+         A=ATAN2(Y,X)
+         B=ATAN2(Z,RXY)
+         AD=(X*YD-Y*XD)/RXY2
+         BD=(ZD*RXY2-Z*XYP)/(R2*RXY)
+      ELSE
+         A=0.0
+         IF (Z.NE.0.0) THEN
+            B=ATAN2(Z,RXY)
+         ELSE
+            B=0.0
+         END IF
+         AD=0.0
+         BD=0.0
+      END IF
+      R=SQRT(R2)
+      IF (R.NE.0.0) THEN
+         RD=(XYP+Z*ZD)/R
+      ELSE
+         RD=0.0
+      END IF
+
+      END
diff --git a/src/slalib/cd2tf.f b/src/slalib/cd2tf.f
new file mode 100644
index 0000000..abd26ef
--- /dev/null
+++ b/src/slalib/cd2tf.f
@@ -0,0 +1,55 @@
+      SUBROUTINE sla_CD2TF (NDP, DAYS, SIGN, IHMSF)
+*+
+*     - - - - - -
+*      C D 2 T F
+*     - - - - - -
+*
+*  Convert an interval in days into hours, minutes, seconds
+*
+*  (single precision)
+*
+*  Given:
+*     NDP       int      number of decimal places of seconds
+*     DAYS      real     interval in days
+*
+*  Returned:
+*     SIGN      char     '+' or '-'
+*     IHMSF     int(4)   hours, minutes, seconds, fraction
+*
+*  Notes:
+*
+*     1)  NDP less than zero is interpreted as zero.
+*
+*     2)  The largest useful value for NDP is determined by the size of
+*         DAYS, the format of REAL floating-point numbers on the target
+*         machine, and the risk of overflowing IHMSF(4).  For example,
+*         on the VAX, for DAYS up to 1.0, the available floating-point
+*         precision corresponds roughly to NDP=3.  This is well below
+*         the ultimate limit of NDP=9 set by the capacity of the 32-bit
+*         integer IHMSF(4).
+*
+*     3)  The absolute value of DAYS may exceed 1.0.  In cases where it
+*         does not, it is up to the caller to test for and handle the
+*         case where DAYS is very nearly 1.0 and rounds up to 24 hours,
+*         by testing for IHMSF(1)=24 and setting IHMSF(1-4) to zero.
+*
+*  Called:  sla_DD2TF
+*
+*  P.T.Wallace   Starlink   12 December 1993
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER NDP
+      REAL DAYS
+      CHARACTER SIGN*(*)
+      INTEGER IHMSF(4)
+
+
+
+*  Call double precision version
+      CALL sla_DD2TF(NDP,DBLE(DAYS),SIGN,IHMSF)
+
+      END
diff --git a/src/slalib/cldj.f b/src/slalib/cldj.f
new file mode 100644
index 0000000..0536259
--- /dev/null
+++ b/src/slalib/cldj.f
@@ -0,0 +1,78 @@
+      SUBROUTINE sla_CLDJ (IY, IM, ID, DJM, J)
+*+
+*     - - - - -
+*      C L D J
+*     - - - - -
+*
+*  Gregorian Calendar to Modified Julian Date
+*
+*  Given:
+*     IY,IM,ID     int    year, month, day in Gregorian calendar
+*
+*  Returned:
+*     DJM          dp     modified Julian Date (JD-2400000.5) for 0 hrs
+*     J            int    status:
+*                           0 = OK
+*                           1 = bad year   (MJD not computed)
+*                           2 = bad month  (MJD not computed)
+*                           3 = bad day    (MJD computed)
+*
+*  The year must be -4699 (i.e. 4700BC) or later.
+*
+*  The algorithm is derived from that of Hatcher 1984
+*  (QJRAS 25, 53-55).
+*
+*  P.T.Wallace   Starlink   11 March 1998
+*
+*  Copyright (C) 1998 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER IY,IM,ID
+      DOUBLE PRECISION DJM
+      INTEGER J
+
+*  Month lengths in days
+      INTEGER MTAB(12)
+      DATA MTAB / 31,28,31,30,31,30,31,31,30,31,30,31 /
+
+
+
+*  Preset status
+      J=0
+
+*  Validate year
+      IF (IY.LT.-4699) THEN
+         J=1
+      ELSE
+
+*     Validate month
+         IF (IM.GE.1.AND.IM.LE.12) THEN
+
+*        Allow for leap year
+            IF (MOD(IY,4).EQ.0) THEN
+               MTAB(2)=29
+            ELSE
+               MTAB(2)=28
+            END IF
+            IF (MOD(IY,100).EQ.0.AND.MOD(IY,400).NE.0)
+     :         MTAB(2)=28
+
+*        Validate day
+            IF (ID.LT.1.OR.ID.GT.MTAB(IM)) J=3
+
+*        Modified Julian Date
+            DJM=DBLE((1461*(IY-(12-IM)/10+4712))/4
+     :               +(306*MOD(IM+9,12)+5)/10
+     :               -(3*((IY-(12-IM)/10+4900)/100))/4
+     :               +ID-2399904)
+
+*        Bad month
+         ELSE
+            J=2
+         END IF
+
+      END IF
+
+      END
diff --git a/src/slalib/clyd.f b/src/slalib/clyd.f
new file mode 100644
index 0000000..ee4fb92
--- /dev/null
+++ b/src/slalib/clyd.f
@@ -0,0 +1,101 @@
+      SUBROUTINE sla_CLYD (IY, IM, ID, NY, ND, JSTAT)
+*+
+*     - - - - -
+*      C L Y D
+*     - - - - -
+*
+*  Gregorian calendar to year and day in year (in a Julian calendar
+*  aligned to the 20th/21st century Gregorian calendar).
+*
+*  Given:
+*     IY,IM,ID   i    year, month, day in Gregorian calendar
+*
+*  Returned:
+*     NY         i    year (re-aligned Julian calendar)
+*     ND         i    day in year (1 = January 1st)
+*     JSTAT      i    status:
+*                       0 = OK
+*                       1 = bad year (before -4711)
+*                       2 = bad month
+*                       3 = bad day (but conversion performed)
+*
+*  Notes:
+*
+*  1  This routine exists to support the low-precision routines
+*     sla_EARTH, sla_MOON and sla_ECOR.
+*
+*  2  Between 1900 March 1 and 2100 February 28 it returns answers
+*     which are consistent with the ordinary Gregorian calendar.
+*     Outside this range there will be a discrepancy which increases
+*     by one day for every non-leap century year.
+*
+*  3  The essence of the algorithm is first to express the Gregorian
+*     date as a Julian Day Number and then to convert this back to
+*     a Julian calendar date, with day-in-year instead of month and
+*     day.  See 12.92-1 and 12.95-1 in the reference.
+*
+*  Reference:  Explanatory Supplement to the Astronomical Almanac,
+*              ed P.K.Seidelmann, University Science Books (1992),
+*              p604-606.
+*
+*  P.T.Wallace   Starlink   26 November 1994
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER IY,IM,ID,NY,ND,JSTAT
+
+      INTEGER I,J,K,L,N
+
+*  Month lengths in days
+      INTEGER MTAB(12)
+      DATA MTAB/31,28,31,30,31,30,31,31,30,31,30,31/
+
+
+
+*  Preset status
+      JSTAT=0
+
+*  Validate year
+      IF (IY.GE.-4711) THEN
+
+*     Validate month
+         IF (IM.GE.1.AND.IM.LE.12) THEN
+
+*        Allow for (Gregorian) leap year
+            IF (MOD(IY,4).EQ.0.AND.
+     :         (MOD(IY,100).NE.0.OR.MOD(IY,400).EQ.0)) THEN
+               MTAB(2)=29
+            ELSE
+               MTAB(2)=28
+            END IF
+
+*        Validate day
+            IF (ID.LT.1.OR.ID.GT.MTAB(IM)) JSTAT=3
+
+*        Perform the conversion
+            I=(14-IM)/12
+            K=IY-I
+            J=(1461*(K+4800))/4+(367*(IM-2+12*I))/12
+     :        -(3*((K+4900)/100))/4+ID-30660
+            K=(J-1)/1461
+            L=J-1461*K
+            N=(L-1)/365-L/1461
+            J=((80*(L-365*N+30))/2447)/11
+            I=N+J
+            ND=59+L-365*I+((4-N)/4)*(1-J)
+            NY=4*K+I-4716
+
+*        Bad month
+         ELSE
+            JSTAT=2
+         END IF
+      ELSE
+
+*     Bad year
+         JSTAT=1
+      END IF
+
+      END
diff --git a/src/slalib/combn.f b/src/slalib/combn.f
new file mode 100644
index 0000000..9e2354d
--- /dev/null
+++ b/src/slalib/combn.f
@@ -0,0 +1,142 @@
+      SUBROUTINE sla_COMBN ( NSEL, NCAND, LIST, J )
+*+
+*     - - - - - -
+*      C O M B N
+*     - - - - - -
+*
+*  Generate the next combination, a subset of a specified size chosen
+*  from a specified number of items.
+*
+*  Given:
+*     NSEL     i        number of items (subset size)
+*     NCAND    i        number of candidates (set size)
+*
+*  Given and returned:
+*     LIST     i(NSEL)  latest combination, LIST(1)=0 to initialize
+*
+*  Returned:
+*     J        i        status: -1 = illegal NSEL or NCAND
+*                                0 = OK
+*                               +1 = no more combinations available
+*
+*  Notes:
+*
+*  1) NSEL and NCAND must both be at least 1, and NSEL must be less
+*     than or equal to NCAND.
+*
+*  2) This routine returns, in the LIST array, a subset of NSEL integers
+*     chosen from the range 1 to NCAND inclusive, in ascending order.
+*     Before calling the routine for the first time, the caller must set
+*     the first element of the LIST array to zero (any value less than 1
+*     will do) to cause initialization.
+*
+*  2) The first combination to be generated is:
+*
+*        LIST(1)=1, LIST(2)=2, ..., LIST(NSEL)=NSEL
+*
+*     This is also the combination returned for the "finished" (J=1)
+*     case.
+*
+*     The final permutation to be generated is:
+*
+*        LIST(1)=NCAND, LIST(2)=NCAND-1, ..., LIST(NSEL)=NCAND-NSEL+1
+*
+*  3) If the "finished" (J=1) status is ignored, the routine
+*     continues to deliver combinations, the pattern repeating
+*     every NCAND!/(NSEL!*(NCAND-NSEL)!) calls.
+*
+*  4) The algorithm is by R.F.Warren-Smith (private communication).
+*
+*  P.T.Wallace   Starlink   25 August 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER NSEL,NCAND,LIST(NSEL),J
+
+      INTEGER I,LISTI,NMAX,M
+      LOGICAL MORE
+
+
+*  Validate, and set status.
+      IF (NSEL.LT.1.OR.NCAND.LT.1.OR.NSEL.GT.NCAND) THEN
+         J = -1
+         GO TO 9999
+      ELSE
+         J = 0
+      END IF
+
+*  Just starting?
+      IF (LIST(1).LT.1) THEN
+
+*     Yes: return 1,2,3...
+         DO I=1,NSEL
+            LIST(I) = I
+         END DO
+
+      ELSE
+
+*     No: find the first selection that we can increment.
+
+*     Start with the first list item.
+         I = 1
+
+*     Loop.
+         MORE = .TRUE.
+         DO WHILE (MORE)
+
+*        Current list item.
+            LISTI = LIST(I)
+
+*        Is this the final list item?
+            IF (I.GE.NSEL) THEN
+
+*           Yes:  comparison value is number of candidates plus one.
+               NMAX = NCAND+1
+            ELSE
+
+*           No:  comparison value is next list item.
+               NMAX = LIST(I+1)
+            END IF
+
+*        Can the current item be incremented?
+            IF (NMAX-LISTI.GT.1) THEN
+
+*           Yes:  increment it.
+               LIST(I) = LISTI+1
+
+*           Reinitialize the preceding items.
+               DO M=1,I-1
+                  LIST(M) = M
+               END DO
+
+*           Break.
+               MORE = .FALSE.
+            ELSE
+
+*           Can't increment the current item:  is it the final one?
+               IF (I.GE.NSEL) THEN
+
+*              Yes:  set the status.
+                  J = 1
+
+*              Restart the sequence.
+                  DO I=1,NSEL
+                     LIST(I) = I
+                  END DO
+
+*              Break.
+                  MORE = .FALSE.
+               ELSE
+
+*              No:  next list item.
+                  I = I+1
+               END IF
+            END IF
+         END DO
+      END IF
+ 9999 CONTINUE
+
+      END
diff --git a/src/slalib/cr2af.f b/src/slalib/cr2af.f
new file mode 100644
index 0000000..74afa0f
--- /dev/null
+++ b/src/slalib/cr2af.f
@@ -0,0 +1,58 @@
+      SUBROUTINE sla_CR2AF (NDP, ANGLE, SIGN, IDMSF)
+*+
+*     - - - - - -
+*      C R 2 A F
+*     - - - - - -
+*
+*  Convert an angle in radians into degrees, arcminutes, arcseconds
+*  (single precision)
+*
+*  Given:
+*     NDP       int      number of decimal places of arcseconds
+*     ANGLE     real     angle in radians
+*
+*  Returned:
+*     SIGN      char     '+' or '-'
+*     IDMSF     int(4)   degrees, arcminutes, arcseconds, fraction
+*
+*  Notes:
+*
+*     1)  NDP less than zero is interpreted as zero.
+*
+*     2)  The largest useful value for NDP is determined by the size of
+*         ANGLE, the format of REAL floating-point numbers on the target
+*         machine, and the risk of overflowing IDMSF(4).  For example,
+*         on the VAX, for ANGLE up to 2pi, the available floating-point
+*         precision corresponds roughly to NDP=3.  This is well below
+*         the ultimate limit of NDP=9 set by the capacity of the 32-bit
+*         integer IHMSF(4).
+*
+*     3)  The absolute value of ANGLE may exceed 2pi.  In cases where it
+*         does not, it is up to the caller to test for and handle the
+*         case where ANGLE is very nearly 2pi and rounds up to 360 deg,
+*         by testing for IDMSF(1)=360 and setting IDMSF(1-4) to zero.
+*
+*  Called:  sla_CD2TF
+*
+*  P.T.Wallace   Starlink   18 March 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER NDP
+      REAL ANGLE
+      CHARACTER SIGN*(*)
+      INTEGER IDMSF(4)
+
+*  Hours to degrees * radians to turns
+      REAL F
+      PARAMETER (F=15.0/6.283185307179586476925287)
+
+
+
+*  Scale then use days to h,m,s routine
+      CALL sla_CD2TF(NDP,ANGLE*F,SIGN,IDMSF)
+
+      END
diff --git a/src/slalib/cr2tf.f b/src/slalib/cr2tf.f
new file mode 100644
index 0000000..3e9214b
--- /dev/null
+++ b/src/slalib/cr2tf.f
@@ -0,0 +1,58 @@
+      SUBROUTINE sla_CR2TF (NDP, ANGLE, SIGN, IHMSF)
+*+
+*     - - - - - -
+*      C R 2 T F
+*     - - - - - -
+*
+*  Convert an angle in radians into hours, minutes, seconds
+*  (single precision)
+*
+*  Given:
+*     NDP       int      number of decimal places of seconds
+*     ANGLE     real     angle in radians
+*
+*  Returned:
+*     SIGN      char     '+' or '-'
+*     IHMSF     int(4)   hours, minutes, seconds, fraction
+*
+*  Notes:
+*
+*  1)  NDP less than zero is interpreted as zero.
+*
+*  2)  The largest useful value for NDP is determined by the size of
+*      ANGLE, the format of REAL floating-point numbers on the target
+*      machine, and the risk of overflowing IHMSF(4).  For example,
+*      on the VAX, for ANGLE up to 2pi, the available floating-point
+*      precision corresponds roughly to NDP=3.  This is well below
+*      the ultimate limit of NDP=9 set by the capacity of the 32-bit
+*      integer IHMSF(4).
+*
+*  3)  The absolute value of ANGLE may exceed 2pi.  In cases where it
+*      does not, it is up to the caller to test for and handle the
+*      case where ANGLE is very nearly 2pi and rounds up to 24 hours,
+*      by testing for IHMSF(1)=24 and setting IHMSF(1-4) to zero.
+*
+*  Called:  sla_CD2TF
+*
+*  P.T.Wallace   Starlink   18 March 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER NDP
+      REAL ANGLE
+      CHARACTER SIGN*(*)
+      INTEGER IHMSF(4)
+
+*  Turns to radians
+      REAL T2R
+      PARAMETER (T2R=6.283185307179586476925287)
+
+
+
+*  Scale then use days to h,m,s routine
+      CALL sla_CD2TF(NDP,ANGLE/T2R,SIGN,IHMSF)
+
+      END
diff --git a/src/slalib/create.com b/src/slalib/create.com
new file mode 100755
index 0000000..161584c
--- /dev/null
+++ b/src/slalib/create.com
@@ -0,0 +1,140 @@
+$!
+$!  - - - - - - -
+$!   C R E A T E
+$!  - - - - - - -
+$!
+$!  Create SLALIB releases from source - VAX and Unix
+$!
+$!  The command is @CREATE
+$!
+$!  The default directory must be the one containing the source
+$!  modules.  The VAX release will be inserted into [.RELEASE]
+$!  and the Unix release into [.UNIX].  Prior contents of any
+$!  pre-existing [.RELEASE] and [.UNIX] directories will be lost.
+$!
+$!  P.T.Wallace   Starlink   22 January 1998
+$!
+$!----------------------------------------------------------------------
+$!
+$!  VMS
+$!
+$!  Create an empty [.RELEASE] directory
+$     IF F$SEARCH("RELEASE.DIR").EQS."" THEN $CREATE/DIR [.RELEASE]
+$     IF F$SEARCH("[.RELEASE]*.*").NES."" THEN $DELETE [.RELEASE]*.*;*
+$!
+$!  Copy the document and news item
+$     COPY SUN67.TEX [.RELEASE]*.*
+$     COPY SLA.NEWS [.RELEASE]*.*
+$!
+$!  Initialise the text and object libraries
+$     LIBR/CREATE/TEXT [.RELEASE]SLALIB.TLB
+$     PURGE [.RELEASE]SLALIB.TLB
+$     LIBR/CREATE [.RELEASE]SLALIB.OLB
+$     PURGE [.RELEASE]SLALIB.OLB
+$!
+$!  Update the libraries
+$UPOBJ:
+$      FILE = F$SEARCH("*.FOR")
+$      IF FILE .EQS. "" THEN GOTO UPOBJX
+$      NAME = F$PARSE(FILE,,,"NAME")
+$      @PUT 'NAME'
+$     GOTO UPOBJ
+$UPOBJX:
+$     @PUT GRESID.VAX
+$     @PUT RANDOM.VAX
+$     @PUT WAIT.VAX
+$!
+$!  Compress
+$     LIBR/COMP/DATA=REDUCE/TEXT/OUTPUT=[.RELEASE]SLALIB.TLB -
+                                        [.RELEASE]SLALIB.TLB
+$     PURGE [.RELEASE]SLALIB.TLB
+$     LIBR/COMP/OUTPUT=[.RELEASE]SLALIB.OLB [.RELEASE]SLALIB.OLB
+$     PURGE [.RELEASE]SLALIB.OLB
+$!
+$!----------------------------------------------------------------------
+$!
+$!  UNIX
+$!
+$!  Create an empty [.UNIX] directory
+$     IF F$SEARCH("UNIX.DIR").EQS."" THEN $CREATE/DIR [.UNIX]
+$     IF F$SEARCH("[.UNIX]*.*").NES."" THEN $DELETE [.UNIX]*.*;*
+$!
+$!  Copy the platform-independent Fortran source
+$FLOOP:
+$     FILE = F$SEARCH("*.FOR")
+$     IF FILE.EQS."" THEN $GOTO FLOOPX
+$     FILE=F$EXTRACT(0,F$LOCATE(";",FILE),FILE)
+$     NAME = F$PARSE(FILE,,,"NAME")
+$     IF NAME .EQS. "GRESID" THEN $GOTO FLOOP
+$     IF NAME .EQS. "RANDOM" THEN $GOTO FLOOP
+$     IF NAME .EQS. "WAIT" THEN $GOTO FLOOP
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT 'FILE' [.UNIX]'NAME'.F
+$     GOTO FLOOP
+$FLOOPX:
+$!
+$!  Copy the platform specific source code
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT GRESID.VAX [.UNIX]GRESID.VAX
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT GRESID.PCM [.UNIX]GRESID.PCM
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT GRESID.CNVX [.UNIX]GRESID.CNVX
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT GRESID.MIPS [.UNIX]GRESID.MIPS
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT GRESID.SUN4 [.UNIX]GRESID.SUN4
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT GRESID.LNX [.UNIX]GRESID.LNX
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT GRESID.DEC [.UNIX]GRESID.DEC
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT RANDOM.VAX [.UNIX]RANDOM.VAX
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT RANDOM.PCM [.UNIX]RANDOM.PCM
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT RANDOM.CNVX [.UNIX]RANDOM.CNVX
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT RANDOM.MIPS [.UNIX]RANDOM.MIPS
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT RANDOM.SUN4 [.UNIX]RANDOM.SUN4
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT RANDOM.LNX [.UNIX]RANDOM.LNX
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT RANDOM.DEC [.UNIX]RANDOM.DEC
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT RTL_RANDOM.C [.UNIX]RTL_RANDOM.C
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT WAIT.VAX [.UNIX]WAIT.VAX
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT WAIT.PCM [.UNIX]WAIT.PCM
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT WAIT.CNVX [.UNIX]WAIT.CNVX
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT WAIT.MIPS [.UNIX]WAIT.MIPS
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT WAIT.SUN4 [.UNIX]WAIT.SUN4
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT WAIT.LNX [.UNIX]WAIT.LNX
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT WAIT.DEC [.UNIX]WAIT.DEC
+$!
+$!  Copy the miscellaneous files
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT MK [.UNIX]MK
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT MAKEFILE [.UNIX]MAKEFILE
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT SLA_LINK [.UNIX]SLA_LINK
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT SLA_LINK_ADAM [.UNIX]SLA_LINK_ADAM
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT SUN67.TEX [.UNIX]SUN67.TEX
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT READ.ME [.UNIX]READ.ME
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT SLA.NEWS [.UNIX]SLA.NEWS
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT PC.BAT [.UNIX]PC.BAT
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT REP.BAT [.UNIX]REP.BAT
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT CREATE.COM [.UNIX]CREATE.COM
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT PUT.COM [.UNIX]PUT.COM
+$     CONVERT/FDL=SYS$SYSTEM:UCX$CONVERT VAX_TO_UNIX.USH [.UNIX]VAX_TO_UNIX.
+$!                                                   ^^^
+$!                                    The USH suffix prevents accidental
+$!                                    execution of the script when the
+$!                                    working directory is .RELEASE instead
+$!                                    of .UNIX
+$!
+$!  Explain what to do next
+$     COPY SYS$INPUT SYS$OUTPUT
+
+   To complete building the Unix release, please do the following:
+
+   1) Login to the Unix machine.
+
+   2) Locate the NFS-served directory corresponding to subdirectory
+      [.UNIX] of the current default directory.
+
+   3) For efficiency, and to avoid possible problems involving case
+      sensitivity in filenames, copy all the files in that directory
+      to a scratch directory on the Unix machine.
+
+   4) Type "vax_to_unix" to archive all the source files.
+
+$!
+$!----------------------------------------------------------------------
+$!
+$!  Wrap up
+$     PURGE [...]
+$     SET FILE/TRUNCATE [...]*.*/EXCLUDE=CREATE.COM
+$     EXIT
diff --git a/src/slalib/cs2c.f b/src/slalib/cs2c.f
new file mode 100644
index 0000000..7d516c8
--- /dev/null
+++ b/src/slalib/cs2c.f
@@ -0,0 +1,41 @@
+      SUBROUTINE sla_CS2C (A, B, V)
+*+
+*     - - - - -
+*      C S 2 C
+*     - - - - -
+*
+*  Spherical coordinates to direction cosines (single precision)
+*
+*  Given:
+*     A,B      real      spherical coordinates in radians
+*                        (RA,Dec), (Long,Lat) etc
+*
+*  Returned:
+*     V        real(3)   x,y,z unit vector
+*
+*  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.
+*
+*  P.T.Wallace   Starlink   October 1984
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL A,B,V(3)
+
+      REAL COSB
+
+
+
+      COSB=COS(B)
+
+      V(1)=COS(A)*COSB
+      V(2)=SIN(A)*COSB
+      V(3)=SIN(B)
+
+      END
diff --git a/src/slalib/cs2c6.f b/src/slalib/cs2c6.f
new file mode 100644
index 0000000..e0b9e06
--- /dev/null
+++ b/src/slalib/cs2c6.f
@@ -0,0 +1,56 @@
+      SUBROUTINE sla_CS2C6 (A, B, R, AD, BD, RD, V)
+*+
+*     - - - - - -
+*      C S 2 C 6
+*     - - - - - -
+*
+*  Conversion of position & velocity in spherical coordinates
+*  to Cartesian coordinates (single precision)
+*
+*  Given:
+*     A     r      longitude (radians)
+*     B     r      latitude (radians)
+*     R     r      radial coordinate
+*     AD    r      longitude derivative (radians per unit time)
+*     BD    r      latitude derivative (radians per unit time)
+*     RD    r      radial derivative
+*
+*  Returned:
+*     V     r(6)   Cartesian position & velocity vector
+*
+*  P.T.Wallace   Starlink   November 1984
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL A,B,R,AD,BD,RD,V(6)
+
+      REAL SA,CA,SB,CB,RCB,X,Y,RBD,CBRD,W
+
+
+
+*  Useful functions
+      SA=SIN(A)
+      CA=COS(A)
+      SB=SIN(B)
+      CB=COS(B)
+      RCB=R*CB
+      X=RCB*CA
+      Y=RCB*SA
+      RBD=R*BD
+      CBRD=CB*RD
+      W=RBD*SB-CB*RD
+
+*  Position
+      V(1)=X
+      V(2)=Y
+      V(3)=R*SB
+
+*  Velocity
+      V(4)=-Y*AD-W*CA
+      V(5)=X*AD-W*SA
+      V(6)=RBD*CB+SB*RD
+
+      END
diff --git a/src/slalib/ctf2d.f b/src/slalib/ctf2d.f
new file mode 100644
index 0000000..9280616
--- /dev/null
+++ b/src/slalib/ctf2d.f
@@ -0,0 +1,56 @@
+      SUBROUTINE sla_CTF2D (IHOUR, IMIN, SEC, DAYS, J)
+*+
+*     - - - - - -
+*      C T F 2 D
+*     - - - - - -
+*
+*  Convert hours, minutes, seconds to days (single precision)
+*
+*  Given:
+*     IHOUR       int       hours
+*     IMIN        int       minutes
+*     SEC         real      seconds
+*
+*  Returned:
+*     DAYS        real      interval in days
+*     J           int       status:  0 = OK
+*                                    1 = IHOUR outside range 0-23
+*                                    2 = IMIN outside range 0-59
+*                                    3 = SEC outside range 0-59.999...
+*
+*  Notes:
+*
+*  1)  The result is computed even if any of the range checks
+*      fail.
+*
+*  2)  The sign must be dealt with outside this routine.
+*
+*  P.T.Wallace   Starlink   November 1984
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER IHOUR,IMIN
+      REAL SEC,DAYS
+      INTEGER J
+
+*  Seconds per day
+      REAL D2S
+      PARAMETER (D2S=86400.0)
+
+
+
+*  Preset status
+      J=0
+
+*  Validate sec, min, hour
+      IF (SEC.LT.0.0.OR.SEC.GE.60.0) J=3
+      IF (IMIN.LT.0.OR.IMIN.GT.59) J=2
+      IF (IHOUR.LT.0.OR.IHOUR.GT.23) J=1
+
+*  Compute interval
+      DAYS=(60.0*(60.0*REAL(IHOUR)+REAL(IMIN))+SEC)/D2S
+
+      END
diff --git a/src/slalib/ctf2r.f b/src/slalib/ctf2r.f
new file mode 100644
index 0000000..585d587
--- /dev/null
+++ b/src/slalib/ctf2r.f
@@ -0,0 +1,54 @@
+      SUBROUTINE sla_CTF2R (IHOUR, IMIN, SEC, RAD, J)
+*+
+*     - - - - - -
+*      C T F 2 R
+*     - - - - - -
+*
+*  Convert hours, minutes, seconds to radians (single precision)
+*
+*  Given:
+*     IHOUR       int       hours
+*     IMIN        int       minutes
+*     SEC         real      seconds
+*
+*  Returned:
+*     RAD         real      angle in radians
+*     J           int       status:  0 = OK
+*                                    1 = IHOUR outside range 0-23
+*                                    2 = IMIN outside range 0-59
+*                                    3 = SEC outside range 0-59.999...
+*
+*  Called:
+*     sla_CTF2D
+*
+*  Notes:
+*
+*  1)  The result is computed even if any of the range checks
+*      fail.
+*
+*  2)  The sign must be dealt with outside this routine.
+*
+*  P.T.Wallace   Starlink   November 1984
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER IHOUR,IMIN
+      REAL SEC,RAD
+      INTEGER J
+
+      REAL TURNS
+
+*  Turns to radians
+      REAL T2R
+      PARAMETER (T2R=6.283185307179586476925287)
+
+
+
+*  Convert to turns then radians
+      CALL sla_CTF2D(IHOUR,IMIN,SEC,TURNS,J)
+      RAD=T2R*TURNS
+
+      END
diff --git a/src/slalib/daf2r.f b/src/slalib/daf2r.f
new file mode 100644
index 0000000..3f89864
--- /dev/null
+++ b/src/slalib/daf2r.f
@@ -0,0 +1,55 @@
+      SUBROUTINE sla_DAF2R (IDEG, IAMIN, ASEC, RAD, J)
+*+
+*     - - - - - -
+*      D A F 2 R
+*     - - - - - -
+*
+*  Convert degrees, arcminutes, arcseconds to radians
+*  (double precision)
+*
+*  Given:
+*     IDEG        int       degrees
+*     IAMIN       int       arcminutes
+*     ASEC        dp        arcseconds
+*
+*  Returned:
+*     RAD         dp        angle in radians
+*     J           int       status:  0 = OK
+*                                    1 = IDEG outside range 0-359
+*                                    2 = IAMIN outside range 0-59
+*                                    3 = ASEC outside range 0-59.999...
+*
+*  Notes:
+*     1)  The result is computed even if any of the range checks
+*         fail.
+*     2)  The sign must be dealt with outside this routine.
+*
+*  P.T.Wallace   Starlink   23 August 1996
+*
+*  Copyright (C) 1996 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER IDEG,IAMIN
+      DOUBLE PRECISION ASEC,RAD
+      INTEGER J
+
+*  Arc seconds to radians
+      DOUBLE PRECISION AS2R
+      PARAMETER (AS2R=0.484813681109535994D-5)
+
+
+
+*  Preset status
+      J=0
+
+*  Validate arcsec, arcmin, deg
+      IF (ASEC.LT.0D0.OR.ASEC.GE.60D0) J=3
+      IF (IAMIN.LT.0.OR.IAMIN.GT.59) J=2
+      IF (IDEG.LT.0.OR.IDEG.GT.359) J=1
+
+*  Compute angle
+      RAD=AS2R*(60D0*(60D0*DBLE(IDEG)+DBLE(IAMIN))+ASEC)
+
+      END
diff --git a/src/slalib/dafin.f b/src/slalib/dafin.f
new file mode 100644
index 0000000..e8dc456
--- /dev/null
+++ b/src/slalib/dafin.f
@@ -0,0 +1,163 @@
+      SUBROUTINE sla_DAFIN (STRING, IPTR, A, J)
+*+
+*     - - - - - -
+*      D A F I N
+*     - - - - - -
+*
+*  Sexagesimal character string to angle (double precision)
+*
+*  Given:
+*     STRING  c*(*)   string containing deg, arcmin, arcsec fields
+*     IPTR      i     pointer to start of decode (1st = 1)
+*
+*  Returned:
+*     IPTR      i     advanced past the decoded angle
+*     A         d     angle in radians
+*     J         i     status:  0 = OK
+*                             +1 = default, A unchanged
+*                             -1 = bad degrees      )
+*                             -2 = bad arcminutes   )  (note 3)
+*                             -3 = bad arcseconds   )
+*
+*  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
+*
+*    A further call to sla_DAFIN, without adjustment of IPTR, will
+*    decode the second angle, 12deg 34min 56.7sec.
+*
+*  Notes:
+*
+*     1)  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 DFLTIN routine and is free-format.
+*
+*     2)  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.
+*
+*     3)  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...
+*
+*     4)  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.
+*
+*     5)  Further fields after the three expected ones are not treated
+*         as an error.  The pointer IPTR is left in the correct state
+*         for further decoding with the present routine or with DFLTIN
+*         etc. See the example, above.
+*
+*     6)  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       =  1D0
+*           d ' "      turns        1/2pi   =  0.1591549430918953358D0
+*           h m s      radians      15      =  15D0
+*           h m s      days         15/2pi  =  2.3873241463784300365D0
+*
+*  Called:  sla_DFLTIN
+*
+*  P.T.Wallace   Starlink   1 August 1996
+*
+*  Copyright (C) 1996 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      CHARACTER*(*) STRING
+      INTEGER IPTR
+      DOUBLE PRECISION A
+      INTEGER J
+
+      DOUBLE PRECISION AS2R
+      PARAMETER (AS2R=4.84813681109535993589914102358D-6)
+      INTEGER JF,JD,JM,JS
+      DOUBLE PRECISION DEG,ARCMIN,ARCSEC
+
+
+
+*  Preset the status to OK
+      JF=0
+
+*  Defaults
+      DEG=0D0
+      ARCMIN=0D0
+      ARCSEC=0D0
+
+*  Decode degrees, arcminutes, arcseconds
+      CALL sla_DFLTIN(STRING,IPTR,DEG,JD)
+      IF (JD.GT.1) THEN
+         JF=-1
+      ELSE
+         CALL sla_DFLTIN(STRING,IPTR,ARCMIN,JM)
+         IF (JM.LT.0.OR.JM.GT.1) THEN
+            JF=-2
+         ELSE
+            CALL sla_DFLTIN(STRING,IPTR,ARCSEC,JS)
+            IF (JS.LT.0.OR.JS.GT.1) THEN
+               JF=-3
+
+*        See if the combination of fields is credible
+            ELSE IF (JD.GT.0) THEN
+*           No degrees:  arcmin, arcsec ought also to be absent
+               IF (JM.EQ.0) THEN
+*              Suspect arcmin
+                  JF=-2
+               ELSE IF (JS.EQ.0) THEN
+*              Suspect arcsec
+                  JF=-3
+               ELSE
+*              All three fields absent
+                  JF=1
+               END IF
+*        Degrees present:  if arcsec present so ought arcmin to be
+            ELSE IF (JM.NE.0.AND.JS.EQ.0) THEN
+               JF=-3
+
+*        Tests for range and integrality
+
+*        Degrees
+            ELSE IF (JM.EQ.0.AND.DINT(DEG).NE.DEG) THEN
+               JF=-1
+*        Arcminutes
+            ELSE IF ((JS.EQ.0.AND.DINT(ARCMIN).NE.ARCMIN).OR.
+     :               ARCMIN.GE.60D0) THEN
+               JF=-2
+*        Arcseconds
+            ELSE IF (ARCSEC.GE.60D0) THEN
+               JF=-3
+            END IF
+         END IF
+      END IF
+
+*  Unless all three fields absent, compute angle value
+      IF (JF.LE.0) THEN
+         A=AS2R*(60D0*(60D0*ABS(DEG)+ARCMIN)+ARCSEC)
+         IF (JD.LT.0) A=-A
+      END IF
+
+*  Return the status
+      J=JF
+
+      END
diff --git a/src/slalib/dat.f b/src/slalib/dat.f
new file mode 100644
index 0000000..423e59b
--- /dev/null
+++ b/src/slalib/dat.f
@@ -0,0 +1,219 @@
+      DOUBLE PRECISION FUNCTION sla_DAT (UTC)
+*+
+*     - - - -
+*      D A T
+*     - - - -
+*
+*  Increment to be applied to Coordinated Universal Time UTC to give
+*  International Atomic Time TAI (double precision)
+*
+*  Given:
+*     UTC      d      UTC date as a modified JD (JD-2400000.5)
+*
+*  Result:  TAI-UTC in seconds
+*
+*  Notes:
+*
+*  1  The UTC is specified to be a date rather than a time to indicate
+*     that care needs to be taken not to specify an instant which lies
+*     within a leap second.  Though in most cases UTC can include the
+*     fractional part, correct behaviour on the day of a leap second
+*     can only be guaranteed up to the end of the second 23:59:59.
+*
+*  2  For epochs from 1961 January 1 onwards, the expressions from the
+*     file ftp://maia.usno.navy.mil/ser7/tai-utc.dat are used.
+*
+*  3  The 5ms timestep at 1961 January 1 is taken from 2.58.1 (p87) of
+*     the 1992 Explanatory Supplement.
+*
+*  4  UTC began at 1960 January 1.0 (JD 2436934.5) and it is improper
+*     to call the routine with an earlier epoch.  However, if this
+*     is attempted, the TAI-UTC expression for the year 1960 is used.
+*
+*
+*     :-----------------------------------------:
+*     :                                         :
+*     :                IMPORTANT                :
+*     :                                         :
+*     :  This routine must be updated on each   :
+*     :     occasion that a leap second is      :
+*     :                announced                :
+*     :                                         :
+*     :  Latest leap second:  1999 January 1    :
+*     :                                         :
+*     :-----------------------------------------:
+*
+*  P.T.Wallace   Starlink   31 May 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION UTC
+
+      DOUBLE PRECISION DT
+
+
+
+      IF (.FALSE.) THEN
+
+* - - - - - - - - - - - - - - - - - - - - - - *
+*  Add new code here on each occasion that a  *
+*  leap second is announced, and update the   *
+*  preamble comments appropriately.           *
+* - - - - - - - - - - - - - - - - - - - - - - *
+
+*     1999 January 1
+      ELSE IF (UTC.GE.51179D0) THEN
+         DT=32D0
+
+*     1997 July 1
+      ELSE IF (UTC.GE.50630D0) THEN
+         DT=31D0
+
+*     1996 January 1
+      ELSE IF (UTC.GE.50083D0) THEN
+         DT=30D0
+
+*     1994 July 1
+      ELSE IF (UTC.GE.49534D0) THEN
+         DT=29D0
+
+*     1993 July 1
+      ELSE IF (UTC.GE.49169D0) THEN
+         DT=28D0
+
+*     1992 July 1
+      ELSE IF (UTC.GE.48804D0) THEN
+         DT=27D0
+
+*     1991 January 1
+      ELSE IF (UTC.GE.48257D0) THEN
+         DT=26D0
+
+*     1990 January 1
+      ELSE IF (UTC.GE.47892D0) THEN
+         DT=25D0
+
+*     1988 January 1
+      ELSE IF (UTC.GE.47161D0) THEN
+         DT=24D0
+
+*     1985 July 1
+      ELSE IF (UTC.GE.46247D0) THEN
+         DT=23D0
+
+*     1983 July 1
+      ELSE IF (UTC.GE.45516D0) THEN
+         DT=22D0
+
+*     1982 July 1
+      ELSE IF (UTC.GE.45151D0) THEN
+         DT=21D0
+
+*     1981 July 1
+      ELSE IF (UTC.GE.44786D0) THEN
+         DT=20D0
+
+*     1980 January 1
+      ELSE IF (UTC.GE.44239D0) THEN
+         DT=19D0
+
+*     1979 January 1
+      ELSE IF (UTC.GE.43874D0) THEN
+         DT=18D0
+
+*     1978 January 1
+      ELSE IF (UTC.GE.43509D0) THEN
+         DT=17D0
+
+*     1977 January 1
+      ELSE IF (UTC.GE.43144D0) THEN
+         DT=16D0
+
+*     1976 January 1
+      ELSE IF (UTC.GE.42778D0) THEN
+         DT=15D0
+
+*     1975 January 1
+      ELSE IF (UTC.GE.42413D0) THEN
+         DT=14D0
+
+*     1974 January 1
+      ELSE IF (UTC.GE.42048D0) THEN
+         DT=13D0
+
+*     1973 January 1
+      ELSE IF (UTC.GE.41683D0) THEN
+         DT=12D0
+
+*     1972 July 1
+      ELSE IF (UTC.GE.41499D0) THEN
+         DT=11D0
+
+*     1972 January 1
+      ELSE IF (UTC.GE.41317D0) THEN
+         DT=10D0
+
+*     1968 February 1
+      ELSE IF (UTC.GE.39887D0) THEN
+         DT=4.2131700D0+(UTC-39126D0)*0.002592D0
+
+*     1966 January 1
+      ELSE IF (UTC.GE.39126D0) THEN
+         DT=4.3131700D0+(UTC-39126D0)*0.002592D0
+
+*     1965 September 1
+      ELSE IF (UTC.GE.39004D0) THEN
+         DT=3.8401300D0+(UTC-38761D0)*0.001296D0
+
+*     1965 July 1
+      ELSE IF (UTC.GE.38942D0) THEN
+         DT=3.7401300D0+(UTC-38761D0)*0.001296D0
+
+*     1965 March 1
+      ELSE IF (UTC.GE.38820D0) THEN
+         DT=3.6401300D0+(UTC-38761D0)*0.001296D0
+
+*     1965 January 1
+      ELSE IF (UTC.GE.38761D0) THEN
+         DT=3.5401300D0+(UTC-38761D0)*0.001296D0
+
+*     1964 September 1
+      ELSE IF (UTC.GE.38639D0) THEN
+         DT=3.4401300D0+(UTC-38761D0)*0.001296D0
+
+*     1964 April 1
+      ELSE IF (UTC.GE.38486D0) THEN
+         DT=3.3401300D0+(UTC-38761D0)*0.001296D0
+
+*     1964 January 1
+      ELSE IF (UTC.GE.38395D0) THEN
+         DT=3.2401300D0+(UTC-38761D0)*0.001296D0
+
+*     1963 November 1
+      ELSE IF (UTC.GE.38334D0) THEN
+         DT=1.9458580D0+(UTC-37665D0)*0.0011232D0
+
+*     1962 January 1
+      ELSE IF (UTC.GE.37665D0) THEN
+         DT=1.8458580D0+(UTC-37665D0)*0.0011232D0
+
+*     1961 August 1
+      ELSE IF (UTC.GE.37512D0) THEN
+         DT=1.3728180D0+(UTC-37300D0)*0.001296D0
+
+*     1961 January 1
+      ELSE IF (UTC.GE.37300D0) THEN
+         DT=1.4228180D0+(UTC-37300D0)*0.001296D0
+
+*     Before that
+      ELSE
+         DT=1.4178180D0+(UTC-37300D0)*0.001296D0
+
+      END IF
+
+      sla_DAT=DT
+
+      END
diff --git a/src/slalib/dav2m.f b/src/slalib/dav2m.f
new file mode 100644
index 0000000..dc3f46c
--- /dev/null
+++ b/src/slalib/dav2m.f
@@ -0,0 +1,67 @@
+      SUBROUTINE sla_DAV2M (AXVEC, RMAT)
+*+
+*     - - - - - -
+*      D A V 2 M
+*     - - - - - -
+*
+*  Form the rotation matrix corresponding to a given axial vector.
+*  (double precision)
+*
+*  A rotation matrix describes a rotation about some arbitrary axis.
+*  The axis is called the Euler axis, and the angle through which the
+*  reference frame rotates is called the Euler angle.  The axial
+*  vector supplied to this routine has the same direction as the
+*  Euler axis, and its magnitude is the Euler angle in radians.
+*
+*  Given:
+*    AXVEC  d(3)     axial vector (radians)
+*
+*  Returned:
+*    RMAT   d(3,3)   rotation matrix
+*
+*  If AXVEC is null, the unit matrix is returned.
+*
+*  The reference frame rotates clockwise as seen looking along
+*  the axial vector from the origin.
+*
+*  P.T.Wallace   Starlink   June 1989
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION AXVEC(3),RMAT(3,3)
+
+      DOUBLE PRECISION X,Y,Z,PHI,S,C,W
+
+
+
+*  Euler angle - magnitude of axial vector - and functions
+      X = AXVEC(1)
+      Y = AXVEC(2)
+      Z = AXVEC(3)
+      PHI = SQRT(X*X+Y*Y+Z*Z)
+      S = SIN(PHI)
+      C = COS(PHI)
+      W = 1D0-C
+
+*  Euler axis - direction of axial vector (perhaps null)
+      IF (PHI.NE.0D0) THEN
+         X = X/PHI
+         Y = Y/PHI
+         Z = Z/PHI
+      END IF
+
+*  Compute the rotation matrix
+      RMAT(1,1) = X*X*W+C
+      RMAT(1,2) = X*Y*W+Z*S
+      RMAT(1,3) = X*Z*W-Y*S
+      RMAT(2,1) = X*Y*W-Z*S
+      RMAT(2,2) = Y*Y*W+C
+      RMAT(2,3) = Y*Z*W+X*S
+      RMAT(3,1) = X*Z*W+Y*S
+      RMAT(3,2) = Y*Z*W-X*S
+      RMAT(3,3) = Z*Z*W+C
+
+      END
diff --git a/src/slalib/dbear.f b/src/slalib/dbear.f
new file mode 100644
index 0000000..7cd5818
--- /dev/null
+++ b/src/slalib/dbear.f
@@ -0,0 +1,42 @@
+      DOUBLE PRECISION FUNCTION sla_DBEAR (A1, B1, A2, B2)
+*+
+*     - - - - - -
+*      D B E A R
+*     - - - - - -
+*
+*  Bearing (position angle) of one point on a sphere relative to another
+*  (double precision)
+*
+*  Given:
+*     A1,B1    d    spherical coordinates of one point
+*     A2,B2    d    spherical coordinates of the other point
+*
+*  (The spherical coordinates are RA,Dec, Long,Lat etc, in radians.)
+*
+*  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.
+*
+*  P.T.Wallace   Starlink   23 March 1991
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION A1,B1,A2,B2
+
+      DOUBLE PRECISION DA,X,Y
+
+
+      DA=A2-A1
+      Y=SIN(DA)*COS(B2)
+      X=SIN(B2)*COS(B1)-COS(B2)*SIN(B1)*COS(DA)
+      IF (X.NE.0D0.OR.Y.NE.0D0) THEN
+         sla_DBEAR=ATAN2(Y,X)
+      ELSE
+         sla_DBEAR=0D0
+      END IF
+
+      END
diff --git a/src/slalib/dbjin.f b/src/slalib/dbjin.f
new file mode 100644
index 0000000..60563e4
--- /dev/null
+++ b/src/slalib/dbjin.f
@@ -0,0 +1,113 @@
+      SUBROUTINE sla_DBJIN (STRING, NSTRT, DRESLT, J1, J2)
+*+
+*     - - - - - -
+*      D B J I N
+*     - - - - - -
+*
+*  Convert free-format input into double precision floating point,
+*  using DFLTIN but with special syntax extensions.
+*
+*  The purpose of the syntax extensions is to help cope with mixed
+*  FK4 and FK5 data.  In addition to the syntax accepted by DFLTIN,
+*  the following two extensions are recognized by DBJIN:
+*
+*     1)  A valid non-null field preceded by the character 'B'
+*         (or 'b') is accepted.
+*
+*     2)  A valid non-null field preceded by the character 'J'
+*         (or 'j') is accepted.
+*
+*  The calling program is notified of the incidence of either of these
+*  extensions through an supplementary status argument.  The rest of
+*  the arguments are as for DFLTIN.
+*
+*  Given:
+*     STRING      char       string containing field to be decoded
+*     NSTRT       int        pointer to 1st character of field in string
+*
+*  Returned:
+*     NSTRT       int        incremented
+*     DRESLT      double     result
+*     J1          int        DFLTIN status: -1 = -OK
+*                                            0 = +OK
+*                                           +1 = null field
+*                                           +2 = error
+*     J2          int        syntax flag:  0 = normal DFLTIN syntax
+*                                         +1 = 'B' or 'b'
+*                                         +2 = 'J' or 'j'
+*
+*  Called:  sla_DFLTIN
+*
+*  For details of the basic syntax, see sla_DFLTIN.
+*
+*  P.T.Wallace   Starlink   23 November 1995
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      CHARACTER*(*) STRING
+      INTEGER NSTRT
+      DOUBLE PRECISION DRESLT
+      INTEGER J1,J2
+
+      INTEGER J2A,LENSTR,NA,J1A,NB,J1B
+      CHARACTER C
+
+
+
+*   Preset syntax flag
+      J2A=0
+
+*   Length of string
+      LENSTR=LEN(STRING)
+
+*   Pointer to current character
+      NA=NSTRT
+
+*   Attempt normal decode
+      CALL sla_DFLTIN(STRING,NA,DRESLT,J1A)
+
+*   Proceed only if pointer still within string
+      IF (NA.GE.1.AND.NA.LE.LENSTR) THEN
+
+*      See if DFLTIN reported a null field
+         IF (J1A.EQ.1) THEN
+
+*         It did: examine character it stuck on
+            C=STRING(NA:NA)
+            IF (C.EQ.'B'.OR.C.EQ.'b') THEN
+*            'B' - provisionally note
+               J2A=1
+            ELSE IF (C.EQ.'J'.OR.C.EQ.'j') THEN
+*            'J' - provisionally note
+               J2A=2
+            END IF
+
+*         Following B or J, attempt to decode a number
+            IF (J2A.EQ.1.OR.J2A.EQ.2) THEN
+               NB=NA+1
+               CALL sla_DFLTIN(STRING,NB,DRESLT,J1B)
+
+*            If successful, copy pointer and status
+               IF (J1B.LE.0) THEN
+                  NA=NB
+                  J1A=J1B
+*            If not, forget about the B or J
+               ELSE
+                  J2A=0
+               END IF
+
+            END IF
+
+         END IF
+
+      END IF
+
+*   Return argument values and exit
+      NSTRT=NA
+      J1=J1A
+      J2=J2A
+
+      END
diff --git a/src/slalib/dc62s.f b/src/slalib/dc62s.f
new file mode 100644
index 0000000..2dd63ba
--- /dev/null
+++ b/src/slalib/dc62s.f
@@ -0,0 +1,82 @@
+      SUBROUTINE sla_DC62S (V, A, B, R, AD, BD, RD)
+*+
+*     - - - - - -
+*      D C 6 2 S
+*     - - - - - -
+*
+*  Conversion of position & velocity in Cartesian coordinates
+*  to spherical coordinates (double precision)
+*
+*  Given:
+*     V      d(6)   Cartesian position & velocity vector
+*
+*  Returned:
+*     A      d      longitude (radians)
+*     B      d      latitude (radians)
+*     R      d      radial coordinate
+*     AD     d      longitude derivative (radians per unit time)
+*     BD     d      latitude derivative (radians per unit time)
+*     RD     d      radial derivative
+*
+*  P.T.Wallace   Starlink   28 April 1996
+*
+*  Copyright (C) 1996 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION V(6),A,B,R,AD,BD,RD
+
+      DOUBLE PRECISION X,Y,Z,XD,YD,ZD,RXY2,RXY,R2,XYP
+
+
+
+*  Components of position/velocity vector
+      X=V(1)
+      Y=V(2)
+      Z=V(3)
+      XD=V(4)
+      YD=V(5)
+      ZD=V(6)
+
+*  Component of R in XY plane squared
+      RXY2=X*X+Y*Y
+
+*  Modulus squared
+      R2=RXY2+Z*Z
+
+*  Protection against null vector
+      IF (R2.EQ.0D0) THEN
+         X=XD
+         Y=YD
+         Z=ZD
+         RXY2=X*X+Y*Y
+         R2=RXY2+Z*Z
+      END IF
+
+*  Position and velocity in spherical coordinates
+      RXY=SQRT(RXY2)
+      XYP=X*XD+Y*YD
+      IF (RXY2.NE.0D0) THEN
+         A=ATAN2(Y,X)
+         B=ATAN2(Z,RXY)
+         AD=(X*YD-Y*XD)/RXY2
+         BD=(ZD*RXY2-Z*XYP)/(R2*RXY)
+      ELSE
+         A=0D0
+         IF (Z.NE.0D0) THEN
+            B=ATAN2(Z,RXY)
+         ELSE
+            B=0D0
+         END IF
+         AD=0D0
+         BD=0D0
+      END IF
+      R=SQRT(R2)
+      IF (R.NE.0D0) THEN
+         RD=(XYP+Z*ZD)/R
+      ELSE
+         RD=0D0
+      END IF
+
+      END
diff --git a/src/slalib/dcc2s.f b/src/slalib/dcc2s.f
new file mode 100644
index 0000000..9f5d0fe
--- /dev/null
+++ b/src/slalib/dcc2s.f
@@ -0,0 +1,53 @@
+      SUBROUTINE sla_DCC2S (V, A, B)
+*+
+*     - - - - - -
+*      D C C 2 S
+*     - - - - - -
+*
+*  Direction cosines to spherical coordinates (double precision)
+*
+*  Given:
+*     V     d(3)   x,y,z vector
+*
+*  Returned:
+*     A,B   d      spherical coordinates in radians
+*
+*  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.
+*
+*  If V is null, zero A and B are returned.
+*  At either pole, zero A is returned.
+*
+*  P.T.Wallace   Starlink   July 1989
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION V(3),A,B
+
+      DOUBLE PRECISION X,Y,Z,R
+
+
+      X = V(1)
+      Y = V(2)
+      Z = V(3)
+      R = SQRT(X*X+Y*Y)
+
+      IF (R.EQ.0D0) THEN
+         A = 0D0
+      ELSE
+         A = ATAN2(Y,X)
+      END IF
+
+      IF (Z.EQ.0D0) THEN
+         B = 0D0
+      ELSE
+         B = ATAN2(Z,R)
+      END IF
+
+      END
diff --git a/src/slalib/dcmpf.f b/src/slalib/dcmpf.f
new file mode 100644
index 0000000..3689e25
--- /dev/null
+++ b/src/slalib/dcmpf.f
@@ -0,0 +1,140 @@
+      SUBROUTINE sla_DCMPF (COEFFS,XZ,YZ,XS,YS,PERP,ORIENT)
+*+
+*     - - - - - -
+*      D C M P F
+*     - - - - - -
+*
+*  Decompose an [X,Y] linear fit into its constituent parameters:
+*  zero points, scales, nonperpendicularity and orientation.
+*
+*  Given:
+*     COEFFS  d(6)      transformation coefficients (see note)
+*
+*  Returned:
+*     XZ       d        x zero point
+*     YZ       d        y zero point
+*     XS       d        x scale
+*     YS       d        y scale
+*     PERP     d        nonperpendicularity (radians)
+*     ORIENT   d        orientation (radians)
+*
+*  The model relates two sets of [X,Y] coordinates as follows.
+*  Naming the elements of COEFFS:
+*
+*     COEFFS(1) = A
+*     COEFFS(2) = B
+*     COEFFS(3) = C
+*     COEFFS(4) = D
+*     COEFFS(5) = E
+*     COEFFS(6) = F
+*
+*  the model transforms coordinates [X1,Y1] into coordinates
+*  [X2,Y2] as follows:
+*
+*     X2 = A + B*X1 + C*Y1
+*     Y2 = D + E*X1 + F*Y1
+*
+*  The transformation can be decomposed into four steps:
+*
+*     1)  Zero points:
+*
+*             x' = XZ + X1
+*             y' = YZ + Y1
+*
+*     2)  Scales:
+*
+*             x'' = XS*x'
+*             y'' = YS*y'
+*
+*     3)  Nonperpendicularity:
+*
+*             x''' = cos(PERP/2)*x'' + sin(PERP/2)*y''
+*             y''' = sin(PERP/2)*x'' + cos(PERP/2)*y''
+*
+*     4)  Orientation:
+*
+*             X2 = cos(ORIENT)*x''' + sin(ORIENT)*y'''
+*             Y2 =-sin(ORIENT)*y''' + cos(ORIENT)*y'''
+*
+*  See also sla_FITXY, sla_PXY, sla_INVF, sla_XY2XY
+*
+*  P.T.Wallace   Starlink   14 August 1994
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION COEFFS(6),XZ,YZ,XS,YS,PERP,ORIENT
+
+      DOUBLE PRECISION A,B,C,D,E,F,RB2E2,RC2F2,XSC,YSC,P1,P2,P,WS,WC,
+     :                 OR,HP,SHP,CHP,SOR,COR,DET,X0,Y0
+
+
+
+*  Copy the six coefficients
+      A=COEFFS(1)
+      B=COEFFS(2)
+      C=COEFFS(3)
+      D=COEFFS(4)
+      E=COEFFS(5)
+      F=COEFFS(6)
+
+*  Scales
+      RB2E2=SQRT(B*B+E*E)
+      RC2F2=SQRT(C*C+F*F)
+      IF (B*F-C*E.GE.0D0) THEN
+         XSC=RB2E2
+      ELSE
+         B=-B
+         C=-C
+         XSC=-RB2E2
+      END IF
+      YSC=RC2F2
+
+*  Non-perpendicularity
+      IF (C.NE.0D0.OR.F.NE.0D0) THEN
+         P1=ATAN2(C,F)
+      ELSE
+         P1=0D0
+      END IF
+      IF (E.NE.0D0.OR.B.NE.0D0) THEN
+         P2=ATAN2(E,B)
+      ELSE
+         P2=0D0
+      END IF
+      P=P1+P2
+
+*  Orientation
+      WS=C*RB2E2-E*RC2F2
+      WC=B*RC2F2+F*RB2E2
+      IF (WS.NE.0D0.OR.WC.NE.0D0) THEN
+         OR=ATAN2(WS,WC)
+      ELSE
+         OR=0D0
+      END IF
+
+*  Zero corrections
+      HP=P/2D0
+      SHP=SIN(HP)
+      CHP=COS(HP)
+      SOR=SIN(OR)
+      COR=COS(OR)
+      DET=XSC*YSC*(CHP+SHP)*(CHP-SHP)
+      IF (ABS(DET).GT.0D0) THEN
+         X0=YSC*(A*(CHP*COR-SHP*SOR)-D*(CHP*SOR+SHP*COR))/DET
+         Y0=XSC*(A*(CHP*SOR-SHP*COR)+D*(CHP*COR+SHP*SOR))/DET
+      ELSE
+         X0=0D0
+         Y0=0D0
+      END IF
+
+*  Results
+      XZ=X0
+      YZ=Y0
+      XS=XSC
+      YS=YSC
+      PERP=P
+      ORIENT=OR
+
+      END
diff --git a/src/slalib/dcs2c.f b/src/slalib/dcs2c.f
new file mode 100644
index 0000000..5c20009
--- /dev/null
+++ b/src/slalib/dcs2c.f
@@ -0,0 +1,41 @@
+      SUBROUTINE sla_DCS2C (A, B, V)
+*+
+*     - - - - - -
+*      D C S 2 C
+*     - - - - - -
+*
+*  Spherical coordinates to direction cosines (double precision)
+*
+*  Given:
+*     A,B       dp      spherical coordinates in radians
+*                        (RA,Dec), (Long,Lat) etc
+*
+*  Returned:
+*     V         dp(3)   x,y,z unit vector
+*
+*  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.
+*
+*  P.T.Wallace   Starlink   October 1984
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION A,B,V(3)
+
+      DOUBLE PRECISION COSB
+
+
+
+      COSB=COS(B)
+
+      V(1)=COS(A)*COSB
+      V(2)=SIN(A)*COSB
+      V(3)=SIN(B)
+
+      END
diff --git a/src/slalib/dd2tf.f b/src/slalib/dd2tf.f
new file mode 100644
index 0000000..2fc0db6
--- /dev/null
+++ b/src/slalib/dd2tf.f
@@ -0,0 +1,89 @@
+      SUBROUTINE sla_DD2TF (NDP, DAYS, SIGN, IHMSF)
+*+
+*     - - - - - -
+*      D D 2 T F
+*     - - - - - -
+*
+*  Convert an interval in days into hours, minutes, seconds
+*  (double precision)
+*
+*  Given:
+*     NDP      i      number of decimal places of seconds
+*     DAYS     d      interval in days
+*
+*  Returned:
+*     SIGN     c      '+' or '-'
+*     IHMSF    i(4)   hours, minutes, seconds, fraction
+*
+*  Notes:
+*
+*     1)  NDP less than zero is interpreted as zero.
+*
+*     2)  The largest useful value for NDP is determined by the size
+*         of DAYS, the format of DOUBLE PRECISION floating-point numbers
+*         on the target machine, and the risk of overflowing IHMSF(4).
+*         For example, on the VAX, for DAYS up to 1D0, the available
+*         floating-point precision corresponds roughly to NDP=12.
+*         However, the practical limit is NDP=9, set by the capacity of
+*         the 32-bit integer IHMSF(4).
+*
+*     3)  The absolute value of DAYS may exceed 1D0.  In cases where it
+*         does not, it is up to the caller to test for and handle the
+*         case where DAYS is very nearly 1D0 and rounds up to 24 hours,
+*         by testing for IHMSF(1)=24 and setting IHMSF(1-4) to zero.
+*
+*  P.T.Wallace   Starlink   19 March 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER NDP
+      DOUBLE PRECISION DAYS
+      CHARACTER SIGN*(*)
+      INTEGER IHMSF(4)
+
+*  Days to seconds
+      DOUBLE PRECISION D2S
+      PARAMETER (D2S=86400D0)
+
+      INTEGER NRS,N
+      DOUBLE PRECISION RS,RM,RH,A,AH,AM,AS,AF
+
+
+
+*  Handle sign
+      IF (DAYS.GE.0D0) THEN
+         SIGN='+'
+      ELSE
+         SIGN='-'
+      END IF
+
+*  Field units in terms of least significant figure
+      NRS=1
+      DO N=1,NDP
+         NRS=NRS*10
+      END DO
+      RS=DBLE(NRS)
+      RM=RS*60D0
+      RH=RM*60D0
+
+*  Round interval and express in smallest units required
+      A=ANINT(RS*D2S*ABS(DAYS))
+
+*  Separate into fields
+      AH=AINT(A/RH)
+      A=A-AH*RH
+      AM=AINT(A/RM)
+      A=A-AM*RM
+      AS=AINT(A/RS)
+      AF=A-AS*RS
+
+*  Return results
+      IHMSF(1)=MAX(NINT(AH),0)
+      IHMSF(2)=MAX(MIN(NINT(AM),59),0)
+      IHMSF(3)=MAX(MIN(NINT(AS),59),0)
+      IHMSF(4)=MAX(NINT(MIN(AF,RS-1D0)),0)
+
+      END
diff --git a/src/slalib/de2h.f b/src/slalib/de2h.f
new file mode 100644
index 0000000..138a3f7
--- /dev/null
+++ b/src/slalib/de2h.f
@@ -0,0 +1,89 @@
+      SUBROUTINE sla_DE2H (HA, DEC, PHI, AZ, EL)
+*+
+*     - - - - -
+*      D E 2 H
+*     - - - - -
+*
+*  Equatorial to horizon coordinates:  HA,Dec to Az,El
+*
+*  (double precision)
+*
+*  Given:
+*     HA      d     hour angle
+*     DEC     d     declination
+*     PHI     d     observatory latitude
+*
+*  Returned:
+*     AZ      d     azimuth
+*     EL      d     elevation
+*
+*  Notes:
+*
+*  1)  All the arguments are angles in radians.
+*
+*  2)  Azimuth is returned in the range 0-2pi;  north is zero,
+*      and east is +pi/2.  Elevation is returned in the range
+*      +/-pi/2.
+*
+*  3)  The latitude must be geodetic.  In critical applications,
+*      corrections for polar motion should be applied.
+*
+*  4)  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.
+*
+*  5)  No range checking of arguments is carried out.
+*
+*  6)  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.
+*
+*  P.T.Wallace   Starlink   9 July 1994
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION HA,DEC,PHI,AZ,EL
+
+      DOUBLE PRECISION D2PI
+      PARAMETER (D2PI=6.283185307179586476925286766559D0)
+
+      DOUBLE PRECISION SH,CH,SD,CD,SP,CP,X,Y,Z,R,A
+
+
+*  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.EQ.0D0) THEN
+         A=0D0
+      ELSE
+         A=ATAN2(Y,X)
+      END IF
+      IF (A.LT.0D0) A=A+D2PI
+      AZ=A
+      EL=ATAN2(Z,R)
+
+      END
diff --git a/src/slalib/deuler.f b/src/slalib/deuler.f
new file mode 100644
index 0000000..6ce1479
--- /dev/null
+++ b/src/slalib/deuler.f
@@ -0,0 +1,163 @@
+      SUBROUTINE sla_DEULER (ORDER, PHI, THETA, PSI, RMAT)
+*+
+*     - - - - - - -
+*      D E U L E R
+*     - - - - - - -
+*
+*  Form a rotation matrix from the Euler angles - three successive
+*  rotations about specified Cartesian axes (double precision)
+*
+*  Given:
+*    ORDER   c*(*)   specifies about which axes the rotations occur
+*    PHI     d       1st rotation (radians)
+*    THETA   d       2nd rotation (   "   )
+*    PSI     d       3rd rotation (   "   )
+*
+*  Returned:
+*    RMAT    d(3,3)  rotation matrix
+*
+*  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.
+*
+*  P.T.Wallace   Starlink   23 May 1997
+*
+*  Copyright (C) 1997 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      CHARACTER*(*) ORDER
+      DOUBLE PRECISION PHI,THETA,PSI,RMAT(3,3)
+
+      INTEGER J,I,L,N,K
+      DOUBLE PRECISION RESULT(3,3),ROTN(3,3),ANGLE,S,C,W,WM(3,3)
+      CHARACTER AXIS
+
+
+
+*  Initialize result matrix
+      DO J=1,3
+         DO I=1,3
+            IF (I.NE.J) THEN
+               RESULT(I,J) = 0D0
+            ELSE
+               RESULT(I,J) = 1D0
+            END IF
+         END DO
+      END DO
+
+*  Establish length of axis string
+      L = LEN(ORDER)
+
+*  Look at each character of axis string until finished
+      DO N=1,3
+         IF (N.LE.L) THEN
+
+*        Initialize rotation matrix for the current rotation
+            DO J=1,3
+               DO I=1,3
+                  IF (I.NE.J) THEN
+                     ROTN(I,J) = 0D0
+                  ELSE
+                     ROTN(I,J) = 1D0
+                  END IF
+               END DO
+            END DO
+
+*        Pick up the appropriate Euler angle and take sine & cosine
+            IF (N.EQ.1) THEN
+               ANGLE = PHI
+            ELSE IF (N.EQ.2) THEN
+               ANGLE = THETA
+            ELSE
+               ANGLE = PSI
+            END IF
+            S = SIN(ANGLE)
+            C = COS(ANGLE)
+
+*        Identify the axis
+            AXIS = ORDER(N:N)
+            IF (AXIS.EQ.'X'.OR.
+     :          AXIS.EQ.'x'.OR.
+     :          AXIS.EQ.'1') THEN
+
+*           Matrix for x-rotation
+               ROTN(2,2) = C
+               ROTN(2,3) = S
+               ROTN(3,2) = -S
+               ROTN(3,3) = C
+
+            ELSE IF (AXIS.EQ.'Y'.OR.
+     :               AXIS.EQ.'y'.OR.
+     :               AXIS.EQ.'2') THEN
+
+*           Matrix for y-rotation
+               ROTN(1,1) = C
+               ROTN(1,3) = -S
+               ROTN(3,1) = S
+               ROTN(3,3) = C
+
+            ELSE IF (AXIS.EQ.'Z'.OR.
+     :               AXIS.EQ.'z'.OR.
+     :               AXIS.EQ.'3') THEN
+
+*           Matrix for z-rotation
+               ROTN(1,1) = C
+               ROTN(1,2) = S
+               ROTN(2,1) = -S
+               ROTN(2,2) = C
+
+            ELSE
+
+*           Unrecognized character - fake end of string
+               L = 0
+
+            END IF
+
+*        Apply the current rotation (matrix ROTN x matrix RESULT)
+            DO I=1,3
+               DO J=1,3
+                  W = 0D0
+                  DO K=1,3
+                     W = W+ROTN(I,K)*RESULT(K,J)
+                  END DO
+                  WM(I,J) = W
+               END DO
+            END DO
+            DO J=1,3
+               DO I=1,3
+                  RESULT(I,J) = WM(I,J)
+               END DO
+            END DO
+
+         END IF
+
+      END DO
+
+*  Copy the result
+      DO J=1,3
+         DO I=1,3
+            RMAT(I,J) = RESULT(I,J)
+         END DO
+      END DO
+
+      END
diff --git a/src/slalib/dfltin.f b/src/slalib/dfltin.f
new file mode 100644
index 0000000..1fbdb94
--- /dev/null
+++ b/src/slalib/dfltin.f
@@ -0,0 +1,280 @@
+      SUBROUTINE sla_DFLTIN (STRING, NSTRT, DRESLT, JFLAG)
+*+
+*     - - - - - - -
+*      D F L T I N
+*     - - - - - - -
+*
+*  Convert free-format input into double precision floating point
+*
+*  Given:
+*     STRING     c     string containing number to be decoded
+*     NSTRT      i     pointer to where decoding is to start
+*     DRESLT     d     current value of result
+*
+*  Returned:
+*     NSTRT      i      advanced to next number
+*     DRESLT     d      result
+*     JFLAG      i      status: -1 = -OK, 0 = +OK, 1 = null, 2 = error
+*
+*  Notes:
+*
+*     1     The reason DFLTIN has separate OK status values for +
+*           and - is to enable minus zero to be detected.   This is
+*           of crucial importance when decoding mixed-radix numbers.
+*           For example, an angle expressed as deg, arcmin, arcsec
+*           may have a leading minus sign but a zero degrees field.
+*
+*     2     A TAB is interpreted as a space, and lowercase characters
+*           are interpreted as uppercase.
+*
+*     3     The basic format is the sequence of fields #^.^@#^, where
+*           # is a sign character + or -, ^ means a string of decimal
+*           digits, and @, which indicates an exponent, means D or E.
+*           Various combinations of these fields can be omitted, and
+*           embedded blanks are permissible in certain places.
+*
+*     4     Spaces:
+*
+*             .  Leading spaces are ignored.
+*
+*             .  Embedded spaces are allowed only after +, -, D or E,
+*                and after the decomal point if the first sequence of
+*                digits is absent.
+*
+*             .  Trailing spaces are ignored;  the first signifies
+*                end of decoding and subsequent ones are skipped.
+*
+*     5     Delimiters:
+*
+*             .  Any character other than +,-,0-9,.,D,E or space may be
+*                used to signal the end of the number and terminate
+*                decoding.
+*
+*             .  Comma is recognized by DFLTIN as a special case;  it
+*                is skipped, leaving the pointer on the next character.
+*                See 13, below.
+*
+*     6     Both signs are optional.  The default is +.
+*
+*     7     The mantissa ^.^ defaults to 1.
+*
+*     8     The exponent @#^ defaults to D0.
+*
+*     9     The strings of decimal digits may be of any length.
+*
+*     10    The decimal point is optional for whole numbers.
+*
+*     11    A "null result" occurs when the string of characters being
+*           decoded does not begin with +,-,0-9,.,D or E, or consists
+*           entirely of spaces.  When this condition is detected, JFLAG
+*           is set to 1 and DRESLT is left untouched.
+*
+*     12    NSTRT = 1 for the first character in the string.
+*
+*     13    On return from DFLTIN, NSTRT is set ready for the next
+*           decode - following trailing blanks and any comma.  If a
+*           delimiter other than comma is being used, NSTRT must be
+*           incremented before the next call to DFLTIN, otherwise
+*           all subsequent calls will return a null result.
+*
+*     14    Errors (JFLAG=2) occur when:
+*
+*             .  a +, -, D or E is left unsatisfied;  or
+*
+*             .  the decimal point is present without at least
+*                one decimal digit before or after it;  or
+*
+*             .  an exponent more than 100 has been presented.
+*
+*     15    When an error has been detected, NSTRT is left
+*           pointing to the character following the last
+*           one used before the error came to light.  This
+*           may be after the point at which a more sophisticated
+*           program could have detected the error.  For example,
+*           DFLTIN does not detect that '1D999' is unacceptable
+*           (on a computer where this is so) until the entire number
+*           has been decoded.
+*
+*     16    Certain highly unlikely combinations of mantissa &
+*           exponent can cause arithmetic faults during the
+*           decode, in some cases despite the fact that they
+*           together could be construed as a valid number.
+*
+*     17    Decoding is left to right, one pass.
+*
+*     18    See also FLOTIN and INTIN
+*
+*  Called:  sla__IDCHF
+*
+*  P.T.Wallace   Starlink   18 March 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      CHARACTER*(*) STRING
+      INTEGER NSTRT
+      DOUBLE PRECISION DRESLT
+      INTEGER JFLAG
+
+      INTEGER NPTR,MSIGN,NEXP,NDP,NVEC,NDIGIT,ISIGNX,J
+      DOUBLE PRECISION DMANT,DIGIT
+
+
+
+*  Current character
+      NPTR=NSTRT
+
+*  Set defaults: mantissa & sign, exponent & sign, decimal place count
+      DMANT=0D0
+      MSIGN=1
+      NEXP=0
+      ISIGNX=1
+      NDP=0
+
+*  Look for sign
+ 100  CONTINUE
+      CALL sla__IDCHF(STRING,NPTR,NVEC,NDIGIT,DIGIT)
+      GO TO ( 400,  100,  800,  500,  300,  200, 9110, 9100, 9110),NVEC
+*             0-9    SP   D/E    .     +     -     ,   ELSE   END
+
+*  Negative
+ 200  CONTINUE
+      MSIGN=-1
+
+*  Look for first leading decimal
+ 300  CONTINUE
+      CALL sla__IDCHF(STRING,NPTR,NVEC,NDIGIT,DIGIT)
+      GO TO ( 400, 300,  800,  500, 9200, 9200, 9200, 9200, 9210),NVEC
+*             0-9   SP   D/E    .     +     -     ,   ELSE   END
+
+*  Accept leading decimals
+ 400  CONTINUE
+      DMANT=DMANT*1D1+DIGIT
+      CALL sla__IDCHF(STRING,NPTR,NVEC,NDIGIT,DIGIT)
+      GO TO ( 400, 1310,  900,  600, 1300, 1300, 1300, 1300, 1310),NVEC
+*             0-9   SP    D/E    .     +     -     ,   ELSE   END
+
+*  Look for decimal when none preceded the point
+ 500  CONTINUE
+      CALL sla__IDCHF(STRING,NPTR,NVEC,NDIGIT,DIGIT)
+      GO TO ( 700, 500, 9200, 9200, 9200, 9200, 9200, 9200, 9210),NVEC
+*             0-9   SP   D/E    .     +     -     ,   ELSE   END
+
+*  Look for trailing decimals
+ 600  CONTINUE
+      CALL sla__IDCHF(STRING,NPTR,NVEC,NDIGIT,DIGIT)
+      GO TO ( 700, 1310,  900, 1300, 1300, 1300, 1300, 1300, 1310),NVEC
+*             0-9   SP    D/E    .     +     -     ,   ELSE   END
+
+*  Accept trailing decimals
+ 700  CONTINUE
+      NDP=NDP+1
+      DMANT=DMANT*1D1+DIGIT
+      GO TO 600
+
+*  Exponent symbol first in field: default mantissa to 1
+ 800  CONTINUE
+      DMANT=1D0
+
+*  Look for sign of exponent
+ 900  CONTINUE
+      CALL sla__IDCHF(STRING,NPTR,NVEC,NDIGIT,DIGIT)
+      GO TO (1200, 900, 9200, 9200, 1100, 1000, 9200, 9200, 9210),NVEC
+*             0-9   SP   D/E    .     +     -     ,   ELSE   END
+
+*  Exponent negative
+ 1000 CONTINUE
+      ISIGNX=-1
+
+*  Look for first digit of exponent
+ 1100 CONTINUE
+      CALL sla__IDCHF(STRING,NPTR,NVEC,NDIGIT,DIGIT)
+      GO TO (1200, 1100, 9200, 9200, 9200, 9200, 9200, 9200, 9210),NVEC
+*             0-9   SP    D/E    .     +     -     ,   ELSE   END
+
+*  Use exponent digit
+ 1200 CONTINUE
+      NEXP=NEXP*10+NDIGIT
+      IF (NEXP.GT.100) GO TO 9200
+
+*  Look for subsequent digits of exponent
+      CALL sla__IDCHF(STRING,NPTR,NVEC,NDIGIT,DIGIT)
+      GO TO (1200, 1310, 1300, 1300, 1300, 1300, 1300, 1300, 1310),NVEC
+*             0-9   SP    D/E    .     +     -     ,   ELSE   END
+
+*  Combine exponent and decimal place count
+ 1300 CONTINUE
+      NPTR=NPTR-1
+ 1310 CONTINUE
+      NEXP=NEXP*ISIGNX-NDP
+
+*  Skip if net exponent negative
+      IF (NEXP.LT.0) GO TO 1500
+
+*  Positive exponent: scale up
+ 1400 CONTINUE
+      IF (NEXP.LT.10) GO TO 1410
+      DMANT=DMANT*1D10
+      NEXP=NEXP-10
+      GO TO 1400
+ 1410 CONTINUE
+      IF (NEXP.LT.1) GO TO 1600
+      DMANT=DMANT*1D1
+      NEXP=NEXP-1
+      GO TO 1410
+
+*  Negative exponent: scale down
+ 1500 CONTINUE
+      IF (NEXP.GT.-10) GO TO 1510
+      DMANT=DMANT/1D10
+      NEXP=NEXP+10
+      GO TO 1500
+ 1510 CONTINUE
+      IF (NEXP.GT.-1) GO TO 1600
+      DMANT=DMANT/1D1
+      NEXP=NEXP+1
+      GO TO 1510
+
+*  Get result & status
+ 1600 CONTINUE
+      J=0
+      IF (MSIGN.EQ.1) GO TO 1610
+      J=-1
+      DMANT=-DMANT
+ 1610 CONTINUE
+      DRESLT=DMANT
+
+*  Skip to end of field
+ 1620 CONTINUE
+      CALL sla__IDCHF(STRING,NPTR,NVEC,NDIGIT,DIGIT)
+      GO TO (1720, 1620, 1720, 1720, 1720, 1720, 9900, 1720, 9900),NVEC
+*             0-9   SP    D/E    .     +     -     ,   ELSE   END
+
+ 1720 CONTINUE
+      NPTR=NPTR-1
+      GO TO 9900
+
+
+*  Exits
+
+*  Null field
+ 9100 CONTINUE
+      NPTR=NPTR-1
+ 9110 CONTINUE
+      J=1
+      GO TO 9900
+
+*  Errors
+ 9200 CONTINUE
+      NPTR=NPTR-1
+ 9210 CONTINUE
+      J=2
+
+*  Return
+ 9900 CONTINUE
+      NSTRT=NPTR
+      JFLAG=J
+
+      END
diff --git a/src/slalib/dh2e.f b/src/slalib/dh2e.f
new file mode 100644
index 0000000..688a087
--- /dev/null
+++ b/src/slalib/dh2e.f
@@ -0,0 +1,83 @@
+      SUBROUTINE sla_DH2E (AZ, EL, PHI, HA, DEC)
+*+
+*     - - - - -
+*      D E 2 H
+*     - - - - -
+*
+*  Horizon to equatorial coordinates:  Az,El to HA,Dec
+*
+*  (double precision)
+*
+*  Given:
+*     AZ      d     azimuth
+*     EL      d     elevation
+*     PHI     d     observatory latitude
+*
+*  Returned:
+*     HA      d     hour angle
+*     DEC     d     declination
+*
+*  Notes:
+*
+*  1)  All the arguments are angles in radians.
+*
+*  2)  The sign convention for azimuth is north zero, east +pi/2.
+*
+*  3)  HA is returned in the range +/-pi.  Declination is returned
+*      in the range +/-pi/2.
+*
+*  4)  The latitude is (in principle) geodetic.  In critical
+*      applications, corrections for polar motion should be applied.
+*
+*  5)  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.
+*
+*  6)  No range checking of arguments is done.
+*
+*  7)  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.
+*
+*  P.T.Wallace   Starlink   21 February 1996
+*
+*  Copyright (C) 1996 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION AZ,EL,PHI,HA,DEC
+
+      DOUBLE PRECISION SA,CA,SE,CE,SP,CP,X,Y,Z,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.EQ.0D0) THEN
+         HA=0D0
+      ELSE
+         HA=ATAN2(Y,X)
+      END IF
+      DEC=ATAN2(Z,R)
+
+      END
diff --git a/src/slalib/dimxv.f b/src/slalib/dimxv.f
new file mode 100644
index 0000000..3da8fad
--- /dev/null
+++ b/src/slalib/dimxv.f
@@ -0,0 +1,51 @@
+      SUBROUTINE sla_DIMXV (DM, VA, VB)
+*+
+*     - - - - - -
+*      D I M X V
+*     - - - - - -
+*
+*  Performs the 3-D backward unitary transformation:
+*
+*     vector VB = (inverse of matrix DM) * vector VA
+*
+*  (double precision)
+*
+*  (n.b.  the matrix must be unitary, as this routine assumes that
+*   the inverse and transpose are identical)
+*
+*  Given:
+*     DM       dp(3,3)    matrix
+*     VA       dp(3)      vector
+*
+*  Returned:
+*     VB       dp(3)      result vector
+*
+*  P.T.Wallace   Starlink   March 1986
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DM(3,3),VA(3),VB(3)
+
+      INTEGER I,J
+      DOUBLE PRECISION W,VW(3)
+
+
+
+*  Inverse of matrix DM * vector VA -> vector VW
+      DO J=1,3
+         W=0D0
+         DO I=1,3
+            W=W+DM(I,J)*VA(I)
+         END DO
+         VW(J)=W
+      END DO
+
+*  Vector VW -> vector VB
+      DO J=1,3
+         VB(J)=VW(J)
+      END DO
+
+      END
diff --git a/src/slalib/djcal.f b/src/slalib/djcal.f
new file mode 100644
index 0000000..7da1a07
--- /dev/null
+++ b/src/slalib/djcal.f
@@ -0,0 +1,77 @@
+      SUBROUTINE sla_DJCAL (NDP, DJM, IYMDF, J)
+*+
+*     - - - - - -
+*      D J C A L
+*     - - - - - -
+*
+*  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)
+*
+*  Given:
+*     NDP      i      number of decimal places of days in fraction
+*     DJM      d      modified Julian Date (JD-2400000.5)
+*
+*  Returned:
+*     IYMDF    i(4)   year, month, day, fraction in Gregorian
+*                     calendar
+*     J        i      status:  nonzero = out of range
+*
+*  Any date after 4701BC March 1 is accepted.
+*
+*  NDP should be 4 or less if internal overflows are to be avoided
+*  on machines which use 32-bit integers.
+*
+*  The algorithm is derived from that of Hatcher 1984
+*  (QJRAS 25, 53-55).
+*
+*  P.T.Wallace   Starlink   27 April 1998
+*
+*  Copyright (C) 1998 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER NDP
+      DOUBLE PRECISION DJM
+      INTEGER IYMDF(4),J
+
+      INTEGER NFD
+      DOUBLE PRECISION FD,DF,F,D
+      INTEGER JD,N4,ND10
+
+
+
+*  Validate
+      IF (DJM.LE.-2395520D0.OR.DJM.GE.1D9) THEN
+         J=-1
+      ELSE
+         J=0
+
+*     Denominator of fraction
+         NFD=10**MAX(NDP,0)
+         FD=DBLE(NFD)
+
+*     Round date and express in units of fraction
+         DF=ANINT(DJM*FD)
+
+*     Separate day and fraction
+         F=MOD(DF,FD)
+         IF (F.LT.0D0) F=F+FD
+         D=(DF-F)/FD
+
+*     Express day in Gregorian calendar
+         JD=NINT(D)+2400001
+
+         N4=4*(JD+((2*((4*JD-17918)/146097)*3)/4+1)/2-37)
+         ND10=10*(MOD(N4-237,1461)/4)+5
+
+         IYMDF(1)=N4/1461-4712
+         IYMDF(2)=MOD(ND10/306+2,12)+1
+         IYMDF(3)=MOD(ND10,306)/10+1
+         IYMDF(4)=NINT(F)
+
+      END IF
+
+      END
diff --git a/src/slalib/djcl.f b/src/slalib/djcl.f
new file mode 100644
index 0000000..add7a48
--- /dev/null
+++ b/src/slalib/djcl.f
@@ -0,0 +1,68 @@
+      SUBROUTINE sla_DJCL (DJM, IY, IM, ID, FD, J)
+*+
+*     - - - - -
+*      D J C L
+*     - - - - -
+*
+*  Modified Julian Date to Gregorian year, month, day,
+*  and fraction of a day.
+*
+*  Given:
+*     DJM      dp     modified Julian Date (JD-2400000.5)
+*
+*  Returned:
+*     IY       int    year
+*     IM       int    month
+*     ID       int    day
+*     FD       dp     fraction of day
+*     J        int    status:
+*                       0 = OK
+*                      -1 = unacceptable date (before 4701BC March 1)
+*
+*  The algorithm is derived from that of Hatcher 1984
+*  (QJRAS 25, 53-55).
+*
+*  P.T.Wallace   Starlink   27 April 1998
+*
+*  Copyright (C) 1998 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DJM
+      INTEGER IY,IM,ID
+      DOUBLE PRECISION FD
+      INTEGER J
+
+      DOUBLE PRECISION F,D
+      INTEGER JD,N4,ND10
+
+
+
+*  Check if date is acceptable
+      IF (DJM.LE.-2395520D0.OR.DJM.GE.1D9) THEN
+         J=-1
+      ELSE
+         J=0
+
+*     Separate day and fraction
+         F=MOD(DJM,1D0)
+         IF (F.LT.0D0) F=F+1D0
+         D=ANINT(DJM-F)
+
+*     Express day in Gregorian calendar
+         JD=NINT(D)+2400001
+
+         N4=4*(JD+((6*((4*JD-17918)/146097))/4+1)/2-37)
+         ND10=10*(MOD(N4-237,1461)/4)+5
+
+         IY=N4/1461-4712
+         IM=MOD(ND10/306+2,12)+1
+         ID=MOD(ND10,306)/10+1
+         FD=F
+
+         J=0
+
+      END IF
+
+      END
diff --git a/src/slalib/dm2av.f b/src/slalib/dm2av.f
new file mode 100644
index 0000000..3f684fb
--- /dev/null
+++ b/src/slalib/dm2av.f
@@ -0,0 +1,59 @@
+      SUBROUTINE sla_DM2AV (RMAT, AXVEC)
+*+
+*     - - - - - -
+*      D M 2 A V
+*     - - - - - -
+*
+*  From a rotation matrix, determine the corresponding axial vector.
+*  (double precision)
+*
+*  A rotation matrix describes a rotation about some arbitrary axis.
+*  The axis is called the Euler axis, and the angle through which the
+*  reference frame rotates is called the Euler angle.  The axial
+*  vector returned by this routine has the same direction as the
+*  Euler axis, and its magnitude is the Euler angle in radians.  (The
+*  magnitude and direction can be separated by means of the routine
+*  sla_DVN.)
+*
+*  Given:
+*    RMAT   d(3,3)   rotation matrix
+*
+*  Returned:
+*    AXVEC  d(3)     axial vector (radians)
+*
+*  The reference frame rotates clockwise as seen looking along
+*  the axial vector from the origin.
+*
+*  If RMAT is null, so is the result.
+*
+*  P.T.Wallace   Starlink   24 December 1992
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION RMAT(3,3),AXVEC(3)
+
+      DOUBLE PRECISION X,Y,Z,S2,C2,PHI,F
+
+
+
+      X = RMAT(2,3)-RMAT(3,2)
+      Y = RMAT(3,1)-RMAT(1,3)
+      Z = RMAT(1,2)-RMAT(2,1)
+      S2 = SQRT(X*X+Y*Y+Z*Z)
+      IF (S2.NE.0D0) THEN
+         C2 = (RMAT(1,1)+RMAT(2,2)+RMAT(3,3)-1D0)
+         PHI = ATAN2(S2/2D0,C2/2D0)
+         F = PHI/S2
+         AXVEC(1) = X*F
+         AXVEC(2) = Y*F
+         AXVEC(3) = Z*F
+      ELSE
+         AXVEC(1) = 0D0
+         AXVEC(2) = 0D0
+         AXVEC(3) = 0D0
+      END IF
+
+      END
diff --git a/src/slalib/dmat.f b/src/slalib/dmat.f
new file mode 100644
index 0000000..2480b82
--- /dev/null
+++ b/src/slalib/dmat.f
@@ -0,0 +1,140 @@
+      SUBROUTINE sla_DMAT (N, A, Y, D, JF, IW)
+*+
+*     - - - - -
+*      D M A T
+*     - - - - -
+*
+*  Matrix inversion & solution of simultaneous equations
+*  (double precision)
+*
+*  For the set of n simultaneous equations in n unknowns:
+*     A.Y = X
+*
+*  where:
+*     A is a non-singular N x N matrix
+*     Y is the vector of N unknowns
+*     X is the known vector
+*
+*  DMATRX computes:
+*     the inverse of matrix A
+*     the determinant of matrix A
+*     the vector of N unknowns
+*
+*  Arguments:
+*
+*     symbol  type   dimension           before              after
+*
+*       N      i                    no. of unknowns       unchanged
+*       A      d      (N,N)             matrix             inverse
+*       Y      d       (N)              vector            solution
+*       D      d                           -             determinant
+*     * JF     i                           -           singularity flag
+*       IW     i       (N)                 -              workspace
+*
+*  *  JF is the singularity flag.  If the matrix is non-singular,
+*    JF=0 is returned.  If the matrix is singular, JF=-1 & D=0D0 are
+*    returned.  In the latter case, the contents of array A on return
+*    are undefined.
+*
+*  Algorithm:
+*     Gaussian elimination with partial pivoting.
+*
+*  Speed:
+*     Very fast.
+*
+*  Accuracy:
+*     Fairly accurate - errors 1 to 4 times those of routines optimized
+*     for accuracy.
+*
+*  P.T.Wallace   Starlink   7 February 1995
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER N
+      DOUBLE PRECISION A(N,N),Y(N),D
+      INTEGER JF
+      INTEGER IW(N)
+
+      DOUBLE PRECISION SFA
+      PARAMETER (SFA=1D-20)
+
+      INTEGER K,IMX,I,J,NP1MK,KI
+      DOUBLE PRECISION AMX,T,AKK,YK,AIK
+
+
+      JF=0
+      D=1D0
+      DO K=1,N
+         AMX=DABS(A(K,K))
+         IMX=K
+         IF (K.NE.N) THEN
+            DO I=K+1,N
+               T=DABS(A(I,K))
+               IF (T.GT.AMX) THEN
+                  AMX=T
+                  IMX=I
+               END IF
+            END DO
+         END IF
+         IF (AMX.LT.SFA) THEN
+            JF=-1
+         ELSE
+            IF (IMX.NE.K) THEN
+               DO J=1,N
+                  T=A(K,J)
+                  A(K,J)=A(IMX,J)
+                  A(IMX,J)=T
+               END DO
+               T=Y(K)
+               Y(K)=Y(IMX)
+               Y(IMX)=T
+               D=-D
+            END IF
+            IW(K)=IMX
+            AKK=A(K,K)
+            D=D*AKK
+            IF (DABS(D).LT.SFA) THEN
+               JF=-1
+            ELSE
+               AKK=1D0/AKK
+               A(K,K)=AKK
+               DO J=1,N
+                  IF (J.NE.K) A(K,J)=A(K,J)*AKK
+               END DO
+               YK=Y(K)*AKK
+               Y(K)=YK
+               DO I=1,N
+                  AIK=A(I,K)
+                  IF (I.NE.K) THEN
+                     DO J=1,N
+                        IF (J.NE.K) A(I,J)=A(I,J)-AIK*A(K,J)
+                     END DO
+                     Y(I)=Y(I)-AIK*YK
+                  END IF
+               END DO
+               DO I=1,N
+                  IF (I.NE.K) A(I,K)=-A(I,K)*AKK
+               END DO
+            END IF
+         END IF
+      END DO
+      IF (JF.NE.0) THEN
+         D=0D0
+      ELSE
+         DO K=1,N
+            NP1MK=N+1-K
+            KI=IW(NP1MK)
+            IF (NP1MK.NE.KI) THEN
+               DO I=1,N
+                  T=A(I,NP1MK)
+                  A(I,NP1MK)=A(I,KI)
+                  A(I,KI)=T
+               END DO
+            END IF
+         END DO
+      END IF
+
+      END
diff --git a/src/slalib/dmoon.f b/src/slalib/dmoon.f
new file mode 100644
index 0000000..7794255
--- /dev/null
+++ b/src/slalib/dmoon.f
@@ -0,0 +1,641 @@
+      SUBROUTINE sla_DMOON (DATE, PV)
+*+
+*     - - - - - -
+*      D M O O N
+*     - - - - - -
+*
+*  Approximate geocentric position and velocity of the Moon
+*  (double precision)
+*
+*  Given:
+*     DATE       D       TDB (loosely ET) as a Modified Julian Date
+*                                                    (JD-2400000.5)
+*
+*  Returned:
+*     PV         D(6)    Moon x,y,z,xdot,ydot,zdot, mean equator and
+*                                         equinox of date (AU, AU/s)
+*
+*  Notes:
+*
+*  1  This routine is a full implementation of the algorithm
+*     published by Meeus (see reference).
+*
+*  2  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. 
+*
+*  3  The original algorithm is expressed in terms of the obsolete
+*     timescale Ephemeris Time.  Either TDB or TT can be used, but
+*     not UT without incurring significant errors (30 arcsec at
+*     the present time) due to the Moon's 0.5 arcsec/sec movement.
+*
+*  4  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.
+*
+*  5  Velocity is obtained by a complete analytical differentiation
+*     of the Meeus model.
+*
+*  Reference:
+*     Meeus, l'Astronomie, June 1984, p348.
+*
+*  P.T.Wallace   Starlink   22 January 1998
+*
+*  Copyright (C) 1998 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DATE,PV(6)
+
+*  Degrees, arcseconds and seconds of time to radians
+      DOUBLE PRECISION D2R,DAS2R,DS2R
+      PARAMETER (D2R=0.0174532925199432957692369D0,
+     :           DAS2R=4.848136811095359935899141D-6,
+     :           DS2R=7.272205216643039903848712D-5)
+
+*  Seconds per Julian century (86400*36525)
+      DOUBLE PRECISION CJ
+      PARAMETER (CJ=3155760000D0)
+
+*  Julian epoch of B1950
+      DOUBLE PRECISION B1950
+      PARAMETER (B1950=1949.9997904423D0)
+
+*  Earth equatorial radius in AU ( = 6378.137 / 149597870 )
+      DOUBLE PRECISION ERADAU
+      PARAMETER (ERADAU=4.2635212653763D-5)
+
+      DOUBLE PRECISION T,THETA,SINOM,COSOM,DOMCOM,WA,DWA,WB,DWB,WOM,
+     :                 DWOM,SINWOM,COSWOM,V,DV,COEFF,EMN,EMPN,DN,FN,EN,
+     :                 DEN,DTHETA,FTHETA,EL,DEL,B,DB,BF,DBF,P,DP,SP,R,
+     :                 DR,X,Y,Z,XD,YD,ZD,SEL,CEL,SB,CB,RCB,RBD,W,EPJ,
+     :                 EQCOR,EPS,SINEPS,COSEPS,ES,EC
+      INTEGER N,I
+
+*
+*  Coefficients for fundamental arguments
+*
+*   at J1900:  T**0, T**1, T**2, T**3
+*   at epoch:  T**0, T**1
+*
+*  Units are degrees for position and Julian centuries for time
+*
+
+*  Moon's mean longitude
+      DOUBLE PRECISION ELP0,ELP1,ELP2,ELP3,ELP,DELP
+      PARAMETER (ELP0=270.434164D0,
+     :           ELP1=481267.8831D0,
+     :           ELP2=-0.001133D0,
+     :           ELP3=0.0000019D0)
+
+*  Sun's mean anomaly
+      DOUBLE PRECISION EM0,EM1,EM2,EM3,EM,DEM
+      PARAMETER (EM0=358.475833D0,
+     :           EM1=35999.0498D0,
+     :           EM2=-0.000150D0,
+     :           EM3=-0.0000033D0)
+
+*  Moon's mean anomaly
+      DOUBLE PRECISION EMP0,EMP1,EMP2,EMP3,EMP,DEMP
+      PARAMETER (EMP0=296.104608D0,
+     :           EMP1=477198.8491D0,
+     :           EMP2=0.009192D0,
+     :           EMP3=0.0000144D0)
+
+*  Moon's mean elongation
+      DOUBLE PRECISION D0,D1,D2,D3,D,DD
+      PARAMETER (D0=350.737486D0,
+     :           D1=445267.1142D0,
+     :           D2=-0.001436D0,
+     :           D3=0.0000019D0)
+
+*  Mean distance of the Moon from its ascending node
+      DOUBLE PRECISION F0,F1,F2,F3,F,DF
+      PARAMETER (F0=11.250889D0,
+     :           F1=483202.0251D0,
+     :           F2=-0.003211D0,
+     :           F3=-0.0000003D0)
+
+*  Longitude of the Moon's ascending node
+      DOUBLE PRECISION OM0,OM1,OM2,OM3,OM,DOM
+      PARAMETER (OM0=259.183275D0,
+     :           OM1=-1934.1420D0,
+     :           OM2=0.002078D0,
+     :           OM3=0.0000022D0)
+
+*  Coefficients for (dimensionless) E factor
+      DOUBLE PRECISION E1,E2,E,DE,ESQ,DESQ
+      PARAMETER (E1=-0.002495D0,E2=-0.00000752D0)
+
+*  Coefficients for periodic variations etc
+      DOUBLE PRECISION PAC,PA0,PA1
+      PARAMETER (PAC=0.000233D0,PA0=51.2D0,PA1=20.2D0)
+      DOUBLE PRECISION PBC
+      PARAMETER (PBC=-0.001778D0)
+      DOUBLE PRECISION PCC
+      PARAMETER (PCC=0.000817D0)
+      DOUBLE PRECISION PDC
+      PARAMETER (PDC=0.002011D0)
+      DOUBLE PRECISION PEC,PE0,PE1,PE2
+      PARAMETER (PEC=0.003964D0,
+     :                     PE0=346.560D0,PE1=132.870D0,PE2=-0.0091731D0)
+      DOUBLE PRECISION PFC
+      PARAMETER (PFC=0.001964D0)
+      DOUBLE PRECISION PGC
+      PARAMETER (PGC=0.002541D0)
+      DOUBLE PRECISION PHC
+      PARAMETER (PHC=0.001964D0)
+      DOUBLE PRECISION PIC
+      PARAMETER (PIC=-0.024691D0)
+      DOUBLE PRECISION PJC,PJ0,PJ1
+      PARAMETER (PJC=-0.004328D0,PJ0=275.05D0,PJ1=-2.30D0)
+      DOUBLE PRECISION CW1
+      PARAMETER (CW1=0.0004664D0)
+      DOUBLE PRECISION CW2
+      PARAMETER (CW2=0.0000754D0)
+
+*
+*  Coefficients for Moon position
+*
+*   Tx(N)       = coefficient of L, B or P term (deg)
+*   ITx(N,1-5)  = coefficients of M, M', D, F, E**n in argument
+*
+      INTEGER NL,NB,NP
+      PARAMETER (NL=50,NB=45,NP=31)
+      DOUBLE PRECISION TL(NL),TB(NB),TP(NP)
+      INTEGER ITL(5,NL),ITB(5,NB),ITP(5,NP)
+*
+*  Longitude
+*                                         M   M'  D   F   n
+      DATA TL( 1)/            +6.288750D0                     /,
+     :     (ITL(I, 1),I=1,5)/            +0, +1, +0, +0,  0   /
+      DATA TL( 2)/            +1.274018D0                     /,
+     :     (ITL(I, 2),I=1,5)/            +0, -1, +2, +0,  0   /
+      DATA TL( 3)/            +0.658309D0                     /,
+     :     (ITL(I, 3),I=1,5)/            +0, +0, +2, +0,  0   /
+      DATA TL( 4)/            +0.213616D0                     /,
+     :     (ITL(I, 4),I=1,5)/            +0, +2, +0, +0,  0   /
+      DATA TL( 5)/            -0.185596D0                     /,
+     :     (ITL(I, 5),I=1,5)/            +1, +0, +0, +0,  1   /
+      DATA TL( 6)/            -0.114336D0                     /,
+     :     (ITL(I, 6),I=1,5)/            +0, +0, +0, +2,  0   /
+      DATA TL( 7)/            +0.058793D0                     /,
+     :     (ITL(I, 7),I=1,5)/            +0, -2, +2, +0,  0   /
+      DATA TL( 8)/            +0.057212D0                     /,
+     :     (ITL(I, 8),I=1,5)/            -1, -1, +2, +0,  1   /
+      DATA TL( 9)/            +0.053320D0                     /,
+     :     (ITL(I, 9),I=1,5)/            +0, +1, +2, +0,  0   /
+      DATA TL(10)/            +0.045874D0                     /,
+     :     (ITL(I,10),I=1,5)/            -1, +0, +2, +0,  1   /
+      DATA TL(11)/            +0.041024D0                     /,
+     :     (ITL(I,11),I=1,5)/            -1, +1, +0, +0,  1   /
+      DATA TL(12)/            -0.034718D0                     /,
+     :     (ITL(I,12),I=1,5)/            +0, +0, +1, +0,  0   /
+      DATA TL(13)/            -0.030465D0                     /,
+     :     (ITL(I,13),I=1,5)/            +1, +1, +0, +0,  1   /
+      DATA TL(14)/            +0.015326D0                     /,
+     :     (ITL(I,14),I=1,5)/            +0, +0, +2, -2,  0   /
+      DATA TL(15)/            -0.012528D0                     /,
+     :     (ITL(I,15),I=1,5)/            +0, +1, +0, +2,  0   /
+      DATA TL(16)/            -0.010980D0                     /,
+     :     (ITL(I,16),I=1,5)/            +0, -1, +0, +2,  0   /
+      DATA TL(17)/            +0.010674D0                     /,
+     :     (ITL(I,17),I=1,5)/            +0, -1, +4, +0,  0   /
+      DATA TL(18)/            +0.010034D0                     /,
+     :     (ITL(I,18),I=1,5)/            +0, +3, +0, +0,  0   /
+      DATA TL(19)/            +0.008548D0                     /,
+     :     (ITL(I,19),I=1,5)/            +0, -2, +4, +0,  0   /
+      DATA TL(20)/            -0.007910D0                     /,
+     :     (ITL(I,20),I=1,5)/            +1, -1, +2, +0,  1   /
+      DATA TL(21)/            -0.006783D0                     /,
+     :     (ITL(I,21),I=1,5)/            +1, +0, +2, +0,  1   /
+      DATA TL(22)/            +0.005162D0                     /,
+     :     (ITL(I,22),I=1,5)/            +0, +1, -1, +0,  0   /
+      DATA TL(23)/            +0.005000D0                     /,
+     :     (ITL(I,23),I=1,5)/            +1, +0, +1, +0,  1   /
+      DATA TL(24)/            +0.004049D0                     /,
+     :     (ITL(I,24),I=1,5)/            -1, +1, +2, +0,  1   /
+      DATA TL(25)/            +0.003996D0                     /,
+     :     (ITL(I,25),I=1,5)/            +0, +2, +2, +0,  0   /
+      DATA TL(26)/            +0.003862D0                     /,
+     :     (ITL(I,26),I=1,5)/            +0, +0, +4, +0,  0   /
+      DATA TL(27)/            +0.003665D0                     /,
+     :     (ITL(I,27),I=1,5)/            +0, -3, +2, +0,  0   /
+      DATA TL(28)/            +0.002695D0                     /,
+     :     (ITL(I,28),I=1,5)/            -1, +2, +0, +0,  1   /
+      DATA TL(29)/            +0.002602D0                     /,
+     :     (ITL(I,29),I=1,5)/            +0, +1, -2, -2,  0   /
+      DATA TL(30)/            +0.002396D0                     /,
+     :     (ITL(I,30),I=1,5)/            -1, -2, +2, +0,  1   /
+      DATA TL(31)/            -0.002349D0                     /,
+     :     (ITL(I,31),I=1,5)/            +0, +1, +1, +0,  0   /
+      DATA TL(32)/            +0.002249D0                     /,
+     :     (ITL(I,32),I=1,5)/            -2, +0, +2, +0,  2   /
+      DATA TL(33)/            -0.002125D0                     /,
+     :     (ITL(I,33),I=1,5)/            +1, +2, +0, +0,  1   /
+      DATA TL(34)/            -0.002079D0                     /,
+     :     (ITL(I,34),I=1,5)/            +2, +0, +0, +0,  2   /
+      DATA TL(35)/            +0.002059D0                     /,
+     :     (ITL(I,35),I=1,5)/            -2, -1, +2, +0,  2   /
+      DATA TL(36)/            -0.001773D0                     /,
+     :     (ITL(I,36),I=1,5)/            +0, +1, +2, -2,  0   /
+      DATA TL(37)/            -0.001595D0                     /,
+     :     (ITL(I,37),I=1,5)/            +0, +0, +2, +2,  0   /
+      DATA TL(38)/            +0.001220D0                     /,
+     :     (ITL(I,38),I=1,5)/            -1, -1, +4, +0,  1   /
+      DATA TL(39)/            -0.001110D0                     /,
+     :     (ITL(I,39),I=1,5)/            +0, +2, +0, +2,  0   /
+      DATA TL(40)/            +0.000892D0                     /,
+     :     (ITL(I,40),I=1,5)/            +0, +1, -3, +0,  0   /
+      DATA TL(41)/            -0.000811D0                     /,
+     :     (ITL(I,41),I=1,5)/            +1, +1, +2, +0,  1   /
+      DATA TL(42)/            +0.000761D0                     /,
+     :     (ITL(I,42),I=1,5)/            -1, -2, +4, +0,  1   /
+      DATA TL(43)/            +0.000717D0                     /,
+     :     (ITL(I,43),I=1,5)/            -2, +1, +0, +0,  2   /
+      DATA TL(44)/            +0.000704D0                     /,
+     :     (ITL(I,44),I=1,5)/            -2, +1, -2, +0,  2   /
+      DATA TL(45)/            +0.000693D0                     /,
+     :     (ITL(I,45),I=1,5)/            +1, -2, +2, +0,  1   /
+      DATA TL(46)/            +0.000598D0                     /,
+     :     (ITL(I,46),I=1,5)/            -1, +0, +2, -2,  1   /
+      DATA TL(47)/            +0.000550D0                     /,
+     :     (ITL(I,47),I=1,5)/            +0, +1, +4, +0,  0   /
+      DATA TL(48)/            +0.000538D0                     /,
+     :     (ITL(I,48),I=1,5)/            +0, +4, +0, +0,  0   /
+      DATA TL(49)/            +0.000521D0                     /,
+     :     (ITL(I,49),I=1,5)/            -1, +0, +4, +0,  1   /
+      DATA TL(50)/            +0.000486D0                     /,
+     :     (ITL(I,50),I=1,5)/            +0, +2, -1, +0,  0   /
+*
+*  Latitude
+*                                         M   M'  D   F   n
+      DATA TB( 1)/            +5.128189D0                     /,
+     :     (ITB(I, 1),I=1,5)/            +0, +0, +0, +1,  0   /
+      DATA TB( 2)/            +0.280606D0                     /,
+     :     (ITB(I, 2),I=1,5)/            +0, +1, +0, +1,  0   /
+      DATA TB( 3)/            +0.277693D0                     /,
+     :     (ITB(I, 3),I=1,5)/            +0, +1, +0, -1,  0   /
+      DATA TB( 4)/            +0.173238D0                     /,
+     :     (ITB(I, 4),I=1,5)/            +0, +0, +2, -1,  0   /
+      DATA TB( 5)/            +0.055413D0                     /,
+     :     (ITB(I, 5),I=1,5)/            +0, -1, +2, +1,  0   /
+      DATA TB( 6)/            +0.046272D0                     /,
+     :     (ITB(I, 6),I=1,5)/            +0, -1, +2, -1,  0   /
+      DATA TB( 7)/            +0.032573D0                     /,
+     :     (ITB(I, 7),I=1,5)/            +0, +0, +2, +1,  0   /
+      DATA TB( 8)/            +0.017198D0                     /,
+     :     (ITB(I, 8),I=1,5)/            +0, +2, +0, +1,  0   /
+      DATA TB( 9)/            +0.009267D0                     /,
+     :     (ITB(I, 9),I=1,5)/            +0, +1, +2, -1,  0   /
+      DATA TB(10)/            +0.008823D0                     /,
+     :     (ITB(I,10),I=1,5)/            +0, +2, +0, -1,  0   /
+      DATA TB(11)/            +0.008247D0                     /,
+     :     (ITB(I,11),I=1,5)/            -1, +0, +2, -1,  1   /
+      DATA TB(12)/            +0.004323D0                     /,
+     :     (ITB(I,12),I=1,5)/            +0, -2, +2, -1,  0   /
+      DATA TB(13)/            +0.004200D0                     /,
+     :     (ITB(I,13),I=1,5)/            +0, +1, +2, +1,  0   /
+      DATA TB(14)/            +0.003372D0                     /,
+     :     (ITB(I,14),I=1,5)/            -1, +0, -2, +1,  1   /
+      DATA TB(15)/            +0.002472D0                     /,
+     :     (ITB(I,15),I=1,5)/            -1, -1, +2, +1,  1   /
+      DATA TB(16)/            +0.002222D0                     /,
+     :     (ITB(I,16),I=1,5)/            -1, +0, +2, +1,  1   /
+      DATA TB(17)/            +0.002072D0                     /,
+     :     (ITB(I,17),I=1,5)/            -1, -1, +2, -1,  1   /
+      DATA TB(18)/            +0.001877D0                     /,
+     :     (ITB(I,18),I=1,5)/            -1, +1, +0, +1,  1   /
+      DATA TB(19)/            +0.001828D0                     /,
+     :     (ITB(I,19),I=1,5)/            +0, -1, +4, -1,  0   /
+      DATA TB(20)/            -0.001803D0                     /,
+     :     (ITB(I,20),I=1,5)/            +1, +0, +0, +1,  1   /
+      DATA TB(21)/            -0.001750D0                     /,
+     :     (ITB(I,21),I=1,5)/            +0, +0, +0, +3,  0   /
+      DATA TB(22)/            +0.001570D0                     /,
+     :     (ITB(I,22),I=1,5)/            -1, +1, +0, -1,  1   /
+      DATA TB(23)/            -0.001487D0                     /,
+     :     (ITB(I,23),I=1,5)/            +0, +0, +1, +1,  0   /
+      DATA TB(24)/            -0.001481D0                     /,
+     :     (ITB(I,24),I=1,5)/            +1, +1, +0, +1,  1   /
+      DATA TB(25)/            +0.001417D0                     /,
+     :     (ITB(I,25),I=1,5)/            -1, -1, +0, +1,  1   /
+      DATA TB(26)/            +0.001350D0                     /,
+     :     (ITB(I,26),I=1,5)/            -1, +0, +0, +1,  1   /
+      DATA TB(27)/            +0.001330D0                     /,
+     :     (ITB(I,27),I=1,5)/            +0, +0, -1, +1,  0   /
+      DATA TB(28)/            +0.001106D0                     /,
+     :     (ITB(I,28),I=1,5)/            +0, +3, +0, +1,  0   /
+      DATA TB(29)/            +0.001020D0                     /,
+     :     (ITB(I,29),I=1,5)/            +0, +0, +4, -1,  0   /
+      DATA TB(30)/            +0.000833D0                     /,
+     :     (ITB(I,30),I=1,5)/            +0, -1, +4, +1,  0   /
+      DATA TB(31)/            +0.000781D0                     /,
+     :     (ITB(I,31),I=1,5)/            +0, +1, +0, -3,  0   /
+      DATA TB(32)/            +0.000670D0                     /,
+     :     (ITB(I,32),I=1,5)/            +0, -2, +4, +1,  0   /
+      DATA TB(33)/            +0.000606D0                     /,
+     :     (ITB(I,33),I=1,5)/            +0, +0, +2, -3,  0   /
+      DATA TB(34)/            +0.000597D0                     /,
+     :     (ITB(I,34),I=1,5)/            +0, +2, +2, -1,  0   /
+      DATA TB(35)/            +0.000492D0                     /,
+     :     (ITB(I,35),I=1,5)/            -1, +1, +2, -1,  1   /
+      DATA TB(36)/            +0.000450D0                     /,
+     :     (ITB(I,36),I=1,5)/            +0, +2, -2, -1,  0   /
+      DATA TB(37)/            +0.000439D0                     /,
+     :     (ITB(I,37),I=1,5)/            +0, +3, +0, -1,  0   /
+      DATA TB(38)/            +0.000423D0                     /,
+     :     (ITB(I,38),I=1,5)/            +0, +2, +2, +1,  0   /
+      DATA TB(39)/            +0.000422D0                     /,
+     :     (ITB(I,39),I=1,5)/            +0, -3, +2, -1,  0   /
+      DATA TB(40)/            -0.000367D0                     /,
+     :     (ITB(I,40),I=1,5)/            +1, -1, +2, +1,  1   /
+      DATA TB(41)/            -0.000353D0                     /,
+     :     (ITB(I,41),I=1,5)/            +1, +0, +2, +1,  1   /
+      DATA TB(42)/            +0.000331D0                     /,
+     :     (ITB(I,42),I=1,5)/            +0, +0, +4, +1,  0   /
+      DATA TB(43)/            +0.000317D0                     /,
+     :     (ITB(I,43),I=1,5)/            -1, +1, +2, +1,  1   /
+      DATA TB(44)/            +0.000306D0                     /,
+     :     (ITB(I,44),I=1,5)/            -2, +0, +2, -1,  2   /
+      DATA TB(45)/            -0.000283D0                     /,
+     :     (ITB(I,45),I=1,5)/            +0, +1, +0, +3,  0   /
+*
+*  Parallax
+*                                         M   M'  D   F   n
+      DATA TP( 1)/            +0.950724D0                     /,
+     :     (ITP(I, 1),I=1,5)/            +0, +0, +0, +0,  0   /
+      DATA TP( 2)/            +0.051818D0                     /,
+     :     (ITP(I, 2),I=1,5)/            +0, +1, +0, +0,  0   /
+      DATA TP( 3)/            +0.009531D0                     /,
+     :     (ITP(I, 3),I=1,5)/            +0, -1, +2, +0,  0   /
+      DATA TP( 4)/            +0.007843D0                     /,
+     :     (ITP(I, 4),I=1,5)/            +0, +0, +2, +0,  0   /
+      DATA TP( 5)/            +0.002824D0                     /,
+     :     (ITP(I, 5),I=1,5)/            +0, +2, +0, +0,  0   /
+      DATA TP( 6)/            +0.000857D0                     /,
+     :     (ITP(I, 6),I=1,5)/            +0, +1, +2, +0,  0   /
+      DATA TP( 7)/            +0.000533D0                     /,
+     :     (ITP(I, 7),I=1,5)/            -1, +0, +2, +0,  1   /
+      DATA TP( 8)/            +0.000401D0                     /,
+     :     (ITP(I, 8),I=1,5)/            -1, -1, +2, +0,  1   /
+      DATA TP( 9)/            +0.000320D0                     /,
+     :     (ITP(I, 9),I=1,5)/            -1, +1, +0, +0,  1   /
+      DATA TP(10)/            -0.000271D0                     /,
+     :     (ITP(I,10),I=1,5)/            +0, +0, +1, +0,  0   /
+      DATA TP(11)/            -0.000264D0                     /,
+     :     (ITP(I,11),I=1,5)/            +1, +1, +0, +0,  1   /
+      DATA TP(12)/            -0.000198D0                     /,
+     :     (ITP(I,12),I=1,5)/            +0, -1, +0, +2,  0   /
+      DATA TP(13)/            +0.000173D0                     /,
+     :     (ITP(I,13),I=1,5)/            +0, +3, +0, +0,  0   /
+      DATA TP(14)/            +0.000167D0                     /,
+     :     (ITP(I,14),I=1,5)/            +0, -1, +4, +0,  0   /
+      DATA TP(15)/            -0.000111D0                     /,
+     :     (ITP(I,15),I=1,5)/            +1, +0, +0, +0,  1   /
+      DATA TP(16)/            +0.000103D0                     /,
+     :     (ITP(I,16),I=1,5)/            +0, -2, +4, +0,  0   /
+      DATA TP(17)/            -0.000084D0                     /,
+     :     (ITP(I,17),I=1,5)/            +0, +2, -2, +0,  0   /
+      DATA TP(18)/            -0.000083D0                     /,
+     :     (ITP(I,18),I=1,5)/            +1, +0, +2, +0,  1   /
+      DATA TP(19)/            +0.000079D0                     /,
+     :     (ITP(I,19),I=1,5)/            +0, +2, +2, +0,  0   /
+      DATA TP(20)/            +0.000072D0                     /,
+     :     (ITP(I,20),I=1,5)/            +0, +0, +4, +0,  0   /
+      DATA TP(21)/            +0.000064D0                     /,
+     :     (ITP(I,21),I=1,5)/            -1, +1, +2, +0,  1   /
+      DATA TP(22)/            -0.000063D0                     /,
+     :     (ITP(I,22),I=1,5)/            +1, -1, +2, +0,  1   /
+      DATA TP(23)/            +0.000041D0                     /,
+     :     (ITP(I,23),I=1,5)/            +1, +0, +1, +0,  1   /
+      DATA TP(24)/            +0.000035D0                     /,
+     :     (ITP(I,24),I=1,5)/            -1, +2, +0, +0,  1   /
+      DATA TP(25)/            -0.000033D0                     /,
+     :     (ITP(I,25),I=1,5)/            +0, +3, -2, +0,  0   /
+      DATA TP(26)/            -0.000030D0                     /,
+     :     (ITP(I,26),I=1,5)/            +0, +1, +1, +0,  0   /
+      DATA TP(27)/            -0.000029D0                     /,
+     :     (ITP(I,27),I=1,5)/            +0, +0, -2, +2,  0   /
+      DATA TP(28)/            -0.000029D0                     /,
+     :     (ITP(I,28),I=1,5)/            +1, +2, +0, +0,  1   /
+      DATA TP(29)/            +0.000026D0                     /,
+     :     (ITP(I,29),I=1,5)/            -2, +0, +2, +0,  2   /
+      DATA TP(30)/            -0.000023D0                     /,
+     :     (ITP(I,30),I=1,5)/            +0, +1, -2, +2,  0   /
+      DATA TP(31)/            +0.000019D0                     /,
+     :     (ITP(I,31),I=1,5)/            -1, -1, +4, +0,  1   /
+
+
+
+*  Centuries since J1900
+      T=(DATE-15019.5D0)/36525D0
+
+*
+*  Fundamental arguments (radians) and derivatives (radians per
+*  Julian century) for the current epoch
+*
+
+*  Moon's mean longitude
+      ELP=D2R*MOD(ELP0+(ELP1+(ELP2+ELP3*T)*T)*T,360D0)
+      DELP=D2R*(ELP1+(2D0*ELP2+3D0*ELP3*T)*T)
+
+*  Sun's mean anomaly
+      EM=D2R*MOD(EM0+(EM1+(EM2+EM3*T)*T)*T,360D0)
+      DEM=D2R*(EM1+(2D0*EM2+3D0*EM3*T)*T)
+
+*  Moon's mean anomaly
+      EMP=D2R*MOD(EMP0+(EMP1+(EMP2+EMP3*T)*T)*T,360D0)
+      DEMP=D2R*(EMP1+(2D0*EMP2+3D0*EMP3*T)*T)
+
+*  Moon's mean elongation
+      D=D2R*MOD(D0+(D1+(D2+D3*T)*T)*T,360D0)
+      DD=D2R*(D1+(2D0*D2+3D0*D3*T)*T)
+
+*  Mean distance of the Moon from its ascending node
+      F=D2R*MOD(F0+(F1+(F2+F3*T)*T)*T,360D0)
+      DF=D2R*(F1+(2D0*F2+3D0*F3*T)*T)
+
+*  Longitude of the Moon's ascending node
+      OM=D2R*MOD(OM0+(OM1+(OM2+OM3*T)*T)*T,360D0)
+      DOM=D2R*(OM1+(2D0*OM2+3D0*OM3*T)*T)
+      SINOM=SIN(OM)
+      COSOM=COS(OM)
+      DOMCOM=DOM*COSOM
+
+*  Add the periodic variations
+      THETA=D2R*(PA0+PA1*T)
+      WA=SIN(THETA)
+      DWA=D2R*PA1*COS(THETA)
+      THETA=D2R*(PE0+(PE1+PE2*T)*T)
+      WB=PEC*SIN(THETA)
+      DWB=D2R*PEC*(PE1+2D0*PE2*T)*COS(THETA)
+      ELP=ELP+D2R*(PAC*WA+WB+PFC*SINOM)
+      DELP=DELP+D2R*(PAC*DWA+DWB+PFC*DOMCOM)
+      EM=EM+D2R*PBC*WA
+      DEM=DEM+D2R*PBC*DWA
+      EMP=EMP+D2R*(PCC*WA+WB+PGC*SINOM)
+      DEMP=DEMP+D2R*(PCC*DWA+DWB+PGC*DOMCOM)
+      D=D+D2R*(PDC*WA+WB+PHC*SINOM)
+      DD=DD+D2R*(PDC*DWA+DWB+PHC*DOMCOM)
+      WOM=OM+D2R*(PJ0+PJ1*T)
+      DWOM=DOM+D2R*PJ1
+      SINWOM=SIN(WOM)
+      COSWOM=COS(WOM)
+      F=F+D2R*(WB+PIC*SINOM+PJC*SINWOM)
+      DF=DF+D2R*(DWB+PIC*DOMCOM+PJC*DWOM*COSWOM)
+
+*  E-factor, and square
+      E=1D0+(E1+E2*T)*T
+      DE=E1+2D0*E2*T
+      ESQ=E*E
+      DESQ=2D0*E*DE
+
+*
+*  Series expansions
+*
+
+*  Longitude
+      V=0D0
+      DV=0D0
+      DO N=NL,1,-1
+         COEFF=TL(N)
+         EMN=DBLE(ITL(1,N))
+         EMPN=DBLE(ITL(2,N))
+         DN=DBLE(ITL(3,N))
+         FN=DBLE(ITL(4,N))
+         I=ITL(5,N)
+         IF (I.EQ.0) THEN
+            EN=1D0
+            DEN=0D0
+         ELSE IF (I.EQ.1) THEN
+            EN=E
+            DEN=DE
+         ELSE
+            EN=ESQ
+            DEN=DESQ
+         END IF
+         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)
+      END DO
+      EL=ELP+D2R*V
+      DEL=(DELP+D2R*DV)/CJ
+
+*  Latitude
+      V=0D0
+      DV=0D0
+      DO N=NB,1,-1
+         COEFF=TB(N)
+         EMN=DBLE(ITB(1,N))
+         EMPN=DBLE(ITB(2,N))
+         DN=DBLE(ITB(3,N))
+         FN=DBLE(ITB(4,N))
+         I=ITB(5,N)
+         IF (I.EQ.0) THEN
+            EN=1D0
+            DEN=0D0
+         ELSE IF (I.EQ.1) THEN
+            EN=E
+            DEN=DE
+         ELSE
+            EN=ESQ
+            DEN=DESQ
+         END IF
+         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)
+      END DO
+      BF=1D0-CW1*COSOM-CW2*COSWOM
+      DBF=CW1*DOM*SINOM+CW2*DWOM*SINWOM
+      B=D2R*V*BF
+      DB=D2R*(DV*BF+V*DBF)/CJ
+
+*  Parallax
+      V=0D0
+      DV=0D0
+      DO N=NP,1,-1
+         COEFF=TP(N)
+         EMN=DBLE(ITP(1,N))
+         EMPN=DBLE(ITP(2,N))
+         DN=DBLE(ITP(3,N))
+         FN=DBLE(ITP(4,N))
+         I=ITP(5,N)
+         IF (I.EQ.0) THEN
+            EN=1D0
+            DEN=0D0
+         ELSE IF (I.EQ.1) THEN
+            EN=E
+            DEN=DE
+         ELSE
+            EN=ESQ
+            DEN=DESQ
+         END IF
+         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)
+      END DO
+      P=D2R*V
+      DP=D2R*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-51544.5D0)/36525D0
+
+*  Fricke equinox correction
+      EPJ=2000D0+T*100D0
+      EQCOR=DS2R*(0.035D0+0.00085D0*(EPJ-B1950))
+
+*  Mean obliquity (IAU 1976)
+      EPS=DAS2R*(84381.448D0+(-46.8150D0+(-0.00059D0+0.001813D0*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(1)=X-EC*Y+ES*Z
+      PV(2)=EQCOR*X+Y*COSEPS-Z*SINEPS
+      PV(3)=Y*SINEPS+Z*COSEPS
+      PV(4)=XD-EC*YD+ES*ZD
+      PV(5)=EQCOR*XD+YD*COSEPS-ZD*SINEPS
+      PV(6)=YD*SINEPS+ZD*COSEPS
+
+      END
diff --git a/src/slalib/dmxm.f b/src/slalib/dmxm.f
new file mode 100644
index 0000000..41f3d99
--- /dev/null
+++ b/src/slalib/dmxm.f
@@ -0,0 +1,56 @@
+      SUBROUTINE sla_DMXM (A, B, C)
+*+
+*     - - - - -
+*      D M X M
+*     - - - - -
+*
+*  Product of two 3x3 matrices:
+*
+*      matrix C  =  matrix A  x  matrix B
+*
+*  (double precision)
+*
+*  Given:
+*      A      dp(3,3)        matrix
+*      B      dp(3,3)        matrix
+*
+*  Returned:
+*      C      dp(3,3)        matrix result
+*
+*  To comply with the ANSI Fortran 77 standard, A, B and C must
+*  be different arrays.  However, the routine is coded so as to
+*  work properly on the VAX and many other systems even if this
+*  rule is violated.
+*
+*  P.T.Wallace   Starlink   5 April 1990
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION A(3,3),B(3,3),C(3,3)
+
+      INTEGER I,J,K
+      DOUBLE PRECISION W,WM(3,3)
+
+
+*  Multiply into scratch matrix
+      DO I=1,3
+         DO J=1,3
+            W=0D0
+            DO K=1,3
+               W=W+A(I,K)*B(K,J)
+            END DO
+            WM(I,J)=W
+         END DO
+      END DO
+
+*  Return the result
+      DO J=1,3
+         DO I=1,3
+            C(I,J)=WM(I,J)
+         END DO
+      END DO
+
+      END
diff --git a/src/slalib/dmxv.f b/src/slalib/dmxv.f
new file mode 100644
index 0000000..e70a28e
--- /dev/null
+++ b/src/slalib/dmxv.f
@@ -0,0 +1,47 @@
+      SUBROUTINE sla_DMXV (DM, VA, VB)
+*+
+*     - - - - -
+*      D M X V
+*     - - - - -
+*
+*  Performs the 3-D forward unitary transformation:
+*
+*     vector VB = matrix DM * vector VA
+*
+*  (double precision)
+*
+*  Given:
+*     DM       dp(3,3)    matrix
+*     VA       dp(3)      vector
+*
+*  Returned:
+*     VB       dp(3)      result vector
+*
+*  P.T.Wallace   Starlink   March 1986
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DM(3,3),VA(3),VB(3)
+
+      INTEGER I,J
+      DOUBLE PRECISION W,VW(3)
+
+
+*  Matrix DM * vector VA -> vector VW
+      DO J=1,3
+         W=0D0
+         DO I=1,3
+            W=W+DM(J,I)*VA(I)
+         END DO
+         VW(J)=W
+      END DO
+
+*  Vector VW -> vector VB
+      DO J=1,3
+         VB(J)=VW(J)
+      END DO
+
+      END
diff --git a/src/slalib/dpav.f b/src/slalib/dpav.f
new file mode 100644
index 0000000..63ad759
--- /dev/null
+++ b/src/slalib/dpav.f
@@ -0,0 +1,72 @@
+      DOUBLE PRECISION FUNCTION sla_DPAV ( V1, V2 )
+*+
+*     - - - - -
+*      D P A V
+*     - - - - -
+*
+*  Position angle of one celestial direction with respect to another.
+*
+*  (double precision)
+*
+*  Given:
+*     V1    d(3)    direction cosines of one point
+*     V2    d(3)    direction cosines of the other point
+*
+*  (The coordinate frames correspond to RA,Dec, Long,Lat etc.)
+*
+*  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.
+*
+*  V1 and V2 need not be unit vectors.
+*
+*  The routine sla_DBEAR performs an equivalent function except
+*  that the points are specified in the form of spherical
+*  coordinates.
+*
+*  Patrick Wallace   Starlink   13 July 1997
+*
+*  Copyright (C) 1997 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION V1(3),V2(3)
+
+      DOUBLE PRECISION X1,Y1,Z1,W,R,XU1,YU1,ZU1,DX,DY,DZ,SQ,CQ
+
+
+
+*  Unit vector to point 1
+      X1=V1(1)
+      Y1=V1(2)
+      Z1=V1(3)
+      W=SQRT(X1*X1+Y1*Y1+Z1*Z1)
+      IF (W.NE.0D0) THEN
+         X1=X1/W
+         Y1=Y1/W
+         Z1=Z1/W
+      END IF
+
+*  Unit vector "north" from point 1
+      R=SQRT(X1*X1+Y1*Y1)
+      IF (R.EQ.0.0) R=1D-5
+      W=Z1/R
+      XU1=-X1*W
+      YU1=-Y1*W
+      ZU1=R
+
+*  Vector from point 1 to point 2
+      DX=V2(1)-X1
+      DY=V2(2)-Y1
+      DZ=V2(3)-Z1
+
+*  Position angle
+      SQ=DX*YU1*Z1+DY*ZU1*X1+DZ*XU1*Y1-DZ*YU1*X1-DY*XU1*Z1-DX*ZU1*Y1
+      CQ=DX*XU1+DY*YU1+DZ*ZU1
+      IF (SQ.EQ.0D0.AND.CQ.EQ.0D0) CQ=1D0
+      sla_DPAV=ATAN2(SQ,CQ)
+
+      END
diff --git a/src/slalib/dr2af.f b/src/slalib/dr2af.f
new file mode 100644
index 0000000..3f9dbf3
--- /dev/null
+++ b/src/slalib/dr2af.f
@@ -0,0 +1,58 @@
+      SUBROUTINE sla_DR2AF (NDP, ANGLE, SIGN, IDMSF)
+*+
+*     - - - - - -
+*      D R 2 A F
+*     - - - - - -
+*
+*  Convert an angle in radians to degrees, arcminutes, arcseconds
+*  (double precision)
+*
+*  Given:
+*     NDP      i      number of decimal places of arcseconds
+*     ANGLE    d      angle in radians
+*
+*  Returned:
+*     SIGN     c      '+' or '-'
+*     IDMSF    i(4)   degrees, arcminutes, arcseconds, fraction
+*
+*  Notes:
+*
+*     1)  NDP less than zero is interpreted as zero.
+*
+*     2)  The largest useful value for NDP is determined by the size
+*         of ANGLE, the format of DOUBLE PRECISION floating-point
+*         numbers on the target machine, and the risk of overflowing
+*         IDMSF(4).  For example, on the VAX, for ANGLE up to 2pi, the
+*         available floating-point precision corresponds roughly to
+*         NDP=12.  However, the practical limit is NDP=9, set by the
+*         capacity of the 32-bit integer IDMSF(4).
+*
+*     3)  The absolute value of ANGLE may exceed 2pi.  In cases where it
+*         does not, it is up to the caller to test for and handle the
+*         case where ANGLE is very nearly 2pi and rounds up to 360 deg,
+*         by testing for IDMSF(1)=360 and setting IDMSF(1-4) to zero.
+*
+*  Called:  sla_DD2TF
+*
+*  P.T.Wallace   Starlink   19 March 1999
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER NDP
+      DOUBLE PRECISION ANGLE
+      CHARACTER SIGN*(*)
+      INTEGER IDMSF(4)
+
+*  Hours to degrees * radians to turns
+      DOUBLE PRECISION F
+      PARAMETER (F=15D0/6.283185307179586476925287D0)
+
+
+
+*  Scale then use days to h,m,s routine
+      CALL sla_DD2TF(NDP,ANGLE*F,SIGN,IDMSF)
+
+      END
diff --git a/src/slalib/dr2tf.f b/src/slalib/dr2tf.f
new file mode 100644
index 0000000..f8f2a71
--- /dev/null
+++ b/src/slalib/dr2tf.f
@@ -0,0 +1,58 @@
+      SUBROUTINE sla_DR2TF (NDP, ANGLE, SIGN, IHMSF)
+*+
+*     - - - - - -
+*      D R 2 T F
+*     - - - - - -
+*
+*  Convert an angle in radians to hours, minutes, seconds
+*  (double precision)
+*
+*  Given:
+*     NDP      i      number of decimal places of seconds
+*     ANGLE    d      angle in radians
+*
+*  Returned:
+*     SIGN     c      '+' or '-'
+*     IHMSF    i(4)   hours, minutes, seconds, fraction
+*
+*  Notes:
+*
+*     1)  NDP less than zero is interpreted as zero.
+*
+*     2)  The largest useful value for NDP is determined by the size
+*         of ANGLE, the format of DOUBLE PRECISION floating-point
+*         numbers on the target machine, and the risk of overflowing
+*         IHMSF(4).  For example, on the VAX, for ANGLE up to 2pi, the
+*         available floating-point precision corresponds roughly to
+*         NDP=12.  However, the practical limit is NDP=9, set by the
+*         capacity of the 32-bit integer IHMSF(4).
+*
+*     3)  The absolute value of ANGLE may exceed 2pi.  In cases where it
+*         does not, it is up to the caller to test for and handle the
+*         case where ANGLE is very nearly 2pi and rounds up to 24 hours,
+*         by testing for IHMSF(1)=24 and setting IHMSF(1-4) to zero.
+*
+*  Called:  sla_DD2TF
+*
+*  P.T.Wallace   Starlink   19 March 1999
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER NDP
+      DOUBLE PRECISION ANGLE
+      CHARACTER SIGN*(*)
+      INTEGER IHMSF(4)
+
+*  Turns to radians
+      DOUBLE PRECISION T2R
+      PARAMETER (T2R=6.283185307179586476925287D0)
+
+
+
+*  Scale then use days to h,m,s routine
+      CALL sla_DD2TF(NDP,ANGLE/T2R,SIGN,IHMSF)
+
+      END
diff --git a/src/slalib/drange.f b/src/slalib/drange.f
new file mode 100644
index 0000000..9e678af
--- /dev/null
+++ b/src/slalib/drange.f
@@ -0,0 +1,32 @@
+      DOUBLE PRECISION FUNCTION sla_DRANGE (ANGLE)
+*+
+*     - - - - - - -
+*      D R A N G E
+*     - - - - - - -
+*
+*  Normalize angle into range +/- pi  (double precision)
+*
+*  Given:
+*     ANGLE     dp      the angle in radians
+*
+*  The result (double precision) is ANGLE expressed in the range +/- pi.
+*
+*  P.T.Wallace   Starlink   23 November 1995
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION ANGLE
+
+      DOUBLE PRECISION DPI,D2PI
+      PARAMETER (DPI=3.141592653589793238462643D0)
+      PARAMETER (D2PI=6.283185307179586476925287D0)
+
+
+      sla_DRANGE=MOD(ANGLE,D2PI)
+      IF (ABS(sla_DRANGE).GE.DPI)
+     :          sla_DRANGE=sla_DRANGE-SIGN(D2PI,ANGLE)
+
+      END
diff --git a/src/slalib/dranrm.f b/src/slalib/dranrm.f
new file mode 100644
index 0000000..ee9af25
--- /dev/null
+++ b/src/slalib/dranrm.f
@@ -0,0 +1,31 @@
+      DOUBLE PRECISION FUNCTION sla_DRANRM (ANGLE)
+*+
+*     - - - - - - -
+*      D R A N R M
+*     - - - - - - -
+*
+*  Normalize angle into range 0-2 pi  (double precision)
+*
+*  Given:
+*     ANGLE     dp      the angle in radians
+*
+*  The result is ANGLE expressed in the range 0-2 pi (double
+*  precision).
+*
+*  P.T.Wallace   Starlink   23 November 1995
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION ANGLE
+
+      DOUBLE PRECISION D2PI
+      PARAMETER (D2PI=6.283185307179586476925286766559D0)
+
+
+      sla_DRANRM=MOD(ANGLE,D2PI)
+      IF (sla_DRANRM.LT.0D0) sla_DRANRM=sla_DRANRM+D2PI
+
+      END
diff --git a/src/slalib/ds2c6.f b/src/slalib/ds2c6.f
new file mode 100644
index 0000000..56298f3
--- /dev/null
+++ b/src/slalib/ds2c6.f
@@ -0,0 +1,57 @@
+      SUBROUTINE sla_DS2C6 (A, B, R, AD, BD, RD, V)
+*+
+*     - - - - - -
+*      D S 2 C 6
+*     - - - - - -
+*
+*  Conversion of position & velocity in spherical coordinates
+*  to Cartesian coordinates
+*
+*  (double precision)
+*
+*  Given:
+*     A     dp      longitude (radians)
+*     B     dp      latitude (radians)
+*     R     dp      radial coordinate
+*     AD    dp      longitude derivative (radians per unit time)
+*     BD    dp      latitude derivative (radians per unit time)
+*     RD    dp      radial derivative
+*
+*  Returned:
+*     V     dp(6)   Cartesian position & velocity vector
+*
+*  P.T.Wallace   Starlink   10 July 1993
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION A,B,R,AD,BD,RD,V(6)
+
+      DOUBLE PRECISION SA,CA,SB,CB,RCB,X,Y,RBD,W
+
+
+
+*  Useful functions
+      SA=SIN(A)
+      CA=COS(A)
+      SB=SIN(B)
+      CB=COS(B)
+      RCB=R*CB
+      X=RCB*CA
+      Y=RCB*SA
+      RBD=R*BD
+      W=RBD*SB-CB*RD
+
+*  Position
+      V(1)=X
+      V(2)=Y
+      V(3)=R*SB
+
+*  Velocity
+      V(4)=-Y*AD-W*CA
+      V(5)=X*AD-W*SA
+      V(6)=RBD*CB+SB*RD
+
+      END
diff --git a/src/slalib/ds2tp.f b/src/slalib/ds2tp.f
new file mode 100644
index 0000000..ab1ccf9
--- /dev/null
+++ b/src/slalib/ds2tp.f
@@ -0,0 +1,67 @@
+      SUBROUTINE sla_DS2TP (RA, DEC, RAZ, DECZ, XI, ETA, J)
+*+
+*     - - - - - -
+*      D S 2 T P
+*     - - - - - -
+*
+*  Projection of spherical coordinates onto tangent plane:
+*  "gnomonic" projection - "standard coordinates" (double precision)
+*
+*  Given:
+*     RA,DEC      dp   spherical coordinates of point to be projected
+*     RAZ,DECZ    dp   spherical coordinates of tangent point
+*
+*  Returned:
+*     XI,ETA      dp   rectangular coordinates on tangent plane
+*     J           int  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
+*
+*  P.T.Wallace   Starlink   18 July 1996
+*
+*  Copyright (C) 1996 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION RA,DEC,RAZ,DECZ,XI,ETA
+      INTEGER J
+
+      DOUBLE PRECISION SDECZ,SDEC,CDECZ,CDEC,
+     :                 RADIF,SRADIF,CRADIF,DENOM
+
+      DOUBLE PRECISION TINY
+      PARAMETER (TINY=1D-6)
+
+
+*  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.GT.TINY) THEN
+         J=0
+      ELSE IF (DENOM.GE.0D0) THEN
+         J=1
+         DENOM=TINY
+      ELSE IF (DENOM.GT.-TINY) THEN
+         J=2
+         DENOM=-TINY
+      ELSE
+         J=3
+      END IF
+
+*  Compute tangent plane coordinates (even in dubious cases)
+      XI=CDEC*SRADIF/DENOM
+      ETA=(SDEC*CDECZ-CDEC*SDECZ*CRADIF)/DENOM
+
+      END
diff --git a/src/slalib/dsep.f b/src/slalib/dsep.f
new file mode 100644
index 0000000..b1bd4be
--- /dev/null
+++ b/src/slalib/dsep.f
@@ -0,0 +1,48 @@
+      DOUBLE PRECISION FUNCTION sla_DSEP (A1, B1, A2, B2)
+*+
+*     - - - - -
+*      D S E P
+*     - - - - -
+*
+*  Angle between two points on a sphere (double precision)
+*
+*  Given:
+*     A1,B1    dp    spherical coordinates of one point
+*     A2,B2    dp    spherical coordinates of the other point
+*
+*  (The spherical coordinates are RA,Dec, Long,Lat etc, in radians.)
+*
+*  The result is the angle, in radians, between the two points.  It
+*  is always positive.
+*
+*  Called:  sla_DCS2C
+*
+*  P.T.Wallace   Starlink   April 1985
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION A1,B1,A2,B2
+
+      INTEGER I
+      DOUBLE PRECISION V1(3),V2(3),W
+
+
+
+*  Convert coordinates from spherical to Cartesian
+      CALL sla_DCS2C(A1,B1,V1)
+      CALL sla_DCS2C(A2,B2,V2)
+
+*  Modulus squared of half the difference vector
+      W=0D0
+      DO I=1,3
+         W=W+(V1(I)-V2(I))**2
+      END DO
+      W=W/4D0
+
+*  Angle between the vectors
+      sla_DSEP=2D0*ATAN2(SQRT(W),SQRT(MAX(0D0,1D0-W)))
+
+      END
diff --git a/src/slalib/dt.f b/src/slalib/dt.f
new file mode 100644
index 0000000..d46c7be
--- /dev/null
+++ b/src/slalib/dt.f
@@ -0,0 +1,79 @@
+      DOUBLE PRECISION FUNCTION sla_DT (EPOCH)
+*+
+*     - - -
+*      D T
+*     - - -
+*
+*  Estimate the offset between dynamical time and Universal Time
+*  for a given historical epoch.
+*
+*  Given:
+*     EPOCH       d        (Julian) epoch (e.g. 1850D0)
+*
+*  The result is a rough estimate of ET-UT (after 1984, TT-UT) at
+*  the given epoch, in seconds.
+*
+*  Notes:
+*
+*  1  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.
+*
+*  2  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).
+*
+*  3  The use of double-precision for both argument and result is
+*     purely for compatibility with other SLALIB time routines.
+*
+*  4  The models used are based on a lunar tidal acceleration value
+*     of -26.00 arcsec per century.
+*
+*  Reference:  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.
+*
+*  P.T.Wallace   Starlink   1 March 1995
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION EPOCH
+      DOUBLE PRECISION T,W,S
+
+
+*  Centuries since 1800
+      T=(EPOCH-1800D0)/100D0
+
+*  Select model
+      IF (EPOCH.GE.1708.185161980887D0) THEN
+
+*     Post-1708: use McCarthy & Babcock
+         W=T-0.19D0
+         S=5.156D0+13.3066D0*W*W
+      ELSE IF (EPOCH.GE.979.0258204760233D0) THEN
+
+*     979-1708: use Stephenson & Morrison's 948-1600 model
+         S=25.5D0*T*T
+      ELSE
+
+*     Pre-979: use Stephenson & Morrison's 390 BC to AD 948 model
+         S=1360.0D0+(320D0+44.3D0*T)*T
+      END IF
+
+*  Result
+      sla_DT=S
+
+      END
diff --git a/src/slalib/dtf2d.f b/src/slalib/dtf2d.f
new file mode 100644
index 0000000..4a25ac6
--- /dev/null
+++ b/src/slalib/dtf2d.f
@@ -0,0 +1,55 @@
+      SUBROUTINE sla_DTF2D (IHOUR, IMIN, SEC, DAYS, J)
+*+
+*     - - - - - -
+*      D T F 2 D
+*     - - - - - -
+*
+*  Convert hours, minutes, seconds to days (double precision)
+*
+*  Given:
+*     IHOUR       int       hours
+*     IMIN        int       minutes
+*     SEC         dp        seconds
+*
+*  Returned:
+*     DAYS        dp        interval in days
+*     J           int       status:  0 = OK
+*                                    1 = IHOUR outside range 0-23
+*                                    2 = IMIN outside range 0-59
+*                                    3 = SEC outside range 0-59.999...
+*
+*  Notes:
+*
+*     1)  The result is computed even if any of the range checks fail.
+*
+*     2)  The sign must be dealt with outside this routine.
+*
+*  P.T.Wallace   Starlink   July 1984
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER IHOUR,IMIN
+      DOUBLE PRECISION SEC,DAYS
+      INTEGER J
+
+*  Seconds per day
+      DOUBLE PRECISION D2S
+      PARAMETER (D2S=86400D0)
+
+
+
+*  Preset status
+      J=0
+
+*  Validate sec, min, hour
+      IF (SEC.LT.0D0.OR.SEC.GE.60D0) J=3
+      IF (IMIN.LT.0.OR.IMIN.GT.59) J=2
+      IF (IHOUR.LT.0.OR.IHOUR.GT.23) J=1
+
+*  Compute interval
+      DAYS=(60D0*(60D0*DBLE(IHOUR)+DBLE(IMIN))+SEC)/D2S
+
+      END
diff --git a/src/slalib/dtf2r.f b/src/slalib/dtf2r.f
new file mode 100644
index 0000000..b100889
--- /dev/null
+++ b/src/slalib/dtf2r.f
@@ -0,0 +1,53 @@
+      SUBROUTINE sla_DTF2R (IHOUR, IMIN, SEC, RAD, J)
+*+
+*     - - - - - -
+*      D T F 2 R
+*     - - - - - -
+*
+*  Convert hours, minutes, seconds to radians (double precision)
+*
+*  Given:
+*     IHOUR       int       hours
+*     IMIN        int       minutes
+*     SEC         dp        seconds
+*
+*  Returned:
+*     RAD         dp        angle in radians
+*     J           int       status:  0 = OK
+*                                    1 = IHOUR outside range 0-23
+*                                    2 = IMIN outside range 0-59
+*                                    3 = SEC outside range 0-59.999...
+*
+*  Called:
+*     sla_DTF2D
+*
+*  Notes:
+*
+*     1)  The result is computed even if any of the range checks fail.
+*
+*     2)  The sign must be dealt with outside this routine.
+*
+*  P.T.Wallace   Starlink   July 1984
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER IHOUR,IMIN
+      DOUBLE PRECISION SEC,RAD
+      INTEGER J
+
+      DOUBLE PRECISION TURNS
+
+*  Turns to radians
+      DOUBLE PRECISION T2R
+      PARAMETER (T2R=6.283185307179586476925287D0)
+
+
+
+*  Convert to turns then radians
+      CALL sla_DTF2D(IHOUR,IMIN,SEC,TURNS,J)
+      RAD=T2R*TURNS
+
+      END
diff --git a/src/slalib/dtp2s.f b/src/slalib/dtp2s.f
new file mode 100644
index 0000000..0a67a11
--- /dev/null
+++ b/src/slalib/dtp2s.f
@@ -0,0 +1,42 @@
+      SUBROUTINE sla_DTP2S (XI, ETA, RAZ, DECZ, RA, DEC)
+*+
+*     - - - - - -
+*      D T P 2 S
+*     - - - - - -
+*
+*  Transform tangent plane coordinates into spherical
+*  (double precision)
+*
+*  Given:
+*     XI,ETA      dp   tangent plane rectangular coordinates
+*     RAZ,DECZ    dp   spherical coordinates of tangent point
+*
+*  Returned:
+*     RA,DEC      dp   spherical coordinates (0-2pi,+/-pi/2)
+*
+*  Called:        sla_DRANRM
+*
+*  P.T.Wallace   Starlink   24 July 1995
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION XI,ETA,RAZ,DECZ,RA,DEC
+
+      DOUBLE PRECISION sla_DRANRM
+
+      DOUBLE PRECISION SDECZ,CDECZ,DENOM
+
+
+
+      SDECZ=SIN(DECZ)
+      CDECZ=COS(DECZ)
+
+      DENOM=CDECZ-ETA*SDECZ
+
+      RA=sla_DRANRM(ATAN2(XI,DENOM)+RAZ)
+      DEC=ATAN2(SDECZ+ETA*CDECZ,SQRT(XI*XI+DENOM*DENOM))
+
+      END
diff --git a/src/slalib/dtp2v.f b/src/slalib/dtp2v.f
new file mode 100644
index 0000000..e1795b9
--- /dev/null
+++ b/src/slalib/dtp2v.f
@@ -0,0 +1,56 @@
+      SUBROUTINE sla_DTP2V (XI, ETA, V0, V)
+*+
+*     - - - - - -
+*      D T P 2 V
+*     - - - - - -
+*
+*  Given the tangent-plane coordinates of a star and the direction
+*  cosines of the tangent point, determine the direction cosines
+*  of the star.
+*
+*  (double precision)
+*
+*  Given:
+*     XI,ETA    d       tangent plane coordinates of star
+*     V0        d(3)    direction cosines of tangent point
+*
+*  Returned:
+*     V         d(3)    direction cosines of star
+*
+*  Notes:
+*
+*  1  If vector V0 is not of unit length, the returned vector V will
+*     be wrong.
+*
+*  2  If vector V0 points at a pole, the returned vector V will be
+*     based on the arbitrary assumption that the RA of the tangent
+*     point is zero.
+*
+*  3  This routine is the Cartesian equivalent of the routine sla_DTP2S.
+*
+*  P.T.Wallace   Starlink   11 February 1995
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION XI,ETA,V0(3),V(3)
+
+      DOUBLE PRECISION X,Y,Z,F,R
+
+
+      X=V0(1)
+      Y=V0(2)
+      Z=V0(3)
+      F=SQRT(1D0+XI*XI+ETA*ETA)
+      R=SQRT(X*X+Y*Y)
+      IF (R.EQ.0D0) THEN
+         R=1D-20
+         X=R
+      END IF
+      V(1)=(X-(XI*Y+ETA*X*Z)/R)/F
+      V(2)=(Y+(XI*X-ETA*Y*Z)/R)/F
+      V(3)=(Z+ETA*R)/F
+
+      END
diff --git a/src/slalib/dtps2c.f b/src/slalib/dtps2c.f
new file mode 100644
index 0000000..43e3bad
--- /dev/null
+++ b/src/slalib/dtps2c.f
@@ -0,0 +1,91 @@
+      SUBROUTINE sla_DTPS2C (XI, ETA, RA, DEC, RAZ1, DECZ1,
+     :                                         RAZ2, DECZ2, N)
+*+
+*     - - - - - - -
+*      D T P S 2 C
+*     - - - - - - -
+*
+*  From the tangent plane coordinates of a star of known RA,Dec,
+*  determine the RA,Dec of the tangent point.
+*
+*  (double precision)
+*
+*  Given:
+*     XI,ETA      d    tangent plane rectangular coordinates
+*     RA,DEC      d    spherical coordinates
+*
+*  Returned:
+*     RAZ1,DECZ1  d    spherical coordinates of tangent point, solution 1
+*     RAZ2,DECZ2  d    spherical coordinates of tangent point, solution 2
+*     N           i    number of solutions:
+*                        0 = no solutions returned (note 2)
+*                        1 = only the first solution is useful (note 3)
+*                        2 = both solutions are useful (note 3)
+*
+*  Notes:
+*
+*  1  The RAZ1 and RAZ2 values are returned in the range 0-2pi.
+*
+*  2  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.
+*
+*  3  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.
+*
+*  4  The DECZ1 and DECZ2 values are returned in the range +/-pi, but
+*     in the usual, non-pole-crossing, case, the range is +/-pi/2.
+*
+*  5  This routine is the spherical equivalent of the routine sla_DTPV2C.
+*
+*  Called:  sla_DRANRM
+*
+*  P.T.Wallace   Starlink   5 June 1995
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION XI,ETA,RA,DEC,RAZ1,DECZ1,RAZ2,DECZ2
+      INTEGER N
+
+      DOUBLE PRECISION X2,Y2,SD,CD,SDF,R2,R,S,C
+
+      DOUBLE PRECISION sla_DRANRM
+
+
+      X2=XI*XI
+      Y2=ETA*ETA
+      SD=SIN(DEC)
+      CD=COS(DEC)
+      SDF=SD*SQRT(1D0+X2+Y2)
+      R2=CD*CD*(1D0+Y2)-SD*SD*X2
+      IF (R2.GE.0D0) THEN
+         R=SQRT(R2)
+         S=SDF-ETA*R
+         C=SDF*ETA+R
+         IF (XI.EQ.0D0.AND.R.EQ.0D0) R=1D0
+         RAZ1=sla_DRANRM(RA-ATAN2(XI,R))
+         DECZ1=ATAN2(S,C)
+         R=-R
+         S=SDF-ETA*R
+         C=SDF*ETA+R
+         RAZ2=sla_DRANRM(RA-ATAN2(XI,R))
+         DECZ2=ATAN2(S,C)
+         IF (ABS(SDF).LT.1D0) THEN
+            N=1
+         ELSE
+            N=2
+         END IF
+      ELSE
+         N=0
+      END IF
+
+      END
diff --git a/src/slalib/dtpv2c.f b/src/slalib/dtpv2c.f
new file mode 100644
index 0000000..6ea2c29
--- /dev/null
+++ b/src/slalib/dtpv2c.f
@@ -0,0 +1,83 @@
+      SUBROUTINE sla_DTPV2C (XI, ETA, V, V01, V02, N)
+*+
+*     - - - - - - -
+*      D T P V 2 C
+*     - - - - - - -
+*
+*  Given the tangent-plane coordinates of a star and its direction
+*  cosines, determine the direction cosines of the tangent-point.
+*
+*  (double precision)
+*
+*  Given:
+*     XI,ETA    d       tangent plane coordinates of star
+*     V         d(3)    direction cosines of star
+*
+*  Returned:
+*     V01       d(3)    direction cosines of tangent point, solution 1
+*     V02       d(3)    direction cosines of tangent point, solution 2
+*     N         i       number of solutions:
+*                         0 = no solutions returned (note 2)
+*                         1 = only the first solution is useful (note 3)
+*                         2 = both solutions are useful (note 3)
+*
+*  Notes:
+*
+*  1  The vector V must be of unit length or the result will be wrong.
+*
+*  2  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.
+*
+*  3  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 can be regarded as valid if the vector V02 is interpreted
+*     as the "over-the-pole" case.
+*
+*  4  This routine is the Cartesian equivalent of the routine sla_DTPS2C.
+*
+*  P.T.Wallace   Starlink   5 June 1995
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION XI,ETA,V(3),V01(3),V02(3)
+      INTEGER N
+
+      DOUBLE PRECISION X,Y,Z,RXY2,XI2,ETA2P1,SDF,R2,R,C
+
+
+      X=V(1)
+      Y=V(2)
+      Z=V(3)
+      RXY2=X*X+Y*Y
+      XI2=XI*XI
+      ETA2P1=ETA*ETA+1D0
+      SDF=Z*SQRT(XI2+ETA2P1)
+      R2=RXY2*ETA2P1-Z*Z*XI2
+      IF (R2.GT.0D0) THEN
+         R=SQRT(R2)
+         C=(SDF*ETA+R)/(ETA2P1*SQRT(RXY2*(R2+XI2)))
+         V01(1)=C*(X*R+Y*XI)
+         V01(2)=C*(Y*R-X*XI)
+         V01(3)=(SDF-ETA*R)/ETA2P1
+         R=-R
+         C=(SDF*ETA+R)/(ETA2P1*SQRT(RXY2*(R2+XI2)))
+         V02(1)=C*(X*R+Y*XI)
+         V02(2)=C*(Y*R-X*XI)
+         V02(3)=(SDF-ETA*R)/ETA2P1
+         IF (ABS(SDF).LT.1D0) THEN
+            N=1
+         ELSE
+            N=2
+         END IF
+      ELSE
+         N=0
+      END IF
+
+      END
diff --git a/src/slalib/dtt.f b/src/slalib/dtt.f
new file mode 100644
index 0000000..9d456ef
--- /dev/null
+++ b/src/slalib/dtt.f
@@ -0,0 +1,46 @@
+      DOUBLE PRECISION FUNCTION sla_DTT (UTC)
+*+
+*     - - - -
+*      D T T
+*     - - - -
+*
+*  Increment to be applied to Coordinated Universal Time UTC to give
+*  Terrestrial Time TT (formerly Ephemeris Time ET)
+*
+*  (double precision)
+*
+*  Given:
+*     UTC      d      UTC date as a modified JD (JD-2400000.5)
+*
+*  Result:  TT-UTC in seconds
+*
+*  Notes:
+*
+*  1  The UTC is specified to be a date rather than a time to indicate
+*     that care needs to be taken not to specify an instant which lies
+*     within a leap second.  Though in most cases UTC can include the
+*     fractional part, correct behaviour on the day of a leap second
+*     can only be guaranteed up to the end of the second 23:59:59.
+*
+*  2  Pre 1972 January 1 a fixed value of 10 + ET-TAI is returned.
+*
+*  3  See also the routine sla_DT, which roughly estimates ET-UT for
+*     historical epochs.
+*
+*  Called:  sla_DAT
+*
+*  P.T.Wallace   Starlink   6 December 1994
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION UTC
+
+      DOUBLE PRECISION sla_DAT
+
+
+      sla_DTT=32.184D0+sla_DAT(UTC)
+
+      END
diff --git a/src/slalib/dv2tp.f b/src/slalib/dv2tp.f
new file mode 100644
index 0000000..9bf2c33
--- /dev/null
+++ b/src/slalib/dv2tp.f
@@ -0,0 +1,78 @@
+      SUBROUTINE sla_DV2TP (V, V0, XI, ETA, J)
+*+
+*     - - - - - -
+*      D V 2 T P
+*     - - - - - -
+*
+*  Given the direction cosines of a star and of the tangent point,
+*  determine the star's tangent-plane coordinates.
+*
+*  (double precision)
+*
+*  Given:
+*     V         d(3)    direction cosines of star
+*     V0        d(3)    direction cosines of tangent point
+*
+*  Returned:
+*     XI,ETA    d       tangent plane coordinates of star
+*     J         i       status:   0 = OK
+*                                 1 = error, star too far from axis
+*                                 2 = error, antistar on tangent plane
+*                                 3 = error, antistar too far from axis
+*
+*  Notes:
+*
+*  1  If vector V0 is not of unit length, or if vector V is of zero
+*     length, the results will be wrong.
+*
+*  2  If V0 points at a pole, the returned XI,ETA will be based on the
+*     arbitrary assumption that the RA of the tangent point is zero.
+*
+*  3  This routine is the Cartesian equivalent of the routine sla_DS2TP.
+*
+*  P.T.Wallace   Starlink   27 November 1996
+*
+*  Copyright (C) 1996 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION V(3),V0(3),XI,ETA
+      INTEGER J
+
+      DOUBLE PRECISION X,Y,Z,X0,Y0,Z0,R2,R,W,D
+
+      DOUBLE PRECISION TINY
+      PARAMETER (TINY=1D-6)
+
+
+      X=V(1)
+      Y=V(2)
+      Z=V(3)
+      X0=V0(1)
+      Y0=V0(2)
+      Z0=V0(3)
+      R2=X0*X0+Y0*Y0
+      R=SQRT(R2)
+      IF (R.EQ.0D0) THEN
+         R=1D-20
+         X0=R
+      END IF
+      W=X*X0+Y*Y0
+      D=W+Z*Z0
+      IF (D.GT.TINY) THEN
+         J=0
+      ELSE IF (D.GE.0D0) THEN
+         J=1
+         D=TINY
+      ELSE IF (D.GT.-TINY) THEN
+         J=2
+         D=-TINY
+      ELSE
+         J=3
+      END IF
+      D=D*R
+      XI=(Y*X0-X*Y0)/D
+      ETA=(Z*R2-Z0*W)/D
+
+      END
diff --git a/src/slalib/dvdv.f b/src/slalib/dvdv.f
new file mode 100644
index 0000000..ab3e411
--- /dev/null
+++ b/src/slalib/dvdv.f
@@ -0,0 +1,27 @@
+      DOUBLE PRECISION FUNCTION sla_DVDV (VA, VB)
+*+
+*     - - - - -
+*      D V D V
+*     - - - - -
+*
+*  Scalar product of two 3-vectors  (double precision)
+*
+*  Given:
+*      VA      dp(3)     first vector
+*      VB      dp(3)     second vector
+*
+*  The result is the scalar product VA.VB (double precision)
+*
+*  P.T.Wallace   Starlink   November 1984
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION VA(3),VB(3)
+
+
+      sla_DVDV=VA(1)*VB(1)+VA(2)*VB(2)+VA(3)*VB(3)
+
+      END
diff --git a/src/slalib/dvn.f b/src/slalib/dvn.f
new file mode 100644
index 0000000..37a4a6d
--- /dev/null
+++ b/src/slalib/dvn.f
@@ -0,0 +1,46 @@
+      SUBROUTINE sla_DVN (V, UV, VM)
+*+
+*     - - - -
+*      D V N
+*     - - - -
+*
+*  Normalizes a 3-vector also giving the modulus (double precision)
+*
+*  Given:
+*     V       dp(3)      vector
+*
+*  Returned:
+*     UV      dp(3)      unit vector in direction of V
+*     VM      dp         modulus of V
+*
+*  If the modulus of V is zero, UV is set to zero as well
+*
+*  P.T.Wallace   Starlink   23 November 1995
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION V(3),UV(3),VM
+
+      INTEGER I
+      DOUBLE PRECISION W1,W2
+
+
+*  Modulus
+      W1=0D0
+      DO I=1,3
+         W2=V(I)
+         W1=W1+W2*W2
+      END DO
+      W1=SQRT(W1)
+      VM=W1
+
+*  Normalize the vector
+      IF (W1.LE.0D0) W1=1D0
+      DO I=1,3
+         UV(I)=V(I)/W1
+      END DO
+
+      END
diff --git a/src/slalib/dvxv.f b/src/slalib/dvxv.f
new file mode 100644
index 0000000..389deb4
--- /dev/null
+++ b/src/slalib/dvxv.f
@@ -0,0 +1,39 @@
+      SUBROUTINE sla_DVXV (VA, VB, VC)
+*+
+*     - - - - -
+*      D V X V
+*     - - - - -
+*
+*  Vector product of two 3-vectors  (double precision)
+*
+*  Given:
+*      VA      dp(3)     first vector
+*      VB      dp(3)     second vector
+*
+*  Returned:
+*      VC      dp(3)     vector result
+*
+*  P.T.Wallace   Starlink   March 1986
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION VA(3),VB(3),VC(3)
+
+      DOUBLE PRECISION VW(3)
+      INTEGER I
+
+
+*  Form the vector product VA cross VB
+      VW(1)=VA(2)*VB(3)-VA(3)*VB(2)
+      VW(2)=VA(3)*VB(1)-VA(1)*VB(3)
+      VW(3)=VA(1)*VB(2)-VA(2)*VB(1)
+
+*  Return the result
+      DO I=1,3
+         VC(I)=VW(I)
+      END DO
+
+      END
diff --git a/src/slalib/e2h.f b/src/slalib/e2h.f
new file mode 100644
index 0000000..03e36d3
--- /dev/null
+++ b/src/slalib/e2h.f
@@ -0,0 +1,89 @@
+      SUBROUTINE sla_E2H (HA, DEC, PHI, AZ, EL)
+*+
+*     - - - -
+*      E 2 H
+*     - - - -
+*
+*  Equatorial to horizon coordinates:  HA,Dec to Az,El
+*
+*  (single precision)
+*
+*  Given:
+*     HA      r     hour angle
+*     DEC     r     declination
+*     PHI     r     observatory latitude
+*
+*  Returned:
+*     AZ      r     azimuth
+*     EL      r     elevation
+*
+*  Notes:
+*
+*  1)  All the arguments are angles in radians.
+*
+*  2)  Azimuth is returned in the range 0-2pi;  north is zero,
+*      and east is +pi/2.  Elevation is returned in the range
+*      +/-pi/2.
+*
+*  3)  The latitude must be geodetic.  In critical applications,
+*      corrections for polar motion should be applied.
+*
+*  4)  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.
+*
+*  5)  No range checking of arguments is carried out.
+*
+*  6)  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.
+*
+*  P.T.Wallace   Starlink   9 July 1994
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL HA,DEC,PHI,AZ,EL
+
+      REAL R2PI
+      PARAMETER (R2PI=6.283185307179586476925286766559)
+
+      REAL SH,CH,SD,CD,SP,CP,X,Y,Z,R,A
+
+
+*  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.EQ.0.0) THEN
+         A=0.0
+      ELSE
+         A=ATAN2(Y,X)
+      END IF
+      IF (A.LT.0.0) A=A+R2PI
+      AZ=A
+      EL=ATAN2(Z,R)
+
+      END
diff --git a/src/slalib/earth.f b/src/slalib/earth.f
new file mode 100644
index 0000000..f37ba2e
--- /dev/null
+++ b/src/slalib/earth.f
@@ -0,0 +1,111 @@
+      SUBROUTINE sla_EARTH (IY, ID, FD, PV)
+*+
+*     - - - - - -
+*      E A R T H
+*     - - - - - -
+*
+*  Approximate heliocentric position and velocity of the Earth
+*
+*  Given:
+*     IY       I       year
+*     ID       I       day in year (1 = Jan 1st)
+*     FD       R       fraction of day
+*
+*  Returned:
+*     PV       R(6)    Earth position & velocity vector
+*
+*  Notes:
+*
+*  1  The date and time is TDB (loosely ET) in a Julian calendar
+*     which has been aligned to the ordinary Gregorian
+*     calendar for the interval 1900 March 1 to 2100 February 28.
+*     The year and day can be obtained by calling sla_CALYD or
+*     sla_CLYD.
+*
+*  2  The Earth heliocentric 6-vector is mean equator and equinox
+*     of date.  Position part, PV(1-3), is in AU;  velocity part,
+*     PV(4-6), is in AU/sec.
+*
+*  3  Max/RMS errors 1950-2050:
+*       13/5 E-5 AU = 19200/7600 km in position
+*       47/26 E-10 AU/s = 0.0070/0.0039 km/s in speed
+*
+*  4  More precise results are obtainable with the routine sla_EVP.
+*
+*  P.T.Wallace   Starlink   23 November 1994
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER IY,ID
+      REAL FD,PV(6)
+
+      INTEGER IY4
+      REAL TWOPI,SPEED,REMB,SEMB,YI,YF,T,ELM,GAMMA,EM,ELT,EPS0,
+     :     E,ESQ,V,R,ELMM,COSELT,SINEPS,COSEPS,W1,W2,SELMM,CELMM
+
+      PARAMETER (TWOPI=6.28318530718)
+
+*  Mean orbital speed of Earth, AU/s
+      PARAMETER (SPEED=1.9913E-7)
+
+*  Mean Earth:EMB distance and speed, AU and AU/s
+      PARAMETER (REMB=3.12E-5,SEMB=8.31E-11)
+
+
+
+*  Whole years & fraction of year, and years since J1900.0
+      YI=FLOAT(IY-1900)
+      IY4=MOD(MOD(IY,4)+4,4)
+      YF=(FLOAT(4*(ID-1/(IY4+1))-IY4-2)+4.0*FD)/1461.0
+      T=YI+YF
+
+*  Geometric mean longitude of Sun
+*  (cf 4.881627938+6.283319509911*T MOD 2PI)
+      ELM=MOD(4.881628+TWOPI*YF+0.00013420*T,TWOPI)
+
+*  Mean longitude of perihelion
+      GAMMA=4.908230+3.0005E-4*T
+
+*  Mean anomaly
+      EM=ELM-GAMMA
+
+*  Mean obliquity
+      EPS0=0.40931975-2.27E-6*T
+
+*  Eccentricity
+      E=0.016751-4.2E-7*T
+      ESQ=E*E
+
+*  True anomaly
+      V=EM+2.0*E*SIN(EM)+1.25*ESQ*SIN(2.0*EM)
+
+*  True ecliptic longitude
+      ELT=V+GAMMA
+
+*  True distance
+      R=(1.0-ESQ)/(1.0+E*COS(V))
+
+*  Moon's mean longitude
+      ELMM=MOD(4.72+83.9971*T,TWOPI)
+
+*  Useful functions
+      COSELT=COS(ELT)
+      SINEPS=SIN(EPS0)
+      COSEPS=COS(EPS0)
+      W1=-R*SIN(ELT)
+      W2=-SPEED*(COSELT+E*COS(GAMMA))
+      SELMM=SIN(ELMM)
+      CELMM=COS(ELMM)
+
+*  Earth position and velocity
+      PV(1)=-R*COSELT-REMB*CELMM
+      PV(2)=(W1-REMB*SELMM)*COSEPS
+      PV(3)=W1*SINEPS
+      PV(4)=SPEED*(SIN(ELT)+E*SIN(GAMMA))+SEMB*SELMM
+      PV(5)=(W2-SEMB*CELMM)*COSEPS
+      PV(6)=W2*SINEPS
+
+      END
diff --git a/src/slalib/ecleq.f b/src/slalib/ecleq.f
new file mode 100644
index 0000000..5aa93c9
--- /dev/null
+++ b/src/slalib/ecleq.f
@@ -0,0 +1,55 @@
+      SUBROUTINE sla_ECLEQ (DL, DB, DATE, DR, DD)
+*+
+*     - - - - - -
+*      E C L E Q
+*     - - - - - -
+*
+*  Transformation from ecliptic coordinates to
+*  J2000.0 equatorial coordinates (double precision)
+*
+*  Given:
+*     DL,DB       dp      ecliptic longitude and latitude
+*                           (mean of date, IAU 1980 theory, radians)
+*     DATE        dp      TDB (loosely ET) as Modified Julian Date
+*                                              (JD-2400000.5)
+*  Returned:
+*     DR,DD       dp      J2000.0 mean RA,Dec (radians)
+*
+*  Called:
+*     sla_DCS2C, sla_ECMAT, sla_DIMXV, sla_PREC, sla_EPJ, sla_DCC2S,
+*     sla_DRANRM, sla_DRANGE
+*
+*  P.T.Wallace   Starlink   March 1986
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DL,DB,DATE,DR,DD
+
+      DOUBLE PRECISION sla_EPJ,sla_DRANRM,sla_DRANGE
+
+      DOUBLE PRECISION RMAT(3,3),V1(3),V2(3)
+
+
+
+*  Spherical to Cartesian
+      CALL sla_DCS2C(DL,DB,V1)
+
+*  Ecliptic to equatorial
+      CALL sla_ECMAT(DATE,RMAT)
+      CALL sla_DIMXV(RMAT,V1,V2)
+
+*  Mean of date to J2000
+      CALL sla_PREC(2000D0,sla_EPJ(DATE),RMAT)
+      CALL sla_DIMXV(RMAT,V2,V1)
+
+*  Cartesian to spherical
+      CALL sla_DCC2S(V1,DR,DD)
+
+*  Express in conventional ranges
+      DR=sla_DRANRM(DR)
+      DD=sla_DRANGE(DD)
+
+      END
diff --git a/src/slalib/ecmat.f b/src/slalib/ecmat.f
new file mode 100644
index 0000000..3a1f8d4
--- /dev/null
+++ b/src/slalib/ecmat.f
@@ -0,0 +1,52 @@
+      SUBROUTINE sla_ECMAT (DATE, RMAT)
+*+
+*     - - - - - -
+*      E C M A T
+*     - - - - - -
+*
+*  Form the equatorial to ecliptic rotation matrix - IAU 1980 theory
+*  (double precision)
+*
+*  Given:
+*     DATE     dp         TDB (loosely ET) as Modified Julian Date
+*                                            (JD-2400000.5)
+*  Returned:
+*     RMAT     dp(3,3)    matrix
+*
+*  Reference:
+*     Murray,C.A., Vectorial Astrometry, section 4.3.
+*
+*  Note:
+*    The matrix is in the sense   V(ecl)  =  RMAT * V(equ);  the
+*    equator, equinox and ecliptic are mean of date.
+*
+*  Called:  sla_DEULER
+*
+*  P.T.Wallace   Starlink   23 August 1996
+*
+*  Copyright (C) 1996 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DATE,RMAT(3,3)
+
+*  Arc seconds to radians
+      DOUBLE PRECISION AS2R
+      PARAMETER (AS2R=0.484813681109535994D-5)
+
+      DOUBLE PRECISION T,EPS0
+
+
+
+*  Interval between basic epoch J2000.0 and current epoch (JC)
+      T = (DATE-51544.5D0)/36525D0
+
+*  Mean obliquity
+      EPS0 = AS2R*
+     :   (84381.448D0+(-46.8150D0+(-0.00059D0+0.001813D0*T)*T)*T)
+
+*  Matrix
+      CALL sla_DEULER('X',EPS0,0D0,0D0,RMAT)
+
+      END
diff --git a/src/slalib/ecor.f b/src/slalib/ecor.f
new file mode 100644
index 0000000..b936909
--- /dev/null
+++ b/src/slalib/ecor.f
@@ -0,0 +1,78 @@
+      SUBROUTINE sla_ECOR (RM, DM, IY, ID, FD, RV, TL)
+*+
+*     - - - - -
+*      E C O R
+*     - - - - -
+*
+*  Component of Earth orbit velocity and heliocentric
+*  light time in a given direction (single precision)
+*
+*  Given:
+*     RM,DM    real    mean RA, Dec of date (radians)
+*     IY       int     year
+*     ID       int     day in year (1 = Jan 1st)
+*     FD       real    fraction of day
+*
+*  Returned:
+*     RV       real    component of Earth orbital velocity (km/sec)
+*     TL       real    component of heliocentric light time (sec)
+*
+*  Notes:
+*
+*  1  The date and time is TDB (loosely ET) in a Julian calendar
+*     which has been aligned to the ordinary Gregorian
+*     calendar for the interval 1900 March 1 to 2100 February 28.
+*     The year and day can be obtained by calling sla_CALYD or
+*     sla_CLYD.
+*
+*  2  Sign convention:
+*
+*     The velocity component is +ve when the Earth is receding from
+*     the given point on the sky.  The light time component is +ve
+*     when the Earth lies between the Sun and the given point on
+*     the sky.
+*
+*  3  Accuracy:
+*
+*     The velocity component is usually within 0.004 km/s of the
+*     correct value and is never in error by more than 0.007 km/s.
+*     The error in light time correction is about 0.03s at worst,
+*     but is usually better than 0.01s. For applications requiring
+*     higher accuracy, see the sla_EVP routine.
+*
+*  Called:  sla_EARTH, sla_CS2C, sla_VDV
+*
+*  P.T.Wallace   Starlink   24 November 1994
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL RM,DM
+      INTEGER IY,ID
+      REAL FD,RV,TL
+
+      REAL sla_VDV
+
+      REAL PV(6),V(3),AUKM,AUSEC
+
+*  AU to km and light sec (1985 Almanac)
+      PARAMETER (AUKM=1.4959787066E8,
+     :           AUSEC=499.0047837)
+
+
+
+*  Sun:Earth position & velocity vector
+      CALL sla_EARTH(IY,ID,FD,PV)
+
+*  Star position vector
+      CALL sla_CS2C(RM,DM,V)
+
+*  Velocity component
+      RV=-AUKM*sla_VDV(PV(4),V)
+
+*  Light time component
+      TL=AUSEC*sla_VDV(PV(1),V)
+
+      END
diff --git a/src/slalib/eg50.f b/src/slalib/eg50.f
new file mode 100644
index 0000000..343fc11
--- /dev/null
+++ b/src/slalib/eg50.f
@@ -0,0 +1,90 @@
+      SUBROUTINE sla_EG50 (DR, DD, DL, DB)
+*+
+*     - - - - -
+*      E G 5 0
+*     - - - - -
+*
+*  Transformation from B1950.0 'FK4' equatorial coordinates to
+*  IAU 1958 galactic coordinates (double precision)
+*
+*  Given:
+*     DR,DD       dp       B1950.0 'FK4' RA,Dec
+*
+*  Returned:
+*     DL,DB       dp       galactic longitude and latitude L2,B2
+*
+*  (all arguments are radians)
+*
+*  Called:
+*     sla_DCS2C, sla_DMXV, sla_DCC2S, sla_SUBET, sla_DRANRM, sla_DRANGE
+*
+*  Note:
+*     The equatorial coordinates are B1950.0 'FK4'.  Use the
+*     routine sla_EQGAL if conversion from J2000.0 coordinates
+*     is required.
+*
+*  Reference:
+*     Blaauw et al, Mon.Not.R.Astron.Soc.,121,123 (1960)
+*
+*  P.T.Wallace   Starlink   5 September 1993
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DR,DD,DL,DB
+
+      DOUBLE PRECISION sla_DRANRM,sla_DRANGE
+
+      DOUBLE PRECISION V1(3),V2(3),R,D
+
+*
+*  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 PRECISION RMAT(3,3)
+      DATA RMAT(1,1),RMAT(1,2),RMAT(1,3),
+     :     RMAT(2,1),RMAT(2,2),RMAT(2,3),
+     :     RMAT(3,1),RMAT(3,2),RMAT(3,3) /
+     : -0.066988739415D0,-0.872755765852D0,-0.483538914632D0,
+     : +0.492728466075D0,-0.450346958020D0,+0.744584633283D0,
+     : -0.867600811151D0,-0.188374601723D0,+0.460199784784D0 /
+
+
+
+*  Remove E-terms
+      CALL sla_SUBET(DR,DD,1950D0,R,D)
+
+*  Spherical to Cartesian
+      CALL sla_DCS2C(R,D,V1)
+
+*  Rotate to galactic
+      CALL sla_DMXV(RMAT,V1,V2)
+
+*  Cartesian to spherical
+      CALL sla_DCC2S(V2,DL,DB)
+
+*  Express angles in conventional ranges
+      DL=sla_DRANRM(DL)
+      DB=sla_DRANGE(DB)
+
+      END
diff --git a/src/slalib/el2ue.f b/src/slalib/el2ue.f
new file mode 100644
index 0000000..49f8ed6
--- /dev/null
+++ b/src/slalib/el2ue.f
@@ -0,0 +1,301 @@
+      SUBROUTINE sla_EL2UE (DATE, JFORM, EPOCH, ORBINC, ANODE,
+     :                      PERIH, AORQ, E, AORL, DM,
+     :                      U, JSTAT)
+*+
+*     - - - - - -
+*      E L 2 U E
+*     - - - - - -
+*
+*  Transform conventional osculating orbital elements into "universal" form.
+*
+*  Given:
+*     DATE     d       epoch (TT MJD) of osculation (Note 3)
+*     JFORM    i       choice of element set (1-3, Note 6)
+*     EPOCH    d       epoch (TT MJD) of the elements
+*     ORBINC   d       inclination (radians)
+*     ANODE    d       longitude of the ascending node (radians)
+*     PERIH    d       longitude or argument of perihelion (radians)
+*     AORQ     d       mean distance or perihelion distance (AU)
+*     E        d       eccentricity
+*     AORL     d       mean anomaly or longitude (radians, JFORM=1,2 only)
+*     DM       d       daily motion (radians, JFORM=1 only)
+*
+*  Returned:
+*     U        d(13)   universal orbital elements (Note 1)
+*
+*                (1)   combined mass (M+m)
+*                (2)   total energy of the orbit (alpha)
+*                (3)   reference (osculating) epoch (t0)
+*              (4-6)   position at reference epoch (r0)
+*              (7-9)   velocity at reference epoch (v0)
+*               (10)   heliocentric distance at reference epoch
+*               (11)   r0.v0
+*               (12)   date (t)
+*               (13)   universal eccentric anomaly (psi) of date, approx
+*
+*     JSTAT    i       status:  0 = OK
+*                              -1 = illegal JFORM
+*                              -2 = illegal E
+*                              -3 = illegal AORQ
+*                              -4 = illegal DM
+*                              -5 = numerical error
+*
+*  Called:  sla_UE2PV, sla_PV2UE
+*
+*  Notes
+*
+*  1  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.
+*
+*  2  The companion routine is sla_UE2PV.  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 sla_UE2PV;
+*     for convenience, the two calls are packaged as the routine
+*     sla_PLANEL.  Multiple predictions may be made by again calling the
+*     present routine once, but then calling sla_UE2PV multiple times,
+*     which is faster than multiple calls to sla_PLANEL.
+*
+*  3  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).
+*
+*  4  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.
+*
+*  5  The universal elements returned in the array U are in canonical
+*     units (solar masses, AU and canonical days).
+*
+*  6  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)
+*
+*  7  Unused elements (DM for JFORM=2, AORL and DM for JFORM=3) are
+*     not accessed.
+*
+*  8  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 & Pitkin, Am.J.Phys. 51, 712 (1983).
+*
+*  P.T.Wallace   Starlink   18 February 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DATE
+      INTEGER JFORM
+      DOUBLE PRECISION EPOCH,ORBINC,ANODE,PERIH,AORQ,E,AORL,DM,U(13)
+      INTEGER JSTAT
+
+*  Gaussian gravitational constant (exact)
+      DOUBLE PRECISION GCON
+      PARAMETER (GCON=0.01720209895D0)
+
+*  Sin and cos of J2000 mean obliquity (IAU 1976)
+      DOUBLE PRECISION SE,CE
+      PARAMETER (SE=0.3977771559319137D0,
+     :           CE=0.9174820620691818D0)
+
+      INTEGER J
+
+      DOUBLE PRECISION 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.LT.1.OR.JFORM.GT.3) THEN
+         JSTAT = -1
+         GO TO 9999
+      END IF
+      IF (E.LT.0D0.OR.E.GT.10D0.OR.(E.GE.1D0.AND.JFORM.NE.3)) THEN
+         JSTAT = -2
+         GO TO 9999
+      END IF
+      IF (AORQ.LE.0D0) THEN
+         JSTAT = -3
+         GO TO 9999
+      END IF
+      IF (JFORM.EQ.1.AND.DM.LE.0D0) THEN
+         JSTAT = -4
+         GO TO 9999
+      END IF
+
+*
+*  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.EQ.1) THEN
+         PHT = EPOCH-(AORL-PERIH)/DM
+         ARGPH = PERIH-ANODE
+         Q = AORQ*(1D0-E)
+         W = DM/GCON
+         CM = W*W*AORQ*AORQ*AORQ
+      ELSE IF (JFORM.EQ.2) THEN
+         PHT = EPOCH-AORL*SQRT(AORQ*AORQ*AORQ)/GCON
+         ARGPH = PERIH
+         Q = AORQ*(1D0-E)
+         CM = 1D0
+      ELSE IF (JFORM.EQ.3) THEN
+         PHT = EPOCH
+         ARGPH = PERIH
+         Q = AORQ
+         CM = 1D0
+      END IF
+
+*  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-1D0)/Q
+
+*  Speed at perihelion.
+
+      PHS = SQRT(ALPHA+2D0*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/GCON).
+
+      DT = (DATE-PHT)*GCON
+
+*  First Approximation to the Universal Eccentric Anomaly, PSI,
+*  based on the circle (FC) and parabola (FP) values.
+
+      FC = DT/Q
+      W = (3D0*DT+SQRT(9D0*DT*DT+8D0*Q*Q*Q))**(1D0/3D0)
+      FP = W-2D0*Q/W
+      PSI = (1D0-E)*FC+E*FP
+
+*  Assemble local copy of element set.
+      UL(1) = CM
+      UL(2) = ALPHA
+      UL(3) = PHT
+      UL(4) = PX
+      UL(5) = PY
+      UL(6) = PZ
+      UL(7) = VX
+      UL(8) = VY
+      UL(9) = VZ
+      UL(10) = Q
+      UL(11) = 0D0
+      UL(12) = DATE
+      UL(13) = PSI
+
+*  Predict position+velocity at epoch of osculation.
+      CALL sla_UE2PV(DATE,UL,PV,J)
+      IF (J.NE.0) GO TO 9010
+
+*  Convert back to universal elements.
+      CALL sla_PV2UE(PV,DATE,CM-1D0,U,J)
+      IF (J.NE.0) GO TO 9010
+
+*  OK exit.
+      JSTAT = 0
+      GO TO 9999
+
+*  Quasi-impossible numerical errors.
+ 9010 CONTINUE
+      JSTAT = -5
+
+ 9999 CONTINUE
+      END
diff --git a/src/slalib/epb.f b/src/slalib/epb.f
new file mode 100644
index 0000000..4cc4d49
--- /dev/null
+++ b/src/slalib/epb.f
@@ -0,0 +1,30 @@
+      DOUBLE PRECISION FUNCTION sla_EPB (DATE)
+*+
+*     - - - -
+*      E P B
+*     - - - -
+*
+*  Conversion of Modified Julian Date to Besselian Epoch
+*  (double precision)
+*
+*  Given:
+*     DATE     dp       Modified Julian Date (JD - 2400000.5)
+*
+*  The result is the Besselian Epoch.
+*
+*  Reference:
+*     Lieske,J.H., 1979. Astron.Astrophys.,73,282.
+*
+*  P.T.Wallace   Starlink   February 1984
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DATE
+
+
+      sla_EPB = 1900D0 + (DATE-15019.81352D0)/365.242198781D0
+
+      END
diff --git a/src/slalib/epb2d.f b/src/slalib/epb2d.f
new file mode 100644
index 0000000..cb1be4f
--- /dev/null
+++ b/src/slalib/epb2d.f
@@ -0,0 +1,30 @@
+      DOUBLE PRECISION FUNCTION sla_EPB2D (EPB)
+*+
+*     - - - - - -
+*      E P B 2 D
+*     - - - - - -
+*
+*  Conversion of Besselian Epoch to Modified Julian Date
+*  (double precision)
+*
+*  Given:
+*     EPB      dp       Besselian Epoch
+*
+*  The result is the Modified Julian Date (JD - 2400000.5).
+*
+*  Reference:
+*     Lieske,J.H., 1979. Astron.Astrophys.,73,282.
+*
+*  P.T.Wallace   Starlink   February 1984
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION EPB
+
+
+      sla_EPB2D = 15019.81352D0 + (EPB-1900D0)*365.242198781D0
+
+      END
diff --git a/src/slalib/epco.f b/src/slalib/epco.f
new file mode 100644
index 0000000..ef642ca
--- /dev/null
+++ b/src/slalib/epco.f
@@ -0,0 +1,51 @@
+      DOUBLE PRECISION FUNCTION sla_EPCO (K0, K, E)
+*+
+*     - - - - -
+*      E P C O
+*     - - - - -
+*
+*  Convert an epoch into the appropriate form - 'B' or 'J'
+*
+*  Given:
+*     K0    char    form of result:  'B'=Besselian, 'J'=Julian
+*     K     char    form of given epoch:  'B' or 'J'
+*     E     dp      epoch
+*
+*  Called:  sla_EPB, sla_EPJ2D, sla_EPJ, sla_EPB2D
+*
+*  Notes:
+*
+*     1) 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.
+*
+*     2) K0 and K 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.
+*
+*        Note that K0 and K won't match if their cases differ.
+*
+*  P.T.Wallace   Starlink   5 September 1993
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      CHARACTER*(*) K0,K
+      DOUBLE PRECISION E
+      DOUBLE PRECISION sla_EPB,sla_EPJ2D,sla_EPJ,sla_EPB2D
+
+
+      IF (K.EQ.K0) THEN
+         sla_EPCO=E
+      ELSE IF (K0.EQ.'B'.OR.K0.EQ.'b') THEN
+         sla_EPCO=sla_EPB(sla_EPJ2D(E))
+      ELSE
+         sla_EPCO=sla_EPJ(sla_EPB2D(E))
+      END IF
+
+      END
diff --git a/src/slalib/epj.f b/src/slalib/epj.f
new file mode 100644
index 0000000..66d5eb9
--- /dev/null
+++ b/src/slalib/epj.f
@@ -0,0 +1,29 @@
+      DOUBLE PRECISION FUNCTION sla_EPJ (DATE)
+*+
+*     - - - -
+*      E P J
+*     - - - -
+*
+*  Conversion of Modified Julian Date to Julian Epoch (double precision)
+*
+*  Given:
+*     DATE     dp       Modified Julian Date (JD - 2400000.5)
+*
+*  The result is the Julian Epoch.
+*
+*  Reference:
+*     Lieske,J.H., 1979. Astron.Astrophys.,73,282.
+*
+*  P.T.Wallace   Starlink   February 1984
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DATE
+
+
+      sla_EPJ = 2000D0 + (DATE-51544.5D0)/365.25D0
+
+      END
diff --git a/src/slalib/epj2d.f b/src/slalib/epj2d.f
new file mode 100644
index 0000000..c6a5c5f
--- /dev/null
+++ b/src/slalib/epj2d.f
@@ -0,0 +1,29 @@
+      DOUBLE PRECISION FUNCTION sla_EPJ2D (EPJ)
+*+
+*     - - - - - -
+*      E P J 2 D
+*     - - - - - -
+*
+*  Conversion of Julian Epoch to Modified Julian Date (double precision)
+*
+*  Given:
+*     EPJ      dp       Julian Epoch
+*
+*  The result is the Modified Julian Date (JD - 2400000.5).
+*
+*  Reference:
+*     Lieske,J.H., 1979. Astron.Astrophys.,73,282.
+*
+*  P.T.Wallace   Starlink   February 1984
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION EPJ
+
+
+      sla_EPJ2D = 51544.5D0 + (EPJ-2000D0)*365.25D0
+
+      END
diff --git a/src/slalib/eqecl.f b/src/slalib/eqecl.f
new file mode 100644
index 0000000..a3a73f6
--- /dev/null
+++ b/src/slalib/eqecl.f
@@ -0,0 +1,55 @@
+      SUBROUTINE sla_EQECL (DR, DD, DATE, DL, DB)
+*+
+*     - - - - - -
+*      E Q E C L
+*     - - - - - -
+*
+*  Transformation from J2000.0 equatorial coordinates to
+*  ecliptic coordinates (double precision)
+*
+*  Given:
+*     DR,DD       dp      J2000.0 mean RA,Dec (radians)
+*     DATE        dp      TDB (loosely ET) as Modified Julian Date
+*                                              (JD-2400000.5)
+*  Returned:
+*     DL,DB       dp      ecliptic longitude and latitude
+*                         (mean of date, IAU 1980 theory, radians)
+*
+*  Called:
+*     sla_DCS2C, sla_PREC, sla_EPJ, sla_DMXV, sla_ECMAT, sla_DCC2S,
+*     sla_DRANRM, sla_DRANGE
+*
+*  P.T.Wallace   Starlink   March 1986
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DR,DD,DATE,DL,DB
+
+      DOUBLE PRECISION sla_EPJ,sla_DRANRM,sla_DRANGE
+
+      DOUBLE PRECISION RMAT(3,3),V1(3),V2(3)
+
+
+
+*  Spherical to Cartesian
+      CALL sla_DCS2C(DR,DD,V1)
+
+*  Mean J2000 to mean of date
+      CALL sla_PREC(2000D0,sla_EPJ(DATE),RMAT)
+      CALL sla_DMXV(RMAT,V1,V2)
+
+*  Equatorial to ecliptic
+      CALL sla_ECMAT(DATE,RMAT)
+      CALL sla_DMXV(RMAT,V2,V1)
+
+*  Cartesian to spherical
+      CALL sla_DCC2S(V1,DL,DB)
+
+*  Express in conventional ranges
+      DL=sla_DRANRM(DL)
+      DB=sla_DRANGE(DB)
+
+      END
diff --git a/src/slalib/eqeqx.f b/src/slalib/eqeqx.f
new file mode 100644
index 0000000..f811039
--- /dev/null
+++ b/src/slalib/eqeqx.f
@@ -0,0 +1,57 @@
+      DOUBLE PRECISION FUNCTION sla_EQEQX (DATE)
+*+
+*     - - - - - -
+*      E Q E Q X
+*     - - - - - -
+*
+*  Equation of the equinoxes  (IAU 1994, double precision)
+*
+*  Given:
+*     DATE    dp      TDB (loosely ET) as Modified Julian Date
+*                                          (JD-2400000.5)
+*
+*  The result is the equation of the equinoxes (double precision)
+*  in radians:
+*
+*     Greenwich apparent ST = GMST + sla_EQEQX
+*
+*  References:  IAU Resolution C7, Recommendation 3 (1994)
+*               Capitaine, N. & Gontier, A.-M., Astron. Astrophys.,
+*               275, 645-650 (1993)
+*               
+*  Called:  sla_NUTC
+*
+*  Patrick Wallace   Starlink   23 August 1996
+*
+*  Copyright (C) 1996 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DATE
+
+*  Turns to arc seconds and arc seconds to radians
+      DOUBLE PRECISION T2AS,AS2R
+      PARAMETER (T2AS=1296000D0,
+     :           AS2R=0.484813681109535994D-5)
+
+      DOUBLE PRECISION T,OM,DPSI,DEPS,EPS0
+
+
+
+*  Interval between basic epoch J2000.0 and current epoch (JC)
+      T=(DATE-51544.5D0)/36525D0
+
+*  Longitude of the mean ascending node of the lunar orbit on the
+*   ecliptic, measured from the mean equinox of date
+      OM=AS2R*(450160.280D0+(-5D0*T2AS-482890.539D0
+     :         +(7.455D0+0.008D0*T)*T)*T)
+
+*  Nutation
+      CALL sla_NUTC(DATE,DPSI,DEPS,EPS0)
+
+*  Equation of the equinoxes
+      sla_EQEQX=DPSI*COS(EPS0)+AS2R*(0.00264D0*SIN(OM)+
+     :                               0.000063D0*SIN(OM+OM))
+
+      END
diff --git a/src/slalib/eqgal.f b/src/slalib/eqgal.f
new file mode 100644
index 0000000..bb59cc6
--- /dev/null
+++ b/src/slalib/eqgal.f
@@ -0,0 +1,79 @@
+      SUBROUTINE sla_EQGAL (DR, DD, DL, DB)
+*+
+*     - - - - - -
+*      E Q G A L
+*     - - - - - -
+*
+*  Transformation from J2000.0 equatorial coordinates to
+*  IAU 1958 galactic coordinates (double precision)
+*
+*  Given:
+*     DR,DD       dp       J2000.0 RA,Dec
+*
+*  Returned:
+*     DL,DB       dp       galactic longitude and latitude L2,B2
+*
+*  (all arguments are radians)
+*
+*  Called:
+*     sla_DCS2C, sla_DMXV, sla_DCC2S, sla_DRANRM, sla_DRANGE
+*
+*  Note:
+*     The equatorial coordinates are J2000.0.  Use the routine
+*     sla_EG50 if conversion from B1950.0 'FK4' coordinates is
+*     required.
+*
+*  Reference:
+*     Blaauw et al, Mon.Not.R.Astron.Soc.,121,123 (1960)
+*
+*  P.T.Wallace   Starlink   21 September 1998
+*
+*  Copyright (C) 1998 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DR,DD,DL,DB
+
+      DOUBLE PRECISION sla_DRANRM,sla_DRANGE
+
+      DOUBLE PRECISION V1(3),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 PRECISION RMAT(3,3)
+      DATA RMAT(1,1),RMAT(1,2),RMAT(1,3),
+     :     RMAT(2,1),RMAT(2,2),RMAT(2,3),
+     :     RMAT(3,1),RMAT(3,2),RMAT(3,3)/
+     : -0.054875539726D0,-0.873437108010D0,-0.483834985808D0,
+     : +0.494109453312D0,-0.444829589425D0,+0.746982251810D0,
+     : -0.867666135858D0,-0.198076386122D0,+0.455983795705D0/
+
+
+
+*  Spherical to Cartesian
+      CALL sla_DCS2C(DR,DD,V1)
+
+*  Equatorial to galactic
+      CALL sla_DMXV(RMAT,V1,V2)
+
+*  Cartesian to spherical
+      CALL sla_DCC2S(V2,DL,DB)
+
+*  Express in conventional ranges
+      DL=sla_DRANRM(DL)
+      DB=sla_DRANGE(DB)
+
+      END
diff --git a/src/slalib/etrms.f b/src/slalib/etrms.f
new file mode 100644
index 0000000..efac204
--- /dev/null
+++ b/src/slalib/etrms.f
@@ -0,0 +1,62 @@
+      SUBROUTINE sla_ETRMS (EP, EV)
+*+
+*     - - - - - -
+*      E T R M S
+*     - - - - - -
+*
+*  Compute the E-terms (elliptic component of annual aberration)
+*  vector (double precision)
+*
+*  Given:
+*     EP      dp      Besselian epoch
+*
+*  Returned:
+*     EV      dp(3)   E-terms as (dx,dy,dz)
+*
+*  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.
+*
+*  References:
+*     1  Smith, C.A. et al., 1989.  Astr.J. 97, 265.
+*     2  Yallop, B.D. et al., 1989.  Astr.J. 97, 274.
+*
+*  P.T.Wallace   Starlink   23 August 1996
+*
+*  Copyright (C) 1996 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION EP,EV(3)
+
+*  Arcseconds to radians
+      DOUBLE PRECISION AS2R
+      PARAMETER (AS2R=0.484813681109535994D-5)
+
+      DOUBLE PRECISION T,E,E0,P,EK,CP
+
+
+
+*  Julian centuries since B1950
+      T=(EP-1950D0)*1.00002135903D-2
+
+*  Eccentricity
+      E=0.01673011D0-(0.00004193D0+0.000000126D0*T)*T
+
+*  Mean obliquity
+      E0=(84404.836D0-(46.8495D0+(0.00319D0+0.00181D0*T)*T)*T)*AS2R
+
+*  Mean longitude of perihelion
+      P=(1015489.951D0+(6190.67D0+(1.65D0+0.012D0*T)*T)*T)*AS2R
+
+*  E-terms
+      EK=E*20.49552D0*AS2R
+      CP=COS(P)
+      EV(1)= EK*SIN(P)
+      EV(2)=-EK*CP*COS(E0)
+      EV(3)=-EK*CP*SIN(E0)
+
+      END
diff --git a/src/slalib/euler.f b/src/slalib/euler.f
new file mode 100644
index 0000000..278da31
--- /dev/null
+++ b/src/slalib/euler.f
@@ -0,0 +1,68 @@
+      SUBROUTINE sla_EULER (ORDER, PHI, THETA, PSI, RMAT)
+*+
+*     - - - - - -
+*      E U L E R
+*     - - - - - -
+*
+*  Form a rotation matrix from the Euler angles - three successive
+*  rotations about specified Cartesian axes (single precision)
+*
+*  Given:
+*    ORDER  c*(*)    specifies about which axes the rotations occur
+*    PHI    r        1st rotation (radians)
+*    THETA  r        2nd rotation (   "   )
+*    PSI    r        3rd rotation (   "   )
+*
+*  Returned:
+*    RMAT   r(3,3)   rotation matrix
+*
+*  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.
+*
+*  Called:  sla_DEULER
+*
+*  P.T.Wallace   Starlink   23 May 1997
+*
+*  Copyright (C) 1997 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      CHARACTER*(*) ORDER
+      REAL PHI,THETA,PSI,RMAT(3,3)
+
+      INTEGER J,I
+      DOUBLE PRECISION W(3,3)
+
+
+
+*  Compute matrix in double precision
+      CALL sla_DEULER(ORDER,DBLE(PHI),DBLE(THETA),DBLE(PSI),W)
+
+*  Copy the result
+      DO J=1,3
+         DO I=1,3
+            RMAT(I,J) = REAL(W(I,J))
+         END DO
+      END DO
+
+      END
diff --git a/src/slalib/evp.f b/src/slalib/evp.f
new file mode 100644
index 0000000..b295a12
--- /dev/null
+++ b/src/slalib/evp.f
@@ -0,0 +1,441 @@
+      SUBROUTINE sla_EVP (DATE, DEQX, DVB, DPB, DVH, DPH)
+*+
+*     - - - -
+*      E V P
+*     - - - -
+*
+*  Barycentric and heliocentric velocity and position of the Earth
+*
+*  All arguments are double precision
+*
+*  Given:
+*
+*     DATE          TDB (loosely ET) as a Modified Julian Date
+*                                         (JD-2400000.5)
+*
+*     DEQX          Julian Epoch (e.g. 2000.0D0) of mean equator and
+*                   equinox of the vectors returned.  If DEQX .LE. 0D0,
+*                   all vectors are referred to the mean equator and
+*                   equinox (FK5) of epoch DATE.
+*
+*  Returned (all 3D Cartesian vectors):
+*
+*     DVB,DPB       barycentric velocity, position
+*
+*     DVH,DPH       heliocentric velocity, position
+*
+*  (Units are AU/s for velocity and AU for position)
+*
+*  Called:  sla_EPJ, sla_PREC
+*
+*  Accuracy:
+*
+*     The maximum deviations from the JPL DE96 ephemeris are as
+*     follows:
+*
+*     barycentric velocity         0.42  m/s
+*     barycentric position         6900  km
+*
+*     heliocentric velocity        0.42  m/s
+*     heliocentric position        1600  km
+*
+*  This routine is adapted from the BARVEL and BARCOR
+*  subroutines of P.Stumpff, which are described in
+*  Astron. Astrophys. Suppl. Ser. 41, 1-8 (1980).  Most of the
+*  changes are merely cosmetic and do not affect the results at
+*  all.  However, some adjustments have been made so as to give
+*  results that refer to the new (IAU 1976 'FK5') equinox
+*  and precession, although the differences these changes make
+*  relative to the results from Stumpff's original 'FK4' version
+*  are smaller than the inherent accuracy of the algorithm.  One
+*  minor shortcoming in the original routines that has NOT been
+*  corrected is that better numerical accuracy could be achieved
+*  if the various polynomial evaluations were nested.  Note also
+*  that one of Stumpff's precession constants differs by 0.001 arcsec
+*  from the value given in the Explanatory Supplement to the A.E.
+*
+*  P.T.Wallace   Starlink   21 March 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DATE,DEQX,DVB(3),DPB(3),DVH(3),DPH(3)
+
+      INTEGER IDEQ,I,J,K
+
+      REAL CC2PI,CCSEC3,CCSGD,CCKM,CCMLD,CCFDI,CCIM,T,TSQ,A,PERTL,
+     :     PERTLD,PERTR,PERTRD,COSA,SINA,ESQ,E,PARAM,TWOE,TWOG,G,
+     :     PHI,F,SINF,COSF,PHID,PSID,PERTP,PERTPD,TL,SINLM,COSLM,
+     :     SIGMA,B,PLON,POMG,PECC,FLATM,FLAT
+
+      DOUBLE PRECISION DC2PI,DS2R,DCSLD,DC1MME,DT,DTSQ,DLOCAL,DML,
+     :                 DEPS,DPARAM,DPSI,D1PDRO,DRD,DRLD,DTL,DSINLS,
+     :                 DCOSLS,DXHD,DYHD,DZHD,DXBD,DYBD,DZBD,DCOSEP,
+     :                 DSINEP,DYAHD,DZAHD,DYABD,DZABD,DR,
+     :                 DXH,DYH,DZH,DXB,DYB,DZB,DYAH,DZAH,DYAB,
+     :                 DZAB,DEPJ,DEQCOR,B1950
+
+      REAL SN(4),CCSEL(3,17),CCAMPS(5,15),CCSEC(3,4),CCAMPM(4,3),
+     :     CCPAMV(4),CCPAM(4),FORBEL(7),SORBEL(17),SINLP(4),COSLP(4)
+      EQUIVALENCE (SORBEL(1),E),(FORBEL(1),G)
+
+      DOUBLE PRECISION DCFEL(3,8),DCEPS(3),DCARGS(2,15),DCARGM(2,3),
+     :                 DPREMA(3,3),W,VW(3)
+
+      DOUBLE PRECISION sla_EPJ
+
+      PARAMETER (DC2PI=6.2831853071796D0,CC2PI=6.283185)
+      PARAMETER (DS2R=0.7272205216643D-4)
+      PARAMETER (B1950=1949.9997904423D0)
+
+*
+*   Constants DCFEL(I,K) of fast changing elements
+*                     I=1                I=2              I=3
+      DATA DCFEL/ 1.7400353D+00, 6.2833195099091D+02, 5.2796D-06,
+     :            6.2565836D+00, 6.2830194572674D+02,-2.6180D-06,
+     :            4.7199666D+00, 8.3997091449254D+03,-1.9780D-05,
+     :            1.9636505D-01, 8.4334662911720D+03,-5.6044D-05,
+     :            4.1547339D+00, 5.2993466764997D+01, 5.8845D-06,
+     :            4.6524223D+00, 2.1354275911213D+01, 5.6797D-06,
+     :            4.2620486D+00, 7.5025342197656D+00, 5.5317D-06,
+     :            1.4740694D+00, 3.8377331909193D+00, 5.6093D-06/
+
+*
+*   Constants DCEPS and CCSEL(I,K) of slowly changing elements
+*                      I=1           I=2           I=3
+      DATA DCEPS/  4.093198D-01,-2.271110D-04,-2.860401D-08 /
+      DATA CCSEL/  1.675104E-02,-4.179579E-05,-1.260516E-07,
+     :             2.220221E-01, 2.809917E-02, 1.852532E-05,
+     :             1.589963E+00, 3.418075E-02, 1.430200E-05,
+     :             2.994089E+00, 2.590824E-02, 4.155840E-06,
+     :             8.155457E-01, 2.486352E-02, 6.836840E-06,
+     :             1.735614E+00, 1.763719E-02, 6.370440E-06,
+     :             1.968564E+00, 1.524020E-02,-2.517152E-06,
+     :             1.282417E+00, 8.703393E-03, 2.289292E-05,
+     :             2.280820E+00, 1.918010E-02, 4.484520E-06,
+     :             4.833473E-02, 1.641773E-04,-4.654200E-07,
+     :             5.589232E-02,-3.455092E-04,-7.388560E-07,
+     :             4.634443E-02,-2.658234E-05, 7.757000E-08,
+     :             8.997041E-03, 6.329728E-06,-1.939256E-09,
+     :             2.284178E-02,-9.941590E-05, 6.787400E-08,
+     :             4.350267E-02,-6.839749E-05,-2.714956E-07,
+     :             1.348204E-02, 1.091504E-05, 6.903760E-07,
+     :             3.106570E-02,-1.665665E-04,-1.590188E-07/
+
+*
+*   Constants of the arguments of the short-period perturbations
+*   by the planets:   DCARGS(I,K)
+*                       I=1               I=2
+      DATA DCARGS/ 5.0974222D+00,-7.8604195454652D+02,
+     :             3.9584962D+00,-5.7533848094674D+02,
+     :             1.6338070D+00,-1.1506769618935D+03,
+     :             2.5487111D+00,-3.9302097727326D+02,
+     :             4.9255514D+00,-5.8849265665348D+02,
+     :             1.3363463D+00,-5.5076098609303D+02,
+     :             1.6072053D+00,-5.2237501616674D+02,
+     :             1.3629480D+00,-1.1790629318198D+03,
+     :             5.5657014D+00,-1.0977134971135D+03,
+     :             5.0708205D+00,-1.5774000881978D+02,
+     :             3.9318944D+00, 5.2963464780000D+01,
+     :             4.8989497D+00, 3.9809289073258D+01,
+     :             1.3097446D+00, 7.7540959633708D+01,
+     :             3.5147141D+00, 7.9618578146517D+01,
+     :             3.5413158D+00,-5.4868336758022D+02/
+
+*
+*   Amplitudes CCAMPS(N,K) of the short-period perturbations
+*           N=1          N=2          N=3          N=4          N=5
+      DATA CCAMPS/
+     : -2.279594E-5, 1.407414E-5, 8.273188E-6, 1.340565E-5,-2.490817E-7,
+     : -3.494537E-5, 2.860401E-7, 1.289448E-7, 1.627237E-5,-1.823138E-7,
+     :  6.593466E-7, 1.322572E-5, 9.258695E-6,-4.674248E-7,-3.646275E-7,
+     :  1.140767E-5,-2.049792E-5,-4.747930E-6,-2.638763E-6,-1.245408E-7,
+     :  9.516893E-6,-2.748894E-6,-1.319381E-6,-4.549908E-6,-1.864821E-7,
+     :  7.310990E-6,-1.924710E-6,-8.772849E-7,-3.334143E-6,-1.745256E-7,
+     : -2.603449E-6, 7.359472E-6, 3.168357E-6, 1.119056E-6,-1.655307E-7,
+     : -3.228859E-6, 1.308997E-7, 1.013137E-7, 2.403899E-6,-3.736225E-7,
+     :  3.442177E-7, 2.671323E-6, 1.832858E-6,-2.394688E-7,-3.478444E-7,
+     :  8.702406E-6,-8.421214E-6,-1.372341E-6,-1.455234E-6,-4.998479E-8,
+     : -1.488378E-6,-1.251789E-5, 5.226868E-7,-2.049301E-7, 0.0E0,
+     : -8.043059E-6,-2.991300E-6, 1.473654E-7,-3.154542E-7, 0.0E0,
+     :  3.699128E-6,-3.316126E-6, 2.901257E-7, 3.407826E-7, 0.0E0,
+     :  2.550120E-6,-1.241123E-6, 9.901116E-8, 2.210482E-7, 0.0E0,
+     : -6.351059E-7, 2.341650E-6, 1.061492E-6, 2.878231E-7, 0.0E0/
+
+*
+*   Constants of the secular perturbations in longitude
+*   CCSEC3 and CCSEC(N,K)
+*                      N=1           N=2           N=3
+      DATA CCSEC3/-7.757020E-08/,
+     :     CCSEC/  1.289600E-06, 5.550147E-01, 2.076942E+00,
+     :             3.102810E-05, 4.035027E+00, 3.525565E-01,
+     :             9.124190E-06, 9.990265E-01, 2.622706E+00,
+     :             9.793240E-07, 5.508259E+00, 1.559103E+01/
+
+*   Sidereal rate DCSLD in longitude, rate CCSGD in mean anomaly
+      DATA DCSLD/1.990987D-07/,
+     :     CCSGD/1.990969E-07/
+
+*   Some constants used in the calculation of the lunar contribution
+      DATA CCKM/3.122140E-05/,
+     :     CCMLD/2.661699E-06/,
+     :     CCFDI/2.399485E-07/
+
+*
+*   Constants DCARGM(I,K) of the arguments of the perturbations
+*   of the motion of the Moon
+*                       I=1               I=2
+      DATA DCARGM/  5.1679830D+00, 8.3286911095275D+03,
+     :              5.4913150D+00,-7.2140632838100D+03,
+     :              5.9598530D+00, 1.5542754389685D+04/
+
+*
+*   Amplitudes CCAMPM(N,K) of the perturbations of the Moon
+*            N=1          N=2           N=3           N=4
+      DATA CCAMPM/
+     :  1.097594E-01, 2.896773E-07, 5.450474E-02, 1.438491E-07,
+     : -2.223581E-02, 5.083103E-08, 1.002548E-02,-2.291823E-08,
+     :  1.148966E-02, 5.658888E-08, 8.249439E-03, 4.063015E-08/
+
+*
+*   CCPAMV(K)=A*M*DL/DT (planets), DC1MME=1-MASS(Earth+Moon)
+      DATA CCPAMV/8.326827E-11,1.843484E-11,1.988712E-12,1.881276E-12/
+      DATA DC1MME/0.99999696D0/
+
+*   CCPAM(K)=A*M(planets), CCIM=INCLINATION(Moon)
+      DATA CCPAM/4.960906E-3,2.727436E-3,8.392311E-4,1.556861E-3/
+      DATA CCIM/8.978749E-2/
+
+
+
+
+*
+*   EXECUTION
+*   ---------
+
+*   Control parameter IDEQ, and time arguments
+      IDEQ = 0
+      IF (DEQX.GT.0D0) IDEQ=1
+      DT = (DATE-15019.5D0)/36525D0
+      T = REAL(DT)
+      DTSQ = DT*DT
+      TSQ = REAL(DTSQ)
+
+*   Values of all elements for the instant DATE
+      DO K=1,8
+         DLOCAL = MOD(DCFEL(1,K)+DT*DCFEL(2,K)+DTSQ*DCFEL(3,K), DC2PI)
+         IF (K.EQ.1) THEN
+            DML = DLOCAL
+         ELSE
+            FORBEL(K-1) = REAL(DLOCAL)
+         END IF
+      END DO
+      DEPS = MOD(DCEPS(1)+DT*DCEPS(2)+DTSQ*DCEPS(3), DC2PI)
+      DO K=1,17
+         SORBEL(K) = MOD(CCSEL(1,K)+T*CCSEL(2,K)+TSQ*CCSEL(3,K),
+     :                   CC2PI)
+      END DO
+
+*   Secular perturbations in longitude
+      DO K=1,4
+         A = MOD(CCSEC(2,K)+T*CCSEC(3,K), CC2PI)
+         SN(K) = SIN(A)
+      END DO
+
+*   Periodic perturbations of the EMB (Earth-Moon barycentre)
+      PERTL =  CCSEC(1,1)          *SN(1) +CCSEC(1,2)*SN(2)+
+     :        (CCSEC(1,3)+T*CCSEC3)*SN(3) +CCSEC(1,4)*SN(4)
+      PERTLD = 0.0
+      PERTR = 0.0
+      PERTRD = 0.0
+      DO K=1,15
+         A = SNGL(MOD(DCARGS(1,K)+DT*DCARGS(2,K), DC2PI))
+         COSA = COS(A)
+         SINA = SIN(A)
+         PERTL = PERTL + CCAMPS(1,K)*COSA+CCAMPS(2,K)*SINA
+         PERTR = PERTR + CCAMPS(3,K)*COSA+CCAMPS(4,K)*SINA
+         IF (K.LT.11) THEN
+            PERTLD = PERTLD+
+     :               (CCAMPS(2,K)*COSA-CCAMPS(1,K)*SINA)*CCAMPS(5,K)
+            PERTRD = PERTRD+
+     :               (CCAMPS(4,K)*COSA-CCAMPS(3,K)*SINA)*CCAMPS(5,K)
+         END IF
+      END DO
+
+*   Elliptic part of the motion of the EMB
+      ESQ = E*E
+      DPARAM = 1D0-DBLE(ESQ)
+      PARAM = REAL(DPARAM)
+      TWOE = E+E
+      TWOG = G+G
+      PHI = TWOE*((1.0-ESQ*0.125)*SIN(G)+E*0.625*SIN(TWOG)
+     :          +ESQ*0.54166667*SIN(G+TWOG) )
+      F = G+PHI
+      SINF = SIN(F)
+      COSF = COS(F)
+      DPSI = DPARAM/(1D0+DBLE(E*COSF))
+      PHID = TWOE*CCSGD*((1.0+ESQ*1.5)*COSF+E*(1.25-SINF*SINF*0.5))
+      PSID = CCSGD*E*SINF/SQRT(PARAM)
+
+*   Perturbed heliocentric motion of the EMB
+      D1PDRO = 1D0+DBLE(PERTR)
+      DRD = D1PDRO*(DBLE(PSID)+DPSI*DBLE(PERTRD))
+      DRLD = D1PDRO*DPSI*(DCSLD+DBLE(PHID)+DBLE(PERTLD))
+      DTL = MOD(DML+DBLE(PHI)+DBLE(PERTL), DC2PI)
+      DSINLS = SIN(DTL)
+      DCOSLS = COS(DTL)
+      DXHD = DRD*DCOSLS-DRLD*DSINLS
+      DYHD = DRD*DSINLS+DRLD*DCOSLS
+
+*   Influence of eccentricity, evection and variation on the
+*   geocentric motion of the Moon
+      PERTL = 0.0
+      PERTLD = 0.0
+      PERTP = 0.0
+      PERTPD = 0.0
+      DO K=1,3
+         A = SNGL(MOD(DCARGM(1,K)+DT*DCARGM(2,K), DC2PI))
+         SINA = SIN(A)
+         COSA = COS(A)
+         PERTL = PERTL +CCAMPM(1,K)*SINA
+         PERTLD = PERTLD+CCAMPM(2,K)*COSA
+         PERTP = PERTP +CCAMPM(3,K)*COSA
+         PERTPD = PERTPD-CCAMPM(4,K)*SINA
+      END DO
+
+*   Heliocentric motion of the Earth
+      TL = FORBEL(2)+PERTL
+      SINLM = SIN(TL)
+      COSLM = COS(TL)
+      SIGMA = CCKM/(1.0+PERTP)
+      A = SIGMA*(CCMLD+PERTLD)
+      B = SIGMA*PERTPD
+      DXHD = DXHD+DBLE(A*SINLM)+DBLE(B*COSLM)
+      DYHD = DYHD-DBLE(A*COSLM)+DBLE(B*SINLM)
+      DZHD =     -DBLE(SIGMA*CCFDI*COS(FORBEL(3)))
+
+*   Barycentric motion of the Earth
+      DXBD = DXHD*DC1MME
+      DYBD = DYHD*DC1MME
+      DZBD = DZHD*DC1MME
+      DO K=1,4
+         PLON = FORBEL(K+3)
+         POMG = SORBEL(K+1)
+         PECC = SORBEL(K+9)
+         TL = MOD(PLON+2.0*PECC*SIN(PLON-POMG), CC2PI)
+         SINLP(K) = SIN(TL)
+         COSLP(K) = COS(TL)
+         DXBD = DXBD+DBLE(CCPAMV(K)*(SINLP(K)+PECC*SIN(POMG)))
+         DYBD = DYBD-DBLE(CCPAMV(K)*(COSLP(K)+PECC*COS(POMG)))
+         DZBD = DZBD-DBLE(CCPAMV(K)*SORBEL(K+13)*COS(PLON-SORBEL(K+5)))
+      END DO
+
+*   Transition to mean equator of date
+      DCOSEP = COS(DEPS)
+      DSINEP = SIN(DEPS)
+      DYAHD = DCOSEP*DYHD-DSINEP*DZHD
+      DZAHD = DSINEP*DYHD+DCOSEP*DZHD
+      DYABD = DCOSEP*DYBD-DSINEP*DZBD
+      DZABD = DSINEP*DYBD+DCOSEP*DZBD
+
+*   Heliocentric coordinates of the Earth
+      DR = DPSI*D1PDRO
+      FLATM = CCIM*SIN(FORBEL(3))
+      A = SIGMA*COS(FLATM)
+      DXH = DR*DCOSLS-DBLE(A*COSLM)
+      DYH = DR*DSINLS-DBLE(A*SINLM)
+      DZH =          -DBLE(SIGMA*SIN(FLATM))
+
+*   Barycentric coordinates of the Earth
+      DXB = DXH*DC1MME
+      DYB = DYH*DC1MME
+      DZB = DZH*DC1MME
+      DO K=1,4
+         FLAT = SORBEL(K+13)*SIN(FORBEL(K+3)-SORBEL(K+5))
+         A = CCPAM(K)*(1.0-SORBEL(K+9)*COS(FORBEL(K+3)-SORBEL(K+1)))
+         B = A*COS(FLAT)
+         DXB = DXB-DBLE(B*COSLP(K))
+         DYB = DYB-DBLE(B*SINLP(K))
+         DZB = DZB-DBLE(A*SIN(FLAT))
+      END DO
+
+*   Transition to mean equator of date
+      DYAH = DCOSEP*DYH-DSINEP*DZH
+      DZAH = DSINEP*DYH+DCOSEP*DZH
+      DYAB = DCOSEP*DYB-DSINEP*DZB
+      DZAB = DSINEP*DYB+DCOSEP*DZB
+
+*   Copy result components into vectors, correcting for FK4 equinox
+      DEPJ=sla_EPJ(DATE)
+      DEQCOR = DS2R*(0.035D0+0.00085D0*(DEPJ-B1950))
+      DVH(1) = DXHD-DEQCOR*DYAHD
+      DVH(2) = DYAHD+DEQCOR*DXHD
+      DVH(3) = DZAHD
+      DVB(1) = DXBD-DEQCOR*DYABD
+      DVB(2) = DYABD+DEQCOR*DXBD
+      DVB(3) = DZABD
+      DPH(1) = DXH-DEQCOR*DYAH
+      DPH(2) = DYAH+DEQCOR*DXH
+      DPH(3) = DZAH
+      DPB(1) = DXB-DEQCOR*DYAB
+      DPB(2) = DYAB+DEQCOR*DXB
+      DPB(3) = DZAB
+
+*   Was precession to another equinox requested?
+      IF (IDEQ.NE.0) THEN
+
+*     Yes: compute precession matrix from MJD DATE to Julian epoch DEQX
+         CALL sla_PREC(DEPJ,DEQX,DPREMA)
+
+*     Rotate DVH
+         DO J=1,3
+            W=0D0
+            DO I=1,3
+               W=W+DPREMA(J,I)*DVH(I)
+            END DO
+            VW(J)=W
+         END DO
+         DO J=1,3
+            DVH(J)=VW(J)
+         END DO
+
+*     Rotate DVB
+         DO J=1,3
+            W=0D0
+            DO I=1,3
+               W=W+DPREMA(J,I)*DVB(I)
+            END DO
+            VW(J)=W
+         END DO
+         DO J=1,3
+            DVB(J)=VW(J)
+         END DO
+
+*     Rotate DPH
+         DO J=1,3
+            W=0D0
+            DO I=1,3
+               W=W+DPREMA(J,I)*DPH(I)
+            END DO
+            VW(J)=W
+         END DO
+         DO J=1,3
+            DPH(J)=VW(J)
+         END DO
+
+*     Rotate DPB
+         DO J=1,3
+            W=0D0
+            DO I=1,3
+               W=W+DPREMA(J,I)*DPB(I)
+            END DO
+            VW(J)=W
+         END DO
+         DO J=1,3
+            DPB(J)=VW(J)
+         END DO
+      END IF
+
+      END
diff --git a/src/slalib/fitxy.f b/src/slalib/fitxy.f
new file mode 100644
index 0000000..97f1e00
--- /dev/null
+++ b/src/slalib/fitxy.f
@@ -0,0 +1,300 @@
+      SUBROUTINE sla_FITXY (ITYPE,NP,XYE,XYM,COEFFS,J)
+*+
+*     - - - - - -
+*      F I T X Y
+*     - - - - - -
+*
+*  Fit a linear model to relate two sets of [X,Y] coordinates.
+*
+*  Given:
+*     ITYPE    i        type of model: 4 or 6 (note 1)
+*     NP       i        number of samples (note 2)
+*     XYE     d(2,np)   expected [X,Y] for each sample
+*     XYM     d(2,np)   measured [X,Y] for each sample
+*
+*  Returned:
+*     COEFFS  d(6)      coefficients of model (note 3)
+*     J        i        status:  0 = OK
+*                               -1 = illegal ITYPE
+*                               -2 = insufficient data
+*                               -3 = singular solution
+*
+*  Notes:
+*
+*  1)  ITYPE, which must be either 4 or 6, selects the type of model
+*      fitted.  Both allowed ITYPE values produce a model COEFFS which
+*      consists of six coefficients, namely the zero points and, for
+*      each of XE and YE, the coefficient of XM and YM.  For ITYPE=6,
+*      all six coefficients are independent, modelling squash and shear
+*      as well as origin, scale, and orientation.  However, ITYPE=4
+*      selects the "solid body rotation" option;  the model COEFFS
+*      still consists of the same six coefficients, but now two of
+*      them are used twice (appropriately signed).  Origin, scale
+*      and orientation are still modelled, but not squash or shear -
+*      the units of X and Y have to be the same.
+*
+*  2)  For NC=4, NP must be at least 2.  For NC=6, NP must be at
+*      least 3.
+*
+*  3)  The model is returned in the array COEFFS.  Naming the
+*      elements of COEFFS as follows:
+*
+*                  COEFFS(1) = A
+*                  COEFFS(2) = B
+*                  COEFFS(3) = C
+*                  COEFFS(4) = D
+*                  COEFFS(5) = E
+*                  COEFFS(6) = F
+*
+*      the model is:
+*
+*            XE = A + B*XM + C*YM
+*            YE = D + E*XM + F*YM
+*
+*      For the "solid body rotation" option (ITYPE=4), the
+*      magnitudes of B and F, and of C and E, are equal.  The
+*      signs of these coefficients depend on whether there is a
+*      sign reversal between XE,YE and XM,YM;  fits are performed
+*      with and without a sign reversal and the best one chosen.
+*
+*  4)  Error status values J=-1 and -2 leave COEFFS unchanged;
+*      if J=-3 COEFFS may have been changed.
+*
+*  See also sla_PXY, sla_INVF, sla_XY2XY, sla_DCMPF
+*
+*  Called:  sla_DMAT, sla_DMXV
+*
+*  P.T.Wallace   Starlink   11 February 1991
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER ITYPE,NP
+      DOUBLE PRECISION XYE(2,NP),XYM(2,NP),COEFFS(6)
+      INTEGER J
+
+      INTEGER I,JSTAT,IW(4),NSOL
+      DOUBLE PRECISION P,SXE,SXEXM,SXEYM,SYE,SYEYM,SYEXM,SXM,
+     :                 SYM,SXMXM,SXMYM,SYMYM,XE,YE,
+     :                 XM,YM,V(4),DM3(3,3),DM4(4,4),DET,
+     :                 SGN,SXXYY,SXYYX,SX2Y2,A,B,C,D,
+     :                 SDR2,XR,YR,AOLD,BOLD,COLD,DOLD,SOLD
+
+
+
+*  Preset the status
+      J=0
+
+*  Float the number of samples
+      P=DBLE(NP)
+
+*  Check ITYPE
+      IF (ITYPE.EQ.6) THEN
+
+*
+*     Six-coefficient linear model
+*     ----------------------------
+
+*     Check enough samples
+         IF (NP.GE.3) THEN
+
+*     Form summations
+         SXE=0D0
+         SXEXM=0D0
+         SXEYM=0D0
+         SYE=0D0
+         SYEYM=0D0
+         SYEXM=0D0
+         SXM=0D0
+         SYM=0D0
+         SXMXM=0D0
+         SXMYM=0D0
+         SYMYM=0D0
+         DO I=1,NP
+            XE=XYE(1,I)
+            YE=XYE(2,I)
+            XM=XYM(1,I)
+            YM=XYM(2,I)
+            SXE=SXE+XE
+            SXEXM=SXEXM+XE*XM
+            SXEYM=SXEYM+XE*YM
+            SYE=SYE+YE
+            SYEYM=SYEYM+YE*YM
+            SYEXM=SYEXM+YE*XM
+            SXM=SXM+XM
+            SYM=SYM+YM
+            SXMXM=SXMXM+XM*XM
+            SXMYM=SXMYM+XM*YM
+            SYMYM=SYMYM+YM*YM
+         END DO
+
+*        Solve for A,B,C in  XE = A + B*XM + C*YM
+            V(1)=SXE
+            V(2)=SXEXM
+            V(3)=SXEYM
+            DM3(1,1)=P
+            DM3(1,2)=SXM
+            DM3(1,3)=SYM
+            DM3(2,1)=SXM
+            DM3(2,2)=SXMXM
+            DM3(2,3)=SXMYM
+            DM3(3,1)=SYM
+            DM3(3,2)=SXMYM
+            DM3(3,3)=SYMYM
+            CALL sla_DMAT(3,DM3,V,DET,JSTAT,IW)
+            IF (JSTAT.EQ.0) THEN
+               DO I=1,3
+                  COEFFS(I)=V(I)
+               END DO
+
+*           Solve for D,E,F in  YE = D + E*XM + F*YM
+               V(1)=SYE
+               V(2)=SYEXM
+               V(3)=SYEYM
+               CALL sla_DMXV(DM3,V,COEFFS(4))
+
+            ELSE
+
+*           No 6-coefficient solution possible
+               J=-3
+
+            END IF
+
+         ELSE
+
+*        Insufficient data for 6-coefficient fit
+            J=-2
+
+         END IF
+
+      ELSE IF (ITYPE.EQ.4) THEN
+
+*
+*     Four-coefficient solid body rotation model
+*     ------------------------------------------
+
+*     Check enough samples
+         IF (NP.GE.2) THEN
+
+*        Try two solutions, first without then with flip in X
+            DO NSOL=1,2
+               IF (NSOL.EQ.1) THEN
+                  SGN=1D0
+               ELSE
+                  SGN=-1D0
+               END IF
+
+*           Form summations
+               SXE=0D0
+               SXXYY=0D0
+               SXYYX=0D0
+               SYE=0D0
+               SXM=0D0
+               SYM=0D0
+               SX2Y2=0D0
+               DO I=1,NP
+                  XE=XYE(1,I)*SGN
+                  YE=XYE(2,I)
+                  XM=XYM(1,I)
+                  YM=XYM(2,I)
+                  SXE=SXE+XE
+                  SXXYY=SXXYY+XE*XM+YE*YM
+                  SXYYX=SXYYX+XE*YM-YE*XM
+                  SYE=SYE+YE
+                  SXM=SXM+XM
+                  SYM=SYM+YM
+                  SX2Y2=SX2Y2+XM*XM+YM*YM
+               END DO
+
+*
+*           Solve for A,B,C,D in:  +/- XE = A + B*XM - C*YM
+*                                    + YE = D + C*XM + B*YM
+               V(1)=SXE
+               V(2)=SXXYY
+               V(3)=SXYYX
+               V(4)=SYE
+               DM4(1,1)=P
+               DM4(1,2)=SXM
+               DM4(1,3)=-SYM
+               DM4(1,4)=0D0
+               DM4(2,1)=SXM
+               DM4(2,2)=SX2Y2
+               DM4(2,3)=0D0
+               DM4(2,4)=SYM
+               DM4(3,1)=SYM
+               DM4(3,2)=0D0
+               DM4(3,3)=-SX2Y2
+               DM4(3,4)=-SXM
+               DM4(4,1)=0D0
+               DM4(4,2)=SYM
+               DM4(4,3)=SXM
+               DM4(4,4)=P
+               CALL sla_DMAT(4,DM4,V,DET,JSTAT,IW)
+               IF (JSTAT.EQ.0) THEN
+                  A=V(1)
+                  B=V(2)
+                  C=V(3)
+                  D=V(4)
+
+*              Determine sum of radial errors squared
+                  SDR2=0D0
+                  DO I=1,NP
+                     XM=XYM(1,I)
+                     YM=XYM(2,I)
+                     XR=A+B*XM-C*YM-XYE(1,I)*SGN
+                     YR=D+C*XM+B*YM-XYE(2,I)
+                     SDR2=SDR2+XR*XR+YR*YR
+                  END DO
+
+               ELSE
+
+*              Singular: set flag
+                  SDR2=-1D0
+
+               END IF
+
+*           If first pass and non-singular, save variables
+               IF (NSOL.EQ.1.AND.JSTAT.EQ.0) THEN
+                  AOLD=A
+                  BOLD=B
+                  COLD=C
+                  DOLD=D
+                  SOLD=SDR2
+               END IF
+
+            END DO
+
+*        Pick the best of the two solutions
+            IF (SOLD.GE.0D0.AND.(SOLD.LE.SDR2.OR.NP.EQ.2)) THEN
+               COEFFS(1)=AOLD
+               COEFFS(2)=BOLD
+               COEFFS(3)=-COLD
+               COEFFS(4)=DOLD
+               COEFFS(5)=COLD
+               COEFFS(6)=BOLD
+            ELSE IF (JSTAT.EQ.0) THEN
+               COEFFS(1)=-A
+               COEFFS(2)=-B
+               COEFFS(3)=C
+               COEFFS(4)=D
+               COEFFS(5)=C
+               COEFFS(6)=B
+            ELSE
+
+*           No 4-coefficient fit possible
+               J=-3
+            END IF
+         ELSE
+
+*        Insufficient data for 4-coefficient fit
+            J=-2
+         END IF
+      ELSE
+
+*     Illegal ITYPE - not 4 or 6
+         J=-1
+      END IF
+
+      END
diff --git a/src/slalib/fk425.f b/src/slalib/fk425.f
new file mode 100644
index 0000000..9b8465f
--- /dev/null
+++ b/src/slalib/fk425.f
@@ -0,0 +1,249 @@
+      SUBROUTINE sla_FK425 (R1950,D1950,DR1950,DD1950,P1950,V1950,
+     :                      R2000,D2000,DR2000,DD2000,P2000,V2000)
+*+
+*     - - - - - -
+*      F K 4 2 5
+*     - - - - - -
+*
+*  Convert B1950.0 FK4 star data to J2000.0 FK5 (double precision)
+*
+*  This routine converts stars from the old, Bessel-Newcomb, FK4
+*  system to the new, IAU 1976, FK5, Fricke 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.
+*
+*  Given:  (all B1950.0,FK4)
+*     R1950,D1950     dp    B1950.0 RA,Dec (rad)
+*     DR1950,DD1950   dp    B1950.0 proper motions (rad/trop.yr)
+*     P1950           dp    parallax (arcsec)
+*     V1950           dp    radial velocity (km/s, +ve = moving away)
+*
+*  Returned:  (all J2000.0,FK5)
+*     R2000,D2000     dp    J2000.0 RA,Dec (rad)
+*     DR2000,DD2000   dp    J2000.0 proper motions (rad/Jul.yr)
+*     P2000           dp    parallax (arcsec)
+*     V2000           dp    radial velocity (km/s, +ve = moving away)
+*
+*  Notes:
+*
+*  1)  The proper motions in RA are dRA/dt rather than
+*      cos(Dec)*dRA/dt, and are per year rather than per century.
+*
+*  2)  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 FK425 is called.
+*
+*  3)  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:
+*
+*     1  Smith, C.A. et al, 1989.  "The transformation of astrometric
+*        catalog systems to the equinox J2000.0".  Astron.J. 97, 265.
+*
+*     2  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.
+*
+*     3  Seidelmann, P.K. (ed), 1992.  "Explanatory Supplement to
+*        the Astronomical Almanac", ISBN 0-935702-68-7.
+*
+*  P.T.Wallace   Starlink   19 December 1993
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION R1950,D1950,DR1950,DD1950,P1950,V1950,
+     :                 R2000,D2000,DR2000,DD2000,P2000,V2000
+
+
+*  Miscellaneous
+      DOUBLE PRECISION R,D,UR,UD,PX,RV,SR,CR,SD,CD,W,WD
+      DOUBLE PRECISION X,Y,Z,XD,YD,ZD
+      DOUBLE PRECISION RXYSQ,RXYZSQ,RXY,RXYZ,SPXY,SPXYZ
+      INTEGER I,J
+
+*  Star position and velocity vectors
+      DOUBLE PRECISION R0(3),RD0(3)
+
+*  Combined position and velocity vectors
+      DOUBLE PRECISION V1(6),V2(6)
+
+*  2Pi
+      DOUBLE PRECISION D2PI
+      PARAMETER (D2PI=6.283185307179586476925287D0)
+
+*  Radians per year to arcsec per century
+      DOUBLE PRECISION PMF
+      PARAMETER (PMF=100D0*60D0*60D0*360D0/D2PI)
+
+*  Small number to avoid arithmetic problems
+      DOUBLE PRECISION TINY
+      PARAMETER (TINY=1D-30)
+
+
+*
+*  CANONICAL CONSTANTS  (see references)
+*
+
+*  Km per sec to AU per tropical century
+*  = 86400 * 36524.2198782 / 149597870
+      DOUBLE PRECISION VF
+      PARAMETER (VF=21.095D0)
+
+*  Constant vector and matrix (by columns)
+      DOUBLE PRECISION A(3),AD(3),EM(6,6)
+      DATA A,AD/ -1.62557D-6,  -0.31919D-6, -0.13843D-6,
+     :           +1.245D-3,    -1.580D-3,   -0.659D-3/
+
+      DATA (EM(I,1),I=1,6) / +0.9999256782D0,
+     :                       +0.0111820610D0,
+     :                       +0.0048579479D0,
+     :                       -0.000551D0,
+     :                       +0.238514D0,
+     :                       -0.435623D0 /
+
+      DATA (EM(I,2),I=1,6) / -0.0111820611D0,
+     :                       +0.9999374784D0,
+     :                       -0.0000271474D0,
+     :                       -0.238565D0,
+     :                       -0.002667D0,
+     :                       +0.012254D0 /
+
+      DATA (EM(I,3),I=1,6) / -0.0048579477D0,
+     :                       -0.0000271765D0,
+     :                       +0.9999881997D0,
+     :                       +0.435739D0,
+     :                       -0.008541D0,
+     :                       +0.002117D0 /
+
+      DATA (EM(I,4),I=1,6) / +0.00000242395018D0,
+     :                       +0.00000002710663D0,
+     :                       +0.00000001177656D0,
+     :                       +0.99994704D0,
+     :                       +0.01118251D0,
+     :                       +0.00485767D0 /
+
+      DATA (EM(I,5),I=1,6) / -0.00000002710663D0,
+     :                       +0.00000242397878D0,
+     :                       -0.00000000006582D0,
+     :                       -0.01118251D0,
+     :                       +0.99995883D0,
+     :                       -0.00002714D0 /
+
+      DATA (EM(I,6),I=1,6) / -0.00000001177656D0,
+     :                       -0.00000000006587D0,
+     :                       +0.00000242410173D0,
+     :                       -0.00485767D0,
+     :                       -0.00002718D0,
+     :                       +1.00000956D0 /
+
+
+
+*  Pick up B1950 data (units radians and arcsec/TC)
+      R=R1950
+      D=D1950
+      UR=DR1950*PMF
+      UD=DD1950*PMF
+      PX=P1950
+      RV=V1950
+
+*  Spherical to Cartesian
+      SR=SIN(R)
+      CR=COS(R)
+      SD=SIN(D)
+      CD=COS(D)
+
+      R0(1)=CR*CD
+      R0(2)=SR*CD
+      R0(3)=   SD
+
+      W=VF*RV*PX
+
+      RD0(1)=-SR*CD*UR-CR*SD*UD+W*R0(1)
+      RD0(2)= CR*CD*UR-SR*SD*UD+W*R0(2)
+      RD0(3)=             CD*UD+W*R0(3)
+
+*  Allow for e-terms and express as position+velocity 6-vector
+      W=R0(1)*A(1)+R0(2)*A(2)+R0(3)*A(3)
+      WD=R0(1)*AD(1)+R0(2)*AD(2)+R0(3)*AD(3)
+      DO I=1,3
+         V1(I)=R0(I)-A(I)+W*R0(I)
+         V1(I+3)=RD0(I)-AD(I)+WD*R0(I)
+      END DO
+
+*  Convert position+velocity vector to Fricke system
+      DO I=1,6
+         W=0D0
+         DO J=1,6
+            W=W+EM(I,J)*V1(J)
+         END DO
+         V2(I)=W
+      END DO
+
+*  Revert to spherical coordinates
+      X=V2(1)
+      Y=V2(2)
+      Z=V2(3)
+      XD=V2(4)
+      YD=V2(5)
+      ZD=V2(6)
+
+      RXYSQ=X*X+Y*Y
+      RXYZSQ=RXYSQ+Z*Z
+      RXY=SQRT(RXYSQ)
+      RXYZ=SQRT(RXYZSQ)
+
+      SPXY=X*XD+Y*YD
+      SPXYZ=SPXY+Z*ZD
+
+      IF (X.EQ.0D0.AND.Y.EQ.0D0) THEN
+         R=0D0
+      ELSE
+         R=ATAN2(Y,X)
+         IF (R.LT.0.0D0) R=R+D2PI
+      END IF
+      D=ATAN2(Z,RXY)
+
+      IF (RXY.GT.TINY) THEN
+         UR=(X*YD-Y*XD)/RXYSQ
+         UD=(ZD*RXYSQ-Z*SPXY)/(RXYZSQ*RXY)
+      END IF
+
+      IF (PX.GT.TINY) THEN
+         RV=SPXYZ/(PX*RXYZ*VF)
+         PX=PX/RXYZ
+      END IF
+
+*  Return results
+      R2000=R
+      D2000=D
+      DR2000=UR/PMF
+      DD2000=UD/PMF
+      V2000=RV
+      P2000=PX
+
+      END
diff --git a/src/slalib/fk45z.f b/src/slalib/fk45z.f
new file mode 100644
index 0000000..350251d
--- /dev/null
+++ b/src/slalib/fk45z.f
@@ -0,0 +1,165 @@
+      SUBROUTINE sla_FK45Z (R1950,D1950,BEPOCH,R2000,D2000)
+*+
+*     - - - - - -
+*      F K 4 5 Z
+*     - - - - - -
+*
+*  Convert B1950.0 FK4 star data to J2000.0 FK5 assuming zero
+*  proper motion in the FK5 frame (double precision)
+*
+*  This routine converts stars from the old, Bessel-Newcomb, FK4
+*  system to the new, 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.
+*
+*  Given:
+*     R1950,D1950     dp    B1950.0 FK4 RA,Dec at epoch (rad)
+*     BEPOCH          dp    Besselian epoch (e.g. 1979.3D0)
+*
+*  Returned:
+*     R2000,D2000     dp    J2000.0 FK5 RA,Dec (rad)
+*
+*  Notes:
+*
+*  1)  The epoch BEPOCH is strictly speaking Besselian, but
+*      if a Julian epoch is supplied the result will be
+*      affected only to a negligible extent.
+*
+*  2)  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 FK45Z is called.
+*
+*  3)  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:
+*
+*     1  Aoki,S., et al, 1983.  Astron.Astrophys., 128, 263.
+*
+*     2  Smith, C.A. et al, 1989.  "The transformation of astrometric
+*        catalog systems to the equinox J2000.0".  Astron.J. 97, 265.
+*
+*     3  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.
+*
+*     4  Seidelmann, P.K. (ed), 1992.  "Explanatory Supplement to
+*        the Astronomical Almanac", ISBN 0-935702-68-7.
+*
+*  Called:  sla_DCS2C, sla_EPJ, sla_EPB2D, sla_DCC2S, sla_DRANRM
+*
+*  P.T.Wallace   Starlink   21 September 1998
+*
+*  Copyright (C) 1998 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION R1950,D1950,BEPOCH,R2000,D2000
+
+      DOUBLE PRECISION D2PI
+      PARAMETER (D2PI=6.283185307179586476925287D0)
+
+      DOUBLE PRECISION W
+      INTEGER I,J
+
+*  Position and position+velocity vectors
+      DOUBLE PRECISION R0(3),A1(3),V1(3),V2(6)
+
+*  Radians per year to arcsec per century
+      DOUBLE PRECISION PMF
+      PARAMETER (PMF=100D0*60D0*60D0*360D0/D2PI)
+
+*  Functions
+      DOUBLE PRECISION sla_EPJ,sla_EPB2D,sla_DRANRM
+
+*
+*  CANONICAL CONSTANTS  (see references)
+*
+
+*  Vectors A and Adot, and matrix M (only half of which is needed here)
+      DOUBLE PRECISION A(3),AD(3),EM(6,3)
+      DATA A,AD/ -1.62557D-6,  -0.31919D-6, -0.13843D-6,
+     :           +1.245D-3,    -1.580D-3,   -0.659D-3/
+
+      DATA (EM(I,1),I=1,6) / +0.9999256782D0,
+     :                       +0.0111820610D0,
+     :                       +0.0048579479D0,
+     :                       -0.000551D0,
+     :                       +0.238514D0,
+     :                       -0.435623D0 /
+
+      DATA (EM(I,2),I=1,6) / -0.0111820611D0,
+     :                       +0.9999374784D0,
+     :                       -0.0000271474D0,
+     :                       -0.238565D0,
+     :                       -0.002667D0,
+     :                       +0.012254D0 /
+
+      DATA (EM(I,3),I=1,6) / -0.0048579477D0,
+     :                       -0.0000271765D0,
+     :                       +0.9999881997D0,
+     :                       +0.435739D0,
+     :                       -0.008541D0,
+     :                       +0.002117D0 /
+
+
+
+*  Spherical to Cartesian
+      CALL sla_DCS2C(R1950,D1950,R0)
+
+*  Adjust vector A to give zero proper motion in FK5
+      W=(BEPOCH-1950D0)/PMF
+      DO I=1,3
+         A1(I)=A(I)+W*AD(I)
+      END DO
+
+*  Remove e-terms
+      W=R0(1)*A1(1)+R0(2)*A1(2)+R0(3)*A1(3)
+      DO I=1,3
+         V1(I)=R0(I)-A1(I)+W*R0(I)
+      END DO
+
+*  Convert position vector to Fricke system
+      DO I=1,6
+         W=0D0
+         DO J=1,3
+            W=W+EM(I,J)*V1(J)
+         END DO
+         V2(I)=W
+      END DO
+
+*  Allow for fictitious proper motion in FK4
+      W=(sla_EPJ(sla_EPB2D(BEPOCH))-2000D0)/PMF
+      DO I=1,3
+         V2(I)=V2(I)+W*V2(I+3)
+      END DO
+
+*  Revert to spherical coordinates
+      CALL sla_DCC2S(V2,W,D2000)
+      R2000=sla_DRANRM(W)
+
+      END
diff --git a/src/slalib/fk524.f b/src/slalib/fk524.f
new file mode 100644
index 0000000..1b990dc
--- /dev/null
+++ b/src/slalib/fk524.f
@@ -0,0 +1,257 @@
+      SUBROUTINE sla_FK524 (R2000,D2000,DR2000,DD2000,P2000,V2000,
+     :                      R1950,D1950,DR1950,DD1950,P1950,V1950)
+*+
+*     - - - - - -
+*      F K 5 2 4
+*     - - - - - -
+*
+*  Convert J2000.0 FK5 star data to B1950.0 FK4 (double precision)
+*
+*  This routine converts stars from the new, IAU 1976, FK5, Fricke
+*  system, to the old, 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.
+*
+*  Given:  (all J2000.0,FK5)
+*     R2000,D2000     dp    J2000.0 RA,Dec (rad)
+*     DR2000,DD2000   dp    J2000.0 proper motions (rad/Jul.yr)
+*     P2000           dp    parallax (arcsec)
+*     V2000           dp    radial velocity (km/s, +ve = moving away)
+*
+*  Returned:  (all B1950.0,FK4)
+*     R1950,D1950     dp    B1950.0 RA,Dec (rad)
+*     DR1950,DD1950   dp    B1950.0 proper motions (rad/trop.yr)
+*     P1950           dp    parallax (arcsec)
+*     V1950           dp    radial velocity (km/s, +ve = moving away)
+*
+*  Notes:
+*
+*  1)  The proper motions in RA are dRA/dt rather than
+*      cos(Dec)*dRA/dt, and are per year rather than per century.
+*
+*  2)  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.
+*
+*  3)  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:
+*
+*     1  Smith, C.A. et al, 1989.  "The transformation of astrometric
+*        catalog systems to the equinox J2000.0".  Astron.J. 97, 265.
+*
+*     2  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.
+*
+*     3  Seidelmann, P.K. (ed), 1992.  "Explanatory Supplement to
+*        the Astronomical Almanac", ISBN 0-935702-68-7.
+*
+*  P.T.Wallace   Starlink   19 December 1993
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION R2000,D2000,DR2000,DD2000,P2000,V2000,
+     :                 R1950,D1950,DR1950,DD1950,P1950,V1950
+
+
+*  Miscellaneous
+      DOUBLE PRECISION R,D,UR,UD,PX,RV
+      DOUBLE PRECISION SR,CR,SD,CD,X,Y,Z,W
+      DOUBLE PRECISION V1(6),V2(6)
+      DOUBLE PRECISION XD,YD,ZD
+      DOUBLE PRECISION RXYZ,WD,RXYSQ,RXY
+      INTEGER I,J
+
+*  2Pi
+      DOUBLE PRECISION D2PI
+      PARAMETER (D2PI=6.283185307179586476925287D0)
+
+*  Radians per year to arcsec per century
+      DOUBLE PRECISION PMF
+      PARAMETER (PMF=100D0*60D0*60D0*360D0/D2PI)
+
+*  Small number to avoid arithmetic problems
+      DOUBLE PRECISION TINY
+      PARAMETER (TINY=1D-30)
+
+*
+*  CANONICAL CONSTANTS  (see references)
+*
+
+*  Km per sec to AU per tropical century
+*  = 86400 * 36524.2198782 / 149597870
+      DOUBLE PRECISION VF
+      PARAMETER (VF=21.095D0)
+
+*  Constant vector and matrix (by columns)
+      DOUBLE PRECISION A(6),EMI(6,6)
+      DATA A/ -1.62557D-6,  -0.31919D-6, -0.13843D-6,
+     :        +1.245D-3,    -1.580D-3,   -0.659D-3/
+
+      DATA (EMI(I,1),I=1,6) / +0.9999256795D0,
+     :                        -0.0111814828D0,
+     :                        -0.0048590040D0,
+     :                        -0.000551D0,
+     :                        -0.238560D0,
+     :                        +0.435730D0 /
+
+      DATA (EMI(I,2),I=1,6) / +0.0111814828D0,
+     :                        +0.9999374849D0,
+     :                        -0.0000271557D0,
+     :                        +0.238509D0,
+     :                        -0.002667D0,
+     :                        -0.008541D0 /
+
+      DATA (EMI(I,3),I=1,6) / +0.0048590039D0,
+     :                        -0.0000271771D0,
+     :                        +0.9999881946D0,
+     :                        -0.435614D0,
+     :                        +0.012254D0,
+     :                        +0.002117D0 /
+
+      DATA (EMI(I,4),I=1,6) / -0.00000242389840D0,
+     :                        +0.00000002710544D0,
+     :                        +0.00000001177742D0,
+     :                        +0.99990432D0,
+     :                        -0.01118145D0,
+     :                        -0.00485852D0 /
+
+      DATA (EMI(I,5),I=1,6) / -0.00000002710544D0,
+     :                        -0.00000242392702D0,
+     :                        +0.00000000006585D0,
+     :                        +0.01118145D0,
+     :                        +0.99991613D0,
+     :                        -0.00002716D0 /
+
+      DATA (EMI(I,6),I=1,6) / -0.00000001177742D0,
+     :                        +0.00000000006585D0,
+     :                        -0.00000242404995D0,
+     :                        +0.00485852D0,
+     :                        -0.00002717D0,
+     :                        +0.99996684D0 /
+
+
+
+*  Pick up J2000 data (units radians and arcsec/JC)
+      R=R2000
+      D=D2000
+      UR=DR2000*PMF
+      UD=DD2000*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=VF*RV*PX
+
+      V1(1)=X
+      V1(2)=Y
+      V1(3)=Z
+
+      V1(4)=-UR*Y-CR*SD*UD+W*X
+      V1(5)= UR*X-SR*SD*UD+W*Y
+      V1(6)=         CD*UD+W*Z
+
+*  Convert position+velocity vector to BN system
+      DO I=1,6
+         W=0D0
+         DO J=1,6
+            W=W+EMI(I,J)*V1(J)
+         END DO
+         V2(I)=W
+      END DO
+
+*  Position vector components and magnitude
+      X=V2(1)
+      Y=V2(2)
+      Z=V2(3)
+      RXYZ=SQRT(X*X+Y*Y+Z*Z)
+
+*  Apply E-terms to position
+      W=X*A(1)+Y*A(2)+Z*A(3)
+      X=X+A(1)*RXYZ-W*X
+      Y=Y+A(2)*RXYZ-W*Y
+      Z=Z+A(3)*RXYZ-W*Z
+
+*  Recompute magnitude
+      RXYZ=SQRT(X*X+Y*Y+Z*Z)
+
+*  Apply E-terms to both position and velocity
+      X=V2(1)
+      Y=V2(2)
+      Z=V2(3)
+      W=X*A(1)+Y*A(2)+Z*A(3)
+      WD=X*A(4)+Y*A(5)+Z*A(6)
+      X=X+A(1)*RXYZ-W*X
+      Y=Y+A(2)*RXYZ-W*Y
+      Z=Z+A(3)*RXYZ-W*Z
+      XD=V2(4)+A(4)*RXYZ-WD*X
+      YD=V2(5)+A(5)*RXYZ-WD*Y
+      ZD=V2(6)+A(6)*RXYZ-WD*Z
+
+*  Convert to spherical
+      RXYSQ=X*X+Y*Y
+      RXY=SQRT(RXYSQ)
+
+      IF (X.EQ.0D0.AND.Y.EQ.0D0) THEN
+         R=0D0
+      ELSE
+         R=ATAN2(Y,X)
+         IF (R.LT.0.0D0) R=R+D2PI
+      END IF
+      D=ATAN2(Z,RXY)
+
+      IF (RXY.GT.TINY) THEN
+         UR=(X*YD-Y*XD)/RXYSQ
+         UD=(ZD*RXYSQ-Z*(X*XD+Y*YD))/((RXYSQ+Z*Z)*RXY)
+      END IF
+
+*  Radial velocity and parallax
+      IF (PX.GT.TINY) THEN
+         RV=(X*XD+Y*YD+Z*ZD)/(PX*VF*RXYZ)
+         PX=PX/RXYZ
+      END IF
+
+*  Return results
+      R1950=R
+      D1950=D
+      DR1950=UR/PMF
+      DD1950=UD/PMF
+      P1950=PX
+      V1950=RV
+
+      END
diff --git a/src/slalib/fk52h.f b/src/slalib/fk52h.f
new file mode 100644
index 0000000..c31a8fe
--- /dev/null
+++ b/src/slalib/fk52h.f
@@ -0,0 +1,105 @@
+      SUBROUTINE sla_FK52H (R5,D5,DR5,DD5,RH,DH,DRH,DDH)
+*+
+*     - - - - - -
+*      F K 5 2 H
+*     - - - - - -
+*
+*  Transform FK5 (J2000) star data into the Hipparcos frame.
+*
+*  (double precision)
+*
+*  This routine transforms FK5 star positions and proper motions
+*  into the frame of the Hipparcos catalogue.
+*
+*  Given (all FK5, equinox J2000, epoch J2000):
+*     R5        d      RA (radians)
+*     D5        d      Dec (radians)
+*     DR5       d      proper motion in RA (dRA/dt, rad/Jyear)
+*     DD5       d      proper motion in Dec (dDec/dt, rad/Jyear)
+*
+*  Returned (all Hipparcos, epoch J2000):
+*     RH        d      RA (radians)
+*     DH        d      Dec (radians)
+*     DRH       d      proper motion in RA (dRA/dt, rad/Jyear)
+*     DDH       d      proper motion in Dec (dDec/dt, rad/Jyear)
+*
+*  Called:  sla_DS2C6, sla_DAV2M, sla_DMXV, sla_DVXV, sla_DC62S,
+*           sla_DRANRM
+*
+*  Notes:
+*
+*  1)  The proper motions in RA are dRA/dt rather than
+*      cos(Dec)*dRA/dt, and are per year rather than per century.
+*
+*  2)  The FK5 to Hipparcos transformation consists of a pure
+*      rotation and spin;  zonal errors in the FK5 catalogue are
+*      not taken into account.
+*
+*  3)  The published orientation and spin components are interpreted
+*      as "axial vectors".  An axial vector points at the pole of the
+*      rotation and its length is the amount of rotation in radians.
+*
+*  4)  See also sla_H2FK5, sla_FK5HZ, sla_HFK5Z.
+*
+*  Reference:
+*
+*     M.Feissel & F.Mignard, Astron. Astrophys. 331, L33-L36 (1998).
+*
+*  P.T.Wallace   Starlink   22 June 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION R5,D5,DR5,DD5,RH,DH,DRH,DDH
+
+      DOUBLE PRECISION AS2R
+      PARAMETER (AS2R=0.484813681109535994D-5)
+
+*  FK5 to Hipparcos orientation and spin (radians, radians/year)
+      DOUBLE PRECISION EPX,EPY,EPZ
+      DOUBLE PRECISION OMX,OMY,OMZ
+
+      PARAMETER ( EPX = -19.9D-3 * AS2R,
+     :            EPY =  -9.1D-3 * AS2R,
+     :            EPZ = +22.9D-3 * AS2R )
+
+      PARAMETER ( OMX = -0.30D-3 * AS2R,
+     :            OMY = +0.60D-3 * AS2R,
+     :            OMZ = +0.70D-3 * AS2R )
+
+      DOUBLE PRECISION PV5(6),ORTN(3),R5H(3,3),S5(3),VV(3),PVH(6),W,R,V
+      INTEGER I
+
+      DOUBLE PRECISION sla_DRANRM
+
+
+
+*  FK5 barycentric position/velocity 6-vector (normalized).
+      CALL sla_DS2C6(R5,D5,1D0,DR5,DD5,0D0,PV5)
+
+*  FK5 to Hipparcos orientation matrix.
+      ORTN(1) = EPX
+      ORTN(2) = EPY
+      ORTN(3) = EPZ
+      CALL sla_DAV2M(ORTN,R5H)
+
+*  Hipparcos wrt FK5 spin vector.
+      S5(1) = OMX
+      S5(2) = OMY
+      S5(3) = OMZ
+
+*  Orient & spin the 6-vector into the Hipparcos frame.
+      CALL sla_DMXV(R5H,PV5,PVH)
+      CALL sla_DVXV(PV5,S5,VV)
+      DO I=1,3
+         VV(I) = PV5(I+3)+VV(I)
+      END DO
+      CALL sla_DMXV(R5H,VV,PVH(4))
+
+*  Hipparcos 6-vector to spherical.
+      CALL sla_DC62S(PVH,W,DH,R,DRH,DDH,V)
+      RH = sla_DRANRM(W)
+
+      END
diff --git a/src/slalib/fk54z.f b/src/slalib/fk54z.f
new file mode 100644
index 0000000..4ab564f
--- /dev/null
+++ b/src/slalib/fk54z.f
@@ -0,0 +1,69 @@
+      SUBROUTINE sla_FK54Z (R2000,D2000,BEPOCH,
+     :                      R1950,D1950,DR1950,DD1950)
+*+
+*     - - - - - -
+*      F K 5 4 Z
+*     - - - - - -
+*
+*  Convert a J2000.0 FK5 star position to B1950.0 FK4 assuming
+*  zero proper motion and parallax (double precision)
+*
+*  This routine converts star positions from the new, IAU 1976,
+*  FK5, Fricke system to the old, Bessel-Newcomb, FK4 system.
+*
+*  Given:
+*     R2000,D2000     dp    J2000.0 FK5 RA,Dec (rad)
+*     BEPOCH          dp    Besselian epoch (e.g. 1950D0)
+*
+*  Returned:
+*     R1950,D1950     dp    B1950.0 FK4 RA,Dec (rad) at epoch BEPOCH
+*     DR1950,DD1950   dp    B1950.0 FK4 proper motions (rad/trop.yr)
+*
+*  Notes:
+*
+*  1)  The proper motion in RA is dRA/dt rather than cos(Dec)*dRA/dt.
+*
+*  2)  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 routines before and
+*      after this routine is called.
+*
+*  3)  Unlike in the sla_FK524 routine, the FK5 proper motions, the
+*      parallax and the radial velocity are presumed zero.
+*
+*  4)  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 routine returns those fictitious proper
+*      motions.
+*
+*  5)  The position returned by this routine is in the B1950
+*      reference frame but at Besselian epoch BEPOCH.  For
+*      comparison with catalogues the BEPOCH argument will
+*      frequently be 1950D0.
+*
+*  Called:  sla_FK524, sla_PM
+*
+*  P.T.Wallace   Starlink   10 April 1990
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION R2000,D2000,BEPOCH,
+     :                 R1950,D1950,DR1950,DD1950
+
+      DOUBLE PRECISION R,D,PX,RV
+
+
+
+*  FK5 equinox J2000 (any epoch) to FK4 equinox B1950 epoch B1950
+      CALL sla_FK524(R2000,D2000,0D0,0D0,0D0,0D0,
+     :               R,D,DR1950,DD1950,PX,RV)
+
+*  Fictitious proper motion to epoch BEPOCH
+      CALL sla_PM(R,D,DR1950,DD1950,0D0,0D0,1950D0,BEPOCH,
+     :            R1950,D1950)
+
+      END
diff --git a/src/slalib/fk5hz.f b/src/slalib/fk5hz.f
new file mode 100644
index 0000000..7aa209d
--- /dev/null
+++ b/src/slalib/fk5hz.f
@@ -0,0 +1,107 @@
+      SUBROUTINE sla_FK5HZ (R5,D5,EPOCH,RH,DH)
+*+
+*     - - - - - -
+*      F K 5 H Z
+*     - - - - - -
+*
+*  Transform an FK5 (J2000) star position into the frame of the
+*  Hipparcos catalogue, assuming zero Hipparcos proper motion.
+*
+*  (double precision)
+*
+*  This routine converts a star position from the FK5 system to
+*  the Hipparcos system, in such a way that the Hipparcos proper
+*  motion is zero.  Because such a star has, in general, a non-zero
+*  proper motion in the FK5 system, the routine requires the epoch
+*  at which the position in the FK5 system was determined.
+*
+*  Given:
+*     R5        d      FK5 RA (radians), equinox J2000, epoch EPOCH
+*     D5        d      FK5 Dec (radians), equinox J2000, epoch EPOCH
+*     EPOCH     d      Julian epoch (TDB)
+*
+*  Returned (all Hipparcos):
+*     RH        d      RA (radians)
+*     DH        d      Dec (radians)
+*
+*  Called:  sla_DCS2C, sla_DAV2M, sla_DIMXV, sla_DMXV, sla_DCC2S,
+*           sla_DRANRM
+*
+*  Notes:
+*
+*  1)  The FK5 to Hipparcos transformation consists of a pure
+*      rotation and spin;  zonal errors in the FK5 catalogue are
+*      not taken into account.
+*
+*  2)  The published orientation and spin components are interpreted
+*      as "axial vectors".  An axial vector points at the pole of the
+*      rotation and its length is the amount of rotation in radians.
+*
+*  3)  See also sla_FK52H, sla_H2FK5, sla_HFK5Z.
+*
+*  Reference:
+*
+*     M.Feissel & F.Mignard, Astron. Astrophys. 331, L33-L36 (1998).
+*
+*  P.T.Wallace   Starlink   22 June 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION R5,D5,EPOCH,RH,DH
+
+      DOUBLE PRECISION AS2R
+      PARAMETER (AS2R=0.484813681109535994D-5)
+
+*  FK5 to Hipparcos orientation and spin (radians, radians/year)
+      DOUBLE PRECISION EPX,EPY,EPZ
+      DOUBLE PRECISION OMX,OMY,OMZ
+
+      PARAMETER ( EPX = -19.9D-3 * AS2R,
+     :            EPY =  -9.1D-3 * AS2R,
+     :            EPZ = +22.9D-3 * AS2R )
+
+      PARAMETER ( OMX = -0.30D-3 * AS2R,
+     :            OMY = +0.60D-3 * AS2R,
+     :            OMZ = +0.70D-3 * AS2R )
+
+      DOUBLE PRECISION P5E(3),ORTN(3),R5H(3,3),T,VST(3),RST(3,3),
+     :                 P5(3),PH(3),W
+
+      DOUBLE PRECISION sla_DRANRM
+
+
+
+*  FK5 barycentric position vector.
+      CALL sla_DCS2C(R5,D5,P5E)
+
+*  FK5 to Hipparcos orientation matrix.
+      ORTN(1) = EPX
+      ORTN(2) = EPY
+      ORTN(3) = EPZ
+      CALL sla_DAV2M(ORTN,R5H)
+
+*  Time interval from epoch to J2000.
+      T = 2000D0-EPOCH
+
+*  Axial vector:  accumulated Hipparcos wrt FK5 spin over that interval.
+      VST(1) = OMX*T
+      VST(2) = OMY*T
+      VST(3) = OMZ*T
+
+*  Express the accumulated spin as a rotation matrix.
+      CALL sla_DAV2M(VST,RST)
+
+*  Derotate the vector's FK5 axes back to epoch.
+      CALL sla_DIMXV(RST,P5E,P5)
+
+*  Rotate the vector into the Hipparcos frame.
+      CALL sla_DMXV(R5H,P5,PH)
+
+*  Hipparcos vector to spherical.
+      CALL sla_DCC2S(PH,W,DH)
+      RH = sla_DRANRM(W)
+
+      END
diff --git a/src/slalib/flotin.f b/src/slalib/flotin.f
new file mode 100644
index 0000000..ce90726
--- /dev/null
+++ b/src/slalib/flotin.f
@@ -0,0 +1,128 @@
+      SUBROUTINE sla_FLOTIN (STRING, NSTRT, RESLT, JFLAG)
+*+
+*     - - - - - - -
+*      F L O T I N
+*     - - - - - - -
+*
+*  Convert free-format input into single precision floating point
+*
+*  Given:
+*     STRING     c     string containing number to be decoded
+*     NSTRT      i     pointer to where decoding is to start
+*     RESLT      r     current value of result
+*
+*  Returned:
+*     NSTRT      i      advanced to next number
+*     RESLT      r      result
+*     JFLAG      i      status: -1 = -OK, 0 = +OK, 1 = null, 2 = error
+*
+*  Called:  sla_DFLTIN
+*
+*  Notes:
+*
+*     1     The reason FLOTIN has separate OK status values for +
+*           and - is to enable minus zero to be detected.   This is
+*           of crucial importance when decoding mixed-radix numbers.
+*           For example, an angle expressed as deg, arcmin, arcsec
+*           may have a leading minus sign but a zero degrees field.
+*
+*     2     A TAB is interpreted as a space, and lowercase characters
+*           are interpreted as uppercase.
+*
+*     3     The basic format is the sequence of fields #^.^@#^, where
+*           # is a sign character + or -, ^ means a string of decimal
+*           digits, and @, which indicates an exponent, means D or E.
+*           Various combinations of these fields can be omitted, and
+*           embedded blanks are permissible in certain places.
+*
+*     4     Spaces:
+*
+*             .  Leading spaces are ignored.
+*
+*             .  Embedded spaces are allowed only after +, -, D or E,
+*                and after the decomal point if the first sequence of
+*                digits is absent.
+*
+*             .  Trailing spaces are ignored;  the first signifies
+*                end of decoding and subsequent ones are skipped.
+*
+*     5     Delimiters:
+*
+*             .  Any character other than +,-,0-9,.,D,E or space may be
+*                used to signal the end of the number and terminate
+*                decoding.
+*
+*             .  Comma is recognized by FLOTIN as a special case;  it
+*                is skipped, leaving the pointer on the next character.
+*                See 13, below.
+*
+*     6     Both signs are optional.  The default is +.
+*
+*     7     The mantissa ^.^ defaults to 1.
+*
+*     8     The exponent @#^ defaults to E0.
+*
+*     9     The strings of decimal digits may be of any length.
+*
+*     10    The decimal point is optional for whole numbers.
+*
+*     11    A "null result" occurs when the string of characters being
+*           decoded does not begin with +,-,0-9,.,D or E, or consists
+*           entirely of spaces.  When this condition is detected, JFLAG
+*           is set to 1 and RESLT is left untouched.
+*
+*     12    NSTRT = 1 for the first character in the string.
+*
+*     13    On return from FLOTIN, NSTRT is set ready for the next
+*           decode - following trailing blanks and any comma.  If a
+*           delimiter other than comma is being used, NSTRT must be
+*           incremented before the next call to FLOTIN, otherwise
+*           all subsequent calls will return a null result.
+*
+*     14    Errors (JFLAG=2) occur when:
+*
+*             .  a +, -, D or E is left unsatisfied;  or
+*
+*             .  the decimal point is present without at least
+*                one decimal digit before or after it;  or
+*
+*             .  an exponent more than 100 has been presented.
+*
+*     15    When an error has been detected, NSTRT is left
+*           pointing to the character following the last
+*           one used before the error came to light.  This
+*           may be after the point at which a more sophisticated
+*           program could have detected the error.  For example,
+*           FLOTIN does not detect that '1E999' is unacceptable
+*           (on a computer where this is so) until the entire number
+*           has been decoded.
+*
+*     16    Certain highly unlikely combinations of mantissa &
+*           exponent can cause arithmetic faults during the
+*           decode, in some cases despite the fact that they
+*           together could be construed as a valid number.
+*
+*     17    Decoding is left to right, one pass.
+*
+*     18    See also DFLTIN and INTIN
+*
+*  P.T.Wallace   Starlink   23 November 1995
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      CHARACTER*(*) STRING
+      INTEGER NSTRT
+      REAL RESLT
+      INTEGER JFLAG
+
+      DOUBLE PRECISION DRESLT
+
+
+*  Call the double precision version
+      CALL sla_DFLTIN(STRING,NSTRT,DRESLT,JFLAG)
+      IF (JFLAG.LE.0) RESLT=REAL(DRESLT)
+
+      END
diff --git a/src/slalib/galeq.f b/src/slalib/galeq.f
new file mode 100644
index 0000000..c2c3718
--- /dev/null
+++ b/src/slalib/galeq.f
@@ -0,0 +1,79 @@
+      SUBROUTINE sla_GALEQ (DL, DB, DR, DD)
+*+
+*     - - - - - -
+*      G A L E Q
+*     - - - - - -
+*
+*  Transformation from IAU 1958 galactic coordinates to
+*  J2000.0 equatorial coordinates (double precision)
+*
+*  Given:
+*     DL,DB       dp       galactic longitude and latitude L2,B2
+*
+*  Returned:
+*     DR,DD       dp       J2000.0 RA,Dec
+*
+*  (all arguments are radians)
+*
+*  Called:
+*     sla_DCS2C, sla_DIMXV, sla_DCC2S, sla_DRANRM, sla_DRANGE
+*
+*  Note:
+*     The equatorial coordinates are J2000.0.  Use the routine
+*     sla_GE50 if conversion to B1950.0 'FK4' coordinates is
+*     required.
+*
+*  Reference:
+*     Blaauw et al, Mon.Not.R.Astron.Soc.,121,123 (1960)
+*
+*  P.T.Wallace   Starlink   21 September 1998
+*
+*  Copyright (C) 1998 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DL,DB,DR,DD
+
+      DOUBLE PRECISION sla_DRANRM,sla_DRANGE
+
+      DOUBLE PRECISION V1(3),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 PRECISION RMAT(3,3)
+      DATA RMAT(1,1),RMAT(1,2),RMAT(1,3),
+     :     RMAT(2,1),RMAT(2,2),RMAT(2,3),
+     :     RMAT(3,1),RMAT(3,2),RMAT(3,3)/
+     : -0.054875539726D0,-0.873437108010D0,-0.483834985808D0,
+     : +0.494109453312D0,-0.444829589425D0,+0.746982251810D0,
+     : -0.867666135858D0,-0.198076386122D0,+0.455983795705D0/
+
+
+
+*  Spherical to Cartesian
+      CALL sla_DCS2C(DL,DB,V1)
+
+*  Galactic to equatorial
+      CALL sla_DIMXV(RMAT,V1,V2)
+
+*  Cartesian to spherical
+      CALL sla_DCC2S(V2,DR,DD)
+
+*  Express in conventional ranges
+      DR=sla_DRANRM(DR)
+      DD=sla_DRANGE(DD)
+
+      END
diff --git a/src/slalib/galsup.f b/src/slalib/galsup.f
new file mode 100644
index 0000000..b2520b9
--- /dev/null
+++ b/src/slalib/galsup.f
@@ -0,0 +1,79 @@
+      SUBROUTINE sla_GALSUP (DL, DB, DSL, DSB)
+*+
+*     - - - - - - -
+*      G A L S U P
+*     - - - - - - -
+*
+*  Transformation from IAU 1958 galactic coordinates to
+*  de Vaucouleurs supergalactic coordinates (double precision)
+*
+*  Given:
+*     DL,DB       dp       galactic longitude and latitude L2,B2
+*
+*  Returned:
+*     DSL,DSB     dp       supergalactic longitude and latitude
+*
+*  (all arguments are radians)
+*
+*  Called:
+*     sla_DCS2C, sla_DMXV, sla_DCC2S, sla_DRANRM, sla_DRANGE
+*
+*  References:
+*
+*     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.)
+*
+*  P.T.Wallace   Starlink   25 January 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DL,DB,DSL,DSB
+
+      DOUBLE PRECISION sla_DRANRM,sla_DRANGE
+
+      DOUBLE PRECISION V1(3),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 PRECISION RMAT(3,3)
+      DATA RMAT(1,1),RMAT(1,2),RMAT(1,3),
+     :     RMAT(2,1),RMAT(2,2),RMAT(2,3),
+     :     RMAT(3,1),RMAT(3,2),RMAT(3,3)/
+     : -0.735742574804D0,+0.677261296414D0,+0.000000000000D0,
+     : -0.074553778365D0,-0.080991471307D0,+0.993922590400D0,
+     : +0.673145302109D0,+0.731271165817D0,+0.110081262225D0/
+
+
+
+*  Spherical to Cartesian
+      CALL sla_DCS2C(DL,DB,V1)
+
+*  Galactic to supergalactic
+      CALL sla_DMXV(RMAT,V1,V2)
+
+*  Cartesian to spherical
+      CALL sla_DCC2S(V2,DSL,DSB)
+
+*  Express in conventional ranges
+      DSL=sla_DRANRM(DSL)
+      DSB=sla_DRANGE(DSB)
+
+      END
diff --git a/src/slalib/ge50.f b/src/slalib/ge50.f
new file mode 100644
index 0000000..fed5728
--- /dev/null
+++ b/src/slalib/ge50.f
@@ -0,0 +1,90 @@
+      SUBROUTINE sla_GE50 (DL, DB, DR, DD)
+*+
+*     - - - - -
+*      G E 5 0
+*     - - - - -
+*
+*  Transformation from IAU 1958 galactic coordinates to
+*  B1950.0 'FK4' equatorial coordinates (double precision)
+*
+*  Given:
+*     DL,DB       dp       galactic longitude and latitude L2,B2
+*
+*  Returned:
+*     DR,DD       dp       B1950.0 'FK4' RA,Dec
+*
+*  (all arguments are radians)
+*
+*  Called:
+*     sla_DCS2C, sla_DIMXV, sla_DCC2S, sla_ADDET, sla_DRANRM, sla_DRANGE
+*
+*  Note:
+*     The equatorial coordinates are B1950.0 'FK4'.  Use the
+*     routine sla_GALEQ if conversion to J2000.0 coordinates
+*     is required.
+*
+*  Reference:
+*     Blaauw et al, Mon.Not.R.Astron.Soc.,121,123 (1960)
+*
+*  P.T.Wallace   Starlink   5 September 1993
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DL,DB,DR,DD
+
+      DOUBLE PRECISION sla_DRANRM,sla_DRANGE
+
+      DOUBLE PRECISION V1(3),V2(3),R,D,RE,DE
+
+*
+*  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 PRECISION RMAT(3,3)
+      DATA RMAT(1,1),RMAT(1,2),RMAT(1,3),
+     :     RMAT(2,1),RMAT(2,2),RMAT(2,3),
+     :     RMAT(3,1),RMAT(3,2),RMAT(3,3) /
+     : -0.066988739415D0,-0.872755765852D0,-0.483538914632D0,
+     : +0.492728466075D0,-0.450346958020D0,+0.744584633283D0,
+     : -0.867600811151D0,-0.188374601723D0,+0.460199784784D0 /
+
+
+
+*  Spherical to Cartesian
+      CALL sla_DCS2C(DL,DB,V1)
+
+*  Rotate to mean B1950.0
+      CALL sla_DIMXV(RMAT,V1,V2)
+
+*  Cartesian to spherical
+      CALL sla_DCC2S(V2,R,D)
+
+*  Introduce E-terms
+      CALL sla_ADDET(R,D,1950D0,RE,DE)
+
+*  Express in conventional ranges
+      DR=sla_DRANRM(RE)
+      DD=sla_DRANGE(DE)
+
+      END
diff --git a/src/slalib/geoc.f b/src/slalib/geoc.f
new file mode 100644
index 0000000..89f51b7
--- /dev/null
+++ b/src/slalib/geoc.f
@@ -0,0 +1,57 @@
+      SUBROUTINE sla_GEOC (P, H, R, Z)
+*+
+*     - - - - -
+*      G E O C
+*     - - - - -
+*
+*  Convert geodetic position to geocentric (double precision)
+*
+*  Given:
+*     P     dp     latitude (geodetic, radians)
+*     H     dp     height above reference spheroid (geodetic, metres)
+*
+*  Returned:
+*     R     dp     distance from Earth axis (AU)
+*     Z     dp     distance from plane of Earth equator (AU)
+*
+*  Notes:
+*     1)  Geocentric latitude can be obtained by evaluating ATAN2(Z,R).
+*     2)  IAU 1976 constants are used.
+*
+*  Reference:
+*     Green,R.M., Spherical Astronomy, CUP 1985, p98.
+*
+*  P.T.Wallace   Starlink   4th October 1989
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION P,H,R,Z
+
+*  Earth equatorial radius (metres)
+      DOUBLE PRECISION A0
+      PARAMETER (A0=6378140D0)
+
+*  Reference spheroid flattening factor and useful function
+      DOUBLE PRECISION F,B
+      PARAMETER (F=1D0/298.257D0,B=(1D0-F)**2)
+
+*  Astronomical unit in metres
+      DOUBLE PRECISION AU
+      PARAMETER (AU=1.49597870D11)
+
+      DOUBLE PRECISION SP,CP,C,S
+
+
+
+*  Geodetic to geocentric conversion
+      SP=SIN(P)
+      CP=COS(P)
+      C=1D0/SQRT(CP*CP+B*SP*SP)
+      S=B*C
+      R=(A0*C+H)*CP/AU
+      Z=(A0*S+H)*SP/AU
+
+      END
diff --git a/src/slalib/gmst.f b/src/slalib/gmst.f
new file mode 100644
index 0000000..b115311
--- /dev/null
+++ b/src/slalib/gmst.f
@@ -0,0 +1,60 @@
+      DOUBLE PRECISION FUNCTION sla_GMST (UT1)
+*+
+*     - - - - -
+*      G M S T
+*     - - - - -
+*
+*  Conversion from universal time to sidereal time (double precision)
+*
+*  Given:
+*    UT1    dp     universal time (strictly UT1) expressed as
+*                  modified Julian Date (JD-2400000.5)
+*
+*  The result is the Greenwich mean sidereal time (double
+*  precision, radians).
+*
+*  The IAU 1982 expression (see page S15 of 1984 Astronomical
+*  Almanac) is used, but rearranged to reduce rounding errors.
+*  This expression is always described as giving the GMST at
+*  0 hours UT.  In fact, it gives the difference between the
+*  GMST and the UT, which happens to equal the GMST (modulo
+*  24 hours) at 0 hours UT each day.  In this routine, the
+*  entire UT is used directly as the argument for the
+*  standard formula, and the fractional part of the UT is
+*  added separately;  note that the factor 1.0027379... does
+*  not appear.
+*
+*  See also the routine sla_GMSTA, which delivers better numerical
+*  precision by accepting the UT date and time as separate arguments.
+*
+*  Called:  sla_DRANRM
+*
+*  P.T.Wallace   Starlink   14 September 1995
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION UT1
+
+      DOUBLE PRECISION sla_DRANRM
+
+      DOUBLE PRECISION D2PI,S2R
+      PARAMETER (D2PI=6.283185307179586476925286766559D0,
+     :           S2R=7.272205216643039903848711535369D-5)
+
+      DOUBLE PRECISION TU
+
+
+
+*  Julian centuries from fundamental epoch J2000 to this UT
+      TU=(UT1-51544.5D0)/36525D0
+
+*  GMST at this UT
+      sla_GMST=sla_DRANRM(MOD(UT1,1D0)*D2PI+
+     :                    (24110.54841D0+
+     :                    (8640184.812866D0+
+     :                    (0.093104D0-6.2D-6*TU)*TU)*TU)*S2R)
+
+      END
diff --git a/src/slalib/gmsta.f b/src/slalib/gmsta.f
new file mode 100644
index 0000000..5259f6f
--- /dev/null
+++ b/src/slalib/gmsta.f
@@ -0,0 +1,80 @@
+      DOUBLE PRECISION FUNCTION sla_GMSTA (DATE, UT)
+*+
+*     - - - - - -
+*      G M S T A
+*     - - - - - -
+*
+*  Conversion from Universal Time to Greenwich mean sidereal time,
+*  with rounding errors minimized.
+*
+*  double precision
+*
+*  Given:
+*    DATE    d      UT1 date (MJD: integer part of JD-2400000.5))
+*    UT      d      UT1 time (fraction of a day)
+*
+*  The result is the Greenwich mean sidereal time (double precision,
+*  radians, in the range 0 to 2pi).
+*
+*  There is no restriction on how the UT is apportioned between the
+*  DATE and UT arguments.  Either of the two arguments could, for
+*  example, be zero and the entire date+time supplied in the other.
+*  However, the routine is designed to deliver maximum accuracy when
+*  the DATE argument is a whole number and the UT lies in the range
+*  0 to 1 (or vice versa).
+*
+*  The algorithm is based on the IAU 1982 expression (see page S15 of
+*  the 1984 Astronomical Almanac).  This is always described as giving
+*  the GMST at 0 hours UT1.  In fact, it gives the difference between
+*  the GMST and the UT, the steady 4-minutes-per-day drawing-ahead of
+*  ST with respect to UT.  When whole days are ignored, the expression
+*  happens to equal the GMST at 0 hours UT1 each day.
+*
+*  In this routine, the entire UT1 (the sum of the two arguments DATE
+*  and UT) is used directly as the argument for the standard formula.
+*  The UT1 is then added, but omitting whole days to conserve accuracy.
+*
+*  See also the routine sla_GMST, which accepts the UT as a single
+*  argument.  Compared with sla_GMST, the extra numerical precision
+*  delivered by the present routine is unlikely to be important in
+*  an absolute sense, but may be useful when critically comparing
+*  algorithms and in applications where two sidereal times close
+*  together are differenced.
+*
+*  Called:  sla_DRANRM
+*
+*  P.T.Wallace   Starlink   13 April 1998
+*
+*  Copyright (C) 1998 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DATE,UT
+
+*  Seconds of time to radians
+      DOUBLE PRECISION S2R
+      PARAMETER (S2R=7.272205216643039903848712D-5)
+
+      DOUBLE PRECISION D1,D2,T
+      DOUBLE PRECISION sla_DRANRM
+
+
+*  Julian centuries since J2000.
+      IF (DATE.LT.UT) THEN
+         D1=DATE
+         D2=UT
+      ELSE
+         D1=UT
+         D2=DATE
+      END IF
+      T=(D1+(D2-51544.5D0))/36525D0
+
+*  GMST at this UT1.
+      sla_GMSTA=sla_DRANRM(S2R*(24110.54841D0+
+     :                         (8640184.812866D0+
+     :                         (0.093104D0
+     :                         -6.2D-6*T)*T)*T
+     :                         +86400D0*(MOD(D1,1D0)+MOD(D2,1D0))))
+
+      END
diff --git a/src/slalib/gresid.f_alpha_OSF1 b/src/slalib/gresid.f_alpha_OSF1
new file mode 100644
index 0000000..9cc021b
--- /dev/null
+++ b/src/slalib/gresid.f_alpha_OSF1
@@ -0,0 +1,76 @@
+      REAL FUNCTION sla_GRESID (S)
+*+
+*     - - - - - - -
+*      G R E S I D
+*     - - - - - - -
+*
+*  Generate pseudo-random normal deviate ( = 'Gaussian residual')
+*  (single precision)
+*
+*  !!! Version for DEC Alpha/OSF1 !!!
+*
+*  Given:
+*     S      real     standard deviation
+*
+*  The results of many calls to this routine will be
+*  normally distributed with mean zero and standard deviation S.
+*
+*  The Box-Muller algorithm is used.  This is described in
+*  Numerical Recipes, section 7.2.
+*
+*  P.T.Wallace   Starlink   14 October 1991
+*    Revised for new recommended RTL RANDOM(3f) function.
+*  B.K.McIlwrath Starlink   12 January 1996
+*-
+
+      IMPLICIT NONE
+
+      REAL S
+
+      REAL X,Y,R,W,GNEXT,G
+      LOGICAL FTF,FIRST
+
+      REAL RANDOM
+
+      SAVE GNEXT,FTF,FIRST
+      DATA FTF,FIRST / .TRUE.,.TRUE. /
+
+*  First time through, initialise the random-number generator
+      IF (FTF) THEN
+         X = RANDOM(12345678)
+         FTF = .FALSE.
+      END IF
+
+*  Second normal deviate of the pair available?
+      IF (FIRST) THEN
+
+*     No - generate two random numbers inside unit circle
+         R = 2.0
+         DO WHILE (R.GE.1.0)
+
+*        Generate two random numbers in range +/- 1
+            X = 2.0*RANDOM(0)-1.0
+            Y = 2.0*RANDOM(0)-1.0
+
+*        Try again if not in unit circle
+            R = X*X+Y*Y
+         END DO
+
+*     Box-Muller transformation, generating two deviates
+         W = SQRT(-2.0*LOG(R)/MAX(R,1E-20))
+         GNEXT = X*W
+         G = Y*W
+
+*     Set flag to indicate availability of next deviate
+         FIRST = .FALSE.
+      ELSE
+
+*     Return second deviate of the pair & reset flag
+         G = GNEXT
+         FIRST = .TRUE.
+      END IF
+
+*  Scale the deviate by the required standard deviation
+      sla_GRESID = G*S
+
+      END
diff --git a/src/slalib/gresid.f_convex b/src/slalib/gresid.f_convex
new file mode 100644
index 0000000..278a79e
--- /dev/null
+++ b/src/slalib/gresid.f_convex
@@ -0,0 +1,80 @@
+      REAL FUNCTION sla_GRESID (S)
+*+
+*     - - - - - - -
+*      G R E S I D
+*     - - - - - - -
+*
+*  Generate pseudo-random normal deviate ( = 'Gaussian residual')
+*  (single precision)
+*
+*  !!! Convex specific !!!
+*
+*  Given:
+*     S      real     standard deviation
+*
+*  The results of many calls to this routine will be
+*  normally distributed with mean zero and standard deviation S.
+*
+*  The Box-Muller algorithm is used.  This is described in
+*  Numerical Recipes, section 7.2.
+*
+*  Called:  RAND (a REAL function from the Convex Fortran Library)
+*
+*  P.T.Wallace   Starlink   28 June 1994
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL S
+
+      REAL X,Y,R,W,GNEXT,G
+      LOGICAL FTF,FIRST
+
+      REAL RAND
+
+      SAVE GNEXT,FIRST
+      DATA FTF,FIRST / .TRUE.,.TRUE. /
+
+
+
+*  First time through, initialise the random-number generator
+      IF (FTF) THEN
+         X = RAND(123456789)
+         FTF = .FALSE.
+      END IF
+
+*  Second normal deviate of the pair available?
+      IF (FIRST) THEN
+
+*     No - generate two random numbers inside unit circle
+         R = 2.0
+         DO WHILE (R.GE.1.0)
+
+*        Generate two random numbers in range +/- 1
+            X = 2.0*RAND(0)-1.0
+            Y = 2.0*RAND(0)-1.0
+
+*        Try again if not in unit circle
+            R = X*X+Y*Y
+         END DO
+
+*     Box-Muller transformation, generating two deviates
+         W = SQRT(-2.0*LOG(R)/MAX(R,1E-20))
+         GNEXT = X*W
+         G = Y*W
+
+*     Set flag to indicate availability of next deviate
+         FIRST = .FALSE.
+      ELSE
+
+*     Return second deviate of the pair & reset flag
+         G = GNEXT
+         FIRST = .TRUE.
+      END IF
+
+*  Scale the deviate by the required standard deviation
+      sla_GRESID = G*S
+
+      END
diff --git a/src/slalib/gresid.f_ix86_Linux b/src/slalib/gresid.f_ix86_Linux
new file mode 100644
index 0000000..ec93bdd
--- /dev/null
+++ b/src/slalib/gresid.f_ix86_Linux
@@ -0,0 +1,74 @@
+      REAL FUNCTION sla_GRESID (S)
+*+
+*     - - - - - - -
+*      G R E S I D
+*     - - - - - - -
+*
+*  Generate pseudo-random normal deviate ( = 'Gaussian residual')
+*  (single precision)
+*
+*  !!! Version for Linux !!!
+*
+*  Given:
+*     S      real     standard deviation
+*
+*  The results of many calls to this routine will be
+*  normally distributed with mean zero and standard deviation S.
+*
+*  The Box-Muller algorithm is used.  This is described in
+*  Numerical Recipes, section 7.2.
+*
+*  B.K.McIlwrath Starlink   12 January 1996
+*-
+
+      IMPLICIT NONE
+
+      REAL S
+
+      REAL X,Y,R,W,GNEXT,G
+      LOGICAL FTF,FIRST
+
+      REAL RANDOM
+
+      SAVE GNEXT,FTF,FIRST
+      DATA FTF,FIRST / .TRUE.,.TRUE. /
+
+*  First time through, initialise the random-number generator
+      IF (FTF) THEN
+         X = RANDOM(12345678)
+         FTF = .FALSE.
+      END IF
+
+*  Second normal deviate of the pair available?
+      IF (FIRST) THEN
+
+*     No - generate two random numbers inside unit circle
+         R = 2.0
+         DO WHILE (R.GE.1.0)
+
+*        Generate two random numbers in range +/- 1
+            X = 2.0*RANDOM(0)-1.0
+            Y = 2.0*RANDOM(0)-1.0
+
+*        Try again if not in unit circle
+            R = X*X+Y*Y
+         END DO
+
+*     Box-Muller transformation, generating two deviates
+         W = SQRT(-2.0*LOG(R)/MAX(R,1E-20))
+         GNEXT = X*W
+         G = Y*W
+
+*     Set flag to indicate availability of next deviate
+         FIRST = .FALSE.
+      ELSE
+
+*     Return second deviate of the pair & reset flag
+         G = GNEXT
+         FIRST = .TRUE.
+      END IF
+
+*  Scale the deviate by the required standard deviation
+      sla_GRESID = G*S
+
+      END
diff --git a/src/slalib/gresid.f_mips b/src/slalib/gresid.f_mips
new file mode 100644
index 0000000..7f353f9
--- /dev/null
+++ b/src/slalib/gresid.f_mips
@@ -0,0 +1,74 @@
+      REAL FUNCTION sla_GRESID (S)
+*+
+*     - - - - - - -
+*      G R E S I D
+*     - - - - - - -
+*
+*  Generate pseudo-random normal deviate ( = 'Gaussian residual')
+*  (single precision)
+*
+*  !!! Version for VAX/VMS and DECstation !!!
+*
+*  Given:
+*     S      real     standard deviation
+*
+*  The results of many calls to this routine will be
+*  normally distributed with mean zero and standard deviation S.
+*
+*  The Box-Muller algorithm is used.  This is described in
+*  Numerical Recipes, section 7.2.
+*
+*  P.T.Wallace   Starlink   14 October 1991
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL S
+
+      REAL X,Y,R,W,GNEXT,G
+      INTEGER ISEED
+      LOGICAL FIRST
+
+      REAL RAN
+
+      SAVE GNEXT,ISEED,FIRST
+      DATA ISEED / 123456789 /
+      DATA FIRST / .TRUE. /
+
+
+
+*  Second normal deviate of the pair available?
+      IF (FIRST) THEN
+
+*     No - generate two random numbers inside unit circle
+         R = 2.0
+         DO WHILE (R.GE.1.0)
+
+*        Generate two random numbers in range +/- 1
+            X = 2.0*RAN(ISEED)-1.0
+            Y = 2.0*RAN(ISEED)-1.0
+
+*        Try again if not in unit circle
+            R = X*X+Y*Y
+         END DO
+
+*     Box-Muller transformation, generating two deviates
+         W = SQRT(-2.0*LOG(R)/MAX(R,1E-20))
+         GNEXT = X*W
+         G = Y*W
+
+*     Set flag to indicate availability of next deviate
+         FIRST = .FALSE.
+      ELSE
+
+*     Return second deviate of the pair & reset flag
+         G = GNEXT
+         FIRST = .TRUE.
+      END IF
+
+*  Scale the deviate by the required standard deviation
+      sla_GRESID = G*S
+
+      END
diff --git a/src/slalib/gresid.f_pcm b/src/slalib/gresid.f_pcm
new file mode 100644
index 0000000..b2c6f76
--- /dev/null
+++ b/src/slalib/gresid.f_pcm
@@ -0,0 +1,73 @@
+      REAL FUNCTION sla_GRESID (S)
+*+
+*     - - - - - - -
+*      G R E S I D
+*     - - - - - - -
+*
+*  Generate pseudo-random normal deviate ( = 'Gaussian residual')
+*  (single precision)
+*
+*  Given:
+*     S      real     standard deviation
+*
+*  The results of many calls to this routine will be
+*  normally distributed with mean zero and standard deviation S.
+*
+*  The Box-Muller algorithm is used.  This is described in
+*  Numerical Recipes, section 7.2.
+*
+*  !!!  Microsoft Fortran dependent - calls the RAN routine   !!!
+*  !!!  To seed the random-number generator, either call the  !!!
+*  !!!  Microsoft SEED routine specifying some INTEGER*2      !!!
+*  !!!  seed or call the function sla_RANDOM specifying some  !!!
+*  !!!  REAL seed.                                            !!!
+*
+*  P.T.Wallace   Starlink   1 April 1993
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL S
+
+      REAL X,Y,RV,R,W,GNEXT,G
+      LOGICAL FIRST
+
+      SAVE GNEXT,RV,FIRST
+      DATA FIRST / .TRUE. /
+
+
+
+*  Second normal deviate of the pair available?
+      IF (FIRST) THEN
+
+*     No - generate two random numbers in range +/- 1
+ 1       CONTINUE
+         CALL RANDOM(RV)               !!! PC
+         X = 2.0*RV-1.0
+         CALL RANDOM(RV)               !!! PC
+         Y = 2.0*RV-1.0
+
+*     Try again if not in unit circle
+         R = X*X+Y*Y
+         IF (R.GE.1.0) GO TO 1
+
+*     Box-Muller transformation, generating two deviates
+         W = SQRT(-2.0*LOG(R)/MAX(R,1E-20))
+         GNEXT = X*W
+         G = Y*W
+
+*     Set flag to indicate availability of next deviate
+         FIRST = .FALSE.
+      ELSE
+
+*     Return second deviate of the pair & reset flag
+         G = GNEXT
+         FIRST = .TRUE.
+      END IF
+
+*  Scale the deviate by the required standard deviation
+      sla_GRESID = G*S
+
+      END
diff --git a/src/slalib/gresid.f_sun4 b/src/slalib/gresid.f_sun4
new file mode 100644
index 0000000..3205062
--- /dev/null
+++ b/src/slalib/gresid.f_sun4
@@ -0,0 +1,80 @@
+      REAL FUNCTION sla_GRESID (S)
+*+
+*     - - - - - - -
+*      G R E S I D
+*     - - - - - - -
+*
+*  Generate pseudo-random normal deviate ( = 'Gaussian residual')
+*  (single precision)
+*
+*  !!! Sun 4 specific !!!
+*
+*  Given:
+*     S      real     standard deviation
+*
+*  The results of many calls to this routine will be
+*  normally distributed with mean zero and standard deviation S.
+*
+*  The Box-Muller algorithm is used.  This is described in
+*  Numerical Recipes, section 7.2.
+*
+*  Called:  RAND (a REAL function from the Sun Fortran Library)
+*
+*  P.T.Wallace   Starlink   14 October 1991
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL S
+
+      REAL X,Y,R,W,GNEXT,G
+      LOGICAL FTF,FIRST
+
+      REAL RAND
+
+      SAVE GNEXT,FIRST
+      DATA FTF,FIRST / .TRUE.,.TRUE. /
+
+
+
+*  First time through, initialise the random-number generator
+      IF (FTF) THEN
+         X = RAND(123456789)
+         FTF = .FALSE.
+      END IF
+
+*  Second normal deviate of the pair available?
+      IF (FIRST) THEN
+
+*     No - generate two random numbers inside unit circle
+         R = 2.0
+         DO WHILE (R.GE.1.0)
+
+*        Generate two random numbers in range +/- 1
+            X = 2.0*RAND(0)-1.0
+            Y = 2.0*RAND(0)-1.0
+
+*        Try again if not in unit circle
+            R = X*X+Y*Y
+         END DO
+
+*     Box-Muller transformation, generating two deviates
+         W = SQRT(-2.0*LOG(R)/MAX(R,1E-20))
+         GNEXT = X*W
+         G = Y*W
+
+*     Set flag to indicate availability of next deviate
+         FIRST = .FALSE.
+      ELSE
+
+*     Return second deviate of the pair & reset flag
+         G = GNEXT
+         FIRST = .TRUE.
+      END IF
+
+*  Scale the deviate by the required standard deviation
+      sla_GRESID = G*S
+
+      END
diff --git a/src/slalib/gresid.f_sun4_Solaris b/src/slalib/gresid.f_sun4_Solaris
new file mode 100644
index 0000000..3205062
--- /dev/null
+++ b/src/slalib/gresid.f_sun4_Solaris
@@ -0,0 +1,80 @@
+      REAL FUNCTION sla_GRESID (S)
+*+
+*     - - - - - - -
+*      G R E S I D
+*     - - - - - - -
+*
+*  Generate pseudo-random normal deviate ( = 'Gaussian residual')
+*  (single precision)
+*
+*  !!! Sun 4 specific !!!
+*
+*  Given:
+*     S      real     standard deviation
+*
+*  The results of many calls to this routine will be
+*  normally distributed with mean zero and standard deviation S.
+*
+*  The Box-Muller algorithm is used.  This is described in
+*  Numerical Recipes, section 7.2.
+*
+*  Called:  RAND (a REAL function from the Sun Fortran Library)
+*
+*  P.T.Wallace   Starlink   14 October 1991
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL S
+
+      REAL X,Y,R,W,GNEXT,G
+      LOGICAL FTF,FIRST
+
+      REAL RAND
+
+      SAVE GNEXT,FIRST
+      DATA FTF,FIRST / .TRUE.,.TRUE. /
+
+
+
+*  First time through, initialise the random-number generator
+      IF (FTF) THEN
+         X = RAND(123456789)
+         FTF = .FALSE.
+      END IF
+
+*  Second normal deviate of the pair available?
+      IF (FIRST) THEN
+
+*     No - generate two random numbers inside unit circle
+         R = 2.0
+         DO WHILE (R.GE.1.0)
+
+*        Generate two random numbers in range +/- 1
+            X = 2.0*RAND(0)-1.0
+            Y = 2.0*RAND(0)-1.0
+
+*        Try again if not in unit circle
+            R = X*X+Y*Y
+         END DO
+
+*     Box-Muller transformation, generating two deviates
+         W = SQRT(-2.0*LOG(R)/MAX(R,1E-20))
+         GNEXT = X*W
+         G = Y*W
+
+*     Set flag to indicate availability of next deviate
+         FIRST = .FALSE.
+      ELSE
+
+*     Return second deviate of the pair & reset flag
+         G = GNEXT
+         FIRST = .TRUE.
+      END IF
+
+*  Scale the deviate by the required standard deviation
+      sla_GRESID = G*S
+
+      END
diff --git a/src/slalib/gresid.f_vax b/src/slalib/gresid.f_vax
new file mode 100644
index 0000000..90dab0a
--- /dev/null
+++ b/src/slalib/gresid.f_vax
@@ -0,0 +1,72 @@
+      REAL FUNCTION sla_GRESID (S)
+*+
+*     - - - - - - -
+*      G R E S I D
+*     - - - - - - -
+*
+*  Generate pseudo-random normal deviate ( = 'Gaussian residual')
+*  (single precision)
+*
+*  !!! Version for VAX/VMS and DECstation !!!
+*
+*  Given:
+*     S      real     standard deviation
+*
+*  The results of many calls to this routine will be
+*  normally distributed with mean zero and standard deviation S.
+*
+*  The Box-Muller algorithm is used.  This is described in
+*  Numerical Recipes, section 7.2.
+*
+*  P.T.Wallace   Starlink   14 October 1991
+*-
+
+      IMPLICIT NONE
+
+      REAL S
+
+      REAL X,Y,R,W,GNEXT,G
+      INTEGER ISEED
+      LOGICAL FIRST
+
+      REAL RAN
+
+      SAVE GNEXT,ISEED,FIRST
+      DATA ISEED / 123456789 /
+      DATA FIRST / .TRUE. /
+
+
+
+*  Second normal deviate of the pair available?
+      IF (FIRST) THEN
+
+*     No - generate two random numbers inside unit circle
+         R = 2.0
+         DO WHILE (R.GE.1.0)
+
+*        Generate two random numbers in range +/- 1
+            X = 2.0*RAN(ISEED)-1.0
+            Y = 2.0*RAN(ISEED)-1.0
+
+*        Try again if not in unit circle
+            R = X*X+Y*Y
+         END DO
+
+*     Box-Muller transformation, generating two deviates
+         W = SQRT(-2.0*LOG(R)/MAX(R,1E-20))
+         GNEXT = X*W
+         G = Y*W
+
+*     Set flag to indicate availability of next deviate
+         FIRST = .FALSE.
+      ELSE
+
+*     Return second deviate of the pair & reset flag
+         G = GNEXT
+         FIRST = .TRUE.
+      END IF
+
+*  Scale the deviate by the required standard deviation
+      sla_GRESID = G*S
+
+      END
diff --git a/src/slalib/gresid.f_x86_64 b/src/slalib/gresid.f_x86_64
new file mode 100644
index 0000000..ec93bdd
--- /dev/null
+++ b/src/slalib/gresid.f_x86_64
@@ -0,0 +1,74 @@
+      REAL FUNCTION sla_GRESID (S)
+*+
+*     - - - - - - -
+*      G R E S I D
+*     - - - - - - -
+*
+*  Generate pseudo-random normal deviate ( = 'Gaussian residual')
+*  (single precision)
+*
+*  !!! Version for Linux !!!
+*
+*  Given:
+*     S      real     standard deviation
+*
+*  The results of many calls to this routine will be
+*  normally distributed with mean zero and standard deviation S.
+*
+*  The Box-Muller algorithm is used.  This is described in
+*  Numerical Recipes, section 7.2.
+*
+*  B.K.McIlwrath Starlink   12 January 1996
+*-
+
+      IMPLICIT NONE
+
+      REAL S
+
+      REAL X,Y,R,W,GNEXT,G
+      LOGICAL FTF,FIRST
+
+      REAL RANDOM
+
+      SAVE GNEXT,FTF,FIRST
+      DATA FTF,FIRST / .TRUE.,.TRUE. /
+
+*  First time through, initialise the random-number generator
+      IF (FTF) THEN
+         X = RANDOM(12345678)
+         FTF = .FALSE.
+      END IF
+
+*  Second normal deviate of the pair available?
+      IF (FIRST) THEN
+
+*     No - generate two random numbers inside unit circle
+         R = 2.0
+         DO WHILE (R.GE.1.0)
+
+*        Generate two random numbers in range +/- 1
+            X = 2.0*RANDOM(0)-1.0
+            Y = 2.0*RANDOM(0)-1.0
+
+*        Try again if not in unit circle
+            R = X*X+Y*Y
+         END DO
+
+*     Box-Muller transformation, generating two deviates
+         W = SQRT(-2.0*LOG(R)/MAX(R,1E-20))
+         GNEXT = X*W
+         G = Y*W
+
+*     Set flag to indicate availability of next deviate
+         FIRST = .FALSE.
+      ELSE
+
+*     Return second deviate of the pair & reset flag
+         G = GNEXT
+         FIRST = .TRUE.
+      END IF
+
+*  Scale the deviate by the required standard deviation
+      sla_GRESID = G*S
+
+      END
diff --git a/src/slalib/h2e.f b/src/slalib/h2e.f
new file mode 100644
index 0000000..e850493
--- /dev/null
+++ b/src/slalib/h2e.f
@@ -0,0 +1,83 @@
+      SUBROUTINE sla_H2E (AZ, EL, PHI, HA, DEC)
+*+
+*     - - - - -
+*      D E 2 H
+*     - - - - -
+*
+*  Horizon to equatorial coordinates:  Az,El to HA,Dec
+*
+*  (single precision)
+*
+*  Given:
+*     AZ      r     azimuth
+*     EL      r     elevation
+*     PHI     r     observatory latitude
+*
+*  Returned:
+*     HA      r     hour angle
+*     DEC     r     declination
+*
+*  Notes:
+*
+*  1)  All the arguments are angles in radians.
+*
+*  2)  The sign convention for azimuth is north zero, east +pi/2.
+*
+*  3)  HA is returned in the range +/-pi.  Declination is returned
+*      in the range +/-pi/2.
+*
+*  4)  The latitude is (in principle) geodetic.  In critical
+*      applications, corrections for polar motion should be applied.
+*
+*  5)  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.
+*
+*  6)  No range checking of arguments is done.
+*
+*  7)  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.
+*
+*  P.T.Wallace   Starlink   21 February 1996
+*
+*  Copyright (C) 1996 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL AZ,EL,PHI,HA,DEC
+
+      DOUBLE PRECISION SA,CA,SE,CE,SP,CP,X,Y,Z,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.EQ.0.0) THEN
+         HA=0.0
+      ELSE
+         HA=ATAN2(Y,X)
+      END IF
+      DEC=ATAN2(Z,R)
+
+      END
diff --git a/src/slalib/h2fk5.f b/src/slalib/h2fk5.f
new file mode 100644
index 0000000..d3a0116
--- /dev/null
+++ b/src/slalib/h2fk5.f
@@ -0,0 +1,109 @@
+      SUBROUTINE sla_H2FK5 (RH,DH,DRH,DDH,R5,D5,DR5,DD5)
+*+
+*     - - - - - -
+*      H 2 F K 5
+*     - - - - - -
+*
+*  Transform Hipparcos star data into the FK5 (J2000) system.
+*
+*  (double precision)
+*
+*  This routine transforms Hipparcos star positions and proper
+*  motions into FK5 J2000.
+*
+*  Given (all Hipparcos, epoch J2000):
+*     RH        d      RA (radians)
+*     DH        d      Dec (radians)
+*     DRH       d      proper motion in RA (dRA/dt, rad/Jyear)
+*     DDH       d      proper motion in Dec (dDec/dt, rad/Jyear)
+*
+*  Returned (all FK5, equinox J2000, epoch J2000):
+*     R5        d      RA (radians)
+*     D5        d      Dec (radians)
+*     DR5       d      proper motion in RA (dRA/dt, rad/Jyear)
+*     DD5       d      proper motion in Dec (dDec/dt, rad/Jyear)
+*
+*  Called:  sla_DS2C6, sla_DAV2M, sla_DMXV, sla_DIMXV, sla_DVXV,
+*           sla_DC62S, sla_DRANRM
+*
+*  Notes:
+*
+*  1)  The proper motions in RA are dRA/dt rather than
+*      cos(Dec)*dRA/dt, and are per year rather than per century.
+*
+*  2)  The FK5 to Hipparcos transformation consists of a pure
+*      rotation and spin;  zonal errors in the FK5 catalogue are
+*      not taken into account.
+*
+*  3)  The published orientation and spin components are interpreted
+*      as "axial vectors".  An axial vector points at the pole of the
+*      rotation and its length is the amount of rotation in radians.
+*
+*  4)  See also sla_FK52H, sla_FK5HZ, sla_HFK5Z.
+*
+*  Reference:
+*
+*     M.Feissel & F.Mignard, Astron. Astrophys. 331, L33-L36 (1998).
+*
+*  P.T.Wallace   Starlink   22 June 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION RH,DH,DRH,DDH,R5,D5,DR5,DD5
+
+      DOUBLE PRECISION AS2R
+      PARAMETER (AS2R=0.484813681109535994D-5)
+
+*  FK5 to Hipparcos orientation and spin (radians, radians/year)
+      DOUBLE PRECISION EPX,EPY,EPZ
+      DOUBLE PRECISION OMX,OMY,OMZ
+
+      PARAMETER ( EPX = -19.9D-3 * AS2R,
+     :            EPY =  -9.1D-3 * AS2R,
+     :            EPZ = +22.9D-3 * AS2R )
+
+      PARAMETER ( OMX = -0.30D-3 * AS2R,
+     :            OMY = +0.60D-3 * AS2R,
+     :            OMZ = +0.70D-3 * AS2R )
+
+      DOUBLE PRECISION PVH(6),ORTN(3),R5H(3,3),S5(3),SH(3),VV(3),
+     :                 PV5(6),W,R,V
+      INTEGER I
+
+      DOUBLE PRECISION sla_DRANRM
+
+
+
+*  Hipparcos barycentric position/velocity 6-vector (normalized).
+      CALL sla_DS2C6(RH,DH,1D0,DRH,DDH,0D0,PVH)
+
+*  FK5 to Hipparcos orientation matrix.
+      ORTN(1) = EPX
+      ORTN(2) = EPY
+      ORTN(3) = EPZ
+      CALL sla_DAV2M(ORTN,R5H)
+
+*  Hipparcos wrt FK5 spin vector.
+      S5(1) = OMX
+      S5(2) = OMY
+      S5(3) = OMZ
+
+*  Rotate the spin vector into the Hipparcos frame.
+      CALL sla_DMXV(R5H,S5,SH)
+
+*  De-orient & de-spin the 6-vector into FK5 J2000.
+      CALL sla_DIMXV(R5H,PVH,PV5)
+      CALL sla_DVXV(PVH,SH,VV)
+      DO I=1,3
+         VV(I) = PVH(I+3)-VV(I)
+      END DO
+      CALL sla_DIMXV(R5H,VV,PV5(4))
+
+*  FK5 6-vector to spherical.
+      CALL sla_DC62S(PV5,W,D5,R,DR5,DD5,V)
+      R5 = sla_DRANRM(W)
+
+      END
diff --git a/src/slalib/hfk5z.f b/src/slalib/hfk5z.f
new file mode 100644
index 0000000..b50d38a
--- /dev/null
+++ b/src/slalib/hfk5z.f
@@ -0,0 +1,122 @@
+      SUBROUTINE sla_HFK5Z (RH,DH,EPOCH,R5,D5,DR5,DD5)
+*+
+*     - - - - - -
+*      H F K 5 Z
+*     - - - - - -
+*
+*  Transform a Hipparcos star position into FK5 J2000, assuming
+*  zero Hipparcos proper motion.
+*
+*  (double precision)
+*
+*  Given:
+*     RH        d      Hipparcos RA (radians)
+*     DH        d      Hipparcos Dec (radians)
+*     EPOCH     d      Julian epoch (TDB)
+*
+*  Returned (all FK5, equinox J2000, epoch EPOCH):
+*     R5        d      RA (radians)
+*     D5        d      Dec (radians)
+*
+*  Called:  sla_DCS2C, sla_DAV2M, sla_DMXV, sla_DAV2M, sla_DMXM,
+*           sla_DIMXV, sla_DVXV, sla_DC62S, sla_DRANRM
+*
+*  Notes:
+*
+*  1)  The proper motion in RA is dRA/dt rather than cos(Dec)*dRA/dt.
+*
+*  2)  The FK5 to Hipparcos transformation consists of a pure
+*      rotation and spin;  zonal errors in the FK5 catalogue are
+*      not taken into account.
+*
+*  3)  The published orientation and spin components are interpreted
+*      as "axial vectors".  An axial vector points at the pole of the
+*      rotation and its length is the amount of rotation in radians.
+*
+*  4)  It was the intention that Hipparcos 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 FK5, and this routine returns those
+*      fictitious proper motions.
+*
+*  5)  The position returned by this routine is in the FK5 J2000
+*      reference frame but at Julian epoch EPOCH.
+*
+*  6)  See also sla_FK52H, sla_H2FK5, sla_FK5ZHZ.
+*
+*  Reference:
+*
+*     M.Feissel & F.Mignard, Astron. Astrophys. 331, L33-L36 (1998).
+*
+*  P.T.Wallace   Starlink   22 June 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION RH,DH,EPOCH,R5,D5,DR5,DD5
+
+      DOUBLE PRECISION AS2R
+      PARAMETER (AS2R=0.484813681109535994D-5)
+
+*  FK5 to Hipparcos orientation and spin (radians, radians/year)
+      DOUBLE PRECISION EPX,EPY,EPZ
+      DOUBLE PRECISION OMX,OMY,OMZ
+
+      PARAMETER ( EPX = -19.9D-3 * AS2R,
+     :            EPY =  -9.1D-3 * AS2R,
+     :            EPZ = +22.9D-3 * AS2R )
+
+      PARAMETER ( OMX = -0.30D-3 * AS2R,
+     :            OMY = +0.60D-3 * AS2R,
+     :            OMZ = +0.70D-3 * AS2R )
+
+      DOUBLE PRECISION PH(6),ORTN(3),R5H(3,3),S5(3),SH(3),T,VST(3),
+     :                 RST(3,3),R5HT(3,3),PV5E(6),VV(3),W,R,V
+
+      DOUBLE PRECISION sla_DRANRM
+
+
+
+*  Hipparcos barycentric position vector (normalized).
+      CALL sla_DCS2C(RH,DH,PH)
+
+*  FK5 to Hipparcos orientation matrix.
+      ORTN(1) = EPX
+      ORTN(2) = EPY
+      ORTN(3) = EPZ
+      CALL sla_DAV2M(ORTN,R5H)
+
+*  Hipparcos wrt FK5 spin vector.
+      S5(1) = OMX
+      S5(2) = OMY
+      S5(3) = OMZ
+
+*  Rotate the spin vector into the Hipparcos frame.
+      CALL sla_DMXV(R5H,S5,SH)
+
+*  Time interval from J2000 to epoch.
+      T = EPOCH-2000D0
+
+*  Axial vector:  accumulated Hipparcos wrt FK5 spin over that interval.
+      VST(1) = OMX*T
+      VST(2) = OMY*T
+      VST(3) = OMZ*T
+
+*  Express the accumulated spin as a rotation matrix.
+      CALL sla_DAV2M(VST,RST)
+
+*  Rotation matrix:  accumulated spin, then FK5 to Hipparcos.
+      CALL sla_DMXM(R5H,RST,R5HT)
+
+*  De-orient & de-spin the vector into FK5 J2000 at epoch.
+      CALL sla_DIMXV(R5HT,PH,PV5E)
+      CALL sla_DVXV(SH,PH,VV)
+      CALL sla_DIMXV(R5HT,VV,PV5E(4))
+
+*  FK5 position/velocity 6-vector to spherical.
+      CALL sla_DC62S(PV5E,W,D5,R,DR5,DD5,V)
+      R5 = sla_DRANRM(W)
+
+      END
diff --git a/src/slalib/idchf.f b/src/slalib/idchf.f
new file mode 100644
index 0000000..2f758bf
--- /dev/null
+++ b/src/slalib/idchf.f
@@ -0,0 +1,94 @@
+      SUBROUTINE sla__IDCHF (STRING, NPTR, NVEC, NDIGIT, DIGIT)
+*+
+*     - - - - - -
+*      I D C H F
+*     - - - - - -
+*
+*  Internal routine used by DFLTIN
+*
+*  Identify next character in string
+*
+*  Given:
+*     STRING      char        string
+*     NPTR        int         pointer to character to be identified
+*
+*  Returned:
+*     NPTR        int         incremented unless end of field
+*     NVEC        int         vector for identified character
+*     NDIGIT      int         0-9 if character was a numeral
+*     DIGIT       double      equivalent of NDIGIT
+*
+*     NVEC takes the following values:
+*
+*      1     0-9
+*      2     space or TAB   !!! n.b. ASCII TAB assumed !!!
+*      3     D,d,E or e
+*      4     .
+*      5     +
+*      6     -
+*      7     ,
+*      8     else
+*      9     outside field
+*
+*  If the character is not 0-9, NDIGIT and DIGIT are either not
+*  altered or are set to arbitrary values.
+*
+*  P.T.Wallace   Starlink   22 December 1992
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      CHARACTER*(*) STRING
+      INTEGER NPTR,NVEC,NDIGIT
+      DOUBLE PRECISION DIGIT
+
+      CHARACTER K
+      INTEGER NCHAR
+
+*  Character/vector tables
+      INTEGER NCREC
+      PARAMETER (NCREC=19)
+      CHARACTER KCTAB(NCREC)
+      INTEGER KVTAB(NCREC)
+      DATA KCTAB/'0','1','2','3','4','5','6','7','8','9',
+     :           ' ','D','d','E','e','.','+','-',','/
+      DATA KVTAB/10*1,2,4*3,4,5,6,7/
+
+
+*  Handle pointer outside field
+      IF (NPTR.LT.1.OR.NPTR.GT.LEN(STRING)) THEN
+         NVEC=9
+      ELSE
+
+*     Not end of field: identify the character
+         K=STRING(NPTR:NPTR)
+         DO NCHAR=1,NCREC
+            IF (K.EQ.KCTAB(NCHAR)) THEN
+
+*           Recognized
+               NVEC=KVTAB(NCHAR)
+               NDIGIT=NCHAR-1
+               DIGIT=DBLE(NDIGIT)
+               GO TO 2300
+            END IF
+         END DO
+
+*     Not recognized: check for TAB    !!! n.b. ASCII assumed !!!
+         IF (K.EQ.CHAR(9)) THEN
+
+*        TAB: treat as space
+            NVEC=2
+         ELSE
+
+*        Unrecognized
+            NVEC=8
+         END IF
+
+*     Increment pointer
+ 2300    CONTINUE
+         NPTR=NPTR+1
+      END IF
+
+      END
diff --git a/src/slalib/idchi.f b/src/slalib/idchi.f
new file mode 100644
index 0000000..56f596f
--- /dev/null
+++ b/src/slalib/idchi.f
@@ -0,0 +1,91 @@
+      SUBROUTINE sla__IDCHI (STRING, NPTR, NVEC, DIGIT)
+*+
+*     - - - - - -
+*      I D C H I
+*     - - - - - -
+*
+*  Internal routine used by INTIN
+*
+*  Identify next character in string
+*
+*  Given:
+*     STRING      char        string
+*     NPTR        int         pointer to character to be identified
+*
+*  Returned:
+*     NPTR        int         incremented unless end of field
+*     NVEC        int         vector for identified character
+*     DIGIT       double      double precision digit if 0-9
+*
+*     NVEC takes the following values:
+*
+*      1     0-9
+*      2     space or TAB   !!! n.b. ASCII TAB assumed !!!
+*      3     +
+*      4     -
+*      5     ,
+*      6     else
+*      7     outside string
+*
+*  If the character is not 0-9, DIGIT is either unaltered or
+*  is set to an arbitrary value.
+*
+*  P.T.Wallace   Starlink   22 December 1992
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      CHARACTER*(*) STRING
+      INTEGER NPTR,NVEC
+      DOUBLE PRECISION DIGIT
+
+      CHARACTER K
+      INTEGER NCHAR
+
+*  Character/vector tables
+      INTEGER NCREC
+      PARAMETER (NCREC=14)
+      CHARACTER KCTAB(NCREC)
+      INTEGER KVTAB(NCREC)
+      DATA KCTAB/'0','1','2','3','4','5','6','7','8','9',
+     :           ' ', '+','-',','/
+      DATA KVTAB/10*1,2,3,4,5/
+
+
+
+*  Handle pointer outside field
+      IF (NPTR.LT.1.OR.NPTR.GT.LEN(STRING)) THEN
+         NVEC=7
+      ELSE
+
+*     Not end of field: identify character
+         K=STRING(NPTR:NPTR)
+         DO NCHAR=1,NCREC
+            IF (K.EQ.KCTAB(NCHAR)) THEN
+
+*           Recognized
+               NVEC=KVTAB(NCHAR)
+               DIGIT=DBLE(NCHAR-1)
+               GO TO 2300
+            END IF
+         END DO
+
+*     Not recognized: check for TAB   !!! n.b. ASCII assumed !!!
+         IF (K.EQ.CHAR(9)) THEN
+
+*        TAB: treat as space
+            NVEC=2
+         ELSE
+
+*        Unrecognized
+            NVEC=6
+         END IF
+
+*     Increment pointer
+ 2300    CONTINUE
+         NPTR=NPTR+1
+      END IF
+
+      END
diff --git a/src/slalib/imxv.f b/src/slalib/imxv.f
new file mode 100644
index 0000000..2aef263
--- /dev/null
+++ b/src/slalib/imxv.f
@@ -0,0 +1,51 @@
+      SUBROUTINE sla_IMXV (RM, VA, VB)
+*+
+*     - - - - -
+*      I M X V
+*     - - - - -
+*
+*  Performs the 3-D backward unitary transformation:
+*
+*     vector VB = (inverse of matrix RM) * vector VA
+*
+*  (single precision)
+*
+*  (n.b.  the matrix must be unitary, as this routine assumes that
+*   the inverse and transpose are identical)
+*
+*  Given:
+*     RM       real(3,3)    matrix
+*     VA       real(3)      vector
+*
+*  Returned:
+*     VB       real(3)      result vector
+*
+*  P.T.Wallace   Starlink   November 1984
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL RM(3,3),VA(3),VB(3)
+
+      INTEGER I,J
+      REAL W,VW(3)
+
+
+
+*  Inverse of matrix RM * vector VA -> vector VW
+      DO J=1,3
+         W=0.0
+         DO I=1,3
+            W=W+RM(I,J)*VA(I)
+         END DO
+         VW(J)=W
+      END DO
+
+*  Vector VW -> vector VB
+      DO J=1,3
+         VB(J)=VW(J)
+      END DO
+
+      END
diff --git a/src/slalib/intin.f b/src/slalib/intin.f
new file mode 100644
index 0000000..a4cee15
--- /dev/null
+++ b/src/slalib/intin.f
@@ -0,0 +1,176 @@
+      SUBROUTINE sla_INTIN (STRING, NSTRT, IRESLT, JFLAG)
+*+
+*     - - - - - -
+*      I N T I N
+*     - - - - - -
+*
+*  Convert free-format input into an integer
+*
+*  Given:
+*     STRING     c     string containing number to be decoded
+*     NSTRT      i     pointer to where decoding is to start
+*     IRESLT     i     current value of result
+*
+*  Returned:
+*     NSTRT      i      advanced to next number
+*     IRESLT     i      result
+*     JFLAG      i      status: -1 = -OK, 0 = +OK, 1 = null, 2 = error
+*
+*  Called:  sla__IDCHI
+*
+*  Notes:
+*
+*     1     The reason INTIN has separate OK status values for +
+*           and - is to enable minus zero to be detected.   This is
+*           of crucial importance when decoding mixed-radix numbers.
+*           For example, an angle expressed as deg, arcmin, arcsec
+*           may have a leading minus sign but a zero degrees field.
+*
+*     2     A TAB is interpreted as a space.
+*
+*     3     The basic format is the sequence of fields #^, where
+*           # is a sign character + or -, and ^ means a string of
+*           decimal digits.
+*
+*     4     Spaces:
+*
+*             .  Leading spaces are ignored.
+*
+*             .  Spaces between the sign and the number are allowed.
+*
+*             .  Trailing spaces are ignored;  the first signifies
+*                end of decoding and subsequent ones are skipped.
+*
+*     5     Delimiters:
+*
+*             .  Any character other than +,-,0-9 or space may be
+*                used to signal the end of the number and terminate
+*                decoding.
+*
+*             .  Comma is recognized by INTIN as a special case;  it
+*                is skipped, leaving the pointer on the next character.
+*                See 9, below.
+*
+*     6     The sign is optional.  The default is +.
+*
+*     7     A "null result" occurs when the string of characters being
+*           decoded does not begin with +,- or 0-9, or consists
+*           entirely of spaces.  When this condition is detected, JFLAG
+*           is set to 1 and IRESLT is left untouched.
+*
+*     8     NSTRT = 1 for the first character in the string.
+*
+*     9     On return from INTIN, NSTRT is set ready for the next
+*           decode - following trailing blanks and any comma.  If a
+*           delimiter other than comma is being used, NSTRT must be
+*           incremented before the next call to INTIN, otherwise
+*           all subsequent calls will return a null result.
+*
+*     10    Errors (JFLAG=2) occur when:
+*
+*             .  there is a + or - but no number;  or
+*
+*             .  the number is greater than BIG (defined below).
+*
+*     11    When an error has been detected, NSTRT is left
+*           pointing to the character following the last
+*           one used before the error came to light.
+*
+*     12    See also FLOTIN and DFLTIN.
+*
+*  P.T.Wallace   Starlink   27 April 1998
+*
+*  Copyright (C) 1998 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      CHARACTER*(*) STRING
+      INTEGER NSTRT,IRESLT,JFLAG
+
+*  Maximum allowed value
+      DOUBLE PRECISION BIG
+      PARAMETER (BIG=2147483647D0)
+
+      INTEGER JPTR,MSIGN,NVEC,J
+      DOUBLE PRECISION DRES,DIGIT
+
+
+
+*  Current character
+      JPTR=NSTRT
+
+*  Set defaults
+      DRES=0D0
+      MSIGN=1
+
+*  Look for sign
+ 100  CONTINUE
+      CALL sla__IDCHI(STRING,JPTR,NVEC,DIGIT)
+      GO TO ( 400, 100,  300,  200, 9110, 9100, 9110),NVEC
+*             0-9   SP     +     -     ,   ELSE   END
+
+*  Negative
+ 200  CONTINUE
+      MSIGN=-1
+
+*  Look for first decimal
+ 300  CONTINUE
+      CALL sla__IDCHI(STRING,JPTR,NVEC,DIGIT)
+      GO TO ( 400, 300, 9200, 9200, 9200, 9200, 9210),NVEC
+*             0-9   SP     +     -     ,   ELSE   END
+
+*  Accept decimals
+ 400  CONTINUE
+      DRES=DRES*1D1+DIGIT
+
+*  Test for overflow
+      IF (DRES.GT.BIG) GO TO 9200
+
+*  Look for subsequent decimals
+      CALL sla__IDCHI(STRING,JPTR,NVEC,DIGIT)
+      GO TO ( 400, 1610, 1600, 1600, 1600, 1600, 1610),NVEC
+*             0-9   SP     +     -     ,   ELSE   END
+
+*  Get result & status
+ 1600 CONTINUE
+      JPTR=JPTR-1
+ 1610 CONTINUE
+      J=0
+      IF (MSIGN.EQ.1) GO TO 1620
+      J=-1
+      DRES=-DRES
+ 1620 CONTINUE
+      IRESLT=NINT(DRES)
+
+*  Skip to end of field
+ 1630 CONTINUE
+      CALL sla__IDCHI(STRING,JPTR,NVEC,DIGIT)
+      GO TO (1720, 1630, 1720, 1720, 9900, 1720, 9900),NVEC
+*             0-9   SP     +     -     ,   ELSE   END
+
+ 1720 CONTINUE
+      JPTR=JPTR-1
+      GO TO 9900
+
+*  Exits
+
+*  Null field
+ 9100 CONTINUE
+      JPTR=JPTR-1
+ 9110 CONTINUE
+      J=1
+      GO TO 9900
+
+*  Errors
+ 9200 CONTINUE
+      JPTR=JPTR-1
+ 9210 CONTINUE
+      J=2
+
+*  Return
+ 9900 CONTINUE
+      NSTRT=JPTR
+      JFLAG=J
+
+      END
diff --git a/src/slalib/invf.f b/src/slalib/invf.f
new file mode 100644
index 0000000..f323228
--- /dev/null
+++ b/src/slalib/invf.f
@@ -0,0 +1,90 @@
+      SUBROUTINE sla_INVF (FWDS,BKWDS,J)
+*+
+*     - - - - -
+*      I N V F
+*     - - - - -
+*
+*  Invert a linear model of the type produced by the
+*  sla_FITXY routine.
+*
+*  Given:
+*     FWDS    d(6)      model coefficients
+*
+*  Returned:
+*     BKWDS   d(6)      inverse model
+*     J        i        status:  0 = OK, -1 = no inverse
+*
+*  The models relate two sets of [X,Y] coordinates as follows.
+*  Naming the elements of FWDS:
+*
+*     FWDS(1) = A
+*     FWDS(2) = B
+*     FWDS(3) = C
+*     FWDS(4) = D
+*     FWDS(5) = E
+*     FWDS(6) = F
+*
+*  where two sets of coordinates [X1,Y1] and [X2,Y1] are related
+*  thus:
+*
+*     X2 = A + B*X1 + C*Y1
+*     Y2 = D + E*X1 + F*Y1
+*
+*  the present routine generates a new set of coefficients:
+*
+*     BKWDS(1) = P
+*     BKWDS(2) = Q
+*     BKWDS(3) = R
+*     BKWDS(4) = S
+*     BKWDS(5) = T
+*     BKWDS(6) = U
+*
+*  such that:
+*
+*     X1 = P + Q*X2 + R*Y2
+*     Y1 = S + T*X2 + U*Y2
+*
+*  Two successive calls to sla_INVF will thus deliver a set
+*  of coefficients equal to the starting values.
+*
+*  To comply with the ANSI Fortran standard, FWDS and BKWDS must
+*  not be the same array, even though the routine is coded to
+*  work on the VAX and most other computers even if this rule
+*  is violated.
+*
+*  See also sla_FITXY, sla_PXY, sla_XY2XY, sla_DCMPF
+*
+*  P.T.Wallace   Starlink   11 April 1990
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION FWDS(6),BKWDS(6)
+      INTEGER J
+
+      DOUBLE PRECISION A,B,C,D,E,F,DET
+
+
+
+      A=FWDS(1)
+      B=FWDS(2)
+      C=FWDS(3)
+      D=FWDS(4)
+      E=FWDS(5)
+      F=FWDS(6)
+      DET=B*F-C*E
+      IF (DET.NE.0D0) THEN
+         BKWDS(1)=(C*D-A*F)/DET
+         BKWDS(2)=F/DET
+         BKWDS(3)=-C/DET
+         BKWDS(4)=(A*E-B*D)/DET
+         BKWDS(5)=-E/DET
+         BKWDS(6)=B/DET
+         J=0
+      ELSE
+         J=-1
+      END IF
+
+      END
diff --git a/src/slalib/kbj.f b/src/slalib/kbj.f
new file mode 100644
index 0000000..6a3ddb4
--- /dev/null
+++ b/src/slalib/kbj.f
@@ -0,0 +1,56 @@
+      SUBROUTINE sla_KBJ (JB, E, K, J)
+*+
+*     - - - -
+*      K B J
+*     - - - -
+*
+*  Select epoch prefix 'B' or 'J'
+*
+*  Given:
+*     JB     int     sla_DBJIN prefix status:  0=none, 1='B', 2='J'
+*     E      dp      epoch - Besselian or Julian
+*
+*  Returned:
+*     K      char    'B' or 'J'
+*     J      int     status:  0=OK
+*
+*  If JB=0, B is assumed for E < 1984D0, otherwise J.
+*
+*  P.T.Wallace   Starlink   31 July 1989
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER JB
+      DOUBLE PRECISION E
+      CHARACTER K*(*)
+      INTEGER J
+
+*  Preset status
+      J=0
+
+*  If prefix given expressly, use it
+      IF (JB.EQ.1) THEN
+         K='B'
+      ELSE IF (JB.EQ.2) THEN
+         K='J'
+
+*  If no prefix, examine the epoch
+      ELSE IF (JB.EQ.0) THEN
+
+*     If epoch is pre-1984.0, assume Besselian;  otherwise Julian
+         IF (E.LT.1984D0) THEN
+            K='B'
+         ELSE
+            K='J'
+         END IF
+
+*  If illegal prefix, return error status
+      ELSE
+         K=' '
+         J=1
+      END IF
+
+      END
diff --git a/src/slalib/m2av.f b/src/slalib/m2av.f
new file mode 100644
index 0000000..1299ed9
--- /dev/null
+++ b/src/slalib/m2av.f
@@ -0,0 +1,59 @@
+      SUBROUTINE sla_M2AV (RMAT, AXVEC)
+*+
+*     - - - - -
+*      M 2 A V
+*     - - - - -
+*
+*  From a rotation matrix, determine the corresponding axial vector
+*  (single precision)
+*
+*  A rotation matrix describes a rotation about some arbitrary axis.
+*  The axis is called the Euler axis, and the angle through which the
+*  reference frame rotates is called the Euler angle.  The axial
+*  vector returned by this routine has the same direction as the
+*  Euler axis, and its magnitude is the Euler angle in radians.  (The
+*  magnitude and direction can be separated by means of the routine
+*  sla_VN.)
+*
+*  Given:
+*    RMAT   r(3,3)   rotation matrix
+*
+*  Returned:
+*    AXVEC  r(3)     axial vector (radians)
+*
+*  The reference frame rotates clockwise as seen looking along
+*  the axial vector from the origin.
+*
+*  If RMAT is null, so is the result.
+*
+*  P.T.Wallace   Starlink   11 April 1990
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL RMAT(3,3),AXVEC(3)
+
+      REAL X,Y,Z,S2,C2,PHI,F
+
+
+
+      X = RMAT(2,3)-RMAT(3,2)
+      Y = RMAT(3,1)-RMAT(1,3)
+      Z = RMAT(1,2)-RMAT(2,1)
+      S2 = SQRT(X*X+Y*Y+Z*Z)
+      IF (S2.NE.0.0) THEN
+         C2 = (RMAT(1,1)+RMAT(2,2)+RMAT(3,3)-1.0)
+         PHI = ATAN2(S2/2.0,C2/2.0)
+         F = PHI/S2
+         AXVEC(1) = X*F
+         AXVEC(2) = Y*F
+         AXVEC(3) = Z*F
+      ELSE
+         AXVEC(1) = 0.0
+         AXVEC(2) = 0.0
+         AXVEC(3) = 0.0
+      END IF
+
+      END
diff --git a/src/slalib/makefile.orig b/src/slalib/makefile.orig
new file mode 100644
index 0000000..ff61e16
--- /dev/null
+++ b/src/slalib/makefile.orig
@@ -0,0 +1,1426 @@
+#+
+#  Name:
+#     makefile
+#
+#  Version:
+#     Library makefile Mk V
+#
+#  Purpose:
+#     Build and install the SLALIB package.
+#
+#  Type of Module:
+#     Description file for the make utility.
+#
+#  Description:
+#     This description file is used by the make utility to build the
+#     SLALIB package from the distributed source files, to install
+#     the resulting system for use, and to perform other housekeeping
+#     tasks.
+#
+#  Invocation:
+#     This makefile is not intended to be used by make when invoked
+#     directly (although this is possible), but instead to be used via
+#     the accompanying mk script.  This script sets up a number of
+#     environment variables which are used as macros within the
+#     makefile and which accommodate differences between machines and
+#     operating systems (it invokes make with the -e option).  Please
+#     consult the mk script prologue for full details.
+#
+#  Targets:
+#     The following make targets are defined in this script for
+#     external use:
+#
+#        [help]
+#           This is the default target.  It outputs a message describing
+#           the mk script and lists the targets provided.
+#
+#        check
+#           Performs a simple check that all necessary source files are
+#           present, and displays the version number and current state
+#           of the package (built/installed/tested, etc.).
+#
+#        build
+#           Compiles the source files and creates all files needed
+#           prior to installing the package for use.
+#
+#        install
+#           Installs the package for use by putting the necessary files
+#           into sub-directories of the $INSTALL directory (the $HOME
+#           directory is used if the environment variable INSTALL is
+#           not defined).  Links to the installed files are left in the
+#           source directory.
+#
+#        deinstall
+#           Reverses the action of the install target, removing files
+#           from sub-directories of the $INSTALL directory and
+#           restoring them to the source directory (the $HOME directory
+#           is used by default if the environment variable INSTALL is
+#           not defined).
+#
+#        test
+#           Builds and runs a simple test program to check for correct
+#           installation of the package.
+#
+#        export
+#           Produces an export copy of the built package suitable for
+#           passing to another user.  A compressed tar file is created
+#           in the $EXPORT directory containing copies of the source
+#           files and built files for the package (the current
+#           directory is used by default if the environment variable
+#           EXPORT is not defined).  The package should normally be
+#           built, installed and tested (see above) before using this
+#           target.  After unpacking the exported file on a similar
+#           machine, the recipient may simply install it for use.
+#
+#        export_run
+#           Produces an export copy of the built package suitable for
+#           passing to another user.  A compressed tar file is created
+#           in the $EXPORT directory containing copies of the built
+#           files for the package (the current directory is used by
+#           default if the environment variable EXPORT is not defined).
+#           The package should normally be built, installed and tested
+#           (see above) before using this target.  After unpacking the
+#           exported file on a similar machine, the recipient may simply
+#           install it for use.
+#
+#        export_source
+#           Produces an export copy of the source for the package
+#           suitable for passing to another user to build (possibly on
+#           a different type of machine).  A compressed tar file is
+#           created in the $EXPORT directory containing copies of just
+#           the source files for the package (the current directory is
+#           used by default if the environment variable EXPORT is not
+#           defined).  After unpacking the exported file, the recipient
+#           must build the package before installing it for use.
+#
+#        clean
+#           Cleans up after building the package, removing all
+#           intermediate files created during the building process, but
+#           leaving the built files themselves.
+#
+#        unbuild
+#           Reverses the building process, removing all intermediate
+#           files along with all the built files.
+#
+#  External Dependencies:
+#     The SLALIB package depends on the following other Starlink
+#     packages which must previously have been installed into the
+#     appropriate sub-directories of the $STARLINK directory (/star is
+#     used if the environment variable STARLINK is not defined).
+#
+#        None.
+#
+#  Notes:
+#     This makefile uses the presence/absence of the hidden files
+#     .BUILT, .INSTALLED_$(SYSTEM) and .TESTED_$(SYSTEM) to record the
+#     current state of the system during housekeeping operations.
+#
+#  Implementation Deficiencies:
+#     The method of generating the list of external libraries passed to
+#     the $(BLD_SHR) command is still preliminary.
+#
+#  Copyright:
+#     Copyright (C) 1995 Rutherford Appleton Laboratory
+#
+#  Authors:
+#     RFWS: R.F.Warren-Smith (Starlink, RAL)
+#     PMA: P.M.Allan (Starlink, RAL)
+#     PTW: P.T.Wallace (Starlink, RAL)
+#     AJC: A.J.Chipperfield (Starlink, RAL)
+#     BLY: M.J.Bly (Starlink, RAL)
+#     {enter_new_authors_here}
+#
+#  History:
+#     1-DEC-1993 (RFWS/PMA):
+#        Starlink template.
+#     1-DEC-1993 (PTW):
+#        SLALIB version.
+#     18-JAN-1994 (PTW):
+#        Corrections to if statements.
+#     10-MAR-1994 (PTW):
+#        sla_RVLSR replaced by sla_RVLSRD and sla_RVLSRK
+#     8-AUG-1994 (PTW):
+#        New routines added: sla_DE2H, sla_DH2E, sla_DTPRD, sla_E2H,
+#        sla_H2E, sla_PRECL, sla_TPRD.  Version number changed to 1.3-4.
+#        Missing dependencies on source archive added.
+#     19-OCT-1994 (PTW):
+#        New routines added: sla_ALTAZ, sla_PDA2H, sla_PDQ2H.  Package
+#        version number changed to 1.4-1.  Library version number
+#        changed to 1.4.
+#     26-OCT-1994 (PTW):
+#        Package version number changed to 1.4-2.
+#     15-DEC-1994 (PTW):
+#        New routines added: sla_PLANET, sla_RDPLAN, sla_DMOON, sla_DT,
+#        sla_CLYD.  Package version number changed to 1.4-4.
+#     3-JAN-1995 (PTW):
+#        Package version number changed to 1.4-5.
+#     13-FEB-1995 (PTW):
+#        New routines added: sla_DTP2V, sla_DTPXYZ, sla_DV2TP, sla_TP2V,
+#        sla_TPXYZ, sla_V2TP.  Package version number changed to 1.4-6.
+#     20-FEB-1995 (PTW):
+#        Package version number changed to 1.4-7 (sla_OBS enhanced).
+#     23-MAR-1995 (PTW):
+#        Unnecessary creation of INSTALL_INC removed.
+#     05-JUN-1995 (PTW):
+#        Four routines replaced: sla_DTPRD, sla_DTPXYZ, sla_TPRD and
+#        sla_TPXYZ become sla_DTPS2C, sla_DTPXYZ, sla_TPS2C and sla_TPV2C.
+#        Package version number changed to 1.5-1.  Library version
+#        number changed to 1.5.
+#     06-JUN-1995 (BLY/AJC):
+#        Updated to match Mk IVa makefile standard.
+#     02-JUL-1995 (PTW):
+#        Package version number changed to 1.5-2.
+#     21-JUL-1995 (PTW):
+#        Package version number changed to 1.5-3.
+#     14-SEP-1995 (PTW):
+#        New routine added:  sla_GMSTA.
+#        Package version number changed to 1.6-1.
+#     04-OCT-1995 (PTW):
+#        New routine added:  sla_ATMDSP.
+#        Package version number changed to 1.6-2.
+#     14-NOV-1995 (PTW):
+#        Bug fix:  sla_DAT.
+#        Package version number changed to 1.6-3.
+#     21-FEB-1996 (PTW):
+#        New routine:  sla_POLMO.
+#        Bug fix:  sla_DC62S, sla_CC62S.
+#        Comment corrections:  sla_DH2E, sla_H2E.
+#        New, html-compatible, document:  SUN/67.34.
+#        Package version number changed to 1.6-4.
+#     04-MAR-1996 (BLY):
+#        Update makefile to Mk V specification.
+#        Add special HLINK macro definitions.
+#        No change to version number.
+#     24-APR-1996 (BLY):
+#        Integrate ix86_Linux version.
+#        Update version to v1.7-0.
+#     10-MAY-1996 (BLY):
+#        Update version to v1.7-1.  No changes to Fortran version.
+#     18-JUL-1996 (PTW):
+#        Comment corrections:  sla_DS2TP, sla_DV2TP, sla_S2TP, sla_V2TP
+#        New, html-compatible, document:  SUN/67.34.
+#        Package version number changed to 1.7-2.
+#     26-NOV-1996 (PTW):
+#        Minor corrections to sla_DV2TP and sla_V2TP.  In sla_OBS,
+#        revision of Parkes position and addition of ATNF Mopra.
+#        Package version number changed to 1.7-3.
+#     28-MAY-1997 (PTW):
+#        New routines:  sla_PLANEL, sla_PLANTE.
+#        Functionally enhanced:  sla_PLANET, sla_RDPLAN.
+#        Minor code improvements:  several.
+#        Comment corrections:  numerous.
+#        Revised document:  SUN/67.36.
+#        Package version number changed to 2.0-1.
+#     6-JAN-1998 (PTW):
+#        Functionally enhanced:  sla_DAT.
+#        Revised document:  SUN/67.38.
+#        Package version number changed to 2.0-3.
+#     15-APR-1998 (PTW):
+#        Code improvements:  sla_GMSTA.
+#        Revised document:  SUN/67.40.
+#        Package version number changed to 2.0-4.
+#     28-MAY-1998 (PTW):
+#        Code improvements:  sla_PLANEL.
+#        New routine:  sla_PV2EL
+#        Revised document:  SUN/67.41.
+#        Package version number changed to 2.1-0.
+#     14-JUL-1998 (PTW):
+#        Makefile updated - sla_PAV had been omitted.
+#     18-JUL-1998 (PTW):
+#        1999 January 1 leap second added to sla_DAT.
+#        Package version number changed to 2.1-1.
+#     11-AUG-1998 (PTW):
+#        Makefile updated - sla_DPAV had been omitted (!).
+#     30-SEP-1998 (PTW):
+#        New routines:  sla_FK52H, sla_H2FK5, sla_FK5HZ and sla_HFK5Z.
+#        Revised document:  SUN/67.43.
+#        Package version number changed to 2.2-0.
+#     19-MAR-1999 (PTW):
+#        New routines:  sla_EL2UE, sla_PERTEL, sla_PERTUE,
+#                       sla_PV2UE, sla_UE2EL and sla_UE2PV
+#        Revised document:  SUN/67.44.
+#        Package version number changed to 2.3-0.
+#     2-AUG-1999 (PTW):
+#        New routines:  sla_COMBN and sla_PERMUT
+#        Revised document:  SUN/67.45.
+#        Package version number changed to 2.4-0.
+#     29-OCT-1999 (PTW):
+#        The F_ROUTINES definition lacked entries for sla_EL2UE,
+#        sla_PERTEL, sla_PERTUE, sla_PV2UE, sla_UE2EL, sla_UE2PV,
+#        sla_COMBN and sla_PERMUT.
+#     {enter_further_changes_here}
+#
+#  Bugs:
+#     {note_any_bugs_here}
+#
+#-------------------------------------------------------------------------------
+
+#  Help target.
+#  ===========
+#
+#  This is the default target, so it appears first.
+
+#  Display information about the mk script and the make targets.
+
+help:
+	@ echo \
+   '   The makefile provided is intended to be used by the make utility when';\
+        echo \
+   '   invoked via the associated mk script.  This script defines environment';\
+        echo \
+   '   variables which are used by make to accommodate differing machine and';\
+        echo \
+   '   operating system characteristics.  Please see the mk script prologue';\
+        echo \
+   '   for full details.';\
+        echo;\
+        echo \
+   '   The following targets are provided:';\
+        echo;\
+        echo \
+   '      help          - Display this message';\
+        echo \
+   '      check         - Check source file presence and show current state';\
+        echo \
+   '      build         - Build the package from source';\
+        echo \
+   '      install       - Install the built package for use';\
+        echo \
+   '      deinstall     - Deinstall the package';\
+        echo \
+   '      test          - Perform a quick test of the installation';\
+        echo \
+   '      export        - Make a compressed tar file for exporting the'\
+   'built package';\
+        echo \
+   '                      complete with source and documentation';\
+        echo \
+   '      export_run    - Make a compressed tar file for exporting the'\
+   'built package';\
+        echo \
+   '                      with documentation but no source';\
+        echo \
+   '      export_source - Make a compressed tar file for exporting the'\
+   'source files';\
+        echo \
+   '      clean         - Tidy up after building the package';\
+        echo \
+   '      unbuild       - Remove all the built files';\
+        echo;\
+        echo \
+   '   To build and install the $(PACK_NAME) package on a supported system:';\
+        echo;\
+        echo \
+   '      mk build; mk install; mk test; mk clean';\
+        echo
+
+#-------------------------------------------------------------------------------
+
+#  Defaults.
+#  ========
+#
+#  This section defines default macros and should rarely need changing.
+#  The values given here should be overridden externally to adapt to
+#  the local system setup (either use the mk script or use environment
+#  variables and invoke "make" with the "-e" option).
+
+#  Name of computer hardware/OS combination.
+
+SYSTEM = unknown
+
+#  Name used to distinguish platform-specific source files.
+
+SOURCE_VARIANT = $(SYSTEM)
+
+#  Pathname of the root directory beneath which other Starlink software
+#  is currently installed.
+
+STARLINK = /star
+
+#  Pathnames of Starlink sub-directories that may be referenced when
+#  building this package.
+
+STAR_BIN = $(STARLINK)/bin
+STAR_DATES = $(STARLINK)/dates
+STAR_DOCS = $(STARLINK)/docs
+STAR_ETC = $(STARLINK)/etc
+STAR_HELP = $(STARLINK)/help
+STAR_INC = $(STARLINK)/include
+STAR_LIB = $(STARLINK)/lib
+
+#  Pathname of the root directory beneath which the built files for
+#  this package should be installed for use.  This defaults to the
+#  user's home directory.
+
+INSTALL = $(HOME)
+
+#  Pathname of the directory into which exported tar files will be
+#  placed.  This defaults to the current working directory.
+
+EXPORT = .
+
+#  Default macros for compiling C and Fortran source code.
+
+CC = c89
+CFLAGS = -O
+FC = fort77
+FFLAGS = -O
+
+#  Command for forming a link to a file.
+
+LINK = ln
+
+#  Command for "randomizing" an object library.  The default acts as a
+#  null command.
+
+RANLIB = :
+
+#  Commands for adding to and extracting from an archive file (.tar).
+
+TAR_IN = pax -w -v -x ustar -f
+TAR_OUT = pax -r -f
+
+#  Command for adding a file to an object archive (.a).
+
+AR_IN = ar -r
+
+#  Default file type extension for a shareable library and command for
+#  building a shareable library (the default acts as a null command).
+
+SHARE = .so
+BLD_SHR = :
+
+#  Default command for linking hypertext document to others, including those
+#  on the RAL document server.
+
+HLINK = :
+
+#-------------------------------------------------------------------------------
+################################################################################
+#
+#  Define package source files.
+#  ===========================
+#
+#  This section defines the set of source files for the package.
+
+#  Name of the package as specified in documentation
+#  The value is used in messages from make to the user.
+
+PACK_NAME = SLALIB
+
+#  Prefix for the package in lower-case as used in filenames etc.
+PKG_NAME = sla
+ 
+#  Prefix for the package in upper-case as used in include file links.
+PKG_LINK = SLA
+ 
+#  Version number (as in the documentation - i.e. not the same thing
+#  as the shared library version number).
+#
+#  The major component of the version number (before the dot) should
+#  normally only be incremented following major changes to the package.
+#  The minor version number (after the dot) is the number normally
+#  incremented following development which introduces new documented
+#  functionality.  Any revision number (appended after a dash) should
+#  be incremented for other minor changes (bug fixes, etc.) which do
+#  not merit documentation changes.
+
+PKG_VERS = 2.4-0
+
+#  Library version number.
+#
+#  n.b. Care needed - may affect existing applications.
+#
+#  The minor component of this number (following the dot) should be
+#  incremented whenever a new routine is added to a library or some
+#  other change is made such that programs built with the latest
+#  version would fail to run using an earlier version.  The major number
+#  should be incremented if a change is made such that existing
+#  programs would have to be re-built in order to work with the new
+#  version.
+
+LIB_VERS = 1.6
+
+#  List of files comprising the distributed source-only system.  This
+#  defines the minimum set of files required to rebuild completely the
+#  package from source (including this makefile, the associated mk
+#  script and any documentation files).
+
+SOURCE_FILES = $(PKG_NAME)_source.tar makefile mk $(DOCUMENTATION)
+
+#  List of public script files.  These are scripts which form part of
+#  the package and will be required by users of it.  They will be
+#  installed in the $(INSTALL_BIN) directory with execute permission
+#  set.
+
+PUBLIC_SCRIPTS = $(PKG_NAME)_link $(PKG_NAME)_link_adam
+
+#  Startup script.  This is the file that must be executed by a
+#  programmer using this package in order to define links to include
+#  files.  It is listed separately from the public scripts as it is
+#  edited by the installation procedure.
+
+STARTUP_SCRIPT =
+
+#  List of public include files.  These are include files which form
+#  part of the package and may be required by users of it.  They will be
+#  installed in the $(INSTALL_INC) directory.
+
+PUBLIC_INCLUDES =
+
+#  List of private include files.  These are additional include files
+#  which form part of the package and are required in order to build
+#  it, but which are not required by users of it.
+
+PRIVATE_INCLUDES =
+
+#  List of external include files.  These are files which are required
+#  in order to build the package but form part of other, externally
+#  installed packages.  This list should contain the names used to
+#  reference the files within the source code, not the actual names of
+#  the files.
+
+EXTERNAL_INCLUDES =
+
+#  List of Fortran routines required for building the package.  This is
+#  just a list of all the Fortran source files (excluding BLOCK DATA
+#  routines, which are treated separately).
+
+F_ROUTINES = \
+        addet.f  \
+        afin.f   \
+        airmas.f \
+        altaz.f  \
+        amp.f    \
+        ampqk.f  \
+        aop.f    \
+        aoppa.f  \
+        aoppat.f \
+        aopqk.f  \
+        atmdsp.f \
+        atms.f   \
+        atmt.f   \
+        av2m.f   \
+        bear.f   \
+        caf2r.f  \
+        caldj.f  \
+        calyd.f  \
+        cc2s.f   \
+        cc62s.f  \
+        cd2tf.f  \
+        cldj.f   \
+        clyd.f   \
+        combn.f  \
+        cr2af.f  \
+        cr2tf.f  \
+        cs2c.f   \
+        cs2c6.f  \
+        ctf2d.f  \
+        ctf2r.f  \
+        daf2r.f  \
+        dafin.f  \
+        dat.f    \
+        dav2m.f  \
+        dbear.f  \
+        dbjin.f  \
+        dc62s.f  \
+        dcc2s.f  \
+        dcmpf.f  \
+        dcs2c.f  \
+        dd2tf.f  \
+        de2h.f   \
+        deuler.f \
+        dfltin.f \
+        dh2e.f   \
+        dimxv.f  \
+        djcal.f  \
+        djcl.f   \
+        dm2av.f  \
+        dmat.f   \
+        dmoon.f  \
+        dmxm.f   \
+        dmxv.f   \
+        dpav.f   \
+        dr2af.f  \
+        dr2tf.f  \
+        drange.f \
+        dranrm.f \
+        ds2c6.f  \
+        ds2tp.f  \
+        dsep.f   \
+        dt.f     \
+        dtf2d.f  \
+        dtf2r.f  \
+        dtp2s.f  \
+        dtp2v.f  \
+        dtps2c.f \
+        dtpv2c.f \
+        dtt.f    \
+        dv2tp.f  \
+        dvdv.f   \
+        dvn.f    \
+        dvxv.f   \
+        e2h.f    \
+        earth.f  \
+        ecleq.f  \
+        ecmat.f  \
+        ecor.f   \
+        eg50.f   \
+        el2ue.f  \
+        epb.f    \
+        epb2d.f  \
+        epco.f   \
+        epj.f    \
+        epj2d.f  \
+        eqecl.f  \
+        eqeqx.f  \
+        eqgal.f  \
+        etrms.f  \
+        euler.f  \
+        evp.f    \
+        fitxy.f  \
+        fk425.f  \
+        fk45z.f  \
+        fk524.f  \
+        fk52h.f  \
+        fk54z.f  \
+        fk5hz.f  \
+        flotin.f \
+        galeq.f  \
+        galsup.f \
+        ge50.f   \
+        geoc.f   \
+        gmst.f   \
+        gmsta.f  \
+        h2e.f    \
+        h2fk5.f  \
+        hfk5z.f  \
+        idchf.f  \
+        idchi.f  \
+        imxv.f   \
+        intin.f  \
+        invf.f   \
+        kbj.f    \
+        m2av.f   \
+        map.f    \
+        mappa.f  \
+        mapqk.f  \
+        mapqkz.f \
+        moon.f   \
+        mxm.f    \
+        mxv.f    \
+        nut.f    \
+        nutc.f   \
+        oap.f    \
+        oapqk.f  \
+        obs.f    \
+        pa.f     \
+        pav.f    \
+        pcd.f    \
+        pda2h.f  \
+        pdq2h.f  \
+        permut.f \
+        pertel.f \
+        pertue.f \
+        planel.f \
+        planet.f \
+        plante.f \
+        pm.f     \
+        polmo.f  \
+        prebn.f  \
+        prec.f   \
+        precl.f  \
+        preces.f \
+        prenut.f \
+        pv2el.f  \
+        pv2ue.f  \
+        pvobs.f  \
+        pxy.f    \
+        range.f  \
+        ranorm.f \
+        rcc.f    \
+        rdplan.f \
+        refco.f  \
+        refro.f  \
+        refv.f   \
+        refz.f   \
+        rverot.f \
+        rvgalc.f \
+        rvlg.f   \
+        rvlsrd.f \
+        rvlsrk.f \
+        s2tp.f   \
+        sep.f    \
+        smat.f   \
+        subet.f  \
+        supgal.f \
+        svd.f    \
+        svdcov.f \
+        svdsol.f \
+        tp2s.f   \
+        tp2v.f   \
+        tps2c.f  \
+        tpv2c.f  \
+        ue2el.f  \
+        ue2pv.f  \
+        unpcd.f  \
+        v2tp.f   \
+        vdv.f    \
+        vn.f     \
+        vxv.f    \
+        xy2xy.f  \
+        zd.f
+
+#  List of Fortran BLOCK DATA routines.
+
+BLOCK_DATA =
+
+#  List of platform specific Fortran routines.  The source tar file will
+#  contain a version of these files for each set of platforms.  The names
+#  given here are the general version of the file, e.g. pkg_open.f.  The
+#  names in the tar file will be pkg_open.f_sun4, pkg_open.f_mips, etc.
+
+PLATFORM_F = \
+        gresid.f \
+        random.f \
+        wait.f
+
+#  C routines required for building the package.  This is just a list of
+#  all the C source files.
+
+C_ROUTINES =
+
+#  Lists of Latex and hypertext documents.
+
+LATEX_DOCS = sun67.tex
+HYPERTEXT_DOCS = sun67.htx
+
+#  List of documentation files.
+
+DOCUMENTATION = $(LATEX_DOCS) $(HYPERTEXT_DOCS:.htx=.htx_tar) \
+$(PKG_NAME).news read.me
+
+################################################################################
+#-------------------------------------------------------------------------------
+
+#  Define files required for building the package.
+#  ==============================================
+#
+#  This section defines the set of files produced from the source files
+#  when the package is built and installed.
+
+#  Use only .o, .c and .f suffix rules.
+
+.SUFFIXES:
+.SUFFIXES: .o .c .f
+
+#  List of files which must be built from the source files before the
+#  package can be installed for use.  This should comprise all the files
+#  that are required to use the package (but excluding the date stamp
+#  file).
+
+BUILT_FILES = $(PUBLIC_SCRIPTS) $(PUBLIC_INCLUDES) $(OBJECT_LIBRARIES) \
+$(SHAREABLE_LIBRARIES) $(STARTUP_SCRIPT)
+
+#  List of links used to access include files during compilation.  This
+#  should comprise all the external include files and any other include
+#  files whose names do not exactly match the names used in the source
+#  code.
+
+INCLUDE_LINKS = $(EXTERNAL_INCLUDES)
+
+#  Rules to set up links to locate each of the above include files.
+
+#  Rules for extracting source files from the source archive.
+
+$(PUBLIC_SCRIPTS) $(PUBLIC_INCLUDES) $(F_ROUTINES) \
+$(BLOCK_DATA) $(C_ROUTINES) $(STARTUP_SCRIPT):
+	$(TAR_OUT) $(PKG_NAME)_source.tar $@
+	@ if test -f $@; then :;\
+           else echo $@ is not in the tar file; exit 1; fi
+
+#  Rules for extracting platform specific source files from the source
+#  archive.
+
+#  It is quite likely that there are no platform-specific source files
+#  and that the macro PLATFORM_F is empty. To prevent a syntax error in
+#  make, a dummy target is present.
+
+$(PLATFORM_F) dummy_target1:
+	$(TAR_OUT) $(PKG_NAME)_source.tar $@_$(SOURCE_VARIANT)
+	@ if test -f $@_$(SOURCE_VARIANT); then :;\
+           else echo $@_$(SOURCE_VARIANT) is not in the tar file; exit 1; fi
+	mv $@_$(SOURCE_VARIANT) $@
+
+#  List of object files produced by compiling the source code and rules
+#  for performing the compilations.
+
+OBJECT_FILES = $(BLOCK_DATA:.f=.o) $(F_ROUTINES:.f=.o) \
+               $(PLATFORM_F:.f=.o) $(C_ROUTINES:.c=.o)
+
+.c.o:
+	$(CC) $(CFLAGS) -c $<
+.f.o:
+	$(FC) $(FFLAGS) -c $<
+
+#  List of object library files to be built and rules for building
+#  them.
+
+OBJECT_LIBRARIES = lib$(PKG_NAME).a
+
+lib$(PKG_NAME).a: $(OBJECT_FILES)
+	$(AR_IN) $@ $?
+	$(RANLIB) $@
+
+#  List of shareable library files to be built and rules for building
+#  them. The third argument to $(BLD_SHR) should provide the information
+#  necessary to link any libraries called by this package.
+
+SHAREABLE_LIBRARIES = lib$(PKG_NAME)$(SHARE)
+
+lib$(PKG_NAME)$(SHARE): $(OBJECT_FILES)
+	touch $@
+	$(BLD_SHR) $@ '$(OBJECT_FILES)'
+
+#  Name of the date stamp file.  This is used to record the time of the
+#  most recent build for use in subsequent operations that require it.
+#  There must be no rule for generating this file; it is updated only
+#  as a side effect of building the package.
+
+DATE_STAMP = $(PKG_NAME)_datestamp
+
+#  Pathnames of directories into which files may be placed when the
+#  package is installed.
+
+INSTALL_BIN = $(INSTALL)/bin
+INSTALL_DATES = $(INSTALL)/dates
+INSTALL_DOCS = $(INSTALL)/docs
+INSTALL_ETC = $(INSTALL)/etc
+INSTALL_HELP = $(INSTALL)/help
+INSTALL_INC = $(INSTALL)/include
+INSTALL_LIB = $(INSTALL)/lib
+INSTALL_SHARE = $(INSTALL)/share
+
+#  List of directories actually used for installation (selected from
+#  those above) and rules to create them.
+
+INSTALL_DIRS = $(INSTALL_BIN) $(INSTALL_DATES) $(INSTALL_DOCS) $(INSTALL_LIB) \
+$(INSTALL_SHARE)
+
+$(INSTALL_DIRS):
+	mkdir -p $@
+
+#-------------------------------------------------------------------------------
+
+#  Primary targets.
+#  ===============
+#
+#  These are the targets intended for normal external use (apart from
+#  help, which appears at the start of the file).
+
+#  check: Check source file presence and show current state.
+#  --------------------------------------------------------
+
+check:
+	@ echo
+	@ echo \
+   '*** This is $(PACK_NAME) version V$(PKG_VERS) on system $(SYSTEM)'
+	@ echo
+	@ nosource='';\
+          for f in $(SOURCE_FILES); do \
+             if test ! -f $$f; then \
+                nosource='1';\
+                break;\
+             else :; fi;\
+          done;\
+          if test -n "$$nosource"; then \
+             echo '    Source files are NOT present';\
+          else \
+             echo '    All essential source files are present';\
+          fi
+	@ echo
+#
+#  Display the current state.
+	@ if test -f .BUILT;\
+          then echo '    The package is currently:  built for system'\
+             `cat .BUILT`;\
+          else echo '    The package is currently:  not built';fi
+	@ if test -f .INSTALLED_$(SYSTEM);\
+          then echo '                               installed in'\
+             `cat .INSTALLED_$(SYSTEM)`;\
+          else echo '                               not installed';fi
+	@ if test -f .TESTED_$(SYSTEM);\
+          then echo '                               tested';\
+          else echo '                               not tested';fi
+	@ echo
+	@ if test -f .BUILT;\
+          then if test "$(SYSTEM)" != "`cat .BUILT`";\
+             then echo '***  WARNING  ***';\
+                echo \
+'    The package is built for a system other than the current one';\
+                echo ;\
+             else :;fi;\
+          else :;fi
+
+#  build: Build the system.
+#  -----------------------
+#
+#  Compile the source and build the required files in the source
+#  directory.
+
+#  The build target first checks that the package is not installed.  If
+#  not, it then causes the .BUILT target to be made which ensures that
+#  the package has been built.
+
+build:
+	@ if test -f .INSTALLED_$(SYSTEM); then \
+           echo;\
+           echo \
+   '*** The $(PACK_NAME) package is currently installed -- please use the';\
+           echo '    "deinstall" target before re-building it';\
+           echo;\
+        elif $(MAKE) .BUILT; then \
+           echo;\
+           echo '*** The $(PACK_NAME) package has been built';\
+           echo;\
+        else \
+           echo;\
+           echo '*** "make" failed building the $(PACK_NAME) package';\
+           echo;\
+           exit 1;\
+        fi
+
+#  The .BUILT target records the time of the most recent build which
+#  modified any of the built files.  It depends on all the built files
+#  being up to date (which causes them to be built).
+
+.BUILT: $(BUILT_FILES)
+#
+#  Enter information about the current machine and build environment
+#  into the date stamp file.
+	@ echo 'Package : $(PACK_NAME)'        >$(DATE_STAMP)
+	@ echo 'Version : V$(PKG_VERS)'       >>$(DATE_STAMP)
+	@ echo 'Library : V$(LIB_VERS)'       >>$(DATE_STAMP)
+	@ echo ''                             >>$(DATE_STAMP)
+	@ echo "Built by: $(USER) on node `uname -n`" \
+                                              >>$(DATE_STAMP)
+	@ echo "On      : `date`"             >>$(DATE_STAMP)
+	@ echo ''                             >>$(DATE_STAMP)
+	@ echo \
+  "Machine : `uname -m` running `uname -s` `uname -v` (release `uname -r`)" \
+                                              >>$(DATE_STAMP)
+	@ echo ''                             >>$(DATE_STAMP)
+	@ echo 'make macros:'                 >>$(DATE_STAMP)
+	@ echo ''                             >>$(DATE_STAMP)
+	@ echo '   SYSTEM  : $(SYSTEM)'       >>$(DATE_STAMP)
+	@ echo ''                             >>$(DATE_STAMP)
+	@ echo '   EXPORT  : $(EXPORT)'       >>$(DATE_STAMP)
+	@ echo '   INSTALL : $(INSTALL)'      >>$(DATE_STAMP)
+	@ echo '   STARLINK: $(STARLINK)'     >>$(DATE_STAMP)
+	@ echo ''                             >>$(DATE_STAMP)
+	@ echo '   AR_IN   : $(AR_IN)'        >>$(DATE_STAMP)
+	@ echo '   BLD_SHR : $(BLD_SHR)'      >>$(DATE_STAMP)
+	@ echo '   CC      : $(CC)'           >>$(DATE_STAMP)
+	@ echo '   CFLAGS  : $(CFLAGS)'       >>$(DATE_STAMP)
+	@ echo '   FC      : $(FC)'           >>$(DATE_STAMP)
+	@ echo '   FFLAGS  : $(FFLAGS)'       >>$(DATE_STAMP)
+	@ echo '   LINK    : $(LINK)'         >>$(DATE_STAMP)
+	@ echo '   RANLIB  : $(RANLIB)'       >>$(DATE_STAMP)
+	@ echo '   SHARE   : $(SHARE)'        >>$(DATE_STAMP)
+	@ echo '   SOURCE_VARIANT: $(SOURCE_VARIANT)' \
+                                              >>$(DATE_STAMP)
+	@ echo '   TAR_IN  : $(TAR_IN)'       >>$(DATE_STAMP)
+	@ echo '   TAR_OUT : $(TAR_OUT)'      >>$(DATE_STAMP)
+	@ echo ''                             >>$(DATE_STAMP)
+#
+#  Record completion of the build.
+	@ echo '$(SYSTEM)' > .BUILT
+
+#  install: Install the package for use.
+#  ------------------------------------
+#
+#  Copy the built files to their installation directories, from where
+#  they may be accessed.
+
+#  The install target first checks if any part of the package is
+#  already installed.  If not, it checks that the system is built for this
+#  SYSTEM and, if it is, causes the .INSTALLED_$(SYSTEM) target to be made
+#  which performs the installation.
+
+install:
+	@ if test -f .INSTALLED_$(SYSTEM); then \
+           echo;\
+           echo \
+   '*** The $(PACK_NAME) package has already been installed -- please use the';\
+           echo \
+   '    "deinstall" target first if you wish to reinstall it';\
+           echo;\
+        elif test -f .BUILT; then \
+           if test "`cat .BUILT`" = "$(SYSTEM)"; then \
+              if $(MAKE) .INSTALLED_$(SYSTEM); then \
+                 echo;\
+                 echo \
+   '*** The $(PACK_NAME) package has been installed in directory $(INSTALL)';\
+                 echo;\
+              else \
+                 echo;\
+                 echo \
+   '*** "make" failed installing the $(PACK_NAME) package in directory $(INSTALL)';\
+                 echo;\
+                 exit 1;\
+              fi;\
+           else \
+              echo;\
+              echo \
+   "*** The $(PACK_NAME) package is built for system `cat .BUILT` -"\
+   'so cannot be installed on system $(SYSTEM)';\
+              echo;\
+              exit 1;\
+           fi;\
+        else \
+           echo;\
+           echo \
+   '*** The $(PACK_NAME) package is not built, so cannot be installed';\
+           echo;\
+           exit 1;\
+        fi
+
+#  The .INSTALLED_$(SYSTEM) target copies each file from the source
+#  directory using "cp -p" to preserve its date, and replaces each
+#  original file by a link to the installed copy.
+
+.INSTALLED_$(SYSTEM): $(INSTALL_DIRS)
+#
+#  Create .INSTALLED_$(SYSTEM), containing $INSTALL, to record that the
+#  package is installed (at least in part).
+	@ echo $(INSTALL) > .INSTALLED_$(SYSTEM)
+#
+#  Install the public scripts, giving them world execute permission.
+	for f in $(PUBLIC_SCRIPTS) ""; do \
+           if test -n "$$f"; then \
+              cp -p $$f $(INSTALL_BIN);\
+              chmod 755 $(INSTALL_BIN)/$$f;\
+              rm -f $$f;\
+              $(LINK) $(INSTALL_BIN)/$$f $$f;\
+           else :; fi;\
+        done
+#
+#  Install the public include files, giving them world read permission.
+	for f in $(PUBLIC_INCLUDES) ""; do \
+           if test -n "$$f"; then \
+              cp -p $$f $(INSTALL_INC);\
+              chmod 644 $(INSTALL_INC)/$$f;\
+              rm -f $$f;\
+              $(LINK) $(INSTALL_INC)/$$f $$f;\
+           else :; fi;\
+        done
+#
+#  Install the object libraries, giving them world read permission.
+	for f in $(OBJECT_LIBRARIES) ""; do \
+           if test -n "$$f"; then \
+              cp -p $$f $(INSTALL_LIB);\
+              chmod 644 $(INSTALL_LIB)/$$f;\
+              rm -f $$f;\
+              $(LINK) $(INSTALL_LIB)/$$f $$f;\
+           else :; fi;\
+        done
+#
+#  Install shareable libraries, giving them read permission (unless
+#  they are dummy, zero size, files in which case they are left in
+#  place).
+	for f in $(SHAREABLE_LIBRARIES) ""; do \
+           if test -n "$$f" -a -s "$$f"; then \
+              cp -p $$f $(INSTALL_SHARE);\
+              chmod 755 $(INSTALL_SHARE)/$$f;\
+              rm -f $$f;\
+              $(LINK) $(INSTALL_SHARE)/$$f $$f;\
+           else :; fi;\
+        done
+#
+#  Install the package startup script.  The name of the directory
+#  containing the installed public include files must be edited into
+#  this, and execute permission given.  Leave the original file in
+#  place.
+	if test -n "$(STARTUP_SCRIPT)"; then \
+           sed -e 's#LINK#$(LINK)#' -e s#INSTALL_INC#$(INSTALL_INC)# \
+              $(STARTUP_SCRIPT) >$(INSTALL_BIN)/$(STARTUP_SCRIPT) ;\
+           chmod 755 $(INSTALL_BIN)/$(STARTUP_SCRIPT) ;\
+        else :; fi
+#
+#  Install the Latex documentation, giving it world read permission,
+#  leaving the source copy in place.
+	for f in $(LATEX_DOCS) ""; do \
+           if test -n "$$f"; then \
+              cp -p $$f $(INSTALL_DOCS);\
+              chmod 644 $(INSTALL_DOCS)/$$f;\
+           else :; fi;\
+        done
+#
+#  Install any hypertext documents, giving world read access to all the files
+#  they contain and linking with other documents.
+	if test -n "$(HYPERTEXT_DOCS)"; then \
+           pwd=`pwd`;\
+           (cd $(INSTALL_DOCS);\
+           for f in $(HYPERTEXT_DOCS) ""; do \
+              if test -n "$$f"; then\
+                 $(TAR_OUT) $$pwd/$${f}_tar;\
+                 chmod 755 `find $$f -type d -print`;\
+                 chmod 644 `find $$f ! -type d -print`;\
+                 touch $$f;\
+              else :; fi;\
+           done);\
+           HTX_PATH='$(STAR_DOCS):$(STAR_HELP)';\
+           export HTX_PATH;\
+           $(HLINK) $(INSTALL_DOCS) $(INSTALL_HELP);\
+        fi;
+#
+#  Install the date stamp file and make it read-only to prevent its
+#  date being changed.
+	cp -p $(DATE_STAMP) $(INSTALL_DATES)
+	chmod 444 $(INSTALL_DATES)/$(DATE_STAMP)
+	chmod 644 $(DATE_STAMP)
+	rm $(DATE_STAMP)
+	$(LINK) $(INSTALL_DATES)/$(DATE_STAMP) $(DATE_STAMP)
+
+#  deinstall: Deinstall the package.
+#  --------------------------------
+#
+#  Reverse the action of the install target, removing the installed
+#  files and returning them to the source directory.
+
+#  The deinstall target checks that the package is installed in the INSTALL
+#  directory.  If so, it causes the do_deinstall target to be made which
+#  performs the deinstallation.
+
+deinstall:
+	@ if test ! -f .INSTALLED_$(SYSTEM); then \
+           echo;\
+           echo '*** The $(PACK_NAME) package is not currently installed';\
+           echo;\
+        else \
+           if test "`cat .INSTALLED_$(SYSTEM)`" = "$(INSTALL)"; then \
+              if $(MAKE) do_deinstall; then \
+                 echo;\
+                 echo \
+'*** The $(PACK_NAME) package has been deinstalled from directory $(INSTALL)';\
+                 echo;\
+              else \
+                 echo;\
+                 echo \
+'*** "make" failed deinstalling the $(PACK_NAME) package from directory $(INSTALL)';\
+                 echo;\
+                 exit 1;\
+              fi;\
+           else \
+              echo;\
+              echo \
+"*** The $(PACK_NAME) package is installed in `cat .INSTALLED_$(SYSTEM)`";\
+              echo \
+"*** and not in your INSTALL directory ($(INSTALL))";\
+              echo '*** Not deinstalled';\
+              exit 1;\
+           fi;\
+        fi
+
+#  The do_deinstall target (which should never exist) checks that an
+#  installed version of each file exists (in case an install failed
+#  part of the way through) and returns it to the source directory,
+#  using "cp -p" to preserve file dates.  Links are removed from the
+#  source directory before copying.
+
+do_deinstall:
+#
+#  Note the package will need to be tested again.
+	@- if test -f .TESTED_$(SYSTEM); then rm -f .TESTED_$(SYSTEM); else :; fi
+#
+#  Deinstall the public script files, if installed versions exist.
+	- for f in $(PUBLIC_SCRIPTS) ""; do \
+           if test -n "$$f" -a -f $(INSTALL_BIN)/$$f; then \
+              rm -f $$f;\
+              cp -p $(INSTALL_BIN)/$$f .;\
+              rm -f $(INSTALL_BIN)/$$f;\
+           else :; fi;\
+        done
+#
+#  Deinstall the public include files, if installed versions exist.
+	- for f in $(PUBLIC_INCLUDES) ""; do \
+           if test -n "$$f" -a -f $(INSTALL_INC)/$$f; then \
+              rm -f $$f;\
+              cp -p $(INSTALL_INC)/$$f .;\
+              rm -f $(INSTALL_INC)/$$f;\
+           else :; fi;\
+        done
+#
+#  Deinstall the object libraries, if installed versions exist.
+	- for f in $(OBJECT_LIBRARIES) ""; do \
+           if test -n "$$f" -a -f $(INSTALL_LIB)/$$f; then \
+              rm -f $$f;\
+              cp -p $(INSTALL_LIB)/$$f .;\
+              rm -f $(INSTALL_LIB)/$$f;\
+           else :; fi;\
+        done
+#
+#  Deinstall the shareable libraries, if installed versions exist.
+	- for f in $(SHAREABLE_LIBRARIES) ""; do \
+           if test -n "$$f" -a -f $(INSTALL_SHARE)/$$f; then \
+              rm -f $$f;\
+              cp -p $(INSTALL_SHARE)/$$f .;\
+              rm -f $(INSTALL_SHARE)/$$f;\
+           else :; fi;\
+        done
+#
+#  Deinstall the package startup file.  Since it will have been edited
+#  during installation, we remove the installed copy, if present, and
+#  then ensure that the original exists.
+	- if test -n "$(STARTUP_SCRIPT)"; then \
+           if test -f $(INSTALL_BIN)/$(STARTUP_SCRIPT); then\
+              rm -f $(INSTALL_BIN)/$(STARTUP_SCRIPT);\
+           else :; fi ;\
+           $(MAKE) $(STARTUP_SCRIPT);\
+        else :; fi
+#
+#  Deinstall the Latex documentation, if installed versions exist.
+	- for f in $(LATEX_DOCS) ""; do \
+           if test -n "$$f" -a -f $(INSTALL_DOCS)/$$f; then \
+              rm -f $(INSTALL_DOCS)/$$f;\
+           else :; fi;\
+        done
+#
+#  Deinstall any hypertext documents,  and relink the hypertext if required.
+	- if test -n "$(HYPERTEXT_DOCS)"; then \
+           for f in $(HYPERTEXT_DOCS) ""; do \
+              if test -n "$$f" -a -d $(INSTALL_DOCS)/$$f; then \
+                 rm -f -r $(INSTALL_DOCS)/$$f;\
+              else :; fi;\
+           done;\
+           HTX_PATH='$(STAR_DOCS):$(STAR_HELP)';\
+           export HTX_PATH;\
+           $(HLINK) $(INSTALL_DOCS) $(INSTALL_HELP);\
+        fi
+#
+#  Deinstall the date stamp file after setting its protection so it may
+#  be removed.
+	- if test -f $(INSTALL_DATES)/$(DATE_STAMP); then \
+           chmod 644 $(DATE_STAMP); rm $(DATE_STAMP);\
+           chmod 644 $(INSTALL_DATES)/$(DATE_STAMP);\
+           cp -p $(INSTALL_DATES)/$(DATE_STAMP) .;\
+           rm $(INSTALL_DATES)/$(DATE_STAMP);\
+        else :; fi
+#
+#  Note the system is no longer installed.  Re-create .BUILT, since we have
+#  returned the built files to the source directory but an unbuild may have
+#  been done.
+	@- rm -f .INSTALLED_$(SYSTEM) 1>/dev/null 2>/dev/null
+	@ echo '$(SYSTEM)' > .BUILT
+
+#  test: Perform an installation test.
+#  ----------------------------------
+#
+#  Check that installed files are in their correct places and that a
+#  simple test program will run correctly.
+
+#  The test target checks that the package is currently installed.  If
+#  so, it causes the do_test target to be made, which performs the
+#  installation test.
+
+test:
+	@ if test ! -f .INSTALLED_$(SYSTEM); then \
+           echo;\
+           echo '*** The $(PACK_NAME) package is not currently installed';\
+           echo;\
+        elif $(MAKE) do_test; then\
+           echo;\
+           echo \
+           '*** Installation test for the $(PACK_NAME) package has been run';\
+           echo;\
+        else \
+           echo;\
+           echo \
+           '*** Installation test for the $(PACK_NAME) package failed';\
+           echo;\
+           exit 1;\
+        fi
+
+#  The do_test target performs the installation test. A file named do_test
+#  should never exist.
+
+do_test: $(EXTERNAL_INCLUDES)
+#
+#  Note the test has not yet succeeded.
+	@- if test -f .TESTED_$(SYSTEM); then rm -f .TESTED_$(SYSTEM); else :; fi
+#
+#  Extract the test program from the archive and set up new links for
+#  the include files which point at the installed versions.  Remove any
+#  pre-existing links first if necessary.
+	$(TAR_OUT) $(PKG_NAME)_source.tar $(PKG_NAME)_test.f
+	@ if test -f $(PKG_NAME)_test.f; then :;\
+           else echo $(PKG_NAME)_test.f is not in the tar file; exit 1; fi
+#
+#  Build the test program, ensuring that the installed version of the library
+#  and link files are used.
+	$(FC) $(FFLAGS) $(PKG_NAME)_test.f -L$(INSTALL_LIB) -L$(STAR_LIB) \
+              `$(INSTALL_BIN)/$(PKG_NAME)_link` -o $(PKG_NAME)_test
+#
+#  Remove the test program source and the include file links used to
+#  build it.
+	rm -f $(PKG_NAME)_test.f $(EXTERNAL_INCLUDES)
+#
+#  Execute the test program and remove the binary file when done.  Note
+#  that any external mechanism for locating shareable libraries (e.g. a
+#  search path) must previously have been set up.
+	./$(PKG_NAME)_test
+	rm -f $(PKG_NAME)_test
+#
+#  Note the test has been run.
+	@ touch .TESTED_$(SYSTEM)
+
+#  export: Export the installed system.
+#  -----------------------------------
+#
+#  Export the source plus all the built files to a new user.
+
+#  The export target depends on the resulting compressed tar file being
+#  up to date.
+
+export: $(EXPORT)/$(PKG_NAME)_$(SYSTEM).tar.Z
+	@ echo
+	@ echo \
+'*** Export copy of the built $(PACK_NAME) package is in the compressed'
+	@ echo \
+'    tar file $(EXPORT)/$(PKG_NAME)_$(SYSTEM).tar.Z'
+	@ echo
+
+#  The compressed tar file is up to date if it exists and is more
+#  recent than all the source files and the date stamp file (which
+#  records the time of the last build which modified any files).
+
+$(EXPORT)/$(PKG_NAME)_$(SYSTEM).tar.Z: $(SOURCE_FILES) $(DATE_STAMP)
+#
+#  Issue a warning if the package has not been tested.
+	@ if test ! -f .TESTED_$(SYSTEM); then \
+           echo;\
+           echo '*** Warning: the $(PACK_NAME) package has not been tested';\
+           echo;\
+        else :; fi
+#
+#  Remove any pre-existing tar files before creating new ones.
+	if test -f $(EXPORT)/$(PKG_NAME)_$(SYSTEM).tar.Z; then \
+           rm -f $(EXPORT)/$(PKG_NAME)_$(SYSTEM).tar.Z; else :; fi
+	$(TAR_IN) - $(SOURCE_FILES) $(BUILT_FILES) $(DATE_STAMP) .BUILT \
+           | compress -v > $(EXPORT)/$(PKG_NAME)_$(SYSTEM).tar.Z
+
+#  export_run: Export the built system (without source).
+#  -----------------------------------------------------
+#
+#  Export all the built files to a new user.
+
+#  The export_run target depends on the resulting compressed tar file being
+#  up to date.
+
+export_run: $(EXPORT)/$(PKG_NAME)_$(SYSTEM)_run.tar.Z
+	@ echo
+	@ echo \
+'*** Export copy of the "runtime" $(PACK_NAME) package is in the compressed'
+	@ echo \
+'    tar file $(EXPORT)/$(PKG_NAME)_$(SYSTEM)_run.tar.Z'
+	@ echo
+
+#  The compressed tar file is up to date if it exists and is more
+#  recent than all the source files and the date stamp file (which
+#  records the time of the last build which modified any files).
+
+$(EXPORT)/$(PKG_NAME)_$(SYSTEM)_run.tar.Z: $(SOURCE_FILES) $(DATE_STAMP)
+#
+#  Issue a warning if the package has not been tested.
+	@ if test ! -f .TESTED_$(SYSTEM); then \
+           echo;\
+           echo '*** Warning: the $(PACK_NAME) package has not been tested';\
+           echo;\
+        else :; fi
+#
+#  Remove any pre-existing tar files before creating new ones.
+	if test -f $(EXPORT)/$(PKG_NAME)_$(SYSTEM)_run.tar.Z; then \
+           rm -f $(EXPORT)/$(PKG_NAME)_$(SYSTEM)_run.tar.Z; else :; fi
+	$(TAR_IN) - mk makefile $(DOCUMENTATION) $(BUILT_FILES) \
+           $(DATE_STAMP) .BUILT \
+           | compress -v > $(EXPORT)/$(PKG_NAME)_$(SYSTEM)_run.tar.Z
+
+#  export_source: Export the source.
+#  --------------------------------
+#
+#  Export the source files only to a new user.
+
+#  This target depends on the resulting compressed tar file being up to
+#  date.
+
+export_source: $(EXPORT)/$(PKG_NAME).tar.Z
+	@ echo
+	@ echo \
+'*** Export copy of the $(PACK_NAME) package source is in the compressed'
+	@ echo \
+'    tar file $(EXPORT)/$(PKG_NAME).tar.Z'
+	@ echo
+
+#  The compressed tar file is up to date if it exists and is more
+#  recent than all the source files.
+
+$(EXPORT)/$(PKG_NAME).tar.Z: $(SOURCE_FILES)
+#
+#  Remove any pre-existing tar files before creating new ones.
+	if test -f $(EXPORT)/$(PKG_NAME).tar.Z; then \
+           rm -f $(EXPORT)/$(PKG_NAME).tar.Z; else :; fi
+	$(TAR_IN) - $(SOURCE_FILES) \
+           | compress -v > $(EXPORT)/$(PKG_NAME).tar.Z
+
+#  clean: Clean up the source directory.
+#  ------------------------------------
+#
+#  Remove all intermediate files.  Do not remove built files.
+
+clean:
+	@- rm -f $(INCLUDE_LINKS) $(F_ROUTINES) \
+                 $(PLATFORM_F) $(BLOCK_DATA) 1>/dev/null 2>/dev/null
+	@- rm -f $(C_ROUTINES) $(OBJECT_FILES) 1>/dev/null 2>/dev/null
+	@ echo
+	@ echo '*** Intermediate files removed'
+	@ echo
+
+#  unbuild: Reverse the build process.
+#  ----------------------------------
+
+#  Remove all intermediate files and all built files, and note that the
+#  package is no longer built or tested.
+
+unbuild: clean
+	@- rm -f $(BUILT_FILES) $(DATE_STAMP) .BUILT 1>/dev/null 2>/dev/null
+	@ echo '*** Built files removed'
+	@ echo
+
+#-------------------------------------------------------------------------------
+
+#  Include file dependencies.
+#  =========================
+
+#  Object file dependencies on include files (or links to those include
+#  files).  These are normally generated automatically from the source
+#  files.
+
+#-------------------------------------------------------------------------------
+
+#  Private targets.
+
+#  Targets for manipulating the hypertext documentation (creating,
+#  generating tar files etc, cleaning etc).
+
+hypertext: sun67.tex sun67.aux
+	star2html -aux -m ptw@star.rl.ac.uk sun67.tex
+
+hypertext_tar:
+	$(TAR_IN) sun67.htx_tar sun67.htx/*
+
+hypertext_clean:
+	rm -rf sun67.htx
+#-------------------------------------------------------------------------------
+#
+#  End of makefile.
+#.
diff --git a/src/slalib/map.f b/src/slalib/map.f
new file mode 100644
index 0000000..6046774
--- /dev/null
+++ b/src/slalib/map.f
@@ -0,0 +1,75 @@
+      SUBROUTINE sla_MAP (RM, DM, PR, PD, PX, RV, EQ, DATE, RA, DA)
+*+
+*     - - - -
+*      M A P
+*     - - - -
+*
+*  Transform star RA,Dec from mean place to geocentric apparent
+*
+*  The reference frames and timescales used are post IAU 1976.
+*
+*  References:
+*     1984 Astronomical Almanac, pp B39-B41.
+*     (also Lederle & Schwan, Astron. Astrophys. 134,
+*      1-6, 1984)
+*
+*  Given:
+*     RM,DM    dp     mean RA,Dec (rad)
+*     PR,PD    dp     proper motions:  RA,Dec changes per Julian year
+*     PX       dp     parallax (arcsec)
+*     RV       dp     radial velocity (km/sec, +ve if receding)
+*     EQ       dp     epoch and equinox of star data (Julian)
+*     DATE     dp     TDB for apparent place (JD-2400000.5)
+*
+*  Returned:
+*     RA,DA    dp     apparent RA,Dec (rad)
+*
+*  Called:
+*     sla_MAPPA       star-independent parameters
+*     sla_MAPQK       quick mean to apparent
+*
+*  Notes:
+*
+*  1)  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 sla_PM to apply proper
+*      motion corrections before using this routine.
+*
+*  2)  The distinction between the required TDB and TT is
+*      always negligible.  Moreover, for all but the most
+*      critical applications UTC is adequate.
+*
+*  3)  The proper motions in RA are dRA/dt rather than
+*      cos(Dec)*dRA/dt.
+*
+*  4)  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 sla_MAPPA routine
+*      once and then either the sla_MAPQK routine (which includes
+*      parallax and proper motion) or sla_MAPQKZ (which assumes
+*      zero parallax and proper motion).
+*
+*  P.T.Wallace   Starlink   19 January 1993
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION RM,DM,PR,PD,PX,RV,EQ,DATE,RA,DA
+
+      DOUBLE PRECISION AMPRMS(21)
+
+
+
+*  Star-independent parameters
+      CALL sla_MAPPA(EQ,DATE,AMPRMS)
+
+*  Mean to apparent
+      CALL sla_MAPQK(RM,DM,PR,PD,PX,RV,AMPRMS,RA,DA)
+
+      END
diff --git a/src/slalib/mappa.f b/src/slalib/mappa.f
new file mode 100644
index 0000000..8dce865
--- /dev/null
+++ b/src/slalib/mappa.f
@@ -0,0 +1,107 @@
+      SUBROUTINE sla_MAPPA (EQ, DATE, AMPRMS)
+*+
+*     - - - - - -
+*      M A P P A
+*     - - - - - -
+*
+*  Compute star-independent parameters in preparation for
+*  conversions between mean place and geocentric apparent place.
+*
+*  The parameters produced by this routine are required in the
+*  parallax, light deflection, aberration, and precession/nutation
+*  parts of the mean/apparent transformations.
+*
+*  The reference frames and timescales used are post IAU 1976.
+*
+*  Given:
+*     EQ       d      epoch of mean equinox to be used (Julian)
+*     DATE     d      TDB (JD-2400000.5)
+*
+*  Returned:
+*     AMPRMS   d(21)  star-independent mean-to-apparent parameters:
+*
+*       (1)      time interval for proper motion (Julian years)
+*       (2-4)    barycentric position of the Earth (AU)
+*       (5-7)    heliocentric direction of the Earth (unit vector)
+*       (8)      (grav rad Sun)*2/(Sun-Earth distance)
+*       (9-11)   ABV: barycentric Earth velocity in units of c
+*       (12)     sqrt(1-v**2) where v=modulus(ABV)
+*       (13-21)  precession/nutation (3,3) matrix
+*
+*  References:
+*     1984 Astronomical Almanac, pp B39-B41.
+*     (also Lederle & Schwan, Astron. Astrophys. 134,
+*      1-6, 1984)
+*
+*  Notes:
+*
+*  1)  For DATE, the distinction between the required TDB and TT
+*      is always negligible.  Moreover, for all but the most
+*      critical applications UTC is adequate.
+*
+*  2)  The accuracy of the routines using the parameters AMPRMS is
+*      limited by the routine sla_EVP, used here to compute the
+*      Earth position and velocity by the methods of Stumpff.
+*      The maximum error in the resulting aberration corrections is
+*      about 0.3 milliarcsecond.
+*
+*  3)  The vectors AMPRMS(2-4) and AMPRMS(5-7) are referred to
+*      the mean equinox and equator of epoch EQ.
+*
+*  4)  The parameters AMPRMS produced by this routine are used by
+*      sla_MAPQK and sla_MAPQKZ.
+*
+*  Called:
+*     sla_EPJ         MDJ to Julian epoch
+*     sla_EVP         earth position & velocity
+*     sla_DVN         normalize vector
+*     sla_PRENUT      precession/nutation matrix
+*
+*  P.T.Wallace   Starlink   23 November 1995
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION EQ,DATE,AMPRMS(21)
+
+*  Light time for 1 AU (sec)
+      DOUBLE PRECISION CR
+      PARAMETER (CR=499.004782D0)
+
+*  Gravitational radius of the sun x 2 (2*mu/c**2, AU)
+      DOUBLE PRECISION GR2
+      PARAMETER (GR2=2D0*9.87063D-9)
+
+      INTEGER I
+
+      DOUBLE PRECISION EBD(3),EHD(3),EH(3),E,VN(3),VM
+
+      DOUBLE PRECISION sla_EPJ
+
+
+
+*  Time interval for proper motion correction
+      AMPRMS(1) = sla_EPJ(DATE)-EQ
+
+*  Get Earth barycentric and heliocentric position and velocity
+      CALL sla_EVP(DATE,EQ,EBD,AMPRMS(2),EHD,EH)
+
+*  Heliocentric direction of earth (normalized) and modulus
+      CALL sla_DVN(EH,AMPRMS(5),E)
+
+*  Light deflection parameter
+      AMPRMS(8) = GR2/E
+
+*  Aberration parameters
+      DO I=1,3
+         AMPRMS(I+8) = EBD(I)*CR
+      END DO
+      CALL sla_DVN(AMPRMS(9),VN,VM)
+      AMPRMS(12) = SQRT(1D0-VM*VM)
+
+*  Precession/nutation matrix
+      CALL sla_PRENUT(EQ,DATE,AMPRMS(13))
+
+      END
diff --git a/src/slalib/mapqk.f b/src/slalib/mapqk.f
new file mode 100644
index 0000000..4cd0f95
--- /dev/null
+++ b/src/slalib/mapqk.f
@@ -0,0 +1,143 @@
+      SUBROUTINE sla_MAPQK (RM, DM, PR, PD, PX, RV, AMPRMS, RA, DA)
+*+
+*     - - - - - -
+*      M A P Q K
+*     - - - - - -
+*
+*  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
+*  sla_MAPPA routine.
+*
+*  If the parallax and proper motions are zero the sla_MAPQKZ
+*  routine can be used instead.
+*
+*  The reference frames and timescales used are post IAU 1976.
+*
+*  Given:
+*     RM,DM    d      mean RA,Dec (rad)
+*     PR,PD    d      proper motions:  RA,Dec changes per Julian year
+*     PX       d      parallax (arcsec)
+*     RV       d      radial velocity (km/sec, +ve if receding)
+*
+*     AMPRMS   d(21)  star-independent mean-to-apparent parameters:
+*
+*       (1)      time interval for proper motion (Julian years)
+*       (2-4)    barycentric position of the Earth (AU)
+*       (5-7)    heliocentric direction of the Earth (unit vector)
+*       (8)      (grav rad Sun)*2/(Sun-Earth distance)
+*       (9-11)   barycentric Earth velocity in units of c
+*       (12)     sqrt(1-v**2) where v=modulus(ABV)
+*       (13-21)  precession/nutation (3,3) matrix
+*
+*  Returned:
+*     RA,DA    d      apparent RA,Dec (rad)
+*
+*  References:
+*     1984 Astronomical Almanac, pp B39-B41.
+*     (also Lederle & Schwan, Astron. Astrophys. 134,
+*      1-6, 1984)
+*
+*  Notes:
+*
+*  1)  The vectors AMPRMS(2-4) and AMPRMS(5-7) are referred to
+*      the mean equinox and equator of epoch EQ.
+*
+*  2)  Strictly speaking, the routine is not valid for solar-system
+*      sources, though the error will usually be extremely small.
+*      However, to prevent gross errors in the case where the
+*      position of the Sun is specified, the gravitational
+*      deflection term is restrained within about 920 arcsec of the
+*      centre of the Sun's disc.  The term has a maximum value of
+*      about 1.85 arcsec at this radius, and decreases to zero as
+*      the centre of the disc is approached.
+*
+*  Called:
+*     sla_DCS2C       spherical to Cartesian
+*     sla_DVDV        dot product
+*     sla_DMXV        matrix x vector
+*     sla_DCC2S       Cartesian to spherical
+*     sla_DRANRM      normalize angle 0-2Pi
+*
+*  P.T.Wallace   Starlink   23 August 1996
+*
+*  Copyright (C) 1996 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION RM,DM,PR,PD,PX,RV,AMPRMS(21),RA,DA
+
+*  Arc seconds to radians
+      DOUBLE PRECISION AS2R
+      PARAMETER (AS2R=0.484813681109535994D-5)
+
+*  Km/s to AU/year
+      DOUBLE PRECISION VF
+      PARAMETER (VF=0.21094502D0)
+
+      INTEGER I
+
+      DOUBLE PRECISION PMT,GR2E,AB1,EB(3),EHN(3),ABV(3),
+     :                 Q(3),PXR,W,EM(3),P(3),PN(3),PDE,PDEP1,
+     :                 P1(3),P1DV,P1DVP1,P2(3),P3(3)
+
+      DOUBLE PRECISION sla_DVDV,sla_DRANRM
+
+
+
+*  Unpack scalar and vector parameters
+      PMT = AMPRMS(1)
+      GR2E = AMPRMS(8)
+      AB1 = AMPRMS(12)
+      DO I=1,3
+         EB(I) = AMPRMS(I+1)
+         EHN(I) = AMPRMS(I+4)
+         ABV(I) = AMPRMS(I+8)
+      END DO
+
+*  Spherical to x,y,z
+      CALL sla_DCS2C(RM,DM,Q)
+
+*  Space motion (radians per year)
+      PXR = PX*AS2R
+      W = VF*RV*PXR
+      EM(1) = -PR*Q(2)-PD*COS(RM)*SIN(DM)+W*Q(1)
+      EM(2) =  PR*Q(1)-PD*SIN(RM)*SIN(DM)+W*Q(2)
+      EM(3) =          PD*COS(DM)        +W*Q(3)
+
+*  Geocentric direction of star (normalized)
+      DO I=1,3
+         P(I) = Q(I)+PMT*EM(I)-PXR*EB(I)
+      END DO
+      CALL sla_DVN(P,PN,W)
+
+*  Light deflection (restrained within the Sun's disc)
+      PDE = sla_DVDV(PN,EHN)
+      PDEP1 = PDE+1D0
+      W = GR2E/MAX(PDEP1,1D-5)
+      DO I=1,3
+         P1(I) = PN(I)+W*(EHN(I)-PDE*PN(I))
+      END DO
+
+*  Aberration
+      P1DV = sla_DVDV(P1,ABV)
+      P1DVP1 = P1DV+1D0
+      W = 1D0+P1DV/(AB1+1D0)
+      DO I=1,3
+         P2(I) = (AB1*P1(I)+W*ABV(I))/P1DVP1
+      END DO
+
+*  Precession and nutation
+      CALL sla_DMXV(AMPRMS(13),P2,P3)
+
+*  Geocentric apparent RA,Dec
+      CALL sla_DCC2S(P3,RA,DA)
+      RA = sla_DRANRM(RA)
+
+      END
diff --git a/src/slalib/mapqkz.f b/src/slalib/mapqkz.f
new file mode 100644
index 0000000..2922874
--- /dev/null
+++ b/src/slalib/mapqkz.f
@@ -0,0 +1,113 @@
+      SUBROUTINE sla_MAPQKZ (RM, DM, AMPRMS, RA, DA)
+*+
+*     - - - - - - -
+*      M A P Q K Z
+*     - - - - - - -
+*
+*  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 routine 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 sla_MAPPA routine.
+*
+*  The corresponding routine for the case of non-zero parallax
+*  and proper motion is sla_MAPQK.
+*
+*  The reference frames and timescales used are post IAU 1976.
+*
+*  Given:
+*     RM,DM    d      mean RA,Dec (rad)
+*     AMPRMS   d(21)  star-independent mean-to-apparent parameters:
+*
+*       (1-4)    not used
+*       (5-7)    heliocentric direction of the Earth (unit vector)
+*       (8)      (grav rad Sun)*2/(Sun-Earth distance)
+*       (9-11)   ABV: barycentric Earth velocity in units of c
+*       (12)     sqrt(1-v**2) where v=modulus(ABV)
+*       (13-21)  precession/nutation (3,3) matrix
+*
+*  Returned:
+*     RA,DA    d      apparent RA,Dec (rad)
+*
+*  References:
+*     1984 Astronomical Almanac, pp B39-B41.
+*     (also Lederle & Schwan, Astron. Astrophys. 134,
+*      1-6, 1984)
+*
+*  Notes:
+*
+*  1)  The vectors AMPRMS(2-4) and AMPRMS(5-7) are referred to the
+*      mean equinox and equator of epoch EQ.
+*
+*  2)  Strictly speaking, the routine is not valid for solar-system
+*      sources, though the error will usually be extremely small.
+*      However, to prevent gross errors in the case where the
+*      position of the Sun is specified, the gravitational
+*      deflection term is restrained within about 920 arcsec of the
+*      centre of the Sun's disc.  The term has a maximum value of
+*      about 1.85 arcsec at this radius, and decreases to zero as
+*      the centre of the disc is approached.
+*
+*  Called:  sla_DCS2C, sla_DVDV, sla_DMXV, sla_DCC2S, sla_DRANRM
+*
+*  P.T.Wallace   Starlink   18 March 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION RM,DM,AMPRMS(21),RA,DA
+
+      INTEGER I
+
+      DOUBLE PRECISION GR2E,AB1,EHN(3),ABV(3),
+     :                 P(3),PDE,PDEP1,W,P1(3),P1DV,
+     :                 P1DVP1,P2(3),P3(3)
+
+      DOUBLE PRECISION sla_DVDV,sla_DRANRM
+
+
+
+
+*  Unpack scalar and vector parameters
+      GR2E = AMPRMS(8)
+      AB1 = AMPRMS(12)
+      DO I=1,3
+         EHN(I) = AMPRMS(I+4)
+         ABV(I) = AMPRMS(I+8)
+      END DO
+
+*  Spherical to x,y,z
+      CALL sla_DCS2C(RM,DM,P)
+
+*  Light deflection
+      PDE = sla_DVDV(P,EHN)
+      PDEP1 = PDE+1D0
+      W = GR2E/MAX(PDEP1,1D-5)
+      DO I=1,3
+         P1(I) = P(I)+W*(EHN(I)-PDE*P(I))
+      END DO
+
+*  Aberration
+      P1DV = sla_DVDV(P1,ABV)
+      P1DVP1 = P1DV+1D0
+      W = 1D0+P1DV/(AB1+1D0)
+      DO I=1,3
+         P2(I) = (AB1*P1(I)+W*ABV(I))/P1DVP1
+      END DO
+
+*  Precession and nutation
+      CALL sla_DMXV(AMPRMS(13),P2,P3)
+
+*  Geocentric apparent RA,Dec
+      CALL sla_DCC2S(P3,RA,DA)
+      RA = sla_DRANRM(RA)
+
+      END
diff --git a/src/slalib/mk b/src/slalib/mk
new file mode 100755
index 0000000..5a186c3
--- /dev/null
+++ b/src/slalib/mk
@@ -0,0 +1,437 @@
+
+#  This is a Bourne shell script.  In order to be POSIX-compliant, the
+#  first line must be blank.
+
+#+
+#  Name:
+#     mk
+#
+#  Version:
+#     Version for Mk V library makefile.
+#
+#  Purpose:
+#     Invoke make to build and install the SLALIB package.
+#
+#  Type of Module:
+#     Shell script.
+#
+#  Description:
+#     This script should normally be used to invoke the make utility
+#     to build and install the SLALIB package and to perform other
+#     housekeeping tasks.  It invokes the make utility after first
+#     defining appropriate environment variables and macros for the
+#     computer system in use.  This file also serves to document the
+#     systems on which SLALIB is implemented.
+#
+#  Invocation:
+#     The user of this script should normally first define the SYSTEM
+#     environment variable to identify the host computer system (see
+#     the "Supported Systems" section).  This script should then be used
+#     in the same way as the make utility would be used.  For instance,
+#     to build, install and test SLALIB, you might use the following
+#     commands:
+#
+#        ./mk build
+#        ./mk install
+#        ./mk test
+#        ./mk clean
+#
+#  Supported Systems:
+#     The following systems are currently supported and may be
+#     identified by defining the SYSTEM environment variable
+#     appropriately before invoking this script:
+#
+#        alpha_OSF1
+#           DEC Alpha machines running OSF1
+#
+#        ix86_Linux
+#           Intel PC machines running Linux
+#
+#        sun4_Solaris
+#           SUN Sparcstations running SunOS 5.x (Solaris)
+#
+#     In addition, the following systems have been supported at some
+#     time in the past.  This script contains the macro definitions
+#     needed for these systems, but it is not known whether {PACKAGE}
+#     will still build or run on these systems:
+#
+#        convex
+#           Convex running ConvexOS
+#
+#        mips
+#           DECstations running Ultrix
+#
+#        sun4
+#           SUN Sparcstations running SunOS 4.x
+#
+#     This script will exit without action if the SYSTEM environment
+#     variable is not defined.  A warning will be issued if it is
+#     defined but is not set to one of the values above.  In this case,
+#     the only environment variable that will be defined by this script
+#     is SOURCE_VARIANT, which is set to unknown (any that are
+#     pre-defined will be passed on to make unaltered). 
+#
+#  Targets:
+#     For details of what targets are provided, see the associated
+#     makefile.  The latter will normally provide a default target
+#     called "help", which outputs a message describing this script
+#     and lists the targets provided.
+#
+#  Notes on Porting:
+#     If your machine or system setup does not appear in this script,
+#     then it should be possible to build and install SLALIB by
+#     adding a new case to this script with appropriate definitions
+#     (probably based on one of the existing implementations).
+#
+#  make Macros:
+#     The following "global" make macros are used in the associated
+#     makefile and may be changed by means of appropriate environment
+#     variable definitions (in each case the default is shown in
+#     parentheses).  Note that these macros are provided to allow
+#     external control over the directories in which software is
+#     installed, etc., so they should not normally be re-defined within
+#     this script.
+#
+#        STARLINK (/star)
+#           Pathname of the root directory beneath which Starlink
+#           software is currently installed.  This indicates to
+#           SLALIB where to find other Starlink software (include
+#           files, libraries, etc.) which it uses.
+#
+#        INSTALL ($HOME)
+#           Pathname of the root directory beneath which SLALIB will
+#           be installed for use.  Your home directory will be used by
+#           default.  This macro is provided to allow SLALIB to be
+#           installed locally for personal use (e.g. during development
+#           or testing).  It should be set to the $STARLINK directory if
+#           you want to add SLALIB into an already installed set of
+#           Starlink software.  You should ensure that the appropriate
+#           sub-directories appear on any relevant search paths which
+#           your system uses for locating software (e.g. binaries and
+#           libraries).
+#
+#        EXPORT (.)
+#           Pathname of the directory into which compressed tar files
+#           will be written if the "export" or "export_source" make
+#           targets are used to produce an exportable copy of SLALIB
+#           or its source files.  The current working directory (i.e.
+#           the SLALIB source directory) will be used by default.
+#
+#     The following "local" make macros are used in the associated
+#     makefile and should normally be overridden by environment variable
+#     definitions within this script.  All the local macros that are
+#     used in building a package should overridden even when the value
+#     is the same as the default.  This documents which macros are used
+#     and ensures that the package will continue to build correctly even
+#     if the default values are changed.  Macros that are not used on a
+#     particular machine (e.g. BLD_SHR on DECstations) should not be
+#     overridden.  In each case the default is shown in parentheses.
+#
+#        AR_IN (ar -r)
+#           The command to use to insert an object (.o) file into an
+#           archive (.a) library.  On some systems the variation 'ar r'
+#           may be required instead.
+#
+#        BLD_SHR (:)
+#           Command to build a shareable library when given three
+#           arguments specifying (1) the name of the library file to be
+#           built (2) a list of the object files to be used in the
+#           library and (3) a list of any additional libraries against
+#           which to link.  By default, it is assumed that shareable
+#           libraries are not available, and the default acts as a null
+#           command.
+#
+#        CC (c89)
+#           The C compiler command to use.
+#
+#        CFLAGS (-O)
+#           The C compiler options to use.
+#
+#        C_ROUTINES ()
+#           Names of the C routines needed to build the library.  Some
+#           systems (ix86_Linux) require extra C routines to provide
+#           missing system functions.
+#
+#        FC (fort77)
+#           The Fortran compiler command to use.  SLALIB requires a Fortran
+#           77 compiler that supports the common "permitted" Starlink
+#           extensions, as documented in Starlink General Paper SGP/16.
+#           (These include only the most common extensions, such as
+#           long names, end of line comments, include files, etc.)
+#
+#        FFLAGS (-O)
+#           The Fortran compiler options to be used.
+#
+#        HLINK (:)
+#           The command required to perform the linking of the package
+#           hypertext documentation into a cohesive whole with the rest
+#           (if any) Starlink documentation at the installation site, and
+#           with the Hypertext document server at RAL.  This service is not
+#           available on Sparc SunOS4, Dec MIPS Ultrix or Convex.  This
+#           macro is not a standard Starlink macro.
+#
+#        LINK (ln)
+#           The command required to establish a link to a file.  The
+#           default assumes POSIX.2 behavior, which only provides a
+#           "hard" link operating within a single file system.  If the
+#           host operating system allows "symbolic" links, then this
+#           macro might be re-defined as 'ln -s'.  Alternatively, if the
+#           use of multiple file systems is essential but not supported
+#           by any form of link, then a copy command could be
+#           substituted (e.g. 'cp -p'), at some cost in file space.
+#
+#        SOURCE_VARIANT ($SYSTEM)
+#           The name used to distinguish between platform-specific
+#           files.  Using the default ($SYSTEM) implies that multiple
+#           copies of the same source may exist under different names.
+#           For example, the files sub1.f_sun4 and sun1.f_sun4_Solaris
+#           may contain identical source code.  If this is to be
+#           avoided (to save space), edit this script to set
+#           SOURCE_VARIANT to a suitable string - for example setting it
+#           to "sun" would allow one copy of the source called
+#           sub1.f_sun to be used. To do this, add to each of the
+#           per-system sections a statement of the form:
+#
+#              SOURCE_VARIANT='string'
+#
+#        RANLIB (:)
+#           The command required to "randomise" an object library.  By
+#           default, this operation is not performed (the default acts
+#           as a null command).  On systems which require it, this
+#           should typically be set to 'ranlib'.
+#
+#        SHARE (.so)
+#           The file type suffix to be applied to produce the name of a
+#           shareable library file.  By default, the ".so" suffix is
+#           applied without a library version number.  For systems which
+#           support version numbers on shareable libraries, the macro
+#           LIB_VERS is defined within the associated makefile and may
+#           be used as part of a definition such as '.so.$(LIB_VERS)'.
+#
+#        TAR_IN (pax -w -v -x ustar -f)
+#           Command to use to insert a file into a .tar archive file.
+#           The default uses the POSIX.2 pax command, which is not
+#           available on traditional UNIX systems.  These typically use
+#           a tar command such as 'tar -cvhf' instead (if symbolic
+#           links are supported, then an option to follow these must be
+#           included in this command).
+#
+#        TAR_OUT (pax -r -f)
+#           Command to use to extract a file from a .tar archive file.
+#           The default uses the POSIX.2 pax command, which is not
+#           available on traditional UNIX systems.  These typically use
+#           a tar command such as 'tar -xf' instead.
+#
+#  Implementation Deficiencies:
+#     -  The implementation of shareable libraries on the alpha_OSF1
+#        system is still preliminary.
+#
+#  Copyright:
+#     Copyright (C) 1995 Rutherford Appleton Laboratory
+#
+#  Authors:
+#     RFWS: R.F.Warren-Smith (Starlink, RAL)
+#     PMA: P.M.Allan (Starlink, RAL)
+#     PTW: P.T.Wallace (Starlink, RAL)
+#     AJC: A.J.Chipperfield (Starlink, RAL)
+#     BLY: M.J.Bly (Starlink, RAL)
+#     BKM: B.K.McIlwrath (Starlink, RAL)
+#     {enter_new_authors_here}
+#
+#  History:
+#     26-NOV-1993 (RFWS/PMA):
+#        Starlink template.
+#     26-NOV-1993 (PTW):
+#        Version for SLALIB.
+#     28-JUN-1993 (PTW):
+#        Convex added.
+#     06-JUN-1995 (BLY):
+#        Updated to Mk IVa standard.
+#     04-MAR-1996 (BLY):
+#        Updated to Mk V specification.
+#        Added HLINK macro and definitions.
+#     24-APR-1996 (BLY):
+#        Integrated Linux support from BKM version.
+#     22-JAN-1998 (BLY):
+#        Removed rtl_sleep.c from C_ROUTINES for Linux case.
+#     {enter_further_changes_here}
+#
+#  Bugs:
+#     {note_any_bugs_here}
+#
+#-
+
+#  Export "local" definitions to the environment for use by make.
+      export AR_IN
+      export BLD_SHR
+      export CC
+      export CFLAGS
+      export C_ROUTINES
+      export FC
+      export FFLAGS
+      export HLINK
+      export LINK
+      export SOURCE_VARIANT
+      export RANLIB
+      export SHARE
+      export TAR_IN
+      export TAR_OUT
+
+#  Check that the SYSTEM environment variable is defined.
+      if test "$SYSTEM" = ""; then
+         echo "mk: Please define the environment variable SYSTEM to identify"
+         echo "    your computer system (the prologue in the mk script file"
+         echo "    contains more information if you require it)."
+
+#  If OK, test for each recognised system.
+      else
+         case "$SYSTEM" in
+
+#  DEC Alpha:
+#  =========
+#  DEC Alpha machines running OSF1.
+#  -------------------------------
+            alpha_OSF1)
+               AR_IN='ar -r'
+#               BLD_SHR=\
+#'f() ld -shared -update_registry $(INSTALL)/share/so_locations -o $$1 $$2 $$3 \
+#-lfor -lFutil -lUfor -lm -lots -lc; f'
+               CC='cc'
+               CFLAGS='-I$(STAR_INC) -O -std1'
+               FC='f77'
+               FFLAGS='-O'
+               HLINK='$(STAR_BIN)/hlink'
+               LINK='ln -s'
+               RANLIB='ranlib'
+#               SHARE='.so'
+               TAR_IN='tar -cvhf'
+               TAR_OUT='tar -xf'
+               echo "mk: Environment variables defined for $SYSTEM system"
+               ;;
+
+#  DECstations:
+#  ===========
+#  DECstations running Ultrix.
+#  --------------------------
+            mips)
+               AR_IN='ar -r'
+               CC='c89'
+               CFLAGS='-I$(STAR_INC) -O'
+               FC='f77'
+               FFLAGS='-O'
+               LINK='ln -s'
+               RANLIB='ranlib'
+               TAR_IN='tar -cvhf'
+               TAR_OUT='tar -xf'
+               echo "mk: Environment variables defined for $SYSTEM system"
+               ;;
+
+#  SUN4 systems:
+#  ============
+#  SUN Sparcstations running SunOS 4.x.
+#  -----------------------------------
+            sun4)
+               AR_IN='ar r'
+               BLD_SHR='f() ld -assert pure-text -o $$1 $$2; f'
+               CC='gcc'
+               CFLAGS='-I$(STAR_INC) -O -fPIC'
+               FC='f77'
+               FFLAGS='-O -PIC'
+               LINK='ln -s'
+               RANLIB='ranlib'
+               SHARE='.so.$(LIB_VERS)'
+               TAR_IN='tar -cvhf'
+               TAR_OUT='tar -xf'
+               echo "mk: Environment variables defined for $SYSTEM system"
+               ;;
+
+#  SUN Sparcstations running SunOS 5.x (Solaris).
+#  ---------------------------------------------
+            sun4_Solaris)
+               AR_IN='ar -r'
+               BLD_SHR='f() ld -G -z text -o $$1 $$2; f'
+               CC='cc'
+               CFLAGS='-I$(STAR_INC) -O -K PIC'
+               FC='f77'
+               FFLAGS='-O -PIC'
+               HLINK='$(STAR_BIN)/hlink'
+               LINK='ln -s'
+               SHARE='.so'
+               TAR_IN='tar -cvhf'
+               TAR_OUT='tar -xf'
+               echo "mk: Environment variables defined for $SYSTEM system"
+               ;;
+
+#  PC systems:
+#  ==========
+#  Intel PC running Linux.
+#  ----------------------
+            ix86_Linux)
+               AR_IN='ar r'
+               CC='gcc'
+               CFLAGS='-O'
+               C_ROUTINES='rtl_random.c'
+               FC='gfortran'
+               FFLAGS='-fno-second-underscore -O'
+               HLINK='$(STAR_BIN)/hlink'
+               LINK='ln -s'
+               RANLIB='ranlib'
+               TAR_IN='tar -cvhf'
+               TAR_OUT='tar -xf'
+               echo "mk: Environment variables defined for $SYSTEM system"
+               ;;
+
+#  Intel PC running Linux on 64 architecture.
+#  -----------------------------------------
+            x86_64)
+               AR_IN='ar r'
+               CC='gcc'
+               CFLAGS='-O -fPIC'
+               C_ROUTINES='rtl_random.c'
+               FC='gfortran'
+               FFLAGS='-fno-second-underscore -O -fPIC'
+               HLINK='$(STAR_BIN)/hlink'
+               LINK='ln -s'
+               RANLIB='ranlib'
+               TAR_IN='tar -cvhf'
+               TAR_OUT='tar -xf'
+               echo "mk: Environment variables defined for $SYSTEM system"
+               ;;
+
+#  Convex running ConvexOS.
+#  ------------------------
+            convex)
+               AR_IN='ar r'
+               FC='fc'
+               FFLAGS='-O3'
+               CC='gcc'
+               CFLAGS='-I$(STAR_INC) -O -fPIC'
+               LINK='ln -s'
+               RANLIB='ranlib'
+               TAR_IN='tar -cvhf'
+               TAR_OUT='tar -xf'
+               echo "mk: Environment variables defined for $SYSTEM system"
+               ;;
+
+#  IMPORTANT NOTE - Because Convex make doesn't support the -e
+#  qualifier (as stipulated by the POSIX standard) it will be
+#  necessary to use another version of make, for example the
+#  GNU one.  This can be accomplished either by editing this script,
+#  or by setting up a link.
+
+#  Issue a warning if SYSTEM is not recognised.
+            *)
+               SOURCE_VARIANT='unknown'
+               echo "mk: WARNING: value of SYSTEM = $SYSTEM not recognised..."
+               echo "             ...assuming default system characteristics"
+               echo '             ...setting SOURCE_VARIANT to "unknown"'
+               ;;
+         esac
+
+#  Invoke make with the appropriate environment variables set to override
+#  default macros defined in the makefile.
+         echo make -e $*
+         make -e $*
+      fi
+
+#  End of script.
diff --git a/src/slalib/mk.sv b/src/slalib/mk.sv
new file mode 100755
index 0000000..5a186c3
--- /dev/null
+++ b/src/slalib/mk.sv
@@ -0,0 +1,437 @@
+
+#  This is a Bourne shell script.  In order to be POSIX-compliant, the
+#  first line must be blank.
+
+#+
+#  Name:
+#     mk
+#
+#  Version:
+#     Version for Mk V library makefile.
+#
+#  Purpose:
+#     Invoke make to build and install the SLALIB package.
+#
+#  Type of Module:
+#     Shell script.
+#
+#  Description:
+#     This script should normally be used to invoke the make utility
+#     to build and install the SLALIB package and to perform other
+#     housekeeping tasks.  It invokes the make utility after first
+#     defining appropriate environment variables and macros for the
+#     computer system in use.  This file also serves to document the
+#     systems on which SLALIB is implemented.
+#
+#  Invocation:
+#     The user of this script should normally first define the SYSTEM
+#     environment variable to identify the host computer system (see
+#     the "Supported Systems" section).  This script should then be used
+#     in the same way as the make utility would be used.  For instance,
+#     to build, install and test SLALIB, you might use the following
+#     commands:
+#
+#        ./mk build
+#        ./mk install
+#        ./mk test
+#        ./mk clean
+#
+#  Supported Systems:
+#     The following systems are currently supported and may be
+#     identified by defining the SYSTEM environment variable
+#     appropriately before invoking this script:
+#
+#        alpha_OSF1
+#           DEC Alpha machines running OSF1
+#
+#        ix86_Linux
+#           Intel PC machines running Linux
+#
+#        sun4_Solaris
+#           SUN Sparcstations running SunOS 5.x (Solaris)
+#
+#     In addition, the following systems have been supported at some
+#     time in the past.  This script contains the macro definitions
+#     needed for these systems, but it is not known whether {PACKAGE}
+#     will still build or run on these systems:
+#
+#        convex
+#           Convex running ConvexOS
+#
+#        mips
+#           DECstations running Ultrix
+#
+#        sun4
+#           SUN Sparcstations running SunOS 4.x
+#
+#     This script will exit without action if the SYSTEM environment
+#     variable is not defined.  A warning will be issued if it is
+#     defined but is not set to one of the values above.  In this case,
+#     the only environment variable that will be defined by this script
+#     is SOURCE_VARIANT, which is set to unknown (any that are
+#     pre-defined will be passed on to make unaltered). 
+#
+#  Targets:
+#     For details of what targets are provided, see the associated
+#     makefile.  The latter will normally provide a default target
+#     called "help", which outputs a message describing this script
+#     and lists the targets provided.
+#
+#  Notes on Porting:
+#     If your machine or system setup does not appear in this script,
+#     then it should be possible to build and install SLALIB by
+#     adding a new case to this script with appropriate definitions
+#     (probably based on one of the existing implementations).
+#
+#  make Macros:
+#     The following "global" make macros are used in the associated
+#     makefile and may be changed by means of appropriate environment
+#     variable definitions (in each case the default is shown in
+#     parentheses).  Note that these macros are provided to allow
+#     external control over the directories in which software is
+#     installed, etc., so they should not normally be re-defined within
+#     this script.
+#
+#        STARLINK (/star)
+#           Pathname of the root directory beneath which Starlink
+#           software is currently installed.  This indicates to
+#           SLALIB where to find other Starlink software (include
+#           files, libraries, etc.) which it uses.
+#
+#        INSTALL ($HOME)
+#           Pathname of the root directory beneath which SLALIB will
+#           be installed for use.  Your home directory will be used by
+#           default.  This macro is provided to allow SLALIB to be
+#           installed locally for personal use (e.g. during development
+#           or testing).  It should be set to the $STARLINK directory if
+#           you want to add SLALIB into an already installed set of
+#           Starlink software.  You should ensure that the appropriate
+#           sub-directories appear on any relevant search paths which
+#           your system uses for locating software (e.g. binaries and
+#           libraries).
+#
+#        EXPORT (.)
+#           Pathname of the directory into which compressed tar files
+#           will be written if the "export" or "export_source" make
+#           targets are used to produce an exportable copy of SLALIB
+#           or its source files.  The current working directory (i.e.
+#           the SLALIB source directory) will be used by default.
+#
+#     The following "local" make macros are used in the associated
+#     makefile and should normally be overridden by environment variable
+#     definitions within this script.  All the local macros that are
+#     used in building a package should overridden even when the value
+#     is the same as the default.  This documents which macros are used
+#     and ensures that the package will continue to build correctly even
+#     if the default values are changed.  Macros that are not used on a
+#     particular machine (e.g. BLD_SHR on DECstations) should not be
+#     overridden.  In each case the default is shown in parentheses.
+#
+#        AR_IN (ar -r)
+#           The command to use to insert an object (.o) file into an
+#           archive (.a) library.  On some systems the variation 'ar r'
+#           may be required instead.
+#
+#        BLD_SHR (:)
+#           Command to build a shareable library when given three
+#           arguments specifying (1) the name of the library file to be
+#           built (2) a list of the object files to be used in the
+#           library and (3) a list of any additional libraries against
+#           which to link.  By default, it is assumed that shareable
+#           libraries are not available, and the default acts as a null
+#           command.
+#
+#        CC (c89)
+#           The C compiler command to use.
+#
+#        CFLAGS (-O)
+#           The C compiler options to use.
+#
+#        C_ROUTINES ()
+#           Names of the C routines needed to build the library.  Some
+#           systems (ix86_Linux) require extra C routines to provide
+#           missing system functions.
+#
+#        FC (fort77)
+#           The Fortran compiler command to use.  SLALIB requires a Fortran
+#           77 compiler that supports the common "permitted" Starlink
+#           extensions, as documented in Starlink General Paper SGP/16.
+#           (These include only the most common extensions, such as
+#           long names, end of line comments, include files, etc.)
+#
+#        FFLAGS (-O)
+#           The Fortran compiler options to be used.
+#
+#        HLINK (:)
+#           The command required to perform the linking of the package
+#           hypertext documentation into a cohesive whole with the rest
+#           (if any) Starlink documentation at the installation site, and
+#           with the Hypertext document server at RAL.  This service is not
+#           available on Sparc SunOS4, Dec MIPS Ultrix or Convex.  This
+#           macro is not a standard Starlink macro.
+#
+#        LINK (ln)
+#           The command required to establish a link to a file.  The
+#           default assumes POSIX.2 behavior, which only provides a
+#           "hard" link operating within a single file system.  If the
+#           host operating system allows "symbolic" links, then this
+#           macro might be re-defined as 'ln -s'.  Alternatively, if the
+#           use of multiple file systems is essential but not supported
+#           by any form of link, then a copy command could be
+#           substituted (e.g. 'cp -p'), at some cost in file space.
+#
+#        SOURCE_VARIANT ($SYSTEM)
+#           The name used to distinguish between platform-specific
+#           files.  Using the default ($SYSTEM) implies that multiple
+#           copies of the same source may exist under different names.
+#           For example, the files sub1.f_sun4 and sun1.f_sun4_Solaris
+#           may contain identical source code.  If this is to be
+#           avoided (to save space), edit this script to set
+#           SOURCE_VARIANT to a suitable string - for example setting it
+#           to "sun" would allow one copy of the source called
+#           sub1.f_sun to be used. To do this, add to each of the
+#           per-system sections a statement of the form:
+#
+#              SOURCE_VARIANT='string'
+#
+#        RANLIB (:)
+#           The command required to "randomise" an object library.  By
+#           default, this operation is not performed (the default acts
+#           as a null command).  On systems which require it, this
+#           should typically be set to 'ranlib'.
+#
+#        SHARE (.so)
+#           The file type suffix to be applied to produce the name of a
+#           shareable library file.  By default, the ".so" suffix is
+#           applied without a library version number.  For systems which
+#           support version numbers on shareable libraries, the macro
+#           LIB_VERS is defined within the associated makefile and may
+#           be used as part of a definition such as '.so.$(LIB_VERS)'.
+#
+#        TAR_IN (pax -w -v -x ustar -f)
+#           Command to use to insert a file into a .tar archive file.
+#           The default uses the POSIX.2 pax command, which is not
+#           available on traditional UNIX systems.  These typically use
+#           a tar command such as 'tar -cvhf' instead (if symbolic
+#           links are supported, then an option to follow these must be
+#           included in this command).
+#
+#        TAR_OUT (pax -r -f)
+#           Command to use to extract a file from a .tar archive file.
+#           The default uses the POSIX.2 pax command, which is not
+#           available on traditional UNIX systems.  These typically use
+#           a tar command such as 'tar -xf' instead.
+#
+#  Implementation Deficiencies:
+#     -  The implementation of shareable libraries on the alpha_OSF1
+#        system is still preliminary.
+#
+#  Copyright:
+#     Copyright (C) 1995 Rutherford Appleton Laboratory
+#
+#  Authors:
+#     RFWS: R.F.Warren-Smith (Starlink, RAL)
+#     PMA: P.M.Allan (Starlink, RAL)
+#     PTW: P.T.Wallace (Starlink, RAL)
+#     AJC: A.J.Chipperfield (Starlink, RAL)
+#     BLY: M.J.Bly (Starlink, RAL)
+#     BKM: B.K.McIlwrath (Starlink, RAL)
+#     {enter_new_authors_here}
+#
+#  History:
+#     26-NOV-1993 (RFWS/PMA):
+#        Starlink template.
+#     26-NOV-1993 (PTW):
+#        Version for SLALIB.
+#     28-JUN-1993 (PTW):
+#        Convex added.
+#     06-JUN-1995 (BLY):
+#        Updated to Mk IVa standard.
+#     04-MAR-1996 (BLY):
+#        Updated to Mk V specification.
+#        Added HLINK macro and definitions.
+#     24-APR-1996 (BLY):
+#        Integrated Linux support from BKM version.
+#     22-JAN-1998 (BLY):
+#        Removed rtl_sleep.c from C_ROUTINES for Linux case.
+#     {enter_further_changes_here}
+#
+#  Bugs:
+#     {note_any_bugs_here}
+#
+#-
+
+#  Export "local" definitions to the environment for use by make.
+      export AR_IN
+      export BLD_SHR
+      export CC
+      export CFLAGS
+      export C_ROUTINES
+      export FC
+      export FFLAGS
+      export HLINK
+      export LINK
+      export SOURCE_VARIANT
+      export RANLIB
+      export SHARE
+      export TAR_IN
+      export TAR_OUT
+
+#  Check that the SYSTEM environment variable is defined.
+      if test "$SYSTEM" = ""; then
+         echo "mk: Please define the environment variable SYSTEM to identify"
+         echo "    your computer system (the prologue in the mk script file"
+         echo "    contains more information if you require it)."
+
+#  If OK, test for each recognised system.
+      else
+         case "$SYSTEM" in
+
+#  DEC Alpha:
+#  =========
+#  DEC Alpha machines running OSF1.
+#  -------------------------------
+            alpha_OSF1)
+               AR_IN='ar -r'
+#               BLD_SHR=\
+#'f() ld -shared -update_registry $(INSTALL)/share/so_locations -o $$1 $$2 $$3 \
+#-lfor -lFutil -lUfor -lm -lots -lc; f'
+               CC='cc'
+               CFLAGS='-I$(STAR_INC) -O -std1'
+               FC='f77'
+               FFLAGS='-O'
+               HLINK='$(STAR_BIN)/hlink'
+               LINK='ln -s'
+               RANLIB='ranlib'
+#               SHARE='.so'
+               TAR_IN='tar -cvhf'
+               TAR_OUT='tar -xf'
+               echo "mk: Environment variables defined for $SYSTEM system"
+               ;;
+
+#  DECstations:
+#  ===========
+#  DECstations running Ultrix.
+#  --------------------------
+            mips)
+               AR_IN='ar -r'
+               CC='c89'
+               CFLAGS='-I$(STAR_INC) -O'
+               FC='f77'
+               FFLAGS='-O'
+               LINK='ln -s'
+               RANLIB='ranlib'
+               TAR_IN='tar -cvhf'
+               TAR_OUT='tar -xf'
+               echo "mk: Environment variables defined for $SYSTEM system"
+               ;;
+
+#  SUN4 systems:
+#  ============
+#  SUN Sparcstations running SunOS 4.x.
+#  -----------------------------------
+            sun4)
+               AR_IN='ar r'
+               BLD_SHR='f() ld -assert pure-text -o $$1 $$2; f'
+               CC='gcc'
+               CFLAGS='-I$(STAR_INC) -O -fPIC'
+               FC='f77'
+               FFLAGS='-O -PIC'
+               LINK='ln -s'
+               RANLIB='ranlib'
+               SHARE='.so.$(LIB_VERS)'
+               TAR_IN='tar -cvhf'
+               TAR_OUT='tar -xf'
+               echo "mk: Environment variables defined for $SYSTEM system"
+               ;;
+
+#  SUN Sparcstations running SunOS 5.x (Solaris).
+#  ---------------------------------------------
+            sun4_Solaris)
+               AR_IN='ar -r'
+               BLD_SHR='f() ld -G -z text -o $$1 $$2; f'
+               CC='cc'
+               CFLAGS='-I$(STAR_INC) -O -K PIC'
+               FC='f77'
+               FFLAGS='-O -PIC'
+               HLINK='$(STAR_BIN)/hlink'
+               LINK='ln -s'
+               SHARE='.so'
+               TAR_IN='tar -cvhf'
+               TAR_OUT='tar -xf'
+               echo "mk: Environment variables defined for $SYSTEM system"
+               ;;
+
+#  PC systems:
+#  ==========
+#  Intel PC running Linux.
+#  ----------------------
+            ix86_Linux)
+               AR_IN='ar r'
+               CC='gcc'
+               CFLAGS='-O'
+               C_ROUTINES='rtl_random.c'
+               FC='gfortran'
+               FFLAGS='-fno-second-underscore -O'
+               HLINK='$(STAR_BIN)/hlink'
+               LINK='ln -s'
+               RANLIB='ranlib'
+               TAR_IN='tar -cvhf'
+               TAR_OUT='tar -xf'
+               echo "mk: Environment variables defined for $SYSTEM system"
+               ;;
+
+#  Intel PC running Linux on 64 architecture.
+#  -----------------------------------------
+            x86_64)
+               AR_IN='ar r'
+               CC='gcc'
+               CFLAGS='-O -fPIC'
+               C_ROUTINES='rtl_random.c'
+               FC='gfortran'
+               FFLAGS='-fno-second-underscore -O -fPIC'
+               HLINK='$(STAR_BIN)/hlink'
+               LINK='ln -s'
+               RANLIB='ranlib'
+               TAR_IN='tar -cvhf'
+               TAR_OUT='tar -xf'
+               echo "mk: Environment variables defined for $SYSTEM system"
+               ;;
+
+#  Convex running ConvexOS.
+#  ------------------------
+            convex)
+               AR_IN='ar r'
+               FC='fc'
+               FFLAGS='-O3'
+               CC='gcc'
+               CFLAGS='-I$(STAR_INC) -O -fPIC'
+               LINK='ln -s'
+               RANLIB='ranlib'
+               TAR_IN='tar -cvhf'
+               TAR_OUT='tar -xf'
+               echo "mk: Environment variables defined for $SYSTEM system"
+               ;;
+
+#  IMPORTANT NOTE - Because Convex make doesn't support the -e
+#  qualifier (as stipulated by the POSIX standard) it will be
+#  necessary to use another version of make, for example the
+#  GNU one.  This can be accomplished either by editing this script,
+#  or by setting up a link.
+
+#  Issue a warning if SYSTEM is not recognised.
+            *)
+               SOURCE_VARIANT='unknown'
+               echo "mk: WARNING: value of SYSTEM = $SYSTEM not recognised..."
+               echo "             ...assuming default system characteristics"
+               echo '             ...setting SOURCE_VARIANT to "unknown"'
+               ;;
+         esac
+
+#  Invoke make with the appropriate environment variables set to override
+#  default macros defined in the makefile.
+         echo make -e $*
+         make -e $*
+      fi
+
+#  End of script.
diff --git a/src/slalib/moon.f b/src/slalib/moon.f
new file mode 100644
index 0000000..eaf1c72
--- /dev/null
+++ b/src/slalib/moon.f
@@ -0,0 +1,362 @@
+      SUBROUTINE sla_MOON (IY, ID, FD, PV)
+*+
+*     - - - - -
+*      M O O N
+*     - - - - -
+*
+*  Approximate geocentric position and velocity of the Moon
+*  (single precision).
+*
+*  Given:
+*     IY       i       year
+*     ID       i       day in year (1 = Jan 1st)
+*     FD       r       fraction of day
+*
+*  Returned:
+*     PV       r(6)    Moon position & velocity vector
+*
+*  Notes:
+*
+*  1  The date and time is TDB (loosely ET) in a Julian calendar
+*     which has been aligned to the ordinary Gregorian
+*     calendar for the interval 1900 March 1 to 2100 February 28.
+*     The year and day can be obtained by calling sla_CALYD or
+*     sla_CLYD.
+*
+*  2  The Moon 6-vector is Moon centre relative to Earth centre,
+*     mean equator and equinox of date.  Position part, PV(1-3),
+*     is in AU;  velocity part, PV(4-6), is in AU/sec.
+*
+*  3  The position is accurate to better than 0.5 arcminute
+*     in direction and 1000 km in distance.  The velocity
+*     is accurate to better than 0.5"/hour in direction and
+*     4 m/s in distance.  (RMS figures with respect to JPL DE200
+*     for the interval 1960-2025 are 14 arcsec and 0.2 arcsec/hour in
+*     longitude, 9 arcsec and 0.2 arcsec/hour in latitude, 350 km and
+*     2 m/s in distance.)  Note that the distance accuracy is
+*     comparatively poor because this routine is principally intended
+*     for computing topocentric direction.
+*
+*  4  This routine is only a partial implementation of the original
+*     Meeus algorithm (reference below), which offers 4 times the
+*     accuracy in direction and 30 times the accuracy in distance
+*     when fully implemented (as it is in sla_DMOON).
+*
+*  Reference:
+*     Meeus, l'Astronomie, June 1984, p348.
+*
+*  Called:  sla_CS2C6
+*
+*  P.T.Wallace   Starlink   8 December 1994
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER IY,ID
+      REAL FD,PV(6)
+
+      INTEGER ITP(4,4),ITL(4,39),ITB(4,29),I,IY4,N
+      REAL D2R,RATCON,ERADAU
+      REAL ELP0,ELP1,ELP1I,ELP1F
+      REAL EM0,EM1,EM1F
+      REAL EMP0,EMP1,EMP1I,EMP1F
+      REAL D0,D1,D1I,D1F
+      REAL F0,F1,F1I,F1F
+      REAL TL(39)
+      REAL TB(29)
+      REAL TP(4)
+      REAL YI,YF,T,ELP,EM,EMP,D,F,EL,ELD,COEFF,CEM,CEMP
+      REAL CD,CF,THETA,THETAD,B,BD,P,PD,SP,R,RD
+      REAL V(6),EPS,SINEPS,COSEPS
+
+*  Degrees to radians
+      PARAMETER (D2R=1.745329252E-2)
+
+*  Rate conversion factor:  D2R**2/(86400*365.25)
+      PARAMETER (RATCON=9.652743551E-12)
+
+*  Earth radius in AU:  6378.137/149597870
+      PARAMETER (ERADAU=4.2635212653763E-5)
+
+*
+*  Coefficients for fundamental arguments
+*
+*  Fixed term (deg), term in T (deg & whole revs + fraction per year)
+*
+*  Moon's mean longitude
+      DATA ELP0,ELP1,ELP1I,ELP1F /
+     :            270.434164, 4812.678831, 4680., 132.678831 /
+*
+*  Sun's mean anomaly
+      DATA EM0,EM1,EM1F /
+     :            358.475833,  359.990498,        359.990498 /
+*
+*  Moon's mean anomaly
+      DATA EMP0,EMP1,EMP1I,EMP1F /
+     :            296.104608, 4771.988491, 4680.,  91.988491 /
+*
+*  Moon's mean elongation
+      DATA D0,D1,D1I,D1F /
+     :            350.737486,  4452.671142, 4320., 132.671142 /
+*
+*  Mean distance of the Moon from its ascending node
+      DATA F0,F1,F1I,F1F /
+     :             11.250889, 4832.020251, 4680., 152.020251 /
+
+*
+*  Coefficients for Moon position
+*
+*   T(N)       = coefficient of term (deg)
+*   IT(N,1-4)  = coefficients of M, M', D, F in argument
+*
+*  Longitude
+*                                         M   M'  D   F
+      DATA TL( 1)/            +6.288750                     /,
+     :     (ITL(I, 1),I=1,4)/             0, +1,  0,  0     /
+      DATA TL( 2)/            +1.274018                     /,
+     :     (ITL(I, 2),I=1,4)/             0, -1, +2,  0     /
+      DATA TL( 3)/            +0.658309                     /,
+     :     (ITL(I, 3),I=1,4)/             0,  0, +2,  0     /
+      DATA TL( 4)/            +0.213616                     /,
+     :     (ITL(I, 4),I=1,4)/             0, +2,  0,  0     /
+      DATA TL( 5)/            -0.185596                     /,
+     :     (ITL(I, 5),I=1,4)/            +1,  0,  0,  0     /
+      DATA TL( 6)/            -0.114336                     /,
+     :     (ITL(I, 6),I=1,4)/             0,  0,  0, +2     /
+      DATA TL( 7)/            +0.058793                     /,
+     :     (ITL(I, 7),I=1,4)/             0, -2, +2,  0     /
+      DATA TL( 8)/            +0.057212                     /,
+     :     (ITL(I, 8),I=1,4)/            -1, -1, +2,  0     /
+      DATA TL( 9)/            +0.053320                     /,
+     :     (ITL(I, 9),I=1,4)/             0, +1, +2,  0     /
+      DATA TL(10)/            +0.045874                     /,
+     :     (ITL(I,10),I=1,4)/            -1,  0, +2,  0     /
+      DATA TL(11)/            +0.041024                     /,
+     :     (ITL(I,11),I=1,4)/            -1, +1,  0,  0     /
+      DATA TL(12)/            -0.034718                     /,
+     :     (ITL(I,12),I=1,4)/             0,  0, +1,  0     /
+      DATA TL(13)/            -0.030465                     /,
+     :     (ITL(I,13),I=1,4)/            +1, +1,  0,  0     /
+      DATA TL(14)/            +0.015326                     /,
+     :     (ITL(I,14),I=1,4)/             0,  0, +2, -2     /
+      DATA TL(15)/            -0.012528                     /,
+     :     (ITL(I,15),I=1,4)/             0, +1,  0, +2     /
+      DATA TL(16)/            -0.010980                     /,
+     :     (ITL(I,16),I=1,4)/             0, -1,  0, +2     /
+      DATA TL(17)/            +0.010674                     /,
+     :     (ITL(I,17),I=1,4)/             0, -1, +4,  0     /
+      DATA TL(18)/            +0.010034                     /,
+     :     (ITL(I,18),I=1,4)/             0, +3,  0,  0     /
+      DATA TL(19)/            +0.008548                     /,
+     :     (ITL(I,19),I=1,4)/             0, -2, +4,  0     /
+      DATA TL(20)/            -0.007910                     /,
+     :     (ITL(I,20),I=1,4)/            +1, -1, +2,  0     /
+      DATA TL(21)/            -0.006783                     /,
+     :     (ITL(I,21),I=1,4)/            +1,  0, +2,  0     /
+      DATA TL(22)/            +0.005162                     /,
+     :     (ITL(I,22),I=1,4)/             0, +1, -1,  0     /
+      DATA TL(23)/            +0.005000                     /,
+     :     (ITL(I,23),I=1,4)/            +1,  0, +1,  0     /
+      DATA TL(24)/            +0.004049                     /,
+     :     (ITL(I,24),I=1,4)/            -1, +1, +2,  0     /
+      DATA TL(25)/            +0.003996                     /,
+     :     (ITL(I,25),I=1,4)/             0, +2, +2,  0     /
+      DATA TL(26)/            +0.003862                     /,
+     :     (ITL(I,26),I=1,4)/             0,  0, +4,  0     /
+      DATA TL(27)/            +0.003665                     /,
+     :     (ITL(I,27),I=1,4)/             0, -3, +2,  0     /
+      DATA TL(28)/            +0.002695                     /,
+     :     (ITL(I,28),I=1,4)/            -1, +2,  0,  0     /
+      DATA TL(29)/            +0.002602                     /,
+     :     (ITL(I,29),I=1,4)/             0, +1, -2, -2     /
+      DATA TL(30)/            +0.002396                     /,
+     :     (ITL(I,30),I=1,4)/            -1, -2, +2,  0     /
+      DATA TL(31)/            -0.002349                     /,
+     :     (ITL(I,31),I=1,4)/             0, +1, +1,  0     /
+      DATA TL(32)/            +0.002249                     /,
+     :     (ITL(I,32),I=1,4)/            -2,  0, +2,  0     /
+      DATA TL(33)/            -0.002125                     /,
+     :     (ITL(I,33),I=1,4)/            +1, +2,  0,  0     /
+      DATA TL(34)/            -0.002079                     /,
+     :     (ITL(I,34),I=1,4)/            +2,  0,  0,  0     /
+      DATA TL(35)/            +0.002059                     /,
+     :     (ITL(I,35),I=1,4)/            -2, -1, +2,  0     /
+      DATA TL(36)/            -0.001773                     /,
+     :     (ITL(I,36),I=1,4)/             0, +1, +2, -2     /
+      DATA TL(37)/            -0.001595                     /,
+     :     (ITL(I,37),I=1,4)/             0,  0, +2, +2     /
+      DATA TL(38)/            +0.001220                     /,
+     :     (ITL(I,38),I=1,4)/            -1, -1, +4,  0     /
+      DATA TL(39)/            -0.001110                     /,
+     :     (ITL(I,39),I=1,4)/             0, +2,  0, +2     /
+*
+*  Latitude
+*                                         M   M'  D   F
+      DATA TB( 1)/            +5.128189                     /,
+     :     (ITB(I, 1),I=1,4)/             0,  0,  0, +1     /
+      DATA TB( 2)/            +0.280606                     /,
+     :     (ITB(I, 2),I=1,4)/             0, +1,  0, +1     /
+      DATA TB( 3)/            +0.277693                     /,
+     :     (ITB(I, 3),I=1,4)/             0, +1,  0, -1     /
+      DATA TB( 4)/            +0.173238                     /,
+     :     (ITB(I, 4),I=1,4)/             0,  0, +2, -1     /
+      DATA TB( 5)/            +0.055413                     /,
+     :     (ITB(I, 5),I=1,4)/             0, -1, +2, +1     /
+      DATA TB( 6)/            +0.046272                     /,
+     :     (ITB(I, 6),I=1,4)/             0, -1, +2, -1     /
+      DATA TB( 7)/            +0.032573                     /,
+     :     (ITB(I, 7),I=1,4)/             0,  0, +2, +1     /
+      DATA TB( 8)/            +0.017198                     /,
+     :     (ITB(I, 8),I=1,4)/             0, +2,  0, +1     /
+      DATA TB( 9)/            +0.009267                     /,
+     :     (ITB(I, 9),I=1,4)/             0, +1, +2, -1     /
+      DATA TB(10)/            +0.008823                     /,
+     :     (ITB(I,10),I=1,4)/             0, +2,  0, -1     /
+      DATA TB(11)/            +0.008247                     /,
+     :     (ITB(I,11),I=1,4)/            -1,  0, +2, -1     /
+      DATA TB(12)/            +0.004323                     /,
+     :     (ITB(I,12),I=1,4)/             0, -2, +2, -1     /
+      DATA TB(13)/            +0.004200                     /,
+     :     (ITB(I,13),I=1,4)/             0, +1, +2, +1     /
+      DATA TB(14)/            +0.003372                     /,
+     :     (ITB(I,14),I=1,4)/            -1,  0, -2, +1     /
+      DATA TB(15)/            +0.002472                     /,
+     :     (ITB(I,15),I=1,4)/            -1, -1, +2, +1     /
+      DATA TB(16)/            +0.002222                     /,
+     :     (ITB(I,16),I=1,4)/            -1,  0, +2, +1     /
+      DATA TB(17)/            +0.002072                     /,
+     :     (ITB(I,17),I=1,4)/            -1, -1, +2, -1     /
+      DATA TB(18)/            +0.001877                     /,
+     :     (ITB(I,18),I=1,4)/            -1, +1,  0, +1     /
+      DATA TB(19)/            +0.001828                     /,
+     :     (ITB(I,19),I=1,4)/             0, -1, +4, -1     /
+      DATA TB(20)/            -0.001803                     /,
+     :     (ITB(I,20),I=1,4)/            +1,  0,  0, +1     /
+      DATA TB(21)/            -0.001750                     /,
+     :     (ITB(I,21),I=1,4)/             0,  0,  0, +3     /
+      DATA TB(22)/            +0.001570                     /,
+     :     (ITB(I,22),I=1,4)/            -1, +1,  0, -1     /
+      DATA TB(23)/            -0.001487                     /,
+     :     (ITB(I,23),I=1,4)/             0,  0, +1, +1     /
+      DATA TB(24)/            -0.001481                     /,
+     :     (ITB(I,24),I=1,4)/            +1, +1,  0, +1     /
+      DATA TB(25)/            +0.001417                     /,
+     :     (ITB(I,25),I=1,4)/            -1, -1,  0, +1     /
+      DATA TB(26)/            +0.001350                     /,
+     :     (ITB(I,26),I=1,4)/            -1,  0,  0, +1     /
+      DATA TB(27)/            +0.001330                     /,
+     :     (ITB(I,27),I=1,4)/             0,  0, -1, +1     /
+      DATA TB(28)/            +0.001106                     /,
+     :     (ITB(I,28),I=1,4)/             0, +3,  0, +1     /
+      DATA TB(29)/            +0.001020                     /,
+     :     (ITB(I,29),I=1,4)/             0,  0, +4, -1     /
+*
+*  Parallax
+*                                         M   M'  D   F
+      DATA TP( 1)/            +0.051818                     /,
+     :     (ITP(I, 1),I=1,4)/             0, +1,  0,  0     /
+      DATA TP( 2)/            +0.009531                     /,
+     :     (ITP(I, 2),I=1,4)/             0, -1, +2,  0     /
+      DATA TP( 3)/            +0.007843                     /,
+     :     (ITP(I, 3),I=1,4)/             0,  0, +2,  0     /
+      DATA TP( 4)/            +0.002824                     /,
+     :     (ITP(I, 4),I=1,4)/             0, +2,  0,  0     /
+
+
+
+*  Whole years & fraction of year, and years since J1900.0
+      YI=FLOAT(IY-1900)
+      IY4=MOD(MOD(IY,4)+4,4)
+      YF=(FLOAT(4*(ID-1/(IY4+1))-IY4-2)+4.0*FD)/1461.0
+      T=YI+YF
+
+*  Moon's mean longitude
+      ELP=D2R*MOD(ELP0+ELP1I*YF+ELP1F*T,360.0)
+
+*  Sun's mean anomaly
+      EM=D2R*MOD(EM0+EM1F*T,360.0)
+
+*  Moon's mean anomaly
+      EMP=D2R*MOD(EMP0+EMP1I*YF+EMP1F*T,360.0)
+
+*  Moon's mean elongation
+      D=D2R*MOD(D0+D1I*YF+D1F*T,360.0)
+
+*  Mean distance of the moon from its ascending node
+      F=D2R*MOD(F0+F1I*YF+F1F*T,360.0)
+
+*  Longitude
+      EL=0.0
+      ELD=0.0
+      DO N=39,1,-1
+         COEFF=TL(N)
+         CEM=FLOAT(ITL(1,N))
+         CEMP=FLOAT(ITL(2,N))
+         CD=FLOAT(ITL(3,N))
+         CF=FLOAT(ITL(4,N))
+         THETA=CEM*EM+CEMP*EMP+CD*D+CF*F
+         THETAD=CEM*EM1+CEMP*EMP1+CD*D1+CF*F1
+         EL=EL+COEFF*SIN(THETA)
+         ELD=ELD+COEFF*COS(THETA)*THETAD
+      END DO
+      EL=EL*D2R+ELP
+      ELD=RATCON*(ELD+ELP1/D2R)
+
+*  Latitude
+      B=0.0
+      BD=0.0
+      DO N=29,1,-1
+         COEFF=TB(N)
+         CEM=FLOAT(ITB(1,N))
+         CEMP=FLOAT(ITB(2,N))
+         CD=FLOAT(ITB(3,N))
+         CF=FLOAT(ITB(4,N))
+         THETA=CEM*EM+CEMP*EMP+CD*D+CF*F
+         THETAD=CEM*EM1+CEMP*EMP1+CD*D1+CF*F1
+         B=B+COEFF*SIN(THETA)
+         BD=BD+COEFF*COS(THETA)*THETAD
+      END DO
+      B=B*D2R
+      BD=RATCON*BD
+
+*  Parallax
+      P=0.0
+      PD=0.0
+      DO N=4,1,-1
+         COEFF=TP(N)
+         CEM=FLOAT(ITP(1,N))
+         CEMP=FLOAT(ITP(2,N))
+         CD=FLOAT(ITP(3,N))
+         CF=FLOAT(ITP(4,N))
+         THETA=CEM*EM+CEMP*EMP+CD*D+CF*F
+         THETAD=CEM*EM1+CEMP*EMP1+CD*D1+CF*F1
+         P=P+COEFF*COS(THETA)
+         PD=PD-COEFF*SIN(THETA)*THETAD
+      END DO
+      P=(P+0.950724)*D2R
+      PD=RATCON*PD
+
+*  Transform parallax to distance (AU, AU/sec)
+      SP=SIN(P)
+      R=ERADAU/SP
+      RD=-R*PD/SP
+
+*  Longitude, latitude to x,y,z (AU)
+      CALL sla_CS2C6(EL,B,R,ELD,BD,RD,V)
+
+*  Mean obliquity
+      EPS=D2R*(23.45229-0.00013*T)
+      SINEPS=SIN(EPS)
+      COSEPS=COS(EPS)
+
+*  Rotate Moon position and velocity into equatorial system
+      PV(1)=V(1)
+      PV(2)=V(2)*COSEPS-V(3)*SINEPS
+      PV(3)=V(2)*SINEPS+V(3)*COSEPS
+      PV(4)=V(4)
+      PV(5)=V(5)*COSEPS-V(6)*SINEPS
+      PV(6)=V(5)*SINEPS+V(6)*COSEPS
+
+      END
diff --git a/src/slalib/mxm.f b/src/slalib/mxm.f
new file mode 100644
index 0000000..67ce113
--- /dev/null
+++ b/src/slalib/mxm.f
@@ -0,0 +1,55 @@
+      SUBROUTINE sla_MXM (A, B, C)
+*+
+*     - - - -
+*      M X M
+*     - - - -
+*
+*  Product of two 3x3 matrices:
+*      matrix C  =  matrix A  x  matrix B
+*
+*  (single precision)
+*
+*  Given:
+*      A      real(3,3)        matrix
+*      B      real(3,3)        matrix
+*
+*  Returned:
+*      C      real(3,3)        matrix result
+*
+*  To comply with the ANSI Fortran 77 standard, A, B and C must
+*  be different arrays.  However, the routine is coded so as to
+*  work properly on the VAX and many other systems even if this
+*  rule is violated.
+*
+*  P.T.Wallace   Starlink   5 April 1990
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL A(3,3),B(3,3),C(3,3)
+
+      INTEGER I,J,K
+      REAL W,WM(3,3)
+
+
+*  Multiply into scratch matrix
+      DO I=1,3
+         DO J=1,3
+            W=0.0
+            DO K=1,3
+               W=W+A(I,K)*B(K,J)
+            END DO
+            WM(I,J)=W
+         END DO
+      END DO
+
+*  Return the result
+      DO J=1,3
+         DO I=1,3
+            C(I,J)=WM(I,J)
+         END DO
+      END DO
+
+      END
diff --git a/src/slalib/mxv.f b/src/slalib/mxv.f
new file mode 100644
index 0000000..2935f72
--- /dev/null
+++ b/src/slalib/mxv.f
@@ -0,0 +1,47 @@
+      SUBROUTINE sla_MXV (RM, VA, VB)
+*+
+*     - - - -
+*      M X V
+*     - - - -
+*
+*  Performs the 3-D forward unitary transformation:
+*
+*     vector VB = matrix RM * vector VA
+*
+*  (single precision)
+*
+*  Given:
+*     RM       real(3,3)    matrix
+*     VA       real(3)      vector
+*
+*  Returned:
+*     VB       real(3)      result vector
+*
+*  P.T.Wallace   Starlink   March 1986
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL RM(3,3),VA(3),VB(3)
+
+      INTEGER I,J
+      REAL W,VW(3)
+
+
+*  Matrix RM * vector VA -> vector VW
+      DO J=1,3
+         W=0.0
+         DO I=1,3
+            W=W+RM(J,I)*VA(I)
+         END DO
+         VW(J)=W
+      END DO
+
+*  Vector VW -> vector VB
+      DO J=1,3
+         VB(J)=VW(J)
+      END DO
+
+      END
diff --git a/src/slalib/nut.f b/src/slalib/nut.f
new file mode 100644
index 0000000..bf2d196
--- /dev/null
+++ b/src/slalib/nut.f
@@ -0,0 +1,44 @@
+      SUBROUTINE sla_NUT (DATE, RMATN)
+*+
+*     - - - -
+*      N U T
+*     - - - -
+*
+*  Form the matrix of nutation for a given date - IAU 1980 theory
+*  (double precision)
+*
+*  References:
+*     Final report of the IAU Working Group on Nutation,
+*      chairman P.K.Seidelmann, 1980.
+*     Kaplan,G.H., 1981, USNO circular no. 163, pA3-6.
+*
+*  Given:
+*     DATE   dp         TDB (loosely ET) as Modified Julian Date
+*                                           (=JD-2400000.5)
+*  Returned:
+*     RMATN  dp(3,3)    nutation matrix
+*
+*  The matrix is in the sense   V(true)  =  RMATN * V(mean)
+*
+*  Called:   sla_NUTC, sla_DEULER
+*
+*  P.T.Wallace   Starlink   1 January 1993
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DATE,RMATN(3,3)
+
+      DOUBLE PRECISION DPSI,DEPS,EPS0
+
+
+
+*  Nutation components and mean obliquity
+      CALL sla_NUTC(DATE,DPSI,DEPS,EPS0)
+
+*  Rotation matrix
+      CALL sla_DEULER('XZX',EPS0,-DPSI,-(EPS0+DEPS),RMATN)
+
+      END
diff --git a/src/slalib/nutc.f b/src/slalib/nutc.f
new file mode 100644
index 0000000..1f5890c
--- /dev/null
+++ b/src/slalib/nutc.f
@@ -0,0 +1,442 @@
+      SUBROUTINE sla_NUTC (DATE, DPSI, DEPS, EPS0)
+*+
+*     - - - - -
+*      N U T C
+*     - - - - -
+*
+*  Nutation:  longitude & obliquity components and mean
+*  obliquity - IAU 1980 theory (double precision)
+*
+*  Given:
+*
+*     DATE        dp    TDB (loosely ET) as Modified Julian Date
+*                                            (JD-2400000.5)
+*  Returned:
+*
+*     DPSI,DEPS   dp    nutation in longitude,obliquity
+*     EPS0        dp    mean obliquity
+*
+*  References:
+*     Final report of the IAU Working Group on Nutation,
+*      chairman P.K.Seidelmann, 1980.
+*     Kaplan,G.H., 1981, USNO circular no. 163, pA3-6.
+*
+*  P.T.Wallace   Starlink   23 August 1996
+*
+*  Copyright (C) 1996 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DATE,DPSI,DEPS,EPS0
+
+      DOUBLE PRECISION T2AS,AS2R,U2R
+      DOUBLE PRECISION T,EL,EL2,EL3
+      DOUBLE PRECISION ELP,ELP2
+      DOUBLE PRECISION F,F2,F4
+      DOUBLE PRECISION D,D2,D4
+      DOUBLE PRECISION OM,OM2
+      DOUBLE PRECISION DP,DE
+      DOUBLE PRECISION A
+
+
+*  Turns to arc seconds
+      PARAMETER (T2AS=1296000D0)
+*  Arc seconds to radians
+      PARAMETER (AS2R=0.484813681109535994D-5)
+*  Units of 0.0001 arcsec to radians
+      PARAMETER (U2R=AS2R/1D4)
+
+
+
+
+*  Interval between basic epoch J2000.0 and current epoch (JC)
+      T=(DATE-51544.5D0)/36525D0
+
+*
+*  FUNDAMENTAL ARGUMENTS in the FK5 reference system
+*
+
+*  Mean longitude of the Moon minus mean longitude of the Moon's perigee
+      EL=AS2R*(485866.733D0+(1325D0*T2AS+715922.633D0
+     :         +(31.310D0+0.064D0*T)*T)*T)
+
+*  Mean longitude of the Sun minus mean longitude of the Sun's perigee
+      ELP=AS2R*(1287099.804D0+(99D0*T2AS+1292581.224D0
+     :         +(-0.577D0-0.012D0*T)*T)*T)
+
+*  Mean longitude of the Moon minus mean longitude of the Moon's node
+      F=AS2R*(335778.877D0+(1342D0*T2AS+295263.137D0
+     :         +(-13.257D0+0.011D0*T)*T)*T)
+
+*  Mean elongation of the Moon from the Sun
+      D=AS2R*(1072261.307D0+(1236D0*T2AS+1105601.328D0
+     :         +(-6.891D0+0.019D0*T)*T)*T)
+
+*  Longitude of the mean ascending node of the lunar orbit on the
+*   ecliptic, measured from the mean equinox of date
+      OM=AS2R*(450160.280D0+(-5D0*T2AS-482890.539D0
+     :         +(7.455D0+0.008D0*T)*T)*T)
+
+*  Multiples of arguments
+      EL2=EL+EL
+      EL3=EL2+EL
+      ELP2=ELP+ELP
+      F2=F+F
+      F4=F2+F2
+      D2=D+D
+      D4=D2+D2
+      OM2=OM+OM
+
+
+*
+*  SERIES FOR THE NUTATION
+*
+      DP=0D0
+      DE=0D0
+
+*  106
+      DP=DP+SIN(ELP+D)
+*  105
+      DP=DP-SIN(F2+D4+OM2)
+*  104
+      DP=DP+SIN(EL2+D2)
+*  103
+      DP=DP-SIN(EL-F2+D2)
+*  102
+      DP=DP-SIN(EL+ELP-D2+OM)
+*  101
+      DP=DP-SIN(-ELP+F2+OM)
+*  100
+      DP=DP-SIN(EL-F2-D2)
+*  99
+      DP=DP-SIN(ELP+D2)
+*  98
+      DP=DP-SIN(F2-D+OM2)
+*  97
+      DP=DP-SIN(-F2+OM)
+*  96
+      DP=DP+SIN(-EL-ELP+D2+OM)
+*  95
+      DP=DP+SIN(ELP+F2+OM)
+*  94
+      DP=DP-SIN(EL+F2-D2)
+*  93
+      DP=DP+SIN(EL3+F2-D2+OM2)
+*  92
+      DP=DP+SIN(F4-D2+OM2)
+*  91
+      DP=DP-SIN(EL+D2+OM)
+*  90
+      DP=DP-SIN(EL2+F2+D2+OM2)
+*  89
+      A=EL2+F2-D2+OM
+      DP=DP+SIN(A)
+      DE=DE-COS(A)
+*  88
+      DP=DP+SIN(EL-ELP-D2)
+*  87
+      DP=DP+SIN(-EL+F4+OM2)
+*  86
+      A=-EL2+F2+D4+OM2
+      DP=DP-SIN(A)
+      DE=DE+COS(A)
+*  85
+      A=EL+F2+D2+OM
+      DP=DP-SIN(A)
+      DE=DE+COS(A)
+*  84
+      A=EL+ELP+F2-D2+OM2
+      DP=DP+SIN(A)
+      DE=DE-COS(A)
+*  83
+      DP=DP-SIN(EL2-D4)
+*  82
+      A=-EL+F2+D4+OM2
+      DP=DP-2D0*SIN(A)
+      DE=DE+COS(A)
+*  81
+      A=-EL2+F2+D2+OM2
+      DP=DP+SIN(A)
+      DE=DE-COS(A)
+*  80
+      DP=DP-SIN(EL-D4)
+*  79
+      A=-EL+OM2
+      DP=DP+SIN(A)
+      DE=DE-COS(A)
+*  78
+      A=F2+D+OM2
+      DP=DP+2D0*SIN(A)
+      DE=DE-COS(A)
+*  77
+      DP=DP+2D0*SIN(EL3)
+*  76
+      A=EL+OM2
+      DP=DP-2D0*SIN(A)
+      DE=DE+COS(A)
+*  75
+      A=EL2+OM
+      DP=DP+2D0*SIN(A)
+      DE=DE-COS(A)
+*  74
+      A=-EL+F2-D2+OM
+      DP=DP-2D0*SIN(A)
+      DE=DE+COS(A)
+*  73
+      A=EL+ELP+F2+OM2
+      DP=DP+2D0*SIN(A)
+      DE=DE-COS(A)
+*  72
+      A=-ELP+F2+D2+OM2
+      DP=DP-3D0*SIN(A)
+      DE=DE+COS(A)
+*  71
+      A=EL3+F2+OM2
+      DP=DP-3D0*SIN(A)
+      DE=DE+COS(A)
+*  70
+      A=-EL2+OM
+      DP=DP-2D0*SIN(A)
+      DE=DE+COS(A)
+*  69
+      A=-EL-ELP+F2+D2+OM2
+      DP=DP-3D0*SIN(A)
+      DE=DE+COS(A)
+*  68
+      A=EL-ELP+F2+OM2
+      DP=DP-3D0*SIN(A)
+      DE=DE+COS(A)
+*  67
+      DP=DP+3D0*SIN(EL+F2)
+*  66
+      DP=DP-3D0*SIN(EL+ELP)
+*  65
+      DP=DP-4D0*SIN(D)
+*  64
+      DP=DP+4D0*SIN(EL-F2)
+*  63
+      DP=DP-4D0*SIN(ELP-D2)
+*  62
+      A=EL2+F2+OM
+      DP=DP-5D0*SIN(A)
+      DE=DE+3D0*COS(A)
+*  61
+      DP=DP+5D0*SIN(EL-ELP)
+*  60
+      A=-D2+OM
+      DP=DP-5D0*SIN(A)
+      DE=DE+3D0*COS(A)
+*  59
+      A=EL+F2-D2+OM
+      DP=DP+6D0*SIN(A)
+      DE=DE-3D0*COS(A)
+*  58
+      A=F2+D2+OM
+      DP=DP-7D0*SIN(A)
+      DE=DE+3D0*COS(A)
+*  57
+      A=D2+OM
+      DP=DP-6D0*SIN(A)
+      DE=DE+3D0*COS(A)
+*  56
+      A=EL2+F2-D2+OM2
+      DP=DP+6D0*SIN(A)
+      DE=DE-3D0*COS(A)
+*  55
+      DP=DP+6D0*SIN(EL+D2)
+*  54
+      A=EL+F2+D2+OM2
+      DP=DP-8D0*SIN(A)
+      DE=DE+3D0*COS(A)
+*  53
+      A=-ELP+F2+OM2
+      DP=DP-7D0*SIN(A)
+      DE=DE+3D0*COS(A)
+*  52
+      A=ELP+F2+OM2
+      DP=DP+7D0*SIN(A)
+      DE=DE-3D0*COS(A)
+*  51
+      DP=DP-7D0*SIN(EL+ELP-D2)
+*  50
+      A=-EL+F2+D2+OM
+      DP=DP-10D0*SIN(A)
+      DE=DE+5D0*COS(A)
+*  49
+      A=EL-D2+OM
+      DP=DP-13D0*SIN(A)
+      DE=DE+7D0*COS(A)
+*  48
+      A=-EL+D2+OM
+      DP=DP+16D0*SIN(A)
+      DE=DE-8D0*COS(A)
+*  47
+      A=-EL+F2+OM
+      DP=DP+21D0*SIN(A)
+      DE=DE-10D0*COS(A)
+*  46
+      DP=DP+26D0*SIN(F2)
+      DE=DE-COS(F2)
+*  45
+      A=EL2+F2+OM2
+      DP=DP-31D0*SIN(A)
+      DE=DE+13D0*COS(A)
+*  44
+      A=EL+F2-D2+OM2
+      DP=DP+29D0*SIN(A)
+      DE=DE-12D0*COS(A)
+*  43
+      DP=DP+29D0*SIN(EL2)
+      DE=DE-COS(EL2)
+*  42
+      A=F2+D2+OM2
+      DP=DP-38D0*SIN(A)
+      DE=DE+16D0*COS(A)
+*  41
+      A=EL+F2+OM
+      DP=DP-51D0*SIN(A)
+      DE=DE+27D0*COS(A)
+*  40
+      A=-EL+F2+D2+OM2
+      DP=DP-59D0*SIN(A)
+      DE=DE+26D0*COS(A)
+*  39
+      A=-EL+OM
+      DP=DP+(-58D0-0.1D0*T)*SIN(A)
+      DE=DE+32D0*COS(A)
+*  38
+      A=EL+OM
+      DP=DP+(63D0+0.1D0*T)*SIN(A)
+      DE=DE-33D0*COS(A)
+*  37
+      DP=DP+63D0*SIN(D2)
+      DE=DE-2D0*COS(D2)
+*  36
+      A=-EL+F2+OM2
+      DP=DP+123D0*SIN(A)
+      DE=DE-53D0*COS(A)
+*  35
+      A=EL-D2
+      DP=DP-158D0*SIN(A)
+      DE=DE-COS(A)
+*  34
+      A=EL+F2+OM2
+      DP=DP-301D0*SIN(A)
+      DE=DE+(129D0-0.1D0*T)*COS(A)
+*  33
+      A=F2+OM
+      DP=DP+(-386D0-0.4D0*T)*SIN(A)
+      DE=DE+200D0*COS(A)
+*  32
+      DP=DP+(712D0+0.1D0*T)*SIN(EL)
+      DE=DE-7D0*COS(EL)
+*  31
+      A=F2+OM2
+      DP=DP+(-2274D0-0.2D0*T)*SIN(A)
+      DE=DE+(977D0-0.5D0*T)*COS(A)
+*  30
+      DP=DP-SIN(ELP+F2-D2)
+*  29
+      DP=DP+SIN(-EL+D+OM)
+*  28
+      DP=DP+SIN(ELP+OM2)
+*  27
+      DP=DP-SIN(ELP-F2+D2)
+*  26
+      DP=DP+SIN(-F2+D2+OM)
+*  25
+      DP=DP+SIN(EL2+ELP-D2)
+*  24
+      DP=DP-4D0*SIN(EL-D)
+*  23
+      A=ELP+F2-D2+OM
+      DP=DP+4D0*SIN(A)
+      DE=DE-2D0*COS(A)
+*  22
+      A=EL2-D2+OM
+      DP=DP+4D0*SIN(A)
+      DE=DE-2D0*COS(A)
+*  21
+      A=-ELP+F2-D2+OM
+      DP=DP-5D0*SIN(A)
+      DE=DE+3D0*COS(A)
+*  20
+      A=-EL2+D2+OM
+      DP=DP-6D0*SIN(A)
+      DE=DE+3D0*COS(A)
+*  19
+      A=-ELP+OM
+      DP=DP-12D0*SIN(A)
+      DE=DE+6D0*COS(A)
+*  18
+      A=ELP2+F2-D2+OM2
+      DP=DP+(-16D0+0.1D0*T)*SIN(A)
+      DE=DE+7D0*COS(A)
+*  17
+      A=ELP+OM
+      DP=DP-15D0*SIN(A)
+      DE=DE+9D0*COS(A)
+*  16
+      DP=DP+(17D0-0.1D0*T)*SIN(ELP2)
+*  15
+      DP=DP-22D0*SIN(F2-D2)
+*  14
+      A=EL2-D2
+      DP=DP+48D0*SIN(A)
+      DE=DE+COS(A)
+*  13
+      A=F2-D2+OM
+      DP=DP+(129D0+0.1D0*T)*SIN(A)
+      DE=DE-70D0*COS(A)
+*  12
+      A=-ELP+F2-D2+OM2
+      DP=DP+(217D0-0.5D0*T)*SIN(A)
+      DE=DE+(-95D0+0.3D0*T)*COS(A)
+*  11
+      A=ELP+F2-D2+OM2
+      DP=DP+(-517D0+1.2D0*T)*SIN(A)
+      DE=DE+(224D0-0.6D0*T)*COS(A)
+*  10
+      DP=DP+(1426D0-3.4D0*T)*SIN(ELP)
+      DE=DE+(54D0-0.1D0*T)*COS(ELP)
+*  9
+      A=F2-D2+OM2
+      DP=DP+(-13187D0-1.6D0*T)*SIN(A)
+      DE=DE+(5736D0-3.1D0*T)*COS(A)
+*  8
+      DP=DP+SIN(EL2-F2+OM)
+*  7
+      A=-ELP2+F2-D2+OM
+      DP=DP-2D0*SIN(A)
+      DE=DE+1D0*COS(A)
+*  6
+      DP=DP-3D0*SIN(EL-ELP-D)
+*  5
+      A=-EL2+F2+OM2
+      DP=DP-3D0*SIN(A)
+      DE=DE+1D0*COS(A)
+*  4
+      DP=DP+11D0*SIN(EL2-F2)
+*  3
+      A=-EL2+F2+OM
+      DP=DP+46D0*SIN(A)
+      DE=DE-24D0*COS(A)
+*  2
+      DP=DP+(2062D0+0.2D0*T)*SIN(OM2)
+      DE=DE+(-895D0+0.5D0*T)*COS(OM2)
+*  1
+      DP=DP+(-171996D0-174.2D0*T)*SIN(OM)
+      DE=DE+(92025D0+8.9D0*T)*COS(OM)
+
+*  Convert results to radians
+      DPSI=DP*U2R
+      DEPS=DE*U2R
+
+*  Mean obliquity
+      EPS0=AS2R*(84381.448D0+
+     :           (-46.8150D0+
+     :           (-0.00059D0+
+     :           0.001813D0*T)*T)*T)
+
+      END
diff --git a/src/slalib/oap.f b/src/slalib/oap.f
new file mode 100644
index 0000000..6376397
--- /dev/null
+++ b/src/slalib/oap.f
@@ -0,0 +1,172 @@
+      SUBROUTINE sla_OAP (TYPE, OB1, OB2, DATE, DUT, ELONGM, PHIM,
+     :                    HM, XP, YP, TDK, PMB, RH, WL, TLR,
+     :                    RAP, DAP)
+*+
+*     - - - -
+*      O A P
+*     - - - -
+*
+*  Observed to apparent place
+*
+*  Given:
+*     TYPE   c*(*)  type of coordinates - 'R', 'H' or 'A' (see below)
+*     OB1    d      observed Az, HA or RA (radians; Az is N=0,E=90)
+*     OB2    d      observed ZD or Dec (radians)
+*     DATE   d      UTC date/time (modified Julian Date, JD-2400000.5)
+*     DUT    d      delta UT:  UT1-UTC (UTC seconds)
+*     ELONGM d      mean longitude of the observer (radians, east +ve)
+*     PHIM   d      mean geodetic latitude of the observer (radians)
+*     HM     d      observer's height above sea level (metres)
+*     XP     d      polar motion x-coordinate (radians)
+*     YP     d      polar motion y-coordinate (radians)
+*     TDK    d      local ambient temperature (DegK; std=273.155D0)
+*     PMB    d      local atmospheric pressure (mB; std=1013.25D0)
+*     RH     d      local relative humidity (in the range 0D0-1D0)
+*     WL     d      effective wavelength (micron, e.g. 0.55D0)
+*     TLR    d      tropospheric lapse rate (DegK/metre, e.g. 0.0065D0)
+*
+*  Returned:
+*     RAP    d      geocentric apparent right ascension
+*     DAP    d      geocentric apparent declination
+*
+*  Notes:
+*
+*  1)  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 is 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.)
+*
+*  2)  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
+*      sla_REFRO routine returns a fixed value of the refraction.
+*      The complementary routines sla_AOP (or sla_AOPQK) and sla_OAP
+*      (or sla_OAPQK) are self-consistent to better than 1 micro-
+*      arcsecond all over the celestial sphere.
+*
+*  3)  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.
+*
+*  4)  "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.
+*
+*  5)  Frequently, mean rather than apparent RA,Dec will be required,
+*      in which case further transformations will be necessary.  The
+*      sla_AMP 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 sla_FK524 etc will also
+*      need to be applied.
+*
+*  6)  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.
+*
+*  7)  The star-independent apparent-to-observed-place parameters
+*      in AOPRMS may be computed by means of the sla_AOPPA routine.
+*      If nothing has changed significantly except the time, the
+*      sla_AOPPAT routine may be used to perform the requisite
+*      partial recomputation of AOPRMS.
+*
+*  8)  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.
+*
+*  9)  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.
+*
+*  10) 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
+*      sla_OBS routine are west-positive, following astronomical
+*      usage, and must be reversed in sign before use in the present
+*      routine.
+*
+*  11) 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.
+*
+*  12) 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 sla_OBS.  If P,
+*      the pressure in millibars, is available, an adequate
+*      estimate of HM can be obtained from the expression
+*
+*             HM ~ -29.3D0*TSL*LOG(P/1013.25D0).
+*
+*      where TSL is the approximate sea-level air temperature in
+*      deg 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 ~ 1013.25D0*EXP(-HM/(29.3D0*TSL)).
+*
+*      Note, however, that the refraction is proportional to the
+*      pressure and that an accurate P value is important for
+*      precise work.
+*
+*  13) The azimuths etc used by the present routine are with respect
+*      to the celestial pole.  Corrections from the terrestrial pole
+*      can be computed using sla_POLMO.
+*
+*  Called:  sla_AOPPA, sla_OAPQK
+*
+*  P.T.Wallace   Starlink   6 September 1999
+*
+*  Copyright (C) 1999 P.T.Wallace and CCLRC
+*-
+
+      IMPLICIT NONE
+
+      CHARACTER*(*) TYPE
+      DOUBLE PRECISION OB1,OB2,DATE,DUT,ELONGM,PHIM,HM,
+     :                 XP,YP,TDK,PMB,RH,WL,TLR,RAP,DAP
+
+      DOUBLE PRECISION AOPRMS(14)
+
+
+      CALL sla_AOPPA(DATE,DUT,ELONGM,PHIM,HM,XP,YP,TDK,PMB,RH,WL,TLR,
+     :               AOPRMS)
+      CALL sla_OAPQK(TYPE,OB1,OB2,AOPRMS,RAP,DAP)
+
+      END
diff --git a/src/slalib/oapqk.f b/src/slalib/oapqk.f
new file mode 100644
index 0000000..c50feb1
--- /dev/null
+++ b/src/slalib/oapqk.f
@@ -0,0 +1,233 @@
+      SUBROUTINE sla_OAPQK (TYPE, OB1, OB2, AOPRMS, RAP, DAP)
+*+
+*     - - - - - -
+*      O A P Q K
+*     - - - - - -
+*
+*  Quick observed to apparent place
+*
+*  Given:
+*     TYPE   c*(*)  type of coordinates - 'R', 'H' or 'A' (see below)
+*     OB1    d      observed Az, HA or RA (radians; Az is N=0,E=90)
+*     OB2    d      observed ZD or Dec (radians)
+*     AOPRMS d(14)  star-independent apparent-to-observed parameters:
+*
+*       (1)      geodetic latitude (radians)
+*       (2,3)    sine and cosine of geodetic latitude
+*       (4)      magnitude of diurnal aberration vector
+*       (5)      height (HM)
+*       (6)      ambient temperature (T)
+*       (7)      pressure (P)
+*       (8)      relative humidity (RH)
+*       (9)      wavelength (WL)
+*       (10)     lapse rate (TLR)
+*       (11,12)  refraction constants A and B (radians)
+*       (13)     longitude + eqn of equinoxes + sidereal DUT (radians)
+*       (14)     local apparent sidereal time (radians)
+*
+*  Returned:
+*     RAP    d      geocentric apparent right ascension
+*     DAP    d      geocentric apparent declination
+*
+*  Notes:
+*
+*  1)  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 is 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.)
+*
+*  2)  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
+*      sla_REFRO routine returns a fixed value of the refraction.
+*      The complementary routines sla_AOP (or sla_AOPQK) and sla_OAP
+*      (or sla_OAPQK) are self-consistent to better than 1 micro-
+*      arcsecond all over the celestial sphere.
+*
+*  3)  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.
+*
+*  5)  "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.
+*
+*  5)  Frequently, mean rather than apparent RA,Dec will be required,
+*      in which case further transformations will be necessary.  The
+*      sla_AMP 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 sla_FK524 etc will also
+*      need to be applied.
+*
+*  6)  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.
+*
+*  7)  The star-independent apparent-to-observed-place parameters
+*      in AOPRMS may be computed by means of the sla_AOPPA routine.
+*      If nothing has changed significantly except the time, the
+*      sla_AOPPAT routine may be used to perform the requisite
+*      partial recomputation of AOPRMS.
+*
+*  8) The azimuths etc used by the present routine are with respect
+*     to the celestial pole.  Corrections from the terrestrial pole
+*     can be computed using sla_POLMO.
+*
+*  Called:  sla_DCS2C, sla_DCC2S, sla_REFRO, sla_DRANRM
+*
+*  P.T.Wallace   Starlink   23 June 1997
+*
+*  Copyright (C) 1996 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      CHARACTER*(*) TYPE
+      DOUBLE PRECISION OB1,OB2,AOPRMS(14),RAP,DAP
+
+*  Breakpoint for fast/slow refraction algorithm:
+*  ZD greater than arctan(4), (see sla_REFCO routine)
+*  or vector Z less than cosine(arctan(Z)) = 1/sqrt(17)
+      DOUBLE PRECISION ZBREAK
+      PARAMETER (ZBREAK=0.242535625D0)
+
+      CHARACTER C
+      DOUBLE PRECISION 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
+
+      DOUBLE PRECISION sla_DRANRM
+
+
+
+*  Coordinate type
+      C = TYPE(1:1)
+
+*  Coordinates
+      C1 = OB1
+      C2 = OB2
+
+*  Sin, cos of latitude
+      SPHI = AOPRMS(2)
+      CPHI = AOPRMS(3)
+
+*  Local apparent sidereal time
+      ST = AOPRMS(14)
+
+*  Standardise coordinate type
+      IF (C.EQ.'R'.OR.C.EQ.'r') THEN
+         C = 'R'
+      ELSE IF (C.EQ.'H'.OR.C.EQ.'h') THEN
+         C = 'H'
+      ELSE
+         C = 'A'
+      END IF
+
+*  If Az,ZD convert to Cartesian (S=0,E=90)
+      IF (C.EQ.'A') THEN
+         CE = SIN(C2)
+         XAEO = -COS(C1)*CE
+         YAEO = SIN(C1)*CE
+         ZAEO = COS(C2)
+      ELSE
+
+*     If RA,Dec convert to HA,Dec
+         IF (C.EQ.'R') THEN
+            C1 = ST-C1
+         END IF
+
+*     To Cartesian -HA,Dec
+         CALL sla_DCS2C(-C1,C2,V)
+         XMHDO = V(1)
+         YMHDO = V(2)
+         ZMHDO = V(3)
+
+*     To Cartesian Az,El (S=0,E=90)
+         XAEO = SPHI*XMHDO-CPHI*ZMHDO
+         YAEO = YMHDO
+         ZAEO = CPHI*XMHDO+SPHI*ZMHDO
+      END IF
+
+*  Azimuth (S=0,E=90)
+      IF (XAEO.NE.0D0.OR.YAEO.NE.0D0) THEN
+         AZ = ATAN2(YAEO,XAEO)
+      ELSE
+         AZ = 0D0
+      END IF
+
+*  Sine of observed ZD, and observed ZD
+      SZ = SQRT(XAEO*XAEO+YAEO*YAEO)
+      ZDO = ATAN2(SZ,ZAEO)
+
+*
+*  Refraction
+*  ----------
+
+*  Large zenith distance?
+      IF (ZAEO.GE.ZBREAK) THEN
+
+*     Fast algorithm using two constant model
+         TZ = SZ/ZAEO
+         DREF = AOPRMS(11)*TZ+AOPRMS(12)*TZ*TZ*TZ
+
+      ELSE
+
+*     Rigorous algorithm for large ZD
+         CALL sla_REFRO(ZDO,AOPRMS(5),AOPRMS(6),AOPRMS(7),AOPRMS(8),
+     :                  AOPRMS(9),AOPRMS(1),AOPRMS(10),1D-8,DREF)
+      END IF
+
+      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(4)
+      F = (1D0-DIURAB*YMHDA)
+      V(1) = F*XMHDA
+      V(2) = F*(YMHDA+DIURAB)
+      V(3) = F*ZMHDA
+
+*  To spherical -HA,Dec
+      CALL sla_DCC2S(V,HMA,DAP)
+
+*  Right Ascension
+      RAP = sla_DRANRM(ST+HMA)
+
+      END
diff --git a/src/slalib/obs.f b/src/slalib/obs.f
new file mode 100644
index 0000000..756678b
--- /dev/null
+++ b/src/slalib/obs.f
@@ -0,0 +1,844 @@
+      SUBROUTINE sla_OBS (N, C, NAME, W, P, H)
+*+
+*     - - - -
+*      O B S
+*     - - - -
+*
+*  Parameters of selected groundbased observing stations
+*
+*  Given:
+*     N       int     number specifying observing station
+*
+*  Either given or returned
+*     C       c*(*)   identifier specifying observing station
+*
+*  Returned:
+*     NAME    c*(*)   name of specified observing station
+*     W       dp      longitude (radians, West +ve)
+*     P       dp      geodetic latitude (radians, North +ve)
+*     H       dp      height above sea level (metres)
+*
+*  Notes:
+*
+*     Station identifiers C may be up to 10 characters long,
+*     and station names NAME may be up to 40 characters long.
+*
+*     C and N are alternative ways of specifying the observing
+*     station.  The C option, which is the most generally useful,
+*     may be selected by specifying an N value of zero or less.
+*     If N is 1 or more, the parameters of the Nth station
+*     in the currently supported list are interrogated, and
+*     the station identifier C is returned as well as NAME, W,
+*     P and H.
+*
+*     If the station parameters are not available, either because
+*     the station identifier C is not recognized, or because an
+*     N value greater than the number of stations supported is
+*     given, a name of '?' is returned and C, W, P and H are left
+*     in their current states.
+*
+*     Programs can obtain a list of all currently supported
+*     stations by calling the routine repeatedly, with N=1,2,3...
+*     When NAME='?' is seen, the list of stations has been
+*     exhausted.
+*
+*     Station numbers, identifiers, names and other details are
+*     subject to change and should not be hardwired into
+*     application programs.
+*
+*     All station identifiers C are uppercase only;  lowercase
+*     characters must be converted to uppercase by the calling
+*     program.  The station names returned may contain both upper-
+*     and lowercase.  All characters up to the first space are
+*     checked;  thus an abbreviated ID will return the parameters
+*     for the first station in the list which matches the
+*     abbreviation supplied, and no station in the list will ever
+*     contain embedded spaces.  C must not have leading spaces.
+*
+*     IMPORTANT -- BEWARE OF THE LONGITUDE SIGN CONVENTION.  The
+*     longitude returned by sla_OBS is west-positive in accordance
+*     with astronomical usage.  However, this sign convention is
+*     left-handed and is the opposite of the one used by geographers;
+*     elsewhere in SLALIB the preferable east-positive convention is
+*     used.  In particular, note that for use in sla_AOP, sla_AOPPA
+*     and sla_OAP 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
+*
+*  P.T.Wallace   Starlink   21 April 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER N
+      CHARACTER C*(*),NAME*(*)
+      DOUBLE PRECISION W,P,H
+
+      INTEGER NMAX,M,NS,I
+      CHARACTER*10 CC
+
+      DOUBLE PRECISION AS2R,WEST,NORTH,EAST,SOUTH
+      INTEGER ID,IAM
+      REAL AS
+      PARAMETER (AS2R=0.484813681109535994D-5)
+
+*  Table of station identifiers
+      PARAMETER (NMAX=75)
+      CHARACTER*10 CTAB(NMAX)
+      DATA CTAB  (1) /'AAT       '/
+      DATA CTAB  (2) /'LPO4.2    '/
+      DATA CTAB  (3) /'LPO2.5    '/
+      DATA CTAB  (4) /'LPO1      '/
+      DATA CTAB  (5) /'LICK120   '/
+      DATA CTAB  (6) /'MMT       '/
+      DATA CTAB  (7) /'DAO72     '/
+      DATA CTAB  (8) /'DUPONT    '/
+      DATA CTAB  (9) /'MTHOP1.5  '/
+      DATA CTAB (10) /'STROMLO74 '/
+      DATA CTAB (11) /'ANU2.3    '/
+      DATA CTAB (12) /'GBVA140   '/
+      DATA CTAB (13) /'TOLOLO4M  '/
+      DATA CTAB (14) /'TOLOLO1.5M'/
+      DATA CTAB (15) /'TIDBINBLA '/
+      DATA CTAB (16) /'BLOEMF    '/
+      DATA CTAB (17) /'BOSQALEGRE'/
+      DATA CTAB (18) /'FLAGSTF61 '/
+      DATA CTAB (19) /'LOWELL72  '/
+      DATA CTAB (20) /'HARVARD   '/
+      DATA CTAB (21) /'OKAYAMA   '/
+      DATA CTAB (22) /'KPNO158   '/
+      DATA CTAB (23) /'KPNO90    '/
+      DATA CTAB (24) /'KPNO84    '/
+      DATA CTAB (25) /'KPNO36FT  '/
+      DATA CTAB (26) /'KOTTAMIA  '/
+      DATA CTAB (27) /'ESO3.6    '/
+      DATA CTAB (28) /'MAUNAK88  '/
+      DATA CTAB (29) /'UKIRT     '/
+      DATA CTAB (30) /'QUEBEC1.6 '/
+      DATA CTAB (31) /'MTEKAR    '/
+      DATA CTAB (32) /'MTLEMMON60'/
+      DATA CTAB (33) /'MCDONLD2.7'/
+      DATA CTAB (34) /'MCDONLD2.1'/
+      DATA CTAB (35) /'PALOMAR200'/
+      DATA CTAB (36) /'PALOMAR60 '/
+      DATA CTAB (37) /'DUNLAP74  '/
+      DATA CTAB (38) /'HPROV1.93 '/
+      DATA CTAB (39) /'HPROV1.52 '/
+      DATA CTAB (40) /'SANPM83   '/
+      DATA CTAB (41) /'SAAO74    '/
+      DATA CTAB (42) /'TAUTNBG   '/
+      DATA CTAB (43) /'CATALINA61'/
+      DATA CTAB (44) /'STEWARD90 '/
+      DATA CTAB (45) /'USSR6     '/
+      DATA CTAB (46) /'ARECIBO   '/
+      DATA CTAB (47) /'CAMB5KM   '/
+      DATA CTAB (48) /'CAMB1MILE '/
+      DATA CTAB (49) /'EFFELSBERG'/
+      DATA CTAB (50) /'GBVA300   '/
+      DATA CTAB (51) /'JODRELL1  '/
+      DATA CTAB (52) /'PARKES    '/
+      DATA CTAB (53) /'VLA       '/
+      DATA CTAB (54) /'SUGARGROVE'/
+      DATA CTAB (55) /'USSR600   '/
+      DATA CTAB (56) /'NOBEYAMA  '/
+      DATA CTAB (57) /'JCMT      '/
+      DATA CTAB (58) /'ESONTT    '/
+      DATA CTAB (59) /'ST.ANDREWS'/
+      DATA CTAB (60) /'APO3.5    '/
+      DATA CTAB (61) /'KECK1     '/
+      DATA CTAB (62) /'TAUTSCHM  '/
+      DATA CTAB (63) /'PALOMAR48 '/
+      DATA CTAB (64) /'UKST      '/
+      DATA CTAB (65) /'KISO      '/
+      DATA CTAB (66) /'ESOSCHM   '/
+      DATA CTAB (67) /'ATCA      '/
+      DATA CTAB (68) /'MOPRA     '/
+      DATA CTAB (69) /'SUBARU    '/
+      DATA CTAB (70) /'CFHT      '/
+      DATA CTAB (71) /'KECK2     '/
+      DATA CTAB (72) /'GEMININ   '/
+      DATA CTAB (73) /'FCRAO     '/
+      DATA CTAB (74) /'IRTF      '/
+      DATA CTAB (75) /'CSO       '/
+
+*  Degrees, arcminutes, arcseconds to radians
+      WEST(ID,IAM,AS)=AS2R*(DBLE(60*(60*ID+IAM))+DBLE(AS))
+      NORTH(ID,IAM,AS)=WEST(ID,IAM,AS)
+      EAST(ID,IAM,AS)=-WEST(ID,IAM,AS)
+      SOUTH(ID,IAM,AS)=-WEST(ID,IAM,AS)
+
+
+
+
+*  Station specified by number or identifier?
+      IF (N.GT.0) THEN
+
+*     Station specified by number
+         M=N
+         IF (M.LE.NMAX) C=CTAB(M)
+
+      ELSE
+
+*     Station specified by identifier:  determine corresponding number
+         CC=C
+         DO NS=1,NMAX
+            DO I=1,10
+               IF (CC(I:I).EQ.' ') GO TO 5
+               IF (CC(I:I).NE.CTAB(NS)(I:I)) GO TO 1
+            END DO
+            GO TO 5
+ 1          CONTINUE
+         END DO
+         NS=NMAX+1
+ 5       CONTINUE
+         IF (C(1:1).NE.' ') THEN
+            M=NS
+         ELSE
+            M=NMAX+1
+         END IF
+
+      END IF
+
+*
+*  Return parameters of Mth station
+*  --------------------------------
+
+      GO TO (10,20,30,40,50,60,70,80,90,100,
+     :       110,120,130,140,150,160,170,180,190,200,
+     :       210,220,230,240,250,260,270,280,290,300,
+     :       310,320,330,340,350,360,370,380,390,400,
+     :       410,420,430,440,450,460,470,480,490,500,
+     :       510,520,530,540,550,560,570,580,590,600,
+     :       610,620,630,640,650,660,670,680,690,700,
+     :       710,720,730,740,750) M
+      GO TO 9000
+
+*  AAT (Observer's Guide)                                            AAT
+ 10   CONTINUE
+      NAME='Anglo-Australian 3.9m Telescope'
+      W=EAST(149,03,57.91)
+      P=SOUTH(31,16,37.34)
+      H=1164D0
+      GO TO 9999
+
+*  WHT (Gemini, April 1987)                                       LPO4.2
+ 20   CONTINUE
+      NAME='William Herschel 4.2m Telescope'
+      W=WEST(17,52,53.9)
+      P=NORTH(28,45,38.1)
+      H=2332D0
+      GO TO 9999
+
+*  INT (Gemini, April 1987)                                       LPO2.5
+ 30   CONTINUE
+      NAME='Isaac Newton 2.5m Telescope'
+      W=WEST(17,52,39.5)
+      P=NORTH(28,45,43.2)
+      H=2336D0
+      GO TO 9999
+
+*  JKT (Gemini, April 1987)                                         LPO1
+ 40   CONTINUE
+      NAME='Jacobus Kapteyn 1m Telescope'
+      W=WEST(17,52,41.2)
+      P=NORTH(28,45,39.9)
+      H=2364D0
+      GO TO 9999
+
+*  Lick 120" (1984 Almanac)                                      LICK120
+ 50   CONTINUE
+      NAME='Lick 120 inch'
+      W=WEST(121,38,09.9)
+      P=NORTH(37,20,35.2)
+      H=1290D0
+      GO TO 9999
+
+*  MMT 6.5m conversion (MMT Observatory website)                     MMT
+ 60   CONTINUE
+      NAME='MMT 6.5m, Mt Hopkins'
+      W=WEST(110,53,04.4)
+      P=NORTH(31,41,19.6)
+      H=2608D0
+      GO TO 9999
+
+*  Victoria B.C. 1.85m (1984 Almanac)                              DAO72
+ 70   CONTINUE
+      NAME='DAO Victoria BC 1.85 metre'
+      W=WEST(123,25,01.18)
+      P=NORTH(48,31,11.9)
+      H=238D0
+      GO TO 9999
+
+*  Las Campanas (1983 Almanac)                                    DUPONT
+ 80   CONTINUE
+      NAME='Du Pont 2.5m Telescope, Las Campanas'
+      W=WEST(70,42,9.)
+      P=SOUTH(29,00,11.)
+      H=2280D0
+      GO TO 9999
+
+*  Mt Hopkins 1.5m (1983 Almanac)                               MTHOP1.5
+ 90   CONTINUE
+      NAME='Mt Hopkins 1.5 metre'
+      W=WEST(110,52,39.00)
+      P=NORTH(31,40,51.4)
+      H=2344D0
+      GO TO 9999
+
+*  Mt Stromlo 74" (1983 Almanac)                               STROMLO74
+ 100  CONTINUE
+      NAME='Mount Stromlo 74 inch'
+      W=EAST(149,00,27.59)
+      P=SOUTH(35,19,14.3)
+      H=767D0
+      GO TO 9999
+
+*  ANU 2.3m, SSO (Gary Hovey)                                     ANU2.3
+ 110  CONTINUE
+      NAME='Siding Spring 2.3 metre'
+      W=EAST(149,03,40.3)
+      P=SOUTH(31,16,24.1)
+      H=1149D0
+      GO TO 9999
+
+*  Greenbank 140' (1983 Almanac)                                 GBVA140
+ 120  CONTINUE
+      NAME='Greenbank 140 foot'
+      W=WEST(79,50,09.61)
+      P=NORTH(38,26,15.4)
+      H=881D0
+      GO TO 9999
+
+*  Cerro Tololo 4m (1982 Almanac)                               TOLOLO4M
+ 130  CONTINUE
+      NAME='Cerro Tololo 4 metre'
+      W=WEST(70,48,53.6)
+      P=SOUTH(30,09,57.8)
+      H=2235D0
+      GO TO 9999
+
+*  Cerro Tololo 1.5m (1982 Almanac)                           TOLOLO1.5M
+ 140  CONTINUE
+      NAME='Cerro Tololo 1.5 metre'
+      W=WEST(70,48,54.5)
+      P=SOUTH(30,09,56.3)
+      H=2225D0
+      GO TO 9999
+
+*  Tidbinbilla 64m (1982 Almanac)                              TIDBINBLA
+ 150  CONTINUE
+      NAME='Tidbinbilla 64 metre'
+      W=EAST(148,58,48.20)
+      P=SOUTH(35,24,14.3)
+      H=670D0
+      GO TO 9999
+
+*  Bloemfontein 1.52m (1981 Almanac)                              BLOEMF
+ 160  CONTINUE
+      NAME='Bloemfontein 1.52 metre'
+      W=EAST(26,24,18.)
+      P=SOUTH(29,02,18.)
+      H=1387D0
+      GO TO 9999
+
+*  Bosque Alegre 1.54m (1981 Almanac)                         BOSQALEGRE
+ 170  CONTINUE
+      NAME='Bosque Alegre 1.54 metre'
+      W=WEST(64,32,48.0)
+      P=SOUTH(31,35,53.)
+      H=1250D0
+      GO TO 9999
+
+*  USNO 61" astrographic reflector, Flagstaff (1981 Almanac)   FLAGSTF61
+ 180  CONTINUE
+      NAME='USNO 61 inch astrograph, Flagstaff'
+      W=WEST(111,44,23.6)
+      P=NORTH(35,11,02.5)
+      H=2316D0
+      GO TO 9999
+
+*  Lowell 72" (1981 Almanac)                                    LOWELL72
+ 190  CONTINUE
+      NAME='Perkins 72 inch, Lowell'
+      W=WEST(111,32,09.3)
+      P=NORTH(35,05,48.6)
+      H=2198D0
+      GO TO 9999
+
+*  Harvard 1.55m (1981 Almanac)                                  HARVARD
+ 200  CONTINUE
+      NAME='Harvard College Observatory 1.55m'
+      W=WEST(71,33,29.32)
+      P=NORTH(42,30,19.0)
+      H=185D0
+      GO TO 9999
+
+*  Okayama 1.88m (1981 Almanac)                                  OKAYAMA
+ 210  CONTINUE
+      NAME='Okayama 1.88 metre'
+      W=EAST(133,35,47.29)
+      P=NORTH(34,34,26.1)
+      H=372D0
+      GO TO 9999
+
+*  Kitt Peak Mayall 4m (1981 Almanac)                            KPNO158
+ 220  CONTINUE
+      NAME='Kitt Peak 158 inch'
+      W=WEST(111,35,57.61)
+      P=NORTH(31,57,50.3)
+      H=2120D0
+      GO TO 9999
+
+*  Kitt Peak 90 inch (1981 Almanac)                               KPNO90
+ 230  CONTINUE
+      NAME='Kitt Peak 90 inch'
+      W=WEST(111,35,58.24)
+      P=NORTH(31,57,46.9)
+      H=2071D0
+      GO TO 9999
+
+*  Kitt Peak 84 inch (1981 Almanac)                               KPNO84
+ 240  CONTINUE
+      NAME='Kitt Peak 84 inch'
+      W=WEST(111,35,51.56)
+      P=NORTH(31,57,29.2)
+      H=2096D0
+      GO TO 9999
+
+*  Kitt Peak 36 foot (1981 Almanac)                             KPNO36FT
+ 250  CONTINUE
+      NAME='Kitt Peak 36 foot'
+      W=WEST(111,36,51.12)
+      P=NORTH(31,57,12.1)
+      H=1939D0
+      GO TO 9999
+
+*  Kottamia 74" (1981 Almanac)                                  KOTTAMIA
+ 260  CONTINUE
+      NAME='Kottamia 74 inch'
+      W=EAST(31,49,30.)
+      P=NORTH(29,55,54.)
+      H=476D0
+      GO TO 9999
+
+*  La Silla 3.6m (1981 Almanac)                                   ESO3.6
+ 270  CONTINUE
+      NAME='ESO 3.6 metre'
+      W=WEST(70,43,36.)
+      P=SOUTH(29,15,36.)
+      H=2428D0
+      GO TO 9999
+
+*  Mauna Kea 88 inch                                            MAUNAK88
+*  (IfA website, Richard Wainscoat)
+ 280  CONTINUE
+      NAME='Mauna Kea 88 inch'
+      W=WEST(155,28,09.96)
+      P=NORTH(19,49,22.77)
+      H=4213.6D0
+      GO TO 9999
+
+*  UKIRT (IfA website, Richard Wainscoat)                          UKIRT
+ 290  CONTINUE
+      NAME='UK Infra Red Telescope'
+      W=WEST(155,28,13.18)
+      P=NORTH(19,49,20.75)
+      H=4198.5D0
+      GO TO 9999
+
+*  Quebec 1.6m (1981 Almanac)                                  QUEBEC1.6
+ 300  CONTINUE
+      NAME='Quebec 1.6 metre'
+      W=WEST(71,09,09.7)
+      P=NORTH(45,27,20.6)
+      H=1114D0
+      GO TO 9999
+
+*  Mt Ekar 1.82m (1981 Almanac)                                   MTEKAR
+ 310  CONTINUE
+      NAME='Mt Ekar 1.82 metre'
+      W=EAST(11,34,15.)
+      P=NORTH(45,50,48.)
+      H=1365D0
+      GO TO 9999
+
+*  Mt Lemmon 60" (1981 Almanac)                               MTLEMMON60
+ 320  CONTINUE
+      NAME='Mt Lemmon 60 inch'
+      W=WEST(110,42,16.9)
+      P=NORTH(32,26,33.9)
+      H=2790D0
+      GO TO 9999
+
+*  Mt Locke 2.7m (1981 Almanac)                               MCDONLD2.7
+ 330  CONTINUE
+      NAME='McDonald 2.7 metre'
+      W=WEST(104,01,17.60)
+      P=NORTH(30,40,17.7)
+      H=2075D0
+      GO TO 9999
+
+*  Mt Locke 2.1m (1981 Almanac)                               MCDONLD2.1
+ 340  CONTINUE
+      NAME='McDonald 2.1 metre'
+      W=WEST(104,01,20.10)
+      P=NORTH(30,40,17.7)
+      H=2075D0
+      GO TO 9999
+
+*  Palomar 200" (1981 Almanac)                                PALOMAR200
+ 350  CONTINUE
+      NAME='Palomar 200 inch'
+      W=WEST(116,51,50.)
+      P=NORTH(33,21,22.)
+      H=1706D0
+      GO TO 9999
+
+*  Palomar 60" (1981 Almanac)                                  PALOMAR60
+ 360  CONTINUE
+      NAME='Palomar 60 inch'
+      W=WEST(116,51,31.)
+      P=NORTH(33,20,56.)
+      H=1706D0
+      GO TO 9999
+
+*  David Dunlap 74" (1981 Almanac)                              DUNLAP74
+ 370  CONTINUE
+      NAME='David Dunlap 74 inch'
+      W=WEST(79,25,20.)
+      P=NORTH(43,51,46.)
+      H=244D0
+      GO TO 9999
+
+*  Haute Provence 1.93m (1981 Almanac)                         HPROV1.93
+ 380  CONTINUE
+      NAME='Haute Provence 1.93 metre'
+      W=EAST(5,42,46.75)
+      P=NORTH(43,55,53.3)
+      H=665D0
+      GO TO 9999
+
+*  Haute Provence 1.52m (1981 Almanac)                         HPROV1.52
+ 390  CONTINUE
+      NAME='Haute Provence 1.52 metre'
+      W=EAST(5,42,43.82)
+      P=NORTH(43,56,00.2)
+      H=667D0
+      GO TO 9999
+
+*  San Pedro Martir 83" (1981 Almanac)                           SANPM83
+ 400  CONTINUE
+      NAME='San Pedro Martir 83 inch'
+      W=WEST(115,27,47.)
+      P=NORTH(31,02,38.)
+      H=2830D0
+      GO TO 9999
+
+*  Sutherland 74" (1981 Almanac)                                  SAAO74
+ 410  CONTINUE
+      NAME='Sutherland 74 inch'
+      W=EAST(20,48,44.3)
+      P=SOUTH(32,22,43.4)
+      H=1771D0
+      GO TO 9999
+
+*  Tautenburg 2m (1981 Almanac)                                  TAUTNBG
+ 420  CONTINUE
+      NAME='Tautenburg 2 metre'
+      W=EAST(11,42,45.)
+      P=NORTH(50,58,51.)
+      H=331D0
+      GO TO 9999
+
+*  Catalina 61" (1981 Almanac)                                CATALINA61
+ 430  CONTINUE
+      NAME='Catalina 61 inch'
+      W=WEST(110,43,55.1)
+      P=NORTH(32,25,00.7)
+      H=2510D0
+      GO TO 9999
+
+*  Steward 90" (1981 Almanac)                                  STEWARD90
+ 440  CONTINUE
+      NAME='Steward 90 inch'
+      W=WEST(111,35,58.24)
+      P=NORTH(31,57,46.9)
+      H=2071D0
+      GO TO 9999
+
+*  Russian 6m (1981 Almanac)                                       USSR6
+ 450  CONTINUE
+      NAME='USSR 6 metre'
+      W=EAST(41,26,30.0)
+      P=NORTH(43,39,12.)
+      H=2100D0
+      GO TO 9999
+
+*  Arecibo 1000' (1981 Almanac)                                  ARECIBO
+ 460  CONTINUE
+      NAME='Arecibo 1000 foot'
+      W=WEST(66,45,11.1)
+      P=NORTH(18,20,36.6)
+      H=496D0
+      GO TO 9999
+
+*  Cambridge 5km (1981 Almanac)                                  CAMB5KM
+ 470  CONTINUE
+      NAME='Cambridge 5km'
+      W=EAST(0,02,37.23)
+      P=NORTH(52,10,12.2)
+      H=17D0
+      GO TO 9999
+
+*  Cambridge 1 mile (1981 Almanac)                             CAMB1MILE
+ 480  CONTINUE
+      NAME='Cambridge 1 mile'
+      W=EAST(0,02,21.64)
+      P=NORTH(52,09,47.3)
+      H=17D0
+      GO TO 9999
+
+*  Bonn 100m (1981 Almanac)                                   EFFELSBERG
+ 490  CONTINUE
+      NAME='Effelsberg 100 metre'
+      W=EAST(6,53,01.5)
+      P=NORTH(50,31,28.6)
+      H=366D0
+      GO TO 9999
+
+*  Greenbank 300' (1981 Almanac)                        GBVA300 (R.I.P.)
+ 500  CONTINUE
+      NAME='Greenbank 300 foot'
+      W=WEST(79,50,56.36)
+      P=NORTH(38,25,46.3)
+      H=894D0
+      GO TO 9999
+
+*  Jodrell Bank Mk 1 (1981 Almanac)                             JODRELL1
+ 510  CONTINUE
+      NAME='Jodrell Bank 250 foot'
+      W=WEST(2,18,25.)
+      P=NORTH(53,14,10.5)
+      H=78D0
+      GO TO 9999
+
+*  Australia Telescope Parkes Observatory                         PARKES
+*  (Peter te Lintel Hekkert, private comm)
+ 520  CONTINUE
+      NAME='Parkes 64 metre'
+      W=EAST(148,15,44.3591)
+      P=SOUTH(32,59,59.8657)
+      H=391.79D0
+      GO TO 9999
+
+*  VLA (1981 Almanac)                                                VLA
+ 530  CONTINUE
+      NAME='Very Large Array'
+      W=WEST(107,37,03.82)
+      P=NORTH(34,04,43.5)
+      H=2124D0
+      GO TO 9999
+
+*  Sugar Grove 150' (1981 Almanac)                            SUGARGROVE
+ 540  CONTINUE
+      NAME='Sugar Grove 150 foot'
+      W=WEST(79,16,23.)
+      P=NORTH(38,31,14.)
+      H=705D0
+      GO TO 9999
+
+*  Russian 600' (1981 Almanac)                                   USSR600
+ 550  CONTINUE
+      NAME='USSR 600 foot'
+      W=EAST(41,35,25.5)
+      P=NORTH(43,49,32.)
+      H=973D0
+      GO TO 9999
+
+*  Nobeyama 45 metre mm dish (based on 1981 Almanac entry)      NOBEYAMA
+ 560  CONTINUE
+      NAME='Nobeyama 45 metre'
+      W=EAST(138,29,12.)
+      P=NORTH(35,56,19.)
+      H=1350D0
+      GO TO 9999
+
+*  James Clerk Maxwell 15 metre mm telescope, Mauna Kea             JCMT
+*  (IfA website, Richard Wainscoat, height from I.Coulson)
+ 570  CONTINUE
+      NAME='JCMT 15 metre'
+      W=WEST(155,28,37.20)
+      P=NORTH(19,49,22.11)
+      H=4111D0
+      GO TO 9999
+
+*  ESO 3.5 metre NTT, La Silla (K.Wirenstrand)                    ESONTT
+ 580  CONTINUE
+      NAME='ESO 3.5 metre NTT'
+      W=WEST(70,43,07.)
+      P=SOUTH(29,15,30.)
+      H=2377D0
+      GO TO 9999
+
+*  St Andrews University Observatory (1982 Almanac)           ST.ANDREWS
+ 590  CONTINUE
+      NAME='St Andrews'
+      W=WEST(2,48,52.5)
+      P=NORTH(56,20,12.)
+      H=30D0
+      GO TO 9999
+
+*  Apache Point 3.5 metre (R.Owen)                                APO3.5
+ 600  CONTINUE
+      NAME='Apache Point 3.5m'
+      W=WEST(105,49,11.56)
+      P=NORTH(32,46,48.96)
+      H=2809D0
+      GO TO 9999
+
+*  W.M.Keck Observatory, Telescope 1                               KECK1
+*  (William Lupton, private comm)
+ 610  CONTINUE
+      NAME='Keck 10m Telescope #1'
+      W=WEST(155,28,28.99)
+      P=NORTH(19,49,33.41)
+      H=4160D0
+      GO TO 9999
+
+*  Tautenberg Schmidt (1983 Almanac)                            TAUTSCHM
+ 620  CONTINUE
+      NAME='Tautenberg 1.34 metre Schmidt'
+      W=EAST(11,42,45.0)
+      P=NORTH(50,58,51.0)
+      H=331D0
+      GO TO 9999
+
+*  Palomar Schmidt (1981 Almanac)                              PALOMAR48
+ 630  CONTINUE
+      NAME='Palomar 48-inch Schmidt'
+      W=WEST(116,51,32.0)
+      P=NORTH(33,21,26.0)
+      H=1706D0
+      GO TO 9999
+
+*  UK Schmidt, Siding Spring (1983 Almanac)                         UKST
+ 640  CONTINUE
+      NAME='UK 1.2 metre Schmidt, Siding Spring'
+      W=EAST(149,04,12.8)
+      P=SOUTH(31,16,27.8)
+      H=1145D0
+      GO TO 9999
+
+*  Kiso Schmidt, Japan (1981 Almanac)                               KISO
+ 650  CONTINUE
+      NAME='Kiso 1.05 metre Schmidt, Japan'
+      W=EAST(137,37,42.2)
+      P=NORTH(35,47,38.7)
+      H=1130D0
+      GO TO 9999
+
+*  ESO Schmidt, La Silla (1981 Almanac)                          ESOSCHM
+ 660  CONTINUE
+      NAME='ESO 1 metre Schmidt, La Silla'
+      W=WEST(70,43,46.5)
+      P=SOUTH(29,15,25.8)
+      H=2347D0
+      GO TO 9999
+
+*  Australia Telescope Compact Array                                ATCA
+*  (WGS84 coordinates of Station 35, Mark Calabretta, private comm)
+ 670  CONTINUE
+      NAME='Australia Telescope Compact Array'
+      W=EAST(149,33,00.500)
+      P=SOUTH(30,18,46.385)
+      H=236.9D0
+      GO TO 9999
+
+*  Australia Telescope Mopra Observatory                           MOPRA
+*  (Peter te Lintel Hekkert, private comm)
+ 680  CONTINUE
+      NAME='ATNF Mopra Observatory'
+      W=EAST(149,05,58.732)
+      P=SOUTH(31,16,04.451)
+      H=850D0
+      GO TO 9999
+
+*  Subaru telescope, Mauna Kea                                     SUBARU
+*  (IfA website, Richard Wainscoat)
+ 690  CONTINUE
+      NAME='Subaru 8m telescope'
+      W=WEST(155,28,33.67)
+      P=NORTH(19,49,31.81)
+      H=4163D0
+      GO TO 9999
+
+*  Canada-France-Hawaii Telescope, Mauna Kea                         CFHT
+*  (IfA website, Richard Wainscoat)
+ 700  CONTINUE
+      NAME='Canada-France-Hawaii 3.6m Telescope'
+      W=WEST(155,28,07.95)
+      P=NORTH(19,49,30.91)
+      H=4204.1D0
+      GO TO 9999
+
+*  W.M.Keck Observatory, Telescope 2                                KECK2
+*  (William Lupton, private comm)
+ 710  CONTINUE
+      NAME='Keck 10m Telescope #2'
+      W=WEST(155,28,27.24)
+      P=NORTH(19,49,35.62)
+      H=4159.6D0
+      GO TO 9999
+
+*  Gemini North, Mauna Kea                                        GEMININ
+*  (IfA website, Richard Wainscoat)
+ 720  CONTINUE
+      NAME='Gemini North 8-m telescope'
+      W=WEST(155,28,08.57)
+      P=NORTH(19,49,25.69)
+      H=4213.4D0
+      GO TO 9999
+
+*  Five College Radio Astronomy Observatory                        FCRAO
+*  (Tim Jenness, private comm)
+ 730  CONTINUE
+      NAME='Five College Radio Astronomy Obs'
+      W=WEST(72,20,42.0)
+      P=NORTH(42,23,30.0)
+      H=314D0
+      GO TO 9999
+
+*  NASA Infra Red Telescope Facility                                IRTF
+*  (IfA website, Richard Wainscoat)
+ 740  CONTINUE
+      NAME='NASA IR Telescope Facility, Mauna Kea'
+      W=WEST(155,28,19.20)
+      P=NORTH(19,49,34.39)
+      H=4168.1D0
+      GO TO 9999
+
+*  Caltech Submillimeter Observatory                                 CSO
+*  (IfA website, Richard Wainscoat; height estimated)
+ 750  CONTINUE
+      NAME='Caltech Sub-mm Observatory, Mauna Kea'
+      W=WEST(155,28,31.79)
+      P=NORTH(19,49,20.78)
+      H=4080D0
+      GO TO 9999
+
+*  Unrecognized station
+ 9000 CONTINUE
+      NAME='?'
+
+*  Exit
+ 9999 CONTINUE
+
+      END
diff --git a/src/slalib/pa.f b/src/slalib/pa.f
new file mode 100644
index 0000000..8c68296
--- /dev/null
+++ b/src/slalib/pa.f
@@ -0,0 +1,46 @@
+      DOUBLE PRECISION FUNCTION sla_PA (HA, DEC, PHI)
+*+
+*     - - -
+*      P A
+*     - - -
+*
+*  HA, Dec to Parallactic Angle (double precision)
+*
+*  Given:
+*     HA     d     hour angle in radians (geocentric apparent)
+*     DEC    d     declination in radians (geocentric apparent)
+*     PHI    d     observatory latitude in radians (geodetic)
+*
+*  The result is in the range -pi to +pi
+*
+*  Notes:
+*
+*  1)  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.
+*
+*  2)  At the pole a zero result is returned.
+*
+*  P.T.Wallace   Starlink   16 August 1994
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION HA,DEC,PHI
+
+      DOUBLE PRECISION CP,SQSZ,CQSZ
+
+
+
+      CP=COS(PHI)
+      SQSZ=CP*SIN(HA)
+      CQSZ=SIN(PHI)*COS(DEC)-CP*SIN(DEC)*COS(HA)
+      IF (SQSZ.EQ.0D0.AND.CQSZ.EQ.0D0) CQSZ=1D0
+      sla_PA=ATAN2(SQSZ,CQSZ)
+
+      END
diff --git a/src/slalib/pav.f b/src/slalib/pav.f
new file mode 100644
index 0000000..7eb1c12
--- /dev/null
+++ b/src/slalib/pav.f
@@ -0,0 +1,53 @@
+      REAL FUNCTION sla_PAV ( V1, V2 )
+*+
+*     - - - -
+*      P A V
+*     - - - -
+*
+*  Position angle of one celestial direction with respect to another.
+*
+*  (single precision)
+*
+*  Given:
+*     V1    r(3)    direction cosines of one point
+*     V2    r(3)    direction cosines of the other point
+*
+*  (The coordinate frames correspond to RA,Dec, Long,Lat etc.)
+*
+*  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.
+*
+*  V1 and V2 do not have to be unit vectors.
+*
+*  The routine sla_BEAR performs an equivalent function except
+*  that the points are specified in the form of spherical
+*  coordinates.
+*
+*  Called:  sla_DPAV
+*
+*  Patrick Wallace   Starlink   23 May 1997
+*
+*  Copyright (C) 1997 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL V1(3),V2(3)
+
+      INTEGER I
+      DOUBLE PRECISION D1(3),D2(3)
+
+      DOUBLE PRECISION sla_DPAV
+
+
+*  Call the double precision version
+      DO I=1,3
+         D1(I)=V1(I)
+         D2(I)=V2(I)
+      END DO
+      sla_PAV=sla_DPAV(D1,D2)
+
+      END
diff --git a/src/slalib/pc.bat b/src/slalib/pc.bat
new file mode 100755
index 0000000..d0f43b4
--- /dev/null
+++ b/src/slalib/pc.bat
@@ -0,0 +1,75 @@
+@echo off
+rem
+rem  - - - - - - -
+rem   P C . B A T
+rem  - - - - - - -
+rem
+rem  Create the SLALIB library, starting either from the release
+rem  version copied from the VAX or from the PC version produced
+rem  by a prior run of the present procedure.
+rem
+rem  Environment variable temp must point to a scratch directory.
+rem
+rem  !!! Non-reversible - it is not possible to recreate !!!
+rem  !!! the VAX version from the PC version             !!!
+rem
+rem  P.T.Wallace   Starlink   25 April 1996
+rem
+if exist *.pcm copy *.pcm *.for
+if exist *.pcm del *.pcm
+if exist *.c del *.c
+if exist *.obj del *.obj
+if exist *.exe del *.exe
+if exist *.olb del *.olb
+if exist *.vax del *.vax
+if exist *.ush del *.ush
+if exist *.cnv del *.cnv
+if exist *.mip del *.mip
+if exist *.sun del *.sun
+if exist *.ind del *.ind
+if exist *.com del *.com
+if exist *.new del *.new
+if exist *.obs del *.obs
+if exist *.toc del *.toc
+if exist *.dir del *.dir
+if exist sla_test.for del sla_test.for
+if exist makefile del makefile
+if exist mk del mk
+if exist sla_link del sla_link
+if exist a*.for fl/c /FPi a*.for
+if exist b*.for fl/c /FPi b*.for
+if exist c*.for fl/c /FPi c*.for
+if exist d*.for fl/c /FPi d*.for
+if exist e*.for fl/c /FPi e*.for
+if exist f*.for fl/c /FPi f*.for
+if exist g*.for fl/c /FPi g*.for
+if exist h*.for fl/c /FPi h*.for
+if exist i*.for fl/c /FPi i*.for
+if exist j*.for fl/c /FPi j*.for
+if exist k*.for fl/c /FPi k*.for
+if exist l*.for fl/c /FPi l*.for
+if exist m*.for fl/c /FPi m*.for
+if exist n*.for fl/c /FPi n*.for
+if exist o*.for fl/c /FPi o*.for
+if exist p*.for fl/c /FPi p*.for
+if exist q*.for fl/c /FPi q*.for
+if exist r*.for fl/c /FPi r*.for
+if exist s*.for fl/c /FPi s*.for
+if exist t*.for fl/c /FPi t*.for
+if exist u*.for fl/c /FPi u*.for
+if exist v*.for fl/c /FPi v*.for
+if exist w*.for fl/c /FPi w*.for
+if exist x*.for fl/c /FPi x*.for
+if exist y*.for fl/c /FPi y*.for
+if exist z*.for fl/c /FPi z*.for
+echo Building library SLALIB.LIB ...
+@echo slalib > %temp%\slalib.tmp
+@echo y >> %temp%\slalib.tmp
+for %%f in (*.obj) do echo +%%f& >> %temp%\slalib.tmp
+@echo ;. >> %temp%\slalib.tmp
+if exist slalib.lib del slalib.lib
+lib @%temp%\slalib.tmp
+del %temp%\slalib.tmp
+del *.obj
+echo ... done.
+echo:
diff --git a/src/slalib/pcd.f b/src/slalib/pcd.f
new file mode 100644
index 0000000..71241a7
--- /dev/null
+++ b/src/slalib/pcd.f
@@ -0,0 +1,59 @@
+      SUBROUTINE sla_PCD (DISCO,X,Y)
+*+
+*     - - - -
+*      P C D
+*     - - - -
+*
+*  Apply pincushion/barrel distortion to a tangent-plane [x,y].
+*
+*  Given:
+*     DISCO    d      pincushion/barrel distortion coefficient
+*     X,Y      d      tangent-plane coordinates
+*
+*  Returned:
+*     X,Y      d      distorted coordinates
+*
+*  Notes:
+*
+*  1)  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.
+*
+*  2)  For pincushion distortion, C is +ve;  for barrel distortion,
+*      C is -ve.
+*
+*  3)  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
+*
+*  4)  There is a companion routine, sla_UNPCD, which performs
+*      an approximately inverse operation.
+*
+*  P.T.Wallace   Starlink   31 December 1992
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DISCO,X,Y
+
+      DOUBLE PRECISION F
+
+
+
+      F=1D0+DISCO*(X*X+Y*Y)
+      X=X*F
+      Y=Y*F
+
+      END
diff --git a/src/slalib/pda2h.f b/src/slalib/pda2h.f
new file mode 100644
index 0000000..cd31acf
--- /dev/null
+++ b/src/slalib/pda2h.f
@@ -0,0 +1,100 @@
+      SUBROUTINE sla_PDA2H (P, D, A, H1, J1, H2, J2)
+*+
+*     - - - - - -
+*      P D A 2 H
+*     - - - - - -
+*
+*  Hour Angle corresponding to a given azimuth
+*
+*  (double precision)
+*
+*  Given:
+*     P       d        latitude
+*     D       d        declination
+*     A       d        azimuth
+*
+*  Returned:
+*     H1      d        hour angle:  first solution if any
+*     J1      i        flag: 0 = solution 1 is valid
+*     H2      d        hour angle:  second solution if any
+*     J2      i        flag: 0 = solution 2 is valid
+*
+*  Called:  sla_DRANGE
+*
+*  P.T.Wallace   Starlink   6 October 1994
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION P,D,A,H1
+      INTEGER J1
+      DOUBLE PRECISION H2
+      INTEGER J2
+
+      DOUBLE PRECISION DPI
+      PARAMETER (DPI=3.141592653589793238462643D0)
+      DOUBLE PRECISION D90
+      PARAMETER (D90=DPI/2D0)
+      DOUBLE PRECISION TINY
+      PARAMETER (TINY=1D-12)
+      DOUBLE PRECISION PN,AN,DN,SA,CA,SASP,QT,QB,HPT,T
+      DOUBLE PRECISION sla_DRANGE
+
+
+*  Preset status flags to OK
+      J1=0
+      J2=0
+
+*  Adjust latitude, azimuth, declination to avoid critical values
+      PN=sla_DRANGE(P)
+      IF (ABS(ABS(PN)-D90).LT.TINY) THEN
+         PN=PN-SIGN(TINY,PN)
+      ELSE IF (ABS(PN).LT.TINY) THEN
+         PN=TINY
+      END IF
+      AN=sla_DRANGE(A)
+      IF (ABS(ABS(AN)-DPI).LT.TINY) THEN
+         AN=AN-SIGN(TINY,AN)
+      ELSE IF (ABS(AN).LT.TINY) THEN
+         AN=TINY
+      END IF
+      DN=sla_DRANGE(D)
+      IF (ABS(ABS(DN)-ABS(P)).LT.TINY) THEN
+         DN=DN-SIGN(TINY,DN)
+      ELSE IF (ABS(ABS(DN)-D90).LT.TINY) THEN
+         DN=DN-SIGN(TINY,DN)
+      ELSE IF (ABS(DN).LT.TINY) THEN
+         DN=TINY
+      END IF
+
+*  Useful functions
+      SA=SIN(AN)
+      CA=COS(AN)
+      SASP=SA*SIN(PN)
+
+*  Quotient giving sin(h+t)
+      QT=SIN(DN)*SA*COS(PN)
+      QB=COS(DN)*SQRT(CA*CA+SASP*SASP)
+
+*  Any solutions?
+      IF (ABS(QT).LE.QB) THEN
+
+*     Yes: find h+t and t
+         HPT=ASIN(QT/QB)
+         T=ATAN2(SASP,-CA)
+
+*     The two solutions
+         H1=sla_DRANGE(HPT-T)
+         H2=sla_DRANGE(-HPT-(T+DPI))
+
+*     Reject unless h and A different signs
+         IF (H1*AN.GT.0D0) J1=-1
+         IF (H2*AN.GT.0D0) J2=-1
+      ELSE
+         J1=-1
+         J2=-1
+      END IF
+
+      END
diff --git a/src/slalib/pdq2h.f b/src/slalib/pdq2h.f
new file mode 100644
index 0000000..a12ba72
--- /dev/null
+++ b/src/slalib/pdq2h.f
@@ -0,0 +1,98 @@
+      SUBROUTINE sla_PDQ2H (P, D, Q, H1, J1, H2, J2)
+*+
+*     - - - - - -
+*      P D Q 2 H
+*     - - - - - -
+*
+*  Hour Angle corresponding to a given parallactic angle
+*
+*  (double precision)
+*
+*  Given:
+*     P       d        latitude
+*     D       d        declination
+*     Q       d        parallactic angle
+*
+*  Returned:
+*     H1      d        hour angle:  first solution if any
+*     J1      i        flag: 0 = solution 1 is valid
+*     H2      d        hour angle:  second solution if any
+*     J2      i        flag: 0 = solution 2 is valid
+*
+*  Called:  sla_DRANGE
+*
+*  P.T.Wallace   Starlink   6 October 1994
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION P,D,Q,H1
+      INTEGER J1
+      DOUBLE PRECISION H2
+      INTEGER J2
+
+      DOUBLE PRECISION DPI
+      PARAMETER (DPI=3.141592653589793238462643D0)
+      DOUBLE PRECISION D90
+      PARAMETER (D90=DPI/2D0)
+      DOUBLE PRECISION TINY
+      PARAMETER (TINY=1D-12)
+      DOUBLE PRECISION PN,QN,DN,SQ,CQ,SQSD,QT,QB,HPT,T
+      DOUBLE PRECISION sla_DRANGE
+
+
+*  Preset status flags to OK
+      J1=0
+      J2=0
+
+*  Adjust latitude, declination, parallactic angle to avoid critical values
+      PN=sla_DRANGE(P)
+      IF (ABS(ABS(PN)-D90).LT.TINY) THEN
+         PN=PN-SIGN(TINY,PN)
+      ELSE IF (ABS(PN).LT.TINY) THEN
+         PN=TINY
+      END IF
+      QN=sla_DRANGE(Q)
+      IF (ABS(ABS(QN)-DPI).LT.TINY) THEN
+         QN=QN-SIGN(TINY,QN)
+      ELSE IF (ABS(QN).LT.TINY) THEN
+         QN=TINY
+      END IF
+      DN=sla_DRANGE(D)
+      IF (ABS(ABS(D)-ABS(P)).LT.TINY) THEN
+         DN=DN-SIGN(TINY,DN)
+      ELSE IF (ABS(ABS(D)-D90).LT.TINY) THEN
+         DN=DN-SIGN(TINY,DN)
+      END IF
+
+*  Useful functions
+      SQ=SIN(QN)
+      CQ=COS(QN)
+      SQSD=SQ*SIN(DN)
+
+*  Quotient giving sin(h+t)
+      QT=SIN(PN)*SQ*COS(DN)
+      QB=COS(PN)*SQRT(CQ*CQ+SQSD*SQSD)
+
+*  Any solutions?
+      IF (ABS(QT).LE.QB) THEN
+
+*     Yes: find h+t and t
+         HPT=ASIN(QT/QB)
+         T=ATAN2(SQSD,CQ)
+
+*     The two solutions
+         H1=sla_DRANGE(HPT-T)
+         H2=sla_DRANGE(-HPT-(T+DPI))
+
+*     Reject if h and Q different signs
+         IF (H1*QN.LT.0D0) J1=-1
+         IF (H2*QN.LT.0D0) J2=-1
+      ELSE
+         J1=-1
+         J2=-1
+      END IF
+
+      END
diff --git a/src/slalib/permut.f b/src/slalib/permut.f
new file mode 100644
index 0000000..20b8a27
--- /dev/null
+++ b/src/slalib/permut.f
@@ -0,0 +1,141 @@
+      SUBROUTINE sla_PERMUT ( N, ISTATE, IORDER, J )
+*+
+*     - - - - - - -
+*      P E R M U T
+*     - - - - - - -
+*
+*  Generate the next permutation of a specified number of items.
+*
+*  Given:
+*     N         i      number of items:  there will be N! permutations
+*     ISTATE    i(N)   state, ISTATE(1)=-1 to initialize
+*
+*  Returned:
+*     ISTATE    i(N)   state, updated ready for next time
+*     IORDER    i(N)   next permutation of numbers 1,2,...,N
+*     J         i      status: -1 = illegal N (zero or less is illegal)
+*                               0 = OK
+*                              +1 = no more permutations available
+*
+*  Notes:
+*
+*  1) This routine returns, in the IORDER array, the integers 1 to N
+*     inclusive, in an order that depends on the current contents of
+*     the ISTATE array.  Before calling the routine for the first
+*     time, the caller must set the first element of the ISTATE array
+*     to -1 (any negative number will do) to cause the ISTATE array
+*     to be fully initialized.
+*
+*  2) The first permutation to be generated is:
+*
+*          IORDER(1)=N, IORDER(2)=N-1, ..., IORDER(N)=1
+*
+*     This is also the permutation returned for the "finished"
+*     (J=1) case.
+*
+*     The final permutation to be generated is:
+*
+*          IORDER(1)=1, IORDER(2)=2, ..., IORDER(N)=N
+*
+*  3) If the "finished" (J=1) status is ignored, the routine continues
+*     to deliver permutations, the pattern repeating every N! calls.
+*
+*  P.T.Wallace   Starlink   25 August 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER N,IORDER(N),ISTATE(N),J
+
+      INTEGER I,IP1,ISLOT,ISKIP
+
+
+*  -------------
+*  Preliminaries
+*  -------------
+
+*  Validate, and set status.
+      IF (N.LT.1) THEN
+         J = -1
+         GO TO 9999
+      ELSE
+         J = 0
+      END IF
+
+*  If just starting, initialize state array
+      IF (ISTATE(1).LT.0) THEN
+         ISTATE(1) = -1
+         DO I=2,N
+            ISTATE(I) = 0
+         END DO
+      END IF
+
+*  --------------------------
+*  Increment the state number
+*  --------------------------
+
+*  The state number, maintained in the ISTATE array, is a mixed-radix
+*  number with N! states.  The least significant digit, with a radix of
+*  1, is in ISTATE(1).  The next digit, in ISTATE(2), has a radix of 2,
+*  and so on.
+
+*  Increment the least-significant digit of the state number.
+      ISTATE(1) = ISTATE(1)+1
+
+*  Digit by digit starting with the least significant.
+      DO I=1,N
+
+*     Carry?
+         IF (ISTATE(I).GE.I) THEN
+
+*        Yes:  reset the current digit.
+            ISTATE(I) = 0
+
+*        Overflow?
+            IF (I.GE.N) THEN
+
+*           Yes:  there are no more permutations.
+               J = 1
+            ELSE
+
+*           No:  carry.
+               IP1 = I+1
+               ISTATE(IP1) = ISTATE(IP1)+1
+            END IF
+         END IF
+      END DO
+
+*  -------------------------------------------------------------------
+*  Translate the state number into the corresponding permutation order
+*  -------------------------------------------------------------------
+
+*  Initialize the order array.  All but one element will be overwritten.
+      DO I=1,N
+         IORDER(I) = 1
+      END DO
+
+*  Look at each state number digit, starting with the most significant.
+      DO I=N,2,-1
+
+*     Initialize the position where the new number will go.
+         ISLOT = 0
+
+*     The state number digit says which unfilled slot is to be used.
+         DO ISKIP=0,ISTATE(I)
+
+*        Increment the slot number until an unused slot is found.
+            ISLOT = ISLOT+1
+            DO WHILE (IORDER(ISLOT).GT.1)
+               ISLOT = ISLOT+1
+            END DO
+         END DO
+
+*     Store the number in the permutation order array.
+         IORDER(ISLOT) = I
+      END DO
+
+ 9999 CONTINUE
+
+      END
diff --git a/src/slalib/pertel.f b/src/slalib/pertel.f
new file mode 100644
index 0000000..45537b4
--- /dev/null
+++ b/src/slalib/pertel.f
@@ -0,0 +1,159 @@
+      SUBROUTINE sla_PERTEL (JFORM, DATE0, DATE1,
+     :                 EPOCH0, ORBI0, ANODE0, PERIH0, AORQ0, E0, AM0,
+     :                 EPOCH1, ORBI1, ANODE1, PERIH1, AORQ1, E1, AM1,
+     :                       JSTAT)
+*+
+*     - - - - - - -
+*      P E R T E L
+*     - - - - - - -
+*
+*  Update the osculating orbital elements of an asteroid or comet by
+*  applying planetary perturbations.
+*
+*  Given (format and dates):
+*     JFORM   i    choice of element set (2 or 3; Note 1)
+*     DATE0   d    date of osculation (TT MJD) for the given elements
+*     DATE1   d    date of osculation (TT MJD) for the updated elements
+*
+*  Given (the unperturbed elements):
+*     EPOCH0  d    epoch (TT MJD) of the given element set (Note 2)
+*     ORBI0   d    inclination (radians)
+*     ANODE0  d    longitude of the ascending node (radians)
+*     PERIH0  d    argument of perihelion (radians)
+*     AORQ0   d    mean distance or perihelion distance (AU)
+*     E0      d    eccentricity
+*     AM0     d    mean anomaly (radians, JFORM=2 only)
+*
+*  Returned (the updated elements):
+*     EPOCH1  d    epoch (TT MJD) of the updated element set (Note 2)
+*     ORBI1   d    inclination (radians)
+*     ANODE1  d    longitude of the ascending node (radians)
+*     PERIH1  d    argument of perihelion (radians)
+*     AORQ1   d    mean distance or perihelion distance (AU)
+*     E1      d    eccentricity
+*     AM1     d    mean anomaly (radians, JFORM=2 only)
+*
+*  Returned (status flag):
+*     JSTAT   i    status: +102 = warning, distant epoch
+*                          +101 = warning, large timespan ( > 100 years)
+*                      +1 to +8 = coincident with major planet (Note 6)
+*                             0 = OK
+*                            -1 = illegal JFORM
+*                            -2 = illegal E0
+*                            -3 = illegal AORQ0
+*                            -4 = internal error
+*                            -5 = numerical error
+*
+*  Notes:
+*
+*  1  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
+*
+*  2  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.
+*
+*  3  The elements are with respect to the J2000 ecliptic and equinox.
+*
+*  4  Unused elements (AM0 and AM1 for JFORM=3) are not accessed.
+*
+*  5  See the sla_PERTUE routine for details of the algorithm used.
+*
+*  6  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 (Mercury=1,...,Neptune=8) as a warning.
+*
+*  Reference:
+*
+*     Sterne, Theodore E., "An Introduction to Celestial Mechanics",
+*     Interscience Publishers Inc., 1960.  Section 6.7, p199.
+*
+*  Called:  sla_EL2UE, sla_PERTUE, sla_UE2EL
+*
+*  P.T.Wallace   Starlink   14 March 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+      INTEGER JFORM
+      DOUBLE PRECISION DATE0,DATE1,
+     :                 EPOCH0,ORBI0,ANODE0,PERIH0,AORQ0,E0,AM0,
+     :                 EPOCH1,ORBI1,ANODE1,PERIH1,AORQ1,E1,AM1
+      INTEGER JSTAT
+
+      DOUBLE PRECISION U(13),DM
+      INTEGER J,JF
+
+
+
+*  Check that the elements are either minor-planet or comet format.
+      IF (JFORM.LT.2.OR.JFORM.GT.3) THEN
+         JSTAT = -1
+         GO TO 9999
+      END IF
+
+*  Transform the elements from conventional to universal form.
+      CALL sla_EL2UE(DATE0,JFORM,EPOCH0,ORBI0,ANODE0,PERIH0,
+     :               AORQ0,E0,AM0,0D0,U,J)
+      IF (J.NE.0) THEN
+         JSTAT = J
+         GO TO 9999
+      END IF
+
+*  Update the universal elements.
+      CALL sla_PERTUE(DATE1,U,J)
+      IF (J.GT.0) THEN
+         JSTAT = J
+      ELSE IF (J.LT.0) THEN
+         JSTAT = -5
+         GO TO 9999
+      END IF
+
+*  Transform from universal to conventional elements.
+      CALL sla_UE2EL(U,2,
+     :               JF, EPOCH1, ORBI1, ANODE1, PERIH1,
+     :               AORQ1, E1, AM1, DM, J)
+      IF (JF.NE.JFORM.OR.J.NE.0) JSTAT=-5
+
+ 9999 CONTINUE
+      END
diff --git a/src/slalib/pertue.f b/src/slalib/pertue.f
new file mode 100644
index 0000000..d6f6f53
--- /dev/null
+++ b/src/slalib/pertue.f
@@ -0,0 +1,535 @@
+      SUBROUTINE sla_PERTUE (DATE, U, JSTAT)
+*+
+*     - - - - - - -
+*      P E R T U E
+*     - - - - - - -
+*
+*  Update the universal elements of an asteroid or comet by applying
+*  planetary perturbations.
+*
+*  Given:
+*     DATE     d       final epoch (TT MJD) for the updated elements
+*
+*  Given and returned:
+*     U        d(13)   universal elements (updated in place)
+*
+*                (1)   combined mass (M+m)
+*                (2)   total energy of the orbit (alpha)
+*                (3)   reference (osculating) epoch (t0)
+*              (4-6)   position at reference epoch (r0)
+*              (7-9)   velocity at reference epoch (v0)
+*               (10)   heliocentric distance at reference epoch
+*               (11)   r0.v0
+*               (12)   date (t)
+*               (13)   universal eccentric anomaly (psi) of date, approx
+*
+*  Returned:
+*     JSTAT    i       status:
+*                          +102 = warning, distant epoch
+*                          +101 = warning, large timespan ( > 100 years)
+*                      +1 to +8 = coincident with major planet (Note 5)
+*                             0 = OK
+*                            -1 = numerical error
+*
+*  Called:  sla_PLANET, sla_UE2PV, sla_PV2UE
+*
+*  Notes:
+*
+*  1  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.
+*
+*  2  The universal elements are with respect to the J2000 equator and
+*     equinox.
+*
+*  3  The epochs DATE, U(3) and U(12) are all Modified Julian Dates
+*     (JD-2400000.5).
+*
+*  4  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 sla_PLANET.  Two
+*     levels of interpolation are used, to enhance speed without
+*     significantly degrading accuracy.  At a low frequency, the routine
+*     sla_PLANET 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, relativistic effects
+*     are not taken into account and the Earth-Moon system is treated as
+*     a single body.
+*
+*     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.
+*
+*  5  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 (Mercury=1,...,Neptune=8) as a
+*     warning.
+*
+*  References:
+*
+*     1  Sterne, Theodore E., "An Introduction to Celestial Mechanics",
+*        Interscience Publishers Inc., 1960.  Section 6.7, p199.
+*
+*     2  Everhart, E. & Pitkin, E.T., Am.J.Phys. 51, 712, 1983.
+*
+*  P.T.Wallace   Starlink   18 March 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+      DOUBLE PRECISION DATE,U(13)
+      INTEGER JSTAT
+
+*  Coefficient relating timestep to perturbing force
+      DOUBLE PRECISION TSC
+      PARAMETER (TSC=1D-4)
+
+*  Minimum and maximum timestep (days)
+      DOUBLE PRECISION TSMIN,TSMAX
+      PARAMETER (TSMIN=0.01D0,TSMAX=10D0)
+
+*  Age limit for major-planet state vector (days)
+      DOUBLE PRECISION AGEPMO
+      PARAMETER (AGEPMO=5D0)
+
+*  Age limit for major-planet mean elements (days)
+      DOUBLE PRECISION AGEPEL
+      PARAMETER (AGEPEL=50D0)
+
+*  Margin for error when deciding whether to renew the planetary data
+      DOUBLE PRECISION TINY
+      PARAMETER (TINY=1D-6)
+
+*  Age limit for the body's osculating elements (before rectification)
+      DOUBLE PRECISION AGEBEL
+      PARAMETER (AGEBEL=100D0)
+
+*  Gaussian gravitational constant (exact) and square
+      DOUBLE PRECISION GCON,GCON2
+      PARAMETER (GCON=0.01720209895D0,GCON2=GCON*GCON)
+
+*  The final epoch
+      DOUBLE PRECISION TFINAL
+
+*  The body's current universal elements
+      DOUBLE PRECISION UL(13)
+
+*  Current reference epoch
+      DOUBLE PRECISION T0
+
+*  Timespan from latest orbit rectification to final epoch (days)
+      DOUBLE PRECISION TSPAN
+
+*  Time left to go before integration is complete
+      DOUBLE PRECISION TLEFT
+
+*  Time direction flag: +1=forwards, -1=backwards
+      DOUBLE PRECISION FB
+
+*  First-time flag
+      LOGICAL FIRST
+
+*
+*  The current perturbations
+*
+*  Epoch (days relative to current reference epoch)
+      DOUBLE PRECISION RTN
+*  Position (AU)
+      DOUBLE PRECISION PERP(3)
+*  Velocity (AU/d)
+      DOUBLE PRECISION PERV(3)
+*  Acceleration (AU/d/d)
+      DOUBLE PRECISION PERA(3)
+*
+
+*  Length of current timestep (days), and half that
+      DOUBLE PRECISION TS,HTS
+
+*  Epoch of middle of timestep
+      DOUBLE PRECISION T
+
+*  Epoch of planetary mean elements
+      DOUBLE PRECISION TPEL
+
+*  Planet number (1=Mercury, 2=Venus, 3=EMB...8=Neptune)
+      INTEGER NP
+
+*  Planetary universal orbital elements
+      DOUBLE PRECISION UP(13,8)
+
+*  Epoch of planetary state vectors
+      DOUBLE PRECISION TPMO
+
+*  State vectors for the major planets (AU,AU/s)
+      DOUBLE PRECISION PVIN(6,8)
+
+*
+*  Correction terms for extrapolated major planet vectors
+*
+*  Sun-to-planet distances squared multiplied by 3
+      DOUBLE PRECISION R2X3(8)
+*  Sunward acceleration terms, G/2R^3
+      DOUBLE PRECISION GC(8)
+*  Tangential-to-circular correction factor
+      DOUBLE PRECISION FC
+*  Radial correction factor due to Sunwards acceleration
+      DOUBLE PRECISION FG
+*
+
+*  The body's unperturbed and perturbed state vectors (AU,AU/s)
+      DOUBLE PRECISION PV0(6),PV(6)
+
+*  The body's perturbed and unperturbed heliocentric distances (AU) cubed
+      DOUBLE PRECISION R03,R3
+
+*  The perturbating accelerations, indirect and direct
+      DOUBLE PRECISION FI(3),FD(3)
+
+*  Sun-to-planet vector, and distance cubed
+      DOUBLE PRECISION RHO(3),RHO3
+
+*  Body-to-planet vector, and distance cubed
+      DOUBLE PRECISION DELTA(3),DELTA3
+
+*  Miscellaneous
+      INTEGER I,J
+      DOUBLE PRECISION R2,W,DT,DT2,FT
+
+*  Planetary inverse masses, Mercury through Neptune
+      DOUBLE PRECISION AMAS(8)
+      DATA AMAS / 6023600D0,408523.5D0,328900.5D0,3098710D0,
+     :            1047.355D0,3498.5D0,22869D0,19314D0 /
+
+*---------------------------------------------------------------------*
+
+
+*  Preset the status to OK.
+      JSTAT = 0
+
+*  Copy the final epoch.
+      TFINAL = DATE
+
+*  Copy the elements (which will be periodically updated).
+      DO I=1,13
+         UL(I) = U(I)
+      END DO
+
+*  Initialize the working reference epoch.
+      T0=UL(3)
+
+*  Total timespan (days) and hence time left.
+      TSPAN = TFINAL-T0
+      TLEFT = TSPAN
+
+*  Warn if excessive.
+      IF (ABS(TSPAN).GT.36525D0) JSTAT=101
+
+*  Time direction: +1 for forwards, -1 for backwards.
+      FB = SIGN(1D0,TSPAN)
+
+*  Initialize relative epoch for start of current timestep.
+      RTN = 0D0
+
+*  Reset the perturbations (position, velocity, acceleration).
+      DO I=1,3
+         PERP(I) = 0D0
+         PERV(I) = 0D0
+         PERA(I) = 0D0
+      END DO
+
+*  Set "first iteration" flag.
+      FIRST = .TRUE.
+
+*  Step through the time left.
+      DO WHILE (FB*TLEFT.GT.0D0)
+
+*     Magnitude of current acceleration due to planetary attractions.
+         IF (FIRST) THEN
+            TS = TSMIN
+         ELSE
+            R2 = 0D0
+            DO I=1,3
+               W = FD(I)
+               R2 = R2+W*W
+            END DO
+            W = SQRT(R2)
+
+*        Use the acceleration to decide how big a timestep can be tolerated.
+            IF (W.NE.0D0) THEN
+               TS = MIN(TSMAX,MAX(TSMIN,TSC/W))
+            ELSE
+               TS = TSMAX
+            END IF
+         END IF
+         TS = TS*FB
+
+*     Override if final epoch is imminent.
+         TLEFT = TSPAN-RTN
+         IF (ABS(TS).GT.ABS(TLEFT)) TS=TLEFT
+
+*     Epoch of middle of timestep.
+         HTS = TS/2D0
+         T = T0+RTN+HTS
+
+*     Is it time to recompute the major-planet elements?
+         IF (FIRST.OR.ABS(T-TPEL)-AGEPEL.GE.TINY) THEN
+
+*        Yes: go forward in time by just under the maximum allowed.
+            TPEL = T+FB*AGEPEL
+
+*        Compute the state vector for the new epoch.
+            DO NP=1,8
+               CALL sla_PLANET(TPEL,NP,PV,J)
+
+*           Warning if remote epoch, abort if error.
+               IF (J.EQ.1) THEN
+                  JSTAT = 102
+               ELSE IF (J.NE.0) THEN
+                  GO TO 9010
+               END IF
+
+*           Transform the vector into universal elements.
+               CALL sla_PV2UE(PV,TPEL,0D0,UP(1,NP),J)
+               IF (J.NE.0) GO TO 9010
+            END DO
+         END IF
+
+*     Is it time to recompute the major-planet motions?
+         IF (FIRST.OR.ABS(T-TPMO)-AGEPMO.GE.TINY) THEN
+
+*        Yes: look ahead.
+            TPMO = T+FB*AGEPMO
+
+*        Compute the motions of each planet (AU,AU/d).
+            DO NP=1,8
+
+*           The planet's position and velocity (AU,AU/s).
+               CALL sla_UE2PV(TPMO,UP(1,NP),PVIN(1,NP),J)
+               IF (J.NE.0) GO TO 9010
+
+*           Scale velocity to AU/d.
+               DO J=4,6
+                  PVIN(J,NP) = PVIN(J,NP)*86400D0
+               END DO
+
+*           Precompute also the extrapolation correction terms.
+               R2 = 0D0
+               DO I=1,3
+                  W = PVIN(I,NP)
+                  R2 = R2+W*W
+               END DO
+               R2X3(NP) = R2*3D0
+               GC(NP) = GCON2/(2D0*R2*SQRT(R2))
+            END DO
+         END IF
+
+*     Reset the first-time flag.
+         FIRST = .FALSE.
+
+*     Unperturbed motion of the body at middle of timestep (AU,AU/s).
+         CALL sla_UE2PV(T,UL,PV0,J)
+         IF (J.NE.0) GO TO 9010
+
+*     Perturbed position of the body (AU) and heliocentric distance cubed.
+         R2 = 0D0
+         DO I=1,3
+            W = PV0(I)+PERP(I)+(PERV(I)+PERA(I)*HTS/2D0)*HTS
+            PV(I) = W
+            R2 = R2+W*W
+         END DO
+         R3 = R2*SQRT(R2)
+
+*     The body's unperturbed heliocentric distance cubed.
+         R2 = 0D0
+         DO I=1,3
+            W = PV0(I)
+            R2 = R2+W*W
+         END DO
+         R03 = R2*SQRT(R2)
+
+*     Compute indirect and initialize direct parts of the perturbation.
+         DO I=1,3
+            FI(I) = PV0(I)/R03-PV(I)/R3
+            FD(I) = 0D0
+         END DO
+
+*     Ready to compute the direct planetary effects.
+
+*     Interval from state-vector epoch to middle of current timestep.
+         DT = T-TPMO
+         DT2 = DT*DT
+
+*     Planet by planet.
+         DO NP=1,8
+
+*        First compute the extrapolation in longitude (squared).
+            R2 = 0D0
+            DO J=4,6
+               W = PVIN(J,NP)*DT
+               R2 = R2+W*W
+            END DO
+
+*        Hence the tangential-to-circular correction factor.
+            FC = 1D0+R2/R2X3(NP)
+
+*        The radial correction factor due to the inwards acceleration.
+            FG = 1D0-GC(NP)*DT2
+
+*        Planet's position, and heliocentric distance cubed.
+            R2 = 0D0
+            DO I=1,3
+               W = FG*(PVIN(I,NP)+FC*PVIN(I+3,NP)*DT)
+               RHO(I) = W
+               R2 = R2+W*W
+            END DO
+            RHO3 = R2*SQRT(R2)
+
+*        Body-to-planet vector, light-time, and distance cubed.
+            R2 = 0D0
+            DO I=1,3
+               W = RHO(I)-PV(I)
+               DELTA(I) = W
+               R2 = R2+W*W
+            END DO
+            W = SQRT(R2)
+            DELTA3 = R2*SQRT(R2)
+
+*        If too close, ignore this planet and set a warning.
+            IF (R2.LT.1D-6) THEN
+               JSTAT = NP
+            ELSE
+
+*           Accumulate "direct" part of perturbation acceleration.
+               W = AMAS(NP)
+               DO I=1,3
+                  FD(I) = FD(I)+(DELTA(I)/DELTA3-RHO(I)/RHO3)/W
+               END DO
+            END IF
+         END DO
+
+*     Update the perturbations to the end of the timestep.
+         RTN = RTN+TS
+         DO I=1,3
+            W = (FI(I)+FD(I))*GCON2
+            FT = W*TS
+            PERP(I) = PERP(I)+(PERV(I)+FT/2D0)*TS
+            PERV(I) = PERV(I)+FT
+            PERA(I) = W
+         END DO
+
+*     Time still to go.
+         TLEFT = TSPAN-RTN
+
+*     Is it either time to rectify the orbit or the last time through?
+         IF (ABS(RTN).GE.AGEBEL.OR.FB*TLEFT.LE.0D0) THEN
+
+*        Yes: update to the end of the current timestep.
+            T0 = T0+RTN
+            RTN = 0D0
+
+*        The body's unperturbed motion (AU,AU/s).
+            CALL sla_UE2PV(T0,UL,PV0,J)
+            IF (J.NE.0) GO TO 9010
+
+*        Add and re-initialize the perturbations.
+            DO I=1,3
+               J = I+3
+               PV(I) = PV0(I)+PERP(I)
+               PV(J) = PV0(J)+PERV(I)/86400D0
+               PERP(I) = 0D0
+               PERV(I) = 0D0
+               PERA(I) = FD(I)*GCON2
+            END DO
+
+*        Use the position and velocity to set up new universal elements.
+            CALL sla_PV2UE(PV,T0,0D0,UL,J)
+            IF (J.NE.0) GO TO 9010
+
+*        Adjust the timespan and time left.
+            TSPAN = TFINAL-T0
+            TLEFT = TSPAN
+         END IF
+
+*     Next timestep.
+      END DO
+
+*  Return the updated universal-element set.
+      DO I=1,13
+         U(I) = UL(I)
+      END DO
+
+*  Finished.
+      GO TO 9999
+
+*  Miscellaneous numerical error.
+ 9010 CONTINUE
+      JSTAT = -1
+
+ 9999 CONTINUE
+      END
diff --git a/src/slalib/planel.f b/src/slalib/planel.f
new file mode 100644
index 0000000..064e51c
--- /dev/null
+++ b/src/slalib/planel.f
@@ -0,0 +1,117 @@
+      SUBROUTINE sla_PLANEL (DATE, JFORM, EPOCH, ORBINC, ANODE, PERIH,
+     :                       AORQ, E, AORL, DM, PV, JSTAT)
+*+
+*     - - - - - - -
+*      P L A N E L
+*     - - - - - - -
+*
+*  Heliocentric position and velocity of a planet, asteroid or comet,
+*  starting from orbital elements.
+*
+*  Given:
+*     DATE      d      date, Modified Julian Date (JD - 2400000.5)
+*     JFORM     i      choice of element set (1-3; Note 3)
+*     EPOCH     d      epoch of elements (TT MJD)
+*     ORBINC    d      inclination (radians)
+*     ANODE     d      longitude of the ascending node (radians)
+*     PERIH     d      longitude or argument of perihelion (radians)
+*     AORQ      d      mean distance or perihelion distance (AU)
+*     E         d      eccentricity
+*     AORL      d      mean anomaly or longitude (radians, JFORM=1,2 only)
+*     DM        d      daily motion (radians, JFORM=1 only)
+*
+*  Returned:
+*     PV        d(6)   heliocentric x,y,z,xdot,ydot,zdot of date,
+*                                       J2000 equatorial triad (AU,AU/s)
+*     JSTAT     i      status:  0 = OK
+*                              -1 = illegal JFORM
+*                              -2 = illegal E
+*                              -3 = illegal AORQ
+*                              -4 = illegal DM
+*                              -5 = numerical error
+*
+*  Called:  sla_EL2UE, sla_UE2PV
+*
+*  Notes
+*
+*  1  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).
+*
+*  2  The elements are with respect to the J2000 ecliptic and equinox.
+*
+*  3  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)
+*
+*  4  Unused elements (DM for JFORM=2, AORL and DM for JFORM=3) are
+*     not accessed.
+*
+*  5  The reference frame for the result is with respect to the mean
+*     equator and equinox of epoch J2000.
+*
+*  6  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.
+*
+*  P.T.Wallace   Starlink   18 March 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DATE
+      INTEGER JFORM
+      DOUBLE PRECISION EPOCH,ORBINC,ANODE,PERIH,AORQ,E,AORL,DM,PV(6)
+      INTEGER JSTAT
+
+      DOUBLE PRECISION U(13)
+      INTEGER J
+
+
+
+*  Validate elements and convert to "universal variables" parameters.
+      CALL sla_EL2UE(DATE,JFORM,
+     :               EPOCH,ORBINC,ANODE,PERIH,AORQ,E,AORL,DM,U,J)
+
+*  Determine the position and velocity.
+      IF (J.EQ.0) THEN
+         CALL sla_UE2PV(DATE,U,PV,J)
+         IF (J.NE.0) J=-5
+      END IF
+
+*  Wrap up.
+      JSTAT = J
+
+      END
diff --git a/src/slalib/planet.f b/src/slalib/planet.f
new file mode 100644
index 0000000..095dff7
--- /dev/null
+++ b/src/slalib/planet.f
@@ -0,0 +1,707 @@
+      SUBROUTINE sla_PLANET (DATE, NP, PV, JSTAT)
+*+
+*     - - - - - - -
+*      P L A N E T
+*     - - - - - - -
+*
+*  Approximate heliocentric position and velocity of a specified
+*  major planet.
+*
+*  Given:
+*     DATE      d      Modified Julian Date (JD - 2400000.5)
+*     NP        i      planet (1=Mercury, 2=Venus, 3=EMB ... 9=Pluto)
+*
+*  Returned:
+*     PV        d(6)   heliocentric x,y,z,xdot,ydot,zdot, J2000
+*                                           equatorial triad (AU,AU/s)
+*     JSTAT     i      status: +1 = warning: date out of range
+*                               0 = OK
+*                              -1 = illegal NP (outside 1-9)
+*                              -2 = solution didn't converge
+*
+*  Called:  sla_PLANEL
+*
+*  Notes
+*
+*  1  The epoch, DATE, is in the TDB timescale and is a Modified
+*     Julian Date (JD-2400000.5).
+*
+*  2  The reference frame is equatorial and is with respect to the
+*     mean equinox and ecliptic of epoch J2000.
+*
+*  3  If an NP value outside the range 1-9 is supplied, an error
+*     status (JSTAT = -1) is returned and the PV vector set to zeroes.
+*
+*  4  The algorithm for obtaining the mean elements of the planets
+*     from Mercury to Neptune is due to J.L. Simon, P. Bretagnon,
+*     J. Chapront, M. Chapront-Touze, G. Francou and J. Laskar
+*     (Bureau des Longitudes, Paris).  The (completely different)
+*     algorithm for calculating the ecliptic coordinates of Pluto
+*     is by Meeus.
+*
+*  5  Comparisons of the present routine with the JPL DE200 ephemeris
+*     give the following RMS errors over the interval 1960-2025:
+*
+*                      position (km)     speed (metre/sec)
+*
+*        Mercury            334               0.437
+*        Venus             1060               0.855
+*        EMB               2010               0.815
+*        Mars              7690               1.98
+*        Jupiter          71700               7.70
+*        Saturn          199000              19.4
+*        Uranus          564000              16.4
+*        Neptune         158000              14.4
+*        Pluto            36400               0.137
+*
+*     From comparisons with DE102, Simon et al quote the following
+*     longitude accuracies over the interval 1800-2200:
+*
+*        Mercury                 4"
+*        Venus                   5"
+*        EMB                     6"
+*        Mars                   17"
+*        Jupiter                71"
+*        Saturn                 81"
+*        Uranus                 86"
+*        Neptune                11"
+*
+*     In the case of Pluto, Meeus quotes an accuracy of 0.6 arcsec
+*     in longitude and 0.2 arcsec in latitude for the period
+*     1885-2099.
+*
+*     For all except Pluto, over the period 1000-3000 the accuracy
+*     is better than 1.5 times that over 1800-2200.  Outside the
+*     period 1000-3000 the accuracy declines.  For Pluto the
+*     accuracy declines rapidly outside the period 1885-2099.
+*     Outside these ranges (1885-2099 for Pluto, 1000-3000 for
+*     the rest) a "date out of range" warning status (JSTAT=+1)
+*     is returned.
+*
+*  6  The algorithms for (i) Mercury through Neptune and (ii) Pluto
+*     are completely independent.  In the Mercury through Neptune
+*     case, the present SLALIB implementation differs from the
+*     original Simon et al Fortran code in the following respects.
+*
+*     *  The date is supplied as a Modified Julian Date rather
+*        than a Julian Date (MJD = JD - 2400000.5).
+*
+*     *  The result is returned only in equatorial Cartesian form;
+*        the ecliptic longitude, latitude and radius vector are not
+*        returned.
+*
+*     *  The velocity is in AU per second, not AU per day.
+*
+*     *  Different error/warning status values are used.
+*
+*     *  Kepler's equation is not solved inline.
+*
+*     *  Polynomials in T are nested to minimize rounding errors.
+*
+*     *  Explicit double-precision constants are used to avoid
+*        mixed-mode expressions.
+*
+*     *  There are other, cosmetic, changes to comply with
+*        Starlink/SLALIB style guidelines.
+*
+*     None of the above changes affects the result significantly.
+*
+*  7  For NP=3 the result is for the Earth-Moon Barycentre.  To
+*     obtain the heliocentric position and velocity of the Earth,
+*     either use the SLALIB routine sla_EVP or call sla_DMOON and
+*     subtract 0.012150581 times the geocentric Moon vector from
+*     the EMB vector produced by the present routine.  (The Moon
+*     vector should be precessed to J2000 first, but this can
+*     be omitted for modern epochs without introducing significant
+*     inaccuracy.)
+*
+*  References:  Simon et al., Astron. Astrophys. 282, 663 (1994).
+*               Meeus, Astronomical Algorithms, Willmann-Bell (1991).
+*
+*  P.T.Wallace   Starlink   27 May 1997
+*
+*  Copyright (C) 1997 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DATE
+      INTEGER NP
+      DOUBLE PRECISION PV(6)
+      INTEGER JSTAT
+
+*  2Pi, deg to radians, arcsec to radians
+      DOUBLE PRECISION D2PI,D2R,AS2R
+      PARAMETER (D2PI=6.283185307179586476925286766559D0,
+     :           D2R=0.017453292519943295769236907684886D0,
+     :           AS2R=4.848136811095359935899141023579D-6)
+
+*  Gaussian gravitational constant (exact)
+      DOUBLE PRECISION GCON
+      PARAMETER (GCON=0.01720209895D0)
+
+*  Seconds per Julian century
+      DOUBLE PRECISION SPC
+      PARAMETER (SPC=36525D0*86400D0)
+
+*  Sin and cos of J2000 mean obliquity (IAU 1976)
+      DOUBLE PRECISION SE,CE
+      PARAMETER (SE=0.3977771559319137D0,
+     :           CE=0.9174820620691818D0)
+
+      INTEGER I,J,IJSP(3,43)
+      DOUBLE PRECISION AMAS(8),A(3,8),DLM(3,8),E(3,8),
+     :                 PI(3,8),DINC(3,8),OMEGA(3,8),
+     :                 DKP(9,8),CA(9,8),SA(9,8),
+     :                 DKQ(10,8),CLO(10,8),SLO(10,8),
+     :                 T,DA,DE,DPE,DI,DO,DMU,ARGA,ARGL,DM,
+     :                 AB(2,3,43),DJ0,DS0,DP0,DL0,DLD0,DB0,DR0,
+     :                 DJ,DS,DP,DJD,DSD,DPD,WLBR(3),WLBRD(3),
+     :                 WJ,WS,WP,AL,ALD,SAL,CAL,
+     :                 AC,BC,DL,DLD,DB,DBD,DR,DRD,
+     :                 SL,CL,SB,CB,SLCB,CLCB,X,Y,Z,XD,YD,ZD
+
+*  -----------------------
+*  Mercury through Neptune
+*  -----------------------
+
+*  Planetary inverse masses
+      DATA AMAS / 6023600D0,408523.5D0,328900.5D0,3098710D0,
+     :            1047.355D0,3498.5D0,22869D0,19314D0 /
+
+*
+*  Tables giving the mean Keplerian elements, limited to T**2 terms:
+*
+*         A       semi-major axis (AU)
+*         DLM     mean longitude (degree and arcsecond)
+*         E       eccentricity
+*         PI      longitude of the perihelion (degree and arcsecond)
+*         DINC    inclination (degree and arcsecond)
+*         OMEGA   longitude of the ascending node (degree and arcsecond)
+*
+      DATA A /
+     :  0.3870983098D0,             0D0,      0D0,
+     :  0.7233298200D0,             0D0,      0D0,
+     :  1.0000010178D0,             0D0,      0D0,
+     :  1.5236793419D0,           3D-10,      0D0,
+     :  5.2026032092D0,       19132D-10,  -39D-10,
+     :  9.5549091915D0, -0.0000213896D0,  444D-10,
+     : 19.2184460618D0,       -3716D-10,  979D-10,
+     : 30.1103868694D0,      -16635D-10,  686D-10 /
+*
+      DATA DLM /
+     : 252.25090552D0, 5381016286.88982D0,  -1.92789D0,
+     : 181.97980085D0, 2106641364.33548D0,   0.59381D0,
+     : 100.46645683D0, 1295977422.83429D0,  -2.04411D0,
+     : 355.43299958D0,  689050774.93988D0,   0.94264D0,
+     :  34.35151874D0,  109256603.77991D0, -30.60378D0,
+     :  50.07744430D0,   43996098.55732D0,  75.61614D0,
+     : 314.05500511D0,   15424811.93933D0,  -1.75083D0,
+     : 304.34866548D0,    7865503.20744D0,   0.21103D0/
+*
+      DATA E /
+     : 0.2056317526D0,  0.0002040653D0,      -28349D-10,
+     : 0.0067719164D0, -0.0004776521D0,       98127D-10,
+     : 0.0167086342D0, -0.0004203654D0, -0.0000126734D0,
+     : 0.0934006477D0,  0.0009048438D0,      -80641D-10,
+     : 0.0484979255D0,  0.0016322542D0, -0.0000471366D0,
+     : 0.0555481426D0, -0.0034664062D0, -0.0000643639D0,
+     : 0.0463812221D0, -0.0002729293D0,  0.0000078913D0,
+     : 0.0094557470D0,  0.0000603263D0,            0D0 /
+*
+      DATA PI /
+     :  77.45611904D0,  5719.11590D0,   -4.83016D0,
+     : 131.56370300D0,   175.48640D0, -498.48184D0,
+     : 102.93734808D0, 11612.35290D0,   53.27577D0,
+     : 336.06023395D0, 15980.45908D0,  -62.32800D0,
+     :  14.33120687D0,  7758.75163D0,  259.95938D0,
+     :  93.05723748D0, 20395.49439D0,  190.25952D0,
+     : 173.00529106D0,  3215.56238D0,  -34.09288D0,
+     :  48.12027554D0,  1050.71912D0,   27.39717D0 /
+*
+      DATA DINC /
+     : 7.00498625D0, -214.25629D0,   0.28977D0,
+     : 3.39466189D0,  -30.84437D0, -11.67836D0,
+     :          0D0,  469.97289D0,  -3.35053D0,
+     : 1.84972648D0, -293.31722D0,  -8.11830D0,
+     : 1.30326698D0,  -71.55890D0,  11.95297D0,
+     : 2.48887878D0,   91.85195D0, -17.66225D0,
+     : 0.77319689D0,  -60.72723D0,   1.25759D0,
+     : 1.76995259D0,    8.12333D0,   0.08135D0 /
+*
+      DATA OMEGA /
+     :  48.33089304D0,  -4515.21727D0,  -31.79892D0,
+     :  76.67992019D0, -10008.48154D0,  -51.32614D0,
+     : 174.87317577D0,  -8679.27034D0,   15.34191D0,
+     :  49.55809321D0, -10620.90088D0, -230.57416D0,
+     : 100.46440702D0,   6362.03561D0,  326.52178D0,
+     : 113.66550252D0,  -9240.19942D0,  -66.23743D0,
+     :  74.00595701D0,   2669.15033D0,  145.93964D0,
+     : 131.78405702D0,   -221.94322D0,   -0.78728D0 /
+*
+*  Tables for trigonometric terms to be added to the mean elements
+*  of the semi-major axes.
+*
+      DATA DKP /
+     : 69613, 75645, 88306, 59899, 15746, 71087, 142173,  3086,    0,
+     : 21863, 32794, 26934, 10931, 26250, 43725,  53867, 28939,    0,
+     : 16002, 21863, 32004, 10931, 14529, 16368,  15318, 32794,    0,
+     : 6345,   7818, 15636,  7077,  8184, 14163,   1107,  4872,    0,
+     : 1760,   1454,  1167,   880,   287,  2640,     19,  2047, 1454,
+     :  574,      0,   880,   287,    19,  1760,   1167,   306,  574,
+     :  204,      0,   177,  1265,     4,   385,    200,   208,  204,
+     :    0,    102,   106,     4,    98,  1367,    487,   204,    0 /
+*
+      DATA CA /
+     :      4,    -13,    11,    -9,    -9,    -3,    -1,     4,    0,
+     :   -156,     59,   -42,     6,    19,   -20,   -10,   -12,    0,
+     :     64,   -152,    62,    -8,    32,   -41,    19,   -11,    0,
+     :    124,    621,  -145,   208,    54,   -57,    30,    15,    0,
+     : -23437,  -2634,  6601,  6259, -1507, -1821,  2620, -2115,-1489,
+     :  62911,-119919, 79336, 17814,-24241, 12068,  8306, -4893, 8902,
+     : 389061,-262125,-44088,  8387,-22976, -2093,  -615, -9720, 6633,
+     :-412235,-157046,-31430, 37817, -9740,   -13, -7449,  9644,    0 /
+*
+      DATA SA /
+     :     -29,    -1,     9,     6,    -6,     5,     4,     0,    0,
+     :     -48,  -125,   -26,   -37,    18,   -13,   -20,    -2,    0,
+     :    -150,   -46,    68,    54,    14,    24,   -28,    22,    0,
+     :    -621,   532,  -694,   -20,   192,   -94,    71,   -73,    0,
+     :  -14614,-19828, -5869,  1881, -4372, -2255,   782,   930,  913,
+     :  139737,     0, 24667, 51123, -5102,  7429, -4095, -1976,-9566,
+     : -138081,     0, 37205,-49039,-41901,-33872,-27037,-12474,18797,
+     :       0, 28492,133236, 69654, 52322,-49577,-26430, -3593,    0 /
+*
+*  Tables giving the trigonometric terms to be added to the mean
+*  elements of the mean longitudes.
+*
+      DATA DKQ /
+     :  3086, 15746, 69613, 59899, 75645, 88306, 12661, 2658,  0,   0,
+     : 21863, 32794, 10931,    73,  4387, 26934,  1473, 2157,  0,   0,
+     :    10, 16002, 21863, 10931,  1473, 32004,  4387,   73,  0,   0,
+     :    10,  6345,  7818,  1107, 15636,  7077,  8184,  532, 10,   0,
+     :    19,  1760,  1454,   287,  1167,   880,   574, 2640, 19,1454,
+     :    19,   574,   287,   306,  1760,    12,    31,   38, 19, 574,
+     :     4,   204,   177,     8,    31,   200,  1265,  102,  4, 204,
+     :     4,   102,   106,     8,    98,  1367,   487,  204,  4, 102 /
+*
+      DATA CLO /
+     :     21,   -95, -157,   41,   -5,   42,   23,   30,     0,    0,
+     :   -160,  -313, -235,   60,  -74,  -76,  -27,   34,     0,    0,
+     :   -325,  -322,  -79,  232,  -52,   97,   55,  -41,     0,    0,
+     :   2268,  -979,  802,  602, -668,  -33,  345,  201,   -55,    0,
+     :   7610, -4997,-7689,-5841,-2617, 1115, -748, -607,  6074,  354,
+     : -18549, 30125,20012, -730,  824,   23, 1289, -352,-14767,-2062,
+     :-135245,-14594, 4197,-4030,-5630,-2898, 2540, -306,  2939, 1986,
+     :  89948,  2103, 8963, 2695, 3682, 1648,  866, -154, -1963, -283 /
+*
+      DATA SLO /
+     :   -342,   136,  -23,   62,   66,  -52,  -33,   17,     0,    0,
+     :    524,  -149,  -35,  117,  151,  122,  -71,  -62,     0,    0,
+     :   -105,  -137,  258,   35, -116,  -88, -112,  -80,     0,    0,
+     :    854,  -205, -936, -240,  140, -341,  -97, -232,   536,    0,
+     : -56980,  8016, 1012, 1448,-3024,-3710,  318,  503,  3767,  577,
+     : 138606,-13478,-4964, 1441,-1319,-1482,  427, 1236, -9167,-1918,
+     :  71234,-41116, 5334,-4935,-1848,   66,  434,-1748,  3780, -701,
+     : -47645, 11647, 2166, 3194,  679,    0, -244, -419, -2531,   48 /
+
+*  -----
+*  Pluto
+*  -----
+
+*
+*  Coefficients for fundamental arguments:  mean longitudes
+*  (degrees) and mean rate of change of longitude (degrees per
+*  Julian century) for Jupiter, Saturn and Pluto
+*
+      DATA DJ0, DJD / 34.35D0, 3034.9057D0 /
+      DATA DS0, DSD / 50.08D0, 1222.1138D0 /
+      DATA DP0, DPD / 238.96D0, 144.9600D0 /
+
+*  Coefficients for latitude, longitude, radius vector
+      DATA DL0,DLD0 / 238.956785D0, 144.96D0 /
+      DATA DB0 / -3.908202D0 /
+      DATA DR0 / 40.7247248D0 /
+
+*
+*  Coefficients for periodic terms (Meeus's Table 36.A)
+*
+*  The coefficients for term n in the series are:
+*
+*    IJSP(1,n)     J
+*    IJSP(2,n)     S
+*    IJSP(3,n)     P
+*    AB(1,1,n)     longitude sine (degrees)
+*    AB(2,1,n)     longitude cosine (degrees)
+*    AB(1,2,n)     latitude sine (degrees)
+*    AB(2,2,n)     latitude cosine (degrees)
+*    AB(1,3,n)     radius vector sine (AU)
+*    AB(2,3,n)     radius vector cosine (AU)
+*
+      DATA (IJSP(I, 1),I=1,3),((AB(J,I, 1),J=1,2),I=1,3) /
+     :                             0,  0,  1,
+     :            -19798886D-6,  19848454D-6,
+     :             -5453098D-6, -14974876D-6,
+     :             66867334D-7,  68955876D-7 /
+      DATA (IJSP(I, 2),I=1,3),((AB(J,I, 2),J=1,2),I=1,3) /
+     :                             0,  0,  2,
+     :               897499D-6,  -4955707D-6,
+     :              3527363D-6,   1672673D-6,
+     :            -11826086D-7,   -333765D-7 /
+      DATA (IJSP(I, 3),I=1,3),((AB(J,I, 3),J=1,2),I=1,3) /
+     :                             0,  0,  3,
+     :               610820D-6,   1210521D-6,
+     :             -1050939D-6,    327763D-6,
+     :              1593657D-7,  -1439953D-7 /
+      DATA (IJSP(I, 4),I=1,3),((AB(J,I, 4),J=1,2),I=1,3) /
+     :                             0,  0,  4,
+     :              -341639D-6,   -189719D-6,
+     :               178691D-6,   -291925D-6,
+     :               -18948D-7,    482443D-7 /
+      DATA (IJSP(I, 5),I=1,3),((AB(J,I, 5),J=1,2),I=1,3) /
+     :                             0,  0,  5,
+     :               129027D-6,    -34863D-6,
+     :                18763D-6,    100448D-6,
+     :               -66634D-7,    -85576D-7 /
+      DATA (IJSP(I, 6),I=1,3),((AB(J,I, 6),J=1,2),I=1,3) /
+     :                             0,  0,  6,
+     :               -38215D-6,     31061D-6,
+     :               -30594D-6,    -25838D-6,
+     :                30841D-7,     -5765D-7 /
+      DATA (IJSP(I, 7),I=1,3),((AB(J,I, 7),J=1,2),I=1,3) /
+     :                             0,  1, -1,
+     :                20349D-6,     -9886D-6,
+     :                 4965D-6,     11263D-6,
+     :                -6140D-7,     22254D-7 /
+      DATA (IJSP(I, 8),I=1,3),((AB(J,I, 8),J=1,2),I=1,3) /
+     :                             0,  1,  0,
+     :                -4045D-6,     -4904D-6,
+     :                  310D-6,      -132D-6,
+     :                 4434D-7,      4443D-7 /
+      DATA (IJSP(I, 9),I=1,3),((AB(J,I, 9),J=1,2),I=1,3) /
+     :                             0,  1,  1,
+     :                -5885D-6,     -3238D-6,
+     :                 2036D-6,      -947D-6,
+     :                -1518D-7,       641D-7 /
+      DATA (IJSP(I,10),I=1,3),((AB(J,I,10),J=1,2),I=1,3) /
+     :                             0,  1,  2,
+     :                -3812D-6,      3011D-6,
+     :                   -2D-6,      -674D-6,
+     :                   -5D-7,       792D-7 /
+      DATA (IJSP(I,11),I=1,3),((AB(J,I,11),J=1,2),I=1,3) /
+     :                             0,  1,  3,
+     :                 -601D-6,      3468D-6,
+     :                 -329D-6,      -563D-6,
+     :                  518D-7,       518D-7 /
+      DATA (IJSP(I,12),I=1,3),((AB(J,I,12),J=1,2),I=1,3) /
+     :                             0,  2, -2,
+     :                 1237D-6,       463D-6,
+     :                  -64D-6,        39D-6,
+     :                  -13D-7,      -221D-7 /
+      DATA (IJSP(I,13),I=1,3),((AB(J,I,13),J=1,2),I=1,3) /
+     :                             0,  2, -1,
+     :                 1086D-6,      -911D-6,
+     :                  -94D-6,       210D-6,
+     :                  837D-7,      -494D-7 /
+      DATA (IJSP(I,14),I=1,3),((AB(J,I,14),J=1,2),I=1,3) /
+     :                             0,  2,  0,
+     :                  595D-6,     -1229D-6,
+     :                   -8D-6,      -160D-6,
+     :                 -281D-7,       616D-7 /
+      DATA (IJSP(I,15),I=1,3),((AB(J,I,15),J=1,2),I=1,3) /
+     :                             1, -1,  0,
+     :                 2484D-6,      -485D-6,
+     :                 -177D-6,       259D-6,
+     :                  260D-7,      -395D-7 /
+      DATA (IJSP(I,16),I=1,3),((AB(J,I,16),J=1,2),I=1,3) /
+     :                             1, -1,  1,
+     :                  839D-6,     -1414D-6,
+     :                   17D-6,       234D-6,
+     :                 -191D-7,      -396D-7 /
+      DATA (IJSP(I,17),I=1,3),((AB(J,I,17),J=1,2),I=1,3) /
+     :                             1,  0, -3,
+     :                 -964D-6,      1059D-6,
+     :                  582D-6,      -285D-6,
+     :                -3218D-7,       370D-7 /
+      DATA (IJSP(I,18),I=1,3),((AB(J,I,18),J=1,2),I=1,3) /
+     :                             1,  0, -2,
+     :                -2303D-6,     -1038D-6,
+     :                 -298D-6,       692D-6,
+     :                 8019D-7,     -7869D-7 /
+      DATA (IJSP(I,19),I=1,3),((AB(J,I,19),J=1,2),I=1,3) /
+     :                             1,  0, -1,
+     :                 7049D-6,       747D-6,
+     :                  157D-6,       201D-6,
+     :                  105D-7,     45637D-7 /
+      DATA (IJSP(I,20),I=1,3),((AB(J,I,20),J=1,2),I=1,3) /
+     :                             1,  0,  0,
+     :                 1179D-6,      -358D-6,
+     :                  304D-6,       825D-6,
+     :                 8623D-7,      8444D-7 /
+      DATA (IJSP(I,21),I=1,3),((AB(J,I,21),J=1,2),I=1,3) /
+     :                             1,  0,  1,
+     :                  393D-6,       -63D-6,
+     :                 -124D-6,       -29D-6,
+     :                 -896D-7,      -801D-7 /
+      DATA (IJSP(I,22),I=1,3),((AB(J,I,22),J=1,2),I=1,3) /
+     :                             1,  0,  2,
+     :                  111D-6,      -268D-6,
+     :                   15D-6,         8D-6,
+     :                  208D-7,      -122D-7 /
+      DATA (IJSP(I,23),I=1,3),((AB(J,I,23),J=1,2),I=1,3) /
+     :                             1,  0,  3,
+     :                  -52D-6,      -154D-6,
+     :                    7D-6,        15D-6,
+     :                 -133D-7,        65D-7 /
+      DATA (IJSP(I,24),I=1,3),((AB(J,I,24),J=1,2),I=1,3) /
+     :                             1,  0,  4,
+     :                  -78D-6,       -30D-6,
+     :                    2D-6,         2D-6,
+     :                  -16D-7,         1D-7 /
+      DATA (IJSP(I,25),I=1,3),((AB(J,I,25),J=1,2),I=1,3) /
+     :                             1,  1, -3,
+     :                  -34D-6,       -26D-6,
+     :                    4D-6,         2D-6,
+     :                  -22D-7,         7D-7 /
+      DATA (IJSP(I,26),I=1,3),((AB(J,I,26),J=1,2),I=1,3) /
+     :                             1,  1, -2,
+     :                  -43D-6,         1D-6,
+     :                    3D-6,         0D-6,
+     :                   -8D-7,        16D-7 /
+      DATA (IJSP(I,27),I=1,3),((AB(J,I,27),J=1,2),I=1,3) /
+     :                             1,  1, -1,
+     :                  -15D-6,        21D-6,
+     :                    1D-6,        -1D-6,
+     :                    2D-7,         9D-7 /
+      DATA (IJSP(I,28),I=1,3),((AB(J,I,28),J=1,2),I=1,3) /
+     :                             1,  1,  0,
+     :                   -1D-6,        15D-6,
+     :                    0D-6,        -2D-6,
+     :                   12D-7,         5D-7 /
+      DATA (IJSP(I,29),I=1,3),((AB(J,I,29),J=1,2),I=1,3) /
+     :                             1,  1,  1,
+     :                    4D-6,         7D-6,
+     :                    1D-6,         0D-6,
+     :                    1D-7,        -3D-7 /
+      DATA (IJSP(I,30),I=1,3),((AB(J,I,30),J=1,2),I=1,3) /
+     :                             1,  1,  3,
+     :                    1D-6,         5D-6,
+     :                    1D-6,        -1D-6,
+     :                    1D-7,         0D-7 /
+      DATA (IJSP(I,31),I=1,3),((AB(J,I,31),J=1,2),I=1,3) /
+     :                             2,  0, -6,
+     :                    8D-6,         3D-6,
+     :                   -2D-6,        -3D-6,
+     :                    9D-7,         5D-7 /
+      DATA (IJSP(I,32),I=1,3),((AB(J,I,32),J=1,2),I=1,3) /
+     :                             2,  0, -5,
+     :                   -3D-6,         6D-6,
+     :                    1D-6,         2D-6,
+     :                    2D-7,        -1D-7 /
+      DATA (IJSP(I,33),I=1,3),((AB(J,I,33),J=1,2),I=1,3) /
+     :                             2,  0, -4,
+     :                    6D-6,       -13D-6,
+     :                   -8D-6,         2D-6,
+     :                   14D-7,        10D-7 /
+      DATA (IJSP(I,34),I=1,3),((AB(J,I,34),J=1,2),I=1,3) /
+     :                             2,  0, -3,
+     :                   10D-6,        22D-6,
+     :                   10D-6,        -7D-6,
+     :                  -65D-7,        12D-7 /
+      DATA (IJSP(I,35),I=1,3),((AB(J,I,35),J=1,2),I=1,3) /
+     :                             2,  0, -2,
+     :                  -57D-6,       -32D-6,
+     :                    0D-6,        21D-6,
+     :                  126D-7,      -233D-7 /
+      DATA (IJSP(I,36),I=1,3),((AB(J,I,36),J=1,2),I=1,3) /
+     :                             2,  0, -1,
+     :                  157D-6,       -46D-6,
+     :                    8D-6,         5D-6,
+     :                  270D-7,      1068D-7 /
+      DATA (IJSP(I,37),I=1,3),((AB(J,I,37),J=1,2),I=1,3) /
+     :                             2,  0,  0,
+     :                   12D-6,       -18D-6,
+     :                   13D-6,        16D-6,
+     :                  254D-7,       155D-7 /
+      DATA (IJSP(I,38),I=1,3),((AB(J,I,38),J=1,2),I=1,3) /
+     :                             2,  0,  1,
+     :                   -4D-6,         8D-6,
+     :                   -2D-6,        -3D-6,
+     :                  -26D-7,        -2D-7 /
+      DATA (IJSP(I,39),I=1,3),((AB(J,I,39),J=1,2),I=1,3) /
+     :                             2,  0,  2,
+     :                   -5D-6,         0D-6,
+     :                    0D-6,         0D-6,
+     :                    7D-7,         0D-7 /
+      DATA (IJSP(I,40),I=1,3),((AB(J,I,40),J=1,2),I=1,3) /
+     :                             2,  0,  3,
+     :                    3D-6,         4D-6,
+     :                    0D-6,         1D-6,
+     :                  -11D-7,         4D-7 /
+      DATA (IJSP(I,41),I=1,3),((AB(J,I,41),J=1,2),I=1,3) /
+     :                             3,  0, -2,
+     :                   -1D-6,        -1D-6,
+     :                    0D-6,         1D-6,
+     :                    4D-7,       -14D-7 /
+      DATA (IJSP(I,42),I=1,3),((AB(J,I,42),J=1,2),I=1,3) /
+     :                             3,  0, -1,
+     :                    6D-6,        -3D-6,
+     :                    0D-6,         0D-6,
+     :                   18D-7,        35D-7 /
+      DATA (IJSP(I,43),I=1,3),((AB(J,I,43),J=1,2),I=1,3) /
+     :                             3,  0,  0,
+     :                   -1D-6,        -2D-6,
+     :                    0D-6,         1D-6,
+     :                   13D-7,         3D-7 /
+
+
+*  Validate the planet number.
+      IF (NP.LT.1.OR.NP.GT.9) THEN
+         JSTAT=-1
+         DO I=1,6
+            PV(I)=0D0
+         END DO
+      ELSE
+
+*     Separate algorithms for Pluto and the rest.
+         IF (NP.NE.9) THEN
+
+*        -----------------------
+*        Mercury through Neptune
+*        -----------------------
+
+*        Time: Julian millennia since J2000.
+            T=(DATE-51544.5D0)/365250D0
+
+*        OK status unless remote epoch.
+            IF (ABS(T).LE.1D0) THEN
+               JSTAT=0
+            ELSE
+               JSTAT=1
+            END IF
+
+*        Compute the mean elements.
+            DA=A(1,NP)+(A(2,NP)+A(3,NP)*T)*T
+            DL=(3600D0*DLM(1,NP)+(DLM(2,NP)+DLM(3,NP)*T)*T)*AS2R
+            DE=E(1,NP)+(E(2,NP)+E(3,NP)*T)*T
+            DPE=MOD((3600D0*PI(1,NP)+(PI(2,NP)+PI(3,NP)*T)*T)*AS2R,D2PI)
+            DI=(3600D0*DINC(1,NP)+(DINC(2,NP)+DINC(3,NP)*T)*T)*AS2R
+            DO=MOD((3600D0*OMEGA(1,NP)
+     :                        +(OMEGA(2,NP)+OMEGA(3,NP)*T)*T)*AS2R,D2PI)
+
+*        Apply the trigonometric terms.
+            DMU=0.35953620D0*T
+            DO J=1,8
+               ARGA=DKP(J,NP)*DMU
+               ARGL=DKQ(J,NP)*DMU
+               DA=DA+(CA(J,NP)*COS(ARGA)+SA(J,NP)*SIN(ARGA))*1D-7
+               DL=DL+(CLO(J,NP)*COS(ARGL)+SLO(J,NP)*SIN(ARGL))*1D-7
+            END DO
+            ARGA=DKP(9,NP)*DMU
+            DA=DA+T*(CA(9,NP)*COS(ARGA)+SA(9,NP)*SIN(ARGA))*1D-7
+            DO J=9,10
+               ARGL=DKQ(J,NP)*DMU
+               DL=DL+T*(CLO(J,NP)*COS(ARGL)+SLO(J,NP)*SIN(ARGL))*1D-7
+            END DO
+            DL=MOD(DL,D2PI)
+
+*        Daily motion.
+            DM=GCON*SQRT((1D0+1D0/AMAS(NP))/(DA*DA*DA))
+
+*        Make the prediction.
+            CALL sla_PLANEL(DATE,1,DATE,DI,DO,DPE,DA,DE,DL,DM,PV,J)
+            IF (J.LT.0) JSTAT=-2
+
+         ELSE
+
+*        -----
+*        Pluto
+*        -----
+
+*        Time: Julian centuries since J2000.
+            T=(DATE-51544.5D0)/36525D0
+
+*        OK status unless remote epoch.
+            IF (T.GE.-1.15D0.AND.T.LE.1D0) THEN
+               JSTAT=0
+            ELSE
+               JSTAT=1
+            END IF
+
+*        Fundamental arguments (radians).
+            DJ=(DJ0+DJD*T)*D2R
+            DS=(DS0+DSD*T)*D2R
+            DP=(DP0+DPD*T)*D2R
+
+*        Initialize coefficients and derivatives.
+            DO I=1,3
+               WLBR(I)=0D0
+               WLBRD(I)=0D0
+            END DO
+
+*        Term by term through Meeus Table 36.A.
+            DO J=1,43
+
+*           Argument and derivative (radians, radians per century).
+               WJ=DBLE(IJSP(1,J))
+               WS=DBLE(IJSP(2,J))
+               WP=DBLE(IJSP(3,J))
+               AL=WJ*DJ+WS*DS+WP*DP
+               ALD=(WJ*DJD+WS*DSD+WP*DPD)*D2R
+
+*           Functions of argument.
+               SAL=SIN(AL)
+               CAL=COS(AL)
+
+*           Periodic terms in longitude, latitude, radius vector.
+               DO I=1,3
+
+*              A and B coefficients (deg, AU).
+                  AC=AB(1,I,J)
+                  BC=AB(2,I,J)
+
+*              Periodic terms (deg, AU, deg/Jc, AU/Jc).
+                  WLBR(I)=WLBR(I)+AC*SAL+BC*CAL
+                  WLBRD(I)=WLBRD(I)+(AC*CAL-BC*SAL)*ALD
+               END DO
+            END DO
+
+*        Heliocentric longitude and derivative (radians, radians/sec).
+            DL=(DL0+DLD0*T+WLBR(1))*D2R
+            DLD=(DLD0+WLBRD(1))*D2R/SPC
+
+*        Heliocentric latitude and derivative (radians, radians/sec).
+            DB=(DB0+WLBR(2))*D2R
+            DBD=WLBRD(2)*D2R/SPC
+
+*        Heliocentric radius vector and derivative (AU, AU/sec).
+            DR=DR0+WLBR(3)
+            DRD=WLBRD(3)/SPC
+
+*        Functions of latitude, longitude, radius vector.
+            SL=SIN(DL)
+            CL=COS(DL)
+            SB=SIN(DB)
+            CB=COS(DB)
+            SLCB=SL*CB
+            CLCB=CL*CB
+
+*        Heliocentric vector and derivative, J2000 ecliptic and equinox.
+            X=DR*CLCB
+            Y=DR*SLCB
+            Z=DR*SB
+            XD=DRD*CLCB-DR*(CL*SB*DBD+SLCB*DLD)
+            YD=DRD*SLCB+DR*(-SL*SB*DBD+CLCB*DLD)
+            ZD=DRD*SB+DR*CB*DBD
+
+*        Transform to J2000 equator and equinox.
+            PV(1)=X
+            PV(2)=Y*CE-Z*SE
+            PV(3)=Y*SE+Z*CE
+            PV(4)=XD
+            PV(5)=YD*CE-ZD*SE
+            PV(6)=YD*SE+ZD*CE
+         END IF
+      END IF
+
+      END
diff --git a/src/slalib/plante.f b/src/slalib/plante.f
new file mode 100644
index 0000000..e8f89d9
--- /dev/null
+++ b/src/slalib/plante.f
@@ -0,0 +1,157 @@
+      SUBROUTINE sla_PLANTE (DATE, ELONG, PHI, JFORM, EPOCH,
+     :                       ORBINC, ANODE, PERIH, AORQ, E,
+     :                       AORL, DM, RA, DEC, R, JSTAT)
+*+
+*     - - - - - - -
+*      P L A N T E
+*     - - - - - - -
+*
+*  Topocentric apparent RA,Dec of a Solar-System object whose
+*  heliocentric orbital elements are known.
+*
+*  Given:
+*     DATE      d     MJD of observation (JD - 2400000.5)
+*     ELONG     d     observer's east longitude (radians)
+*     PHI       d     observer's geodetic latitude (radians)
+*     JFORM     i     choice of element set (1-3; Note 4)
+*     EPOCH     d     epoch of elements (TT MJD)
+*     ORBINC    d     inclination (radians)
+*     ANODE     d     longitude of the ascending node (radians)
+*     PERIH     d     longitude or argument of perihelion (radians)
+*     AORQ      d     mean distance or perihelion distance (AU)
+*     E         d     eccentricity
+*     AORL      d     mean anomaly or longitude (radians, JFORM=1,2 only)
+*     DM        d     daily motion (radians, JFORM=1 only )
+*
+*  Returned:
+*     RA,DEC    d     RA, Dec (topocentric apparent, radians)
+*     R         d     distance from observer (AU)
+*     JSTAT     i     status:  0 = OK
+*                             -1 = illegal JFORM
+*                             -2 = illegal E
+*                             -3 = illegal AORQ
+*                             -4 = illegal DM
+*                             -5 = numerical error
+*
+*  Notes:
+*
+*  1  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).
+*
+*  2  The longitude and latitude allow correction for geocentric
+*     parallax.  This is usually a small effect, but can become
+*     important for Earth-crossing asteroids.  Geocentric positions
+*     can be generated by appropriate use of routines sla_EVP and
+*     sla_PLANEL.
+*
+*  3  The elements are with respect to the J2000 ecliptic and equinox.
+*
+*  4  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
+*     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
+*
+*  5  Unused elements (DM for JFORM=2, AORL and DM for JFORM=3) are
+*     not accessed.
+*
+*  Called: sla_GMST, sla_DT, sla_EPJ, sla_PVOBS, sla_PRENUT,
+*          sla_PLANEL, sla_DMXV, sla_DCC2S, sla_DRANRM
+*
+*  P.T.Wallace   Starlink   17 March 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DATE,ELONG,PHI
+      INTEGER JFORM
+      DOUBLE PRECISION EPOCH,ORBINC,ANODE,PERIH,AORQ,E,
+     :                 AORL,DM,RA,DEC,R
+      INTEGER JSTAT
+
+*  Light time for unit distance (sec)
+      DOUBLE PRECISION TAU
+      PARAMETER (TAU=499.004782D0)
+
+      INTEGER I
+      DOUBLE PRECISION DVB(3),DPB(3),VSG(6),VSP(6),V(6),RMAT(3,3),
+     :                 VGP(6),STL,VGO(6),DX,DY,DZ,D,TL
+      DOUBLE PRECISION sla_GMST,sla_DT,sla_EPJ,sla_DRANRM
+
+
+
+*  Sun to geocentre (J2000).
+      CALL sla_EVP(DATE,2000D0,DVB,DPB,VSG(4),VSG)
+
+*  Sun to planet (J2000).
+      CALL sla_PLANEL(DATE,JFORM,EPOCH,ORBINC,ANODE,PERIH,AORQ,
+     :                E,AORL,DM,VSP,JSTAT)
+
+*  Geocentre to planet (J2000).
+      DO I=1,6
+         V(I)=VSP(I)-VSG(I)
+      END DO
+
+*  Precession and nutation to date.
+      CALL sla_PRENUT(2000D0,DATE,RMAT)
+      CALL sla_DMXV(RMAT,V,VGP)
+      CALL sla_DMXV(RMAT,V(4),VGP(4))
+
+*  Geocentre to observer (date).
+      STL=sla_GMST(DATE-sla_DT(sla_EPJ(DATE))/86400D0)+ELONG
+      CALL sla_PVOBS(PHI,0D0,STL,VGO)
+
+*  Observer to planet (date).
+      DO I=1,6
+         V(I)=VGP(I)-VGO(I)
+      END DO
+
+*  Geometric distance (AU).
+      DX=V(1)
+      DY=V(2)
+      DZ=V(3)
+      D=SQRT(DX*DX+DY*DY+DZ*DZ)
+
+*  Light time (sec).
+      TL=TAU*D
+
+*  Correct position for planetary aberration
+      DO I=1,3
+         V(I)=V(I)-TL*V(I+3)
+      END DO
+
+*  To RA,Dec.
+      CALL sla_DCC2S(V,RA,DEC)
+      RA=sla_DRANRM(RA)
+      R=D
+
+      END
diff --git a/src/slalib/pm.f b/src/slalib/pm.f
new file mode 100644
index 0000000..82a5772
--- /dev/null
+++ b/src/slalib/pm.f
@@ -0,0 +1,74 @@
+      SUBROUTINE sla_PM (R0, D0, PR, PD, PX, RV, EP0, EP1, R1, D1)
+*+
+*     - - -
+*      P M
+*     - - -
+*
+*  Apply corrections for proper motion to a star RA,Dec
+*  (double precision)
+*
+*  References:
+*     1984 Astronomical Almanac, pp B39-B41.
+*     (also Lederle & Schwan, Astron. Astrophys. 134,
+*      1-6, 1984)
+*
+*  Given:
+*     R0,D0    dp     RA,Dec at epoch EP0 (rad)
+*     PR,PD    dp     proper motions:  RA,Dec changes per year of epoch
+*     PX       dp     parallax (arcsec)
+*     RV       dp     radial velocity (km/sec, +ve if receding)
+*     EP0      dp     start epoch in years (e.g. Julian epoch)
+*     EP1      dp     end epoch in years (same system as EP0)
+*
+*  Returned:
+*     R1,D1    dp     RA,Dec at epoch EP1 (rad)
+*
+*  Called:
+*     sla_DCS2C       spherical to Cartesian
+*     sla_DCC2S       Cartesian to spherical
+*     sla_DRANRM      normalize angle 0-2Pi
+*
+*  Note:
+*     The proper motions in RA are dRA/dt rather than
+*     cos(Dec)*dRA/dt, and are in the same coordinate
+*     system as R0,D0.
+*
+*  P.T.Wallace   Starlink   23 August 1996
+*
+*  Copyright (C) 1996 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION R0,D0,PR,PD,PX,RV,EP0,EP1,R1,D1
+
+*  Km/s to AU/year multiplied by arc seconds to radians
+      DOUBLE PRECISION VFR
+      PARAMETER (VFR=0.21094502D0*0.484813681109535994D-5)
+
+      INTEGER I
+      DOUBLE PRECISION sla_DRANRM
+      DOUBLE PRECISION W,EM(3),T,P(3)
+
+
+
+*  Spherical to Cartesian
+      CALL sla_DCS2C(R0,D0,P)
+
+*  Space motion (radians per year)
+      W=VFR*RV*PX
+      EM(1)=-PR*P(2)-PD*COS(R0)*SIN(D0)+W*P(1)
+      EM(2)= PR*P(1)-PD*SIN(R0)*SIN(D0)+W*P(2)
+      EM(3)=         PD*COS(D0)        +W*P(3)
+
+*  Apply the motion
+      T=EP1-EP0
+      DO I=1,3
+         P(I)=P(I)+T*EM(I)
+      END DO
+
+*  Cartesian to spherical
+      CALL sla_DCC2S(P,R1,D1)
+      R1=sla_DRANRM(R1)
+
+      END
diff --git a/src/slalib/polmo.f b/src/slalib/polmo.f
new file mode 100644
index 0000000..4532ca8
--- /dev/null
+++ b/src/slalib/polmo.f
@@ -0,0 +1,133 @@
+      SUBROUTINE sla_POLMO ( ELONGM, PHIM, XP, YP, ELONG, PHI, DAZ )
+*+
+*     - - - - - -
+*      P O L M O
+*     - - - - - -
+*
+*  Polar motion:  correct site longitude and latitude for polar
+*  motion and calculate azimuth difference between celestial and
+*  terrestrial poles.
+*
+*  Given:
+*     ELONGM   d      mean longitude of the observer (radians, east +ve)
+*     PHIM     d      mean geodetic latitude of the observer (radians)
+*     XP       d      polar motion x-coordinate (radians)
+*     YP       d      polar motion y-coordinate (radians)
+*
+*  Returned:
+*     ELONG    d      true longitude of the observer (radians, east +ve)
+*     PHI      d      true geodetic latitude of the observer (radians)
+*     DAZ      d      azimuth correction (terrestrial-celestial, radians)
+*
+*  Notes:
+*
+*   1)  "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.
+*
+*   2)  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.
+*
+*   3)  "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).
+*
+*   4)  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.
+*
+*   5)  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.
+*
+*  P.T.Wallace   Starlink   22 February 1996
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION ELONGM,PHIM,XP,YP,ELONG,PHI,DAZ
+
+      DOUBLE PRECISION 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.EQ.0D0) XT=1D0
+      SEL=YT/CPH
+      CEL=XT/CPH
+
+*  Return true longitude and true geodetic latitude of site
+      ELONG=ATAN2(YT,XT)
+      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
+      DAZ=ATAN2(-YNT,-XNT)
+
+      END
diff --git a/src/slalib/prebn.f b/src/slalib/prebn.f
new file mode 100644
index 0000000..a99dd51
--- /dev/null
+++ b/src/slalib/prebn.f
@@ -0,0 +1,62 @@
+      SUBROUTINE sla_PREBN (BEP0, BEP1, RMATP)
+*+
+*     - - - - - -
+*      P R E B N
+*     - - - - - -
+*
+*  Generate the matrix of precession between two epochs,
+*  using the old, pre-IAU1976, Bessel-Newcomb model, using
+*  Kinoshita's formulation (double precision)
+*
+*  Given:
+*     BEP0    dp         beginning Besselian epoch
+*     BEP1    dp         ending Besselian epoch
+*
+*  Returned:
+*     RMATP  dp(3,3)    precession matrix
+*
+*  The matrix is in the sense   V(BEP1)  =  RMATP * V(BEP0)
+*
+*  Reference:
+*     Kinoshita, H. (1975) 'Formulas for precession', SAO Special
+*     Report No. 364, Smithsonian Institution Astrophysical
+*     Observatory, Cambridge, Massachusetts.
+*
+*  Called:  sla_DEULER
+*
+*  P.T.Wallace   Starlink   23 August 1996
+*
+*  Copyright (C) 1996 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION BEP0,BEP1,RMATP(3,3)
+
+*  Arc seconds to radians
+      DOUBLE PRECISION AS2R
+      PARAMETER (AS2R=0.484813681109535994D-5)
+
+      DOUBLE PRECISION BIGT,T,TAS2R,W,ZETA,Z,THETA
+
+
+
+*  Interval between basic epoch B1850.0 and beginning epoch in TC
+      BIGT = (BEP0-1850D0)/100D0
+
+*  Interval over which precession required, in tropical centuries
+      T = (BEP1-BEP0)/100D0
+
+*  Euler angles
+      TAS2R = T*AS2R
+      W = 2303.5548D0+(1.39720D0+0.000059D0*BIGT)*BIGT
+
+      ZETA = (W+(0.30242D0-0.000269D0*BIGT+0.017996D0*T)*T)*TAS2R
+      Z = (W+(1.09478D0+0.000387D0*BIGT+0.018324D0*T)*T)*TAS2R
+      THETA = (2005.1125D0+(-0.85294D0-0.000365D0*BIGT)*BIGT+
+     :        (-0.42647D0-0.000365D0*BIGT-0.041802D0*T)*T)*TAS2R
+
+*  Rotation matrix
+      CALL sla_DEULER('ZYZ',-ZETA,THETA,-Z,RMATP)
+
+      END
diff --git a/src/slalib/prec.f b/src/slalib/prec.f
new file mode 100644
index 0000000..65a4bb6
--- /dev/null
+++ b/src/slalib/prec.f
@@ -0,0 +1,79 @@
+      SUBROUTINE sla_PREC (EP0, EP1, RMATP)
+*+
+*     - - - - -
+*      P R E C
+*     - - - - -
+*
+*  Form the matrix of precession between two epochs (IAU 1976, FK5)
+*  (double precision)
+*
+*  Given:
+*     EP0    dp         beginning epoch
+*     EP1    dp         ending epoch
+*
+*  Returned:
+*     RMATP  dp(3,3)    precession matrix
+*
+*  Notes:
+*
+*     1)  The epochs are TDB (loosely ET) Julian epochs.
+*
+*     2)  The matrix is in the sense   V(EP1)  =  RMATP * V(EP0)
+*
+*     3)  Though the matrix method itself is rigorous, the precession
+*         angles are expressed through canonical polynomials which are
+*         valid only for a limited time span.  There are also known
+*         errors in the IAU precession rate.  The absolute accuracy
+*         of the present formulation is better than 0.1 arcsec from
+*         1960AD to 2040AD, better than 1 arcsec from 1640AD to 2360AD,
+*         and remains below 3 arcsec for the whole of the period
+*         500BC to 3000AD.  The errors exceed 10 arcsec outside the
+*         range 1200BC to 3900AD, exceed 100 arcsec outside 4200BC to
+*         5600AD and exceed 1000 arcsec outside 6800BC to 8200AD.
+*         The SLALIB routine sla_PRECL implements a more elaborate
+*         model which is suitable for problems spanning several
+*         thousand years.
+*
+*  References:
+*     Lieske,J.H., 1979. Astron.Astrophys.,73,282.
+*      equations (6) & (7), p283.
+*     Kaplan,G.H., 1981. USNO circular no. 163, pA2.
+*
+*  Called:  sla_DEULER
+*
+*  P.T.Wallace   Starlink   23 August 1996
+*
+*  Copyright (C) 1996 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION EP0,EP1,RMATP(3,3)
+
+*  Arc seconds to radians
+      DOUBLE PRECISION AS2R
+      PARAMETER (AS2R=0.484813681109535994D-5)
+
+      DOUBLE PRECISION T0,T,TAS2R,W,ZETA,Z,THETA
+
+
+
+*  Interval between basic epoch J2000.0 and beginning epoch (JC)
+      T0 = (EP0-2000D0)/100D0
+
+*  Interval over which precession required (JC)
+      T = (EP1-EP0)/100D0
+
+*  Euler angles
+      TAS2R = T*AS2R
+      W = 2306.2181D0+(1.39656D0-0.000139D0*T0)*T0
+
+      ZETA = (W+((0.30188D0-0.000344D0*T0)+0.017998D0*T)*T)*TAS2R
+      Z = (W+((1.09468D0+0.000066D0*T0)+0.018203D0*T)*T)*TAS2R
+      THETA = ((2004.3109D0+(-0.85330D0-0.000217D0*T0)*T0)
+     :        +((-0.42665D0-0.000217D0*T0)-0.041833D0*T)*T)*TAS2R
+
+*  Rotation matrix
+      CALL sla_DEULER('ZYZ',-ZETA,THETA,-Z,RMATP)
+
+      END
diff --git a/src/slalib/preces.f b/src/slalib/preces.f
new file mode 100644
index 0000000..09f946e
--- /dev/null
+++ b/src/slalib/preces.f
@@ -0,0 +1,84 @@
+      SUBROUTINE sla_PRECES (SYSTEM, EP0, EP1, RA, DC)
+*+
+*     - - - - - - -
+*      P R E C E S
+*     - - - - - - -
+*
+*  Precession - either FK4 (Bessel-Newcomb, pre IAU 1976) or
+*  FK5 (Fricke, post IAU 1976) as required.
+*
+*  Given:
+*     SYSTEM     char   precession to be applied: 'FK4' or 'FK5'
+*     EP0,EP1    dp     starting and ending epoch
+*     RA,DC      dp     RA,Dec, mean equator & equinox of epoch EP0
+*
+*  Returned:
+*     RA,DC      dp     RA,Dec, mean equator & equinox of epoch EP1
+*
+*  Called:    sla_DRANRM, sla_PREBN, sla_PREC, sla_DCS2C,
+*             sla_DMXV, sla_DCC2S
+*
+*  Notes:
+*
+*     1)  Lowercase characters in SYSTEM are acceptable.
+*
+*     2)  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:
+*             CALL sla_PRECES ('FK4', 1900D0, 1950D0, RA, DC)
+*
+*     3)  This routine will NOT correctly convert between the old and
+*         the new systems - for example conversion from B1950 to J2000.
+*         For these purposes see sla_FK425, sla_FK524, sla_FK45Z and
+*         sla_FK54Z.
+*
+*     4)  If an invalid SYSTEM is supplied, values of -99D0,-99D0 will
+*         be returned for both RA and DC.
+*
+*  P.T.Wallace   Starlink   20 April 1990
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      CHARACTER SYSTEM*(*)
+      DOUBLE PRECISION EP0,EP1,RA,DC
+
+      DOUBLE PRECISION PM(3,3),V1(3),V2(3)
+      CHARACTER SYSUC*3
+
+      DOUBLE PRECISION sla_DRANRM
+
+
+
+
+*  Convert to uppercase and validate SYSTEM
+      SYSUC=SYSTEM
+      IF (SYSUC(1:1).EQ.'f') SYSUC(1:1)='F'
+      IF (SYSUC(2:2).EQ.'k') SYSUC(2:2)='K'
+      IF (SYSUC.NE.'FK4'.AND.SYSUC.NE.'FK5') THEN
+         RA=-99D0
+         DC=-99D0
+      ELSE
+
+*     Generate appropriate precession matrix
+         IF (SYSUC.EQ.'FK4') THEN
+            CALL sla_PREBN(EP0,EP1,PM)
+         ELSE
+            CALL sla_PREC(EP0,EP1,PM)
+         END IF
+
+*     Convert RA,Dec to x,y,z
+         CALL sla_DCS2C(RA,DC,V1)
+
+*     Precess
+         CALL sla_DMXV(PM,V1,V2)
+
+*     Back to RA,Dec
+         CALL sla_DCC2S(V2,RA,DC)
+         RA=sla_DRANRM(RA)
+
+      END IF
+
+      END
diff --git a/src/slalib/precl.f b/src/slalib/precl.f
new file mode 100644
index 0000000..e24b3d3
--- /dev/null
+++ b/src/slalib/precl.f
@@ -0,0 +1,125 @@
+      SUBROUTINE sla_PRECL (EP0, EP1, RMATP)
+*+
+*     - - - - - -
+*      P R E C L
+*     - - - - - -
+*
+*  Form the matrix of precession between two epochs, using the
+*  model of Simon et al (1994), which is suitable for long
+*  periods of time.
+*
+*  (double precision)
+*
+*  Given:
+*     EP0    dp         beginning epoch
+*     EP1    dp         ending epoch
+*
+*  Returned:
+*     RMATP  dp(3,3)    precession matrix
+*
+*  Notes:
+*
+*     1)  The epochs are TDB Julian epochs.
+*
+*     2)  The matrix is in the sense   V(EP1)  =  RMATP * V(EP0)
+*
+*     3)  The absolute accuracy of the model is limited by the
+*         uncertainty in the general precession, about 0.3 arcsec per
+*         1000 years.  The remainder of the formulation provides a
+*         precision of 1 mas over the interval from 1000AD to 3000AD,
+*         0.1 arcsec from 1000BC to 5000AD and 1 arcsec from
+*         4000BC to 8000AD.
+*
+*  Reference:
+*     Simon, J.L. et al., 1994. Astron.Astrophys., 282, 663-683.
+*
+*  Called:  sla_DEULER
+*
+*  P.T.Wallace   Starlink   23 August 1996
+*
+*  Copyright (C) 1996 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION EP0,EP1,RMATP(3,3)
+
+*  Arc seconds to radians
+      DOUBLE PRECISION AS2R
+      PARAMETER (AS2R=0.484813681109535994D-5)
+
+      DOUBLE PRECISION T0,T,TAS2R,W,ZETA,Z,THETA
+
+
+
+*  Interval between basic epoch J2000.0 and beginning epoch (1000JY)
+      T0 = (EP0-2000D0)/1000D0
+
+*  Interval over which precession required (1000JY)
+      T = (EP1-EP0)/1000D0
+
+*  Euler angles
+      TAS2R = T*AS2R
+      W =      23060.9097D0+
+     :          (139.7459D0+
+     :           (-0.0038D0+
+     :           (-0.5918D0+
+     :           (-0.0037D0+
+     :             0.0007D0*T0)*T0)*T0)*T0)*T0
+
+      ZETA =   (W+(30.2226D0+
+     :            (-0.2523D0+
+     :            (-0.3840D0+
+     :            (-0.0014D0+
+     :              0.0007D0*T0)*T0)*T0)*T0+
+     :            (18.0183D0+
+     :            (-0.1326D0+
+     :             (0.0006D0+
+     :              0.0005D0*T0)*T0)*T0+
+     :            (-0.0583D0+
+     :            (-0.0001D0+
+     :              0.0007D0*T0)*T0+
+     :            (-0.0285D0+
+     :            (-0.0002D0)*T)*T)*T)*T)*T)*TAS2R
+
+      Z =     (W+(109.5270D0+
+     :             (0.2446D0+
+     :            (-1.3913D0+
+     :            (-0.0134D0+
+     :              0.0026D0*T0)*T0)*T0)*T0+
+     :            (18.2667D0+
+     :            (-1.1400D0+
+     :            (-0.0173D0+
+     :              0.0044D0*T0)*T0)*T0+
+     :            (-0.2821D0+
+     :            (-0.0093D0+
+     :              0.0032D0*T0)*T0+
+     :            (-0.0301D0+
+     :              0.0006D0*T0
+     :             -0.0001D0*T)*T)*T)*T)*T)*TAS2R
+
+      THETA =  (20042.0207D0+
+     :           (-85.3131D0+
+     :            (-0.2111D0+
+     :             (0.3642D0+
+     :             (0.0008D0+
+     :            (-0.0005D0)*T0)*T0)*T0)*T0)*T0+
+     :           (-42.6566D0+
+     :            (-0.2111D0+
+     :             (0.5463D0+
+     :             (0.0017D0+
+     :            (-0.0012D0)*T0)*T0)*T0)*T0+
+     :           (-41.8238D0+
+     :             (0.0359D0+
+     :             (0.0027D0+
+     :            (-0.0001D0)*T0)*T0)*T0+
+     :            (-0.0731D0+
+     :             (0.0019D0+
+     :              0.0009D0*T0)*T0+
+     :            (-0.0127D0+
+     :              0.0011D0*T0+0.0004D0*T)*T)*T)*T)*T)*TAS2R
+
+*  Rotation matrix
+      CALL sla_DEULER('ZYZ',-ZETA,THETA,-Z,RMATP)
+
+      END
diff --git a/src/slalib/prenut.f b/src/slalib/prenut.f
new file mode 100644
index 0000000..96d6bdc
--- /dev/null
+++ b/src/slalib/prenut.f
@@ -0,0 +1,48 @@
+      SUBROUTINE sla_PRENUT (EPOCH, DATE, RMATPN)
+*+
+*     - - - - - - -
+*      P R E N U T
+*     - - - - - - -
+*
+*  Form the matrix of precession and nutation (IAU1976/FK5)
+*  (double precision)
+*
+*  Given:
+*     EPOCH   dp         Julian Epoch for mean coordinates
+*     DATE    dp         Modified Julian Date (JD-2400000.5)
+*                        for true coordinates
+*
+*  Returned:
+*     RMATPN  dp(3,3)    combined precession/nutation matrix
+*
+*  Called:  sla_PREC, sla_EPJ, sla_NUT, sla_DMXM
+*
+*  Notes:
+*
+*  1)  The epoch and date are TDB (loosely ET).
+*
+*  2)  The matrix is in the sense   V(true)  =  RMATPN * V(mean)
+*
+*  P.T.Wallace   Starlink   April 1987
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION EPOCH,DATE,RMATPN(3,3)
+
+      DOUBLE PRECISION RMATP(3,3),RMATN(3,3),sla_EPJ
+
+
+
+*  Precession
+      CALL sla_PREC(EPOCH,sla_EPJ(DATE),RMATP)
+
+*  Nutation
+      CALL sla_NUT(DATE,RMATN)
+
+*  Combine the matrices:  PN = N x P
+      CALL sla_DMXM(RMATN,RMATP,RMATPN)
+
+      END
diff --git a/src/slalib/put.com b/src/slalib/put.com
new file mode 100755
index 0000000..fc42fe8
--- /dev/null
+++ b/src/slalib/put.com
@@ -0,0 +1,38 @@
+$!
+$!  - - - -
+$!   P U T
+$!  - - - -
+$!
+$!  Update one SLALIB routine from Fortran source
+$!
+$!  DCL command is @PUT file
+$!
+$!  The default directory must be the one containing the
+$!  Fortran source, with the libraries in [.RELEASE].
+$!
+$!  P T Wallace   Starlink   22 January 1993
+$!
+$!  Save supplied file name and strip recognized extensions
+$     FILE=''P1''
+$     P1=P1-".FOR"-".VAX"
+$!
+$!  No action required for TEST program
+      IF P1.EQS."TEST" THEN $ GOTO DONE
+$!
+$!  If platform-specific module, make .FOR file ...
+$     IF F$SEARCH("''P1'.VAX").NES."" THEN $ COPY 'P1'.VAX *.FOR
+$!
+$!  Update the source library
+$     LIBR/REPL/TEXT [.RELEASE]SLALIB.TLB 'P1'.FOR
+$!
+$!  Compile, update object library, delete object
+$     FORTRAN/NOLIST 'P1'.FOR
+$     LIBR/REPL [.RELEASE]SLALIB.OLB 'P1'.OBJ
+$     DELETE 'P1'.OBJ;*
+$!
+$!  If module just updated was platform-specific, delete the .FOR version
+$     IF F$SEARCH("''P1'.VAX",1).NES."" THEN $ DELETE 'P1'.FOR;*
+$!
+$!  Finished
+$DONE:
+$     EXIT
diff --git a/src/slalib/pv2el.f b/src/slalib/pv2el.f
new file mode 100644
index 0000000..e45ad64
--- /dev/null
+++ b/src/slalib/pv2el.f
@@ -0,0 +1,351 @@
+      SUBROUTINE sla_PV2EL (PV, DATE, PMASS, JFORMR,
+     :                      JFORM, EPOCH, ORBINC, ANODE, PERIH,
+     :                      AORQ, E, AORL, DM, JSTAT)
+*+
+*     - - - - - -
+*      P V 2 E L
+*     - - - - - -
+*
+*  Heliocentric osculating elements obtained from instantaneous position
+*  and velocity.
+*
+*  Given:
+*     PV        d(6)   heliocentric x,y,z,xdot,ydot,zdot of date,
+*                      J2000 equatorial triad (AU,AU/s; Note 1)
+*     DATE      d      date (TT Modified Julian Date = JD-2400000.5)
+*     PMASS     d      mass of the planet (Sun=1; Note 2)
+*     JFORMR    i      requested element set (1-3; Note 3)
+*
+*  Returned:
+*     JFORM     d      element set actually returned (1-3; Note 4)
+*     EPOCH     d      epoch of elements (TT MJD)
+*     ORBINC    d      inclination (radians)
+*     ANODE     d      longitude of the ascending node (radians)
+*     PERIH     d      longitude or argument of perihelion (radians)
+*     AORQ      d      mean distance or perihelion distance (AU)
+*     E         d      eccentricity
+*     AORL      d      mean anomaly or longitude (radians, JFORM=1,2 only)
+*     DM        d      daily motion (radians, JFORM=1 only)
+*     JSTAT     i      status:  0 = OK
+*                              -1 = illegal PMASS
+*                              -2 = illegal JFORMR
+*                              -3 = position/velocity out of range
+*
+*  Notes
+*
+*  1  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.
+*
+*  2  The mass, PMASS, is important only for the larger planets.  For
+*     most purposes (e.g. asteroids) use 0D0.  Values less than zero
+*     are illegal.
+*
+*  3  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
+*
+*  4  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
+*
+*  5  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
+*
+*  6  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.
+*
+*  Reference:  Sterne, Theodore E., "An Introduction to Celestial
+*              Mechanics", Interscience Publishers, 1960
+*
+*  Called:  sla_DRANRM
+*
+*  P.T.Wallace   Starlink   13 February 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION PV(6),DATE,PMASS
+      INTEGER JFORMR,JFORM
+      DOUBLE PRECISION EPOCH,ORBINC,ANODE,PERIH,AORQ,E,AORL,DM
+      INTEGER JSTAT
+
+*  Seconds to days
+      DOUBLE PRECISION DAY
+      PARAMETER (DAY=86400D0)
+
+*  Gaussian gravitational constant (exact)
+      DOUBLE PRECISION GCON
+      PARAMETER (GCON=0.01720209895D0)
+
+*  Sin and cos of J2000 mean obliquity (IAU 1976)
+      DOUBLE PRECISION SE,CE
+      PARAMETER (SE=0.3977771559319137D0,
+     :           CE=0.9174820620691818D0)
+
+*  Minimum allowed distance (AU) and speed (AU/day)
+      DOUBLE PRECISION RMIN,VMIN
+      PARAMETER (RMIN=1D-3,VMIN=1D-8)
+
+*  How close to unity the eccentricity has to be to call it a parabola
+      DOUBLE PRECISION PARAB
+      PARAMETER (PARAB=1D-8)
+
+      DOUBLE PRECISION 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
+
+      INTEGER JF
+
+      DOUBLE PRECISION sla_DRANRM
+
+
+*  Validate arguments PMASS and JFORMR.
+      IF (PMASS.LT.0D0) THEN
+         JSTAT = -1
+         GO TO 999
+      END IF
+      IF (JFORMR.LT.1.OR.JFORMR.GT.3) THEN
+         JSTAT = -2
+         GO TO 999
+      END IF
+
+*  Provisionally assume the elements will be in the chosen form.
+      JF = JFORMR
+
+*  Rotate the position from equatorial to ecliptic coordinates.
+      X = PV(1)
+      Y = PV(2)*CE+PV(3)*SE
+      Z = -PV(2)*SE+PV(3)*CE
+
+*  Rotate the velocity similarly, scaling to AU/day.
+      XD = DAY*PV(4)
+      YD = DAY*(PV(5)*CE+PV(6)*SE)
+      ZD = DAY*(-PV(5)*SE+PV(6)*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.LT.RMIN.OR.V.LT.VMIN) THEN
+         JSTAT = -3
+         GO TO 999
+      END IF
+
+*  R dot V.
+      RDV = X*XD+Y*YD+Z*ZD
+
+*  Mu.
+      GMU = (1D0+PMASS)*GCON*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.NE.0D0.OR.HY.NE.0D0) THEN
+         BIGOM = ATAN2(HX,-HY)
+      ELSE
+         BIGOM=0D0
+      END IF
+
+*  Reciprocal of mean distance etc.
+      AR = 2D0/R-V2/GMU
+
+*  Eccentricity.
+      ECC = SQRT(MAX(1D0-AR*H2/GMU,0D0))
+
+*  True anomaly.
+      S = H*RDV
+      C = H2-R*GMU
+      IF (S.NE.0D0.AND.C.NE.0D0) THEN
+         AT = ATAN2(S,C)
+      ELSE
+         AT = 0D0
+      END IF
+
+*  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 (ABS(ECC-1D0).LT.PARAB) ECC=1D0
+
+*  Comply with JFORMR = 1 or 2 only if orbit is elliptical.
+      IF (ECC.GE.1D0) JF=3
+
+*  Functions.
+      GAR3 = GMU*AR*AR*AR
+      EM1 = ECC-1D0
+      EP1 = ECC+1D0
+      HAT = AT/2D0
+      SHAT = SIN(HAT)
+      CHAT = COS(HAT)
+
+*  Ellipse?
+      IF (ECC.LT.1D0 ) THEN
+
+*     Eccentric anomaly.
+         AE = 2D0*ATAN2(SQRT(-EM1)*SHAT,SQRT(EP1)*CHAT)
+
+*     Mean anomaly.
+         AM = AE-ECC*SIN(AE)
+
+*     Daily motion.
+         DN = SQRT(GAR3)
+      END IF
+
+*  "Major planet" element set?
+      IF (JF.EQ.1) THEN
+
+*     Longitude of perihelion.
+         PL = BIGOM+OM
+
+*     Longitude at epoch.
+         EL = PL+AM
+      END IF
+
+*  "Comet" element set?
+      IF (JF.EQ.3) THEN
+
+*     Perihelion distance.
+         Q = H2/(GMU*EP1)
+
+*     Ellipse, parabola, hyperbola?
+         IF (ECC.LT.1D0) THEN
+
+*        Ellipse: epoch of perihelion.
+            TP = DATE-AM/DN
+         ELSE
+
+*        Parabola or hyperbola: evaluate tan ( ( true anomaly ) / 2 )
+            THAT = SHAT/CHAT
+            IF (ECC.EQ.1D0) THEN
+
+*           Parabola: epoch of perihelion.
+               TP = DATE-THAT*(1D0+THAT*THAT/3D0)*H*H2/(2D0*GMU*GMU)
+            ELSE
+
+*           Hyperbola: epoch of perihelion.
+               THHF = SQRT(EM1/EP1)*THAT
+               F = LOG(1D0+THHF)-LOG(1D0-THHF)
+               TP = DATE-(ECC*SINH(F)-F)/SQRT(-GAR3)
+            END IF
+         END IF
+      END IF
+
+*  Return the appropriate set of elements.
+      JFORM = JF
+      ORBINC = OI
+      ANODE = sla_DRANRM(BIGOM)
+      E = ECC
+      IF (JF.EQ.1) THEN
+         PERIH = sla_DRANRM(PL)
+         AORL = sla_DRANRM(EL)
+         DM = DN
+      ELSE
+         PERIH = sla_DRANRM(OM)
+         IF (JF.EQ.2) AORL = sla_DRANRM(AM)
+      END IF
+      IF (JF.NE.3) THEN
+         EPOCH = DATE
+         AORQ = 1D0/AR
+      ELSE
+         EPOCH = TP
+         AORQ = Q
+      END IF
+      JSTAT = 0
+
+ 999  CONTINUE
+      END
diff --git a/src/slalib/pv2ue.f b/src/slalib/pv2ue.f
new file mode 100644
index 0000000..de141e3
--- /dev/null
+++ b/src/slalib/pv2ue.f
@@ -0,0 +1,150 @@
+      SUBROUTINE sla_PV2UE (PV, DATE, PMASS, U, JSTAT)
+*+
+*     - - - - - -
+*      P V 2 U E
+*     - - - - - -
+*
+*  Construct a universal element set based on an instantaneous position
+*  and velocity.
+*
+*  Given:
+*     PV        d(6)   heliocentric x,y,z,xdot,ydot,zdot of date,
+*                      (AU,AU/s; Note 1)
+*     DATE      d      date (TT Modified Julian Date = JD-2400000.5)
+*     PMASS     d      mass of the planet (Sun=1; Note 2)
+*
+*  Returned:
+*     U         d(13)  universal orbital elements (Note 3)
+*
+*                 (1)  combined mass (M+m)
+*                 (2)  total energy of the orbit (alpha)
+*                 (3)  reference (osculating) epoch (t0)
+*               (4-6)  position at reference epoch (r0)
+*               (7-9)  velocity at reference epoch (v0)
+*                (10)  heliocentric distance at reference epoch
+*                (11)  r0.v0
+*                (12)  date (t)
+*                (13)  universal eccentric anomaly (psi) of date, approx
+*
+*     JSTAT     i      status:  0 = OK
+*                              -1 = illegal PMASS
+*                              -2 = too close to Sun
+*                              -3 = too slow
+*
+*  Notes
+*
+*  1  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.
+*
+*  2  The mass, PMASS, is important only for the larger planets.  For
+*     most purposes (e.g. asteroids) use 0D0.  Values less than zero
+*     are illegal.
+*
+*  3  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.
+*
+*  P.T.Wallace   Starlink   18 March 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION PV(6),DATE,PMASS,U(13)
+      INTEGER JSTAT
+
+*  Gaussian gravitational constant (exact)
+      DOUBLE PRECISION GCON
+      PARAMETER (GCON=0.01720209895D0)
+
+*  Canonical days to seconds
+      DOUBLE PRECISION CD2S
+      PARAMETER (CD2S=GCON/86400D0)
+
+*  Minimum allowed distance (AU) and speed (AU per canonical day)
+      DOUBLE PRECISION RMIN,VMIN
+      PARAMETER (RMIN=1D-3,VMIN=1D-3)
+
+      DOUBLE PRECISION T0,CM,X,Y,Z,XD,YD,ZD,R,V2,V,ALPHA,RDV
+
+
+*  Reference epoch.
+      T0 = DATE
+
+*  Combined mass (mu=M+m).
+      IF (PMASS.LT.0D0) GO TO 9010
+      CM = 1D0+PMASS
+
+*  Unpack the state vector, expressing velocity in AU per canonical day.
+      X = PV(1)
+      Y = PV(2)
+      Z = PV(3)
+      XD = PV(4)/CD2S
+      YD = PV(5)/CD2S
+      ZD = PV(6)/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.LT.RMIN) GO TO 9020
+      IF (V.LT.VMIN) GO TO 9030
+
+*  Total energy of the orbit.
+      ALPHA = V2-2D0*CM/R
+
+*  Outward component of velocity.
+      RDV = X*XD+Y*YD+Z*ZD
+
+*  Construct the universal-element set.
+      U(1) = CM
+      U(2) = ALPHA
+      U(3) = T0
+      U(4) = X
+      U(5) = Y
+      U(6) = Z
+      U(7) = XD
+      U(8) = YD
+      U(9) = ZD
+      U(10) = R
+      U(11) = RDV
+      U(12) = T0
+      U(13) = 0D0
+
+*  Exit.
+      JSTAT = 0
+      GO TO 9999
+
+*  Negative PMASS.
+ 9010 CONTINUE
+      JSTAT = -1
+      GO TO 9999
+
+*  Too close.
+ 9020 CONTINUE
+      JSTAT = -2
+      GO TO 9999
+
+*  Too slow.
+ 9030 CONTINUE
+      JSTAT = -3
+
+ 9999 CONTINUE
+      END
diff --git a/src/slalib/pvobs.f b/src/slalib/pvobs.f
new file mode 100644
index 0000000..116bc06
--- /dev/null
+++ b/src/slalib/pvobs.f
@@ -0,0 +1,59 @@
+      SUBROUTINE sla_PVOBS (P, H, STL, PV)
+*+
+*     - - - - - -
+*      P V O B S
+*     - - - - - -
+*
+*  Position and velocity of an observing station (double precision)
+*
+*  Given:
+*     P     dp     latitude (geodetic, radians)
+*     H     dp     height above reference spheroid (geodetic, metres)
+*     STL   dp     local apparent sidereal time (radians)
+*
+*  Returned:
+*     PV    dp(6)  position/velocity 6-vector (AU, AU/s, true equator
+*                                              and equinox of date)
+*
+*  Called:  sla_GEOC
+*
+*  IAU 1976 constants are used.
+*
+*  P.T.Wallace   Starlink   14 November 1994
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION P,H,STL,PV(6)
+
+      DOUBLE PRECISION R,Z,S,C,V
+
+*  Mean sidereal rate (at J2000) in radians per (UT1) second
+      DOUBLE PRECISION SR
+      PARAMETER (SR=7.292115855306589D-5)
+
+
+
+*  Geodetic to geocentric conversion
+      CALL sla_GEOC(P,H,R,Z)
+
+*  Functions of ST
+      S=SIN(STL)
+      C=COS(STL)
+
+*  Speed
+      V=SR*R
+
+*  Position
+      PV(1)=R*C
+      PV(2)=R*S
+      PV(3)=Z
+
+*  Velocity
+      PV(4)=-V*S
+      PV(5)=V*C
+      PV(6)=0D0
+
+      END
diff --git a/src/slalib/pxy.f b/src/slalib/pxy.f
new file mode 100644
index 0000000..3dd880f
--- /dev/null
+++ b/src/slalib/pxy.f
@@ -0,0 +1,92 @@
+      SUBROUTINE sla_PXY (NP,XYE,XYM,COEFFS,XYP,XRMS,YRMS,RRMS)
+*+
+*     - - - -
+*      P X Y
+*     - - - -
+*
+*  Given arrays of "expected" and "measured" [X,Y] coordinates, and a
+*  linear model relating them (as produced by sla_FITXY), compute
+*  the array of "predicted" coordinates and the RMS residuals.
+*
+*  Given:
+*     NP       i        number of samples
+*     XYE     d(2,np)   expected [X,Y] for each sample
+*     XYM     d(2,np)   measured [X,Y] for each sample
+*     COEFFS  d(6)      coefficients of model (see below)
+*
+*  Returned:
+*     XYP     d(2,np)   predicted [X,Y] for each sample
+*     XRMS     d        RMS in X
+*     YRMS     d        RMS in Y
+*     RRMS     d        total RMS (vector sum of XRMS and YRMS)
+*
+*  The model is supplied in the array COEFFS.  Naming the
+*  elements of COEFF as follows:
+*
+*     COEFFS(1) = A
+*     COEFFS(2) = B
+*     COEFFS(3) = C
+*     COEFFS(4) = D
+*     COEFFS(5) = E
+*     COEFFS(6) = F
+*
+*  the model is applied thus:
+*
+*     XP = A + B*XM + C*YM
+*     YP = D + E*XM + F*YM
+*
+*  The residuals are (XP-XE) and (YP-YE).
+*
+*  If NP is less than or equal to zero, no coordinates are
+*  transformed, and the RMS residuals are all zero.
+*
+*  See also sla_FITXY, sla_INVF, sla_XY2XY, sla_DCMPF
+*
+*  Called:  sla_XY2XY
+*
+*  P.T.Wallace   Starlink   22 May 1996
+*
+*  Copyright (C) 1996 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER NP
+      DOUBLE PRECISION XYE(2,NP),XYM(2,NP),COEFFS(6),
+     :                 XYP(2,NP),XRMS,YRMS,RRMS
+
+      INTEGER I
+      DOUBLE PRECISION SDX2,SDY2,XP,YP,DX,DY,DX2,DY2,P
+
+
+
+*  Initialize summations
+      SDX2=0D0
+      SDY2=0D0
+
+*  Loop by sample
+      DO I=1,NP
+
+*     Transform "measured" [X,Y] to "predicted" [X,Y]
+         CALL sla_XY2XY(XYM(1,I),XYM(2,I),COEFFS,XP,YP)
+         XYP(1,I)=XP
+         XYP(2,I)=YP
+
+*     Compute residuals in X and Y, and update summations
+         DX=XYE(1,I)-XP
+         DY=XYE(2,I)-YP
+         DX2=DX*DX
+         DY2=DY*DY
+         SDX2=SDX2+DX2
+         SDY2=SDY2+DY2
+
+*     Next sample
+      END DO
+
+*  Compute RMS values
+      P=MAX(1D0,DBLE(NP))
+      XRMS=SQRT(SDX2/P)
+      YRMS=SQRT(SDY2/P)
+      RRMS=SQRT(XRMS*XRMS+YRMS*YRMS)
+
+      END
diff --git a/src/slalib/random.f_alpha_OSF1 b/src/slalib/random.f_alpha_OSF1
new file mode 100644
index 0000000..54544e3
--- /dev/null
+++ b/src/slalib/random.f_alpha_OSF1
@@ -0,0 +1,56 @@
+      REAL FUNCTION sla_RANDOM (SEED)
+*+
+*     - - - - - - -
+*      R A N D O M
+*     - - - - - - -
+*
+*  Generate pseudo-random real number in the range 0 <= X < 1.
+*  (single precision)
+*
+*  !!!  Version for Alpha/OSF1 !!!
+*
+*  Given:
+*     SEED     real     an arbitrary real number
+*
+*  Notes:
+*
+*  1)  The result is a pseudo-random REAL number in the range
+*      0 <= sla_RANDOM < 1.
+*
+*  2)  SEED is used first time through only.
+*
+*  Called:  RANDOM (a REAL function from the DEC Fortran Library)
+*
+*  P.T.Wallace   Starlink   14 October 1991
+*    Revised for new recommended RTL RANDOM(3f) function.
+*  B.K.McIlwrath Starlink   12 January 1996
+*-
+
+      IMPLICIT NONE
+
+      REAL SEED
+
+      REAL RANDOM
+
+      REAL AS
+      INTEGER ISEED
+      LOGICAL FIRST
+      SAVE FIRST
+      DATA FIRST /.TRUE./
+
+
+
+*  If first time, turn SEED into a large, odd integer
+      IF (FIRST) THEN
+         AS=ABS(SEED)+1.0
+         ISEED=NINT(AS/10.0**(NINT(ALOG10(AS))-6))
+         IF (MOD(ISEED,2).EQ.0) ISEED=ISEED+1
+         FIRST=.FALSE.
+      ELSE
+         ISEED = 0
+      END IF
+
+*  Next pseudo-random number
+      sla_RANDOM=RANDOM(ISEED)
+
+      END
diff --git a/src/slalib/random.f_convex b/src/slalib/random.f_convex
new file mode 100644
index 0000000..336983f
--- /dev/null
+++ b/src/slalib/random.f_convex
@@ -0,0 +1,56 @@
+      REAL FUNCTION sla_RANDOM (SEED)
+*+
+*     - - - - - - -
+*      R A N D O M
+*     - - - - - - -
+*
+*  Generate pseudo-random real number in the range 0 <= X < 1.
+*  (single precision)
+*
+*  !!! Convex dependent !!!
+*
+*  Given:
+*     SEED     real     an arbitrary real number
+*
+*  Notes:
+*
+*  1)  The result is a pseudo-random REAL number in the range
+*      0 <= sla_RANDOM < 1.
+*
+*  2)  SEED is used first time through only.
+*
+*  Called:  RAND (a REAL function from the Convex Fortran Library)
+*
+*  P.T.Wallace   Starlink   28 June 1994
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL SEED
+
+      REAL RAND
+
+      REAL AS
+      INTEGER ISEED
+      LOGICAL FIRST
+      SAVE FIRST
+      DATA FIRST /.TRUE./
+
+
+
+*  If first time, turn SEED into a large, odd integer, and start the
+*  generator
+      IF (FIRST) THEN
+         AS=ABS(SEED)+1.0
+         ISEED=NINT(AS/10.0**(NINT(ALOG10(AS))-6))
+         IF (MOD(ISEED,2).EQ.0) ISEED=ISEED+1
+         FIRST=.FALSE.
+         AS=RAND(ISEED)
+      END IF
+
+*  Next pseudo-random number
+      sla_RANDOM=RAND(0)
+
+      END
diff --git a/src/slalib/random.f_ix86_Linux b/src/slalib/random.f_ix86_Linux
new file mode 100644
index 0000000..acd1047
--- /dev/null
+++ b/src/slalib/random.f_ix86_Linux
@@ -0,0 +1,54 @@
+      REAL FUNCTION sla_RANDOM (SEED)
+*+
+*     - - - - - - -
+*      R A N D O M
+*     - - - - - - -
+*
+*  Generate pseudo-random real number in the range 0 <= X < 1.
+*  (single precision)
+*
+*  !!!  Version for Linux !!!
+*
+*  Given:
+*     SEED     real     an arbitrary real number
+*
+*  Notes:
+*
+*  1)  The result is a pseudo-random REAL number in the range
+*      0 <= sla_RANDOM < 1.
+*
+*  2)  SEED is used first time through only.
+*
+*  Called:  RANDOM (a REAL function compiled by the makefile from rtl_random.c)
+*
+*  B.K.McIlwrath Starlink   12 January 1996
+*-
+
+      IMPLICIT NONE
+
+      REAL SEED
+
+      REAL RANDOM
+
+      REAL AS
+      INTEGER ISEED
+      LOGICAL FIRST
+      SAVE FIRST
+      DATA FIRST /.TRUE./
+
+
+
+*  If first time, turn SEED into a large, odd integer
+      IF (FIRST) THEN
+         AS=ABS(SEED)+1.0
+         ISEED=NINT(AS/10.0**(NINT(ALOG10(AS))-6))
+         IF (MOD(ISEED,2).EQ.0) ISEED=ISEED+1
+         FIRST=.FALSE.
+      ELSE
+         ISEED = 0
+      END IF
+
+*  Next pseudo-random number
+      sla_RANDOM=RANDOM(ISEED)
+
+      END
diff --git a/src/slalib/random.f_mips b/src/slalib/random.f_mips
new file mode 100644
index 0000000..b82b1bb
--- /dev/null
+++ b/src/slalib/random.f_mips
@@ -0,0 +1,54 @@
+      REAL FUNCTION sla_RANDOM (SEED)
+*+
+*     - - - - - - -
+*      R A N D O M
+*     - - - - - - -
+*
+*  Generate pseudo-random real number in the range 0 <= X < 1.
+*  (single precision)
+*
+*  !!!  Version for VAX/VMS and DECstation !!!
+*
+*  Given:
+*     SEED     real     an arbitrary real number
+*
+*  Notes:
+*
+*  1)  The result is a pseudo-random REAL number in the range
+*      0 <= sla_RANDOM < 1.
+*
+*  2)  SEED is used first time through only.
+*
+*  Called:  RAN (a REAL function from the DEC Fortran Library)
+*
+*  P.T.Wallace   Starlink   14 October 1991
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL SEED
+
+      REAL RAN
+
+      REAL AS
+      INTEGER ISEED
+      LOGICAL FIRST
+      SAVE FIRST
+      DATA FIRST /.TRUE./
+
+
+
+*  If first time, turn SEED into a large, odd integer
+      IF (FIRST) THEN
+         AS=ABS(SEED)+1.0
+         ISEED=NINT(AS/10.0**(NINT(ALOG10(AS))-6))
+         IF (MOD(ISEED,2).EQ.0) ISEED=ISEED+1
+         FIRST=.FALSE.
+      END IF
+
+*  Next pseudo-random number
+      sla_RANDOM=RAN(ISEED)
+
+      END
diff --git a/src/slalib/random.f_pcm b/src/slalib/random.f_pcm
new file mode 100644
index 0000000..4f96ddb
--- /dev/null
+++ b/src/slalib/random.f_pcm
@@ -0,0 +1,42 @@
+      REAL FUNCTION sla_RANDOM (XSEED)
+*+
+*     - - - - - - -
+*      R A N D O M
+*     - - - - - - -
+*
+*  Generate pseudo-random real number in the range 0 <= X < 1.
+*
+*  (single precision)
+*
+*  !!!  Microsoft Fortran dependent  !!!
+*
+*  Given (but used first time only):
+*     XSEED    real     an arbitrary real number
+*
+*  The value returned is a pseudo-random number such that
+*  0 <= sla_RANDOM < 1.
+*
+*  Called:  RANDOM (Microsoft run-time library)
+*
+*  P.T.Wallace   Starlink   28 February 1993
+*
+*+
+
+      IMPLICIT NONE
+
+      REAL XSEED
+
+      REAL X
+      LOGICAL FIRST
+      SAVE FIRST
+      DATA FIRST /.TRUE./
+
+
+      IF (FIRST) THEN
+         CALL SEED(NINT(MOD(XSEED*1.234E7,32E3)))  ! Microsoft Fortran
+         FIRST=.FALSE.
+      END IF
+      CALL RANDOM(X)                               ! Microsoft Fortran
+      sla_RANDOM=X
+
+      END
diff --git a/src/slalib/random.f_sun4 b/src/slalib/random.f_sun4
new file mode 100644
index 0000000..9f49fb6
--- /dev/null
+++ b/src/slalib/random.f_sun4
@@ -0,0 +1,56 @@
+      REAL FUNCTION sla_RANDOM (SEED)
+*+
+*     - - - - - - -
+*      R A N D O M
+*     - - - - - - -
+*
+*  Generate pseudo-random real number in the range 0 <= X < 1.
+*  (single precision)
+*
+*  !!! Sun 4 dependent !!!
+*
+*  Given:
+*     SEED     real     an arbitrary real number
+*
+*  Notes:
+*
+*  1)  The result is a pseudo-random REAL number in the range
+*      0 <= sla_RANDOM < 1.
+*
+*  2)  SEED is used first time through only.
+*
+*  Called:  RAND (a REAL function from the Sun Fortran Library)
+*
+*  P.T.Wallace   Starlink   14 October 1991
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL SEED
+
+      REAL RAND
+
+      REAL AS
+      INTEGER ISEED
+      LOGICAL FIRST
+      SAVE FIRST
+      DATA FIRST /.TRUE./
+
+
+
+*  If first time, turn SEED into a large, odd integer, and start the
+*  generator
+      IF (FIRST) THEN
+         AS=ABS(SEED)+1.0
+         ISEED=NINT(AS/10.0**(NINT(ALOG10(AS))-6))
+         IF (MOD(ISEED,2).EQ.0) ISEED=ISEED+1
+         FIRST=.FALSE.
+         AS=RAND(ISEED)
+      END IF
+
+*  Next pseudo-random number
+      sla_RANDOM=RAND(0)
+
+      END
diff --git a/src/slalib/random.f_sun4_Solaris b/src/slalib/random.f_sun4_Solaris
new file mode 100644
index 0000000..9f49fb6
--- /dev/null
+++ b/src/slalib/random.f_sun4_Solaris
@@ -0,0 +1,56 @@
+      REAL FUNCTION sla_RANDOM (SEED)
+*+
+*     - - - - - - -
+*      R A N D O M
+*     - - - - - - -
+*
+*  Generate pseudo-random real number in the range 0 <= X < 1.
+*  (single precision)
+*
+*  !!! Sun 4 dependent !!!
+*
+*  Given:
+*     SEED     real     an arbitrary real number
+*
+*  Notes:
+*
+*  1)  The result is a pseudo-random REAL number in the range
+*      0 <= sla_RANDOM < 1.
+*
+*  2)  SEED is used first time through only.
+*
+*  Called:  RAND (a REAL function from the Sun Fortran Library)
+*
+*  P.T.Wallace   Starlink   14 October 1991
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL SEED
+
+      REAL RAND
+
+      REAL AS
+      INTEGER ISEED
+      LOGICAL FIRST
+      SAVE FIRST
+      DATA FIRST /.TRUE./
+
+
+
+*  If first time, turn SEED into a large, odd integer, and start the
+*  generator
+      IF (FIRST) THEN
+         AS=ABS(SEED)+1.0
+         ISEED=NINT(AS/10.0**(NINT(ALOG10(AS))-6))
+         IF (MOD(ISEED,2).EQ.0) ISEED=ISEED+1
+         FIRST=.FALSE.
+         AS=RAND(ISEED)
+      END IF
+
+*  Next pseudo-random number
+      sla_RANDOM=RAND(0)
+
+      END
diff --git a/src/slalib/random.f_vax b/src/slalib/random.f_vax
new file mode 100644
index 0000000..bdf9ffe
--- /dev/null
+++ b/src/slalib/random.f_vax
@@ -0,0 +1,52 @@
+      REAL FUNCTION sla_RANDOM (SEED)
+*+
+*     - - - - - - -
+*      R A N D O M
+*     - - - - - - -
+*
+*  Generate pseudo-random real number in the range 0 <= X < 1.
+*  (single precision)
+*
+*  !!!  Version for VAX/VMS and DECstation !!!
+*
+*  Given:
+*     SEED     real     an arbitrary real number
+*
+*  Notes:
+*
+*  1)  The result is a pseudo-random REAL number in the range
+*      0 <= sla_RANDOM < 1.
+*
+*  2)  SEED is used first time through only.
+*
+*  Called:  RAN (a REAL function from the DEC Fortran Library)
+*
+*  P.T.Wallace   Starlink   14 October 1991
+*-
+
+      IMPLICIT NONE
+
+      REAL SEED
+
+      REAL RAN
+
+      REAL AS
+      INTEGER ISEED
+      LOGICAL FIRST
+      SAVE FIRST
+      DATA FIRST /.TRUE./
+
+
+
+*  If first time, turn SEED into a large, odd integer
+      IF (FIRST) THEN
+         AS=ABS(SEED)+1.0
+         ISEED=NINT(AS/10.0**(NINT(ALOG10(AS))-6))
+         IF (MOD(ISEED,2).EQ.0) ISEED=ISEED+1
+         FIRST=.FALSE.
+      END IF
+
+*  Next pseudo-random number
+      sla_RANDOM=RAN(ISEED)
+
+      END
diff --git a/src/slalib/random.f_x86_64 b/src/slalib/random.f_x86_64
new file mode 100644
index 0000000..acd1047
--- /dev/null
+++ b/src/slalib/random.f_x86_64
@@ -0,0 +1,54 @@
+      REAL FUNCTION sla_RANDOM (SEED)
+*+
+*     - - - - - - -
+*      R A N D O M
+*     - - - - - - -
+*
+*  Generate pseudo-random real number in the range 0 <= X < 1.
+*  (single precision)
+*
+*  !!!  Version for Linux !!!
+*
+*  Given:
+*     SEED     real     an arbitrary real number
+*
+*  Notes:
+*
+*  1)  The result is a pseudo-random REAL number in the range
+*      0 <= sla_RANDOM < 1.
+*
+*  2)  SEED is used first time through only.
+*
+*  Called:  RANDOM (a REAL function compiled by the makefile from rtl_random.c)
+*
+*  B.K.McIlwrath Starlink   12 January 1996
+*-
+
+      IMPLICIT NONE
+
+      REAL SEED
+
+      REAL RANDOM
+
+      REAL AS
+      INTEGER ISEED
+      LOGICAL FIRST
+      SAVE FIRST
+      DATA FIRST /.TRUE./
+
+
+
+*  If first time, turn SEED into a large, odd integer
+      IF (FIRST) THEN
+         AS=ABS(SEED)+1.0
+         ISEED=NINT(AS/10.0**(NINT(ALOG10(AS))-6))
+         IF (MOD(ISEED,2).EQ.0) ISEED=ISEED+1
+         FIRST=.FALSE.
+      ELSE
+         ISEED = 0
+      END IF
+
+*  Next pseudo-random number
+      sla_RANDOM=RANDOM(ISEED)
+
+      END
diff --git a/src/slalib/range.f b/src/slalib/range.f
new file mode 100644
index 0000000..a3684cb
--- /dev/null
+++ b/src/slalib/range.f
@@ -0,0 +1,33 @@
+      REAL FUNCTION sla_RANGE (ANGLE)
+*+
+*     - - - - - -
+*      R A N G E
+*     - - - - - -
+*
+*  Normalize angle into range +/- pi  (single precision)
+*
+*  Given:
+*     ANGLE     dp      the angle in radians
+*
+*  The result is ANGLE expressed in the +/- pi (single
+*  precision).
+*
+*  P.T.Wallace   Starlink   23 November 1995
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL ANGLE
+
+      REAL API,A2PI
+      PARAMETER (API=3.141592653589793238462643)
+      PARAMETER (A2PI=6.283185307179586476925287)
+
+
+      sla_RANGE=MOD(ANGLE,A2PI)
+      IF (ABS(sla_RANGE).GE.API)
+     :          sla_RANGE=sla_RANGE-SIGN(A2PI,ANGLE)
+
+      END
diff --git a/src/slalib/ranorm.f b/src/slalib/ranorm.f
new file mode 100644
index 0000000..c2e32a5
--- /dev/null
+++ b/src/slalib/ranorm.f
@@ -0,0 +1,31 @@
+      REAL FUNCTION sla_RANORM (ANGLE)
+*+
+*     - - - - - - -
+*      R A N O R M
+*     - - - - - - -
+*
+*  Normalize angle into range 0-2 pi  (single precision)
+*
+*  Given:
+*     ANGLE     dp      the angle in radians
+*
+*  The result is ANGLE expressed in the range 0-2 pi (single
+*  precision).
+*
+*  P.T.Wallace   Starlink   23 November 1995
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL ANGLE
+
+      REAL A2PI
+      PARAMETER (A2PI=6.283185307179586476925287)
+
+
+      sla_RANORM=MOD(ANGLE,A2PI)
+      IF (sla_RANORM.LT.0.0) sla_RANORM=sla_RANORM+A2PI
+
+      END
diff --git a/src/slalib/rcc.f b/src/slalib/rcc.f
new file mode 100644
index 0000000..74a8874
--- /dev/null
+++ b/src/slalib/rcc.f
@@ -0,0 +1,1063 @@
+      DOUBLE PRECISION FUNCTION sla_RCC (TDB, UT1, WL, U, V)
+*+
+*     - - - -
+*      R C C
+*     - - - -
+*
+*  Relativistic clock correction:  the difference between proper time at
+*  a point on the surface of the Earth and coordinate time in the Solar
+*  System barycentric space-time frame of reference.
+*
+*  The proper time is Terrestrial Time TT;  the coordinate
+*  time is an implementation of the Barycentric Dynamical Time TDB.
+*
+*  Given:
+*    TDB   dp   coordinate time (MJD: JD-2400000.5)
+*    UT1   dp   universal time (fraction of one day)
+*    WL    dp   clock longitude (radians west)
+*    U     dp   clock distance from Earth spin axis (km)
+*    V     dp   clock distance north of Earth equatorial plane (km)
+*
+*  Returned:
+*    The clock correction, TDB-TT, in seconds.  TDB may be considered
+*    to be the coordinate time in the Solar System barycentre frame of
+*    reference, and TT is the proper time given by clocks at mean sea
+*    level on the Earth.
+*
+*    The result has a main (annual) sinusoidal term of amplitude
+*    approximately 0.00166 seconds, plus planetary terms up to about
+*    20 microseconds, and lunar and diurnal terms up to 2 microseconds.
+*    The variation arises from the transverse Doppler effect and the
+*    gravitational red-shift as the observer varies in speed and moves
+*    through different gravitational potentials.
+*
+*  The argument TDB is, strictly, the barycentric coordinate time;
+*  however, the terrestrial proper time (TT) can in practice be used.
+*
+*  The geocentric model is that of Fairhead & Bretagnon (1990), in its
+*  full form.  It was supplied by Fairhead (private communication) as a
+*  FORTRAN subroutine.  The original Fairhead routine used explicit
+*  formulae, in such large numbers that problems were experienced with
+*  certain compilers (Microsoft Fortran on PC aborted with stack
+*  overflow, Convex compiled successfully but extremely slowly).  The
+*  present implementation is a complete recoding, with the original
+*  Fairhead coefficients held in a table.  To optimise arithmetic
+*  precision, the terms are accumulated in reverse order, smallest
+*  first.  A number of other coding changes were made, in order to match
+*  the calling sequence of previous versions of the present routine, and
+*  to comply with Starlink programming standards.  Under VAX/VMS, the
+*  numerical results compared with those from the Fairhead form are
+*  essentially unaffected by the changes, the differences being at the
+*  10^-20 sec level.
+*
+*  The topocentric part of the model is from Moyer (1981) and
+*  Murray (1983).
+*
+*  During the interval 1950-2050, the absolute accuracy is better
+*  than +/- 3 nanoseconds relative to direct numerical integrations
+*  using the JPL DE200/LE200 solar system ephemeris.
+*
+*  The IAU definition of TDB is that it must differ from TT only by
+*  periodic terms.  Though practical, this is an imprecise definition
+*  which ignores the existence of very long-period and secular effects
+*  in the dynamics of the solar system.  As a consequence, different
+*  implementations of TDB will, in general, differ in zero-point and
+*  will drift linearly relative to one other.
+*
+*  References:
+*    Bretagnon P, 1982 Astron. Astrophys., 114, 278-288.
+*    Fairhead L & Bretagnon P, 1990, Astron. Astrophys., 229, 240-247.
+*    Meeus J, 1984, l'Astronomie, 348-354.
+*    Moyer T D, 1981, Cel. Mech., 23, 33.
+*    Murray C A, 1983, Vectorial Astrometry, Adam Hilger.
+*
+*  P.T.Wallace   Starlink   10 November 1995
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION TDB,UT1,WL,U,V
+
+      DOUBLE PRECISION D2PI
+      PARAMETER (D2PI=6.283185307179586476925287D0)
+
+      DOUBLE PRECISION T,TSOL,RLE,RGE,RTJ,RTS,RDMOON,
+     :                 WT,W0,W1,W2,W3,W4,WF,WJ
+
+* -----------------------------------------------------------------------
+*
+*  Fairhead and Bretagnon canonical coefficients
+*
+*  787 sets of three coefficients.
+*
+*  Each set is amplitude (microseconds)
+*              frequency (radians per Julian millenium since J2000),
+*              phase (radians).
+*
+*  Sets   1-474 are the T**0 terms,
+*   "   475-679  "   "  T**1   "
+*   "   680-764  "   "  T**2   "
+*   "   765-784  "   "  T**3   "
+*   "   785-787  "   "  T**4   "  .
+*
+      DOUBLE PRECISION FAIRHD(3,787)
+      INTEGER I,J
+      DATA ((FAIRHD(I,J),I=1,3),J=  1, 10) /
+     : 1656.674564D-6,    6283.075849991D0, 6.240054195D0,
+     :   22.417471D-6,    5753.384884897D0, 4.296977442D0,
+     :   13.839792D-6,   12566.151699983D0, 6.196904410D0,
+     :    4.770086D-6,     529.690965095D0, 0.444401603D0,
+     :    4.676740D-6,    6069.776754553D0, 4.021195093D0,
+     :    2.256707D-6,     213.299095438D0, 5.543113262D0,
+     :    1.694205D-6,      -3.523118349D0, 5.025132748D0,
+     :    1.554905D-6,   77713.771467920D0, 5.198467090D0,
+     :    1.276839D-6,    7860.419392439D0, 5.988822341D0,
+     :    1.193379D-6,    5223.693919802D0, 3.649823730D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J= 11, 20) /
+     :    1.115322D-6,    3930.209696220D0, 1.422745069D0,
+     :    0.794185D-6,   11506.769769794D0, 2.322313077D0,
+     :    0.447061D-6,      26.298319800D0, 3.615796498D0,
+     :    0.435206D-6,    -398.149003408D0, 4.349338347D0,
+     :    0.600309D-6,    1577.343542448D0, 2.678271909D0,
+     :    0.496817D-6,    6208.294251424D0, 5.696701824D0,
+     :    0.486306D-6,    5884.926846583D0, 0.520007179D0,
+     :    0.432392D-6,      74.781598567D0, 2.435898309D0,
+     :    0.468597D-6,    6244.942814354D0, 5.866398759D0,
+     :    0.375510D-6,    5507.553238667D0, 4.103476804D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J= 21, 30) /
+     :    0.243085D-6,    -775.522611324D0, 3.651837925D0,
+     :    0.173435D-6,   18849.227549974D0, 6.153743485D0,
+     :    0.230685D-6,    5856.477659115D0, 4.773852582D0,
+     :    0.203747D-6,   12036.460734888D0, 4.333987818D0,
+     :    0.143935D-6,    -796.298006816D0, 5.957517795D0,
+     :    0.159080D-6,   10977.078804699D0, 1.890075226D0,
+     :    0.119979D-6,      38.133035638D0, 4.551585768D0,
+     :    0.118971D-6,    5486.777843175D0, 1.914547226D0,
+     :    0.116120D-6,    1059.381930189D0, 0.873504123D0,
+     :    0.137927D-6,   11790.629088659D0, 1.135934669D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J= 31, 40) /
+     :    0.098358D-6,    2544.314419883D0, 0.092793886D0,
+     :    0.101868D-6,   -5573.142801634D0, 5.984503847D0,
+     :    0.080164D-6,     206.185548437D0, 2.095377709D0,
+     :    0.079645D-6,    4694.002954708D0, 2.949233637D0,
+     :    0.062617D-6,      20.775395492D0, 2.654394814D0,
+     :    0.075019D-6,    2942.463423292D0, 4.980931759D0,
+     :    0.064397D-6,    5746.271337896D0, 1.280308748D0,
+     :    0.063814D-6,    5760.498431898D0, 4.167901731D0,
+     :    0.048042D-6,    2146.165416475D0, 1.495846011D0,
+     :    0.048373D-6,     155.420399434D0, 2.251573730D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J= 41, 50) /
+     :    0.058844D-6,     426.598190876D0, 4.839650148D0,
+     :    0.046551D-6,      -0.980321068D0, 0.921573539D0,
+     :    0.054139D-6,   17260.154654690D0, 3.411091093D0,
+     :    0.042411D-6,    6275.962302991D0, 2.869567043D0,
+     :    0.040184D-6,      -7.113547001D0, 3.565975565D0,
+     :    0.036564D-6,    5088.628839767D0, 3.324679049D0,
+     :    0.040759D-6,   12352.852604545D0, 3.981496998D0,
+     :    0.036507D-6,     801.820931124D0, 6.248866009D0,
+     :    0.036955D-6,    3154.687084896D0, 5.071801441D0,
+     :    0.042732D-6,     632.783739313D0, 5.720622217D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J= 51, 60) /
+     :    0.042560D-6,  161000.685737473D0, 1.270837679D0,
+     :    0.040480D-6,   15720.838784878D0, 2.546610123D0,
+     :    0.028244D-6,   -6286.598968340D0, 5.069663519D0,
+     :    0.033477D-6,    6062.663207553D0, 4.144987272D0,
+     :    0.034867D-6,     522.577418094D0, 5.210064075D0,
+     :    0.032438D-6,    6076.890301554D0, 0.749317412D0,
+     :    0.030215D-6,    7084.896781115D0, 3.389610345D0,
+     :    0.029247D-6,  -71430.695617928D0, 4.183178762D0,
+     :    0.033529D-6,    9437.762934887D0, 2.404714239D0,
+     :    0.032423D-6,    8827.390269875D0, 5.541473556D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J= 61, 70) /
+     :    0.027567D-6,    6279.552731642D0, 5.040846034D0,
+     :    0.029862D-6,   12139.553509107D0, 1.770181024D0,
+     :    0.022509D-6,   10447.387839604D0, 1.460726241D0,
+     :    0.020937D-6,    8429.241266467D0, 0.652303414D0,
+     :    0.020322D-6,     419.484643875D0, 3.735430632D0,
+     :    0.024816D-6,   -1194.447010225D0, 1.087136918D0,
+     :    0.025196D-6,    1748.016413067D0, 2.901883301D0,
+     :    0.021691D-6,   14143.495242431D0, 5.952658009D0,
+     :    0.017673D-6,    6812.766815086D0, 3.186129845D0,
+     :    0.022567D-6,    6133.512652857D0, 3.307984806D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J= 71, 80) /
+     :    0.016155D-6,   10213.285546211D0, 1.331103168D0,
+     :    0.014751D-6,    1349.867409659D0, 4.308933301D0,
+     :    0.015949D-6,    -220.412642439D0, 4.005298270D0,
+     :    0.015974D-6,   -2352.866153772D0, 6.145309371D0,
+     :    0.014223D-6,   17789.845619785D0, 2.104551349D0,
+     :    0.017806D-6,      73.297125859D0, 3.475975097D0,
+     :    0.013671D-6,    -536.804512095D0, 5.971672571D0,
+     :    0.011942D-6,    8031.092263058D0, 2.053414715D0,
+     :    0.014318D-6,   16730.463689596D0, 3.016058075D0,
+     :    0.012462D-6,     103.092774219D0, 1.737438797D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J= 81, 90) /
+     :    0.010962D-6,       3.590428652D0, 2.196567739D0,
+     :    0.015078D-6,   19651.048481098D0, 3.969480770D0,
+     :    0.010396D-6,     951.718406251D0, 5.717799605D0,
+     :    0.011707D-6,   -4705.732307544D0, 2.654125618D0,
+     :    0.010453D-6,    5863.591206116D0, 1.913704550D0,
+     :    0.012420D-6,    4690.479836359D0, 4.734090399D0,
+     :    0.011847D-6,    5643.178563677D0, 5.489005403D0,
+     :    0.008610D-6,    3340.612426700D0, 3.661698944D0,
+     :    0.011622D-6,    5120.601145584D0, 4.863931876D0,
+     :    0.010825D-6,     553.569402842D0, 0.842715011D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J= 91,100) /
+     :    0.008666D-6,    -135.065080035D0, 3.293406547D0,
+     :    0.009963D-6,     149.563197135D0, 4.870690598D0,
+     :    0.009858D-6,    6309.374169791D0, 1.061816410D0,
+     :    0.007959D-6,     316.391869657D0, 2.465042647D0,
+     :    0.010099D-6,     283.859318865D0, 1.942176992D0,
+     :    0.007147D-6,    -242.728603974D0, 3.661486981D0,
+     :    0.007505D-6,    5230.807466803D0, 4.920937029D0,
+     :    0.008323D-6,   11769.853693166D0, 1.229392026D0,
+     :    0.007490D-6,   -6256.777530192D0, 3.658444681D0,
+     :    0.009370D-6,  149854.400134205D0, 0.673880395D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=101,110) /
+     :    0.007117D-6,      38.027672636D0, 5.294249518D0,
+     :    0.007857D-6,   12168.002696575D0, 0.525733528D0,
+     :    0.007019D-6,    6206.809778716D0, 0.837688810D0,
+     :    0.006056D-6,     955.599741609D0, 4.194535082D0,
+     :    0.008107D-6,   13367.972631107D0, 3.793235253D0,
+     :    0.006731D-6,    5650.292110678D0, 5.639906583D0,
+     :    0.007332D-6,      36.648562930D0, 0.114858677D0,
+     :    0.006366D-6,    4164.311989613D0, 2.262081818D0,
+     :    0.006858D-6,    5216.580372801D0, 0.642063318D0,
+     :    0.006919D-6,    6681.224853400D0, 6.018501522D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=111,120) /
+     :    0.006826D-6,    7632.943259650D0, 3.458654112D0,
+     :    0.005308D-6,   -1592.596013633D0, 2.500382359D0,
+     :    0.005096D-6,   11371.704689758D0, 2.547107806D0,
+     :    0.004841D-6,    5333.900241022D0, 0.437078094D0,
+     :    0.005582D-6,    5966.683980335D0, 2.246174308D0,
+     :    0.006304D-6,   11926.254413669D0, 2.512929171D0,
+     :    0.006603D-6,   23581.258177318D0, 5.393136889D0,
+     :    0.005123D-6,      -1.484472708D0, 2.999641028D0,
+     :    0.004648D-6,    1589.072895284D0, 1.275847090D0,
+     :    0.005119D-6,    6438.496249426D0, 1.486539246D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=121,130) /
+     :    0.004521D-6,    4292.330832950D0, 6.140635794D0,
+     :    0.005680D-6,   23013.539539587D0, 4.557814849D0,
+     :    0.005488D-6,      -3.455808046D0, 0.090675389D0,
+     :    0.004193D-6,    7234.794256242D0, 4.869091389D0,
+     :    0.003742D-6,    7238.675591600D0, 4.691976180D0,
+     :    0.004148D-6,    -110.206321219D0, 3.016173439D0,
+     :    0.004553D-6,   11499.656222793D0, 5.554998314D0,
+     :    0.004892D-6,    5436.993015240D0, 1.475415597D0,
+     :    0.004044D-6,    4732.030627343D0, 1.398784824D0,
+     :    0.004164D-6,   12491.370101415D0, 5.650931916D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=131,140) /
+     :    0.004349D-6,   11513.883316794D0, 2.181745369D0,
+     :    0.003919D-6,   12528.018664345D0, 5.823319737D0,
+     :    0.003129D-6,    6836.645252834D0, 0.003844094D0,
+     :    0.004080D-6,   -7058.598461315D0, 3.690360123D0,
+     :    0.003270D-6,      76.266071276D0, 1.517189902D0,
+     :    0.002954D-6,    6283.143160294D0, 4.447203799D0,
+     :    0.002872D-6,      28.449187468D0, 1.158692983D0,
+     :    0.002881D-6,     735.876513532D0, 0.349250250D0,
+     :    0.003279D-6,    5849.364112115D0, 4.893384368D0,
+     :    0.003625D-6,    6209.778724132D0, 1.473760578D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=141,150) /
+     :    0.003074D-6,     949.175608970D0, 5.185878737D0,
+     :    0.002775D-6,    9917.696874510D0, 1.030026325D0,
+     :    0.002646D-6,   10973.555686350D0, 3.918259169D0,
+     :    0.002575D-6,   25132.303399966D0, 6.109659023D0,
+     :    0.003500D-6,     263.083923373D0, 1.892100742D0,
+     :    0.002740D-6,   18319.536584880D0, 4.320519510D0,
+     :    0.002464D-6,     202.253395174D0, 4.698203059D0,
+     :    0.002409D-6,       2.542797281D0, 5.325009315D0,
+     :    0.003354D-6,  -90955.551694697D0, 1.942656623D0,
+     :    0.002296D-6,    6496.374945429D0, 5.061810696D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=151,160) /
+     :    0.003002D-6,    6172.869528772D0, 2.797822767D0,
+     :    0.003202D-6,   27511.467873537D0, 0.531673101D0,
+     :    0.002954D-6,   -6283.008539689D0, 4.533471191D0,
+     :    0.002353D-6,     639.897286314D0, 3.734548088D0,
+     :    0.002401D-6,   16200.772724501D0, 2.605547070D0,
+     :    0.003053D-6,  233141.314403759D0, 3.029030662D0,
+     :    0.003024D-6,   83286.914269554D0, 2.355556099D0,
+     :    0.002863D-6,   17298.182327326D0, 5.240963796D0,
+     :    0.002103D-6,   -7079.373856808D0, 5.756641637D0,
+     :    0.002303D-6,   83996.847317911D0, 2.013686814D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=161,170) /
+     :    0.002303D-6,   18073.704938650D0, 1.089100410D0,
+     :    0.002381D-6,      63.735898303D0, 0.759188178D0,
+     :    0.002493D-6,    6386.168624210D0, 0.645026535D0,
+     :    0.002366D-6,       3.932153263D0, 6.215885448D0,
+     :    0.002169D-6,   11015.106477335D0, 4.845297676D0,
+     :    0.002397D-6,    6243.458341645D0, 3.809290043D0,
+     :    0.002183D-6,    1162.474704408D0, 6.179611691D0,
+     :    0.002353D-6,    6246.427287062D0, 4.781719760D0,
+     :    0.002199D-6,    -245.831646229D0, 5.956152284D0,
+     :    0.001729D-6,    3894.181829542D0, 1.264976635D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=171,180) /
+     :    0.001896D-6,   -3128.388765096D0, 4.914231596D0,
+     :    0.002085D-6,      35.164090221D0, 1.405158503D0,
+     :    0.002024D-6,   14712.317116458D0, 2.752035928D0,
+     :    0.001737D-6,    6290.189396992D0, 5.280820144D0,
+     :    0.002229D-6,     491.557929457D0, 1.571007057D0,
+     :    0.001602D-6,   14314.168113050D0, 4.203664806D0,
+     :    0.002186D-6,     454.909366527D0, 1.402101526D0,
+     :    0.001897D-6,   22483.848574493D0, 4.167932508D0,
+     :    0.001825D-6,   -3738.761430108D0, 0.545828785D0,
+     :    0.001894D-6,    1052.268383188D0, 5.817167450D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=181,190) /
+     :    0.001421D-6,      20.355319399D0, 2.419886601D0,
+     :    0.001408D-6,   10984.192351700D0, 2.732084787D0,
+     :    0.001847D-6,   10873.986030480D0, 2.903477885D0,
+     :    0.001391D-6,   -8635.942003763D0, 0.593891500D0,
+     :    0.001388D-6,      -7.046236698D0, 1.166145902D0,
+     :    0.001810D-6,  -88860.057071188D0, 0.487355242D0,
+     :    0.001288D-6,   -1990.745017041D0, 3.913022880D0,
+     :    0.001297D-6,   23543.230504682D0, 3.063805171D0,
+     :    0.001335D-6,    -266.607041722D0, 3.995764039D0,
+     :    0.001376D-6,   10969.965257698D0, 5.152914309D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=191,200) /
+     :    0.001745D-6,  244287.600007027D0, 3.626395673D0,
+     :    0.001649D-6,   31441.677569757D0, 1.952049260D0,
+     :    0.001416D-6,    9225.539273283D0, 4.996408389D0,
+     :    0.001238D-6,    4804.209275927D0, 5.503379738D0,
+     :    0.001472D-6,    4590.910180489D0, 4.164913291D0,
+     :    0.001169D-6,    6040.347246017D0, 5.841719038D0,
+     :    0.001039D-6,    5540.085789459D0, 2.769753519D0,
+     :    0.001004D-6,    -170.672870619D0, 0.755008103D0,
+     :    0.001284D-6,   10575.406682942D0, 5.306538209D0,
+     :    0.001278D-6,      71.812653151D0, 4.713486491D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=201,210) /
+     :    0.001321D-6,   18209.330263660D0, 2.624866359D0,
+     :    0.001297D-6,   21228.392023546D0, 0.382603541D0,
+     :    0.000954D-6,    6282.095528923D0, 0.882213514D0,
+     :    0.001145D-6,    6058.731054289D0, 1.169483931D0,
+     :    0.000979D-6,    5547.199336460D0, 5.448375984D0,
+     :    0.000987D-6,   -6262.300454499D0, 2.656486959D0,
+     :    0.001070D-6, -154717.609887482D0, 1.827624012D0,
+     :    0.000991D-6,    4701.116501708D0, 4.387001801D0,
+     :    0.001155D-6,     -14.227094002D0, 3.042700750D0,
+     :    0.001176D-6,     277.034993741D0, 3.335519004D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=211,220) /
+     :    0.000890D-6,   13916.019109642D0, 5.601498297D0,
+     :    0.000884D-6,   -1551.045222648D0, 1.088831705D0,
+     :    0.000876D-6,    5017.508371365D0, 3.969902609D0,
+     :    0.000806D-6,   15110.466119866D0, 5.142876744D0,
+     :    0.000773D-6,   -4136.910433516D0, 0.022067765D0,
+     :    0.001077D-6,     175.166059800D0, 1.844913056D0,
+     :    0.000954D-6,   -6284.056171060D0, 0.968480906D0,
+     :    0.000737D-6,    5326.786694021D0, 4.923831588D0,
+     :    0.000845D-6,    -433.711737877D0, 4.749245231D0,
+     :    0.000819D-6,    8662.240323563D0, 5.991247817D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=221,230) /
+     :    0.000852D-6,     199.072001436D0, 2.189604979D0,
+     :    0.000723D-6,   17256.631536341D0, 6.068719637D0,
+     :    0.000940D-6,    6037.244203762D0, 6.197428148D0,
+     :    0.000885D-6,   11712.955318231D0, 3.280414875D0,
+     :    0.000706D-6,   12559.038152982D0, 2.824848947D0,
+     :    0.000732D-6,    2379.164473572D0, 2.501813417D0,
+     :    0.000764D-6,   -6127.655450557D0, 2.236346329D0,
+     :    0.000908D-6,     131.541961686D0, 2.521257490D0,
+     :    0.000907D-6,   35371.887265976D0, 3.370195967D0,
+     :    0.000673D-6,    1066.495477190D0, 3.876512374D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=231,240) /
+     :    0.000814D-6,   17654.780539750D0, 4.627122566D0,
+     :    0.000630D-6,      36.027866677D0, 0.156368499D0,
+     :    0.000798D-6,     515.463871093D0, 5.151962502D0,
+     :    0.000798D-6,     148.078724426D0, 5.909225055D0,
+     :    0.000806D-6,     309.278322656D0, 6.054064447D0,
+     :    0.000607D-6,     -39.617508346D0, 2.839021623D0,
+     :    0.000601D-6,     412.371096874D0, 3.984225404D0,
+     :    0.000646D-6,   11403.676995575D0, 3.852959484D0,
+     :    0.000704D-6,   13521.751441591D0, 2.300991267D0,
+     :    0.000603D-6,  -65147.619767937D0, 4.140083146D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=241,250) /
+     :    0.000609D-6,   10177.257679534D0, 0.437122327D0,
+     :    0.000631D-6,    5767.611978898D0, 4.026532329D0,
+     :    0.000576D-6,   11087.285125918D0, 4.760293101D0,
+     :    0.000674D-6,   14945.316173554D0, 6.270510511D0,
+     :    0.000726D-6,    5429.879468239D0, 6.039606892D0,
+     :    0.000710D-6,   28766.924424484D0, 5.672617711D0,
+     :    0.000647D-6,   11856.218651625D0, 3.397132627D0,
+     :    0.000678D-6,   -5481.254918868D0, 6.249666675D0,
+     :    0.000618D-6,   22003.914634870D0, 2.466427018D0,
+     :    0.000738D-6,    6134.997125565D0, 2.242668890D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=251,260) /
+     :    0.000660D-6,     625.670192312D0, 5.864091907D0,
+     :    0.000694D-6,    3496.032826134D0, 2.668309141D0,
+     :    0.000531D-6,    6489.261398429D0, 1.681888780D0,
+     :    0.000611D-6, -143571.324284214D0, 2.424978312D0,
+     :    0.000575D-6,   12043.574281889D0, 4.216492400D0,
+     :    0.000553D-6,   12416.588502848D0, 4.772158039D0,
+     :    0.000689D-6,    4686.889407707D0, 6.224271088D0,
+     :    0.000495D-6,    7342.457780181D0, 3.817285811D0,
+     :    0.000567D-6,    3634.621024518D0, 1.649264690D0,
+     :    0.000515D-6,   18635.928454536D0, 3.945345892D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=261,270) /
+     :    0.000486D-6,    -323.505416657D0, 4.061673868D0,
+     :    0.000662D-6,   25158.601719765D0, 1.794058369D0,
+     :    0.000509D-6,     846.082834751D0, 3.053874588D0,
+     :    0.000472D-6,  -12569.674818332D0, 5.112133338D0,
+     :    0.000461D-6,    6179.983075773D0, 0.513669325D0,
+     :    0.000641D-6,   83467.156352816D0, 3.210727723D0,
+     :    0.000520D-6,   10344.295065386D0, 2.445597761D0,
+     :    0.000493D-6,   18422.629359098D0, 1.676939306D0,
+     :    0.000478D-6,    1265.567478626D0, 5.487314569D0,
+     :    0.000472D-6,     -18.159247265D0, 1.999707589D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=271,280) /
+     :    0.000559D-6,   11190.377900137D0, 5.783236356D0,
+     :    0.000494D-6,    9623.688276691D0, 3.022645053D0,
+     :    0.000463D-6,    5739.157790895D0, 1.411223013D0,
+     :    0.000432D-6,   16858.482532933D0, 1.179256434D0,
+     :    0.000574D-6,   72140.628666286D0, 1.758191830D0,
+     :    0.000484D-6,   17267.268201691D0, 3.290589143D0,
+     :    0.000550D-6,    4907.302050146D0, 0.864024298D0,
+     :    0.000399D-6,      14.977853527D0, 2.094441910D0,
+     :    0.000491D-6,     224.344795702D0, 0.878372791D0,
+     :    0.000432D-6,   20426.571092422D0, 6.003829241D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=281,290) /
+     :    0.000481D-6,    5749.452731634D0, 4.309591964D0,
+     :    0.000480D-6,    5757.317038160D0, 1.142348571D0,
+     :    0.000485D-6,    6702.560493867D0, 0.210580917D0,
+     :    0.000426D-6,    6055.549660552D0, 4.274476529D0,
+     :    0.000480D-6,    5959.570433334D0, 5.031351030D0,
+     :    0.000466D-6,   12562.628581634D0, 4.959581597D0,
+     :    0.000520D-6,   39302.096962196D0, 4.788002889D0,
+     :    0.000458D-6,   12132.439962106D0, 1.880103788D0,
+     :    0.000470D-6,   12029.347187887D0, 1.405611197D0,
+     :    0.000416D-6,   -7477.522860216D0, 1.082356330D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=291,300) /
+     :    0.000449D-6,   11609.862544012D0, 4.179989585D0,
+     :    0.000465D-6,   17253.041107690D0, 0.353496295D0,
+     :    0.000362D-6,   -4535.059436924D0, 1.583849576D0,
+     :    0.000383D-6,   21954.157609398D0, 3.747376371D0,
+     :    0.000389D-6,      17.252277143D0, 1.395753179D0,
+     :    0.000331D-6,   18052.929543158D0, 0.566790582D0,
+     :    0.000430D-6,   13517.870106233D0, 0.685827538D0,
+     :    0.000368D-6,   -5756.908003246D0, 0.731374317D0,
+     :    0.000330D-6,   10557.594160824D0, 3.710043680D0,
+     :    0.000332D-6,   20199.094959633D0, 1.652901407D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=301,310) /
+     :    0.000384D-6,   11933.367960670D0, 5.827781531D0,
+     :    0.000387D-6,   10454.501386605D0, 2.541182564D0,
+     :    0.000325D-6,   15671.081759407D0, 2.178850542D0,
+     :    0.000318D-6,     138.517496871D0, 2.253253037D0,
+     :    0.000305D-6,    9388.005909415D0, 0.578340206D0,
+     :    0.000352D-6,    5749.861766548D0, 3.000297967D0,
+     :    0.000311D-6,    6915.859589305D0, 1.693574249D0,
+     :    0.000297D-6,   24072.921469776D0, 1.997249392D0,
+     :    0.000363D-6,    -640.877607382D0, 5.071820966D0,
+     :    0.000323D-6,   12592.450019783D0, 1.072262823D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=311,320) /
+     :    0.000341D-6,   12146.667056108D0, 4.700657997D0,
+     :    0.000290D-6,    9779.108676125D0, 1.812320441D0,
+     :    0.000342D-6,    6132.028180148D0, 4.322238614D0,
+     :    0.000329D-6,    6268.848755990D0, 3.033827743D0,
+     :    0.000374D-6,   17996.031168222D0, 3.388716544D0,
+     :    0.000285D-6,    -533.214083444D0, 4.687313233D0,
+     :    0.000338D-6,    6065.844601290D0, 0.877776108D0,
+     :    0.000276D-6,      24.298513841D0, 0.770299429D0,
+     :    0.000336D-6,   -2388.894020449D0, 5.353796034D0,
+     :    0.000290D-6,    3097.883822726D0, 4.075291557D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=321,330) /
+     :    0.000318D-6,     709.933048357D0, 5.941207518D0,
+     :    0.000271D-6,   13095.842665077D0, 3.208912203D0,
+     :    0.000331D-6,    6073.708907816D0, 4.007881169D0,
+     :    0.000292D-6,     742.990060533D0, 2.714333592D0,
+     :    0.000362D-6,   29088.811415985D0, 3.215977013D0,
+     :    0.000280D-6,   12359.966151546D0, 0.710872502D0,
+     :    0.000267D-6,   10440.274292604D0, 4.730108488D0,
+     :    0.000262D-6,     838.969287750D0, 1.327720272D0,
+     :    0.000250D-6,   16496.361396202D0, 0.898769761D0,
+     :    0.000325D-6,   20597.243963041D0, 0.180044365D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=331,340) /
+     :    0.000268D-6,    6148.010769956D0, 5.152666276D0,
+     :    0.000284D-6,    5636.065016677D0, 5.655385808D0,
+     :    0.000301D-6,    6080.822454817D0, 2.135396205D0,
+     :    0.000294D-6,    -377.373607916D0, 3.708784168D0,
+     :    0.000236D-6,    2118.763860378D0, 1.733578756D0,
+     :    0.000234D-6,    5867.523359379D0, 5.575209112D0,
+     :    0.000268D-6, -226858.238553767D0, 0.069432392D0,
+     :    0.000265D-6,  167283.761587465D0, 4.369302826D0,
+     :    0.000280D-6,   28237.233459389D0, 5.304829118D0,
+     :    0.000292D-6,   12345.739057544D0, 4.096094132D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=341,350) /
+     :    0.000223D-6,   19800.945956225D0, 3.069327406D0,
+     :    0.000301D-6,   43232.306658416D0, 6.205311188D0,
+     :    0.000264D-6,   18875.525869774D0, 1.417263408D0,
+     :    0.000304D-6,   -1823.175188677D0, 3.409035232D0,
+     :    0.000301D-6,     109.945688789D0, 0.510922054D0,
+     :    0.000260D-6,     813.550283960D0, 2.389438934D0,
+     :    0.000299D-6,  316428.228673312D0, 5.384595078D0,
+     :    0.000211D-6,    5756.566278634D0, 3.789392838D0,
+     :    0.000209D-6,    5750.203491159D0, 1.661943545D0,
+     :    0.000240D-6,   12489.885628707D0, 5.684549045D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=351,360) /
+     :    0.000216D-6,    6303.851245484D0, 3.862942261D0,
+     :    0.000203D-6,    1581.959348283D0, 5.549853589D0,
+     :    0.000200D-6,    5642.198242609D0, 1.016115785D0,
+     :    0.000197D-6,     -70.849445304D0, 4.690702525D0,
+     :    0.000227D-6,    6287.008003254D0, 2.911891613D0,
+     :    0.000197D-6,     533.623118358D0, 1.048982898D0,
+     :    0.000205D-6,   -6279.485421340D0, 1.829362730D0,
+     :    0.000209D-6,  -10988.808157535D0, 2.636140084D0,
+     :    0.000208D-6,    -227.526189440D0, 4.127883842D0,
+     :    0.000191D-6,     415.552490612D0, 4.401165650D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=361,370) /
+     :    0.000190D-6,   29296.615389579D0, 4.175658539D0,
+     :    0.000264D-6,   66567.485864652D0, 4.601102551D0,
+     :    0.000256D-6,   -3646.350377354D0, 0.506364778D0,
+     :    0.000188D-6,   13119.721102825D0, 2.032195842D0,
+     :    0.000185D-6,    -209.366942175D0, 4.694756586D0,
+     :    0.000198D-6,   25934.124331089D0, 3.832703118D0,
+     :    0.000195D-6,    4061.219215394D0, 3.308463427D0,
+     :    0.000234D-6,    5113.487598583D0, 1.716090661D0,
+     :    0.000188D-6,    1478.866574064D0, 5.686865780D0,
+     :    0.000222D-6,   11823.161639450D0, 1.942386641D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=371,380) /
+     :    0.000181D-6,   10770.893256262D0, 1.999482059D0,
+     :    0.000171D-6,    6546.159773364D0, 1.182807992D0,
+     :    0.000206D-6,      70.328180442D0, 5.934076062D0,
+     :    0.000169D-6,   20995.392966449D0, 2.169080622D0,
+     :    0.000191D-6,   10660.686935042D0, 5.405515999D0,
+     :    0.000228D-6,   33019.021112205D0, 4.656985514D0,
+     :    0.000184D-6,   -4933.208440333D0, 3.327476868D0,
+     :    0.000220D-6,    -135.625325010D0, 1.765430262D0,
+     :    0.000166D-6,   23141.558382925D0, 3.454132746D0,
+     :    0.000191D-6,    6144.558353121D0, 5.020393445D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=381,390) /
+     :    0.000180D-6,    6084.003848555D0, 0.602182191D0,
+     :    0.000163D-6,   17782.732072784D0, 4.960593133D0,
+     :    0.000225D-6,   16460.333529525D0, 2.596451817D0,
+     :    0.000222D-6,    5905.702242076D0, 3.731990323D0,
+     :    0.000204D-6,     227.476132789D0, 5.636192701D0,
+     :    0.000159D-6,   16737.577236597D0, 3.600691544D0,
+     :    0.000200D-6,    6805.653268085D0, 0.868220961D0,
+     :    0.000187D-6,   11919.140866668D0, 2.629456641D0,
+     :    0.000161D-6,     127.471796607D0, 2.862574720D0,
+     :    0.000205D-6,    6286.666278643D0, 1.742882331D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=391,400) /
+     :    0.000189D-6,     153.778810485D0, 4.812372643D0,
+     :    0.000168D-6,   16723.350142595D0, 0.027860588D0,
+     :    0.000149D-6,   11720.068865232D0, 0.659721876D0,
+     :    0.000189D-6,    5237.921013804D0, 5.245313000D0,
+     :    0.000143D-6,    6709.674040867D0, 4.317625647D0,
+     :    0.000146D-6,    4487.817406270D0, 4.815297007D0,
+     :    0.000144D-6,    -664.756045130D0, 5.381366880D0,
+     :    0.000175D-6,    5127.714692584D0, 4.728443327D0,
+     :    0.000162D-6,    6254.626662524D0, 1.435132069D0,
+     :    0.000187D-6,   47162.516354635D0, 1.354371923D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=401,410) /
+     :    0.000146D-6,   11080.171578918D0, 3.369695406D0,
+     :    0.000180D-6,    -348.924420448D0, 2.490902145D0,
+     :    0.000148D-6,     151.047669843D0, 3.799109588D0,
+     :    0.000157D-6,    6197.248551160D0, 1.284375887D0,
+     :    0.000167D-6,     146.594251718D0, 0.759969109D0,
+     :    0.000133D-6,   -5331.357443741D0, 5.409701889D0,
+     :    0.000154D-6,      95.979227218D0, 3.366890614D0,
+     :    0.000148D-6,   -6418.140930027D0, 3.384104996D0,
+     :    0.000128D-6,   -6525.804453965D0, 3.803419985D0,
+     :    0.000130D-6,   11293.470674356D0, 0.939039445D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=411,420) /
+     :    0.000152D-6,   -5729.506447149D0, 0.734117523D0,
+     :    0.000138D-6,     210.117701700D0, 2.564216078D0,
+     :    0.000123D-6,    6066.595360816D0, 4.517099537D0,
+     :    0.000140D-6,   18451.078546566D0, 0.642049130D0,
+     :    0.000126D-6,   11300.584221356D0, 3.485280663D0,
+     :    0.000119D-6,   10027.903195729D0, 3.217431161D0,
+     :    0.000151D-6,    4274.518310832D0, 4.404359108D0,
+     :    0.000117D-6,    6072.958148291D0, 0.366324650D0,
+     :    0.000165D-6,   -7668.637425143D0, 4.298212528D0,
+     :    0.000117D-6,   -6245.048177356D0, 5.379518958D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=421,430) /
+     :    0.000130D-6,   -5888.449964932D0, 4.527681115D0,
+     :    0.000121D-6,    -543.918059096D0, 6.109429504D0,
+     :    0.000162D-6,    9683.594581116D0, 5.720092446D0,
+     :    0.000141D-6,    6219.339951688D0, 0.679068671D0,
+     :    0.000118D-6,   22743.409379516D0, 4.881123092D0,
+     :    0.000129D-6,    1692.165669502D0, 0.351407289D0,
+     :    0.000126D-6,    5657.405657679D0, 5.146592349D0,
+     :    0.000114D-6,     728.762966531D0, 0.520791814D0,
+     :    0.000120D-6,      52.596639600D0, 0.948516300D0,
+     :    0.000115D-6,      65.220371012D0, 3.504914846D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=431,440) /
+     :    0.000126D-6,    5881.403728234D0, 5.577502482D0,
+     :    0.000158D-6,  163096.180360983D0, 2.957128968D0,
+     :    0.000134D-6,   12341.806904281D0, 2.598576764D0,
+     :    0.000151D-6,   16627.370915377D0, 3.985702050D0,
+     :    0.000109D-6,    1368.660252845D0, 0.014730471D0,
+     :    0.000131D-6,    6211.263196841D0, 0.085077024D0,
+     :    0.000146D-6,    5792.741760812D0, 0.708426604D0,
+     :    0.000146D-6,     -77.750543984D0, 3.121576600D0,
+     :    0.000107D-6,    5341.013788022D0, 0.288231904D0,
+     :    0.000138D-6,    6281.591377283D0, 2.797450317D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=441,450) /
+     :    0.000113D-6,   -6277.552925684D0, 2.788904128D0,
+     :    0.000115D-6,    -525.758811831D0, 5.895222200D0,
+     :    0.000138D-6,    6016.468808270D0, 6.096188999D0,
+     :    0.000139D-6,   23539.707386333D0, 2.028195445D0,
+     :    0.000146D-6,   -4176.041342449D0, 4.660008502D0,
+     :    0.000107D-6,   16062.184526117D0, 4.066520001D0,
+     :    0.000142D-6,   83783.548222473D0, 2.936315115D0,
+     :    0.000128D-6,    9380.959672717D0, 3.223844306D0,
+     :    0.000135D-6,    6205.325306007D0, 1.638054048D0,
+     :    0.000101D-6,    2699.734819318D0, 5.481603249D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=451,460) /
+     :    0.000104D-6,    -568.821874027D0, 2.205734493D0,
+     :    0.000103D-6,    6321.103522627D0, 2.440421099D0,
+     :    0.000119D-6,    6321.208885629D0, 2.547496264D0,
+     :    0.000138D-6,    1975.492545856D0, 2.314608466D0,
+     :    0.000121D-6,     137.033024162D0, 4.539108237D0,
+     :    0.000123D-6,   19402.796952817D0, 4.538074405D0,
+     :    0.000119D-6,   22805.735565994D0, 2.869040566D0,
+     :    0.000133D-6,   64471.991241142D0, 6.056405489D0,
+     :    0.000129D-6,     -85.827298831D0, 2.540635083D0,
+     :    0.000131D-6,   13613.804277336D0, 4.005732868D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=461,470) /
+     :    0.000104D-6,    9814.604100291D0, 1.959967212D0,
+     :    0.000112D-6,   16097.679950283D0, 3.589026260D0,
+     :    0.000123D-6,    2107.034507542D0, 1.728627253D0,
+     :    0.000121D-6,   36949.230808424D0, 6.072332087D0,
+     :    0.000108D-6,  -12539.853380183D0, 3.716133846D0,
+     :    0.000113D-6,   -7875.671863624D0, 2.725771122D0,
+     :    0.000109D-6,    4171.425536614D0, 4.033338079D0,
+     :    0.000101D-6,    6247.911759770D0, 3.441347021D0,
+     :    0.000113D-6,    7330.728427345D0, 0.656372122D0,
+     :    0.000113D-6,   51092.726050855D0, 2.791483066D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=471,480) /
+     :    0.000106D-6,    5621.842923210D0, 1.815323326D0,
+     :    0.000101D-6,     111.430161497D0, 5.711033677D0,
+     :    0.000103D-6,     909.818733055D0, 2.812745443D0,
+     :    0.000101D-6,    1790.642637886D0, 1.965746028D0,
+
+*  T
+     :  102.156724D-6,    6283.075849991D0, 4.249032005D0,
+     :    1.706807D-6,   12566.151699983D0, 4.205904248D0,
+     :    0.269668D-6,     213.299095438D0, 3.400290479D0,
+     :    0.265919D-6,     529.690965095D0, 5.836047367D0,
+     :    0.210568D-6,      -3.523118349D0, 6.262738348D0,
+     :    0.077996D-6,    5223.693919802D0, 4.670344204D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=481,490) /
+     :    0.054764D-6,    1577.343542448D0, 4.534800170D0,
+     :    0.059146D-6,      26.298319800D0, 1.083044735D0,
+     :    0.034420D-6,    -398.149003408D0, 5.980077351D0,
+     :    0.032088D-6,   18849.227549974D0, 4.162913471D0,
+     :    0.033595D-6,    5507.553238667D0, 5.980162321D0,
+     :    0.029198D-6,    5856.477659115D0, 0.623811863D0,
+     :    0.027764D-6,     155.420399434D0, 3.745318113D0,
+     :    0.025190D-6,    5746.271337896D0, 2.980330535D0,
+     :    0.022997D-6,    -796.298006816D0, 1.174411803D0,
+     :    0.024976D-6,    5760.498431898D0, 2.467913690D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=491,500) /
+     :    0.021774D-6,     206.185548437D0, 3.854787540D0,
+     :    0.017925D-6,    -775.522611324D0, 1.092065955D0,
+     :    0.013794D-6,     426.598190876D0, 2.699831988D0,
+     :    0.013276D-6,    6062.663207553D0, 5.845801920D0,
+     :    0.011774D-6,   12036.460734888D0, 2.292832062D0,
+     :    0.012869D-6,    6076.890301554D0, 5.333425680D0,
+     :    0.012152D-6,    1059.381930189D0, 6.222874454D0,
+     :    0.011081D-6,      -7.113547001D0, 5.154724984D0,
+     :    0.010143D-6,    4694.002954708D0, 4.044013795D0,
+     :    0.009357D-6,    5486.777843175D0, 3.416081409D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=501,510) /
+     :    0.010084D-6,     522.577418094D0, 0.749320262D0,
+     :    0.008587D-6,   10977.078804699D0, 2.777152598D0,
+     :    0.008628D-6,    6275.962302991D0, 4.562060226D0,
+     :    0.008158D-6,    -220.412642439D0, 5.806891533D0,
+     :    0.007746D-6,    2544.314419883D0, 1.603197066D0,
+     :    0.007670D-6,    2146.165416475D0, 3.000200440D0,
+     :    0.007098D-6,      74.781598567D0, 0.443725817D0,
+     :    0.006180D-6,    -536.804512095D0, 1.302642751D0,
+     :    0.005818D-6,    5088.628839767D0, 4.827723531D0,
+     :    0.004945D-6,   -6286.598968340D0, 0.268305170D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=511,520) /
+     :    0.004774D-6,    1349.867409659D0, 5.808636673D0,
+     :    0.004687D-6,    -242.728603974D0, 5.154890570D0,
+     :    0.006089D-6,    1748.016413067D0, 4.403765209D0,
+     :    0.005975D-6,   -1194.447010225D0, 2.583472591D0,
+     :    0.004229D-6,     951.718406251D0, 0.931172179D0,
+     :    0.005264D-6,     553.569402842D0, 2.336107252D0,
+     :    0.003049D-6,    5643.178563677D0, 1.362634430D0,
+     :    0.002974D-6,    6812.766815086D0, 1.583012668D0,
+     :    0.003403D-6,   -2352.866153772D0, 2.552189886D0,
+     :    0.003030D-6,     419.484643875D0, 5.286473844D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=521,530) /
+     :    0.003210D-6,      -7.046236698D0, 1.863796539D0,
+     :    0.003058D-6,    9437.762934887D0, 4.226420633D0,
+     :    0.002589D-6,   12352.852604545D0, 1.991935820D0,
+     :    0.002927D-6,    5216.580372801D0, 2.319951253D0,
+     :    0.002425D-6,    5230.807466803D0, 3.084752833D0,
+     :    0.002656D-6,    3154.687084896D0, 2.487447866D0,
+     :    0.002445D-6,   10447.387839604D0, 2.347139160D0,
+     :    0.002990D-6,    4690.479836359D0, 6.235872050D0,
+     :    0.002890D-6,    5863.591206116D0, 0.095197563D0,
+     :    0.002498D-6,    6438.496249426D0, 2.994779800D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=531,540) /
+     :    0.001889D-6,    8031.092263058D0, 3.569003717D0,
+     :    0.002567D-6,     801.820931124D0, 3.425611498D0,
+     :    0.001803D-6,  -71430.695617928D0, 2.192295512D0,
+     :    0.001782D-6,       3.932153263D0, 5.180433689D0,
+     :    0.001694D-6,   -4705.732307544D0, 4.641779174D0,
+     :    0.001704D-6,   -1592.596013633D0, 3.997097652D0,
+     :    0.001735D-6,    5849.364112115D0, 0.417558428D0,
+     :    0.001643D-6,    8429.241266467D0, 2.180619584D0,
+     :    0.001680D-6,      38.133035638D0, 4.164529426D0,
+     :    0.002045D-6,    7084.896781115D0, 0.526323854D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=541,550) /
+     :    0.001458D-6,    4292.330832950D0, 1.356098141D0,
+     :    0.001437D-6,      20.355319399D0, 3.895439360D0,
+     :    0.001738D-6,    6279.552731642D0, 0.087484036D0,
+     :    0.001367D-6,   14143.495242431D0, 3.987576591D0,
+     :    0.001344D-6,    7234.794256242D0, 0.090454338D0,
+     :    0.001438D-6,   11499.656222793D0, 0.974387904D0,
+     :    0.001257D-6,    6836.645252834D0, 1.509069366D0,
+     :    0.001358D-6,   11513.883316794D0, 0.495572260D0,
+     :    0.001628D-6,    7632.943259650D0, 4.968445721D0,
+     :    0.001169D-6,     103.092774219D0, 2.838496795D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=551,560) /
+     :    0.001162D-6,    4164.311989613D0, 3.408387778D0,
+     :    0.001092D-6,    6069.776754553D0, 3.617942651D0,
+     :    0.001008D-6,   17789.845619785D0, 0.286350174D0,
+     :    0.001008D-6,     639.897286314D0, 1.610762073D0,
+     :    0.000918D-6,   10213.285546211D0, 5.532798067D0,
+     :    0.001011D-6,   -6256.777530192D0, 0.661826484D0,
+     :    0.000753D-6,   16730.463689596D0, 3.905030235D0,
+     :    0.000737D-6,   11926.254413669D0, 4.641956361D0,
+     :    0.000694D-6,    3340.612426700D0, 2.111120332D0,
+     :    0.000701D-6,    3894.181829542D0, 2.760823491D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=561,570) /
+     :    0.000689D-6,    -135.065080035D0, 4.768800780D0,
+     :    0.000700D-6,   13367.972631107D0, 5.760439898D0,
+     :    0.000664D-6,    6040.347246017D0, 1.051215840D0,
+     :    0.000654D-6,    5650.292110678D0, 4.911332503D0,
+     :    0.000788D-6,    6681.224853400D0, 4.699648011D0,
+     :    0.000628D-6,    5333.900241022D0, 5.024608847D0,
+     :    0.000755D-6,    -110.206321219D0, 4.370971253D0,
+     :    0.000628D-6,    6290.189396992D0, 3.660478857D0,
+     :    0.000635D-6,   25132.303399966D0, 4.121051532D0,
+     :    0.000534D-6,    5966.683980335D0, 1.173284524D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=571,580) /
+     :    0.000543D-6,    -433.711737877D0, 0.345585464D0,
+     :    0.000517D-6,   -1990.745017041D0, 5.414571768D0,
+     :    0.000504D-6,    5767.611978898D0, 2.328281115D0,
+     :    0.000485D-6,    5753.384884897D0, 1.685874771D0,
+     :    0.000463D-6,    7860.419392439D0, 5.297703006D0,
+     :    0.000604D-6,     515.463871093D0, 0.591998446D0,
+     :    0.000443D-6,   12168.002696575D0, 4.830881244D0,
+     :    0.000570D-6,     199.072001436D0, 3.899190272D0,
+     :    0.000465D-6,   10969.965257698D0, 0.476681802D0,
+     :    0.000424D-6,   -7079.373856808D0, 1.112242763D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=581,590) /
+     :    0.000427D-6,     735.876513532D0, 1.994214480D0,
+     :    0.000478D-6,   -6127.655450557D0, 3.778025483D0,
+     :    0.000414D-6,   10973.555686350D0, 5.441088327D0,
+     :    0.000512D-6,    1589.072895284D0, 0.107123853D0,
+     :    0.000378D-6,   10984.192351700D0, 0.915087231D0,
+     :    0.000402D-6,   11371.704689758D0, 4.107281715D0,
+     :    0.000453D-6,    9917.696874510D0, 1.917490952D0,
+     :    0.000395D-6,     149.563197135D0, 2.763124165D0,
+     :    0.000371D-6,    5739.157790895D0, 3.112111866D0,
+     :    0.000350D-6,   11790.629088659D0, 0.440639857D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=591,600) /
+     :    0.000356D-6,    6133.512652857D0, 5.444568842D0,
+     :    0.000344D-6,     412.371096874D0, 5.676832684D0,
+     :    0.000383D-6,     955.599741609D0, 5.559734846D0,
+     :    0.000333D-6,    6496.374945429D0, 0.261537984D0,
+     :    0.000340D-6,    6055.549660552D0, 5.975534987D0,
+     :    0.000334D-6,    1066.495477190D0, 2.335063907D0,
+     :    0.000399D-6,   11506.769769794D0, 5.321230910D0,
+     :    0.000314D-6,   18319.536584880D0, 2.313312404D0,
+     :    0.000424D-6,    1052.268383188D0, 1.211961766D0,
+     :    0.000307D-6,      63.735898303D0, 3.169551388D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=601,610) /
+     :    0.000329D-6,      29.821438149D0, 6.106912080D0,
+     :    0.000357D-6,    6309.374169791D0, 4.223760346D0,
+     :    0.000312D-6,   -3738.761430108D0, 2.180556645D0,
+     :    0.000301D-6,     309.278322656D0, 1.499984572D0,
+     :    0.000268D-6,   12043.574281889D0, 2.447520648D0,
+     :    0.000257D-6,   12491.370101415D0, 3.662331761D0,
+     :    0.000290D-6,     625.670192312D0, 1.272834584D0,
+     :    0.000256D-6,    5429.879468239D0, 1.913426912D0,
+     :    0.000339D-6,    3496.032826134D0, 4.165930011D0,
+     :    0.000283D-6,    3930.209696220D0, 4.325565754D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=611,620) /
+     :    0.000241D-6,   12528.018664345D0, 3.832324536D0,
+     :    0.000304D-6,    4686.889407707D0, 1.612348468D0,
+     :    0.000259D-6,   16200.772724501D0, 3.470173146D0,
+     :    0.000238D-6,   12139.553509107D0, 1.147977842D0,
+     :    0.000236D-6,    6172.869528772D0, 3.776271728D0,
+     :    0.000296D-6,   -7058.598461315D0, 0.460368852D0,
+     :    0.000306D-6,   10575.406682942D0, 0.554749016D0,
+     :    0.000251D-6,   17298.182327326D0, 0.834332510D0,
+     :    0.000290D-6,    4732.030627343D0, 4.759564091D0,
+     :    0.000261D-6,    5884.926846583D0, 0.298259862D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=621,630) /
+     :    0.000249D-6,    5547.199336460D0, 3.749366406D0,
+     :    0.000213D-6,   11712.955318231D0, 5.415666119D0,
+     :    0.000223D-6,    4701.116501708D0, 2.703203558D0,
+     :    0.000268D-6,    -640.877607382D0, 0.283670793D0,
+     :    0.000209D-6,    5636.065016677D0, 1.238477199D0,
+     :    0.000193D-6,   10177.257679534D0, 1.943251340D0,
+     :    0.000182D-6,    6283.143160294D0, 2.456157599D0,
+     :    0.000184D-6,    -227.526189440D0, 5.888038582D0,
+     :    0.000182D-6,   -6283.008539689D0, 0.241332086D0,
+     :    0.000228D-6,   -6284.056171060D0, 2.657323816D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=631,640) /
+     :    0.000166D-6,    7238.675591600D0, 5.930629110D0,
+     :    0.000167D-6,    3097.883822726D0, 5.570955333D0,
+     :    0.000159D-6,    -323.505416657D0, 5.786670700D0,
+     :    0.000154D-6,   -4136.910433516D0, 1.517805532D0,
+     :    0.000176D-6,   12029.347187887D0, 3.139266834D0,
+     :    0.000167D-6,   12132.439962106D0, 3.556352289D0,
+     :    0.000153D-6,     202.253395174D0, 1.463313961D0,
+     :    0.000157D-6,   17267.268201691D0, 1.586837396D0,
+     :    0.000142D-6,   83996.847317911D0, 0.022670115D0,
+     :    0.000152D-6,   17260.154654690D0, 0.708528947D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=641,650) /
+     :    0.000144D-6,    6084.003848555D0, 5.187075177D0,
+     :    0.000135D-6,    5756.566278634D0, 1.993229262D0,
+     :    0.000134D-6,    5750.203491159D0, 3.457197134D0,
+     :    0.000144D-6,    5326.786694021D0, 6.066193291D0,
+     :    0.000160D-6,   11015.106477335D0, 1.710431974D0,
+     :    0.000133D-6,    3634.621024518D0, 2.836451652D0,
+     :    0.000134D-6,   18073.704938650D0, 5.453106665D0,
+     :    0.000134D-6,    1162.474704408D0, 5.326898811D0,
+     :    0.000128D-6,    5642.198242609D0, 2.511652591D0,
+     :    0.000160D-6,     632.783739313D0, 5.628785365D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=651,660) /
+     :    0.000132D-6,   13916.019109642D0, 0.819294053D0,
+     :    0.000122D-6,   14314.168113050D0, 5.677408071D0,
+     :    0.000125D-6,   12359.966151546D0, 5.251984735D0,
+     :    0.000121D-6,    5749.452731634D0, 2.210924603D0,
+     :    0.000136D-6,    -245.831646229D0, 1.646502367D0,
+     :    0.000120D-6,    5757.317038160D0, 3.240883049D0,
+     :    0.000134D-6,   12146.667056108D0, 3.059480037D0,
+     :    0.000137D-6,    6206.809778716D0, 1.867105418D0,
+     :    0.000141D-6,   17253.041107690D0, 2.069217456D0,
+     :    0.000129D-6,   -7477.522860216D0, 2.781469314D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=661,670) /
+     :    0.000116D-6,    5540.085789459D0, 4.281176991D0,
+     :    0.000116D-6,    9779.108676125D0, 3.320925381D0,
+     :    0.000129D-6,    5237.921013804D0, 3.497704076D0,
+     :    0.000113D-6,    5959.570433334D0, 0.983210840D0,
+     :    0.000122D-6,    6282.095528923D0, 2.674938860D0,
+     :    0.000140D-6,     -11.045700264D0, 4.957936982D0,
+     :    0.000108D-6,   23543.230504682D0, 1.390113589D0,
+     :    0.000106D-6,  -12569.674818332D0, 0.429631317D0,
+     :    0.000110D-6,    -266.607041722D0, 5.501340197D0,
+     :    0.000115D-6,   12559.038152982D0, 4.691456618D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=671,680) /
+     :    0.000134D-6,   -2388.894020449D0, 0.577313584D0,
+     :    0.000109D-6,   10440.274292604D0, 6.218148717D0,
+     :    0.000102D-6,    -543.918059096D0, 1.477842615D0,
+     :    0.000108D-6,   21228.392023546D0, 2.237753948D0,
+     :    0.000101D-6,   -4535.059436924D0, 3.100492232D0,
+     :    0.000103D-6,      76.266071276D0, 5.594294322D0,
+     :    0.000104D-6,     949.175608970D0, 5.674287810D0,
+     :    0.000101D-6,   13517.870106233D0, 2.196632348D0,
+     :    0.000100D-6,   11933.367960670D0, 4.056084160D0,
+     :    4.322990D-6,    6283.075849991D0, 2.642893748D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=681,690) /
+     :    0.406495D-6,       0.000000000D0, 4.712388980D0,
+     :    0.122605D-6,   12566.151699983D0, 2.438140634D0,
+     :    0.019476D-6,     213.299095438D0, 1.642186981D0,
+     :    0.016916D-6,     529.690965095D0, 4.510959344D0,
+     :    0.013374D-6,      -3.523118349D0, 1.502210314D0,
+     :    0.008042D-6,      26.298319800D0, 0.478549024D0,
+     :    0.007824D-6,     155.420399434D0, 5.254710405D0,
+     :    0.004894D-6,    5746.271337896D0, 4.683210850D0,
+     :    0.004875D-6,    5760.498431898D0, 0.759507698D0,
+     :    0.004416D-6,    5223.693919802D0, 6.028853166D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=691,700) /
+     :    0.004088D-6,      -7.113547001D0, 0.060926389D0,
+     :    0.004433D-6,   77713.771467920D0, 3.627734103D0,
+     :    0.003277D-6,   18849.227549974D0, 2.327912542D0,
+     :    0.002703D-6,    6062.663207553D0, 1.271941729D0,
+     :    0.003435D-6,    -775.522611324D0, 0.747446224D0,
+     :    0.002618D-6,    6076.890301554D0, 3.633715689D0,
+     :    0.003146D-6,     206.185548437D0, 5.647874613D0,
+     :    0.002544D-6,    1577.343542448D0, 6.232904270D0,
+     :    0.002218D-6,    -220.412642439D0, 1.309509946D0,
+     :    0.002197D-6,    5856.477659115D0, 2.407212349D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=701,710) /
+     :    0.002897D-6,    5753.384884897D0, 5.863842246D0,
+     :    0.001766D-6,     426.598190876D0, 0.754113147D0,
+     :    0.001738D-6,    -796.298006816D0, 2.714942671D0,
+     :    0.001695D-6,     522.577418094D0, 2.629369842D0,
+     :    0.001584D-6,    5507.553238667D0, 1.341138229D0,
+     :    0.001503D-6,    -242.728603974D0, 0.377699736D0,
+     :    0.001552D-6,    -536.804512095D0, 2.904684667D0,
+     :    0.001370D-6,    -398.149003408D0, 1.265599125D0,
+     :    0.001889D-6,   -5573.142801634D0, 4.413514859D0,
+     :    0.001722D-6,    6069.776754553D0, 2.445966339D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=711,720) /
+     :    0.001124D-6,    1059.381930189D0, 5.041799657D0,
+     :    0.001258D-6,     553.569402842D0, 3.849557278D0,
+     :    0.000831D-6,     951.718406251D0, 2.471094709D0,
+     :    0.000767D-6,    4694.002954708D0, 5.363125422D0,
+     :    0.000756D-6,    1349.867409659D0, 1.046195744D0,
+     :    0.000775D-6,     -11.045700264D0, 0.245548001D0,
+     :    0.000597D-6,    2146.165416475D0, 4.543268798D0,
+     :    0.000568D-6,    5216.580372801D0, 4.178853144D0,
+     :    0.000711D-6,    1748.016413067D0, 5.934271972D0,
+     :    0.000499D-6,   12036.460734888D0, 0.624434410D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=721,730) /
+     :    0.000671D-6,   -1194.447010225D0, 4.136047594D0,
+     :    0.000488D-6,    5849.364112115D0, 2.209679987D0,
+     :    0.000621D-6,    6438.496249426D0, 4.518860804D0,
+     :    0.000495D-6,   -6286.598968340D0, 1.868201275D0,
+     :    0.000456D-6,    5230.807466803D0, 1.271231591D0,
+     :    0.000451D-6,    5088.628839767D0, 0.084060889D0,
+     :    0.000435D-6,    5643.178563677D0, 3.324456609D0,
+     :    0.000387D-6,   10977.078804699D0, 4.052488477D0,
+     :    0.000547D-6,  161000.685737473D0, 2.841633844D0,
+     :    0.000522D-6,    3154.687084896D0, 2.171979966D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=731,740) /
+     :    0.000375D-6,    5486.777843175D0, 4.983027306D0,
+     :    0.000421D-6,    5863.591206116D0, 4.546432249D0,
+     :    0.000439D-6,    7084.896781115D0, 0.522967921D0,
+     :    0.000309D-6,    2544.314419883D0, 3.172606705D0,
+     :    0.000347D-6,    4690.479836359D0, 1.479586566D0,
+     :    0.000317D-6,     801.820931124D0, 3.553088096D0,
+     :    0.000262D-6,     419.484643875D0, 0.606635550D0,
+     :    0.000248D-6,    6836.645252834D0, 3.014082064D0,
+     :    0.000245D-6,   -1592.596013633D0, 5.519526220D0,
+     :    0.000225D-6,    4292.330832950D0, 2.877956536D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=741,750) /
+     :    0.000214D-6,    7234.794256242D0, 1.605227587D0,
+     :    0.000205D-6,    5767.611978898D0, 0.625804796D0,
+     :    0.000180D-6,   10447.387839604D0, 3.499954526D0,
+     :    0.000229D-6,     199.072001436D0, 5.632304604D0,
+     :    0.000214D-6,     639.897286314D0, 5.960227667D0,
+     :    0.000175D-6,    -433.711737877D0, 2.162417992D0,
+     :    0.000209D-6,     515.463871093D0, 2.322150893D0,
+     :    0.000173D-6,    6040.347246017D0, 2.556183691D0,
+     :    0.000184D-6,    6309.374169791D0, 4.732296790D0,
+     :    0.000227D-6,  149854.400134205D0, 5.385812217D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=751,760) /
+     :    0.000154D-6,    8031.092263058D0, 5.120720920D0,
+     :    0.000151D-6,    5739.157790895D0, 4.815000443D0,
+     :    0.000197D-6,    7632.943259650D0, 0.222827271D0,
+     :    0.000197D-6,      74.781598567D0, 3.910456770D0,
+     :    0.000138D-6,    6055.549660552D0, 1.397484253D0,
+     :    0.000149D-6,   -6127.655450557D0, 5.333727496D0,
+     :    0.000137D-6,    3894.181829542D0, 4.281749907D0,
+     :    0.000135D-6,    9437.762934887D0, 5.979971885D0,
+     :    0.000139D-6,   -2352.866153772D0, 4.715630782D0,
+     :    0.000142D-6,    6812.766815086D0, 0.513330157D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=761,770) /
+     :    0.000120D-6,   -4705.732307544D0, 0.194160689D0,
+     :    0.000131D-6,  -71430.695617928D0, 0.000379226D0,
+     :    0.000124D-6,    6279.552731642D0, 2.122264908D0,
+     :    0.000108D-6,   -6256.777530192D0, 0.883445696D0,
+     :    0.143388D-6,    6283.075849991D0, 1.131453581D0,
+     :    0.006671D-6,   12566.151699983D0, 0.775148887D0,
+     :    0.001480D-6,     155.420399434D0, 0.480016880D0,
+     :    0.000934D-6,     213.299095438D0, 6.144453084D0,
+     :    0.000795D-6,     529.690965095D0, 2.941595619D0,
+     :    0.000673D-6,    5746.271337896D0, 0.120415406D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=771,780) /
+     :    0.000672D-6,    5760.498431898D0, 5.317009738D0,
+     :    0.000389D-6,    -220.412642439D0, 3.090323467D0,
+     :    0.000373D-6,    6062.663207553D0, 3.003551964D0,
+     :    0.000360D-6,    6076.890301554D0, 1.918913041D0,
+     :    0.000316D-6,     -21.340641002D0, 5.545798121D0,
+     :    0.000315D-6,    -242.728603974D0, 1.884932563D0,
+     :    0.000278D-6,     206.185548437D0, 1.266254859D0,
+     :    0.000238D-6,    -536.804512095D0, 4.532664830D0,
+     :    0.000185D-6,     522.577418094D0, 4.578313856D0,
+     :    0.000245D-6,   18849.227549974D0, 0.587467082D0 /
+      DATA ((FAIRHD(I,J),I=1,3),J=781,787) /
+     :    0.000180D-6,     426.598190876D0, 5.151178553D0,
+     :    0.000200D-6,     553.569402842D0, 5.355983739D0,
+     :    0.000141D-6,    5223.693919802D0, 1.336556009D0,
+     :    0.000104D-6,    5856.477659115D0, 4.239842759D0,
+     :    0.003826D-6,    6283.075849991D0, 5.705257275D0,
+     :    0.000303D-6,   12566.151699983D0, 5.407132842D0,
+     :    0.000209D-6,     155.420399434D0, 1.989815753D0 /
+* -----------------------------------------------------------------------
+
+
+
+*  Time since J2000.0 in Julian millennia
+      T=(TDB-51544.5D0)/365250D0
+
+* -------------------- Topocentric terms -------------------------------
+
+*  Convert UT1 to local solar time in radians
+      TSOL = MOD(UT1,1D0)*D2PI - WL
+
+*  Planetary arguments:  taken or derived from Bretagnon 1982
+
+*  RLp = mean longitude, mean equinox of date
+*  RGp = mean anomaly
+*  RTp = mean longitude difference, EMB minus planet
+
+*  EMB
+      RLE = MOD (1.75347031435D0 + 6283.3196666635D0 * T, D2PI)
+      RGE = MOD (6.24005997418D0 + 6283.0195512850D0 * T, D2PI)
+*  Jupiter
+      RTJ = MOD (1.15392381696D0 + 5753.3848591241D0 * T, D2PI)
+*  Saturn
+      RTS = MOD (0.87945355785D0 + 6069.7767103654D0 * T, D2PI)
+
+*  Lunar mean elongation:  derived from Meeus 1984.
+      RDMOON = MOD (5.198468D0 + 77713.77144D0 * T, D2PI)
+
+*  Topocentric terms (Moyer 1981 and Murray 1983)
+      WT =  + 0.00029D-10 * U * SIN (TSOL+RTS)
+     :      + 0.00100D-10 * U * SIN (TSOL-2D0*RGE)
+     :      + 0.00133D-10 * U * SIN (TSOL-RDMOON)
+     :      + 0.00133D-10 * U * SIN (TSOL+RTJ)
+     :      - 0.00229D-10 * U * SIN (TSOL+2D0*RLE+RGE)
+     :      - 0.0220 D-10 * V * SIN (RLE+RGE)
+     :      + 0.05312D-10 * U * SIN (TSOL-RGE)
+     :      - 0.13677D-10 * U * SIN (TSOL+2D0*RLE)
+     :      - 1.3184 D-10 * V * COS (RLE)
+     :      + 3.17679D-10 * U * SIN (TSOL)
+
+* --------------- Fairhead model ---------------------------------------
+
+*  T**0
+      W0=0D0
+      DO I=474,1,-1
+         W0=W0+FAIRHD(1,I)*SIN(FAIRHD(2,I)*T+FAIRHD(3,I))
+      END DO
+
+*  T**1
+      W1=0D0
+      DO I=679,475,-1
+         W1=W1+FAIRHD(1,I)*SIN(FAIRHD(2,I)*T+FAIRHD(3,I))
+      END DO
+
+*  T**2
+      W2=0D0
+      DO I=764,680,-1
+         W2=W2+FAIRHD(1,I)*SIN(FAIRHD(2,I)*T+FAIRHD(3,I))
+      END DO
+
+*  T**3
+      W3=0D0
+      DO I=784,765,-1
+         W3=W3+FAIRHD(1,I)*SIN(FAIRHD(2,I)*T+FAIRHD(3,I))
+      END DO
+
+*  T**4
+      W4=0D0
+      DO I=787,785,-1
+         W4=W4+FAIRHD(1,I)*SIN(FAIRHD(2,I)*T+FAIRHD(3,I))
+      END DO
+
+*  Multiply by powers of T and combine
+      WF=T*(T*(T*(T*W4+W3)+W2)+W1)+W0
+
+*  Adjustments to use JPL planetary masses instead of IAU
+      WJ=     0.00065D-6  * SIN(   6069.776754D0   *T + 4.021194D0   ) +
+     :        0.00033D-6  * SIN(    213.299095D0   *T + 5.543132D0   ) +
+     :      (-0.00196D-6  * SIN(   6208.294251D0   *T + 5.696701D0   ))+
+     :      (-0.00173D-6  * SIN(     74.781599D0   *T + 2.435900D0   ))+
+     :        0.03638D-6*T*T
+
+* -----------------------------------------------------------------------
+
+*  Final result:  TDB-TT in seconds
+      sla_RCC=WT+WF+WJ
+
+      END
diff --git a/src/slalib/rdplan.f b/src/slalib/rdplan.f
new file mode 100644
index 0000000..e00ec1d
--- /dev/null
+++ b/src/slalib/rdplan.f
@@ -0,0 +1,183 @@
+      SUBROUTINE sla_RDPLAN (DATE, NP, ELONG, PHI, RA, DEC, DIAM)
+*+
+*     - - - - - - -
+*      R D P L A N
+*     - - - - - - -
+*
+*  Approximate topocentric apparent RA,Dec of a planet, and its
+*  angular diameter.
+*
+*  Given:
+*     DATE        d       MJD of observation (JD - 2400000.5)
+*     NP          i       planet: 1 = Mercury
+*                                 2 = Venus
+*                                 3 = Moon
+*                                 4 = Mars
+*                                 5 = Jupiter
+*                                 6 = Saturn
+*                                 7 = Uranus
+*                                 8 = Neptune
+*                                 9 = Pluto
+*                              else = Sun
+*     ELONG,PHI   d       observer's east longitude and geodetic
+*                                               latitude (radians)
+*
+*  Returned:
+*     RA,DEC      d        RA, Dec (topocentric apparent, radians)
+*     DIAM        d        angular diameter (equatorial, radians)
+*
+*  Notes:
+*
+*  1  The date is in a dynamical timescale (TDB, formerly ET) and is
+*     in the form of a Modified Julian Date (JD-2400000.5).  For all
+*     practical purposes, TT can be used instead of TDB, and for many
+*     applications UT will do (except for the Moon).
+*
+*  2  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 sla_DMOON and sla_PLANET.
+*
+*  3  The direction accuracy (arcsec, 1000-3000AD) is of order:
+*
+*            Sun              5
+*            Mercury          2
+*            Venus           10
+*            Moon            30
+*            Mars            50
+*            Jupiter         90
+*            Saturn          90
+*            Uranus          90
+*            Neptune         10
+*            Pluto            1   (1885-2099AD only)
+*
+*     The angular diameter accuracy is about 0.4% for the Moon,
+*     and 0.01% or better for the Sun and planets.
+*
+*  See the sla_PLANET routine for references.
+*
+*  Called: sla_GMST, sla_DT, sla_EPJ, sla_DMOON, sla_PVOBS, sla_PRENUT,
+*          sla_PLANET, sla_DMXV, sla_DCC2S, sla_DRANRM
+*
+*  P.T.Wallace   Starlink   26 May 1997
+*
+*  Copyright (C) 1997 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DATE
+      INTEGER NP
+      DOUBLE PRECISION ELONG,PHI,RA,DEC,DIAM
+
+*  AU in km
+      DOUBLE PRECISION AUKM
+      PARAMETER (AUKM=1.49597870D8)
+
+*  Light time for unit distance (sec)
+      DOUBLE PRECISION TAU
+      PARAMETER (TAU=499.004782D0)
+
+      INTEGER IP,J,I
+      DOUBLE PRECISION EQRAU(0:9),STL,VGM(6),V(6),RMAT(3,3),
+     :                 VSE(6),VSG(6),VSP(6),VGO(6),DX,DY,DZ,R,TL
+      DOUBLE PRECISION sla_GMST,sla_DT,sla_EPJ,sla_DRANRM
+
+*  Equatorial radii (km)
+      DATA EQRAU / 696000D0,2439.7D0,6051.9D0,1738D0,3397D0,71492D0,
+     :             60268D0,25559D0,24764D0,1151D0 /
+
+
+
+*  Classify NP
+      IP=NP
+      IF (IP.LT.0.OR.IP.GT.9) IP=0
+
+*  Approximate local ST
+      STL=sla_GMST(DATE-sla_DT(sla_EPJ(DATE))/86400D0)+ELONG
+
+*  Geocentre to Moon (mean of date)
+      CALL sla_DMOON(DATE,V)
+
+*  Nutation to true of date
+      CALL sla_NUT(DATE,RMAT)
+      CALL sla_DMXV(RMAT,V,VGM)
+      CALL sla_DMXV(RMAT,V(4),VGM(4))
+
+*  Moon?
+      IF (IP.EQ.3) THEN
+
+*     Yes: geocentre to Moon (true of date)
+         DO I=1,6
+            V(I)=VGM(I)
+         END DO
+      ELSE
+
+*     No: precession/nutation matrix, J2000 to date
+         CALL sla_PRENUT(2000D0,DATE,RMAT)
+
+*     Sun to Earth-Moon Barycentre (J2000)
+         CALL sla_PLANET(DATE,3,V,J)
+
+*     Precession and nutation to date
+         CALL sla_DMXV(RMAT,V,VSE)
+         CALL sla_DMXV(RMAT,V(4),VSE(4))
+
+*     Sun to geocentre (true of date)
+         DO I=1,6
+            VSG(I)=VSE(I)-0.012150581D0*VGM(I)
+         END DO
+
+*     Sun?
+         IF (IP.EQ.0) THEN
+
+*        Yes: geocentre to Sun
+            DO I=1,6
+               V(I)=-VSG(I)
+            END DO
+         ELSE
+
+*        No: Sun to Planet (J2000)
+            CALL sla_PLANET(DATE,IP,V,J)
+
+*        Precession and nutation to date
+            CALL sla_DMXV(RMAT,V,VSP)
+            CALL sla_DMXV(RMAT,V(4),VSP(4))
+
+*        Geocentre to planet
+            DO I=1,6
+               V(I)=VSP(I)-VSG(I)
+            END DO
+         END IF
+      END IF
+
+*  Refer to origin at the observer
+      CALL sla_PVOBS(PHI,0D0,STL,VGO)
+      DO I=1,6
+         V(I)=V(I)-VGO(I)
+      END DO
+
+*  Geometric distance (AU)
+      DX=V(1)
+      DY=V(2)
+      DZ=V(3)
+      R=SQRT(DX*DX+DY*DY+DZ*DZ)
+
+*  Light time (sec)
+      TL=TAU*R
+
+*  Correct position for planetary aberration
+      DO I=1,3
+         V(I)=V(I)-TL*V(I+3)
+      END DO
+
+*  To RA,Dec
+      CALL sla_DCC2S(V,RA,DEC)
+      RA=sla_DRANRM(RA)
+
+*  Angular diameter (radians)
+      DIAM=2D0*ASIN(EQRAU(IP)/(R*AUKM))
+
+      END
diff --git a/src/slalib/read.me b/src/slalib/read.me
new file mode 100644
index 0000000..bfa92ba
--- /dev/null
+++ b/src/slalib/read.me
@@ -0,0 +1,441 @@
+READ.ME
+
+Revision date 17 August 1999                       SLALIB Version 2.4-0
+
+-----------------------------------------------------------------------
+
+FILES IN THE ORIGINAL SOURCE DIRECTORY (VAX)
+
+   READ.ME           this file
+   *.FOR             Fortran source (separate modules)
+   *.OBS             ditto, but obsolete routines
+   *.NEW             ditto, but new and not yet ready for release
+   *.VAX             Fortran source for VAX/VMS
+   *.CNVX            Fortran source for Convex
+   *.MIPS            Fortran source for DECstation
+   *.SUN4            Fortran source for Sun SPARCstation
+   *.LNX             Fortran source for Linux
+   *.PCM             Microsoft Fortran source for PC
+   *.C               C functions needed for Linux version
+   PC.BAT            rebuilds PC version
+   REP.BAT           on PC, compiles one module and updates library
+   CREATE.COM        complete rebuild of VAX and Unix releases
+   PUT.COM           compile one module and update libraries
+   VAX_TO_UNIX.USH   script to complete transfer to Unix platforms
+   SLA.NEWS          NEWS item for latest release
+   MAKEFILE          Unix make file
+   MK                C-shell script to run make
+   SUN67.TEX         document
+
+FILES IN [.RELEASE] DIRECTORY ON VAX
+
+   SLALIB.OLB        object library
+   SLALIB.TLB        source library
+   SUN67.TEX         document
+
+FILES IN [.UNIX] DIRECTORY ON VAX
+
+   MAKEFILE          make file for DECstation and Sun SPARC
+   MK                C-shell script to run make
+   SLA.A             archive file containing everything else
+   VAX_TO_UNIX       script to complete transfer to Unix platforms
+   SLA.NEWS          NEWS item for latest release
+   SUN67.TEX         document
+
+FILES IN (INFORMAL) FTP DIRECTORIES
+
+   The files distributed informally through anonymous FTP may differ
+   slightly in both content and name from the ones listed above.  For
+   example the PC Fortran modules may be stored in archive files and
+   called xxx.f_pcm rather than XXX.PCM etc.
+
+-----------------------------------------------------------------------
+
+DISTRIBUTION - THIS DIRECTORY
+
+   Nothing from this directory needs to be distributed.
+
+DISTRIBUTION - [.RELEASE] DIRECTORY
+
+   SLALIB.*          SLALIB_DIR
+   SLA.NEWS          SLALIB_DIR
+   SUN67.TEX         DOCSDIR
+
+INSTRUCTIONS FOR SAVING SPACE
+
+   Extract from the SLALIB_DIR BACKUP save set only the file SLALIB.OLB.
+
+-----------------------------------------------------------------------
+
+PORTING FORTRAN SLALIB TO OTHER SYSTEMS
+
+FORTRAN SLALIB runs on VAX (VMS), PC (Linux+f2c), PC (Microsoft FORTRAN),
+Convex (ConvexOS), DECstation (Ultrix), DEC Alpha (OSF-1) and Sun
+SPARCstation (SunOS and Solaris).
+
+For most platforms, the required changes are confined to these routines:
+
+    sla_GRESID
+    sla_RANDOM
+    sla_WAIT
+
+VAX, CONVEX, DECSTATION/ALPHA, SUN & PC
+
+Versions suitable for the above platforms are supplied in the
+development directory as *.VAX, *,CNVX, *.MIPS, *.SUN4, *.PCM and
+*.LNX respectively.
+
+
+-----------------------------------------------------------------------
+
+LATEST RELEASE INFORMATION
+
+The latest release of SLALIB includes the following changes (most recent
+at the end):
+
+*  In sla_RCC, the topocentric term of coefficient 1.3184D-10 sec
+   had the wrong sign.  Minus is correct.
+
+*  The IAU decided in 1991 to rename the Terrestrial Dynamical
+   Time, TDT, which is now called "Terrestrial Time" or TT.
+   Appropriate changes have been made in the SLALIB documentation.
+   The same IAU resolutions introduced the timescales TCG and TCB;
+   there are at present no SLALIB routines to handle these new
+   timescales.
+
+*  The Keck 1 Telescope has been added to sla_OBS.
+
+*  The handling of the random-number seed in the PC versions of
+   sla_RANDOM and sla_GRESID was flawed and has been improved.
+
+*  The UTC leap second at the end of June 1993 has been added to the
+   routine sla_DAT.  Existing applications which call sla_DAT or
+   sla_DTT require relinking.
+
+*  Some unnecessary code in sla_AMPQK has been removed.
+
+*  Minor reorganization of the sla_REFRO code has led to an improvement
+   in speed of about 20%, and precautions have been taken against
+   potential arithmetic errors.
+
+*  There have been small revisions to sla_FK425 and sla_FK524.  The
+   results are not significantly affected, except in the pathological
+   case of large proper motion combined with immense distance, where
+   sla_FK524 could produce erroneous radial velocity values.  The
+   latest versions are close to the algorithms published in the 1992
+   Explanatory Supplement to the Astronomical Almanac.
+
+*  The leap second at the end of June 1994 has been added to sla_DAT.
+
+*  THE SLA_RVLSR ROUTINE HAS BEEN RETIRED.  Its place has been taken
+   by two new routines: sla_RVLSRK and sla_RVLSRD.  The original
+   sla_RVLSR had used a "kinematical" LSR.  When this was later changed
+   to a "dynamical" LSR for (what seemed liked good reasons at the time),
+   the small differences were noticed by spectral-line radio observers,
+   who had to fall back on old copies of the routine to remain consistent
+   with existing practice.  The new routines provide both sorts of LSR:
+   sla_RVLSRK uses a kinematical LSR and sla_RVLSRD uses the dynamical LSR.
+
+*  The sla_PA routine (computation of parallactic angle) used an
+   unnecessarily complicated formulation, which has been simplified.
+   The results are unaffected.
+
+*  The sla_ZD routine (computation of zenith distance) used a
+   straightforward cosine-formula-based method, which suffered from
+   decreased accuracy near the zenith.  A better, vector-derived,
+   formulation has been substituted, without materially affecting
+   the results.  Because sla_ZD is double precision, the old
+   formulation was always adequate;  however, had anyone transcribed
+   the code in single precision errors approaching 1 arcmin could
+   have resulted.  The new formulation delivers good results all
+   over the sky even in a single precision version.
+
+*  Routines have been added to transform equatorial coordinates
+   (HA,Dec) to horizon coordinates (Az,El) and back.  Single and
+   double precision are both supported.  The routines are called
+   sla_E2H, sla_DE2H, sla_H2E, sla_DH2E.
+
+*  A new routine has been added to the tangent-plane projection set.
+   The single and double precision versions are called sla_TPRD and
+   sla_DTPRD respectively.  Given the RA,Dec of a star and its
+   xi,eta coordinates, the routine determines the "plate centre".
+
+*  The existing routine sla_PREC for obtaining the precession matrix
+   uses the official IAU model and should continue to be used for
+   canonical purposes.  A new version, called sla_PRECL, uses a
+   more up-to-date model which delivers better accuracy, especially
+   over intervals of millennia.
+
+*  The routine sla_PVOBS was returning velocities in AU per sidereal
+   second rather than per UT second.  This has been corrected.  The
+   maximum error was equivalent to about 0.001 km/s.
+
+*  In sla_MAPQK and sla_MAPQKZ, the area within which the gravitional
+   light-deflection term is restrained has been extended from its
+   original 300 arcsec radius to about 920 arcsec, just inside the
+   Sun's disc.
+
+*  A chapter of explanation, with examples, has been added to SUN/67,
+   which has also undergone various cosmetic revisions.
+
+*  There were two discrepancies between the documentation of sla_DCMPF
+   (program comments and SUN/67) and the code.  The first was that the
+   formulae for the nonperpendicularity used PERP instead of PERP/2;
+   the documentation has been corrected.  The other was that the
+   documentation showed the zero point corrections being applied first,
+   whereas the code returned zero point corrections corresponding to
+   being applied last.  The code has been corrected to match the
+   documentation.
+
+*  The C module slaCldj gave incorrect answers for dates during
+   January and February.  The error, which did not affect the Fortran
+   version, has been corrected.
+
+*  THE CALLS FOR sla_TPRD AND sla_DTPRD HAS BEEN CHANGED.  An integer
+   status argument has been added;  non-zero means the supplied RA,Dec
+   and Xi,Eta describe an impossible case.  (This can only happen
+   near the pole and with non-zero Xi.)  Also, a slightly neater
+   formulation has been introduced.
+
+*  Three new routines have been added.  sla_ALTAZ takes a star's HA,Dec
+   and produces position, velocity and acceleration for azimuth,
+   elevation and parallactic angle.  sla_PDA2H predicts the HA at which
+   a given azimuth will be reached.  sla_PDQ2H does the same for
+   position angle.
+
+*  In the sla_OBS routine, the wrong sign was returned for the Perkins
+   72 inch telescope at Lowell - fixed.
+
+*  A revised model for the equation of the equinoxes has been
+   installed in sla_EQEQX, in line with recent IAU resolutions.  The
+   change amounts to less than 3 mas.
+
+*  A bug in sla_DFLTIN has been corrected.  A negative number following
+   an E- or D-format number without intervening spaces lost its sign.
+
+*  Four stations have been added to sla_OBS:
+
+     TAUTENBERG  Tautenberg 1.34 metre Schmidt
+     PALOMAR48   Palomar 48-inch Schmidt
+     UKST        UK 1.2 metre Schmidt, Siding Spring
+     KISO        Kiso 1.05 metre Schmidt, Japan
+     ESOSCHMIDT  ESO 1 metre Schmidt, La Silla
+
+*  The sla_EARTH and sla_MOON routines could give an integer divide by zero
+   for years before 1 BC.  This has been corrected.
+
+*  sla_CALYD (provided to support the sla_EARTH and sla_MOON routines)
+   has been upgraded to work outside the interval 1900 March 1 to
+   2100 February 28.  The status value indicating dates outside that
+   range has been dropped;  a new error value for year before -4711
+   has been introduced.
+
+*  A new routine, sla_CLYD, has been added.  It is a version of sla_CALYD
+   without the century-default feature and is to enable 1st-century
+   dates to be supplied to sla_EARTH and sla_MOON.
+
+*  Two new routines, sla_PLANET and sla_RDPLAN, have been added, which
+   compute approximate planetary ephemerides.
+
+*  A new routine, sla_DMOON, implements the same (Meeus) model as the
+   sla_MOON routine, but in full and in double precision.  The time
+   argument is a straightforward MJD rather than sla_MOON's year and
+   day-in-year.
+
+*  The sla_REFRO code has been speeded up by a factor of two (and is
+   also clearer).
+
+*  sla_REFV and sla_REFZ have, in different ways, been made more accurate
+   for cases close to the horizon.  The improvement to sla_REFV is
+   relatively modest, but sla_REFZ is now capable of delivering useful
+   results for rise/set phenomena.
+
+*  sla_AOPQK has been speeded up for low-elevation cases.
+
+*  Versions of the tangent-plane routines working directly in x,y,z
+   instead of spherical coordinates have been added.  They may be
+   faster in some applications.  The routines are sla_DV2TP, sla_V2TP,
+   sla_DTP2V, sla_TP2V, sla_DTPXYZ, sla_TPXYZ.
+
+*  The coordinates of the Australia Telescope Compact Array have been
+   added to sla_OBS.  The name is 'ATCA'.
+
+*  Despite their recent introduction THE ROUTINES sla_DTPRD, sla_DTPXYZ,
+   sla_TPRD AND sla_TPXYZ HAVE BEEN WITHDRAWN.  They have been replaced
+   by the new routines sla_DTPS2C, sla_DTPV2C, sla_TPS2C and sla_TPV2C.
+   These are functionally equivalent to the earlier routines but return
+   two solutions instead of one:  the second solution can arise near a
+   pole.
+
+*  The UTC leap second at the end of 1995 has been added to sla_DAT.
+
+*  The refraction routine sla_REFRO has been extensively revised.  The
+   principal motivation was to improve the radio predictions by
+   introducing better humidity models.  The models previously in
+   use had been entirely adequate for the optical case, for which
+   they had been devised, but improved models were required for
+   the radio case.  None of the changes significantly affects the
+   optical results with respect to the earlier version of the sla_REFRO
+   routine.  For example, at 70 deg zenith distance the new version
+   agrees with the old version to better than 0.05 arcsec for any
+   reasonable combination of parameters.  However, the improved
+   water-vapour expressions do make a significant difference in the
+   radio band, at 70 deg zenith distance reaching almost 4 arcsec
+   for a hot, humid, low-altitude site during a period of low pressure.
+
+*  There was a bug in slaRdplan, the (private) C version of sla_RDPLAN.
+   The answers were unaffected but there could be floating-point
+   problems on some platforms.
+
+*  A new routine has been added, sla_GMSTA.  This gives greater numerical
+   precision than the existing GMST function by allowing the date and
+   time to be specified separately rather than as a single MJD.
+
+*  Measures taken in sla_MAPQK to avoid trouble when processing Solar
+   positions had not been carried through into sla_MAPQKZ.  The two
+   routines now use the same strategy.
+
+*  In sla_REFRO, at zenith distances well beyond 90 deg and under some
+   conditions, it was possible to encounter arithmetic errors due to
+   failure of the tropospheric model-atmosphere to deliver sensible
+   temperatures.  This is inherent in the published algorithm.  To
+   avoid the problem, the temperature delivered by the model has been
+   constrained to the range 200 to 320 deg K.
+
+*  A new routine has been added, sla_ATMDSP, for rapidly recalculating
+   the A,B refraction coefficients for different wavelengths.
+
+*  The first UTC leap-second date in the sla_DAT routine was one day early.
+   This will have had no effect on the results for more recent epochs.
+
+*  slaObs, the C version of sla_OBS, had some problems related to character
+   string handling.  A call using the "number" option retured an invalid
+   station ID, and station ID and name strings of the stipulated 10
+   and 40 character lengths were improperly terminated.
+
+*  A new routine, sla_POLMO has been added.  This is a specialist tool
+   to do with Earth polar motion.
+
+*  sla_DC62S and sla_CC62S could give floating point errors if vectors in
+   unlikely units were supplied.  The handling of difficult cases  has
+   been improved.
+
+*  Support for Linux has been added.
+
+*  slaRefreo, the C version of sla_REFRO, was not re-entrant.  It is now;
+   there has been a small (4%) speed penalty.
+
+*  The C routines slaRandom, slaGresid and slaWait have been dropped.
+   They could not easily be made re-entrant and posed perennial platform-
+   dependency problems.
+
+*  The value for the arcsec to radians factor in several routines
+   had an incorrect (and superfluous) 19th digit, which has been
+   removed.
+
+*  There was a minor bug in sla_DV2TP and sla_V2TP, to do with protection
+   against the special case where the tangent point is the pole.
+
+*  In sla_OBS, the position of the Parkes radiotelescope has been revised,
+   and the ATNF Mopra observatory has been added.
+
+*  Two new routines have been added.  sla_PAV (single precision) and
+   sla_DPAV (double precision) are like sla_BEAR and sla_DBEAR but start
+   with direction cosines rather than spherical coordinates - they return
+   the position angle of one point with respect to the other.
+
+*  slaRefro, the C version of sla_REFRO, still wasn't re-entrant, but is
+   now.
+
+*  slaDtf2d, the C version of sla_DTF2D, used to accept 60.0 in the seconds
+   field;  this has been corrected.
+
+*  The sla_PLANET and sla_RDPLAN routines now include Pluto.  The ephemeris
+   is accurate (sub-arcsecond) but covers the 20th and 21st centuries
+   only.
+
+   !!!  IMPORTANT NOTE  !!!
+
+   sla_RDPLAN used to interpret any planet number outside the range 1-8
+   as meaning the Sun.  The new version uses planet number 9.  Existing
+   programs using 9 for the Sun should be changed to use 0.  The rule
+   has not been changed, except that the range is now 1-9 instead of
+   1-8, as it is unlikely that the equivalent problem will arise in the
+   future.
+
+*  Two new routines have been added, sla_PLANEL and sla_PLANTE.  They are
+   analogues of sla_PLANET and sla_RDPLAN but for the case where orbital
+   elements are available.  They can be used for predicting the
+   positions of asteroids and comets, and, if up-to-date osculating
+   elements are supplied, more accurate positions for the major
+   planets than can be provided through the sla_PLANET and sla_RDPLAN
+   routines.
+
+*  The sla_REFRO routine could give inaccurate results for low temperatures
+   (subzero C).  This was caused by over-cautious defensive programming,
+   which prevented the tropospheric temperature falling below 200 K.
+
+*  A new routine has been added, sla_REFCOQ.  This calculates the coefficients
+   of a two-term refraction model.  It complements the existing sla_REFCO
+   routine, being much faster at the expense of some accuracy.
+
+*  The 1997 July 1 UTC leap second has been added to the sla_DAT routine.
+
+*  A bug in slaSvd, the C version of sla_SVD, caused occasional false
+   indications of ill-conditioning.  The results of least-squares
+   fits do not seem to have been affected.  The Fortran version did not
+   have the bug.
+
+*  The Subaru telescope (Japanese National 8-metre telescope, Mauna Kea)
+   has been added to the sla_OBS routine.
+
+*  The sla_DAT routine has been extended back to the inception of UTC in
+   1960.
+
+*  The "earliest date possible" in DJCL sla_was two days out (disagreeing
+   with sla_DJCAL, which had the correct value).
+
+*  The sla_GMSTA code has been improved.
+
+*  A new routine, sla_PV2EL, takes a heliocentric J2000 equatorial position
+   and velocity and produces the equivalent set of osculating elements.
+
+*  The 1999 January 1 UTC leap second has been added to the sla_DAT routine.
+
+*  Four new routines have been introduced which transform between the
+   FK5 system and the ICRS (Hipparcos) system.  sla_FK52H and sla_H2FK5
+   transform star positions and proper motions from FK5 coordinates to
+   Hipparcos coordinates and vice versa.  sla_FK5HZ and sla_HFK5Z do the
+   same but for the case where the Hipparcos proper motions are zero.
+
+*  Six new routines have been introduced for dealing with orbital elements.
+   Four of them (sla_EL2UE, sla_PV2UE, sla_UE2EL and sla_UE2PV) provide
+   applications with direct access to the "universal variables" method
+   that was already being used internally.  Compared with using conventional
+   (angular) elements and solving Kepler's equation, the universal variables
+   approach has a number of advantages, including better handling of near-
+   parabolic orbits and greater efficiency.  The remaining two routines
+   (sla_PERTEL and sla_PERTUE) generate updated elements by applying
+   major-planet perturbations.  The new elements can then be used to
+   predict positions that are much more accurate.  For minor planets,
+   sub-arcsecond accuracy over a decade is achievable.
+
+*  Several observatory sites have been added to the OBS routine:  CFHT,
+   Keck 2, Gemini North, FCRAO, IRTF and CSO.  The coordinates for all
+   the Mauna Kea sites have been updated in accordance with recent aerial
+   photography results made available by the Institute for Astronomy,
+   University of Hawaii.
+
+*  A bug in sla_DAT has been corrected.  It used to give incorrect
+   results for dates in the first 54 days of 1972.
+
+*  There are new routines for generating permutations (sla_PERMUT) and
+   combinations (sla_COMBN).
+
+-----------------------------------------------------------------------
+
+
+ P.T.Wallace
+
+ ptw@star.rl.ac.uk
+ +44-1235-44-5372
diff --git a/src/slalib/refco.f b/src/slalib/refco.f
new file mode 100644
index 0000000..3bc8816
--- /dev/null
+++ b/src/slalib/refco.f
@@ -0,0 +1,70 @@
+      SUBROUTINE sla_REFCO (HM, TDK, PMB, RH, WL, PHI, TLR, EPS,
+     :                      REFA, REFB)
+*+
+*     - - - - - -
+*      R E F C O
+*     - - - - - -
+*
+*  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.
+*
+*  Given:
+*    HM      d     height of the observer above sea level (metre)
+*    TDK     d     ambient temperature at the observer (deg K)
+*    PMB     d     pressure at the observer (millibar)
+*    RH      d     relative humidity at the observer (range 0-1)
+*    WL      d     effective wavelength of the source (micrometre)
+*    PHI     d     latitude of the observer (radian, astronomical)
+*    TLR     d     temperature lapse rate in the troposphere (degK/metre)
+*    EPS     d     precision required to terminate iteration (radian)
+*
+*  Returned:
+*    REFA    d     tan Z coefficient (radian)
+*    REFB    d     tan**3 Z coefficient (radian)
+*
+*  Called:  sla_REFRO
+*
+*  Notes:
+*
+*  1  Typical values for the TLR and EPS arguments might be 0.0065D0 and
+*     1D-10 respectively.
+*
+*  2  The radio refraction is chosen by specifying WL > 100 micrometres.
+*
+*  3  The routine is a slower but more accurate alternative to the
+*     sla_REFCOQ routine.  The constants it produces give perfect
+*     agreement with sla_REFRO 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.
+*
+*  P.T.Wallace   Starlink   3 June 1997
+*
+*  Copyright (C) 1997 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION HM,TDK,PMB,RH,WL,PHI,TLR,EPS,REFA,REFB
+
+      DOUBLE PRECISION ATN1,ATN4,R1,R2
+
+*  Sample zenith distances: arctan(1) and arctan(4)
+      PARAMETER (ATN1=0.7853981633974483D0,
+     :           ATN4=1.325817663668033D0)
+
+
+
+*  Determine refraction for the two sample zenith distances
+      CALL sla_REFRO(ATN1,HM,TDK,PMB,RH,WL,PHI,TLR,EPS,R1)
+      CALL sla_REFRO(ATN4,HM,TDK,PMB,RH,WL,PHI,TLR,EPS,R2)
+
+*  Solve for refraction constants
+      REFA = (64D0*R1-R2)/60D0
+      REFB = (R2-4D0*R1)/60D0
+
+      END
diff --git a/src/slalib/refcoq.f b/src/slalib/refcoq.f
new file mode 100644
index 0000000..15e3af0
--- /dev/null
+++ b/src/slalib/refcoq.f
@@ -0,0 +1,208 @@
+      SUBROUTINE sla_REFCOQ (TDK, PMB, RH, WL, REFA, REFB)
+*+
+*     - - - - - - -
+*      R E F C O Q
+*     - - - - - - -
+*
+*  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 sla_REFCO routine - see notes.
+*
+*  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.
+*
+*  Given:
+*    TDK      d      ambient temperature at the observer (deg K)
+*    PMB      d      pressure at the observer (millibar)
+*    RH       d      relative humidity at the observer (range 0-1)
+*    WL       d      effective wavelength of the source (micrometre)
+*
+*  Returned:
+*    REFA     d      tan Z coefficient (radian)
+*    REFB     d      tan**3 Z coefficient (radian)
+*
+*  The radio refraction is chosen by specifying WL > 100 micrometres.
+*
+*  Notes:
+*
+*  1  The model is an approximation, for moderate zenith distances,
+*     to the predictions of the sla_REFRO routine.  The approximation
+*     is maintained across a range of conditions, and applies to
+*     both optical/IR and radio.
+*
+*  2  The algorithm is a fast alternative to the sla_REFCO routine.
+*     The latter calls the sla_REFRO routine itself:  this involves
+*     integrations through a model atmosphere, and is costly in
+*     processor time.  However, the model which is produced is precisely
+*     correct for two zenith distance (45 degrees and about 76 degrees)
+*     and at other zenith distances is limited in accuracy only by the
+*     A tan Z + B tan**3 Z formulation itself.  The present routine
+*     is not as accurate, though it satisfies most practical
+*     requirements.
+*
+*  3  The model omits the effects of (i) height above sea level (apart
+*     from the reduced pressure itself), (ii) latitude (i.e. the
+*     flattening of the Earth) and (iii) variations in tropospheric
+*     lapse rate.
+*
+*     The model was tested using the following range of conditions:
+*
+*       lapse rates 0.0055, 0.0065, 0.0075 deg/metre
+*       latitudes 0, 25, 50, 75 degrees
+*       heights 0, 2500, 5000 metres ASL
+*       pressures mean for height -10% to +5% in steps of 5%
+*       temperatures -10 deg to +20 deg with respect to 280 deg at SL
+*       relative humidity 0, 0.5, 1
+*       wavelengths 0.4, 0.6, ... 2 micron, + radio
+*       zenith distances 15, 45, 75 degrees
+*
+*     The accuracy with respect to direct use of the sla_REFRO routine
+*     was as follows:
+*
+*                            worst         RMS
+*
+*       optical/IR           62 mas       8 mas
+*       radio               319 mas      49 mas
+*
+*     For this particular set of conditions:
+*
+*       lapse rate 0.0065 degK/metre
+*       latitude 50 degrees
+*       sea level
+*       pressure 1005 mB
+*       temperature 280.15 degK
+*       humidity 80%
+*       wavelength 5740 Angstroms
+*
+*     the results were as follows:
+*
+*       ZD        sla_REFRO   sla_REFCOQ  Saastamoinen
+*
+*       10         10.27        10.27        10.27
+*       20         21.19        21.20        21.19
+*       30         33.61        33.61        33.60
+*       40         48.82        48.83        48.81
+*       45         58.16        58.18        58.16
+*       50         69.28        69.30        69.27
+*       55         82.97        82.99        82.95
+*       60        100.51       100.54       100.50
+*       65        124.23       124.26       124.20
+*       70        158.63       158.68       158.61
+*       72        177.32       177.37       177.31
+*       74        200.35       200.38       200.32
+*       76        229.45       229.43       229.42
+*       78        267.44       267.29       267.41
+*       80        319.13       318.55       319.10
+*
+*      deg        arcsec       arcsec       arcsec
+*
+*     The values for Saastamoinen's formula (which includes terms
+*     up to tan^5) are taken from Hohenkerk and Sinclair (1985).
+*
+*     The results from the much slower but more accurate sla_REFCO
+*     routine have not been included in the tabulation as they are
+*     identical to those in the sla_REFRO column to the 0.01 arcsec
+*     resolution used.
+*
+*  4  Outlandish input parameters are silently limited to mathematically
+*     safe values.  Zero pressure is permissible, and causes zeroes to
+*     be returned.
+*
+*  5  The algorithm draws on several sources, as follows:
+*
+*     a) The formula for the saturation vapour pressure of water as
+*        a function of temperature and temperature is taken from
+*        expressions A4.5-A4.7 of Gill (1982).
+*
+*     b) The formula for the water vapour pressure, given the
+*        saturation pressure and the relative humidity, is from
+*        Crane (1976), expression 2.5.5.
+*
+*     c) The refractivity of air is a function of temperature,
+*        total pressure, water-vapour pressure and, in the case
+*        of optical/IR but not radio, wavelength.  The formulae
+*        for the two cases are developed from the Essen and Froome
+*        expressions adopted in Resolution 1 of the 12th International
+*        Geodesy Association General Assembly (1963).
+*
+*     The above three items are as used in the sla_REFRO routine.
+*
+*     d) The formula for beta, the ratio of the scale height of the
+*        atmosphere to the geocentric distance of the observer, is
+*        an adaption of expression 9 from Stone (1996).  The
+*        adaptations, arrived at empirically, consist of (i) a
+*        small adjustment to the coefficient and (ii) a humidity
+*        term for the radio case only.
+*
+*     e) The formulae for the refraction constants as a function of
+*        n-1 and beta are from Green (1987), expression 4.31.
+*
+*  References:
+*
+*     Crane, R.K., Meeks, M.L. (ed), "Refraction Effects in the Neutral
+*     Atmosphere", Methods of Experimental Physics: Astrophysics 12B,
+*     Academic Press, 1976.
+*
+*     Gill, Adrian E., "Atmosphere-Ocean Dynamics", Academic Press, 1982.
+*
+*     Hohenkerk, C.Y., & Sinclair, A.T., NAO Technical Note No. 63, 1985.
+*
+*     International Geodesy Association General Assembly, Bulletin
+*     Geodesique 70 p390, 1963.
+*
+*     Stone, Ronald C., P.A.S.P. 108 1051-1058, 1996.
+*
+*     Green, R.M., "Spherical Astronomy", Cambridge University Press, 1987.
+*
+*  P.T.Wallace   Starlink   4 June 1997
+*
+*  Copyright (C) 1997 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION TDK,PMB,RH,WL,REFA,REFB
+
+      LOGICAL OPTIC
+      DOUBLE PRECISION T,P,R,W,TDC,PS,PW,WLSQ,GAMMA,BETA
+
+
+
+*  Decide whether optical/IR or radio case:  switch at 100 microns.
+      OPTIC = WL.LE.100D0
+
+*  Restrict parameters to safe values.
+      T = MIN(MAX(TDK,100D0),500D0)
+      P = MIN(MAX(PMB,0D0),10000D0)
+      R = MIN(MAX(RH,0D0),1D0)
+      W = MIN(MAX(WL,0.1D0),1D6)
+
+*  Water vapour pressure at the observer.
+      IF (P.GT.0D0) THEN
+         TDC = T-273.15D0
+         PS = 10D0**((0.7859D0+0.03477D0*TDC)/(1D0+0.00412D0*TDC))*
+     :                                    (1D0+P*(4.5D-6+6D-10*TDC*TDC))
+         PW = R*PS/(1D0-(1D0-R)*PS/P)
+      ELSE
+         PW = 0D0
+      END IF
+
+*  Refractive index minus 1 at the observer.
+      IF (OPTIC) THEN
+         WLSQ = WL*WL
+         GAMMA = ((77.532D-6+(4.391D-7+3.57D-9/WLSQ)/WLSQ)*P
+     :                                                 -11.2684D-6*PW)/T
+      ELSE
+         GAMMA = (77.624D-6*P-(12.92D-6-0.371897D0/T)*PW)/T
+      END IF
+
+*  Formula for beta adapted from Stone, with empirical adjustments.
+      BETA=4.4474D-6*T
+      IF (.NOT.OPTIC) BETA=BETA-0.0074D0*PW*BETA
+
+*  Refraction constants from Green.
+      REFA = GAMMA*(1D0-BETA)
+      REFB = -GAMMA*(BETA-GAMMA/2D0)
+
+      END
diff --git a/src/slalib/refro.f b/src/slalib/refro.f
new file mode 100644
index 0000000..8d11184
--- /dev/null
+++ b/src/slalib/refro.f
@@ -0,0 +1,374 @@
+      SUBROUTINE sla_REFRO (ZOBS, HM, TDK, PMB, RH, WL, PHI, TLR,
+     :                      EPS, REF)
+*+
+*     - - - - - -
+*      R E F R O
+*     - - - - - -
+*
+*  Atmospheric refraction for radio and optical/IR wavelengths.
+*
+*  Given:
+*    ZOBS    d  observed zenith distance of the source (radian)
+*    HM      d  height of the observer above sea level (metre)
+*    TDK     d  ambient temperature at the observer (deg K)
+*    PMB     d  pressure at the observer (millibar)
+*    RH      d  relative humidity at the observer (range 0-1)
+*    WL      d  effective wavelength of the source (micrometre)
+*    PHI     d  latitude of the observer (radian, astronomical)
+*    TLR     d  temperature lapse rate in the troposphere (degK/metre)
+*    EPS     d  precision required to terminate iteration (radian)
+*
+*  Returned:
+*    REF     d  refraction: in vacuo ZD minus observed ZD (radian)
+*
+*  Notes:
+*
+*  1  A suggested value for the TLR argument is 0.0065D0.  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.
+*
+*  2  A suggested value for the EPS argument is 1D-8.  The result is
+*     usually at least two orders of magnitude more computationally
+*     precise than the supplied EPS value.
+*
+*  3  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).
+*
+*  4  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).
+*
+*     .  Provision for radio wavelengths has been added using
+*        expressions devised by A.T.Sinclair, RGO (private
+*        communication 1989), based on the Essen & Froome
+*        refractivity formula adopted in Resolution 1 of the
+*        13th International Geodesy Association General Assembly
+*        (Bulletin Geodesique 70 p390, 1963).
+*
+*     .  Various small changes have been made to gain speed.
+*
+*     None of the changes significantly affects the optical/IR results
+*     with respect to the algorithm given in the 1992 Explanatory
+*     Supplement.  For example, at 70 deg zenith distance the present
+*     routine agrees with the ES algorithm to better than 0.05 arcsec
+*     for any reasonable combination of parameters.  However, the
+*     improved water-vapour expressions do make a significant difference
+*     in the radio band, at 70 deg zenith distance reaching almost
+*     4 arcsec for a hot, humid, low-altitude site during a period of
+*     low pressure.
+*
+*  5  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.
+*
+*  6  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.
+*
+*  7  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.
+*
+*  8  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.
+*
+*  9  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).
+*
+*  Called:  sla_DRANGE, sla__ATMT, sla__ATMS
+*
+*  P.T.Wallace   Starlink   3 June 1997
+*
+*  Copyright (C) 1997 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION ZOBS,HM,TDK,PMB,RH,WL,PHI,TLR,EPS,REF
+
+*
+*  Fixed parameters
+*
+      DOUBLE PRECISION D93,GCR,DMD,DMW,S,DELTA,HT,HS
+*  93 degrees in radians
+      PARAMETER (D93=1.623156204D0)
+*  Universal gas constant
+      PARAMETER (GCR=8314.32D0)
+*  Molecular weight of dry air
+      PARAMETER (DMD=28.9644D0)
+*  Molecular weight of water vapour
+      PARAMETER (DMW=18.0152D0)
+*  Mean Earth radius (metre)
+      PARAMETER (S=6378120D0)
+*  Exponent of temperature dependence of water vapour pressure
+      PARAMETER (DELTA=18.36D0)
+*  Height of tropopause (metre)
+      PARAMETER (HT=11000D0)
+*  Upper limit for refractive effects (metre)
+      PARAMETER (HS=80000D0)
+
+      INTEGER IS,K,N,I,J
+      LOGICAL OPTIC,LOOP
+      DOUBLE PRECISION 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
+
+      DOUBLE PRECISION sla_DRANGE
+
+*  The refraction integrand
+      DOUBLE PRECISION REFI
+      REFI(R,DN,RDNDR) = RDNDR/(DN+RDNDR)
+
+
+
+*  Transform ZOBS into the normal range.
+      ZOBS1 = sla_DRANGE(ZOBS)
+      ZOBS2 = MIN(ABS(ZOBS1),D93)
+
+*  Keep other arguments within safe bounds.
+      HMOK = MIN(MAX(HM,-1D3),10D3)
+      TDKOK = MIN(MAX(TDK,100D0),500D0)
+      PMBOK = MIN(MAX(PMB,0D0),10000D0)
+      RHOK = MIN(MAX(RH,0D0),1D0)
+      WLOK = MAX(WL,0.1D0)
+      ALPHA = MIN(MAX(ABS(TLR),0.001D0),0.01D0)
+
+*  Tolerance for iteration.
+      TOL = MIN(MAX(ABS(EPS),1D-12),0.1D0)/2D0
+
+*  Decide whether optical/IR or radio case - switch at 100 microns.
+      OPTIC = WLOK.LE.100D0
+
+*  Set up model atmosphere parameters defined at the observer.
+      WLSQ = WLOK*WLOK
+      GB = 9.784D0*(1D0-0.0026D0*COS(PHI+PHI)-0.00000028D0*HMOK)
+      IF (OPTIC) THEN
+         A = (287.604D0+(1.6288D0+0.0136D0/WLSQ)/WLSQ)
+     :                                              *273.15D-6/1013.25D0
+      ELSE
+         A = 77.624D-6
+      END IF
+      GAMAL = (GB*DMD)/GCR
+      GAMMA = GAMAL/ALPHA
+      GAMM2 = GAMMA-2D0
+      DELM2 = DELTA-2D0
+      TDC = TDKOK-273.15D0
+      PSAT = 10D0**((0.7859D0+0.03477D0*TDC)/(1D0+0.00412D0*TDC))*
+     :                                (1D0+PMBOK*(4.5D-6+6D-10*TDC*TDC))
+      IF (PMBOK.GT.0D0) THEN
+         PWO = RHOK*PSAT/(1D0-(1D0-RHOK)*PSAT/PMBOK)
+      ELSE
+         PWO = 0D0
+      END IF
+      W = PWO*(1D0-DMW/DMD)*GAMMA/(DELTA-GAMMA)
+      C1 = A*(PMBOK+W)/TDKOK
+      IF (OPTIC) THEN
+         C2 = (A*W+11.2684D-6*PWO)/TDKOK
+      ELSE
+         C2 = (A*W+12.92D-6*PWO)/TDKOK
+      END IF
+      C3 = (GAMMA-1D0)*ALPHA*C1/TDKOK
+      C4 = (DELTA-1D0)*ALPHA*C2/TDKOK
+      IF (OPTIC) THEN
+         C5 = 0D0
+         C6 = 0D0
+      ELSE
+         C5 = 371897D-6*PWO/TDKOK
+         C6 = C5*DELM2*ALPHA/(TDKOK*TDKOK)
+      END IF
+
+*  Conditions at the observer.
+      R0 = S+HMOK
+      CALL sla__ATMT(R0,TDKOK,ALPHA,GAMM2,DELM2,C1,C2,C3,C4,C5,C6,
+     :                                              R0,TEMPO,DN0,RDNDR0)
+      SK0 = DN0*R0*SIN(ZOBS2)
+      F0 = REFI(R0,DN0,RDNDR0)
+
+*  Conditions in the troposphere at the tropopause.
+      RT = S+HT
+      CALL sla__ATMT(R0,TDKOK,ALPHA,GAMM2,DELM2,C1,C2,C3,C4,C5,C6,
+     :                                                 RT,TT,DNT,RDNDRT)
+      SINE = SK0/(RT*DNT)
+      ZT = ATAN2(SINE,SQRT(MAX(1D0-SINE*SINE,0D0)))
+      FT = REFI(RT,DNT,RDNDRT)
+
+*  Conditions in the stratosphere at the tropopause.
+      CALL sla__ATMS(RT,TT,DNT,GAMAL,RT,DNTS,RDNDRP)
+      SINE = SK0/(RT*DNTS)
+      ZTS = ATAN2(SINE,SQRT(MAX(1D0-SINE*SINE,0D0)))
+      FTS = REFI(RT,DNTS,RDNDRP)
+
+*  Conditions at the stratosphere limit.
+      RS = S+HS
+      CALL sla__ATMS(RT,TT,DNT,GAMAL,RS,DNS,RDNDRS)
+      SINE = SK0/(RS*DNS)
+      ZS = ATAN2(SINE,SQRT(MAX(1D0-SINE*SINE,0D0)))
+      FS = REFI(RS,DNS,RDNDRS)
+
+*
+*  Integrate the refraction integral in two parts;  first in the
+*  troposphere (K=1), then in the stratosphere (K=2).
+*
+
+*  Initialize previous refraction to ensure at least two iterations.
+      REFOLD = 1D6
+
+*  Start off with 8 strips for the troposphere integration, and then
+*  use the final troposphere value for the stratosphere integration,
+*  which tends to need more strips.
+      IS = 8
+
+*  Troposphere then stratosphere.
+      DO K = 1,2
+
+*     Start Z, Z range, and start and end values.
+         IF (K.EQ.1) THEN
+            Z0 = ZOBS2
+            ZRANGE = ZT-Z0
+            FB = F0
+            FF = FT
+         ELSE
+            Z0 = ZTS
+            ZRANGE = ZS-Z0
+            FB = FTS
+            FF = FS
+         END IF
+
+*     Sums of odd and even values.
+         FO = 0D0
+         FE = 0D0
+
+*     First time through the loop we have to do every point.
+         N = 1
+
+*     Start of iteration loop (terminates at specified precision).
+         LOOP = .TRUE.
+         DO WHILE (LOOP)
+
+*        Strip width.
+            H = ZRANGE/DBLE(IS)
+
+*        Initialize distance from Earth centre for quadrature pass.
+            IF (K.EQ.1) THEN
+               R = R0
+            ELSE
+               R = RT
+            END IF
+
+*        One pass (no need to compute evens after first time).
+            DO I=1,IS-1,N
+
+*           Sine of observed zenith distance.
+               SZ = SIN(Z0+H*DBLE(I))
+
+*           Find R (to the nearest metre, maximum four iterations).
+               IF (SZ.GT.1D-20) THEN
+                  W = SK0/SZ
+                  RG = R
+                  DR = 1D6
+                  J = 0
+                  DO WHILE (ABS(DR).GT.1D0.AND.J.LT.4)
+                     J=J+1
+                     IF (K.EQ.1) THEN
+                        CALL sla__ATMT(R0,TDKOK,ALPHA,GAMM2,DELM2,
+     :                                 C1,C2,C3,C4,C5,C6,RG,TG,DN,RDNDR)
+                     ELSE
+                        CALL sla__ATMS(RT,TT,DNT,GAMAL,RG,DN,RDNDR)
+                     END IF
+                     DR = (RG*DN-W)/(DN+RDNDR)
+                     RG = RG-DR
+                  END DO
+                  R = RG
+               END IF
+
+*           Find the refractive index and integrand at R.
+               IF (K.EQ.1) THEN
+                  CALL sla__ATMT(R0,TDKOK,ALPHA,GAMM2,DELM2,
+     :                                   C1,C2,C3,C4,C5,C6,R,T,DN,RDNDR)
+               ELSE
+                  CALL sla__ATMS(RT,TT,DNT,GAMAL,R,DN,RDNDR)
+               END IF
+               F = REFI(R,DN,RDNDR)
+
+*           Accumulate odd and (first time only) even values.
+               IF (N.EQ.1.AND.MOD(I,2).EQ.0) THEN
+                  FE = FE+F
+               ELSE
+                  FO = FO+F
+               END IF
+            END DO
+
+*        Evaluate the integrand using Simpson's Rule.
+            REFP = H*(FB+4D0*FO+2D0*FE+FF)/3D0
+
+*        Has the required precision been achieved?
+            IF (ABS(REFP-REFOLD).GT.TOL) THEN
+
+*           No: prepare for next iteration.
+
+*           Save current value for convergence test.
+               REFOLD = REFP
+
+*           Double the number of strips.
+               IS = IS+IS
+
+*           Sum of all current values = sum of next pass's even values.
+               FE = FE+FO
+
+*           Prepare for new odd values.
+               FO = 0D0
+
+*           Skip even values next time.
+               N = 2
+            ELSE
+
+*           Yes: save troposphere component and terminate the loop.
+               IF (K.EQ.1) REFT = REFP
+               LOOP = .FALSE.
+            END IF
+         END DO
+      END DO
+
+*  Result.
+      REF = REFT+REFP
+      IF (ZOBS1.LT.0D0) REF = -REF
+
+      END
diff --git a/src/slalib/refv.f b/src/slalib/refv.f
new file mode 100644
index 0000000..e81b03c
--- /dev/null
+++ b/src/slalib/refv.f
@@ -0,0 +1,106 @@
+      SUBROUTINE sla_REFV (VU, REFA, REFB, VR)
+*+
+*     - - - - -
+*      R E F V
+*     - - - - -
+*
+*  Adjust an unrefracted Cartesian vector to include the effect of
+*  atmospheric refraction, using the simple A tan Z + B tan**3 Z
+*  model.
+*
+*  Given:
+*    VU    dp    unrefracted position of the source (Az/El 3-vector)
+*    REFA  dp    tan Z coefficient (radian)
+*    REFB  dp    tan**3 Z coefficient (radian)
+*
+*  Returned:
+*    VR    dp    refracted position of the source (Az/El 3-vector)
+*
+*  Notes:
+*
+*  1  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.
+*
+*  2  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.
+*
+*  3  At low elevations (below about 3 degrees) the refraction
+*     correction is held back to prevent arithmetic problems and
+*     wildly wrong results.  Over a wide range of observer heights
+*     and corresponding temperatures and pressures, the following
+*     levels of accuracy (arcsec) are achieved, relative to numerical
+*     integration through a model atmosphere:
+*
+*              ZD    error
+*
+*              80      0.4
+*              81      0.8
+*              82      1.6
+*              83      3
+*              84      7
+*              85     17
+*              86     45
+*              87    150
+*              88    340
+*              89    620
+*              90   1100
+*              91   1900         } relevant only to
+*              92   3200         } high-elevation sites
+*
+*  4  See also the routine sla_REFZ, which performs the adjustment to
+*     the zenith distance rather than in Cartesian Az/El coordinates.
+*     The present routine is faster than sla_REFZ and, except very low down,
+*     is equally accurate for all practical purposes.  However, beyond
+*     about ZD 84 degrees sla_REFZ should be used, and for the utmost
+*     accuracy iterative use of sla_REFRO should be considered.
+*
+*  P.T.Wallace   Starlink   26 December 1994
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION VU(3),REFA,REFB,VR(3)
+
+      DOUBLE PRECISION X,Y,Z1,Z,ZSQ,RSQ,R,WB,WT,D,CD,F
+
+
+
+*  Initial estimate = unrefracted vector
+      X = VU(1)
+      Y = VU(2)
+      Z1 = VU(3)
+
+*  Keep correction approximately constant below about 3 deg elevation
+      Z = MAX(Z1,0.05D0)
+
+*  One Newton-Raphson iteration
+      ZSQ = Z*Z
+      RSQ = X*X+Y*Y
+      R = SQRT(RSQ)
+      WB = REFB*RSQ/ZSQ
+      WT = (REFA+WB)/(1D0+(REFA+3D0*WB)*(ZSQ+RSQ)/ZSQ)
+      D = WT*R/Z
+      CD = 1D0-D*D/2D0
+      F = CD*(1D0-WT)
+
+*  Post-refraction x,y,z
+      VR(1) = X*F
+      VR(2) = Y*F
+      VR(3) = CD*(Z+D*R)+(Z1-Z)
+
+      END
diff --git a/src/slalib/refz.f b/src/slalib/refz.f
new file mode 100644
index 0000000..d558c87
--- /dev/null
+++ b/src/slalib/refz.f
@@ -0,0 +1,139 @@
+      SUBROUTINE sla_REFZ (ZU, REFA, REFB, ZR)
+*+
+*     - - - - -
+*      R E F Z
+*     - - - - -
+*
+*  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).
+*
+*  Given:
+*    ZU    dp    unrefracted zenith distance of the source (radian)
+*    REFA  dp    tan Z coefficient (radian)
+*    REFB  dp    tan**3 Z coefficient (radian)
+*
+*  Returned:
+*    ZR    dp    refracted zenith distance (radian)
+*
+*  Notes:
+*
+*  1  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
+*     sla_REFCO for more information.
+*
+*  2  At ZD 83 degrees, the rapidly-worsening A tan Z + B tan**3 Z
+*     model is abandoned and an empirical formula takes over.  Over a
+*     wide range of observer heights and corresponding temperatures and
+*     pressures, the following levels of accuracy (arcsec) are
+*     typically achieved, relative to numerical integration through a
+*     model atmosphere:
+*
+*              ZR    error
+*
+*              80      0.4
+*              81      0.8
+*              82      1.5
+*              83      3.2
+*              84      4.9
+*              85      5.8
+*              86      6.1
+*              87      7.1
+*              88     10
+*              89     20
+*              90     40
+*              91    100         } relevant only to
+*              92    200         } high-elevation sites
+*
+*     The high-ZD model is scaled to match the normal model at the
+*     transition point;  there is no glitch.
+*
+*  3  Beyond 93 deg zenith distance, the refraction is held at its
+*     93 deg value.
+*
+*  4  See also the routine sla_REFV, which performs the adjustment in
+*     Cartesian Az/El coordinates, and with the emphasis on speed
+*     rather than numerical accuracy.
+*
+*  P.T.Wallace   Starlink   19 September 1995
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION ZU,REFA,REFB,ZR
+
+*  Radians to degrees
+      DOUBLE PRECISION R2D
+      PARAMETER (R2D=57.29577951308232D0)
+
+*  Largest usable ZD (deg)
+      DOUBLE PRECISION D93
+      PARAMETER (D93=93D0)
+
+*  Coefficients for high ZD model (used beyond ZD 83 deg)
+      DOUBLE PRECISION C1,C2,C3,C4,C5
+      PARAMETER (C1=+0.55445D0,
+     :           C2=-0.01133D0,
+     :           C3=+0.00202D0,
+     :           C4=+0.28385D0,
+     :           C5=+0.02390D0)
+
+*  ZD at which one model hands over to the other (radians)
+      DOUBLE PRECISION Z83
+      PARAMETER (Z83=83D0/R2D)
+
+*  High-ZD-model prediction (deg) for that point
+      DOUBLE PRECISION REF83
+      PARAMETER (REF83=(C1+C2*7D0+C3*49D0)/(1D0+C4*7D0+C5*49D0))
+
+      DOUBLE PRECISION ZU1,ZL,S,C,T,TSQ,TCU,REF,E,E2
+
+
+
+*  Perform calculations for ZU or 83 deg, whichever is smaller
+      ZU1 = MIN(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)/(1D0+(REFA+3D0*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)/(1D0+(REFA+3D0*REFB*TSQ)/(C*C))
+
+*  Special handling for large ZU
+      IF (ZU.GT.ZU1) THEN
+         E = 90D0-MIN(D93,ZU*R2D)
+         E2 = E*E
+         REF = (REF/REF83)*(C1+C2*E+C3*E2)/(1D0+C4*E+C5*E2)
+      END IF
+
+*  Return refracted ZD
+      ZR = ZU-REF
+
+      END
diff --git a/src/slalib/rep.bat b/src/slalib/rep.bat
new file mode 100755
index 0000000..0d00777
--- /dev/null
+++ b/src/slalib/rep.bat
@@ -0,0 +1,21 @@
+@echo off
+rem
+rem  - - - - - - - -
+rem   R E P . B A T
+rem  - - - - - - - -
+rem
+rem  Update one module in the SLALIB library
+rem
+rem  Command:
+rem
+rem     REP module
+rem
+rem  File SLALIB.BAK is deleted.
+rem
+rem  P.T.Wallace   Starlink   5 April 1992
+rem
+fl/c /FPi %1.for
+lib slalib -+%1;
+del %1.obj
+del slalib.bak
+echo:
diff --git a/src/slalib/rtl_random.c b/src/slalib/rtl_random.c
new file mode 100644
index 0000000..a8730c0
--- /dev/null
+++ b/src/slalib/rtl_random.c
@@ -0,0 +1,33 @@
+#include <stdlib.h>
+
+float
+random_ ( int *iseed )
+/*
+**  - - - - - - -
+**   r a n d o m
+**  - - - - - - -
+**
+**  Generate pseudo-random real number in the range 0 <= x < 1.
+**
+**  (single precision)
+**
+**  This function is designed to replace the Fortran->C interface routine
+**  random(3f) on systems which do not have this library (for example Linux)
+**
+**  Fortran call:   X = RANDOM(ISEED)
+**
+**  Given:
+**     iseed     int     seed value
+**
+**     If iseed !=0  random-number generator is initialised and first number
+**                   is returned.
+**        iseed == 0 next number in the sequence is returned
+**
+**  B.K.McIlwrath    Starlink   12 January 1996
+*/
+{
+   if( *iseed != 0 )
+      srand(*iseed);
+
+   return (float) rand() / (float) RAND_MAX;
+}
diff --git a/src/slalib/rverot.f b/src/slalib/rverot.f
new file mode 100644
index 0000000..5fbe6d9
--- /dev/null
+++ b/src/slalib/rverot.f
@@ -0,0 +1,48 @@
+      REAL FUNCTION sla_RVEROT (PHI, RA, DA, ST)
+*+
+*     - - - - - - -
+*      R V E R O T
+*     - - - - - - -
+*
+*  Velocity component in a given direction due to Earth rotation
+*  (single precision)
+*
+*  Given:
+*     PHI     real    latitude of observing station (geodetic)
+*     RA,DA   real    apparent RA,DEC
+*     ST      real    local apparent sidereal time
+*
+*  PHI, RA, DEC and ST are all in radians.
+*
+*  Result:
+*     Component of Earth rotation in direction RA,DA (km/s)
+*
+*  Sign convention:
+*     The result is +ve when the observatory is receding from the
+*     given point on the sky.
+*
+*  Accuracy:
+*     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
+*     sla_PVOBS.
+*
+*  P.T.Wallace   Starlink   20 July 1994
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL PHI,RA,DA,ST
+
+*  Nominal mean sidereal speed of Earth equator in km/s (the actual
+*  value is about 0.4651)
+      REAL ESPEED
+      PARAMETER (ESPEED=0.4655)
+
+
+      sla_RVEROT=ESPEED*COS(PHI)*SIN(ST-RA)*COS(DA)
+
+      END
diff --git a/src/slalib/rvgalc.f b/src/slalib/rvgalc.f
new file mode 100644
index 0000000..868c307
--- /dev/null
+++ b/src/slalib/rvgalc.f
@@ -0,0 +1,69 @@
+      REAL FUNCTION sla_RVGALC (R2000, D2000)
+*+
+*     - - - - - - -
+*      R V G A L C
+*     - - - - - - -
+*
+*  Velocity component in a given direction due to the rotation
+*  of the Galaxy (single precision)
+*
+*  Given:
+*     R2000,D2000   real    J2000.0 mean RA,Dec (radians)
+*
+*  Result:
+*     Component of dynamical LSR motion in direction R2000,D2000 (km/s)
+*
+*  Sign convention:
+*     The result is +ve when the dynamical LSR is receding from the
+*     given point on the sky.
+*
+*  Note:  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.
+*
+*  Called:
+*     sla_CS2C, sla_VDV
+*
+*  P.T.Wallace   Starlink   23 March 1994
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL R2000,D2000
+
+      REAL VA(3), VB(3)
+
+      REAL sla_VDV
+
+*
+*  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)
+
+      DATA VA / -108.70408, +97.86251, -164.33610 /
+
+
+
+*  Convert given J2000 RA,Dec to x,y,z
+      CALL sla_CS2C(R2000,D2000,VB)
+
+*  Compute dot product with LSR motion vector
+      sla_RVGALC=sla_VDV(VA,VB)
+
+      END
diff --git a/src/slalib/rvlg.f b/src/slalib/rvlg.f
new file mode 100644
index 0000000..ba0216e
--- /dev/null
+++ b/src/slalib/rvlg.f
@@ -0,0 +1,64 @@
+      REAL FUNCTION sla_RVLG (R2000, D2000)
+*+
+*     - - - - -
+*      R V L G
+*     - - - - -
+*
+*  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 (single precision)
+*
+*  Given:
+*     R2000,D2000   real    J2000.0 mean RA,Dec (radians)
+*
+*  Result:
+*     Component of SOLAR motion in direction R2000,D2000 (km/s)
+*
+*  Sign convention:
+*     The result is +ve when the Sun is receding from the
+*     given point on the sky.
+*
+*  Reference:
+*     IAU Trans 1976, 168, p201.
+*
+*  Called:
+*     sla_CS2C, sla_VDV
+*
+*  P.T.Wallace   Starlink   June 1985
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL R2000,D2000
+
+      REAL VA(3), VB(3)
+
+      REAL sla_VDV
+
+*
+*  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)
+
+      DATA VA / -148.23284, +133.44888, -224.09467 /
+
+
+
+*  Convert given J2000 RA,Dec to x,y,z
+      CALL sla_CS2C(R2000,D2000,VB)
+
+*  Compute dot product with Solar motion vector
+      sla_RVLG=sla_VDV(VA,VB)
+
+      END
diff --git a/src/slalib/rvlsrd.f b/src/slalib/rvlsrd.f
new file mode 100644
index 0000000..96f90c9
--- /dev/null
+++ b/src/slalib/rvlsrd.f
@@ -0,0 +1,78 @@
+      REAL FUNCTION sla_RVLSRD (R2000, D2000)
+*+
+*     - - - - - - -
+*      R V L S R D
+*     - - - - - - -
+*
+*  Velocity component in a given direction due to the Sun's motion
+*  with respect to the dynamical Local Standard of Rest.
+*
+*  (single precision)
+*
+*  Given:
+*     R2000,D2000   r    J2000.0 mean RA,Dec (radians)
+*
+*  Result:
+*     Component of "peculiar" solar motion in direction R2000,D2000 (km/s)
+*
+*  Sign convention:
+*     The result is +ve when the Sun is receding from the given point on
+*     the sky.
+*
+*  Note:  The Local Standard of Rest used here is the "dynamical" LSR,
+*         a point in the vicinity of the Sun which is in a circular
+*         orbit around the Galactic centre.  The Sun's motion with
+*         respect to the dynamical LSR is called the "peculiar" solar
+*         motion.
+*
+*         There is another type of LSR, called a "kinematical" LSR.  A
+*         kinematical LSR is the mean standard of rest of specified star
+*         catalogues or stellar populations, and several slightly
+*         different kinematical LSRs are in use.  The Sun's motion with
+*         respect to an agreed kinematical LSR is known as the "standard"
+*         solar motion.  To obtain a radial velocity correction with
+*         respect to an adopted kinematical LSR use the routine sla_RVLSRK.
+*
+*  Reference:  Delhaye (1965), in "Stars and Stellar Systems", vol 5,
+*              p73.
+*
+*  Called:
+*     sla_CS2C, sla_VDV
+*
+*  P.T.Wallace   Starlink   9 March 1994
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL R2000,D2000
+
+      REAL VA(3), VB(3)
+
+      REAL sla_VDV
+
+*
+*  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)
+
+      DATA VA / +0.63823, +14.58542, -7.80116 /
+
+
+
+*  Convert given J2000 RA,Dec to x,y,z
+      CALL sla_CS2C(R2000,D2000,VB)
+
+*  Compute dot product with solar motion vector
+      sla_RVLSRD=sla_VDV(VA,VB)
+
+      END
diff --git a/src/slalib/rvlsrk.f b/src/slalib/rvlsrk.f
new file mode 100644
index 0000000..b484fe8
--- /dev/null
+++ b/src/slalib/rvlsrk.f
@@ -0,0 +1,77 @@
+      REAL FUNCTION sla_RVLSRK (R2000, D2000)
+*+
+*     - - - - - - -
+*      R V L S R K
+*     - - - - - - -
+*
+*  Velocity component in a given direction due to the Sun's motion
+*  with respect to an adopted kinematic Local Standard of Rest.
+*
+*  (single precision)
+*
+*  Given:
+*     R2000,D2000   r    J2000.0 mean RA,Dec (radians)
+*
+*  Result:
+*     Component of "standard" solar motion in direction R2000,D2000 (km/s)
+*
+*  Sign convention:
+*     The result is +ve when the Sun is receding from the given point on
+*     the sky.
+*
+*  Note:  The Local Standard of Rest used here is one of several
+*         "kinematical" LSRs in common use.  A kinematical LSR is the
+*         mean standard of rest of specified star catalogues or stellar
+*         populations.  The Sun's motion with respect to a kinematical
+*         LSR is known as the "standard" solar motion.
+*
+*         There is another sort of LSR, the "dynamical" LSR, which is a
+*         point in the vicinity of the Sun which is in a circular orbit
+*         around the Galactic centre.  The Sun's motion with respect to
+*         the dynamical LSR is called the "peculiar" solar motion.  To
+*         obtain a radial velocity correction with respect to the
+*         dynamical LSR use the routine sla_RVLSRD.
+*
+*  Reference:  Delhaye (1965), in "Stars and Stellar Systems", vol 5,
+*              p73.
+*
+*  Called:
+*     sla_CS2C, sla_VDV
+*
+*  P.T.Wallace   Starlink   11 March 1994
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL R2000,D2000
+
+      REAL VA(3), VB(3)
+
+      REAL sla_VDV
+
+*
+*  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)
+
+      DATA VA / -0.29000, +17.31726, -10.00141 /
+
+
+
+*  Convert given J2000 RA,Dec to x,y,z
+      CALL sla_CS2C(R2000,D2000,VB)
+
+*  Compute dot product with solar motion vector
+      sla_RVLSRK=sla_VDV(VA,VB)
+
+      END
diff --git a/src/slalib/s2tp.f b/src/slalib/s2tp.f
new file mode 100644
index 0000000..1ec36f2
--- /dev/null
+++ b/src/slalib/s2tp.f
@@ -0,0 +1,67 @@
+      SUBROUTINE sla_S2TP (RA, DEC, RAZ, DECZ, XI, ETA, J)
+*+
+*     - - - - -
+*      S 2 T P
+*     - - - - -
+*
+*  Projection of spherical coordinates onto tangent plane:
+*  "gnomonic" projection - "standard coordinates"
+*  (single precision)
+*
+*  Given:
+*     RA,DEC      real  spherical coordinates of point to be projected
+*     RAZ,DECZ    real  spherical coordinates of tangent point
+*
+*  Returned:
+*     XI,ETA      real  rectangular coordinates on tangent plane
+*     J           int   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
+*
+*  P.T.Wallace   Starlink   18 July 1996
+*
+*  Copyright (C) 1996 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL RA,DEC,RAZ,DECZ,XI,ETA
+      INTEGER J
+
+      REAL SDECZ,SDEC,CDECZ,CDEC,RADIF,SRADIF,CRADIF,DENOM
+
+      REAL TINY
+      PARAMETER (TINY=1E-6)
+
+
+*  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.GT.TINY) THEN
+         J=0
+      ELSE IF (DENOM.GE.0.0) THEN
+         J=1
+         DENOM=TINY
+      ELSE IF (DENOM.GT.-TINY) THEN
+         J=2
+         DENOM=-TINY
+      ELSE
+         J=3
+      END IF
+
+*  Compute tangent plane coordinates (even in dubious cases)
+      XI=CDEC*SRADIF/DENOM
+      ETA=(SDEC*CDECZ-CDEC*SDECZ*CRADIF)/DENOM
+
+      END
diff --git a/src/slalib/sep.f b/src/slalib/sep.f
new file mode 100644
index 0000000..c977985
--- /dev/null
+++ b/src/slalib/sep.f
@@ -0,0 +1,48 @@
+      REAL FUNCTION sla_SEP (A1, B1, A2, B2)
+*+
+*     - - - -
+*      S E P
+*     - - - -
+*
+*  Angle between two points on a sphere (single precision)
+*
+*  Given:
+*     A1,B1    real    spherical coordinates of one point
+*     A2,B2    real    spherical coordinates of the other point
+*
+*  (The spherical coordinates are RA,Dec, Long,Lat etc, in radians.)
+*
+*  The result is the angle, in radians, between the two points.  It
+*  is always positive.
+*
+*  Called:  sla_CS2C
+*
+*  P.T.Wallace   Starlink   April 1985
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL A1,B1,A2,B2
+
+      INTEGER I
+      REAL V1(3),V2(3),W
+
+
+
+*  Convert coordinates from spherical to Cartesian
+      CALL sla_CS2C(A1,B1,V1)
+      CALL sla_CS2C(A2,B2,V2)
+
+*  Modulus squared of half the difference vector
+      W=0.0
+      DO I=1,3
+         W=W+(V1(I)-V2(I))**2
+      END DO
+      W=W/4.0
+
+*  Angle between the vectors
+      sla_SEP=2.0*ATAN2(SQRT(W),SQRT(MAX(0.0,1.0-W)))
+
+      END
diff --git a/src/slalib/sla.news b/src/slalib/sla.news
new file mode 100644
index 0000000..51b2888
--- /dev/null
+++ b/src/slalib/sla.news
@@ -0,0 +1,40 @@
+SLALIB_Version_2.4-0                                  Expiry 31 December 1999
+
+The latest releases of SLALIB include the following changes:
+
+*  Four new routines have been introduced which transform between the
+   FK5 system and the ICRS (Hipparcos) system.  sla_FK52H and sla_H2FK5
+   transform star positions and proper motions from FK5 coordinates to
+   Hipparcos coordinates and vice versa.  sla_FK5HZ and sla_HFK5Z do the
+   same but for the case where the Hipparcos proper motions are zero.
+
+*  Six new routines have been introduced for dealing with orbital elements.
+   Four of them (sla_EL2UE, sla_PV2UE, sla_UE2EL and sla_UE2PV) provide
+   applications with direct access to the "universal variables" method
+   that was already being used internally.  Compared with using conventional
+   (angular) elements and solving Kepler's equation, the universal variables
+   approach has a number of advantages, including better handling of near-
+   parabolic orbits and greater efficiency.  The remaining two routines
+   (sla_PERTEL and sla_PERTUE) generate updated elements by applying
+   major-planet perturbations.  The new elements can then be used to
+   predict positions that are much more accurate.  For minor planets,
+   sub-arcsecond accuracy over a decade is achievable.
+
+*  Several observatory sites have been added to the sla_OBS routine:  CFHT,
+   Keck 2, Gemini North, FCRAO, IRTF and CSO.  The coordinates for all
+   the Mauna Kea sites have been updated in accordance with recent aerial
+   photography results made available by the Institute for Astronomy,
+   University of Hawaii.
+
+*  A bug in sla_DAT has been corrected.  It used to give incorrect
+   results for dates in the first 54 days of 1972.
+
+*  There are new routines for generating permutations (sla_PERMUT) and
+   combinations (sla_COMBN).
+ 
+ P.T.Wallace
+ 17 August 1999
+
+ ptw@star.rl.ac.uk
+ +44-1235-44-5372
+--------------------------------------------------------------------------
diff --git a/src/slalib/sla_link b/src/slalib/sla_link
new file mode 100755
index 0000000..40aa195
--- /dev/null
+++ b/src/slalib/sla_link
@@ -0,0 +1 @@
+echo -lsla
diff --git a/src/slalib/sla_link_adam b/src/slalib/sla_link_adam
new file mode 100755
index 0000000..40aa195
--- /dev/null
+++ b/src/slalib/sla_link_adam
@@ -0,0 +1 @@
+echo -lsla
diff --git a/src/slalib/sla_test.f b/src/slalib/sla_test.f
new file mode 100644
index 0000000..c094c26
--- /dev/null
+++ b/src/slalib/sla_test.f
@@ -0,0 +1,28 @@
+      PROGRAM SLA_TEST
+*+
+*     - - - - -
+*      T E S T
+*     - - - - -
+*
+*  Simple test of SLALIB library - checks that a program can be
+*  linked and a correct result returned from at least one subprogram.
+*
+*  P.T.Wallace   Starlink   24 August 1992
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION D
+      INTEGER J
+
+
+      CALL sla_CALDJ(1946,4,30,D,J)
+      IF (J.EQ.0.AND.NINT(D).EQ.31940) THEN
+         PRINT *,'SLALIB test completed satisfactorily.'
+      ELSE
+         PRINT *,'SLALIB test fails!'
+      END IF
+
+      END
diff --git a/src/slalib/smat.f b/src/slalib/smat.f
new file mode 100644
index 0000000..93dbee7
--- /dev/null
+++ b/src/slalib/smat.f
@@ -0,0 +1,141 @@
+      SUBROUTINE sla_SMAT (N, A, Y, D, JF, IW)
+*+
+*     - - - - -
+*      S M A T
+*     - - - - -
+*
+*  Matrix inversion & solution of simultaneous equations
+*  (single precision)
+*
+*  For the set of n simultaneous equations in n unknowns:
+*     A.Y = X
+*
+*  where:
+*     A is a non-singular N x N matrix
+*     Y is the vector of N unknowns
+*     X is the known vector
+*
+*  SMATRX computes:
+*     the inverse of matrix A
+*     the determinant of matrix A
+*     the vector of N unknowns
+*
+*  Arguments:
+*
+*     symbol  type dimension           before              after
+*
+*       N      int                 no. of unknowns       unchanged
+*       A      real  (N,N)             matrix             inverse
+*       Y      real   (N)              vector            solution
+*       D      real                       -             determinant
+*     * JF     int                        -           singularity flag
+*       IW     int    (N)                 -              workspace
+*
+*  *  JF is 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.
+*
+*  Algorithm:
+*     Gaussian elimination with partial pivoting.
+*
+*  Speed:
+*     Very fast.
+*
+*  Accuracy:
+*     Fairly accurate - errors 1 to 4 times those of routines optimised
+*     for accuracy.
+*
+*  Note:  replaces the obsolete sla_SMATRX routine.
+*
+*  P.T.Wallace   Starlink   10 September 1990
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER N
+      REAL A(N,N),Y(N),D
+      INTEGER JF
+      INTEGER IW(N)
+
+      REAL SFA
+      PARAMETER (SFA=1E-20)
+
+      INTEGER K,IMX,I,J,NP1MK,KI
+      REAL AMX,T,AKK,YK,AIK
+
+
+      JF=0
+      D=1.0
+      DO K=1,N
+         AMX=ABS(A(K,K))
+         IMX=K
+         IF (K.NE.N) THEN
+            DO I=K+1,N
+               T=ABS(A(I,K))
+               IF (T.GT.AMX) THEN
+                  AMX=T
+                  IMX=I
+               END IF
+            END DO
+         END IF
+         IF (AMX.LT.SFA) THEN
+            JF=-1
+         ELSE
+            IF (IMX.NE.K) THEN
+               DO J=1,N
+                  T=A(K,J)
+                  A(K,J)=A(IMX,J)
+                  A(IMX,J)=T
+               END DO
+               T=Y(K)
+               Y(K)=Y(IMX)
+               Y(IMX)=T
+               D=-D
+            END IF
+            IW(K)=IMX
+            AKK=A(K,K)
+            D=D*AKK
+            IF (ABS(D).LT.SFA) THEN
+               JF=-1
+            ELSE
+               AKK=1.0/AKK
+               A(K,K)=AKK
+               DO J=1,N
+                  IF (J.NE.K) A(K,J)=A(K,J)*AKK
+               END DO
+               YK=Y(K)*AKK
+               Y(K)=YK
+               DO I=1,N
+                  AIK=A(I,K)
+                  IF (I.NE.K) THEN
+                     DO J=1,N
+                        IF (J.NE.K) A(I,J)=A(I,J)-AIK*A(K,J)
+                     END DO
+                     Y(I)=Y(I)-AIK*YK
+                  END IF
+               END DO
+               DO I=1,N
+                  IF (I.NE.K) A(I,K)=-A(I,K)*AKK
+               END DO
+            END IF
+         END IF
+      END DO
+      IF (JF.NE.0) THEN
+         D=0.0
+      ELSE
+         DO K=1,N
+            NP1MK=N+1-K
+            KI=IW(NP1MK)
+            IF (NP1MK.NE.KI) THEN
+               DO I=1,N
+                  T=A(I,NP1MK)
+                  A(I,NP1MK)=A(I,KI)
+                  A(I,KI)=T
+               END DO
+            END IF
+         END DO
+      END IF
+      END
diff --git a/src/slalib/subet.f b/src/slalib/subet.f
new file mode 100644
index 0000000..e36575b
--- /dev/null
+++ b/src/slalib/subet.f
@@ -0,0 +1,66 @@
+      SUBROUTINE sla_SUBET (RC, DC, EQ, RM, DM)
+*+
+*     - - - - - -
+*      S U B E T
+*     - - - - - -
+*
+*  Remove the E-terms (elliptic component of annual aberration)
+*  from a pre IAU 1976 catalogue RA,Dec to give a mean place
+*  (double precision)
+*
+*  Given:
+*     RC,DC     dp     RA,Dec (radians) with E-terms included
+*     EQ        dp     Besselian epoch of mean equator and equinox
+*
+*  Returned:
+*     RM,DM     dp     RA,Dec (radians) without E-terms
+*
+*  Called:
+*     sla_ETRMS, sla_DCS2C, sla_,DVDV, sla_DCC2S, sla_DRANRM
+*
+*  Explanation:
+*     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).
+*
+*  Reference:
+*     Explanatory Supplement to the Astronomical Ephemeris,
+*     section 2D, page 48.
+*
+*  P.T.Wallace   Starlink   10 May 1990
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION RC,DC,EQ,RM,DM
+
+      DOUBLE PRECISION sla_DRANRM,sla_DVDV
+      DOUBLE PRECISION A(3),V(3),F
+
+      INTEGER I
+
+
+
+*  E-terms
+      CALL sla_ETRMS(EQ,A)
+
+*  Spherical to Cartesian
+      CALL sla_DCS2C(RC,DC,V)
+
+*  Include the E-terms
+      F=1D0+sla_DVDV(V,A)
+      DO I=1,3
+         V(I)=F*V(I)-A(I)
+      END DO
+
+*  Cartesian to spherical
+      CALL sla_DCC2S(V,RM,DM)
+
+*  Bring RA into conventional range
+      RM=sla_DRANRM(RM)
+
+      END
diff --git a/src/slalib/sun67.htx/blueball.gif b/src/slalib/sun67.htx/blueball.gif
new file mode 100644
index 0000000..c481395
--- /dev/null
+++ b/src/slalib/sun67.htx/blueball.gif
diff --git a/src/slalib/sun67.htx/change_begin.gif b/src/slalib/sun67.htx/change_begin.gif
new file mode 100644
index 0000000..dbe8d7e
--- /dev/null
+++ b/src/slalib/sun67.htx/change_begin.gif
diff --git a/src/slalib/sun67.htx/change_begin_right.gif b/src/slalib/sun67.htx/change_begin_right.gif
new file mode 100644
index 0000000..331ddf2
--- /dev/null
+++ b/src/slalib/sun67.htx/change_begin_right.gif
diff --git a/src/slalib/sun67.htx/change_delete.gif b/src/slalib/sun67.htx/change_delete.gif
new file mode 100644
index 0000000..63398f5
--- /dev/null
+++ b/src/slalib/sun67.htx/change_delete.gif
diff --git a/src/slalib/sun67.htx/change_delete_right.gif b/src/slalib/sun67.htx/change_delete_right.gif
new file mode 100644
index 0000000..63398f5
--- /dev/null
+++ b/src/slalib/sun67.htx/change_delete_right.gif
diff --git a/src/slalib/sun67.htx/change_end.gif b/src/slalib/sun67.htx/change_end.gif
new file mode 100644
index 0000000..8f1e455
--- /dev/null
+++ b/src/slalib/sun67.htx/change_end.gif
diff --git a/src/slalib/sun67.htx/change_end_right.gif b/src/slalib/sun67.htx/change_end_right.gif
new file mode 100644
index 0000000..409246c
--- /dev/null
+++ b/src/slalib/sun67.htx/change_end_right.gif
diff --git a/src/slalib/sun67.htx/contents.xbm b/src/slalib/sun67.htx/contents.xbm
new file mode 100644
index 0000000..a3aed9f
--- /dev/null
+++ b/src/slalib/sun67.htx/contents.xbm
@@ -0,0 +1,12 @@
+#define contents_width 63
+#define contents_height 16
+static char contents_bits[] = {
+ 0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,
+ 0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,
+ 0x00,0x00,0xc0,0x01,0x00,0x08,0x00,0x00,0x01,0x00,0x20,0x02,0x00,0x08,0x00,
+ 0x00,0x01,0x00,0x20,0xe2,0x74,0x7c,0x9c,0x8e,0x8f,0x03,0x20,0x10,0x99,0x08,
+ 0x22,0x13,0x41,0x04,0x20,0x10,0x89,0x08,0x3e,0x11,0x81,0x03,0x20,0x12,0x89,
+ 0x08,0x02,0x11,0x01,0x04,0x20,0x12,0x89,0x88,0x22,0x11,0x51,0x04,0xc0,0xe1,
+ 0x9c,0x71,0x9c,0x33,0x8e,0x03,0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,
+ 0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00,
+ 0x00,0x00,0x00,0x00,0x00,0x00,0x00,0x00};
diff --git a/src/slalib/sun67.htx/contents_motif.gif b/src/slalib/sun67.htx/contents_motif.gif
new file mode 100644
index 0000000..7b3c904
--- /dev/null
+++ b/src/slalib/sun67.htx/contents_motif.gif
diff --git a/src/slalib/sun67.htx/cross_ref_motif.gif b/src/slalib/sun67.htx/cross_ref_motif.gif
new file mode 100644
index 0000000..4c074e1
--- /dev/null
+++ b/src/slalib/sun67.htx/cross_ref_motif.gif
diff --git a/src/slalib/sun67.htx/foot_motif.gif b/src/slalib/sun67.htx/foot_motif.gif
new file mode 100644
index 0000000..f29222a
--- /dev/null
+++ b/src/slalib/sun67.htx/foot_motif.gif
diff --git a/src/slalib/sun67.htx/footnode.html b/src/slalib/sun67.htx/footnode.html
new file mode 100644
index 0000000..b6bcb72
--- /dev/null
+++ b/src/slalib/sun67.htx/footnode.html
@@ -0,0 +1,224 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Footnotes</TITLE>
+<META NAME="description" CONTENT="Footnotes">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="previous" HREF="node228.html">
+<LINK REL="up" HREF="sun67.html">
+</HEAD>
+<BODY >
+<P><DL>
+<DT><A NAME="412">...SLALIB</A>
+<DD>The name isn't an acronym;
+it just stands for ``Subprogram Library&nbsp;A''.
+<PRE>.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+</PRE>
+<DT><A NAME="27724">...papers;</A>
+<DD>One frame not included in
+Figure&nbsp;1 is that of the Hipparcos catalogue.  This is currently the
+best available implementation in the optical of the <I>International
+Celestial Reference System</I> (ICRS), which is based on extragalactic
+radio sources observed by VLBI.  The distinction between FK5 J2000
+and Hipparcos coordinates only becomes important when accuracies of
+50&nbsp;mas or better are required.  More details are given in
+Section&nbsp;4.14.
+<PRE>.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+</PRE>
+<DT><A NAME="27833">...<I>equinox</I>.</A>
+<DD>With
+the introduction of the International Celestial Reference System (ICRS), the
+connection between (i)&nbsp;star coordinates and (ii)&nbsp;the Earth's orientation
+and orbit has been broken.  However, the orientation of the
+International Celestial Reference Frame (ICRF) axes was, for convenience,
+chosen to match J2000 FK5, and for most practical purposes ICRF coordinates
+(for example entries in the Hipparcos catalogue) can be regarded as
+synonymous with J2000 FK5.  See Section 4.14 for further details.
+<PRE>.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+</PRE>
+<DT><A NAME="27903">...used.</A>
+<DD>An equinox is, however, not required for coordinates
+in the International Celestial Reference System.  Such coordinates must
+be labelled simply ``ICRS'', or the specific catalogue can be mentioned,
+such as ``Hipparcos'';  constructions such as ``Hipparcos, J2000'' are
+redundant and misleading.
+<PRE>.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+</PRE>
+<DT><A NAME="28038">...catalogues.</A>
+<DD>This was
+true until the inception of the International Celestial Reference
+System, which is based on the idea of axes locked into the
+distant background.  The coordinates
+of the extragalactic sources which realize these
+axes have no individual significance; there is a ``no net rotation''
+condition which has to be satisfied each time any revisions take
+place.
+<PRE>.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+.
+</PRE>
+</DL><ADDRESS>
+<I>SLALIB -- Positional Astronomy Library
+<BR>
+Starlink User Note 67
+<BR>
+P. T. Wallace
+<BR>
+12 October 1999
+<BR>
+E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/greenball.gif b/src/slalib/sun67.htx/greenball.gif
new file mode 100644
index 0000000..2ffbb22
--- /dev/null
+++ b/src/slalib/sun67.htx/greenball.gif
diff --git a/src/slalib/sun67.htx/icons.html b/src/slalib/sun67.htx/icons.html
new file mode 100644
index 0000000..d6b38c3
--- /dev/null
+++ b/src/slalib/sun67.htx/icons.html
@@ -0,0 +1,42 @@
+
+<FORM METHOD="POST" >
+<INPUT TYPE="submit" VALUE="Next">
+ <P>
+<INPUT TYPE="submit" VALUE="Previous">
+ <P>
+<INPUT TYPE="submit" VALUE="Up">
+ <P>
+<INPUT TYPE="submit" VALUE="Next Group">
+ <P>
+<INPUT TYPE="submit" VALUE="Previous Group">
+ <P>
+<INPUT TYPE="submit" VALUE="Contents">
+ <P>
+<INPUT TYPE="submit" VALUE="Index">
+ <P>
+<INPUT TYPE="submit" VALUE="        New         ">
+ <P>
+<INPUT TYPE="submit" VALUE="      Deleted       ">
+ <P>
+<INPUT TYPE="submit" VALUE="Browse">
+ <P>
+<INPUT TYPE="submit" VALUE="Search">
+ <P>
+<INPUT TYPE="submit" VALUE="Home">
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+[330
+
+
+] (images.aux) ) 
+Here is how much of TeX's memory you used:
+ 351 strings out of 10906
+ 3619 string characters out of 71914
+ 61584 words of memory out of 262141
+ 3274 multiletter control sequences out of 9500
+ 7308 words of font info for 26 fonts, out of 150000 for 255
+ 14 hyphenation exceptions out of 607
+ 21i,13n,21p,242b,498s stack positions out of 300i,40n,60p,3000b,4000s
+
+Output written on images.dvi (330 pages, 51052 bytes).
diff --git a/src/slalib/sun67.htx/images.pl b/src/slalib/sun67.htx/images.pl
new file mode 100644
index 0000000..498f422
--- /dev/null
+++ b/src/slalib/sun67.htx/images.pl
@@ -0,0 +1,1686 @@
+# LaTeX2HTML 97.1 (release) (July 13th, 1997)
+# Associate images original text with physical files.
+
+
+$key = q/{_inline}1hspace-0.05em^'hspace-0.1em'hspace-0.4em.74{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="31" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img294.gif"
+ ALT="$1\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.74$">|; 
+
+$key = q/{_inline}cosdeltaE{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="48" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img249.gif"
+ ALT="$\cos \delta E$">|; 
+
+$key = q/{_inline}0^rmshspace-0.3em.03{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="32" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img96.gif"
+ ALT="$0^{\rm s}\hspace{-0.3em}.03$">|; 
+
+$key = q/{_inline}0leqx<1{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="72" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img145.gif"
+ ALT="$0 \leq x < 1$">|; 
+
+$key = q/{_inline}zeta=80^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="56" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img208.gif"
+ ALT="$\zeta=80^\circ$">|; 
+
+$key = q/{_inline}-75^circ,59^',27^''.2{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="102" HEIGHT="35" ALIGN="MIDDLE" BORDER="0"
+ SRC="img288.gif"
+ ALT="$-75^{\circ}\,59^{'}\,27^{''}.2$">|; 
+
+$key = q/{_inline}150hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="33" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img197.gif"
+ ALT="$150\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}2hspace-0.05em^'hspace-0.1em'hspace-0.4em.3{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img78.gif"
+ ALT="$2\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.3$">|; 
+
+$key = q/{_inline}1hspace-0.05em^'hspace-0.1em'hspace-0.4em.6{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img189.gif"
+ ALT="$1\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.6$">|; 
+
+$key = q/{displaymath}zeta_vacapproxzeta_obs+Atanzeta_obs+Btan^3zeta_obs{displaymath}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="255" HEIGHT="27"
+ SRC="img302.gif"
+ ALT="\begin{displaymath}
+\zeta _{vac} \approx \zeta _{obs}
+ + A \tan \zeta _{obs}
+ + B \tan ^{3}\zeta _{obs} \end{displaymath}">|; 
+
+$key = q/{_inline}1000times20{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="72" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img330.gif"
+ ALT="$1000\times20$">|; 
+
+$key = q/{_inline}times3602pi{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="66" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img9.gif"
+ ALT="$\times 360/2\pi$">|; 
+
+$key = q/{_inline}21hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="25" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img218.gif"
+ ALT="$21\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}12^h,07^m,58^s.09{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="104" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img262.gif"
+ ALT="$12^{h}\,07^{m}\,58^{s}.09$">|; 
+
+$key = q/{_inline}81^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img186.gif"
+ ALT="$81^\circ$">|; 
+
+$key = q/{_inline}omega{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$">|; 
+
+$key = q/{_inline}30^rmm{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="30" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img87.gif"
+ ALT="$30^{\rm m}$">|; 
+
+$key = q/{_inline}89^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img200.gif"
+ ALT="$89^\circ$">|; 
+
+$key = q/{displaymath}zeta_obsapproxzeta_vac-fracAtanzeta_vac+Btan^3zeta_vac1+(A+3Btan^2zeta_vac)sec^2zeta_vac{displaymath}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="313" HEIGHT="45"
+ SRC="img306.gif"
+ ALT="\begin{displaymath}
+\zeta _{obs} \approx \zeta _{vac}
+ - \frac{A \tan \zeta _{va...
+ ...
+ {1 + ( A + 3 B \tan ^{2}\zeta _{vac} ) \sec ^{2}\zeta _{vac}}\end{displaymath}">|; 
+
+$key = q/{_inline}1^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="18" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img318.gif"
+ ALT="$1^\circ$">|; 
+
+$key = q/{_inline}=Deltapsicosepsilon{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="78" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img300.gif"
+ ALT="$=\Delta\psi\cos\epsilon$">|; 
+
+$key = q/{_inline}(3times3){_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="51" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img259.gif"
+ ALT="$(3\times3)$">|; 
+
+$key = q/{_inline}epsilon{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="9" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img257.gif"
+ ALT="$\epsilon$">|; 
+
+$key = q/{_inline}290^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="34" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img37.gif"
+ ALT="$290^\circ$">|; 
+
+$key = q/{_inline}+1^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="30" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img236.gif"
+ ALT="$+1^{\circ}$">|; 
+
+$key = q/{_inline}20,murmm{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="45" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img42.gif"
+ ALT="$20\,\mu{\rm m}$">|; 
+
+$key = q/{_inline}0hspace-0.05em^'hspace-0.1em'hspace-0.4em.6{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img137.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.6$">|; 
+
+$key = q/{_inline}7hspace-0.05em^'hspace-0.1em'hspace-0.4em.1{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img217.gif"
+ ALT="$7\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.1$">|; 
+
+$key = q/{_inline}C_3!=!-10.0{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="79" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img327.gif"
+ ALT="$C_3\!=\!-10.0$">|; 
+
+$key = q/{_inline}~sinalpha+({_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="70" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img279.gif"
+ ALT="$~\sin \alpha +
+ ($">|; 
+
+$key = q/{_inline}xi{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="10" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img92.gif"
+ ALT="$\xi$">|; 
+
+$key = q/{_inline}1100hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="41" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img202.gif"
+ ALT="$1100\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}[lambda,phi]{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="38" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img46.gif"
+ ALT="$[\lambda,\phi]$">|; 
+
+$key = q/{_inline}30hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img82.gif"
+ ALT="$30\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}1.0027379cdots{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="94" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img120.gif"
+ ALT="$1.0027379\cdots$">|; 
+
+$key = q/{_inline}90^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img22.gif"
+ ALT="$90^{\circ}$">|; 
+
+$key = q/{_inline}14hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="25" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img126.gif"
+ ALT="$14\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}rho=r(1+cr^2){_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="103" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img128.gif"
+ ALT="$\rho = r (1 + c r^{2})$">|; 
+
+$key = q/{_inline}pmn{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img123.gif"
+ ALT="$\pm n$">|; 
+
+$key = q/{_inline}bfD{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="17" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img240.gif"
+ ALT="${\bf D}$">|; 
+
+$key = q/{_inline}0hspace-0.05em^'hspace-0.1em'hspace-0.4em.24{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="31" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img81.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.24$">|; 
+
+$key = q/{_inline}0^rmshspace-0.3em.015869{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="65" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img267.gif"
+ ALT="$0^{\rm s}\hspace{-0.3em}.015869$">|; 
+
+$key = q/{_inline}0hspace-0.05em^'hspace-0.1em'hspace-0.4em.43549{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="56" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img277.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.43549$">|; 
+
+$key = q/{_inline}[,Deltax,Deltay,Deltaz,]{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="99" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img239.gif"
+ ALT="$[\,\Delta x,\Delta y, \Delta z\,]$">|; 
+
+$key = q/{_inline}86hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img136.gif"
+ ALT="$86\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}(0leqe<1){_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="83" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img106.gif"
+ ALT="$( 0 \leq e < 1 )$">|; 
+
+$key = q/{_inline}0^rmh{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="18" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img49.gif"
+ ALT="$0^{\rm h}$">|; 
+
+$key = q/{_inline}~cosalpha-{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="58" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img273.gif"
+ ALT="$~\cos \alpha
+ -$">|; 
+
+$key = q/{_inline}[theta,phi,dottheta,dotphi]{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="69" HEIGHT="35" ALIGN="MIDDLE" BORDER="0"
+ SRC="img252.gif"
+ ALT="$[\theta,\phi,\dot{\theta},\dot{\phi}]$">|; 
+
+$key = q/{_inline}1hspace-0.05em^'hspace-0.1em'hspace-0.4em.0{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img178.gif"
+ ALT="$1\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.0$">|; 
+
+$key = q/{_inline}nu=rho_wrho_s{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="75" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img181.gif"
+ ALT="$\nu=\rho_w/\rho_s$">|; 
+
+$key = q/{_inline}0hspace-0.05em^'hspace-0.1em'hspace-0.4em.3{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img32.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.3$">|; 
+
+$key = q/{_inline}varpi=Omega+omega{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="81" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img321.gif"
+ ALT="$\varpi = \Omega + \omega$">|; 
+
+$key = q/{_inline}6hspace-0.05em^'hspace-0.1em'hspace-0.4em.1{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img216.gif"
+ ALT="$6\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.1$">|; 
+
+$key = q/{_inline}mu_delta,=+{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="56" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img276.gif"
+ ALT="$\mu_\delta\,=+$">|; 
+
+$key = q/{_inline}920hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="33" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img124.gif"
+ ALT="$920\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}b^I!I=0{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="51" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img223.gif"
+ ALT="$b^{I\!I}=0$">|; 
+
+$key = q/{_inline}x'=x_1+rmXZ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="96" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
+ SRC="img57.gif"
+ ALT="$x' = x_{1} + {\rm XZ}$">|; 
+
+$key = q/{_inline}mu_alpha={_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="38" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img289.gif"
+ ALT="$\mu_\alpha=$">|; 
+
+$key = q/{_inline}rmbfr_0{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="17" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img102.gif"
+ ALT="${\rm \bf r}_0$">|; 
+
+$key = q/{_inline}zeta_vac{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="29" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img303.gif"
+ ALT="$\zeta _{vac}$">|; 
+
+$key = q/{_inline}86^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img194.gif"
+ ALT="$86^\circ$">|; 
+
+$key = q/{_inline}y'''=+x''sinrmPERP2+y''cosrmPERP2{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="286" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
+ SRC="img62.gif"
+ ALT="$y''' = + x'' \sin {\rm PERP}/2 + y'' \cos {\rm PERP}/2$">|; 
+
+$key = q/{_inline}C_2!=!-2.0{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="71" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img326.gif"
+ ALT="$C_2\!=\!-2.0$">|; 
+
+$key = q/{_inline}0.0065^circm^-1{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="86" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img38.gif"
+ ALT="$0.0065^\circ m^{-1}$">|; 
+
+$key = q/{_inline}alpha=18^rmh,delta=+30^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="132" HEIGHT="33" ALIGN="MIDDLE" BORDER="0"
+ SRC="img225.gif"
+ ALT="$\alpha=18^{\rm h},\delta=+30^{\circ}$">|; 
+
+$key = q/{_inline}[mu_alpha,mu_delta]{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="54" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img264.gif"
+ ALT="$[\mu_\alpha,\mu_\delta]$">|; 
+
+$key = q/{_inline}5^rmh,25^rmm{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="49" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img320.gif"
+ ALT="$5^{\rm h}\,25^{\rm m}$">|; 
+
+$key = q/{figure}centertabular|cccccc|hline&&&&&hspace5em&hspace5em&hspace5em&hspace5em&halloftheprecessionandE-termscorrectionsaresuperfluous.{figure}MSF=1.5;FSF=1;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="450" HEIGHT="642"
+ SRC="img255.gif"
+ ALT="\begin{figure}
+\begin{center}
+\begin{tabular}
+{\vert cccccc\vert} \hline
+& & & &...
+ ...2000, all of the precession and E-terms corrections
+are superfluous.\end{figure}">|; 
+
+$key = q/{_inline}~sinalpha-{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="56" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
+ SRC="img281.gif"
+ ALT="$~\sin \alpha
+ -$">|; 
+
+$key = q/{_inline}equiv123{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="44" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img67.gif"
+ ALT="$\equiv123$">|; 
+
+$key = q/{_inline}3hspace-0.05em^'hspace-0.1em'hspace-0.4em.7{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img77.gif"
+ ALT="$3\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.7$">|; 
+
+$key = q/{_inline}12^circ,34^',56^''.7{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="90" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img4.gif"
+ ALT="$12^{\circ}\,34^{'}\,56^{''}.7$">|; 
+
+$key = q/{_inline}y'=y_1+rmYZ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="94" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
+ SRC="img58.gif"
+ ALT="$y' = y_{1} + {\rm YZ}$">|; 
+
+$key = q/{_inline}+0hspace-0.05em^'hspace-0.1em'hspace-0.4em.103{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="52" HEIGHT="35" ALIGN="MIDDLE" BORDER="0"
+ SRC="img292.gif"
+ ALT="$+0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.103$">|; 
+
+$key = q/{_inline}=93^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="43" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img177.gif"
+ ALT="$=93^\circ$">|; 
+
+$key = q/{_inline}0hspace-0.05em^'hspace-0.1em'hspace-0.4em.0001{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="47" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img258.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.0001$">|; 
+
+$key = q/{_inline}[x_e,y_e,]{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="52" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img114.gif"
+ ALT="$[x_{e},y_{e}\,]$">|; 
+
+$key = q/{_inline}[,0,,1,]{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="43" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img121.gif"
+ ALT="$[\,0,\,1\,]$">|; 
+
+$key = q/{_inline}20hspace-0.05em^'hspace-0.1em'hspace-0.4em.5{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="31" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img265.gif"
+ ALT="$20\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.5$">|; 
+
+$key = q/{_inline}theta{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img298.gif"
+ ALT="$\theta$">|; 
+
+$key = q/{_inline}zeta<80^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="56" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img157.gif"
+ ALT="$\zeta<80^{\circ}$">|; 
+
+$key = q/{_inline}0^rmshspace-0.3em.000340{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="65" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img270.gif"
+ ALT="$0^{\rm s}\hspace{-0.3em}.000340$">|; 
+
+$key = q/{_inline}deltaEcosE{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="64" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img247.gif"
+ ALT="$\delta E \cos E$">|; 
+
+$key = q/{_inline}[x_m,y_m,]{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="63" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img113.gif"
+ ALT="$[x_{m},y_{m}\,]$">|; 
+
+$key = q/{_inline}-0hspace-0.05em^'hspace-0.1em'hspace-0.4em.06{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="44" HEIGHT="35" ALIGN="MIDDLE" BORDER="0"
+ SRC="img305.gif"
+ ALT="$-0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.06$">|; 
+
+$key = q/{_inline}340hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="33" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img199.gif"
+ ALT="$340\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}l^I!I,b^I!I{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="45" HEIGHT="32" ALIGN="MIDDLE" BORDER="0"
+ SRC="img254.gif"
+ ALT="$l^{I\!I},b^{I\!I}$">|; 
+
+$key = q/{_inline}20^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img296.gif"
+ ALT="$20^\circ$">|; 
+
+$key = q/{_inline}_j)]cdot({_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="38" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img231.gif"
+ ALT="$_{j})]
+ \cdot ($">|; 
+
+$key = q/{_inline}times{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="15" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img84.gif"
+ ALT="$\times$">|; 
+
+$key = q/{_inline}20hspace-0.05em^'hspace-0.1em'hspace-0.4em.49552{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="64" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img110.gif"
+ ALT="$20\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.49552$">|; 
+
+$key = q/{_inline}tan^3zeta{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="44" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img152.gif"
+ ALT="$\tan^{3} \zeta$">|; 
+
+$key = q/{_inline}E=90^circ-zeta_true{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="113" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img211.gif"
+ ALT="$E=90^\circ-\zeta_{true}$">|; 
+
+$key = q/{_inline}83^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img190.gif"
+ ALT="$83^\circ$">|; 
+
+$key = q/{_inline}0^rmshspace-0.3em.9{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="24" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img31.gif"
+ ALT="$0^{\rm s}\hspace{-0.3em}.9$">|; 
+
+$key = q/{_inline}(0leqeleq10){_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="91" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img107.gif"
+ ALT="$( 0 \leq e \leq 10 )$">|; 
+
+$key = q/{_inline}17hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img133.gif"
+ ALT="$17\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}0.4,murmm{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="50" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img35.gif"
+ ALT="$0.4\,\mu{\rm m}$">|; 
+
+$key = q/{_inline}3^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="18" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img27.gif"
+ ALT="$3^{\circ}$">|; 
+
+$key = q/{_inline}20^rms{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="24" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img86.gif"
+ ALT="$20^{\rm s}$">|; 
+
+$key = q/{_inline}1hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="17" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img140.gif"
+ ALT="$1\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}zeta=70^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="56" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img183.gif"
+ ALT="$\zeta=70^\circ$">|; 
+
+$key = q/{_inline}0hspace-0.05em^'hspace-0.1em'hspace-0.4em.001{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="39" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img112.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.001$">|; 
+
+$key = q/{_inline}DeltarmT{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="28" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img315.gif"
+ ALT="$\Delta {\rm T}$">|; 
+
+$key = q/{_inline}pm{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="15" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img30.gif"
+ ALT="$\pm$">|; 
+
+$key = q/{_inline}C_1!=!+50.0{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="79" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img325.gif"
+ ALT="$C_1\!=\!+50.0$">|; 
+
+$key = q/{_inline}l^I!I=90^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="64" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img222.gif"
+ ALT="$l^{I\!I}=90^{\circ}$">|; 
+
+$key = q/{_inline}50^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img163.gif"
+ ALT="$50^\circ$">|; 
+
+$key = q/{_inline}[,theta,phi~]{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="45" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img238.gif"
+ ALT="$[\,\theta,\phi~]$">|; 
+
+$key = q/{_inline}x!pm!n{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="36" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img69.gif"
+ ALT="$x\!\pm\!n$">|; 
+
+$key = q/{_inline}mu_delta={_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="36" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img291.gif"
+ ALT="$\mu_\delta=$">|; 
+
+$key = q/{_inline}3times3{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img18.gif"
+ ALT="$3\times3$">|; 
+
+$key = q/{_inline}50hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img261.gif"
+ ALT="$50\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}1.0,murmm{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="50" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img40.gif"
+ ALT="$1.0\,\mu{\rm m}$">|; 
+
+$key = q/{_inline}92^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img205.gif"
+ ALT="$92^\circ$">|; 
+
+$key = q/{_inline}18hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img79.gif"
+ ALT="$18\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}0.7,murmm{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="50" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img34.gif"
+ ALT="$0.7\,\mu{\rm m}$">|; 
+
+$key = q/{_inline}timesn{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img226.gif"
+ ALT="$\times n$">|; 
+
+$key = q/{_inline}rmMJD=(rmJD-2400000.5{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="177" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img138.gif"
+ ALT="${\rm MJD} = ({\rm JD} - 2400000.5$">|; 
+
+$key = q/{_inline}0^circhspace-0.37em.hspace0.02em5{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="25" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img301.gif"
+ ALT="$0^{\circ}
+ \hspace{-0.37em}.\hspace{0.02em}5$">|; 
+
+$key = q/{_inline}tan^-14{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="54" HEIGHT="16" ALIGN="BOTTOM" BORDER="0"
+ SRC="img155.gif"
+ ALT="$\tan^{-1} 4$">|; 
+
+$key = q/{_inline}0^rmshspace-0.3em.01{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="32" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img97.gif"
+ ALT="$0^{\rm s}\hspace{-0.3em}.01$">|; 
+
+$key = q/{_inline}100hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="33" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img141.gif"
+ ALT="$100\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}2hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="17" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img316.gif"
+ ALT="$2\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}[,xi,eta,]{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img85.gif"
+ ALT="$[\,\xi,\eta\,]$">|; 
+
+$key = q/{_inline}00^h,00^m,00^s.0{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="96" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img309.gif"
+ ALT="$00^{h}\,00^{m}\,00^{s}.0$">|; 
+
+$key = q/{_inline}0!-!pi{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="35" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img234.gif"
+ ALT="$0\!-\!\pi$">|; 
+
+$key = q/{_inline}280^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="34" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img167.gif"
+ ALT="$280^\circ$">|; 
+
+$key = q/{_inline}beta{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="12" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img173.gif"
+ ALT="$\beta$">|; 
+
+$key = q/{_inline}0^rmshspace-0.3em.000083{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="65" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img274.gif"
+ ALT="$0^{\rm s}\hspace{-0.3em}.000083$">|; 
+
+$key = q/{_inline}0hspace-0.05em^'hspace-0.1em'hspace-0.4em.00510{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="56" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img278.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.00510$">|; 
+
+$key = q/{_inline}zeta=87^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="56" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img8.gif"
+ ALT="$\zeta = 87^{\circ}$">|; 
+
+$key = q/{_inline}90^circ-delta{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="54" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img297.gif"
+ ALT="$90^\circ-\delta$">|; 
+
+$key = q/{_inline}2murmm{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="34" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img168.gif"
+ ALT="$2\mu{\rm m}$">|; 
+
+$key = q/{_inline}<bfV1+bfD>{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="95" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img243.gif"
+ ALT="$<{\bf V1}+{\bf D}\gt$">|; 
+
+$key = q/{_inline}5hspace-0.05em^'hspace-0.1em'hspace-0.4em.8{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img215.gif"
+ ALT="$5\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.8$">|; 
+
+$key = q/{_inline}25^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img162.gif"
+ ALT="$25^\circ$">|; 
+
+$key = q/{_inline}80^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img179.gif"
+ ALT="$80^\circ$">|; 
+
+$key = q/{_inline}pmpi2{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img15.gif"
+ ALT="$\pm\pi/2$">|; 
+
+$key = q/{_inline}0hspace-0.05em^'hspace-0.1em'hspace-0.4em.01{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="31" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img158.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.01$">|; 
+
+$key = q/{_inline}rho{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="11" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img129.gif"
+ ALT="$\rho$">|; 
+
+$key = q/{_inline}152pi=2.3873241463784300365{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="235" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img7.gif"
+ ALT="$15/{2\pi} = 2.3873241463784300365$">|; 
+
+$key = q/{_inline}2pi{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="20" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img52.gif"
+ ALT="$2\pi$">|; 
+
+$key = q/{_inline}43hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img219.gif"
+ ALT="$43\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}sim20{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="36" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img324.gif"
+ ALT="$\sim20$">|; 
+
+$key = q/{_inline}[,alpha,delta,]{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">|; 
+
+$key = q/{_inline}dotalpha{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="13" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img115.gif"
+ ALT="$\dot{\alpha}$">|; 
+
+$key = q/{_inline}0^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="18" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img1.gif"
+ ALT="$0^{\circ}$">|; 
+
+$key = q/{_inline}88^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img198.gif"
+ ALT="$88^\circ$">|; 
+
+$key = q/{_inline}bfV1{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img241.gif"
+ ALT="${\bf V1}$">|; 
+
+$key = q/{_inline}tan^-11{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="54" HEIGHT="16" ALIGN="BOTTOM" BORDER="0"
+ SRC="img153.gif"
+ ALT="$\tan^{-1} 1$">|; 
+
+$key = q/{_inline}0^circhspace-0.37em.hspace0.02em2{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="25" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img260.gif"
+ ALT="$0^{\circ}
+ \hspace{-0.37em}.\hspace{0.02em}2$">|; 
+
+$key = q/{_inline}-19^circ,44^',37^''.1{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="102" HEIGHT="35" ALIGN="MIDDLE" BORDER="0"
+ SRC="img263.gif"
+ ALT="$-19^{\circ}\,44^{'}\,37^{''}.1$">|; 
+
+$key = q/{_inline}cdot~[diag(1{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="71" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img230.gif"
+ ALT="$\cdot~[diag(1/$">|; 
+
+$key = q/{_inline}alpha=0{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="43" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img89.gif"
+ ALT="$\alpha=0$">|; 
+
+$key = q/{_inline}~cosalpha)sindelta-{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="98" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img271.gif"
+ ALT="$~\cos \alpha ) \sin \delta
+ -$">|; 
+
+$key = q/{_inline}zeta{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="11" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img149.gif"
+ ALT="$\zeta$">|; 
+
+$key = q/{_inline}3hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="17" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img75.gif"
+ ALT="$3\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}tanzeta{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="37" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img151.gif"
+ ALT="$\tan \zeta$">|; 
+
+$key = q/{_inline}0^rmshspace-0.3em.000105{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="65" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img272.gif"
+ ALT="$0^{\rm s}\hspace{-0.3em}.000105$">|; 
+
+$key = q/{_inline}0hspace-0.05em^'hspace-0.1em'hspace-0.4em.4{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img185.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.4$">|; 
+
+$key = q/{_inline}~sinalpha)secdelta{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="84" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img275.gif"
+ ALT="$~\sin \alpha ) \sec \delta $">|; 
+
+$key = q/{_inline}-1^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="30" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img2.gif"
+ ALT="$-1^{\circ}$">|; 
+
+$key = q/{_inline}times10^-5{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="48" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img93.gif"
+ ALT="$\times10^{-5}$">|; 
+
+$key = q/{_inline}C_4!=!+25.0{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="79" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img328.gif"
+ ALT="$C_4\!=\!+25.0$">|; 
+
+$key = q/{_inline}60hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img304.gif"
+ ALT="$60\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}76^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img33.gif"
+ ALT="$76^\circ$">|; 
+
+$key = q/{_inline}x'''=+x''cosrmPERP2+y''sinrmPERP2{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="287" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
+ SRC="img61.gif"
+ ALT="$x''' = + x'' \cos {\rm PERP}/2 + y'' \sin {\rm PERP}/2$">|; 
+
+$key = q/{_inline}deltaE{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="23" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img245.gif"
+ ALT="$\delta E$">|; 
+
+$key = q/{_inline}times2{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="31" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img16.gif"
+ ALT="$\times 2 / $">|; 
+
+$key = q/{_inline}zeta_obs{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img184.gif"
+ ALT="$\zeta_{obs}$">|; 
+
+$key = q/{_inline}0hspace-0.05em^'hspace-0.1em'hspace-0.4em.1{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img25.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.1$">|; 
+
+$key = q/{_inline}4hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="17" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img130.gif"
+ ALT="$4\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}0^rmshspace-0.3em.0016{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="48" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img312.gif"
+ ALT="$0^{\rm s}\hspace{-0.3em}.0016$">|; 
+
+$key = q/{_inline}zeta=84^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="56" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img207.gif"
+ ALT="$\zeta=84^\circ$">|; 
+
+$key = q/{_inline}100mum{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="51" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img307.gif"
+ ALT="$100\mu m$">|; 
+
+$key = q/{_inline}sigma=5.0{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="55" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img329.gif"
+ ALT="$\sigma=5.0$">|; 
+
+$key = q/{_inline}circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="10" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img5.gif"
+ ALT="${\circ}$">|; 
+
+$key = q/{_inline}[x_1,y_1,]{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="53" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img55.gif"
+ ALT="$[x_{1},y_{1}\,]$">|; 
+
+$key = q/{_inline}L=varpi+M{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="87" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img322.gif"
+ ALT="$L = \varpi + M$">|; 
+
+$key = q/{_inline}16^h,09^m,55^s.13{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="104" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img286.gif"
+ ALT="$16^{h}\,09^{m}\,55^{s}.13$">|; 
+
+$key = q/{_inline}times(2pi86400)^2times(3602pi){_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="186" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img12.gif"
+ ALT="$\times (2\pi/86400)^2 \times (360/2\pi)$">|; 
+
+$key = q/{_inline}xi,eta{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img90.gif"
+ ALT="$\xi,\eta$">|; 
+
+$key = q/{_inline}Deltazeta=atanzeta+btan^3zeta{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="164" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img148.gif"
+ ALT="$\Delta \zeta = a \tan \zeta + b \tan^{3} \zeta$">|; 
+
+$key = q/{_inline}23^circhspace-0.37em.hspace0.02em5{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="33" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img256.gif"
+ ALT="$23^{\circ}
+ \hspace{-0.37em}.\hspace{0.02em}5$">|; 
+
+$key = q/{_inline}rightarrow{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="19" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img10.gif"
+ ALT="$\rightarrow$">|; 
+
+$key = q/{_inline}pmn.nxpmn{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="78" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img68.gif"
+ ALT="$\pm n.n x \pm n$">|; 
+
+$key = q/{_inline}cdot{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$">|; 
+
+$key = q/{_inline}85^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img193.gif"
+ ALT="$85^\circ$">|; 
+
+$key = q/{_inline}45hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img195.gif"
+ ALT="$45\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}pm3{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="23" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img147.gif"
+ ALT="$\pm3$">|; 
+
+$key = q/{_inline}0^rmshspace-0.3em.0013{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="48" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img313.gif"
+ ALT="$0^{\rm s}\hspace{-0.3em}.0013$">|; 
+
+$key = q/{_inline}zeta<70^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="56" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img26.gif"
+ ALT="$\zeta<70^{\circ}$">|; 
+
+$key = q/{_inline}tan^5{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="33" HEIGHT="16" ALIGN="BOTTOM" BORDER="0"
+ SRC="img171.gif"
+ ALT="$\tan^5$">|; 
+
+$key = q/{_inline}5hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="17" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img131.gif"
+ ALT="$5\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}~sinalpha+{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="56" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
+ SRC="img269.gif"
+ ALT="$~\sin \alpha
+ +$">|; 
+
+$key = q/{_inline}620hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="33" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img201.gif"
+ ALT="$620\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}ntimesn{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="42" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img73.gif"
+ ALT="$n \times n$">|; 
+
+$key = q/{_inline}Deltazeta{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="24" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img150.gif"
+ ALT="$\Delta \zeta$">|; 
+
+$key = q/{_inline}0hspace-0.05em^'hspace-0.1em'hspace-0.4em.00125{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="56" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img282.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.00125$">|; 
+
+$key = q/{_inline}10^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img117.gif"
+ ALT="$10^{\circ}$">|; 
+
+$key = q/{_inline}varpi{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="16" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img100.gif"
+ ALT="$\varpi$">|; 
+
+$key = q/{_inline}lambda,beta{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="29" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img253.gif"
+ ALT="$\lambda,\beta$">|; 
+
+$key = q/{_inline}0.3,murmm{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="50" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img41.gif"
+ ALT="$0.3\,\mu{\rm m}$">|; 
+
+$key = q/{_inline}pm100{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img317.gif"
+ ALT="$\pm100$">|; 
+
+$key = q/{_inline}1900hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="41" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img204.gif"
+ ALT="$1900\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}times10^-10{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="55" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img94.gif"
+ ALT="$\times10^{-10}$">|; 
+
+$key = q/{_inline}M_odot=1{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="59" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img323.gif"
+ ALT="$M_\odot = 1$">|; 
+
+$key = q/{_inline}Deltaalpha{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="27" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img118.gif"
+ ALT="$\Delta\alpha$">|; 
+
+$key = q/{displaymath}Deltazeta=Fleft(frac0^circhspace-0.37em.hspace0.02em55445-0^circhsp-0.37em.hspace0.02em00202E^21+0.28385E+0.02390E^2right){displaymath}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="321" HEIGHT="49"
+ SRC="img210.gif"
+ ALT="\begin{displaymath}
+\Delta \zeta = F \left(
+ \frac{0^\circ\hspace{-0.37em}.\hspa...
+ ...hspace{0.02em}00202 E^2}
+ {1 + 0.28385 E +0.02390 E^2} \right) \end{displaymath}">|; 
+
+$key = q/{_inline}times(2pi86400)times(3602pi){_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="178" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img11.gif"
+ ALT="$\times (2\pi/86400) \times (360/2\pi)$">|; 
+
+$key = q/{_inline}zeta<45^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="56" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img160.gif"
+ ALT="$\zeta<45^{\circ}$">|; 
+
+$key = q/{_inline}[,Az,El~]{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="66" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img28.gif"
+ ALT="$[\,Az,El~]$">|; 
+
+$key = q/{_inline}6hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="17" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img132.gif"
+ ALT="$6\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}^Tcdot{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="17" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img70.gif"
+ ALT="$^{T}\cdot$">|; 
+
+$key = q/{_inline}3hspace-0.05em^'hspace-0.1em'hspace-0.4em.2{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img213.gif"
+ ALT="$3\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.2$">|; 
+
+$key = q/{_inline}[x_p,y_p,]{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="53" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img144.gif"
+ ALT="$[x_{p},y_{p}\,]$">|; 
+
+$key = q/{_inline}[x_2,y_2,]{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="53" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img56.gif"
+ ALT="$[x_{2},y_{2}\,]$">|; 
+
+$key = q/{_inline}0hspace-0.05em^'hspace-0.1em'hspace-0.4em.00158{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="56" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img280.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.00158$">|; 
+
+$key = q/{_inline}x_2=+x'''cosrmORIENT+y'''sinrmORIENT{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="298" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
+ SRC="img63.gif"
+ ALT="$x_{2} = + x''' \cos {\rm ORIENT} +
+ y''' \sin {\rm ORIENT}$">|; 
+
+$key = q/{_inline}61^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img235.gif"
+ ALT="$61^\circ$">|; 
+
+$key = q/{_inline}y_2=-x'''sinrmORIENT+y'''cosrmORIENT{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="297" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
+ SRC="img64.gif"
+ ALT="$y_{2} = - x''' \sin {\rm ORIENT} +
+ y''' \cos {\rm ORIENT}$">|; 
+
+$key = q/{_inline}82^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img188.gif"
+ ALT="$82^\circ$">|; 
+
+$key = q/{_inline}0!-!2pi{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="43" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img66.gif"
+ ALT="$0\!-\!2\pi$">|; 
+
+$key = q/{_inline}71hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img134.gif"
+ ALT="$71\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}0hspace-0.05em^'hspace-0.1em'hspace-0.4em.05{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="31" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img175.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.05$">|; 
+
+$key = q/{_inline}sqrt1-left|mboxbfvright|^2{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="72" HEIGHT="45" ALIGN="MIDDLE" BORDER="0"
+ SRC="img17.gif"
+ ALT="$\sqrt{1-\left\vert\mbox{\bf v}\right\vert^2}$">|; 
+
+$key = q/{_inline}murmm{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img21.gif"
+ ALT="$\mu{\rm m}$">|; 
+
+$key = q/{_inline}alpha,deltarightarrowlambda,beta{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="81" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img95.gif"
+ ALT="$\alpha,\delta\rightarrow\lambda,\beta$">|; 
+
+$key = q/{displaymath}h=theta-alpha{displaymath}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="70" HEIGHT="25"
+ SRC="img299.gif"
+ ALT="\begin{displaymath}
+h = \theta - \alpha \end{displaymath}">|; 
+
+$key = q/{_inline}2^circhspace-0.37em.hspace0.02em4{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="25" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img232.gif"
+ ALT="$2^{\circ}
+ \hspace{-0.37em}.\hspace{0.02em}4$">|; 
+
+$key = q/{_inline}1hspace-0.05em^'hspace-0.1em'hspace-0.4em.85{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="31" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img125.gif"
+ ALT="$1\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.85$">|; 
+
+$key = q/{_inline}+pi2{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img14.gif"
+ ALT="$+\pi/2$">|; 
+
+$key = q/{_inline}sim!76^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="40" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img161.gif"
+ ALT="$\sim\!76^\circ$">|; 
+
+$key = q/{_inline}[,x,y,z,dotx,doty,dotz,]{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="106" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img51.gif"
+ ALT="$[\,x,y,z,\dot{x},\dot{y},\dot{z}\,]$">|; 
+
+$key = q/{_inline}6.5^circKkm^-1{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="86" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img169.gif"
+ ALT="$6.5^\circ K km^{-1}$">|; 
+
+$key = q/{_inline}270^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="34" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img139.gif"
+ ALT="$270^\circ$">|; 
+
+$key = q/{_inline}7hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="17" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img192.gif"
+ ALT="$7\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}tandeltaEapproxdeltaE{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="92" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img246.gif"
+ ALT="${\tan \delta E\approx\delta E}$">|; 
+
+$key = q/{_inline}cdots{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="21" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img48.gif"
+ ALT="$\cdots$">|; 
+
+$key = q/{_inline}1hspace-0.05em^'hspace-0.1em'hspace-0.4em.5{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img212.gif"
+ ALT="$1\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.5$">|; 
+
+$key = q/{_inline}0hspace-0.05em^'hspace-0.1em'hspace-0.4em.8{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img187.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.8$">|; 
+
+$key = q/{_inline}(1-deltaE^22){_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="88" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img250.gif"
+ ALT="$(1-\delta E^2 /2)$">|; 
+
+$key = q/{_inline}mu{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="12" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img146.gif"
+ ALT="$\mu$">|; 
+
+$key = q/{_inline}15^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img39.gif"
+ ALT="$15^\circ$">|; 
+
+$key = q/{_inline}[Deltax,Deltay,Deltaz,]{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="96" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img109.gif"
+ ALT="$[\Delta x, \Delta y, \Delta z\,]$">|; 
+
+$key = q/{_inline}70^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img174.gif"
+ ALT="$70^\circ$">|; 
+
+$key = q/{_inline}DeltarmT=rmET-rmUT{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="117" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img314.gif"
+ ALT="$\Delta {\rm T} = {\rm ET} - {\rm UT}$">|; 
+
+$key = q/{_inline}0hspace-0.05em^'hspace-0.1em'hspace-0.4em.02{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="31" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img295.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.02$">|; 
+
+$key = q/{_inline}91^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img203.gif"
+ ALT="$91^\circ$">|; 
+
+$key = q/{_inline}Delta{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">|; 
+
+$key = q/{_inline}l^I!I=53^circ,b^I!I=+25^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="148" HEIGHT="32" ALIGN="MIDDLE" BORDER="0"
+ SRC="img224.gif"
+ ALT="$l^{I\!I}=53^{\circ},b^{I\!I}=+25^{\circ}$">|; 
+
+$key = q/{_inline}y''=y'rmYS{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="74" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
+ SRC="img60.gif"
+ ALT="$y'' = y' {\rm YS}$">|; 
+
+$key = q/{_inline}bfV2{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img242.gif"
+ ALT="${\bf V2}$">|; 
+
+$key = q/{_inline}[,0,2pi,]{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="50" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img13.gif"
+ ALT="$[\,0,2\pi\,]$">|; 
+
+$key = q/{_inline}mgeqn{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="48" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img227.gif"
+ ALT="$m \geq n$">|; 
+
+$key = q/{_inline}360^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="34" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img53.gif"
+ ALT="$360^{\circ}$">|; 
+
+$key = q/{_inline}0hspace-0.05em^'hspace-0.1em'hspace-0.4em.5{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img83.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.5$">|; 
+
+$key = q/{_inline}alpha,delta{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img91.gif"
+ ALT="$\alpha,\delta$">|; 
+
+$key = q/{_inline}8hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="17" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img319.gif"
+ ALT="$8\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}deltaEsinE{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="62" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img248.gif"
+ ALT="$\delta E \sin E$">|; 
+
+$key = q/{_inline}alpha={_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="30" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img285.gif"
+ ALT="$\alpha=$">|; 
+
+$key = q/{_inline}4hspace-0.05em^'hspace-0.1em'hspace-0.4em.9{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img214.gif"
+ ALT="$4\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.9$">|; 
+
+$key = q/{_inline}45^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img154.gif"
+ ALT="$45^\circ$">|; 
+
+$key = q/{_inline}3200hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="41" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img206.gif"
+ ALT="$3200\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}equiv{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="15" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img251.gif"
+ ALT="$\equiv$">|; 
+
+$key = q/{_inline}delta{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$">|; 
+
+$key = q/{_inline}-26hspace-0.05em^'hspace-0.1em'hspace-0.4em.00{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="52" HEIGHT="35" ALIGN="MIDDLE" BORDER="0"
+ SRC="img88.gif"
+ ALT="$-26\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.00$">|; 
+
+$key = q/{_inline}psi{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="14" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img105.gif"
+ ALT="$\psi$">|; 
+
+$key = q/{_inline}-10^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="38" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img165.gif"
+ ALT="$-10^\circ$">|; 
+
+$key = q/{_inline}81hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img135.gif"
+ ALT="$81\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}l^I!I=137.37{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="86" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img119.gif"
+ ALT="$l^{I\!I}=137.37$">|; 
+
+$key = q/{_inline}87^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img196.gif"
+ ALT="$87^\circ$">|; 
+
+$key = q/{_inline}(mu-1){_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="53" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img45.gif"
+ ALT="$(\mu-1)$">|; 
+
+$key = q/{_inline}23^h,59^m,60^s.0{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="96" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img308.gif"
+ ALT="$23^{h}\,59^{m}\,60^{s}.0$">|; 
+
+$key = q/{_inline}[,x,y,z,]{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$">|; 
+
+$key = q/{_inline}(1-bfDcdotbfV1){_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="93" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img244.gif"
+ ALT="$(1-{\bf D}\cdot{\bf V1})$">|; 
+
+$key = q/{_inline}24^h,59^m,59^s.999{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="113" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img237.gif"
+ ALT="$24^{h}\,59^{m}\,59^{s}.999$">|; 
+
+$key = q/{_inline}7^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="18" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img170.gif"
+ ALT="$7^\circ$">|; 
+
+$key = q/{_inline}220hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="33" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img221.gif"
+ ALT="$220\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}0hspace-0.05em^'hspace-0.1em'hspace-0.4em.2{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img76.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.2$">|; 
+
+$key = q/{_inline}dotalphacosdelta{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="48" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img116.gif"
+ ALT="$\dot{\alpha}\cos\delta$">|; 
+
+$key = q/{_inline}9hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="17" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img127.gif"
+ ALT="$9\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}h,delta{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="27" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img65.gif"
+ ALT="$h,\delta$">|; 
+
+$key = q/{_inline}beta~(=H_0r_0){_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="91" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img172.gif"
+ ALT="$\beta~(=H_0/r_0)$">|; 
+
+$key = q/{_inline}0^rmshspace-0.3em.029032{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="65" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img268.gif"
+ ALT="$0^{\rm s}\hspace{-0.3em}.029032$">|; 
+
+$key = q/{_inline}32^rmshspace-0.3em.184{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="48" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img311.gif"
+ ALT="$32^{\rm s}\hspace{-0.3em}.184$">|; 
+
+$key = q/{_inline}10hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img74.gif"
+ ALT="$10\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}alpha{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$">|; 
+
+$key = q/{_inline}nu=p_wp_s{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="75" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img180.gif"
+ ALT="$\nu=p_w/p_s$">|; 
+
+$key = q/{_inline}0-2pi{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="48" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img143.gif"
+ ALT="$0-2\pi$">|; 
+
+$key = q/{_inline}[,dotx,doty,dotz,]{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img111.gif"
+ ALT="$[\,\dot{x},\dot{y},\dot{z}\,]$">|; 
+
+$key = q/{_inline}75^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img164.gif"
+ ALT="$75^\circ$">|; 
+
+$key = q/{_inline}100,murmm{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="53" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img44.gif"
+ ALT="$100\,\mu{\rm m}$">|; 
+
+$key = q/{_inline}x''=x'rmXS{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="76" HEIGHT="16" ALIGN="BOTTOM" BORDER="0"
+ SRC="img59.gif"
+ ALT="$x'' = x' {\rm XS}$">|; 
+
+$key = q/{_inline}[,x,y,]{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$">|; 
+
+$key = q/{_inline}Deltapsi,cos,epsilon{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="62" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img108.gif"
+ ALT="$\Delta\psi\,cos\,\epsilon$">|; 
+
+$key = q/{_inline}bfrmM{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="17" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img71.gif"
+ ALT="${\bf \rm M}$">|; 
+
+$key = q/{_inline}zeta<60^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="56" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img159.gif"
+ ALT="$\zeta<60^{\circ}$">|; 
+
+$key = q/{_inline}Deltapsicosepsilon{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="61" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img310.gif"
+ ALT="$\Delta\psi\cos\epsilon$">|; 
+
+$key = q/{_inline}zeta=83^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="56" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img209.gif"
+ ALT="$\zeta=83^\circ$">|; 
+
+$key = q/{_inline}mtimesn{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="46" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img228.gif"
+ ALT="$m \times n$">|; 
+
+$key = q/{_inline}0hspace-0.05em^'hspace-0.1em'hspace-0.4em.062{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="39" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img293.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.062$">|; 
+
+$key = q/{_inline}12pi=0.1591549430918953358{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="227" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img6.gif"
+ ALT="$1/{2 \pi} = 0.1591549430918953358$">|; 
+
+$key = q/{_inline}42^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img233.gif"
+ ALT="$42^{\circ}$">|; 
+
+$key = q/{_inline}1000hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="41" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img142.gif"
+ ALT="$1000\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}11hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="25" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img43.gif"
+ ALT="$11\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+$key = q/{_inline}29^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img36.gif"
+ ALT="$29^\circ$">|; 
+
+$key = q/{_inline}84^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img191.gif"
+ ALT="$84^\circ$">|; 
+
+$key = q/{_inline}[,l^I!I,b^I!I,]{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="59" HEIGHT="32" ALIGN="MIDDLE" BORDER="0"
+ SRC="img98.gif"
+ ALT="$[\,l^{I\!I},b^{I\!I}\,]$">|; 
+
+$key = q/{_inline}rmbfv_0{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="19" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img103.gif"
+ ALT="${\rm \bf v}_0$">|; 
+
+$key = q/{_inline}mu_alpha=-{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="56" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img266.gif"
+ ALT="$\mu_\alpha=-$">|; 
+
+$key = q/{_inline}w_iigeq0{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="54" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img229.gif"
+ ALT="$w_{ii} \geq 0$">|; 
+
+$key = q/{_inline}sim76^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="43" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img156.gif"
+ ALT="$\sim 76^\circ$">|; 
+
+$key = q/{_inline}bfM{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="20" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img122.gif"
+ ALT="${\bf M}$">|; 
+
+$key = q/{_inline}pmpi{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$">|; 
+
+$key = q/{_inline}23^rmh,59^rmm,59^rms{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="82" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img54.gif"
+ ALT="$23^{\rm h}\,59^{\rm m}\,59^{\rm s}$">|; 
+
+$key = q/{_inline}30^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img182.gif"
+ ALT="$30^\circ$">|; 
+
+$key = q/{_inline}rmbfr_0.rmbfv_0{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img104.gif"
+ ALT="${\rm \bf r}_0.{\rm \bf v}_0$">|; 
+
+$key = q/{_inline}0hspace-0.05em^'hspace-0.1em'hspace-0.4em.00066{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="56" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img283.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.00066$">|; 
+
+$key = q/{_inline}-0^rmshspace-0.3em.0312{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="61" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
+ SRC="img290.gif"
+ ALT="$-0^{\rm s}\hspace{-0.3em}.0312$">|; 
+
+$key = q/{_inline}delta={_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="28" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img287.gif"
+ ALT="$\delta=$">|; 
+
+$key = q/{_inline}Omega{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$">|; 
+
+$key = q/{_inline}93^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img176.gif"
+ ALT="$93^\circ$">|; 
+
+$key = q/{_inline}+20^circ{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="38" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img166.gif"
+ ALT="$+20^\circ$">|; 
+
+$key = q/{_inline}0hspace-0.05em^'hspace-0.1em'hspace-0.4em.50{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="31" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img80.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.50$">|; 
+
+$key = q/{_inline}~cosdelta{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="43" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img284.gif"
+ ALT="$~\cos \delta $">|; 
+
+$key = q/{_inline}[,h,delta,]{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$">|; 
+
+$key = q/{_inline}92hspace-0.05em^'hspace-0.1em'{_inline}MSF=1.5;AAT;/;
+$cached_env_img{$key} = q|<IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img220.gif"
+ ALT="$92\hspace{-0.05em}^{'\hspace{-0.1em}'}$">|; 
+
+1;
+
diff --git a/src/slalib/sun67.htx/images.tex b/src/slalib/sun67.htx/images.tex
new file mode 100644
index 0000000..8881d62
--- /dev/null
+++ b/src/slalib/sun67.htx/images.tex
@@ -0,0 +1,2852 @@
+\batchmode
+\documentclass[11pt,twoside]{article}
+\makeatletter
+\input{/home/user1/dec/ptw/hypertext/sun67_htx/html.sty}
+\input{/home/user1/dec/ptw/hypertext/sun67_htx/star2html.sty} 
+\setcounter{tocdepth}{2}
+\pagestyle{myheadings}
+
+\markright{SUN/67.45}
+
+\setlength {\textwidth}{160mm}
+        
+\setlength {\textheight}{230mm}
+       
+\setlength {\topmargin}{-5mm}
+         
+
+\setlength {\textwidth}{160mm}
+ 
+
+\setlength {\textheight}{230mm}
+ 
+
+\setlength {\topmargin}{-2mm}
+ 
+
+\setlength {\oddsidemargin}{0mm}
+ 
+
+\setlength {\evensidemargin}{0mm}
+ 
+
+\setlength {\parindent}{0mm}
+ 
+
+\setlength {\parskip}{\medskipamount}
+ 
+
+\setlength {\unitlength}{1mm}
+ 
+
+\latex{\renewcommand {\_}{{\tt\symbol{95}}}}
+
+\newlength {\oldspacing}
+ 
+
+\newcommand{\stardoccategory}  {Starlink User Note}
+
+\newcommand{\stardocinitials}  {SUN}
+
+\newcommand{\stardocsource}    {sun67.45}
+
+\newcommand{\stardocnumber}    {67.45}
+
+\newcommand{\stardocauthors}   {P.\,T.\,Wallace}
+
+\newcommand{\stardocdate}      {12 October 1999}
+
+\newcommand{\stardoctitle}     {SLALIB --- Positional Astronomy Library}
+
+\newcommand{\stardocversion}   {2.4-0}
+
+\newcommand{\stardocmanual}    {Programmer's Manual}
+
+\newcommand{\stardocname}{\stardocinitials /\stardocnumber}
+
+\newcommand{\htmladdnormallinkfoot}[2]{#1\footnote{#2}}
+
+\newcommand{\htmladdnormallink}[2]{#1}
+
+\newcommand{\htmladdimg}[1]{}
+
+\newenvironment{latexonly}{}{}
+
+\newcommand{\hyperref}[4]{#2\ref{#4}#3}
+
+\newcommand{\htmlref}[2]{#1}
+
+\newcommand{\htmlimage}[1]{}
+
+\newcommand{\htmladdtonavigation}[1]{}
+
+\newcommand{\xref}[3]{#1}
+
+\newcommand{\xlabel}[1]{}
+
+\newcommand{\latextohtml}{{\bf LaTeX}{2}{\tt{HTML}}}
+
+\newcommand{\latex}[1]{#1}
+
+\newcommand{\setunderscore}{\renewcommand {\_}{{\tt\symbol{95}}}}
+
+\newcommand{\latexonlytoc}[0]{\tableofcontents}
+
+\newcommand{\nroutines} {183}
+
+\newcommand{\radec}     {$[\,\alpha,\delta\,]$}
+
+\newcommand{\hadec}     {$[\,h,\delta\,]$}
+
+\newcommand{\xieta}     {$[\,\xi,\eta\,]$}
+
+\newcommand{\azel}      {$[\,Az,El~]$}
+
+\newcommand{\ecl}       {$[\,\lambda,\beta~]$}
+
+\newcommand{\gal}       {$[\,l^{I\!I},b^{I\!I}\,]$}
+
+\newcommand{\xy}        {$[\,x,y\,]$}
+
+\newcommand{\xyz}       {$[\,x,y,z\,]$}
+
+\newcommand{\xyzd}      {$[\,\dot{x},\dot{y},\dot{z}\,]$}
+
+\newcommand{\xyzxyzd}   {$[\,x,y,z,\dot{x},\dot{y},\dot{z}\,]$}
+
+\newcommand{\degree}[2] {$#1^{\circ}
+                        \hspace{-0.37em}.\hspace{0.02em}#2$}
+
+\newcommand{\arcsec}[2] {\arcseci{#1}$\hspace{-0.4em}.#2$}
+
+\newcommand{\arcseci}[1] {$#1\hspace{-0.05em}$\raisebox{-0.5ex}
+                         {$^{'\hspace{-0.1em}'}$}}
+
+\renewcommand{\arcseci}[1] {$#1\hspace{-0.05em}^{'\hspace{-0.1em}'}$}
+
+\newcommand{\dms}[4]    {$#1^{\circ}\,#2\raisebox{-0.5ex}
+                        {$^{'}$}\,$\arcsec{#3}{#4}}
+
+\renewcommand{\dms}[4]{$#1^{\circ}\,#2^{'}\,#3^{''}.#4$}
+
+\newcommand{\tseci}[1]   {$#1$\mbox{$^{\rm s}$}}
+
+\newcommand{\tsec}[2]    {\tseci{#1}$\hspace{-0.3em}.#2$}
+
+\renewcommand{\tsec}[2] {$#1^{\rm s}\hspace{-0.3em}.#2$}
+
+\newcommand{\hms}[4]    {$#1^{\rm h}\,#2^{\rm m}\,$\tsec{#3}{#4}}
+
+\renewcommand{\hms}[4] {$#1^{h}\,#2^{m}\,#3^{s}.#4$}
+
+\newcommand{\callhead}[1]{\goodbreak\vspace{\bigskipamount}{\large\bf{#1}}}
+
+\newenvironment{callset}{\begin{list}{}{\setlength{\leftmargin}{2cm}
+                             \setlength{\parsep}{\smallskipamount}}}{\end{list}}
+
+\newcommand{\subp}[1]{\item\hspace{-1cm}#1\\}
+
+\newcommand{\subq}[2]{\item\hspace{-1cm}#1\\\hspace*{-1cm}#2\\}
+
+\newcommand{\name}[1]{\mbox{#1}}
+
+\newcommand{\fortvar}[1]{\mbox{\em #1}}
+
+\newcommand{\routine}[3]
+{\hbadness=10000
+  \vbox
+  {
+    \rule{\textwidth}{0.3mm}\\    {\Large {\bf #1} \hfill #2 \hfill {\bf #1}}\\    \setlength{\oldspacing}{\topsep}
+    \setlength{\topsep}{0.3ex}
+    \begin{description}
+      #3
+    \end{description}
+    \setlength{\topsep}{\oldspacing}
+  }
+}
+
+\renewcommand{\routine}[3]
+   {
+      \subsection{#1\xlabel{#1} - #2\label{#1}}
+       \begin{description}
+         #3
+       \end{description}
+   }
+
+\newcommand{\action}[1]
+{\item[ACTION]: #1}
+
+\newcommand{\call}[1]
+{\item[CALL]: \hspace{0.4em}{\tt #1}}
+
+\renewcommand{\call}[1]
+   {
+    \item[CALL:] {\tt #1}
+   }
+
+\newcommand{\args}[2]
+{
+  \goodbreak
+  \setlength{\oldspacing}{\topsep}
+  \setlength{\topsep}{0.3ex}
+  \begin{description}
+  \item[#1]:\\[1.5ex]
+    \begin{tabular}{p{7em}p{6em}p{22em}}
+      #2
+    \end{tabular}
+  \end{description}
+  \setlength{\topsep}{\oldspacing}
+}
+
+\renewcommand{\args}[2]
+   {
+     \begin{description}
+        \item[#1:]\\        \begin{tabular}{p{7em}p{6em}l}
+           #2
+        \end{tabular}
+     \end{description}
+   }
+
+\newcommand{\spec}[3]
+{
+  {\em {#1}} & {\bf \mbox{#2}} & {#3}
+}
+
+\newcommand{\specel}[2]
+{
+  \multicolumn{1}{c}{#1} & {} & {#2}
+}
+
+\newcommand{\anote}[1]
+{
+  \goodbreak
+  \setlength{\oldspacing}{\topsep}
+  \setlength{\topsep}{0.3ex}
+  \begin{description}
+    \item[NOTE]:
+        #1
+  \end{description}
+  \setlength{\topsep}{\oldspacing}
+}
+
+\renewcommand{\anote}[1]
+   {
+      \begin{description}
+      \item[NOTE:]
+          #1
+      \end{description}
+   }
+
+\newcommand{\notes}[1]
+{
+  \goodbreak
+  \setlength{\oldspacing}{\topsep}
+  \setlength{\topsep}{0.3ex}
+  \begin{description}
+    \item[NOTES]:
+        #1
+  \end{description}
+  \setlength{\topsep}{\oldspacing}
+}
+
+\renewcommand{\notes}[1]
+   {
+      \begin{description}
+         \item[NOTES:]
+            #1
+      \end{description}
+   }
+
+\newcommand{\aref}[1]
+{
+  \goodbreak
+  \setlength{\oldspacing}{\topsep}
+  \setlength{\topsep}{0.3ex}
+  \begin{description}
+    \item[REFERENCE]:
+        #1
+  \end{description}
+  \setlength{\topsep}{\oldspacing}
+}
+
+\newcommand{\refs}[1]
+{
+  \goodbreak
+  \setlength{\oldspacing}{\topsep}
+  \setlength{\topsep}{0.3ex}
+  \begin{description}
+    \item[REFERENCES]:
+        #1
+  \end{description}
+  \setlength{\topsep}{\oldspacing}
+}
+
+\newcommand{\exampleitem}{\item [EXAMPLE]:}
+
+\renewcommand{\exampleitem}{\item [EXAMPLE:]}
+
+\renewcommand{\thepage}{\roman{page}}
+
+\renewcommand{\latexonlytoc}[0]{}
+
+\renewcommand{\thepage}{\arabic{page}}
+\input{/home/user1/dec/ptw/hypertext/sun67_htx/star2html.sty}
+
+
+\makeatother
+\ifx\AtBeginDocument\undefined \newcommand{\AtBeginDocument}[1]{}\fi
+\newenvironment{tex2html_wrap}{}{}
+\newbox\sizebox
+\setlength{\hoffset}{0pt}\setlength{\voffset}{0pt}
+\addtolength{\textheight}{\footskip}\setlength{\footskip}{0pt}
+\addtolength{\textheight}{\topmargin}\setlength{\topmargin}{0pt}
+\addtolength{\textheight}{\headheight}\setlength{\headheight}{0pt}
+\addtolength{\textheight}{\headsep}\setlength{\headsep}{0pt}
+\setlength{\textwidth}{451pt}
+\newwrite\lthtmlwrite
+\makeatletter
+\let\realnormalsize=\normalsize
+\topskip=0pt
+\def\preveqno{}\let\real@float=\@float \let\realend@float=\end@float
+\def\@float{\let\@savefreelist\@freelist\real@float}
+\def\end@float{\realend@float\global\let\@freelist\@savefreelist}
+\let\real@dbflt=\@dbflt \let\end@dblfloat=\end@float
+\let\@largefloatcheck=\relax
+\def\@dbflt{\let\@savefreelist\@freelist\real@dbflt}
+\def\adjustnormalsize{\def\normalsize{\mathsurround=0pt \realnormalsize\parindent=0pt\abovedisplayskip=0pt\belowdisplayskip=0pt}\normalsize}
+\def\lthtmltypeout#1{{\let\protect\string\immediate\write\lthtmlwrite{#1}}}%
+\newcommand\lthtmlhboxmathA{\adjustnormalsize\setbox\sizebox=\hbox\bgroup}%
+\newcommand\lthtmlvboxmathA{\adjustnormalsize\setbox\sizebox=\vbox\bgroup%
+ \let\ifinner=\iffalse }%
+\newcommand\lthtmlboxmathZ{\@next\next\@currlist{}{\def\next{\voidb@x}}%
+ \expandafter\box\next\egroup}%
+\newcommand\lthtmlmathtype[1]{\def\lthtmlmathenv{#1}}%
+\newcommand\lthtmllogmath{\lthtmltypeout{l2hSize %
+:\lthtmlmathenv:\the\ht\sizebox::\the\dp\sizebox::\the\wd\sizebox.\preveqno}}%
+\newcommand\lthtmlfigureA[1]{\let\@savefreelist\@freelist
+       \lthtmlmathtype{#1}\lthtmlvboxmathA}%
+\newcommand\lthtmlfigureZ{\lthtmlboxmathZ\lthtmllogmath\copy\sizebox
+       \global\let\@freelist\@savefreelist}%
+\newcommand\lthtmldisplayA[1]{\lthtmlmathtype{#1}\lthtmlvboxmathA}%
+\newcommand\lthtmldisplayB[1]{\edef\preveqno{(\theequation)}%
+  \lthtmldisplayA{#1}\let\@eqnnum\relax}%
+\newcommand\lthtmldisplayZ{\lthtmlboxmathZ\lthtmllogmath\lthtmlsetmath}%
+\newcommand\lthtmlinlinemathA[1]{\lthtmlmathtype{#1}\lthtmlhboxmathA  \vrule height1.5ex width0pt }%
+\newcommand\lthtmlinlinemathZ{\egroup\expandafter\ifdim\dp\sizebox>0pt %
+  \expandafter\centerinlinemath\fi\lthtmllogmath\lthtmlsetmath}
+\def\lthtmlsetmath{\hbox{\vrule width.5pt\vtop{\vbox{%
+  \kern.5pt\kern0.75 pt\hbox{\hglue.5pt\copy\sizebox\hglue0.75 pt}\kern.5pt%
+  \ifdim\dp\sizebox>0pt\kern0.75 pt\fi}%
+  \ifdim\hsize>\wd\sizebox \hrule depth1pt\fi}}}
+\def\centerinlinemath{\dimen1=\ht\sizebox
+  \ifdim\dimen1<\dp\sizebox \ht\sizebox=\dp\sizebox
+  \else \dp\sizebox=\ht\sizebox \fi}
+
+\def\lthtmlcheckvsize{\ifdim\ht\sizebox<\vsize\expandafter\vfill
+  \else\expandafter\vss\fi}%
+\makeatletter
+
+
+\begin{document}
+\pagestyle{empty}\thispagestyle{empty}%
+\lthtmltypeout{latex2htmlLength hsize=\the\hsize}%
+\lthtmltypeout{latex2htmlLength vsize=\the\vsize}%
+\lthtmltypeout{latex2htmlLength hoffset=\the\hoffset}%
+\lthtmltypeout{latex2htmlLength voffset=\the\voffset}%
+\lthtmltypeout{latex2htmlLength topmargin=\the\topmargin}%
+\lthtmltypeout{latex2htmlLength topskip=\the\topskip}%
+\lthtmltypeout{latex2htmlLength headheight=\the\headheight}%
+\lthtmltypeout{latex2htmlLength headsep=\the\headsep}%
+\lthtmltypeout{latex2htmlLength parskip=\the\parskip}%
+\lthtmltypeout{latex2htmlLength oddsidemargin=\the\oddsidemargin}%
+\makeatletter
+\if@twoside\lthtmltypeout{latex2htmlLength evensidemargin=\the\evensidemargin}%
+\else\lthtmltypeout{latex2htmlLength evensidemargin=\the\oddsidemargin}\fi%
+\makeatother
+\setcounter{tocdepth}{2}
+\stepcounter{section}
+\setcounter{page}{1}
+\stepcounter{section}
+\stepcounter{subsection}
+\stepcounter{subsection}
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline417}%
+$0^{\circ}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline419}%
+$-1^{\circ}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+\stepcounter{subsection}
+\stepcounter{subsection}
+\stepcounter{subsection}
+\stepcounter{subsection}
+\stepcounter{subsection}
+\stepcounter{subsection}
+\stepcounter{subsection}
+\stepcounter{section}
+\stepcounter{section}
+\stepcounter{subsection}
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline528}%
+$[\,\alpha,\delta\,]$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+\stepcounter{subsection}
+
+\setlength {\oldspacing}{\topsep}
+%
+
+
+\setlength {\topsep}{0.3ex}
+%
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline786}%
+$12^{\circ}\,34^{'}\,56^{''}.7$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+
+\setlength {\topsep}{\oldspacing}
+%
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline788}%
+${\circ}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline802}%
+$1/{2 \pi} = 0.1591549430918953358$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline806}%
+$15/{2\pi} = 2.3873241463784300365$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+\stepcounter{subsection}
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline893}%
+$\zeta = 87^{\circ}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+\stepcounter{subsection}
+
+\setlength {\parskip}{\medskipamount}
+%
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline1090}%
+$\times 360/2\pi$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline1092}%
+$\rightarrow$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline1094}%
+$\times (2\pi/86400) \times (360/2\pi)$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline1098}%
+$\times (2\pi/86400)^2 \times (360/2\pi)$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline1102}%
+$[\,0,2\pi\,]$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline1104}%
+$+\pi/2$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline1106}%
+$\pm\pi/2$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+\stepcounter{subsection}
+\stepcounter{subsection}
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline1373}%
+$\times 2 / $%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline1375}%
+$\sqrt{1-\left|\mbox{\bf v}\right|^2}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline1377}%
+$3\times3$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+\stepcounter{subsection}
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline1701}%
+$\Delta$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline1705}%
+$[\,x,y\,]$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline1707}%
+$\mu{\rm m}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline1709}%
+$90^{\circ}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline1711}%
+$\delta$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline1713}%
+$\alpha$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline1715}%
+$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.1$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline1717}%
+$\zeta<70^{\circ}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline1721}%
+$3^{\circ}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline1725}%
+$[\,Az,El~]$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline1729}%
+$[\,h,\delta\,]$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline1745}%
+$\pm$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline1747}%
+$0^{\rm s}\hspace{-0.3em}.9$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline1749}%
+$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.3$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+\stepcounter{subsection}
+\stepcounter{subsection}
+\stepcounter{subsection}
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline2524}%
+$76^\circ$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+\stepcounter{subsection}
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline2704}%
+$0.7\,\mu{\rm m}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline2706}%
+$0.4\,\mu{\rm m}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline2708}%
+$29^\circ$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline2710}%
+$290^\circ$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline2712}%
+$0.0065^\circ m^{-1}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline2716}%
+$15^\circ$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline2718}%
+$1.0\,\mu{\rm m}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline2720}%
+$0.3\,\mu{\rm m}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline2722}%
+$20\,\mu{\rm m}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline2724}%
+$11\hspace{-0.05em}^{'\hspace{-0.1em}'}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline2726}%
+$100\,\mu{\rm m}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline2728}%
+$(\mu-1)$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+\stepcounter{subsection}
+\stepcounter{subsection}
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline2867}%
+$[\lambda,\phi]$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline2869}%
+$\pm \pi$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+\stepcounter{subsection}
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline3016}%
+$\cdots$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+\stepcounter{subsection}
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline3160}%
+$0^{\rm h}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+\stepcounter{subsection}
+\stepcounter{subsection}
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline3380}%
+$[\,x,y,z\,]$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+\stepcounter{subsection}
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline3493}%
+$[\,x,y,z,\dot{x},\dot{y},\dot{z}\,]$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+\stepcounter{subsection}
+\stepcounter{subsection}
+\stepcounter{subsection}
+\stepcounter{subsection}
+\stepcounter{subsection}
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline4117}%
+$2\pi$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline4123}%
+$360^{\circ}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+\stepcounter{subsection}
+\stepcounter{subsection}
+\stepcounter{subsection}
+\stepcounter{subsection}
+\stepcounter{subsection}
+\stepcounter{subsection}
+\stepcounter{subsection}
+
+\setlength {\oldspacing}{\topsep}
+%
+
+
+\setlength {\topsep}{0.3ex}
+%
+
+
+\setlength {\topsep}{\oldspacing}
+%
+
+\stepcounter{subsection}
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline5205}%
+$23^{\rm h}\,59^{\rm m}\,59^{\rm s}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+\stepcounter{subsection}
+\stepcounter{subsection}
+\stepcounter{subsection}
+\stepcounter{subsection}
+\stepcounter{subsection}
+\stepcounter{subsection}
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline5954}%
+$[x_{1},y_{1}\,]$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline5956}%
+$[x_{2},y_{2}\,]$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline5962}%
+$x' = x_{1} + {\rm XZ}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline5964}%
+$y' = y_{1} + {\rm YZ}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline5966}%
+$x'' = x' {\rm XS}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline5968}%
+$y'' = y' {\rm YS}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline5970}%
+$x''' = + x'' \cos {\rm PERP}/2 + y'' \sin {\rm PERP}/2$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline5972}%
+$y''' = + x'' \sin {\rm PERP}/2 + y'' \cos {\rm PERP}/2$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline5974}%
+$x_{2} = + x''' \cos {\rm ORIENT} +
+                          y''' \sin {\rm ORIENT}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline5976}%
+$y_{2} = - x''' \sin {\rm ORIENT} +
+                          y''' \cos {\rm ORIENT}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+\stepcounter{subsection}
+\stepcounter{subsection}
+\stepcounter{subsection}
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline6230}%
+$h,\delta$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline6232}%
+$0\!-\!2\pi$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+\stepcounter{subsection}
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline6347}%
+$\equiv123$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+\stepcounter{subsection}
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline6475}%
+$\pm n.n x \pm n$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline6491}%
+$x\!\pm\!n$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+\stepcounter{subsection}
+\stepcounter{subsection}
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline6713}%
+$^{T}\cdot$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline6717}%
+${\bf \rm M}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+\stepcounter{subsection}
+\stepcounter{subsection}
+\stepcounter{subsection}
+\stepcounter{subsection}
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline7186}%
+$\cdot$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline7188}%
+$n \times n$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+\stepcounter{subsection}
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline7358}%
+$10\hspace{-0.05em}^{'\hspace{-0.1em}'}$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline7360}%
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+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline7362}%
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+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline7364}%
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+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline7366}%
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+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline7368}%
+$18\hspace{-0.05em}^{'\hspace{-0.1em}'}$%
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+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline7370}%
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+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline7374}%
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+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline7376}%
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+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline7378}%
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+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+\stepcounter{subsection}
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline7465}%
+$\times$%
+\lthtmlinlinemathZ
+\hfill\lthtmlcheckvsize\clearpage}
+
+\stepcounter{subsection}
+\stepcounter{subsection}
+\stepcounter{subsection}
+\stepcounter{subsection}
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+\stepcounter{subsection}
+\stepcounter{subsection}
+\stepcounter{subsection}
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+{\newpage\clearpage
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+\stepcounter{subsection}
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+\stepcounter{subsection}
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+\stepcounter{subsection}
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+{\newpage\clearpage
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+{\newpage\clearpage
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+\stepcounter{subsection}
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+
+\stepcounter{subsection}
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+
+{\newpage\clearpage
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+\stepcounter{subsection}
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+{\newpage\clearpage
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+\stepcounter{subsection}
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+
+{\newpage\clearpage
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+
+\stepcounter{subsection}
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+{\newpage\clearpage
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+
+{\newpage\clearpage
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+
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+
+\stepcounter{subsection}
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+\stepcounter{subsection}
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+{\newpage\clearpage
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+\stepcounter{subsection}
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+
+{\newpage\clearpage
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+\stepcounter{subsection}
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+
+{\newpage\clearpage
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+
+\stepcounter{subsection}
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+
+{\newpage\clearpage
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+{\newpage\clearpage
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+
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+
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+
+{\newpage\clearpage
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+
+{\newpage\clearpage
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+
+{\newpage\clearpage
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+
+{\newpage\clearpage
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+{\newpage\clearpage
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+
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+
+{\newpage\clearpage
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+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
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+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
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+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
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+
+{\newpage\clearpage
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+
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+
+{\newpage\clearpage
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+
+{\newpage\clearpage
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+
+{\newpage\clearpage
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+
+{\newpage\clearpage
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+
+{\newpage\clearpage
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+$+20^\circ$%
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+
+{\newpage\clearpage
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+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline22666}%
+$2\mu{\rm m}$%
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+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline22678}%
+$6.5^\circ K km^{-1}$%
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+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
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+$7^\circ$%
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+
+{\newpage\clearpage
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+$\tan^5$%
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+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
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+
+{\newpage\clearpage
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+
+\stepcounter{subsection}
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+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline22935}%
+$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.05$%
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+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
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+$93^\circ$%
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+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline22949}%
+$=93^\circ$%
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+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
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+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
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+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline22959}%
+$\nu=p_w/p_s$%
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+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline22961}%
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+
+\stepcounter{subsection}
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+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline23164}%
+$\zeta=70^\circ$%
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+\hfill\lthtmlcheckvsize\clearpage}
+
+{\newpage\clearpage
+\lthtmlinlinemathA{tex2html_wrap_inline23168}%
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+\lthtmlfigureA{figure27550}%
+\begin{figure}\begin{center}
+\begin{tabular}{|cccccc|}   \hline
+& & & & & \\\hspace{5em} & \hspace{5em} & \hspace{5em} &
+   \hspace{5em} & \hspace{5em} & \hspace{5em}  \\\multicolumn{2}{|c}{\hspace{0em}
+\fbox {\parbox{8.5em}{\center \vspace{-2ex}
+                                                   mean $[\,\alpha,\delta\,]$, FK4, \\                                                   any equinox
+                                                   \vspace{0.5ex}}}
+} &
+ \multicolumn{2}{c}{\hspace{0em}
+\fbox {\parbox{8.5em}{\center \vspace{-2ex}
+                                                   mean $[\,\alpha,\delta\,]$, FK4,
+                                                   no $\mu$, any equinox
+                                                   \vspace{0.5ex}}}
+} &
+\multicolumn{2}{c|}{\hspace{0em}
+\fbox {\parbox{8.5em}{\center \vspace{-2ex}
+                                                   mean $[\,\alpha,\delta\,]$, FK5, \\                                                   any equinox
+                                                   \vspace{0.5ex}}}
+} \\& \multicolumn{2}{|c|}{} & \multicolumn{2}{c|}{} & \\\multicolumn{2}{|c}{space motion} & \multicolumn{1}{c|}{} & &
+   \multicolumn{2}{c|}{space motion} \\\multicolumn{2}{|c}{-- E-terms} &
+   \multicolumn{2}{c}{-- E-terms} & \multicolumn{1}{c|}{} & \\\multicolumn{2}{|c}{precess to B1950} & \multicolumn{2}{c}{precess to B1950} &
+   \multicolumn{2}{c|}{precess to J2000} \\\multicolumn{2}{|c}{+ E-terms} &
+   \multicolumn{2}{c}{+ E-terms} & \multicolumn{1}{c|}{} & \\\multicolumn{2}{|c}{FK4 to FK5, no $\mu$} &
+   \multicolumn{2}{c}{FK4 to FK5, no $\mu$} & \multicolumn{1}{c|}{} & \\\multicolumn{2}{|c}{parallax} & \multicolumn{1}{c|}{} & &
+   \multicolumn{2}{c|}{parallax} \\& \multicolumn{2}{|c|}{} & \multicolumn{2}{c|}{} & \\ \cline{2-5}
+\multicolumn{3}{|c|}{} & & & \\& \multicolumn{4}{c}{
+\fbox {\parbox{18em}{\center \vspace{-2ex}
+                                   FK5, J2000, current epoch, geocentric
+                                          \vspace{0.5ex}}}
+} & \\\multicolumn{3}{|c|}{} & & & \\& \multicolumn{4}{c}{light deflection} & \\& \multicolumn{4}{c}{annual aberration} & \\& \multicolumn{4}{c}{precession/nutation} & \\\multicolumn{3}{|c|}{} & & & \\& \multicolumn{4}{c}{
+\fbox {Apparent $[\,\alpha,\delta\,]$}
+} & \\\multicolumn{3}{|c|}{} & & & \\& \multicolumn{4}{c}{Earth rotation} & \\\multicolumn{3}{|c|}{} & & & \\& \multicolumn{4}{c}{
+\fbox {Apparent $[\,h,\delta\,]$}
+} & \\\multicolumn{3}{|c|}{} & & & \\& \multicolumn{4}{c}{diurnal aberration} & \\\multicolumn{3}{|c|}{} & & & \\& \multicolumn{4}{c}{
+\fbox {Topocentric $[\,h,\delta\,]$}
+} & \\\multicolumn{3}{|c|}{} & & & \\& \multicolumn{4}{c}{$[\,h,\delta\,]$\ to $[\,Az,El~]$} & \\\multicolumn{3}{|c|}{} & & & \\& \multicolumn{4}{c}{
+\fbox {Topocentric $[\,Az,El~]$}
+} & \\\multicolumn{3}{|c|}{} & & & \\& \multicolumn{4}{c}{refraction} & \\\multicolumn{3}{|c|}{} & & & \\& \multicolumn{4}{c}{
+\fbox {Observed $[\,Az,El~]$}
+} & \\& & & & & \\& & & & & \\ \hline
+\end{tabular}
+\end{center}
+\vspace{-0.5ex}
+Star positions are published or catalogued using
+one of the mean $[\,\alpha,\delta\,]$\ systems shown at
+the top.  The ``FK4'' systems
+were used before about 1980 and are usually
+equinox B1950.  The ``FK5'' system, equinox J2000, is now preferred,
+or rather its modern equivalent, the International Celestial Reference
+Frame (in the optical, the Hipparcos catalogue).
+The figure relates a star's mean $[\,\alpha,\delta\,]$\ to the actual
+line-of-sight to the star.
+Note that for the conventional choices of equinox, namely
+B1950 or J2000, all of the precession and E-terms corrections
+are superfluous.
+\end{figure}%
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diff --git a/src/slalib/sun67.htx/img1.gif b/src/slalib/sun67.htx/img1.gif
new file mode 100644
index 0000000..d7b5e28
--- /dev/null
+++ b/src/slalib/sun67.htx/img1.gif
diff --git a/src/slalib/sun67.htx/img10.gif b/src/slalib/sun67.htx/img10.gif
new file mode 100644
index 0000000..b62f1a8
--- /dev/null
+++ b/src/slalib/sun67.htx/img10.gif
diff --git a/src/slalib/sun67.htx/img100.gif b/src/slalib/sun67.htx/img100.gif
new file mode 100644
index 0000000..398505a
--- /dev/null
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diff --git a/src/slalib/sun67.htx/img101.gif b/src/slalib/sun67.htx/img101.gif
new file mode 100644
index 0000000..f058067
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new file mode 100644
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diff --git a/src/slalib/sun67.htx/img103.gif b/src/slalib/sun67.htx/img103.gif
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new file mode 100644
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new file mode 100644
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new file mode 100644
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--- /dev/null
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new file mode 100644
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--- /dev/null
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new file mode 100644
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new file mode 100644
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new file mode 100644
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new file mode 100644
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new file mode 100644
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new file mode 100644
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new file mode 100644
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new file mode 100644
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new file mode 100644
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new file mode 100644
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new file mode 100644
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new file mode 100644
index 0000000..cf79e82
--- /dev/null
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new file mode 100644
index 0000000..a1b4481
--- /dev/null
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new file mode 100644
index 0000000..4acedf7
--- /dev/null
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new file mode 100644
index 0000000..308e155
--- /dev/null
+++ b/src/slalib/sun67.htx/img99.gif
diff --git a/src/slalib/sun67.htx/index_motif.gif b/src/slalib/sun67.htx/index_motif.gif
new file mode 100644
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--- /dev/null
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diff --git a/src/slalib/sun67.htx/internals.pl b/src/slalib/sun67.htx/internals.pl
new file mode 100644
index 0000000..d340e74
--- /dev/null
+++ b/src/slalib/sun67.htx/internals.pl
@@ -0,0 +1,1482 @@
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+$noresave{$key} = "$nosave";
+
+$key = q/SLA_PERTEL/;
+$ref_files{$key} = "$dir".q|node144.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_CLYD/;
+$ref_files{$key} = "$dir".q|node34.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DAT/;
+$ref_files{$key} = "$dir".q|node44.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_EPB2D/;
+$ref_files{$key} = "$dir".q|node93.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_SVDSOL/;
+$ref_files{$key} = "$dir".q|node182.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_GRESID/;
+$ref_files{$key} = "$dir".q|node117.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_PRENUT/;
+$ref_files{$key} = "$dir".q|node155.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_DTF2D/;
+$ref_files{$key} = "$dir".q|node74.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_EPJ2D/;
+$ref_files{$key} = "$dir".q|node96.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_PERTUE/;
+$ref_files{$key} = "$dir".q|node145.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_PXY/;
+$ref_files{$key} = "$dir".q|node159.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DS2C6/;
+$ref_files{$key} = "$dir".q|node70.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_ECOR/;
+$ref_files{$key} = "$dir".q|node89.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_CR2TF/;
+$ref_files{$key} = "$dir".q|node37.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_DTF2R/;
+$ref_files{$key} = "$dir".q|node75.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_PDA2H/;
+$ref_files{$key} = "$dir".q|node141.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_CD2TF/;
+$ref_files{$key} = "$dir".q|node32.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_EARTH/;
+$ref_files{$key} = "$dir".q|node86.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_SMAT/;
+$ref_files{$key} = "$dir".q|node177.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_ECLEQ/;
+$ref_files{$key} = "$dir".q|node87.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_EPB/;
+$ref_files{$key} = "$dir".q|node92.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_DTT/;
+$ref_files{$key} = "$dir".q|node80.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_MOON/;
+$ref_files{$key} = "$dir".q|node130.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_SVD/;
+$ref_files{$key} = "$dir".q|node180.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_DR2AF/;
+$ref_files{$key} = "$dir".q|node66.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_RANORM/;
+$ref_files{$key} = "$dir".q|node162.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_DV2TP/;
+$ref_files{$key} = "$dir".q|node81.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_AIRMAS/;
+$ref_files{$key} = "$dir".q|node16.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_CLDJ/;
+$ref_files{$key} = "$dir".q|node33.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_PERMUT/;
+$ref_files{$key} = "$dir".q|node143.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_EPJ/;
+$ref_files{$key} = "$dir".q|node95.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_PDQ2H/;
+$ref_files{$key} = "$dir".q|node142.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_SVDCOV/;
+$ref_files{$key} = "$dir".q|node181.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_M2AV/;
+$ref_files{$key} = "$dir".q|node125.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_INTIN/;
+$ref_files{$key} = "$dir".q|node122.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_SVDSOL/;
+$ref_files{$key} = "$dir".q|node182.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_GRESID/;
+$ref_files{$key} = "$dir".q|node117.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_CALDJ/;
+$ref_files{$key} = "$dir".q|node28.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_PRENUT/;
+$ref_files{$key} = "$dir".q|node155.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_CALYD/;
+$ref_files{$key} = "$dir".q|node29.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_CS2C6/;
+$ref_files{$key} = "$dir".q|node39.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DAF2R/;
+$ref_files{$key} = "$dir".q|node42.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DCC2S/;
+$ref_files{$key} = "$dir".q|node49.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DCS2C/;
+$ref_files{$key} = "$dir".q|node51.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_PA/;
+$ref_files{$key} = "$dir".q|node138.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_FK5HZ/;
+$ref_files{$key} = "$dir".q|node109.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_PV2EL/;
+$ref_files{$key} = "$dir".q|node156.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DAV2M/;
+$ref_files{$key} = "$dir".q|node45.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_OAPQK/;
+$ref_files{$key} = "$dir".q|node136.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_EULER/;
+$ref_files{$key} = "$dir".q|node101.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_EL2UE/;
+$ref_files{$key} = "$dir".q|node91.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_PM/;
+$ref_files{$key} = "$dir".q|node149.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_MAP/;
+$ref_files{$key} = "$dir".q|node126.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DBEAR/;
+$ref_files{$key} = "$dir".q|node46.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_PV2UE/;
+$ref_files{$key} = "$dir".q|node157.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_E2H/;
+$ref_files{$key} = "$dir".q|node85.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_DVDV/;
+$ref_files{$key} = "$dir".q|node82.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_DM2AV/;
+$ref_files{$key} = "$dir".q|node60.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_SEP/;
+$ref_files{$key} = "$dir".q|node176.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_AIRMAS/;
+$ref_files{$key} = "$dir".q|node16.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_PERMUT/;
+$ref_files{$key} = "$dir".q|node143.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_UE2EL/;
+$ref_files{$key} = "$dir".q|node187.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/stardoccontents/;
+$ref_files{$key} = "$dir".q|sun67.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_H2FK5/;
+$ref_files{$key} = "$dir".q|node119.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_FK425/;
+$ref_files{$key} = "$dir".q|node104.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DS2TP/;
+$ref_files{$key} = "$dir".q|node71.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_DH2E/;
+$ref_files{$key} = "$dir".q|node56.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DTPS2C/;
+$ref_files{$key} = "$dir".q|node78.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_AOPPA/;
+$ref_files{$key} = "$dir".q|node21.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_REFV/;
+$ref_files{$key} = "$dir".q|node168.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_DVN/;
+$ref_files{$key} = "$dir".q|node83.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_abstract/;
+$ref_files{$key} = "$dir".q|node1.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_GALEQ/;
+$ref_files{$key} = "$dir".q|node111.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_DPAV/;
+$ref_files{$key} = "$dir".q|node65.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_REFZ/;
+$ref_files{$key} = "$dir".q|node169.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_CAF2R/;
+$ref_files{$key} = "$dir".q|node27.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_UNPCD/;
+$ref_files{$key} = "$dir".q|node189.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_ALTAZ/;
+$ref_files{$key} = "$dir".q|node17.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_PA/;
+$ref_files{$key} = "$dir".q|node138.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_INVF/;
+$ref_files{$key} = "$dir".q|node123.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_CC62S/;
+$ref_files{$key} = "$dir".q|node31.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DE2H/;
+$ref_files{$key} = "$dir".q|node53.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_AMPQK/;
+$ref_files{$key} = "$dir".q|node19.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DMAT/;
+$ref_files{$key} = "$dir".q|node61.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_PM/;
+$ref_files{$key} = "$dir".q|node149.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_GEOC/;
+$ref_files{$key} = "$dir".q|node114.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_AMP/;
+$ref_files{$key} = "$dir".q|node18.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_ETRMS/;
+$ref_files{$key} = "$dir".q|node100.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_OAP/;
+$ref_files{$key} = "$dir".q|node135.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_FLOTIN/;
+$ref_files{$key} = "$dir".q|node110.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DTT/;
+$ref_files{$key} = "$dir".q|node80.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DSEP/;
+$ref_files{$key} = "$dir".q|node72.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_SVD/;
+$ref_files{$key} = "$dir".q|node180.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_ADDET/;
+$ref_files{$key} = "$dir".q|node14.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_IMXV/;
+$ref_files{$key} = "$dir".q|node121.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_HFK5Z/;
+$ref_files{$key} = "$dir".q|node120.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_TP2S/;
+$ref_files{$key} = "$dir".q|node183.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_PREBN/;
+$ref_files{$key} = "$dir".q|node151.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_TP2V/;
+$ref_files{$key} = "$dir".q|node184.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_DTPS2C/;
+$ref_files{$key} = "$dir".q|node78.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_AOPQK/;
+$ref_files{$key} = "$dir".q|node23.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_AFIN/;
+$ref_files{$key} = "$dir".q|node15.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_DMXM/;
+$ref_files{$key} = "$dir".q|node63.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_EQEQX/;
+$ref_files{$key} = "$dir".q|node98.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DRANRM/;
+$ref_files{$key} = "$dir".q|node69.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DBJIN/;
+$ref_files{$key} = "$dir".q|node47.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_POLMO/;
+$ref_files{$key} = "$dir".q|node150.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_RVLG/;
+$ref_files{$key} = "$dir".q|node172.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_GMSTA/;
+$ref_files{$key} = "$dir".q|node116.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DCMPF/;
+$ref_files{$key} = "$dir".q|node50.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_PVOBS/;
+$ref_files{$key} = "$dir".q|node158.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_DMXV/;
+$ref_files{$key} = "$dir".q|node64.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_FK524/;
+$ref_files{$key} = "$dir".q|node106.html|; 
+$noresave{$key} = "$nosave";
+
+1;
+
diff --git a/src/slalib/sun67.htx/invis_anchor.xbm b/src/slalib/sun67.htx/invis_anchor.xbm
new file mode 100644
index 0000000..cc208a3
--- /dev/null
+++ b/src/slalib/sun67.htx/invis_anchor.xbm
@@ -0,0 +1,4 @@
+#define dot_anchor_width 1
+#define dot_anchor_height 1
+static char dot_anchor_bits[] = {
+ 0xfe};
diff --git a/src/slalib/sun67.htx/labels.pl b/src/slalib/sun67.htx/labels.pl
new file mode 100644
index 0000000..ab31648
--- /dev/null
+++ b/src/slalib/sun67.htx/labels.pl
@@ -0,0 +1,1482 @@
+# LaTeX2HTML 97.1 (release) (July 13th, 1997)
+# Associate labels original text with physical files.
+
+
+$key = q/SLA_DR2TF/;
+$external_labels{$key} = "$URL/" . q|node67.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_OBS/;
+$external_labels{$key} = "$URL/" . q|node137.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DD2TF/;
+$external_labels{$key} = "$URL/" . q|node52.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_DIMXV/;
+$external_labels{$key} = "$URL/" . q|node57.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_PRECL/;
+$external_labels{$key} = "$URL/" . q|node154.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_EVP/;
+$external_labels{$key} = "$URL/" . q|node102.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_FLOTIN/;
+$external_labels{$key} = "$URL/" . q|node110.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_DTP2S/;
+$external_labels{$key} = "$URL/" . q|node76.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_RANGE/;
+$external_labels{$key} = "$URL/" . q|node161.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_NUTC/;
+$external_labels{$key} = "$URL/" . q|node134.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_TPV2C/;
+$external_labels{$key} = "$URL/" . q|node186.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_DTP2V/;
+$external_labels{$key} = "$URL/" . q|node77.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_VDV/;
+$external_labels{$key} = "$URL/" . q|node191.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_FK52H/;
+$external_labels{$key} = "$URL/" . q|node107.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DVN/;
+$external_labels{$key} = "$URL/" . q|node83.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_PREC/;
+$external_labels{$key} = "$URL/" . q|node152.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_EQECL/;
+$external_labels{$key} = "$URL/" . q|node97.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_H2E/;
+$external_labels{$key} = "$URL/" . q|node118.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_AOP/;
+$external_labels{$key} = "$URL/" . q|node20.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_DS2C6/;
+$external_labels{$key} = "$URL/" . q|node70.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_DRANRM/;
+$external_labels{$key} = "$URL/" . q|node69.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_PAV/;
+$external_labels{$key} = "$URL/" . q|node139.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_FITXY/;
+$external_labels{$key} = "$URL/" . q|node103.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_CS2C/;
+$external_labels{$key} = "$URL/" . q|node38.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_CC2S/;
+$external_labels{$key} = "$URL/" . q|node30.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DT/;
+$external_labels{$key} = "$URL/" . q|node73.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_PDA2H/;
+$external_labels{$key} = "$URL/" . q|node141.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_RVLSRD/;
+$external_labels{$key} = "$URL/" . q|node173.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_EG50/;
+$external_labels{$key} = "$URL/" . q|node90.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DMOON/;
+$external_labels{$key} = "$URL/" . q|node62.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DJCAL/;
+$external_labels{$key} = "$URL/" . q|node58.html|; 
+$noresave{$key} = "$nosave";
+
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+
+$key = q/SLA_DVN/;
+$external_labels{$key} = "$URL/" . q|node83.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_abstract/;
+$external_labels{$key} = "$URL/" . q|node1.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_GALEQ/;
+$external_labels{$key} = "$URL/" . q|node111.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_DPAV/;
+$external_labels{$key} = "$URL/" . q|node65.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_REFZ/;
+$external_labels{$key} = "$URL/" . q|node169.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_CAF2R/;
+$external_labels{$key} = "$URL/" . q|node27.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_UNPCD/;
+$external_labels{$key} = "$URL/" . q|node189.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_ALTAZ/;
+$external_labels{$key} = "$URL/" . q|node17.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_PA/;
+$external_labels{$key} = "$URL/" . q|node138.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_INVF/;
+$external_labels{$key} = "$URL/" . q|node123.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_CC62S/;
+$external_labels{$key} = "$URL/" . q|node31.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DE2H/;
+$external_labels{$key} = "$URL/" . q|node53.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_AMPQK/;
+$external_labels{$key} = "$URL/" . q|node19.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DMAT/;
+$external_labels{$key} = "$URL/" . q|node61.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_PM/;
+$external_labels{$key} = "$URL/" . q|node149.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_GEOC/;
+$external_labels{$key} = "$URL/" . q|node114.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_AMP/;
+$external_labels{$key} = "$URL/" . q|node18.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_ETRMS/;
+$external_labels{$key} = "$URL/" . q|node100.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_OAP/;
+$external_labels{$key} = "$URL/" . q|node135.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_FLOTIN/;
+$external_labels{$key} = "$URL/" . q|node110.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DTT/;
+$external_labels{$key} = "$URL/" . q|node80.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DSEP/;
+$external_labels{$key} = "$URL/" . q|node72.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_SVD/;
+$external_labels{$key} = "$URL/" . q|node180.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_ADDET/;
+$external_labels{$key} = "$URL/" . q|node14.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_IMXV/;
+$external_labels{$key} = "$URL/" . q|node121.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_HFK5Z/;
+$external_labels{$key} = "$URL/" . q|node120.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_TP2S/;
+$external_labels{$key} = "$URL/" . q|node183.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_PREBN/;
+$external_labels{$key} = "$URL/" . q|node151.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_TP2V/;
+$external_labels{$key} = "$URL/" . q|node184.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_DTPS2C/;
+$external_labels{$key} = "$URL/" . q|node78.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_AOPQK/;
+$external_labels{$key} = "$URL/" . q|node23.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_AFIN/;
+$external_labels{$key} = "$URL/" . q|node15.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_DMXM/;
+$external_labels{$key} = "$URL/" . q|node63.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_EQEQX/;
+$external_labels{$key} = "$URL/" . q|node98.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DRANRM/;
+$external_labels{$key} = "$URL/" . q|node69.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DBJIN/;
+$external_labels{$key} = "$URL/" . q|node47.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_POLMO/;
+$external_labels{$key} = "$URL/" . q|node150.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_RVLG/;
+$external_labels{$key} = "$URL/" . q|node172.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_GMSTA/;
+$external_labels{$key} = "$URL/" . q|node116.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_DCMPF/;
+$external_labels{$key} = "$URL/" . q|node50.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_PVOBS/;
+$external_labels{$key} = "$URL/" . q|node158.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/SLA_DMXV/;
+$external_labels{$key} = "$URL/" . q|node64.html|; 
+$noresave{$key} = "$nosave";
+
+$key = q/xref_SLA_FK524/;
+$external_labels{$key} = "$URL/" . q|node106.html|; 
+$noresave{$key} = "$nosave";
+
+1;
+
diff --git a/src/slalib/sun67.htx/next_group_motif.gif b/src/slalib/sun67.htx/next_group_motif.gif
new file mode 100644
index 0000000..833af4d
--- /dev/null
+++ b/src/slalib/sun67.htx/next_group_motif.gif
diff --git a/src/slalib/sun67.htx/next_group_motif_gr.gif b/src/slalib/sun67.htx/next_group_motif_gr.gif
new file mode 100644
index 0000000..c04fec3
--- /dev/null
+++ b/src/slalib/sun67.htx/next_group_motif_gr.gif
diff --git a/src/slalib/sun67.htx/next_motif.gif b/src/slalib/sun67.htx/next_motif.gif
new file mode 100644
index 0000000..7a2dbe9
--- /dev/null
+++ b/src/slalib/sun67.htx/next_motif.gif
diff --git a/src/slalib/sun67.htx/next_motif_gr.gif b/src/slalib/sun67.htx/next_motif_gr.gif
new file mode 100644
index 0000000..1416b1c
--- /dev/null
+++ b/src/slalib/sun67.htx/next_motif_gr.gif
diff --git a/src/slalib/sun67.htx/node1.html b/src/slalib/sun67.htx/node1.html
new file mode 100644
index 0000000..0a5b6da
--- /dev/null
+++ b/src/slalib/sun67.htx/node1.html
@@ -0,0 +1,65 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Abstract</TITLE>
+<META NAME="description" CONTENT="Abstract">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node2.html">
+<LINK REL="previous" HREF="sun67.html">
+<LINK REL="up" HREF="sun67.html">
+<LINK REL="next" HREF="node2.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html246" HREF="node2.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html244" HREF="sun67.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html238" HREF="sun67.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html247" HREF="node2.html">INTRODUCTION</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html245" HREF="sun67.html">SLALIB   Positional Astronomy Library</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html239" HREF="sun67.html">SLALIB   Positional Astronomy Library</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H1><A NAME="SECTION00010000000000000000">Abstract</A>
+<A NAME="xref_abstract">&#160;</A>
+</H1>
+SLALIB is a library used by writers of positional-astronomy applications.
+Most of the 183 routines are concerned with astronomical position and time,
+but a number have wider trigonometrical, numerical or general applications.
+<P>
+<BR> <HR>
+<A NAME="tex2html246" HREF="node2.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html244" HREF="sun67.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html238" HREF="sun67.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html247" HREF="node2.html">INTRODUCTION</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html245" HREF="sun67.html">SLALIB   Positional Astronomy Library</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html239" HREF="sun67.html">SLALIB   Positional Astronomy Library</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node10.html b/src/slalib/sun67.htx/node10.html
new file mode 100644
index 0000000..4a6a393
--- /dev/null
+++ b/src/slalib/sun67.htx/node10.html
@@ -0,0 +1,75 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>New Functions</TITLE>
+<META NAME="description" CONTENT="New Functions">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node11.html">
+<LINK REL="previous" HREF="node9.html">
+<LINK REL="up" HREF="node2.html">
+<LINK REL="next" HREF="node11.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html345" HREF="node11.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html343" HREF="node2.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html337" HREF="node9.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html346" HREF="node11.html">Acknowledgements</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html344" HREF="node2.html">INTRODUCTION</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html338" HREF="node9.html">Future Versions</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION00028000000000000000">
+New Functions</A>
+</H2>
+In a package like SLALIB it is difficult to know how far to go.  Is it
+enough to provide the primitive operations, or should more
+complicated functions be packaged?  Is it worth encroaching on
+specialist areas, where individual experts have all written their
+own software already?  To what extent should CPU efficiency be
+an issue?  How much support of different numerical precisions is
+required?  And so on.
+<P>
+In practice, almost all the routines in SLALIB are there because they were
+needed for some specific application, and this is likely to remain the
+pattern for any enhancements in the future.
+Suggestions for additional SLALIB routines should be addressed to the
+author.
+<P>
+<BR> <HR>
+<A NAME="tex2html345" HREF="node11.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html343" HREF="node2.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html337" HREF="node9.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html346" HREF="node11.html">Acknowledgements</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html344" HREF="node2.html">INTRODUCTION</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html338" HREF="node9.html">Future Versions</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node100.html b/src/slalib/sun67.htx/node100.html
new file mode 100644
index 0000000..104db1d
--- /dev/null
+++ b/src/slalib/sun67.htx/node100.html
@@ -0,0 +1,110 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_ETRMS - E-terms of Aberration</TITLE>
+<META NAME="description" CONTENT="SLA_ETRMS - E-terms of Aberration">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node101.html">
+<LINK REL="previous" HREF="node99.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node101.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1426" HREF="node101.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1424" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1418" HREF="node99.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1427" HREF="node101.html">SLA_EULER - Rotation Matrix from Euler Angles</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1425" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1419" HREF="node99.html">SLA_EQGAL - J2000 to Galactic</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000487000000000000000">SLA_ETRMS - E-terms of Aberration</A>
+<A NAME="xref_SLA_ETRMS">&#160;</A><A NAME="SLA_ETRMS">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Compute the E-terms vector - the part of the annual
+aberration which arises from the eccentricity of the
+         Earth's orbit.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_ETRMS (EP, EV)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EP</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>Besselian epoch</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EV</EM></TD>
+<TH ALIGN="LEFT"><B>D(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>E-terms as <IMG WIDTH="96" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img109.gif"
+ ALT="$[\Delta x, \Delta y, \Delta z\,]$"></TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTE:</STRONG>
+<DD>Note the use of the J2000 aberration constant (
+<IMG WIDTH="64" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img110.gif"
+ ALT="$20\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.49552$">   ).
+       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.
+      </DL>
+<P>     <DL>
+<DT><STRONG>REFERENCES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Smith, C.A. <I>et al.</I>, 1989.  <I>Astr.J.</I> <B>97</B>, 265.
+<DT>2.
+<DD>Yallop, B.D. <I>et al.</I>, 1989.  <I>Astr.J.</I> <B>97</B>, 274.
+</DL></DL>
+<BR> <HR>
+<A NAME="tex2html1426" HREF="node101.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1424" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1418" HREF="node99.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1427" HREF="node101.html">SLA_EULER - Rotation Matrix from Euler Angles</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1425" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1419" HREF="node99.html">SLA_EQGAL - J2000 to Galactic</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node101.html b/src/slalib/sun67.htx/node101.html
new file mode 100644
index 0000000..e5bdda2
--- /dev/null
+++ b/src/slalib/sun67.htx/node101.html
@@ -0,0 +1,132 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_EULER - Rotation Matrix from Euler Angles</TITLE>
+<META NAME="description" CONTENT="SLA_EULER - Rotation Matrix from Euler Angles">
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+<BR>
+<B>Up:</B> <A NAME="tex2html1435" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
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+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000488000000000000000">SLA_EULER - Rotation Matrix from Euler Angles</A>
+<A NAME="xref_SLA_EULER">&#160;</A><A NAME="SLA_EULER">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Form a rotation matrix from the Euler angles - three
+successive rotations about specified Cartesian axes
+         (single precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_EULER (ORDER, PHI, THETA, PSI, RMAT)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ORDER</EM></TD>
+<TH ALIGN="LEFT"><B>C*(*)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>specifies about which axes the rotations occur</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PHI</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>1st rotation (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>THETA</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>2nd rotation (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PSI</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>3rd rotation (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RMAT</EM></TD>
+<TH ALIGN="LEFT"><B>R(3,3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>rotation matrix</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>A rotation is positive when the reference frame rotates
+anticlockwise as seen looking towards the origin from the
+positive region of the specified axis.
+  <DT>2.
+<DD>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 <I>z</I>-axis, followed by THETA radians about the resulting
+        <I>x</I>-axis,
+        then PSI radians about the resulting <I>z</I>-axis.  In detail:
+        <UL>
+<LI> 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 <I>xyz</I> (<IMG WIDTH="44" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img67.gif"
+ ALT="$\equiv123$">)               triad is right-handed.  Thus, the `ZXZ' example given above
+               could be written `zxz' or `313' (or even `ZxZ' or `3xZ').
+<LI> ORDER is terminated by length or by the first unrecognized
+               character.
+<LI> Fewer than three rotations are acceptable, in which case
+               the later angle arguments are ignored.
+        </UL>
+  <DT>3.
+<DD>Zero rotations produces a unit RMAT.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1436" HREF="node102.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1437" HREF="node102.html">SLA_EVP - Earth Position &amp; Velocity</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1435" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1429" HREF="node100.html">SLA_ETRMS - E-terms of Aberration</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node102.html b/src/slalib/sun67.htx/node102.html
new file mode 100644
index 0000000..d22b187
--- /dev/null
+++ b/src/slalib/sun67.htx/node102.html
@@ -0,0 +1,149 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_EVP - Earth Position &amp; Velocity</TITLE>
+<META NAME="description" CONTENT="SLA_EVP - Earth Position &amp; Velocity">
+<META NAME="keywords" CONTENT="sun67">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1447" HREF="node103.html">SLA_FITXY - Fit Linear Model to Two Sets</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1445" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
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+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000489000000000000000">SLA_EVP - Earth Position &amp; Velocity</A>
+<A NAME="xref_SLA_EVP">&#160;</A><A NAME="SLA_EVP">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Barycentric and heliocentric velocity and position of the Earth.
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_EVP (DATE, DEQX, DVB, DPB, DVH, DPH)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>TDB (formerly ET) as a Modified Julian Date
+(JD-2400000.5)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DEQX</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>Julian Epoch (<I>e.g.</I> 2000D0) of mean equator and
+equinox of the vectors returned.  If DEQX&nbsp;&lt;0,
+all vectors are referred to the mean equator and
+equinox (FK5) of date DATE.</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DVB</EM></TD>
+<TH ALIGN="LEFT"><B>D(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>barycentric <IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img111.gif"
+ ALT="$[\,\dot{x},\dot{y},\dot{z}\,]$">, AU&nbsp;s<SUP>-1</SUP></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DPB</EM></TD>
+<TD ALIGN="LEFT"><B>D(3)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>barycentric <IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$">, AU</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DVH</EM></TD>
+<TD ALIGN="LEFT"><B>D(3)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>heliocentric <IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img111.gif"
+ ALT="$[\,\dot{x},\dot{y},\dot{z}\,]$">, AU&nbsp;s<SUP>-1</SUP></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DPH</EM></TD>
+<TD ALIGN="LEFT"><B>D(3)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>heliocentric <IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$">, AU</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>This routine is used when accuracy is more important
+than CPU time, yet the extra complication of reading a
+pre-computed ephemeris is not justified.  The maximum
+        deviations from the JPL&nbsp;DE96 ephemeris are as follows:
+        <UL>
+<LI> velocity (barycentric or heliocentric): 420&nbsp;mm&nbsp;s<SUP>-1</SUP>
+<LI> position (barycentric): 6900&nbsp;km
+<LI> position (heliocentric): 1600&nbsp;km
+        </UL>
+  <DT>2.
+<DD>The routine is an adaption of the BARVEL and BARCOR
+        subroutines of P.Stumpff, which are described in
+        <I>Astr.Astrophys.Suppl.Ser.</I> <B>41</B>, 1-8 (1980).
+        Most of the changes are merely cosmetic and do not affect
+        the results at all.  However, some adjustments have been
+        made so as to give results that refer to the new (IAU 1976
+        `FK5') equinox and precession, although the differences these
+        changes make relative to the results from Stumpff's original
+        `FK4' version are smaller than the inherent accuracy of the
+        algorithm.  One minor shortcoming in the original routines
+        that has <B>not</B> been corrected is that slightly better
+        numerical accuracy could be achieved if the various polynomial
+        evaluations were to be so arranged that the smallest terms were
+        computed first.  Note also that one of Stumpff's precession
+        constants differs by 
+      <IMG WIDTH="39" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img112.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.001$">    from the value given in the
+        <I>Explanatory Supplement</I>.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1446" HREF="node103.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+<A NAME="tex2html1438" HREF="node101.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1447" HREF="node103.html">SLA_FITXY - Fit Linear Model to Two Sets</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1445" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1439" HREF="node101.html">SLA_EULER - Rotation Matrix from Euler Angles</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node103.html b/src/slalib/sun67.htx/node103.html
new file mode 100644
index 0000000..4525328
--- /dev/null
+++ b/src/slalib/sun67.htx/node103.html
@@ -0,0 +1,170 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_FITXY - Fit Linear Model to Two Sets</TITLE>
+<META NAME="description" CONTENT="SLA_FITXY - Fit Linear Model to Two Sets">
+<META NAME="keywords" CONTENT="sun67">
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+<A NAME="tex2html1454" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1448" HREF="node102.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1457" HREF="node104.html">SLA_FK425 - FK4 to FK5</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1455" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1449" HREF="node102.html">SLA_EVP - Earth Position &amp; Velocity</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000490000000000000000">&#160;</A><A NAME="xref_SLA_FITXY">&#160;</A><A NAME="SLA_FITXY">&#160;</A>
+<BR>
+SLA_FITXY - Fit Linear Model to Two <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> Sets
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Fit a linear model to relate two sets of <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> coordinates.
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_FITXY (ITYPE,NP,XYE,XYM,COEFFS,J)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ITYPE</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>type of model: 4 or 6 (note 1)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NP</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>number of samples (note 2)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>XYE</EM></TD>
+<TD ALIGN="LEFT"><B>D(2,NP)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>expected <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> for each sample</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>XYM</EM></TD>
+<TD ALIGN="LEFT"><B>D(2,NP)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>measured <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> for each sample</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>COEFFS</EM></TD>
+<TH ALIGN="LEFT"><B>D(6)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>coefficients of model (note 3)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  0 = OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -1 = illegal ITYPE</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -2 = insufficient data</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -3 = singular solution</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>ITYPE, which must be either 4 or 6, selects the type of model
+fitted.  Both allowed ITYPE values produce a model COEFFS which
+consists of six coefficients, namely the zero points and, for
+        each of XE and YE, the coefficient of XM and YM.  For ITYPE=6,
+        all six coefficients are independent, modelling squash and shear
+        as well as origin, scale, and orientation.  However, ITYPE=4
+        selects the <I>solid body rotation</I> option;  the model COEFFS
+        still consists of the same six coefficients, but now two of
+        them are used twice (appropriately signed).  Origin, scale
+        and orientation are still modelled, but not squash or shear -
+        the units of X and Y have to be the same.
+  <DT>2.
+<DD>For NC=4, NP must be at least 2.  For NC=6, NP must be at
+        least 3.
+  <DT>3.
+<DD>The model is returned in the array COEFFS.  Naming the
+        six elements of COEFFS <I>a</I>,<I>b</I>,<I>c</I>,<I>d</I>,<I>e</I> &amp; <I>f</I>,
+        the model transforms <I>measured</I> coordinates
+        <IMG WIDTH="63" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img113.gif"
+ ALT="$[x_{m},y_{m}\,]$"> into <I>expected</I> coordinates
+        <IMG WIDTH="52" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img114.gif"
+ ALT="$[x_{e},y_{e}\,]$"> as follows:
+        <BLOCKQUOTE><I>x</I><SUB><I>e</I></SUB> = <I>a</I> + <I>bx</I><SUB><I>m</I></SUB> + <I>cy</I><SUB><I>m</I></SUB> <BR>
+         <I>y</I><SUB><I>e</I></SUB> = <I>d</I> + <I>ex</I><SUB><I>m</I></SUB> + <I>fy</I><SUB><I>m</I></SUB></BLOCKQUOTE>
+        For the <I>solid body rotation</I> option (ITYPE=4), the
+        magnitudes of <I>b</I> and <I>f</I>, and of <I>c</I> and <I>e</I>, are equal.  The
+        signs of these coefficients depend on whether there is a
+        sign reversal between [<I>x</I><SUB><I>e</I></SUB>,<I>y</I><SUB><I>e</I></SUB>] and [<I>x</I><SUB><I>m</I></SUB>,<I>y</I><SUB><I>m</I></SUB>];
+        fits are performed
+        with and without a sign reversal and the best one chosen.
+  <DT>4.
+<DD>Error status values J=-1 and -2 leave COEFFS unchanged;
+        if J=-3 COEFFS may have been changed.
+  <DT>5.
+<DD>See also sla_PXY, sla_INVF, sla_XY2XY, sla_DCMPF.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1456" HREF="node104.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1454" HREF="node13.html">
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+<A NAME="tex2html1448" HREF="node102.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1457" HREF="node104.html">SLA_FK425 - FK4 to FK5</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1455" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1449" HREF="node102.html">SLA_EVP - Earth Position &amp; Velocity</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node104.html b/src/slalib/sun67.htx/node104.html
new file mode 100644
index 0000000..0a2f9ca
--- /dev/null
+++ b/src/slalib/sun67.htx/node104.html
@@ -0,0 +1,208 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_FK425 - FK4 to FK5</TITLE>
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1467" HREF="node105.html">SLA_FK45Z - FK4 to FK5, no P.M. or Parallax</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1465" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1459" HREF="node103.html">SLA_FITXY - Fit Linear Model to Two Sets</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000491000000000000000">SLA_FK425 - FK4 to FK5</A>
+<A NAME="xref_SLA_FK425">&#160;</A><A NAME="SLA_FK425">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Convert B1950.0 FK4 star data to J2000.0 FK5.
+This routine converts stars from the old, Bessel-Newcomb, FK4
+         system to the new, IAU&nbsp;1976, FK5, Fricke system.  The precepts
+         of Smith&nbsp;<I>et&nbsp;al.</I> (see reference&nbsp;1) are followed,
+         using the implementation
+         by Yallop&nbsp;<I>et&nbsp;al.</I> (reference&nbsp;2) of a matrix method
+         due to Standish.
+         Kinoshita's development of Andoyer's post-Newcomb precession is
+         used.  The numerical constants from 
+         Seidelmann&nbsp;<I>et&nbsp;al.</I>  (reference&nbsp;3) are used canonically.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_FK425 (
+         R1950,D1950,DR1950,DD1950,P1950,V1950,
+         R2000,D2000,DR2000,DD2000,P2000,V2000)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>R1950</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>B1950.0 <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>D1950</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>B1950.0 <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DR1950</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>B1950.0 proper motion in <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$">(radians per tropical year)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DD1950</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>B1950.0 proper motion in <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$">(radians per tropical year)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>P1950</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>B1950.0 parallax (arcsec)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V1950</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>B1950.0 radial velocity (km&nbsp;s<SUP>-1</SUP>, +ve = moving away)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>R2000</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>D2000</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DR2000</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 proper motion in <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$">(radians per Julian year)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DD2000</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 proper motion in <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$">(radians per Julian year)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>P2000</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 parallax (arcsec)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V2000</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 radial velocity (km&nbsp;s<SUP>-1</SUP>, +ve = moving away)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> proper motions are <IMG WIDTH="13" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img115.gif"
+ ALT="$\dot{\alpha}$"> rather than
+<IMG WIDTH="48" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img116.gif"
+ ALT="$\dot{\alpha}\cos\delta$">, and are per year rather than per century.
+<DT>2.
+<DD>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 FK425
+        is called.
+  <DT>3.
+<DD>In the FK4 catalogue the proper motions of stars within
+        <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img117.gif"
+ ALT="$10^{\circ}$"> of the poles do not include the <I>differential
+        E-terms</I> 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 J2000,
+        and measuring on the sky rather than in terms of <IMG WIDTH="27" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img118.gif"
+ ALT="$\Delta\alpha$">,        the errors resulting from this simplification are less than
+        1&nbsp;milliarcsecond in position and 1&nbsp;milliarcsecond per
+        century in proper motion.
+  <DT>4.
+<DD>See also sla_FK45Z, sla_FK524, sla_FK54Z.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Smith, C.A. <I>et al.</I>, 1989.  <I>Astr.J.</I> <B>97</B>, 265.
+<DT>2.
+<DD>Yallop, B.D. <I>et al.</I>, 1989. <I>Astr.J.</I> <B>97</B>, 274.
+<DT>3.
+<DD>Seidelmann, P.K. (ed), 1992.  <I>Explanatory
+        Supplement to the Astronomical Almanac,</I> ISBN&nbsp;0-935702-68-7.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1466" HREF="node105.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1467" HREF="node105.html">SLA_FK45Z - FK4 to FK5, no P.M. or Parallax</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1465" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1459" HREF="node103.html">SLA_FITXY - Fit Linear Model to Two Sets</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node105.html b/src/slalib/sun67.htx/node105.html
new file mode 100644
index 0000000..dde5fc9
--- /dev/null
+++ b/src/slalib/sun67.htx/node105.html
@@ -0,0 +1,166 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_FK45Z - FK4 to FK5, no P.M. or Parallax</TITLE>
+<META NAME="description" CONTENT="SLA_FK45Z - FK4 to FK5, no P.M. or Parallax">
+<META NAME="keywords" CONTENT="sun67">
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+<B> Next:</B> <A NAME="tex2html1477" HREF="node106.html">SLA_FK524 - FK5 to FK4</A>
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+<B>Up:</B> <A NAME="tex2html1475" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1469" HREF="node104.html">SLA_FK425 - FK4 to FK5</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000492000000000000000">SLA_FK45Z - FK4 to FK5, no P.M. or Parallax</A>
+<A NAME="xref_SLA_FK45Z">&#160;</A><A NAME="SLA_FK45Z">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Convert B1950.0 FK4 star data to J2000.0 FK5 assuming zero
+proper motion in the FK5 frame.
+         This routine converts stars from the old, Bessel-Newcomb, FK4
+         system to the new, IAU&nbsp;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&nbsp;2 of
+         reference&nbsp;1, but using the constants of reference&nbsp;4.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_FK45Z (R1950,D1950,BEPOCH,R2000,D2000)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>R1950</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>B1950.0 FK4 <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> at epoch BEPOCH (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>D1950</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>B1950.0 FK4 <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$"> at epoch BEPOCH (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>BEPOCH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>Besselian epoch (<I>e.g.</I> 1979.3D0)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>R2000</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 FK5 <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>D2000</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 FK5 <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$"> (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The epoch BEPOCH is strictly speaking Besselian, but
+if a Julian epoch is supplied the result will be
+affected only to a negligible extent.
+  <DT>2.
+<DD>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 FK45Z is called.
+  <DT>3.
+<DD>In the FK4 catalogue the proper motions of stars within
+        <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img117.gif"
+ ALT="$10^{\circ}$"> of the poles do not include the <I>differential
+        E-terms</I> 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 <IMG WIDTH="27" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img118.gif"
+ ALT="$\Delta\alpha$">,        the errors resulting from this simplification are less than
+        1&nbsp;milliarcsecond in position and 1&nbsp;milliarcsecond per
+        century in proper motion.
+  <DT>4.
+<DD>See also sla_FK425, sla_FK524, sla_FK54Z.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Aoki, S., <I>et al.</I>, 1983. <I>Astr.Astrophys.</I>, <B>128</B>, 263.
+<DT>2.
+<DD>Smith, C.A. <I>et al.</I>, 1989.  <I>Astr.J.</I> <B>97</B>, 265.
+<DT>3.
+<DD>Yallop, B.D. <I>et al.</I>, 1989. <I>Astr.J.</I> <B>97</B>, 274.
+  <DT>4.
+<DD>Seidelmann, P.K. (ed), 1992.  <I>Explanatory
+        Supplement to the Astronomical Almanac,</I> ISBN&nbsp;0-935702-68-7.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1476" HREF="node106.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1474" HREF="node13.html">
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+<A NAME="tex2html1468" HREF="node104.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1477" HREF="node106.html">SLA_FK524 - FK5 to FK4</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1475" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1469" HREF="node104.html">SLA_FK425 - FK4 to FK5</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node106.html b/src/slalib/sun67.htx/node106.html
new file mode 100644
index 0000000..8c1e64a
--- /dev/null
+++ b/src/slalib/sun67.htx/node106.html
@@ -0,0 +1,207 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_FK524 - FK5 to FK4</TITLE>
+<META NAME="description" CONTENT="SLA_FK524 - FK5 to FK4">
+<META NAME="keywords" CONTENT="sun67">
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+<BR>
+<B> Next:</B> <A NAME="tex2html1487" HREF="node107.html">SLA_FK52H - FK5 to Hipparcos</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1485" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1479" HREF="node105.html">SLA_FK45Z - FK4 to FK5, no P.M. or Parallax</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000493000000000000000">SLA_FK524 - FK5 to FK4</A>
+<A NAME="xref_SLA_FK524">&#160;</A><A NAME="SLA_FK524">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Convert J2000.0 FK5 star data to B1950.0 FK4.
+This routine converts stars from the new, IAU&nbsp;1976, FK5, Fricke
+         system, to the old, Bessel-Newcomb, FK4 system.
+         The precepts of Smith&nbsp;<I>et&nbsp;al.</I> (reference&nbsp;1) are followed,
+         using the implementation by Yallop&nbsp;<I>et&nbsp;al.</I> (reference&nbsp;2)
+         of a matrix method due to Standish.  Kinoshita's development of
+         Andoyer's post-Newcomb precession is used.  The numerical
+         constants from Seidelmann&nbsp;<I>et&nbsp;al.</I> (reference&nbsp;3) are
+         used canonically.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_FK524 (
+         R2000,D2000,DR2000,DD2000,P2000,V2000,
+         R1950,D1950,DR1950,DD1950,P1950,V1950)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>R2000</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>D2000</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DR2000</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 proper motion in <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$">(radians per Julian year)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DD2000</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 proper motion in <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$">(radians per Julian year)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>P2000</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 parallax (arcsec)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V2000</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>J2000 radial velocity (km&nbsp;s<SUP>-1</SUP>, +ve = moving away)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>R1950</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>B1950.0 <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>D1950</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>B1950.0 <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DR1950</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>B1950.0 proper motion in <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$">(radians per tropical year)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DD1950</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>B1950.0 proper motion in <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$">(radians per tropical year)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>P1950</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>B1950.0 parallax (arcsec)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V1950</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>radial velocity (km&nbsp;s<SUP>-1</SUP>, +ve = moving away)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> proper motions are <IMG WIDTH="13" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img115.gif"
+ ALT="$\dot{\alpha}$"> rather than
+<IMG WIDTH="48" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img116.gif"
+ ALT="$\dot{\alpha}\cos\delta$">, and are per year rather than per century.
+<DT>2.
+<DD>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.
+  <DT>3.
+<DD>In the FK4 catalogue the proper motions of stars within
+        <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img117.gif"
+ ALT="$10^{\circ}$"> of the poles do not include the <I>differential
+        E-terms</I> 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 <IMG WIDTH="27" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img118.gif"
+ ALT="$\Delta\alpha$">,        the errors resulting from this simplification are less than
+        1&nbsp;milliarcsecond in position and 1&nbsp;milliarcsecond per
+        century in proper motion.
+  <DT>4.
+<DD>See also sla_FK425, sla_FK45Z, sla_FK54Z.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Smith, C.A. <I>et al.</I>, 1989.  <I>Astr.J.</I> <B>97</B>, 265.
+<DT>2.
+<DD>Yallop, B.D. <I>et al.</I>, 1989. <I>Astr.J.</I> <B>97</B>, 274.
+<DT>3.
+<DD>Seidelmann, P.K. (ed), 1992.  <I>Explanatory
+        Supplement to the Astronomical Almanac,</I> ISBN&nbsp;0-935702-68-7.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1486" HREF="node107.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1484" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1478" HREF="node105.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1487" HREF="node107.html">SLA_FK52H - FK5 to Hipparcos</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1485" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1479" HREF="node105.html">SLA_FK45Z - FK4 to FK5, no P.M. or Parallax</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node107.html b/src/slalib/sun67.htx/node107.html
new file mode 100644
index 0000000..e63af95
--- /dev/null
+++ b/src/slalib/sun67.htx/node107.html
@@ -0,0 +1,188 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_FK52H - FK5 to Hipparcos</TITLE>
+<META NAME="description" CONTENT="SLA_FK52H - FK5 to Hipparcos">
+<META NAME="keywords" CONTENT="sun67">
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+<META NAME="distribution" CONTENT="global">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1497" HREF="node108.html">SLA_FK54Z - FK5 to FK4, no P.M. or Parallax</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1495" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1489" HREF="node106.html">SLA_FK524 - FK5 to FK4</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000494000000000000000">SLA_FK52H - FK5 to Hipparcos</A>
+<A NAME="xref_SLA_FK52H">&#160;</A><A NAME="SLA_FK52H">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Transform an FK5 (J2000) position and proper motion
+into the frame of the Hipparcos catalogue.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_FK52H (R5,D5,DR5,DD5,RH,DH,DRH,DDH)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>R5</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 FK5 <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>D5</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 FK5 <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DR5</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 FK5 proper motion in <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$">(radians per Julian year)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DD5</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 FK5 proper motion in <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$">(radians per Julian year)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RH</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>Hipparcos <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>Hipparcos <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DRH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>Hipparcos proper motion in <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$">(radians per Julian year)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DDH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>Hipparcos proper motion in <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$">(radians per Julian year)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> proper motions are <IMG WIDTH="13" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img115.gif"
+ ALT="$\dot{\alpha}$"> rather than
+<IMG WIDTH="48" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img116.gif"
+ ALT="$\dot{\alpha}\cos\delta$">, and are per year rather than per century.
+<DT>2.
+<DD>The FK5 to Hipparcos
+        transformation consists of a pure rotation and spin;
+        zonal errors in the FK5 catalogue are not taken into account.
+  <DT>3.
+<DD>The adopted epoch J2000.0 FK5 to Hipparcos orientation and spin
+        values are as follows (see reference):
+<P>        <BR>
+<BR>
+<BR>
+<P>        &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;
+        <TABLE CELLPADDING=3 BORDER="1">
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>&nbsp;</TD>
+<TH ALIGN="CENTER" NOWRAP COLSPAN=1><I>orientation</I></TH>
+<TH ALIGN="CENTER" NOWRAP COLSPAN=1><I>&nbsp;&nbsp;&nbsp;spin&nbsp;&nbsp;&nbsp;</I></TH>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP><I>x</I></TD>
+<TD ALIGN="RIGHT" NOWRAP>-19.9&nbsp;&nbsp;&nbsp;&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP>&nbsp;-0.30&nbsp;&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP><I>y</I></TD>
+<TD ALIGN="RIGHT" NOWRAP>-9.1&nbsp;&nbsp;&nbsp;&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP>&nbsp;+0.60&nbsp;&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP><I>z</I></TD>
+<TD ALIGN="RIGHT" NOWRAP>+22.9&nbsp;&nbsp;&nbsp;&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP>&nbsp;+0.70&nbsp;&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP><I>mas</I>&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP>&nbsp;<I>mas/y</I>&nbsp;</TD>
+</TR>
+</TABLE>
+<P>        <BR>
+<BR>
+<BR>
+<BR>
+<P>
+These orientation and spin components are interpreted as
+        <I>axial vectors.</I>  An axial vector points at the pole of
+        the rotation and its length is the amount of rotation in radians.
+  <DT>4.
+<DD>See also sla_FK5HZ, sla_H2FK5, sla_HFK5Z.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Feissel, M. &amp; Mignard, F., 1998.,  <I>Astron.Astrophys.</I> <B>331</B>, L33-L36.
+     </DL>
+<BR> <HR>
+<A NAME="tex2html1496" HREF="node108.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1494" HREF="node13.html">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1497" HREF="node108.html">SLA_FK54Z - FK5 to FK4, no P.M. or Parallax</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1495" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1489" HREF="node106.html">SLA_FK524 - FK5 to FK4</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node108.html b/src/slalib/sun67.htx/node108.html
new file mode 100644
index 0000000..504a1a6
--- /dev/null
+++ b/src/slalib/sun67.htx/node108.html
@@ -0,0 +1,156 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_FK54Z - FK5 to FK4, no P.M. or Parallax</TITLE>
+<META NAME="description" CONTENT="SLA_FK54Z - FK5 to FK4, no P.M. or Parallax">
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+<BR>
+<B>Up:</B> <A NAME="tex2html1505" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1499" HREF="node107.html">SLA_FK52H - FK5 to Hipparcos</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000495000000000000000">SLA_FK54Z - FK5 to FK4, no P.M. or Parallax</A>
+<A NAME="xref_SLA_FK54Z">&#160;</A><A NAME="SLA_FK54Z">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Convert a J2000.0 FK5 star position to B1950.0 FK4 assuming
+FK5 zero proper motion and parallax.
+         This routine converts star positions from the new, IAU&nbsp;1976,
+         FK5, Fricke system to the old, Bessel-Newcomb, FK4 system.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_FK54Z (R2000,D2000,BEPOCH,R1950,D1950,DR1950,DD1950)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>R2000</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 FK5 <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>D2000</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 FK5 <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>BEPOCH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>Besselian epoch (<I>e.g.</I> 1950D0)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>R1950</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>B1950.0 FK4 <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> at epoch BEPOCH (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>D1950</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>B1950.0 FK4 <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$"> at epoch BEPOCH (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DR1950</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>B1950.0 FK4 proper motion in <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$">(radians per tropical year)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DD1950</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>B1950.0 FK4 proper motion in <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$">(radians per tropical year)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> proper motions are <IMG WIDTH="13" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img115.gif"
+ ALT="$\dot{\alpha}$"> rather than
+<IMG WIDTH="48" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img116.gif"
+ ALT="$\dot{\alpha}\cos\delta$">, and are per year rather than per century.
+<DT>2.
+<DD>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 routines before and
+        after this routine is called.
+  <DT>3.
+<DD>Unlike in the sla_FK524 routine, the FK5 proper motions, the
+        parallax and the radial velocity are presumed zero.
+  <DT>4.
+<DD>It was 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 routine returns those <I>fictitious proper
+        motions</I>.
+  <DT>5.
+<DD>The position returned by this routine is in the B1950
+        reference frame but at Besselian epoch BEPOCH.  For
+        comparison with catalogues the BEPOCH argument will
+        frequently be 1950D0.
+  <DT>6.
+<DD>See also sla_FK425, sla_FK45Z, sla_FK524.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1506" HREF="node109.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1507" HREF="node109.html">SLA_FK5HZ - FK5 to Hipparcos, no P.M.</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1505" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1499" HREF="node107.html">SLA_FK52H - FK5 to Hipparcos</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node109.html b/src/slalib/sun67.htx/node109.html
new file mode 100644
index 0000000..ddda44d
--- /dev/null
+++ b/src/slalib/sun67.htx/node109.html
@@ -0,0 +1,168 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_FK5HZ - FK5 to Hipparcos, no P.M.</TITLE>
+<META NAME="description" CONTENT="SLA_FK5HZ - FK5 to Hipparcos, no P.M.">
+<META NAME="keywords" CONTENT="sun67">
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+<BODY >
+<BR> <HR>
+<A NAME="tex2html1516" HREF="node110.html">
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+<A NAME="tex2html1514" HREF="node13.html">
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+<A NAME="tex2html1508" HREF="node108.html">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1517" HREF="node110.html">SLA_FLOTIN - Decode a Real Number</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1515" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1509" HREF="node108.html">SLA_FK54Z - FK5 to FK4, no P.M. or Parallax</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000496000000000000000">SLA_FK5HZ - FK5 to Hipparcos, no P.M.</A>
+<A NAME="xref_SLA_FK5HZ">&#160;</A><A NAME="SLA_FK5HZ">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Transform an FK5 (J2000) star position into the frame of the
+Hipparcos catalogue, assuming zero Hipparcos proper motion.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_FK52H (R5,D5,EPOCH,RH,DH)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>R5</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 FK5 <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>D5</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 FK5 <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EPOCH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>Julian epoch (TDB)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RH</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>Hipparcos <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>Hipparcos <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$"> (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> proper motions are <IMG WIDTH="13" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img115.gif"
+ ALT="$\dot{\alpha}$"> rather than
+<IMG WIDTH="48" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img116.gif"
+ ALT="$\dot{\alpha}\cos\delta$">, and are per year rather than per century.
+<DT>2.
+<DD>The FK5 to Hipparcos
+        transformation consists of a pure rotation and spin;
+        zonal errors in the FK5 catalogue are not taken into account.
+  <DT>3.
+<DD>The adopted epoch J2000.0 FK5 to Hipparcos orientation and spin
+        values are as follows (see reference):
+<P>        <BR>
+<BR>
+<BR>
+<P>        &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;
+        <TABLE CELLPADDING=3 BORDER="1">
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>&nbsp;</TD>
+<TH ALIGN="CENTER" NOWRAP COLSPAN=1><I>orientation</I></TH>
+<TH ALIGN="CENTER" NOWRAP COLSPAN=1><I>&nbsp;&nbsp;&nbsp;spin&nbsp;&nbsp;&nbsp;</I></TH>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP><I>x</I></TD>
+<TD ALIGN="RIGHT" NOWRAP>-19.9&nbsp;&nbsp;&nbsp;&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP>&nbsp;-0.30&nbsp;&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP><I>y</I></TD>
+<TD ALIGN="RIGHT" NOWRAP>-9.1&nbsp;&nbsp;&nbsp;&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP>&nbsp;+0.60&nbsp;&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP><I>z</I></TD>
+<TD ALIGN="RIGHT" NOWRAP>+22.9&nbsp;&nbsp;&nbsp;&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP>&nbsp;+0.70&nbsp;&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP><I>mas</I>&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP>&nbsp;<I>mas/y</I>&nbsp;</TD>
+</TR>
+</TABLE>
+<P>        <BR>
+<BR>
+<BR>
+<BR>
+<P>
+These orientation and spin components are interpreted as
+        <I>axial vectors.</I>  An axial vector points at the pole of
+        the rotation and its length is the amount of rotation in radians.
+  <DT>4.
+<DD>See also sla_FK52H, sla_H2FK5, sla_HFK5Z.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Feissel, M. &amp; Mignard, F., 1998.,  <I>Astron.Astrophys.</I> <B>331</B>, L33-L36.
+     </DL>
+<BR> <HR>
+<A NAME="tex2html1516" HREF="node110.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1517" HREF="node110.html">SLA_FLOTIN - Decode a Real Number</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1515" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1509" HREF="node108.html">SLA_FK54Z - FK5 to FK4, no P.M. or Parallax</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node11.html b/src/slalib/sun67.htx/node11.html
new file mode 100644
index 0000000..a950b04
--- /dev/null
+++ b/src/slalib/sun67.htx/node11.html
@@ -0,0 +1,102 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Acknowledgements</TITLE>
+<META NAME="description" CONTENT="Acknowledgements">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="previous" HREF="node10.html">
+<LINK REL="up" HREF="node2.html">
+<LINK REL="next" HREF="node12.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html353" HREF="node12.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html351" HREF="node2.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html347" HREF="node10.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html354" HREF="node12.html">LINKING</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html352" HREF="node2.html">INTRODUCTION</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html348" HREF="node10.html">New Functions</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION00029000000000000000">
+Acknowledgements</A>
+</H2>
+SLALIB is descended from a package of routines written
+for the AAO 16-bit minicomputers
+in the mid-1970s.  The coming of the VAX
+allowed a much more comprehensive and thorough package
+to be designed for Starlink, especially important
+at a time when the adoption
+of the IAU 1976 resolutions meant that astronomers
+would have to cope with a mixture of reference frames,
+timescales and nomenclature.
+<P>
+Much of the preparatory work on SLALIB was done by
+Althea&nbsp;Wilkinson of Manchester University.
+During its development,
+Andrew&nbsp;Murray,
+Catherine&nbsp;Hohenkerk,
+Andrew&nbsp;Sinclair,
+Bernard&nbsp;Yallop
+and
+Brian&nbsp;Emerson of Her Majesty's Nautical Almanac Office were consulted
+on many occasions; their advice was indispensable.
+I am especially grateful to
+Catherine&nbsp;Hohenkerk
+for supplying preprints of papers, and test data. A number of
+enhancements to SLALIB were at the suggestion of
+Russell&nbsp;Owen, University of Washington,
+the late Phil&nbsp;Hill, St&nbsp;Andrews University,
+Bill&nbsp;Vacca, JILA, Boulder and
+Ron&nbsp;Maddalena, NRAO.
+Mark&nbsp;Calabretta, CSIRO Radiophysics, Sydney supplied changes to suit Convex.
+I am indebted to Derek&nbsp;Jones (RGO) for introducing me to the
+``universal variables'' method of calculating orbits.
+<P>
+The first C version of SLALIB was a hand-coded transcription
+of the Starlink Fortran version carried out by
+Steve&nbsp;Eaton (University of Leeds) in the course of
+MSc work.  This was later
+enhanced by John&nbsp;Straede (AAO) and Martin&nbsp;Shepherd (Caltech).
+The current C SLALIB is a complete rewrite by the present author and
+includes a comprehensive validation suite.
+Additional comments on the C version came from Bob&nbsp;Payne (NRAO) and
+Jeremy&nbsp;Bailey (AAO).
+<P>
+<BR> <HR>
+<A NAME="tex2html353" HREF="node12.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html351" HREF="node2.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html347" HREF="node10.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html354" HREF="node12.html">LINKING</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html352" HREF="node2.html">INTRODUCTION</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html348" HREF="node10.html">New Functions</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node110.html b/src/slalib/sun67.htx/node110.html
new file mode 100644
index 0000000..c13c949
--- /dev/null
+++ b/src/slalib/sun67.htx/node110.html
@@ -0,0 +1,200 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_FLOTIN - Decode a Real Number</TITLE>
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+<BR>
+<B> Next:</B> <A NAME="tex2html1527" HREF="node111.html">SLA_GALEQ - Galactic to J2000</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1525" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1519" HREF="node109.html">SLA_FK5HZ - FK5 to Hipparcos, no P.M.</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000497000000000000000">SLA_FLOTIN - Decode a Real Number</A>
+<A NAME="xref_SLA_FLOTIN">&#160;</A><A NAME="SLA_FLOTIN">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Convert free-format input into single precision floating point.
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_FLOTIN (STRING, NSTRT, RESLT, JFLAG)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>STRING</EM></TD>
+<TH ALIGN="LEFT"><B>C</B></TH>
+<TD ALIGN="LEFT" NOWRAP>string containing number to be decoded</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NSTRT</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>pointer to where decoding is to commence</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RESLT</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>current value of result</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NSTRT</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>advanced to next number</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RESLT</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>result</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JFLAG</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status: -1&nbsp;=&nbsp;-OK, 0&nbsp;=&nbsp;+OK, 1&nbsp;=&nbsp;null result, 2&nbsp;=&nbsp;error</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The reason sla_FLOTIN has separate `OK' status values
+for + and - is to enable minus zero to be detected.
+This is of crucial importance
+       when decoding mixed-radix numbers.  For example, an angle
+       expressed as degrees, arcminutes and arcseconds may have a
+       leading minus sign but a zero degrees field.
+ <DT>2.
+<DD>A TAB is interpreted as a space, and lowercase characters are
+       interpreted as uppercase.  <I>n.b.</I> The test for TAB is
+       ASCII-specific.
+ <DT>3.
+<DD>The basic format is the sequence of fields <IMG WIDTH="78" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img68.gif"
+ ALT="$\pm n.n x \pm n$">,       where <IMG WIDTH="15" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img30.gif"
+ ALT="$\pm$"> is a sign
+       character `+' or `-', <I>n</I> means a string of decimal digits,
+       `.' is a decimal point, and <I>x</I>, which indicates an exponent,
+       means `D' or `E'.  Various combinations of these fields can be
+       omitted, and embedded blanks are permissible in certain places.
+ <DT>4.
+<DD>Spaces:
+       <UL>
+<LI> Leading spaces are ignored.
+<LI> Embedded spaces are allowed only after +, -, D or E,
+             and after the decimal point if the first sequence of
+             digits is absent.
+<LI> Trailing spaces are ignored;  the first signifies
+             end of decoding and subsequent ones are skipped.
+       </UL>
+ <DT>5.
+<DD>Delimiters:
+       <UL>
+<LI> Any character other than +,-,0-9,.,D,E or space may be
+             used to signal the end of the number and terminate decoding.
+<LI> Comma is recognized by sla_FLOTIN as a special case; it
+             is skipped, leaving the pointer on the next character.  See
+             13, below.
+<LI> Decoding will in all cases terminate if end of string
+             is reached.
+       </UL>
+ <DT>6.
+<DD>Both signs are optional.  The default is +.
+ <DT>7.
+<DD>The mantissa <I>n</I>.<I>n</I> defaults to unity.
+ <DT>8.
+<DD>The exponent <IMG WIDTH="36" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img69.gif"
+ ALT="$x\!\pm\!n$"> defaults to `E0'.
+ <DT>9.
+<DD>The strings of decimal digits may be of any length.
+ <DT>10.
+<DD>The decimal point is optional for whole numbers.
+ <DT>11.
+<DD>A <I>null result</I> occurs when the string of characters
+       being decoded does not begin with +,-,0-9,.,D or E, or
+       consists entirely of spaces.  When this condition is
+       detected, JFLAG is set to 1 and RESLT is left untouched.
+ <DT>12.
+<DD>NSTRT = 1 for the first character in the string.
+ <DT>13.
+<DD>On return from sla_FLOTIN, NSTRT is set ready for the next
+       decode - following trailing blanks and any comma.  If a
+       delimiter other than comma is being used, NSTRT must be
+       incremented before the next call to sla_FLOTIN, otherwise
+       all subsequent calls will return a null result.
+ <DT>14.
+<DD>Errors (JFLAG=2) occur when:
+       <UL>
+<LI> a +, -, D or E is left unsatisfied; or
+<LI> the decimal point is present without at least
+             one decimal digit before or after it; or
+<LI> an exponent more than 100 has been presented.
+       </UL>
+ <DT>15.
+<DD>When an error has been detected, NSTRT is left
+       pointing to the character following the last
+       one used before the error came to light.  This
+       may be after the point at which a more sophisticated
+       program could have detected the error.  For example,
+       sla_FLOTIN does not detect that `1E999' is unacceptable
+       (on a computer where this is so)
+       until the entire number has been decoded.
+ <DT>16.
+<DD>Certain highly unlikely combinations of mantissa and
+       exponent can cause arithmetic faults during the
+       decode, in some cases despite the fact that they
+       together could be construed as a valid number.
+ <DT>17.
+<DD>Decoding is left to right, one pass.
+ <DT>18.
+<DD>See also sla_DFLTIN and sla_INTIN.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1526" HREF="node111.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1527" HREF="node111.html">SLA_GALEQ - Galactic to J2000</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1525" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1519" HREF="node109.html">SLA_FK5HZ - FK5 to Hipparcos, no P.M.</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node111.html b/src/slalib/sun67.htx/node111.html
new file mode 100644
index 0000000..6e7927c
--- /dev/null
+++ b/src/slalib/sun67.htx/node111.html
@@ -0,0 +1,104 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_GALEQ - Galactic to J2000 </TITLE>
+<META NAME="description" CONTENT="SLA_GALEQ - Galactic to J2000 ">
+<META NAME="keywords" CONTENT="sun67">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1537" HREF="node112.html">SLA_GALSUP - Galactic to Supergalactic</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1535" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1529" HREF="node110.html">SLA_FLOTIN - Decode a Real Number</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000498000000000000000">&#160;</A><A NAME="xref_SLA_GALEQ">&#160;</A><A NAME="SLA_GALEQ">&#160;</A>
+<BR>
+SLA_GALEQ - Galactic to J2000 <IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img91.gif"
+ ALT="$\alpha,\delta$"></H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Transformation from IAU 1958 galactic coordinates
+to J2000.0 FK5 equatorial coordinates.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_GALEQ (DL, DB, DR, DD)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DL,DB</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>galactic longitude and latitude <IMG WIDTH="59" HEIGHT="32" ALIGN="MIDDLE" BORDER="0"
+ SRC="img98.gif"
+ ALT="$[\,l^{I\!I},b^{I\!I}\,]$"></TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DR,DD</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"></TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>All arguments are in radians.
+<DT>2.
+<DD>The equatorial coordinates are J2000.0 FK5.  Use the routine
+sla_GE50 if conversion to B1950.0 FK4 coordinates is
+                           required.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1536" HREF="node112.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1537" HREF="node112.html">SLA_GALSUP - Galactic to Supergalactic</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1535" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1529" HREF="node110.html">SLA_FLOTIN - Decode a Real Number</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node112.html b/src/slalib/sun67.htx/node112.html
new file mode 100644
index 0000000..cfbdd9b
--- /dev/null
+++ b/src/slalib/sun67.htx/node112.html
@@ -0,0 +1,107 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_GALSUP - Galactic to Supergalactic</TITLE>
+<META NAME="description" CONTENT="SLA_GALSUP - Galactic to Supergalactic">
+<META NAME="keywords" CONTENT="sun67">
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+</HEAD>
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+<BR> <HR>
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+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1544" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1538" HREF="node111.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1547" HREF="node113.html">SLA_GE50 - Galactic to B1950</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1545" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1539" HREF="node111.html">SLA_GALEQ - Galactic to J2000</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000499000000000000000">SLA_GALSUP - Galactic to Supergalactic</A>
+<A NAME="xref_SLA_GALSUP">&#160;</A><A NAME="SLA_GALSUP">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Transformation from IAU 1958 galactic coordinates to
+de Vaucouleurs supergalactic coordinates.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_GALSUP (DL, DB, DSL, DSB)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DL,DB</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>galactic longitude and latitude <IMG WIDTH="59" HEIGHT="32" ALIGN="MIDDLE" BORDER="0"
+ SRC="img98.gif"
+ ALT="$[\,l^{I\!I},b^{I\!I}\,]$"> (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DSL,DSB</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>supergalactic longitude and latitude (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>de Vaucouleurs, de Vaucouleurs, &amp; Corwin, <I>Second Reference
+Catalogue of Bright Galaxies</I>, U.Texas, p8.
+<DT>2.
+<DD>Systems &amp; Applied Sciences Corp., documentation for the
+        machine-readable version of the above catalogue,
+        Contract NAS 5-26490.
+ </DL>
+ (These two references give different values for the galactic
+ longitude of the supergalactic origin.  Both are wrong;  the
+ correct value is <IMG WIDTH="86" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img119.gif"
+ ALT="$l^{I\!I}=137.37$">.)
+<P>     </DL>
+<BR> <HR>
+<A NAME="tex2html1546" HREF="node113.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1544" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1538" HREF="node111.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1547" HREF="node113.html">SLA_GE50 - Galactic to B1950</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1545" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1539" HREF="node111.html">SLA_GALEQ - Galactic to J2000</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node113.html b/src/slalib/sun67.htx/node113.html
new file mode 100644
index 0000000..e12bf51
--- /dev/null
+++ b/src/slalib/sun67.htx/node113.html
@@ -0,0 +1,109 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_GE50 - Galactic to B1950 </TITLE>
+<META NAME="description" CONTENT="SLA_GE50 - Galactic to B1950 ">
+<META NAME="keywords" CONTENT="sun67">
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+<BR> <HR>
+<A NAME="tex2html1556" HREF="node114.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1554" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1548" HREF="node112.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1557" HREF="node114.html">SLA_GEOC - Geodetic to Geocentric</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1555" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1549" HREF="node112.html">SLA_GALSUP - Galactic to Supergalactic</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004100000000000000000">&#160;</A><A NAME="xref_SLA_GE50">&#160;</A><A NAME="SLA_GE50">&#160;</A>
+<BR>
+SLA_GE50 - Galactic to B1950 <IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img91.gif"
+ ALT="$\alpha,\delta$"></H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Transformation from IAU 1958 galactic coordinates to
+B1950.0 FK4 equatorial coordinates.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_GE50 (DL, DB, DR, DD)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DL,DB</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>galactic longitude and latitude <IMG WIDTH="59" HEIGHT="32" ALIGN="MIDDLE" BORDER="0"
+ SRC="img98.gif"
+ ALT="$[\,l^{I\!I},b^{I\!I}\,]$"></TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DR,DD</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>B1950.0 <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"></TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>All arguments are in radians.
+<DT>2.
+<DD>The equatorial coordinates are B1950.0 FK4.  Use the
+routine sla_GALEQ if conversion to J2000.0 FK5 coordinates
+        is required.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Blaauw <I>et al.</I>, 1960, <I>Mon.Not.R.astr.Soc.</I>,
+<B>121</B>, 123.
+     </DL>
+<BR> <HR>
+<A NAME="tex2html1556" HREF="node114.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1554" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1548" HREF="node112.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1557" HREF="node114.html">SLA_GEOC - Geodetic to Geocentric</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1555" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1549" HREF="node112.html">SLA_GALSUP - Galactic to Supergalactic</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node114.html b/src/slalib/sun67.htx/node114.html
new file mode 100644
index 0000000..a2e570a
--- /dev/null
+++ b/src/slalib/sun67.htx/node114.html
@@ -0,0 +1,107 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_GEOC - Geodetic to Geocentric</TITLE>
+<META NAME="description" CONTENT="SLA_GEOC - Geodetic to Geocentric">
+<META NAME="keywords" CONTENT="sun67">
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+<A NAME="tex2html1564" HREF="node13.html">
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+<A NAME="tex2html1558" HREF="node113.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1567" HREF="node115.html">SLA_GMST - UT to GMST</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1565" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1559" HREF="node113.html">SLA_GE50 - Galactic to B1950</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004101000000000000000">SLA_GEOC - Geodetic to Geocentric</A>
+<A NAME="xref_SLA_GEOC">&#160;</A><A NAME="SLA_GEOC">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Convert geodetic position to geocentric.
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_GEOC (P, H, R, Z)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>P</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>latitude (geodetic, radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>H</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>height above reference spheroid (geodetic, metres)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>R</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>distance from Earth axis (AU)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>Z</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>distance from plane of Earth equator (AU)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Geocentric latitude can be obtained by evaluating <TT>ATAN2(Z,R)</TT>.
+<DT>2.
+<DD>IAU 1976 constants are used.
+</DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Green, R.M., 1985. <I>Spherical Astronomy</I>, Cambridge U.P., p98.
+</DL>
+<BR> <HR>
+<A NAME="tex2html1566" HREF="node115.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1564" HREF="node13.html">
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+<A NAME="tex2html1558" HREF="node113.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1567" HREF="node115.html">SLA_GMST - UT to GMST</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1565" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1559" HREF="node113.html">SLA_GE50 - Galactic to B1950</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node115.html b/src/slalib/sun67.htx/node115.html
new file mode 100644
index 0000000..cee01cc
--- /dev/null
+++ b/src/slalib/sun67.htx/node115.html
@@ -0,0 +1,115 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_GMST - UT to GMST</TITLE>
+<META NAME="description" CONTENT="SLA_GMST - UT to GMST">
+<META NAME="keywords" CONTENT="sun67">
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+<A NAME="tex2html1574" HREF="node13.html">
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+<A NAME="tex2html1568" HREF="node114.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1577" HREF="node116.html">SLA_GMSTA - UT to GMST (extra precision)</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1575" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1569" HREF="node114.html">SLA_GEOC - Geodetic to Geocentric</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004102000000000000000">SLA_GMST - UT to GMST</A>
+<A NAME="xref_SLA_GMST">&#160;</A><A NAME="SLA_GMST">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Conversion from universal time UT1 to Greenwich mean
+sidereal time.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>D&nbsp;=&nbsp;sla_GMST (UT1)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>UT1</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>universal time (strictly UT1) expressed as
+modified Julian Date (JD-2400000.5)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_GMST</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>Greenwich mean sidereal time (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The IAU&nbsp;1982 expression
+(see page&nbsp;S15 of the 1984 <I>Astronomical
+Almanac</I>) is used, but rearranged to reduce rounding errors.  This
+       expression is always described as giving the GMST at <IMG WIDTH="18" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img49.gif"
+ ALT="$0^{\rm h}$">UT;
+       in fact, it gives the difference between the
+       GMST and the UT, which happens to equal the GMST (modulo
+       24&nbsp;hours) at <IMG WIDTH="18" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img49.gif"
+ ALT="$0^{\rm h}$">UT each day.  In sla_GMST, the
+       entire UT is used directly as the argument for the
+       canonical formula, and the fractional part of the UT is
+       added separately;  note that the factor <IMG WIDTH="94" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img120.gif"
+ ALT="$1.0027379\cdots$"> does
+       not appear.
+       <DT>2.
+<DD>See also the routine sla_GMSTA, which
+       delivers better numerical
+       precision by accepting the UT date and time as separate arguments.
+  </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1576" HREF="node116.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1574" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1568" HREF="node114.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1577" HREF="node116.html">SLA_GMSTA - UT to GMST (extra precision)</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1575" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1569" HREF="node114.html">SLA_GEOC - Geodetic to Geocentric</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node116.html b/src/slalib/sun67.htx/node116.html
new file mode 100644
index 0000000..5055ecb
--- /dev/null
+++ b/src/slalib/sun67.htx/node116.html
@@ -0,0 +1,116 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_GMSTA - UT to GMST (extra precision)</TITLE>
+<META NAME="description" CONTENT="SLA_GMSTA - UT to GMST (extra precision)">
+<META NAME="keywords" CONTENT="sun67">
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+<A NAME="tex2html1578" HREF="node115.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1587" HREF="node117.html">SLA_GRESID - Gaussian Residual</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1585" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1579" HREF="node115.html">SLA_GMST - UT to GMST</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004103000000000000000">SLA_GMSTA - UT to GMST (extra precision)</A>
+<A NAME="xref_SLA_GMSTA">&#160;</A><A NAME="SLA_GMSTA">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Conversion from universal time UT1 to Greenwich Mean
+sidereal time, with rounding errors minimized.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>D&nbsp;=&nbsp;sla_GMSTA (DATE, UT1)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>UT1 date as Modified Julian Date (integer part
+of JD-2400000.5)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>UT1</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>UT1 time (fraction of a day)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_GMST</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>Greenwich mean sidereal time (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The algorithm is derived from the IAU 1982 expression
+(see page&nbsp;S15 of the 1984 Astronomical Almanac).
+<DT>2.
+<DD>There is no restriction on how the UT is apportioned between the
+       DATE and UT1 arguments.  Either of the two arguments could, for
+       example, be zero and the entire date+time supplied in the other.
+       However, the routine is designed to deliver maximum accuracy when
+       the DATE argument is a whole number and the UT1 argument
+       lies in the range <IMG WIDTH="43" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img121.gif"
+ ALT="$[\,0,\,1\,]$">, or <I>vice versa</I>.
+       <DT>3.
+<DD>See also the routine sla_GMST, which accepts the UT1 as a single
+       argument.  Compared with sla_GMST, the extra numerical precision
+       delivered by the present routine is unlikely to be important in
+       an absolute sense, but may be useful when critically comparing
+       algorithms and in applications where two sidereal times close
+       together are differenced.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1586" HREF="node117.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1584" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1578" HREF="node115.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1587" HREF="node117.html">SLA_GRESID - Gaussian Residual</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1585" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1579" HREF="node115.html">SLA_GMST - UT to GMST</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node117.html b/src/slalib/sun67.htx/node117.html
new file mode 100644
index 0000000..980f93a
--- /dev/null
+++ b/src/slalib/sun67.htx/node117.html
@@ -0,0 +1,92 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_GRESID - Gaussian Residual</TITLE>
+<META NAME="description" CONTENT="SLA_GRESID - Gaussian Residual">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
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+<A NAME="tex2html1588" HREF="node116.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1597" HREF="node118.html">SLA_H2E - Az,El to</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1595" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1589" HREF="node116.html">SLA_GMSTA - UT to GMST (extra precision)</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004104000000000000000">SLA_GRESID - Gaussian Residual</A>
+<A NAME="xref_SLA_GRESID">&#160;</A><A NAME="SLA_GRESID">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Generate pseudo-random normal deviate or <I>Gaussian residual</I>.
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>R&nbsp;=&nbsp;sla_GRESID (S)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>S</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>standard deviation</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The results of many calls to this routine will be
+normally distributed with mean zero and standard deviation S.
+<DT>2.
+<DD>The Box-Muller algorithm is used.
+  <DT>3.
+<DD>The implementation is machine-dependent.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Ahrens &amp; Dieter, 1972. <I>Comm.A.C.M.</I> <B>15</B>, 873.
+</DL>
+<BR> <HR>
+<A NAME="tex2html1596" HREF="node118.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1594" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1588" HREF="node116.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1597" HREF="node118.html">SLA_H2E - Az,El to</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1595" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1589" HREF="node116.html">SLA_GMSTA - UT to GMST (extra precision)</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node118.html b/src/slalib/sun67.htx/node118.html
new file mode 100644
index 0000000..83df4b3
--- /dev/null
+++ b/src/slalib/sun67.htx/node118.html
@@ -0,0 +1,146 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_H2E - Az,El to </TITLE>
+<META NAME="description" CONTENT="SLA_H2E - Az,El to ">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node119.html">
+<LINK REL="previous" HREF="node117.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node119.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1606" HREF="node119.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1604" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1598" HREF="node117.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1607" HREF="node119.html">SLA_H2FK5 - Hipparcos to FK5</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1605" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1599" HREF="node117.html">SLA_GRESID - Gaussian Residual</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004105000000000000000">&#160;</A><A NAME="xref_SLA_H2E">&#160;</A><A NAME="SLA_H2E">&#160;</A>
+<BR>
+SLA_H2E - Az,El to <IMG WIDTH="27" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img65.gif"
+ ALT="$h,\delta$"></H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Horizon to equatorial coordinates
+(single precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_H2E (AZ, EL, PHI, HA, DEC)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AZ</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>azimuth (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EL</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>elevation (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PHI</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>latitude (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>HA</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>hour angle (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DEC</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>declination (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The sign convention for azimuth is north zero, east <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img14.gif"
+ ALT="$+\pi/2$">.<DT>2.
+<DD>HA is returned in the range <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$">.  Declination is returned
+in the range <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$">.  <DT>3.
+<DD>The latitude is (in principle) geodetic.  In critical
+        applications, corrections for polar motion should be applied
+        (see sla_POLMO).
+  <DT>4.
+<DD>In some applications it will be important to specify the
+        correct type of elevation in order to produce the required
+        type of <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$">.  In particular, it may be important to
+        distinguish between the elevation as affected by refraction,
+        which will yield the <I>observed</I> <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$">, and the elevation
+        <I>in vacuo</I>, which will yield the <I>topocentric</I>
+        <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$">.  If the
+        effects of diurnal aberration can be neglected, the
+        topocentric <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$"> may be used as an approximation to the
+        <I>apparent</I> <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$">.  <DT>5.
+<DD>No range checking of arguments is carried out.
+  <DT>6.
+<DD>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.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1606" HREF="node119.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1604" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1598" HREF="node117.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1607" HREF="node119.html">SLA_H2FK5 - Hipparcos to FK5</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1605" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1599" HREF="node117.html">SLA_GRESID - Gaussian Residual</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node119.html b/src/slalib/sun67.htx/node119.html
new file mode 100644
index 0000000..9133db9
--- /dev/null
+++ b/src/slalib/sun67.htx/node119.html
@@ -0,0 +1,188 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_H2FK5 - Hipparcos to FK5</TITLE>
+<META NAME="description" CONTENT="SLA_H2FK5 - Hipparcos to FK5">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
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+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
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+<LINK REL="up" HREF="node13.html">
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+<BR> <HR>
+<A NAME="tex2html1616" HREF="node120.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1614" HREF="node13.html">
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+<A NAME="tex2html1608" HREF="node118.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1617" HREF="node120.html">SLA_HFK5Z - Hipparcos to FK5, no P.M.</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1615" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1609" HREF="node118.html">SLA_H2E - Az,El to</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004106000000000000000">SLA_H2FK5 - Hipparcos to FK5</A>
+<A NAME="xref_SLA_H2FK5">&#160;</A><A NAME="SLA_H2FK5">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Transform a Hipparcos star position and proper motion
+into the FK5 (J2000) frame.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_H2FK5 (RH,DH,DRH,DDH,R5,D5,DR5,DD5)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RH</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>Hipparcos <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>Hipparcos <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DRH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>Hipparcos proper motion in <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$">(radians per Julian year)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DDH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>Hipparcos proper motion in <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$">(radians per Julian year)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>R5</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 FK5 <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>D5</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 FK5 <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DR5</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 FK5 proper motion in <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$">(radians per Julian year)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DD5</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>FK5 J2000.0 proper motion in <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$">(radians per Julian year)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> proper motions are <IMG WIDTH="13" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img115.gif"
+ ALT="$\dot{\alpha}$"> rather than
+<IMG WIDTH="48" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img116.gif"
+ ALT="$\dot{\alpha}\cos\delta$">, and are per year rather than per century.
+<DT>2.
+<DD>The FK5 to Hipparcos
+        transformation consists of a pure rotation and spin;
+        zonal errors in the FK5 catalogue are not taken into account.
+  <DT>3.
+<DD>The adopted epoch J2000.0 FK5 to Hipparcos orientation and spin
+        values are as follows (see reference):
+<P>        <BR>
+<BR>
+<BR>
+<P>        &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;
+        <TABLE CELLPADDING=3 BORDER="1">
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>&nbsp;</TD>
+<TH ALIGN="CENTER" NOWRAP COLSPAN=1><I>orientation</I></TH>
+<TH ALIGN="CENTER" NOWRAP COLSPAN=1><I>&nbsp;&nbsp;&nbsp;spin&nbsp;&nbsp;&nbsp;</I></TH>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP><I>x</I></TD>
+<TD ALIGN="RIGHT" NOWRAP>-19.9&nbsp;&nbsp;&nbsp;&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP>&nbsp;-0.30&nbsp;&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP><I>y</I></TD>
+<TD ALIGN="RIGHT" NOWRAP>-9.1&nbsp;&nbsp;&nbsp;&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP>&nbsp;+0.60&nbsp;&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP><I>z</I></TD>
+<TD ALIGN="RIGHT" NOWRAP>+22.9&nbsp;&nbsp;&nbsp;&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP>&nbsp;+0.70&nbsp;&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP><I>mas</I>&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP>&nbsp;<I>mas/y</I>&nbsp;</TD>
+</TR>
+</TABLE>
+<P>        <BR>
+<BR>
+<BR>
+<BR>
+<P>
+These orientation and spin components are interpreted as
+        <I>axial vectors.</I>  An axial vector points at the pole of
+        the rotation and its length is the amount of rotation in radians.
+  <DT>4.
+<DD>See also sla_FK52H, sla_FK5HZ, sla_HFK5Z.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Feissel, M. &amp; Mignard, F., 1998.,  <I>Astron.Astrophys.</I> <B>331</B>, L33-L36.
+     </DL>
+<BR> <HR>
+<A NAME="tex2html1616" HREF="node120.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1614" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1608" HREF="node118.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1617" HREF="node120.html">SLA_HFK5Z - Hipparcos to FK5, no P.M.</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1615" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1609" HREF="node118.html">SLA_H2E - Az,El to</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node12.html b/src/slalib/sun67.htx/node12.html
new file mode 100644
index 0000000..d75415d
--- /dev/null
+++ b/src/slalib/sun67.htx/node12.html
@@ -0,0 +1,75 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>LINKING</TITLE>
+<META NAME="description" CONTENT="LINKING">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node13.html">
+<LINK REL="previous" HREF="node2.html">
+<LINK REL="up" HREF="sun67.html">
+<LINK REL="next" HREF="node13.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html363" HREF="node13.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html361" HREF="sun67.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html355" HREF="node11.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html364" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html362" HREF="sun67.html">SLALIB   Positional Astronomy Library</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html356" HREF="node11.html">Acknowledgements</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H1><A NAME="SECTION00030000000000000000">
+LINKING</A>
+</H1>
+<P>
+On Unix systems (Sun, DEC Alpha <I>etc.</I>):
+<BLOCKQUOTE><TT>%&nbsp;&nbsp;f77 progname.o -L/star/lib `sla_link` -o progname</TT>
+</BLOCKQUOTE>
+(The above assumes that all Starlink directories have been added to
+the <TT>LD_LIBRARY_PATH</TT> and <TT>PATH</TT> environment variables
+as described in SUN/202.)
+<P>
+On VAX/VMS:
+<BLOCKQUOTE><TT>$&nbsp;&nbsp;LINK progname,SLALIB_DIR:SLALIB/LIB</TT>
+</BLOCKQUOTE>
+<P>
+<BR>
+<P>
+<BR> <HR>
+<A NAME="tex2html363" HREF="node13.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html361" HREF="sun67.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html355" HREF="node11.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html364" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html362" HREF="sun67.html">SLALIB   Positional Astronomy Library</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html356" HREF="node11.html">Acknowledgements</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node120.html b/src/slalib/sun67.htx/node120.html
new file mode 100644
index 0000000..ffd038a
--- /dev/null
+++ b/src/slalib/sun67.htx/node120.html
@@ -0,0 +1,190 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_HFK5Z - Hipparcos to FK5, no P.M.</TITLE>
+<META NAME="description" CONTENT="SLA_HFK5Z - Hipparcos to FK5, no P.M.">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node121.html">
+<LINK REL="previous" HREF="node119.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node121.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1626" HREF="node121.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1624" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1618" HREF="node119.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1627" HREF="node121.html">SLA_IMXV - Apply 3D Reverse Rotation</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1625" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1619" HREF="node119.html">SLA_H2FK5 - Hipparcos to FK5</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004107000000000000000">SLA_HFK5Z - Hipparcos to FK5, no P.M.</A>
+<A NAME="xref_SLA_HFK5Z">&#160;</A><A NAME="SLA_HFK5Z">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Transform a Hipparcos star position
+into the FK5 (J2000) frame assuming zero Hipparcos proper motion.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_HFK5Z (RH,DH,EPOCH,R5,D5,DR5,DD5)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RH</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>Hipparcos <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>Hipparcos <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EPOCH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>Julian epoch (TDB)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>R5</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 FK5 <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>D5</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 FK5 <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DR5</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 FK5 proper motion in <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$">(radians per Julian year)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DD5</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>FK5 J2000.0 proper motion in <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$">(radians per Julian year)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> proper motions are <IMG WIDTH="13" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img115.gif"
+ ALT="$\dot{\alpha}$"> rather than
+<IMG WIDTH="48" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img116.gif"
+ ALT="$\dot{\alpha}\cos\delta$">, and are per year rather than per century.
+<DT>2.
+<DD>The FK5 to Hipparcos
+        transformation consists of a pure rotation and spin;
+        zonal errors in the FK5 catalogue are not taken into account.
+  <DT>3.
+<DD>The adopted epoch J2000.0 FK5 to Hipparcos orientation and spin
+        values are as follows (see reference):
+<P>        <BR>
+<BR>
+<BR>
+<P>        &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;
+        <TABLE CELLPADDING=3 BORDER="1">
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>&nbsp;</TD>
+<TH ALIGN="CENTER" NOWRAP COLSPAN=1><I>orientation</I></TH>
+<TH ALIGN="CENTER" NOWRAP COLSPAN=1><I>&nbsp;&nbsp;&nbsp;spin&nbsp;&nbsp;&nbsp;</I></TH>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP><I>x</I></TD>
+<TD ALIGN="RIGHT" NOWRAP>-19.9&nbsp;&nbsp;&nbsp;&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP>&nbsp;-0.30&nbsp;&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP><I>y</I></TD>
+<TD ALIGN="RIGHT" NOWRAP>-9.1&nbsp;&nbsp;&nbsp;&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP>&nbsp;+0.60&nbsp;&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP><I>z</I></TD>
+<TD ALIGN="RIGHT" NOWRAP>+22.9&nbsp;&nbsp;&nbsp;&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP>&nbsp;+0.70&nbsp;&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP><I>mas</I>&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP>&nbsp;<I>mas/y</I>&nbsp;</TD>
+</TR>
+</TABLE>
+<P>        <BR>
+<BR>
+<BR>
+<BR>
+<P>
+These orientation and spin components are interpreted as
+        <I>axial vectors.</I>  An axial vector points at the pole of
+        the rotation and its length is the amount of rotation in radians.
+        The order of the rotations, which are very small,
+  <DT>4.
+<DD>It was the intention that Hipparcos 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 FK5, and this routine returns those
+        <I>fictitious proper motions.</I>
+  <DT>5.
+<DD>The position returned by this routine is in the FK5 J2000
+        reference frame but at Julian epoch EPOCH.
+  <DT>6.
+<DD>See also sla_FK52H, sla_FK5HZ, sla_H2FK5.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Feissel, M. &amp; Mignard, F., 1998.,  <I>Astron.Astrophys.</I> <B>331</B>, L33-L36.
+     </DL>
+<BR> <HR>
+<A NAME="tex2html1626" HREF="node121.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1624" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1618" HREF="node119.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1627" HREF="node121.html">SLA_IMXV - Apply 3D Reverse Rotation</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1625" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1619" HREF="node119.html">SLA_H2FK5 - Hipparcos to FK5</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node121.html b/src/slalib/sun67.htx/node121.html
new file mode 100644
index 0000000..68ace5b
--- /dev/null
+++ b/src/slalib/sun67.htx/node121.html
@@ -0,0 +1,118 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_IMXV - Apply 3D Reverse Rotation</TITLE>
+<META NAME="description" CONTENT="SLA_IMXV - Apply 3D Reverse Rotation">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node122.html">
+<LINK REL="previous" HREF="node120.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node122.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1636" HREF="node122.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1634" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1628" HREF="node120.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1637" HREF="node122.html">SLA_INTIN - Decode an Integer Number</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1635" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1629" HREF="node120.html">SLA_HFK5Z - Hipparcos to FK5, no P.M.</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004108000000000000000">SLA_IMXV - Apply 3D Reverse Rotation</A>
+<A NAME="xref_SLA_IMXV">&#160;</A><A NAME="SLA_IMXV">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Multiply a 3-vector by the inverse of a rotation
+matrix (single precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_IMXV (RM, VA, VB)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RM</EM></TD>
+<TH ALIGN="LEFT"><B>R(3,3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>rotation matrix</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>VA</EM></TD>
+<TD ALIGN="LEFT"><B>R(3)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>vector to be rotated</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>VB</EM></TD>
+<TH ALIGN="LEFT"><B>R(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>result vector</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>This routine performs the operation:
+<BLOCKQUOTE><B>b</B> = <B>M</B><IMG WIDTH="17" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img70.gif"
+ ALT="$^{T}\cdot$"><B>a</B>
+</BLOCKQUOTE>
+        where <B>a</B> and <B>b</B> are the 3-vectors VA and VB
+        respectively, and <B>M</B> is the <IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img18.gif"
+ ALT="$3\times3$"> matrix RM.
+  <DT>2.
+<DD>The main function of this routine is apply an inverse
+        rotation;  under these circumstances, <IMG WIDTH="20" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img122.gif"
+ ALT="${\bf M}$"> is
+        <I>orthogonal</I>, with its inverse the same as its transpose.
+  <DT>3.
+<DD>To comply with the ANSI Fortran 77 standard, VA and VB must
+        <B>not</B> be the same array.  The routine is, in fact, coded
+        so as to work properly on the VAX and many other systems even
+        if this rule is violated, something that is <B>not</B>, however,
+        recommended.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1636" HREF="node122.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1634" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1628" HREF="node120.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1637" HREF="node122.html">SLA_INTIN - Decode an Integer Number</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1635" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1629" HREF="node120.html">SLA_HFK5Z - Hipparcos to FK5, no P.M.</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node122.html b/src/slalib/sun67.htx/node122.html
new file mode 100644
index 0000000..b06d5d3
--- /dev/null
+++ b/src/slalib/sun67.htx/node122.html
@@ -0,0 +1,170 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
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+<TITLE>SLA_INTIN - Decode an Integer Number</TITLE>
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+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004109000000000000000">SLA_INTIN - Decode an Integer Number</A>
+<A NAME="xref_SLA_INTIN">&#160;</A><A NAME="SLA_INTIN">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Convert free-format input into an integer.
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_INTIN (STRING, NSTRT, IRESLT, JFLAG)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>STRING</EM></TD>
+<TH ALIGN="LEFT"><B>C</B></TH>
+<TD ALIGN="LEFT" NOWRAP>string containing number to be decoded</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NSTRT</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>pointer to where decoding is to commence</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IRESLT</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>current value of result</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NSTRT</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>advanced to next number</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IRESLT</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>result</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JFLAG</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status: -1 = -OK, 0&nbsp;=&nbsp;+OK, 1&nbsp;=&nbsp;null result, 2&nbsp;=&nbsp;error</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The reason sla_INTIN has separate `OK' status values
+for + and - is to enable minus zero to be detected.
+This is of crucial importance
+       when decoding mixed-radix numbers.  For example, an angle
+       expressed as degrees, arcminutes and arcseconds may have a
+       leading minus sign but a zero degrees field.
+ <DT>2.
+<DD>A TAB is interpreted as a space. <I>n.b.</I> The test for TAB is
+       ASCII-specific.
+ <DT>3.
+<DD>The basic format is the sequence of fields <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img123.gif"
+ ALT="$\pm n$">,       where <IMG WIDTH="15" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img30.gif"
+ ALT="$\pm$"> is a sign
+       character `+' or `-', and <I>n</I> means a string of decimal digits.
+ <DT>4.
+<DD>Spaces:
+       <UL>
+<LI> Leading spaces are ignored.
+<LI> Spaces between the sign and the number are allowed.
+<LI> Trailing spaces are ignored;  the first signifies
+             end of decoding and subsequent ones are skipped.
+       </UL>
+ <DT>5.
+<DD>Delimiters:
+       <UL>
+<LI> Any character other than +,-,0-9 or space may be
+             used to signal the end of the number and terminate decoding.
+<LI> Comma is recognized by sla_INTIN as a special case; it
+             is skipped, leaving the pointer on the next character.  See
+             9, below.
+<LI> Decoding will in all cases terminate if end of string
+             is reached.
+       </UL>
+ <DT>6.
+<DD>The sign is optional.  The default is +.
+ <DT>7.
+<DD>A <I>null result</I> occurs when the string of characters
+       being decoded does not begin with +,- or 0-9, or
+       consists entirely of spaces.  When this condition is
+       detected, JFLAG is set to 1 and IRESLT is left untouched.
+ <DT>8.
+<DD>NSTRT = 1 for the first character in the string.
+ <DT>9.
+<DD>On return from sla_INTIN, NSTRT is set ready for the next
+       decode - following trailing blanks and any comma.  If a
+       delimiter other than comma is being used, NSTRT must be
+       incremented before the next call to sla_INTIN, otherwise
+       all subsequent calls will return a null result.
+ <DT>10.
+<DD>Errors (JFLAG=2) occur when:
+       <UL>
+<LI> there is a + or - but no number; or
+<LI> the number is greater than 2<SUP>31</SUP>-1.
+       </UL>
+ <DT>11.
+<DD>When an error has been detected, NSTRT is left
+       pointing to the character following the last
+       one used before the error came to light.
+ <DT>12.
+<DD>See also sla_FLOTIN and sla_DFLTIN.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1646" HREF="node123.html">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1647" HREF="node123.html">SLA_INVF - Invert Linear Model</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1645" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1639" HREF="node121.html">SLA_IMXV - Apply 3D Reverse Rotation</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node123.html b/src/slalib/sun67.htx/node123.html
new file mode 100644
index 0000000..a3d1a77
--- /dev/null
+++ b/src/slalib/sun67.htx/node123.html
@@ -0,0 +1,122 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_INVF - Invert Linear Model</TITLE>
+<META NAME="description" CONTENT="SLA_INVF - Invert Linear Model">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1657" HREF="node124.html">SLA_KBJ - Select Epoch Prefix</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1655" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1649" HREF="node122.html">SLA_INTIN - Decode an Integer Number</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004110000000000000000">SLA_INVF - Invert Linear Model</A>
+<A NAME="xref_SLA_INVF">&#160;</A><A NAME="SLA_INVF">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Invert a linear model of the type produced by the
+sla_FITXY routine.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_INVF (FWDS,BKWDS,J)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>FWDS</EM></TD>
+<TH ALIGN="LEFT"><B>D(6)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>model coefficients</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>BKWDS</EM></TD>
+<TH ALIGN="LEFT"><B>D(6)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>inverse model</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:  0 = OK, -1 = no inverse</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The models relate two sets of <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> coordinates as follows.
+Naming the six elements of FWDS <I>a</I>,<I>b</I>,<I>c</I>,<I>d</I>,<I>e</I> &amp; <I>f</I>,
+where two sets of coordinates [<I>x<SUB>1</SUB></I>,<I>y<SUB>1</SUB></I>] and
+        <IMG WIDTH="53" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img56.gif"
+ ALT="$[x_{2},y_{2}\,]$"> are related thus:
+        <BLOCKQUOTE><I>x<SUB>2</SUB></I> = <I>a</I> + <I>bx<SUB>1</SUB></I> + <I>cy<SUB>1</SUB></I> <BR>
+         <I>y<SUB>2</SUB></I> = <I>d</I> + <I>ex<SUB>1</SUB></I> + <I>fy<SUB>1</SUB></I></BLOCKQUOTE>
+        The present routine generates a new set of coefficients
+        <I>p</I>,<I>q</I>,<I>r</I>,<I>s</I>,<I>t</I> &amp; <I>u</I> (the array BKWDS) such that:
+        <BLOCKQUOTE><I>x<SUB>1</SUB></I> = <I>p</I> + <I>qx<SUB>2</SUB></I> + <I>ry<SUB>2</SUB></I> <BR>
+         <I>y<SUB>1</SUB></I> = <I>s</I> + <I>tx<SUB>2</SUB></I> + <I>uy<SUB>2</SUB></I></BLOCKQUOTE>
+  <DT>2.
+<DD>Two successive calls to this routine will deliver a set
+        of coefficients equal to the starting values.
+  <DT>3.
+<DD>To comply with the ANSI Fortran 77 standard, FWDS and BKWDS must
+        <B>not</B> be the same array.  The routine is, in fact, coded
+        so as to work properly on the VAX and many other systems even
+        if this rule is violated, something that is <B>not</B>, however,
+        recommended.
+  <DT>4.
+<DD>See also sla_FITXY, sla_PXY, sla_XY2XY, sla_DCMPF.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1656" HREF="node124.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1657" HREF="node124.html">SLA_KBJ - Select Epoch Prefix</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1655" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1649" HREF="node122.html">SLA_INTIN - Decode an Integer Number</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node124.html b/src/slalib/sun67.htx/node124.html
new file mode 100644
index 0000000..6337e94
--- /dev/null
+++ b/src/slalib/sun67.htx/node124.html
@@ -0,0 +1,104 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_KBJ - Select Epoch Prefix</TITLE>
+<META NAME="description" CONTENT="SLA_KBJ - Select Epoch Prefix">
+<META NAME="keywords" CONTENT="sun67">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1667" HREF="node125.html">SLA_M2AV - Rotation Matrix to Axial Vector</A>
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+<H2><A NAME="SECTION0004111000000000000000">SLA_KBJ - Select Epoch Prefix</A>
+<A NAME="xref_SLA_KBJ">&#160;</A><A NAME="SLA_KBJ">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Select epoch prefix `B' or `J'.
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_KBJ (JB, E, K, J)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JB</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>sla_DBJIN prefix status:  0=none, 1=`B', 2=`J'</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>E</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>epoch - Besselian or Julian</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>K</EM></TD>
+<TH ALIGN="LEFT"><B>C</B></TH>
+<TD ALIGN="LEFT" NOWRAP>`B' or `J'</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:  0=OK</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTE:</STRONG>
+<DD>The routine is mainly intended for use in conjunction with the
+sla_DBJIN routine.  If the value of JB indicates that an explicit
+       B or J prefix was detected by sla_DBJIN, a `B' or `J'
+       is returned to match.  If JB indicates that no explicit B or J
+       was supplied, the choice is made on the basis of the epoch
+       itself;  B is assumed for E &lt;1984, otherwise J.
+      </DL>
+<BR> <HR>
+<A NAME="tex2html1666" HREF="node125.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1667" HREF="node125.html">SLA_M2AV - Rotation Matrix to Axial Vector</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1665" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1659" HREF="node123.html">SLA_INVF - Invert Linear Model</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node125.html b/src/slalib/sun67.htx/node125.html
new file mode 100644
index 0000000..2542649
--- /dev/null
+++ b/src/slalib/sun67.htx/node125.html
@@ -0,0 +1,107 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_M2AV - Rotation Matrix to Axial Vector</TITLE>
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1677" HREF="node126.html">SLA_MAP - Mean to Apparent</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1675" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1669" HREF="node124.html">SLA_KBJ - Select Epoch Prefix</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004112000000000000000">SLA_M2AV - Rotation Matrix to Axial Vector</A>
+<A NAME="xref_SLA_M2AV">&#160;</A><A NAME="SLA_M2AV">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>From a rotation matrix, determine the corresponding axial vector
+(single precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_M2AV (RMAT, AXVEC)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RMAT</EM></TD>
+<TH ALIGN="LEFT"><B>R(3,3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>rotation matrix</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AXVEC</EM></TD>
+<TH ALIGN="LEFT"><B>R(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>axial vector (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>A rotation matrix describes a rotation about some arbitrary axis.
+The axis is called the <I>Euler axis</I>, and the angle through
+which the reference frame rotates is called the <I>Euler angle</I>.
+        The <I>axial vector</I> returned by this routine has the same
+        direction as the Euler axis, and its magnitude is the Euler angle
+        in radians.
+  <DT>2.
+<DD>The magnitude and direction of the axial vector can be separated
+        by means of the routine sla_VN.
+  <DT>3.
+<DD>The reference frame rotates clockwise as seen looking along
+        the axial vector from the origin.
+  <DT>4.
+<DD>If RMAT is null, so is the result.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1676" HREF="node126.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1677" HREF="node126.html">SLA_MAP - Mean to Apparent</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1675" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1669" HREF="node124.html">SLA_KBJ - Select Epoch Prefix</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node126.html b/src/slalib/sun67.htx/node126.html
new file mode 100644
index 0000000..abe5fb6
--- /dev/null
+++ b/src/slalib/sun67.htx/node126.html
@@ -0,0 +1,157 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_MAP - Mean to Apparent</TITLE>
+<META NAME="description" CONTENT="SLA_MAP - Mean to Apparent">
+<META NAME="keywords" CONTENT="sun67">
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+ SRC="contents_motif.gif"></A>
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+<B> Next:</B> <A NAME="tex2html1687" HREF="node127.html">SLA_MAPPA - Mean to Apparent Parameters</A>
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+<B>Up:</B> <A NAME="tex2html1685" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1679" HREF="node125.html">SLA_M2AV - Rotation Matrix to Axial Vector</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004113000000000000000">SLA_MAP - Mean to Apparent</A>
+<A NAME="xref_SLA_MAP">&#160;</A><A NAME="SLA_MAP">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Transform star <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> from mean place to geocentric apparent.
+The reference frames and timescales used are post IAU&nbsp;1976.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_MAP (RM, DM, PR, PD, PX, RV, EQ, DATE, RA, DA)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RM,DM</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>mean <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PR,PD</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>proper motions:  <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> changes per Julian year</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PX</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>parallax (arcsec)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RV</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>radial velocity (km&nbsp;s<SUP>-1</SUP>, +ve if receding)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EQ</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>epoch and equinox of star data (Julian)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>TDB for apparent place (JD-2400000.5)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RA,DA</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>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 sla_PM to apply proper
+        motion corrections before using this routine.
+  <DT>2.
+<DD>The distinction between the required TDB and TT is
+        always negligible.  Moreover, for all but the most
+        critical applications UTC is adequate.
+  <DT>3.
+<DD>The <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> proper motions are <IMG WIDTH="13" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img115.gif"
+ ALT="$\dot{\alpha}$"> rather than
+        <IMG WIDTH="48" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img116.gif"
+ ALT="$\dot{\alpha}\cos\delta$">, and are per year rather than per century.
+  <DT>4.
+<DD>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 sla_MAPPA routine
+        once and then either the sla_MAPQK routine (which includes
+        parallax and proper motion) or sla_MAPQKZ (which assumes
+        zero parallax and FK5 proper motion).
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>1984 <I>Astronomical Almanac</I>, pp B39-B41.
+<DT>2.
+<DD>Lederle &amp; Schwan, 1984. <I>Astr.Astrophys.</I> <B>134</B>, 1-6.
+</DL></DL>
+<BR> <HR>
+<A NAME="tex2html1686" HREF="node127.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1687" HREF="node127.html">SLA_MAPPA - Mean to Apparent Parameters</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1685" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1679" HREF="node125.html">SLA_M2AV - Rotation Matrix to Axial Vector</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node127.html b/src/slalib/sun67.htx/node127.html
new file mode 100644
index 0000000..6ed5222
--- /dev/null
+++ b/src/slalib/sun67.htx/node127.html
@@ -0,0 +1,159 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_MAPPA - Mean to Apparent Parameters</TITLE>
+<META NAME="description" CONTENT="SLA_MAPPA - Mean to Apparent Parameters">
+<META NAME="keywords" CONTENT="sun67">
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+<A NAME="tex2html1688" HREF="node126.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1697" HREF="node128.html">SLA_MAPQK - Quick Mean to Apparent</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1695" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1689" HREF="node126.html">SLA_MAP - Mean to Apparent</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004114000000000000000">SLA_MAPPA - Mean to Apparent Parameters</A>
+<A NAME="xref_SLA_MAPPA">&#160;</A><A NAME="SLA_MAPPA">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Compute star-independent parameters in preparation for
+conversions between mean place and geocentric apparent place.
+         The parameters produced by this routine are required in the
+         parallax, light deflection, aberration, and precession/nutation
+         parts of the mean/apparent transformations.
+         The reference frames and timescales used are post IAU&nbsp;1976.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_MAPPA (EQ, DATE, AMPRMS)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EQ</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>epoch of mean equinox to be used (Julian)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>TDB (JD-2400000.5)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AMPRMS</EM></TD>
+<TH ALIGN="LEFT"><B>D(21)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>star-independent mean-to-apparent parameters:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(1)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>time interval for proper motion (Julian years)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(2-4)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>barycentric position of the Earth (AU)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(5-7)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>heliocentric direction of the Earth (unit vector)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(8)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>(gravitational radius of
+Sun)<IMG WIDTH="31" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img16.gif"
+ ALT="$\times 2 / $">(Sun-Earth distance)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(9-11)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP><B>v</B>: barycentric Earth velocity in units of c</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(12)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="72" HEIGHT="45" ALIGN="MIDDLE" BORDER="0"
+ SRC="img17.gif"
+ ALT="$\sqrt{1-\left\vert\mbox{\bf v}\right\vert^2}$"></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(13-21)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>precession/nutation <IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img18.gif"
+ ALT="$3\times3$"> matrix</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>For DATE, the distinction between the required TDB and TT
+is always negligible.  Moreover, for all but the most
+critical applications UTC is adequate.
+  <DT>2.
+<DD>The accuracy of the routines using the parameters AMPRMS is
+        limited by the routine sla_EVP, used here to compute the
+        Earth position and velocity by the methods of Stumpff.
+        The maximum error in the resulting aberration corrections is
+        about 0.3 milliarcsecond.
+  <DT>3.
+<DD>The vectors AMPRMS(2-4) and AMPRMS(5-7) are referred to
+        the mean equinox and equator of epoch EQ.
+  <DT>4.
+<DD>The parameters produced by this routine are used by
+        sla_MAPQK and sla_MAPQKZ.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>1984 <I>Astronomical Almanac</I>, pp B39-B41.
+<DT>2.
+<DD>Lederle &amp; Schwan, 1984. <I>Astr.Astrophys.</I> <B>134</B>, 1-6.
+</DL></DL>
+<BR> <HR>
+<A NAME="tex2html1696" HREF="node128.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1697" HREF="node128.html">SLA_MAPQK - Quick Mean to Apparent</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1695" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1689" HREF="node126.html">SLA_MAP - Mean to Apparent</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node128.html b/src/slalib/sun67.htx/node128.html
new file mode 100644
index 0000000..b705fa9
--- /dev/null
+++ b/src/slalib/sun67.htx/node128.html
@@ -0,0 +1,187 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1707" HREF="node129.html">SLA_MAPQKZ - Quick Mean-Appt, no PM etc.</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1705" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1699" HREF="node127.html">SLA_MAPPA - Mean to Apparent Parameters</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004115000000000000000">SLA_MAPQK - Quick Mean to Apparent</A>
+<A NAME="xref_SLA_MAPQK">&#160;</A><A NAME="SLA_MAPQK">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Quick mean to apparent place:  transform a star <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> from
+mean place to geocentric apparent place, given the
+         star-independent parameters.  The reference frames and
+         timescales used are post IAU 1976.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_MAPQK (RM, DM, PR, PD, PX, RV, AMPRMS, RA, DA)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RM,DM</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>mean <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PR,PD</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>proper motions:  <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> changes per Julian year</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PX</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>parallax (arcsec)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RV</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>radial velocity (km&nbsp;s<SUP>-1</SUP>, +ve if receding)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AMPRMS</EM></TD>
+<TD ALIGN="LEFT"><B>D(21)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>star-independent mean-to-apparent parameters:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(1)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>time interval for proper motion (Julian years)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(2-4)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>barycentric position of the Earth (AU)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(5-7)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>heliocentric direction of the Earth (unit vector)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(8)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>(gravitational radius of
+Sun)<IMG WIDTH="31" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img16.gif"
+ ALT="$\times 2 / $">(Sun-Earth distance)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(9-11)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP><B>v</B>: barycentric Earth velocity in units of c</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(12)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="72" HEIGHT="45" ALIGN="MIDDLE" BORDER="0"
+ SRC="img17.gif"
+ ALT="$\sqrt{1-\left\vert\mbox{\bf v}\right\vert^2}$"></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(13-21)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>precession/nutation <IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img18.gif"
+ ALT="$3\times3$"> matrix</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RA,DA</EM></TD>
+<TH ALIGN="LEFT"><B>D </B></TH>
+<TD ALIGN="LEFT" NOWRAP>apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>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
+        sla_MAPPA routine.
+  <DT>2.
+<DD>If the parallax and proper motions are zero the sla_MAPQKZ
+        routine can be used instead.
+  <DT>3.
+<DD>The vectors AMPRMS(2-4) and AMPRMS(5-7) are referred to
+        the mean equinox and equator of epoch EQ.
+  <DT>4.
+<DD>Strictly speaking, the routine is not valid for solar-system
+        sources, though the error will usually be extremely small.
+        However, to prevent gross errors in the case where the
+        position of the Sun is specified, the gravitational
+        deflection term is restrained within about <IMG WIDTH="33" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img124.gif"
+ ALT="$920\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> of the
+        centre of the Sun's disc.  The term has a maximum value of
+        about 
+      <IMG WIDTH="31" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img125.gif"
+ ALT="$1\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.85$">    at this radius, and decreases to zero as
+        the centre of the disc is approached.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>1984 <I>Astronomical Almanac</I>, pp B39-B41.
+<DT>2.
+<DD>Lederle &amp; Schwan, 1984. <I>Astr.Astrophys.</I> <B>134</B>, 1-6.
+</DL></DL>
+<BR> <HR>
+<A NAME="tex2html1706" HREF="node129.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1704" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1698" HREF="node127.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1707" HREF="node129.html">SLA_MAPQKZ - Quick Mean-Appt, no PM etc.</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1705" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1699" HREF="node127.html">SLA_MAPPA - Mean to Apparent Parameters</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node129.html b/src/slalib/sun67.htx/node129.html
new file mode 100644
index 0000000..6cb5fed
--- /dev/null
+++ b/src/slalib/sun67.htx/node129.html
@@ -0,0 +1,175 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_MAPQKZ - Quick Mean-Appt, no PM etc.</TITLE>
+<META NAME="description" CONTENT="SLA_MAPQKZ - Quick Mean-Appt, no PM etc.">
+<META NAME="keywords" CONTENT="sun67">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1717" HREF="node130.html">SLA_MOON - Approx Moon Pos/Vel</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1715" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1709" HREF="node128.html">SLA_MAPQK - Quick Mean to Apparent</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004116000000000000000">SLA_MAPQKZ - Quick Mean-Appt, no PM <I>etc.</I></A>
+<A NAME="xref_SLA_MAPQKZ">&#160;</A><A NAME="SLA_MAPQKZ">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Quick mean to apparent place:  transform a star <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> from
+mean place to geocentric apparent place, given the
+         star-independent parameters, and assuming zero parallax
+         and FK5 proper motion.
+         The reference frames and timescales used are post IAU&nbsp;1976.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_MAPQKZ (RM, DM, AMPRMS, RA, DA)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RM,DM</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>mean <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AMPRMS</EM></TD>
+<TD ALIGN="LEFT"><B>D(21)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>star-independent mean-to-apparent parameters:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(1)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>time interval for proper motion (Julian years)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(2-4)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>barycentric position of the Earth (AU)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(5-7)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>heliocentric direction of the Earth (unit vector)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(8)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>(gravitational radius of
+Sun)<IMG WIDTH="31" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img16.gif"
+ ALT="$\times 2 / $">(Sun-Earth distance)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(9-11)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP><B>v</B>: barycentric Earth velocity in units of c</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(12)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="72" HEIGHT="45" ALIGN="MIDDLE" BORDER="0"
+ SRC="img17.gif"
+ ALT="$\sqrt{1-\left\vert\mbox{\bf v}\right\vert^2}$"></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(13-21)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>precession/nutation <IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img18.gif"
+ ALT="$3\times3$"> matrix</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RA,DA</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Use of this routine 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 sla_MAPPA routine.
+  <DT>2.
+<DD>The corresponding routine for the case of non-zero parallax
+        and FK5 proper motion is sla_MAPQK.
+  <DT>3.
+<DD>The vectors AMPRMS(2-4) and AMPRMS(5-7) are referred to the
+        mean equinox and equator of epoch EQ.
+  <DT>4.
+<DD>Strictly speaking, the routine is not valid for solar-system
+        sources, though the error will usually be extremely small.
+        However, to prevent gross errors in the case where the
+        position of the Sun is specified, the gravitational
+        deflection term is restrained within about <IMG WIDTH="33" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img124.gif"
+ ALT="$920\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> of the
+        centre of the Sun's disc.  The term has a maximum value of
+        about 
+      <IMG WIDTH="31" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img125.gif"
+ ALT="$1\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.85$">    at this radius, and decreases to zero as
+        the centre of the disc is approached.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>1984 <I>Astronomical Almanac</I>, pp B39-B41.
+<DT>2.
+<DD>Lederle &amp; Schwan, 1984. <I>Astr.Astrophys.</I> <B>134</B>, 1-6.
+</DL></DL>
+<BR> <HR>
+<A NAME="tex2html1716" HREF="node130.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1714" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1708" HREF="node128.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1717" HREF="node130.html">SLA_MOON - Approx Moon Pos/Vel</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1715" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1709" HREF="node128.html">SLA_MAPQK - Quick Mean to Apparent</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node13.html b/src/slalib/sun67.htx/node13.html
new file mode 100644
index 0000000..c8106bf
--- /dev/null
+++ b/src/slalib/sun67.htx/node13.html
@@ -0,0 +1,489 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SUBPROGRAM SPECIFICATIONS</TITLE>
+<META NAME="description" CONTENT="SUBPROGRAM SPECIFICATIONS">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node197.html">
+<LINK REL="previous" HREF="node12.html">
+<LINK REL="up" HREF="sun67.html">
+<LINK REL="next" HREF="node14.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html373" HREF="node14.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html371" HREF="sun67.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html365" HREF="node12.html">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html374" HREF="node14.html">SLA_ADDET - Add E-terms of Aberration</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html372" HREF="sun67.html">SLALIB   Positional Astronomy Library</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html366" HREF="node12.html">LINKING</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H1><A NAME="SECTION00040000000000000000">
+SUBPROGRAM SPECIFICATIONS</A>
+</H1>
+<P>      <BR><HR>
+<!--Table of Child-Links-->
+<A NAME="CHILD_LINKS">&#160;</A>
+<UL>
+<LI><A NAME="tex2html375" HREF="node14.html#SECTION00041000000000000000">
+SLA_ADDET - Add E-terms of Aberration</A>
+<LI><A NAME="tex2html376" HREF="node15.html#SECTION00042000000000000000">
+SLA_AFIN - Sexagesimal character string to angle</A>
+<LI><A NAME="tex2html377" HREF="node16.html#SECTION00043000000000000000">
+SLA_AIRMAS - Air Mass</A>
+<LI><A NAME="tex2html378" HREF="node17.html#SECTION00044000000000000000">
+SLA_ALTAZ - Velocities <I>etc.</I> for Altazimuth Mount</A>
+<LI><A NAME="tex2html379" HREF="node18.html#SECTION00045000000000000000">
+SLA_AMP - Apparent to Mean</A>
+<LI><A NAME="tex2html380" HREF="node19.html#SECTION00046000000000000000">
+SLA_AMPQK - Quick Apparent to Mean</A>
+<LI><A NAME="tex2html381" HREF="node20.html#SECTION00047000000000000000">
+SLA_AOP - Apparent to Observed</A>
+<LI><A NAME="tex2html382" HREF="node21.html#SECTION00048000000000000000">
+SLA_AOPPA - Appt-to-Obs Parameters</A>
+<LI><A NAME="tex2html383" HREF="node22.html#SECTION00049000000000000000">
+SLA_AOPPAT - Update Appt-to-Obs Parameters</A>
+<LI><A NAME="tex2html384" HREF="node23.html#SECTION000410000000000000000">
+SLA_AOPQK - Quick Appt-to-Observed</A>
+<LI><A NAME="tex2html385" HREF="node24.html#SECTION000411000000000000000">
+SLA_ATMDSP - Atmospheric Dispersion</A>
+<LI><A NAME="tex2html386" HREF="node25.html#SECTION000412000000000000000">
+SLA_AV2M - Rotation Matrix from Axial Vector</A>
+<LI><A NAME="tex2html387" HREF="node26.html#SECTION000413000000000000000">
+SLA_BEAR - Direction Between Points on a Sphere</A>
+<LI><A NAME="tex2html388" HREF="node27.html#SECTION000414000000000000000">
+SLA_CAF2R - Deg,Arcmin,Arcsec to Radians</A>
+<LI><A NAME="tex2html389" HREF="node28.html#SECTION000415000000000000000">
+SLA_CALDJ - Calendar Date to MJD</A>
+<LI><A NAME="tex2html390" HREF="node29.html#SECTION000416000000000000000">
+SLA_CALYD - Calendar to Year, Day</A>
+<LI><A NAME="tex2html391" HREF="node30.html#SECTION000417000000000000000">
+SLA_CC2S - Cartesian to Spherical</A>
+<LI><A NAME="tex2html392" HREF="node31.html#SECTION000418000000000000000">
+SLA_CC62S - Cartesian 6-Vector to Spherical</A>
+<LI><A NAME="tex2html393" HREF="node32.html#SECTION000419000000000000000">
+SLA_CD2TF - Days to Hour,Min,Sec</A>
+<LI><A NAME="tex2html394" HREF="node33.html#SECTION000420000000000000000">
+SLA_CLDJ - Calendar to MJD</A>
+<LI><A NAME="tex2html395" HREF="node34.html#SECTION000421000000000000000">
+SLA_CLYD - Calendar to Year, Day</A>
+<LI><A NAME="tex2html396" HREF="node35.html#SECTION000422000000000000000">
+SLA_COMBN - Next Combination</A>
+<LI><A NAME="tex2html397" HREF="node36.html#SECTION000423000000000000000">
+SLA_CR2AF - Radians to Deg,Arcmin,Arcsec</A>
+<LI><A NAME="tex2html398" HREF="node37.html#SECTION000424000000000000000">
+SLA_CR2TF - Radians to Hour,Min,Sec</A>
+<LI><A NAME="tex2html399" HREF="node38.html#SECTION000425000000000000000">
+SLA_CS2C - Spherical to Cartesian</A>
+<LI><A NAME="tex2html400" HREF="node39.html#SECTION000426000000000000000">
+SLA_CS2C6 - Spherical Pos/Vel to Cartesian</A>
+<LI><A NAME="tex2html401" HREF="node40.html#SECTION000427000000000000000">
+SLA_CTF2D - Hour,Min,Sec to Days</A>
+<LI><A NAME="tex2html402" HREF="node41.html#SECTION000428000000000000000">
+SLA_CTF2R - Hour,Min,Sec to Radians</A>
+<LI><A NAME="tex2html403" HREF="node42.html#SECTION000429000000000000000">
+SLA_DAF2R - Deg,Arcmin,Arcsec to Radians</A>
+<LI><A NAME="tex2html404" HREF="node43.html#SECTION000430000000000000000">
+SLA_DAFIN - Sexagesimal character string to angle</A>
+<LI><A NAME="tex2html405" HREF="node44.html#SECTION000431000000000000000">
+SLA_DAT - TAI-UTC</A>
+<LI><A NAME="tex2html406" HREF="node45.html#SECTION000432000000000000000">
+SLA_DAV2M - Rotation Matrix from Axial Vector</A>
+<LI><A NAME="tex2html407" HREF="node46.html#SECTION000433000000000000000">
+SLA_DBEAR - Direction Between Points on a Sphere</A>
+<LI><A NAME="tex2html408" HREF="node47.html#SECTION000434000000000000000">
+SLA_DBJIN - Decode String to B/J Epoch (DP)</A>
+<LI><A NAME="tex2html409" HREF="node48.html#SECTION000435000000000000000">
+SLA_DC62S - Cartesian 6-Vector to Spherical</A>
+<LI><A NAME="tex2html410" HREF="node49.html#SECTION000436000000000000000">
+SLA_DCC2S - Cartesian to Spherical</A>
+<LI><A NAME="tex2html411" HREF="node50.html#SECTION000437000000000000000">
+SLA_DCMPF - Interpret Linear Fit</A>
+<LI><A NAME="tex2html412" HREF="node51.html#SECTION000438000000000000000">
+SLA_DCS2C - Spherical to Cartesian</A>
+<LI><A NAME="tex2html413" HREF="node52.html#SECTION000439000000000000000">
+SLA_DD2TF - Days to Hour,Min,Sec</A>
+<LI><A NAME="tex2html414" HREF="node53.html#SECTION000440000000000000000">
+SLA_DE2H - <IMG WIDTH="27" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img65.gif"
+ ALT="$h,\delta$"> to Az,El</A>
+<LI><A NAME="tex2html415" HREF="node54.html#SECTION000441000000000000000">
+SLA_DEULER - Euler Angles to Rotation Matrix</A>
+<LI><A NAME="tex2html416" HREF="node55.html#SECTION000442000000000000000">
+SLA_DFLTIN - Decode a Double Precision Number</A>
+<LI><A NAME="tex2html417" HREF="node56.html#SECTION000443000000000000000">
+SLA_DH2E - Az,El to <IMG WIDTH="27" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img65.gif"
+ ALT="$h,\delta$"></A>
+<LI><A NAME="tex2html418" HREF="node57.html#SECTION000444000000000000000">
+SLA_DIMXV - Apply 3D Reverse Rotation</A>
+<LI><A NAME="tex2html419" HREF="node58.html#SECTION000445000000000000000">
+SLA_DJCAL - MJD to Gregorian for Output</A>
+<LI><A NAME="tex2html420" HREF="node59.html#SECTION000446000000000000000">
+SLA_DJCL - MJD to Year,Month,Day,Frac</A>
+<LI><A NAME="tex2html421" HREF="node60.html#SECTION000447000000000000000">
+SLA_DM2AV - Rotation Matrix to Axial Vector</A>
+<LI><A NAME="tex2html422" HREF="node61.html#SECTION000448000000000000000">
+SLA_DMAT - Solve Simultaneous Equations</A>
+<LI><A NAME="tex2html423" HREF="node62.html#SECTION000449000000000000000">
+SLA_DMOON - Approx Moon Pos/Vel</A>
+<LI><A NAME="tex2html424" HREF="node63.html#SECTION000450000000000000000">
+SLA_DMXM - Multiply <IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img18.gif"
+ ALT="$3\times3$"> Matrices</A>
+<LI><A NAME="tex2html425" HREF="node64.html#SECTION000451000000000000000">
+SLA_DMXV - Apply 3D Rotation</A>
+<LI><A NAME="tex2html426" HREF="node65.html#SECTION000452000000000000000">
+SLA_DPAV - Position-Angle Between Two Directions</A>
+<LI><A NAME="tex2html427" HREF="node66.html#SECTION000453000000000000000">
+SLA_DR2AF - Radians to Deg,Min,Sec,Frac</A>
+<LI><A NAME="tex2html428" HREF="node67.html#SECTION000454000000000000000">
+SLA_DR2TF - Radians to Hour,Min,Sec,Frac</A>
+<LI><A NAME="tex2html429" HREF="node68.html#SECTION000455000000000000000">
+SLA_DRANGE - Put Angle into Range <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$"></A>
+<LI><A NAME="tex2html430" HREF="node69.html#SECTION000456000000000000000">
+SLA_DRANRM - Put Angle into Range <IMG WIDTH="43" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img66.gif"
+ ALT="$0\!-\!2\pi$"></A>
+<LI><A NAME="tex2html431" HREF="node70.html#SECTION000457000000000000000">
+SLA_DS2C6 - Spherical Pos/Vel to Cartesian</A>
+<LI><A NAME="tex2html432" HREF="node71.html#SECTION000458000000000000000">
+SLA_DS2TP - Spherical to Tangent Plane</A>
+<LI><A NAME="tex2html433" HREF="node72.html#SECTION000459000000000000000">
+SLA_DSEP - Angle Between 2 Points on Sphere</A>
+<LI><A NAME="tex2html434" HREF="node73.html#SECTION000460000000000000000">
+SLA_DT - Approximate ET minus UT</A>
+<LI><A NAME="tex2html435" HREF="node74.html#SECTION000461000000000000000">
+SLA_DTF2D - Hour,Min,Sec to Days</A>
+<LI><A NAME="tex2html436" HREF="node75.html#SECTION000462000000000000000">
+SLA_DTF2R - Hour,Min,Sec to Radians</A>
+<LI><A NAME="tex2html437" HREF="node76.html#SECTION000463000000000000000">
+SLA_DTP2S - Tangent Plane to Spherical</A>
+<LI><A NAME="tex2html438" HREF="node77.html#SECTION000464000000000000000">
+SLA_DTP2V - Tangent Plane to Direction Cosines</A>
+<LI><A NAME="tex2html439" HREF="node78.html#SECTION000465000000000000000">
+SLA_DTPS2C - Plate centre from <IMG WIDTH="26" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img90.gif"
+ ALT="$\xi,\eta$"> and <IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img91.gif"
+ ALT="$\alpha,\delta$"></A>
+<LI><A NAME="tex2html440" HREF="node79.html#SECTION000466000000000000000">
+SLA_DTPV2C - Plate centre from <IMG WIDTH="26" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img90.gif"
+ ALT="$\xi,\eta$"> and <I>x</I>,<I>y</I>,<I>z</I></A>
+<LI><A NAME="tex2html441" HREF="node80.html#SECTION000467000000000000000">
+SLA_DTT - TT minus UTC</A>
+<LI><A NAME="tex2html442" HREF="node81.html#SECTION000468000000000000000">
+SLA_DV2TP - Direction Cosines to Tangent Plane</A>
+<LI><A NAME="tex2html443" HREF="node82.html#SECTION000469000000000000000">
+SLA_DVDV - Scalar Product</A>
+<LI><A NAME="tex2html444" HREF="node83.html#SECTION000470000000000000000">
+SLA_DVN - Normalize Vector</A>
+<LI><A NAME="tex2html445" HREF="node84.html#SECTION000471000000000000000">
+SLA_DVXV - Vector Product</A>
+<LI><A NAME="tex2html446" HREF="node85.html#SECTION000472000000000000000">
+SLA_E2H - <IMG WIDTH="27" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img65.gif"
+ ALT="$h,\delta$"> to Az,El</A>
+<LI><A NAME="tex2html447" HREF="node86.html#SECTION000473000000000000000">
+SLA_EARTH - Approx Earth Pos/Vel</A>
+<LI><A NAME="tex2html448" HREF="node87.html#SECTION000474000000000000000">
+SLA_ECLEQ - Ecliptic to Equatorial</A>
+<LI><A NAME="tex2html449" HREF="node88.html#SECTION000475000000000000000">
+SLA_ECMAT - Form <IMG WIDTH="81" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img95.gif"
+ ALT="$\alpha,\delta\rightarrow\lambda,\beta$"> Matrix</A>
+<LI><A NAME="tex2html450" HREF="node89.html#SECTION000476000000000000000">
+SLA_ECOR - RV &amp; Time Corrns to Sun</A>
+<LI><A NAME="tex2html451" HREF="node90.html#SECTION000477000000000000000">
+SLA_EG50 - B1950 <IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img91.gif"
+ ALT="$\alpha,\delta$"> to Galactic</A>
+<LI><A NAME="tex2html452" HREF="node91.html#SECTION000478000000000000000">
+SLA_EL2UE - Conventional to Universal Elements</A>
+<LI><A NAME="tex2html453" HREF="node92.html#SECTION000479000000000000000">
+SLA_EPB - MJD to Besselian Epoch</A>
+<LI><A NAME="tex2html454" HREF="node93.html#SECTION000480000000000000000">
+SLA_EPB2D - Besselian Epoch to MJD</A>
+<LI><A NAME="tex2html455" HREF="node94.html#SECTION000481000000000000000">
+SLA_EPCO - Convert Epoch to B or J</A>
+<LI><A NAME="tex2html456" HREF="node95.html#SECTION000482000000000000000">
+SLA_EPJ - MJD to Julian Epoch</A>
+<LI><A NAME="tex2html457" HREF="node96.html#SECTION000483000000000000000">
+SLA_EPJ2D - Julian Epoch to MJD</A>
+<LI><A NAME="tex2html458" HREF="node97.html#SECTION000484000000000000000">
+SLA_EQECL - J2000 <IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img91.gif"
+ ALT="$\alpha,\delta$"> to Ecliptic</A>
+<LI><A NAME="tex2html459" HREF="node98.html#SECTION000485000000000000000">
+SLA_EQEQX - Equation of the Equinoxes</A>
+<LI><A NAME="tex2html460" HREF="node99.html#SECTION000486000000000000000">
+SLA_EQGAL - J2000 <IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img91.gif"
+ ALT="$\alpha,\delta$"> to Galactic</A>
+<LI><A NAME="tex2html461" HREF="node100.html#SECTION000487000000000000000">
+SLA_ETRMS - E-terms of Aberration</A>
+<LI><A NAME="tex2html462" HREF="node101.html#SECTION000488000000000000000">
+SLA_EULER - Rotation Matrix from Euler Angles</A>
+<LI><A NAME="tex2html463" HREF="node102.html#SECTION000489000000000000000">
+SLA_EVP - Earth Position &amp; Velocity</A>
+<LI><A NAME="tex2html464" HREF="node103.html#SECTION000490000000000000000">
+SLA_FITXY - Fit Linear Model to Two <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> Sets</A>
+<LI><A NAME="tex2html465" HREF="node104.html#SECTION000491000000000000000">
+SLA_FK425 - FK4 to FK5</A>
+<LI><A NAME="tex2html466" HREF="node105.html#SECTION000492000000000000000">
+SLA_FK45Z - FK4 to FK5, no P.M. or Parallax</A>
+<LI><A NAME="tex2html467" HREF="node106.html#SECTION000493000000000000000">
+SLA_FK524 - FK5 to FK4</A>
+<LI><A NAME="tex2html468" HREF="node107.html#SECTION000494000000000000000">
+SLA_FK52H - FK5 to Hipparcos</A>
+<LI><A NAME="tex2html469" HREF="node108.html#SECTION000495000000000000000">
+SLA_FK54Z - FK5 to FK4, no P.M. or Parallax</A>
+<LI><A NAME="tex2html470" HREF="node109.html#SECTION000496000000000000000">
+SLA_FK5HZ - FK5 to Hipparcos, no P.M.</A>
+<LI><A NAME="tex2html471" HREF="node110.html#SECTION000497000000000000000">
+SLA_FLOTIN - Decode a Real Number</A>
+<LI><A NAME="tex2html472" HREF="node111.html#SECTION000498000000000000000">
+SLA_GALEQ - Galactic to J2000 <IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img91.gif"
+ ALT="$\alpha,\delta$"></A>
+<LI><A NAME="tex2html473" HREF="node112.html#SECTION000499000000000000000">
+SLA_GALSUP - Galactic to Supergalactic</A>
+<LI><A NAME="tex2html474" HREF="node113.html#SECTION0004100000000000000000">
+SLA_GE50 - Galactic to B1950 <IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img91.gif"
+ ALT="$\alpha,\delta$"></A>
+<LI><A NAME="tex2html475" HREF="node114.html#SECTION0004101000000000000000">
+SLA_GEOC - Geodetic to Geocentric</A>
+<LI><A NAME="tex2html476" HREF="node115.html#SECTION0004102000000000000000">
+SLA_GMST - UT to GMST</A>
+<LI><A NAME="tex2html477" HREF="node116.html#SECTION0004103000000000000000">
+SLA_GMSTA - UT to GMST (extra precision)</A>
+<LI><A NAME="tex2html478" HREF="node117.html#SECTION0004104000000000000000">
+SLA_GRESID - Gaussian Residual</A>
+<LI><A NAME="tex2html479" HREF="node118.html#SECTION0004105000000000000000">
+SLA_H2E - Az,El to <IMG WIDTH="27" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img65.gif"
+ ALT="$h,\delta$"></A>
+<LI><A NAME="tex2html480" HREF="node119.html#SECTION0004106000000000000000">
+SLA_H2FK5 - Hipparcos to FK5</A>
+<LI><A NAME="tex2html481" HREF="node120.html#SECTION0004107000000000000000">
+SLA_HFK5Z - Hipparcos to FK5, no P.M.</A>
+<LI><A NAME="tex2html482" HREF="node121.html#SECTION0004108000000000000000">
+SLA_IMXV - Apply 3D Reverse Rotation</A>
+<LI><A NAME="tex2html483" HREF="node122.html#SECTION0004109000000000000000">
+SLA_INTIN - Decode an Integer Number</A>
+<LI><A NAME="tex2html484" HREF="node123.html#SECTION0004110000000000000000">
+SLA_INVF - Invert Linear Model</A>
+<LI><A NAME="tex2html485" HREF="node124.html#SECTION0004111000000000000000">
+SLA_KBJ - Select Epoch Prefix</A>
+<LI><A NAME="tex2html486" HREF="node125.html#SECTION0004112000000000000000">
+SLA_M2AV - Rotation Matrix to Axial Vector</A>
+<LI><A NAME="tex2html487" HREF="node126.html#SECTION0004113000000000000000">
+SLA_MAP - Mean to Apparent</A>
+<LI><A NAME="tex2html488" HREF="node127.html#SECTION0004114000000000000000">
+SLA_MAPPA - Mean to Apparent Parameters</A>
+<LI><A NAME="tex2html489" HREF="node128.html#SECTION0004115000000000000000">
+SLA_MAPQK - Quick Mean to Apparent</A>
+<LI><A NAME="tex2html490" HREF="node129.html#SECTION0004116000000000000000">
+SLA_MAPQKZ - Quick Mean-Appt, no PM <I>etc.</I></A>
+<LI><A NAME="tex2html491" HREF="node130.html#SECTION0004117000000000000000">
+SLA_MOON - Approx Moon Pos/Vel</A>
+<LI><A NAME="tex2html492" HREF="node131.html#SECTION0004118000000000000000">
+SLA_MXM - Multiply <IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img18.gif"
+ ALT="$3\times3$"> Matrices</A>
+<LI><A NAME="tex2html493" HREF="node132.html#SECTION0004119000000000000000">
+SLA_MXV - Apply 3D Rotation</A>
+<LI><A NAME="tex2html494" HREF="node133.html#SECTION0004120000000000000000">
+SLA_NUT - Nutation Matrix</A>
+<LI><A NAME="tex2html495" HREF="node134.html#SECTION0004121000000000000000">
+SLA_NUTC - Nutation Components</A>
+<LI><A NAME="tex2html496" HREF="node135.html#SECTION0004122000000000000000">
+SLA_OAP - Observed to Apparent</A>
+<LI><A NAME="tex2html497" HREF="node136.html#SECTION0004123000000000000000">
+SLA_OAPQK - Quick Observed to Apparent</A>
+<LI><A NAME="tex2html498" HREF="node137.html#SECTION0004124000000000000000">
+SLA_OBS - Observatory Parameters</A>
+<LI><A NAME="tex2html499" HREF="node138.html#SECTION0004125000000000000000">
+SLA_PA - <IMG WIDTH="27" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img65.gif"
+ ALT="$h,\delta$"> to Parallactic Angle</A>
+<LI><A NAME="tex2html500" HREF="node139.html#SECTION0004126000000000000000">
+SLA_PAV - Position-Angle Between Two Directions</A>
+<LI><A NAME="tex2html501" HREF="node140.html#SECTION0004127000000000000000">
+SLA_PCD - Apply Radial Distortion</A>
+<LI><A NAME="tex2html502" HREF="node141.html#SECTION0004128000000000000000">
+SLA_PDA2H - H.A. for a Given Azimuth</A>
+<LI><A NAME="tex2html503" HREF="node142.html#SECTION0004129000000000000000">
+SLA_PDQ2H - H.A. for a Given P.A.</A>
+<LI><A NAME="tex2html504" HREF="node143.html#SECTION0004130000000000000000">
+SLA_PERMUT - Next Permutation</A>
+<LI><A NAME="tex2html505" HREF="node144.html#SECTION0004131000000000000000">
+SLA_PERTEL - Perturbed Orbital Elements</A>
+<LI><A NAME="tex2html506" HREF="node145.html#SECTION0004132000000000000000">
+SLA_PERTUE - Perturbed Universal Elements</A>
+<LI><A NAME="tex2html507" HREF="node146.html#SECTION0004133000000000000000">
+SLA_PLANEL - Planet Position from Elements</A>
+<LI><A NAME="tex2html508" HREF="node147.html#SECTION0004134000000000000000">
+SLA_PLANET - Planetary Ephemerides</A>
+<LI><A NAME="tex2html509" HREF="node148.html#SECTION0004135000000000000000">
+SLA_PLANTE - <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> of Planet from Elements</A>
+<LI><A NAME="tex2html510" HREF="node149.html#SECTION0004136000000000000000">
+SLA_PM - Proper Motion</A>
+<LI><A NAME="tex2html511" HREF="node150.html#SECTION0004137000000000000000">
+SLA_POLMO - Polar Motion</A>
+<LI><A NAME="tex2html512" HREF="node151.html#SECTION0004138000000000000000">
+SLA_PREBN - Precession Matrix (FK4)</A>
+<LI><A NAME="tex2html513" HREF="node152.html#SECTION0004139000000000000000">
+SLA_PREC - Precession Matrix (FK5)</A>
+<LI><A NAME="tex2html514" HREF="node153.html#SECTION0004140000000000000000">
+SLA_PRECES - Precession</A>
+<LI><A NAME="tex2html515" HREF="node154.html#SECTION0004141000000000000000">
+SLA_PRECL - Precession Matrix (latest)</A>
+<LI><A NAME="tex2html516" HREF="node155.html#SECTION0004142000000000000000">
+SLA_PRENUT - Precession/Nutation Matrix</A>
+<LI><A NAME="tex2html517" HREF="node156.html#SECTION0004143000000000000000">
+SLA_PV2EL - Orbital Elements from Position/Velocity</A>
+<LI><A NAME="tex2html518" HREF="node157.html#SECTION0004144000000000000000">
+SLA_PV2UE - Position/Velocity to Universal Elements</A>
+<LI><A NAME="tex2html519" HREF="node158.html#SECTION0004145000000000000000">
+SLA_PVOBS - Observatory Position &amp; Velocity</A>
+<LI><A NAME="tex2html520" HREF="node159.html#SECTION0004146000000000000000">
+SLA_PXY - Apply Linear Model</A>
+<LI><A NAME="tex2html521" HREF="node160.html#SECTION0004147000000000000000">
+SLA_RANDOM - Random Number</A>
+<LI><A NAME="tex2html522" HREF="node161.html#SECTION0004148000000000000000">
+SLA_RANGE - Put Angle into Range <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$"></A>
+<LI><A NAME="tex2html523" HREF="node162.html#SECTION0004149000000000000000">
+SLA_RANORM - Put Angle into Range <IMG WIDTH="43" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img66.gif"
+ ALT="$0\!-\!2\pi$"></A>
+<LI><A NAME="tex2html524" HREF="node163.html#SECTION0004150000000000000000">
+SLA_RCC - Barycentric Coordinate Time</A>
+<LI><A NAME="tex2html525" HREF="node164.html#SECTION0004151000000000000000">
+SLA_RDPLAN - Apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> of Planet</A>
+<LI><A NAME="tex2html526" HREF="node165.html#SECTION0004152000000000000000">
+SLA_REFCO - Refraction Constants</A>
+<LI><A NAME="tex2html527" HREF="node166.html#SECTION0004153000000000000000">
+SLA_REFCOQ - Refraction Constants (fast)</A>
+<LI><A NAME="tex2html528" HREF="node167.html#SECTION0004154000000000000000">
+SLA_REFRO - Refraction</A>
+<LI><A NAME="tex2html529" HREF="node168.html#SECTION0004155000000000000000">
+SLA_REFV - Apply Refraction to Vector</A>
+<LI><A NAME="tex2html530" HREF="node169.html#SECTION0004156000000000000000">
+SLA_REFZ - Apply Refraction to ZD</A>
+<LI><A NAME="tex2html531" HREF="node170.html#SECTION0004157000000000000000">
+SLA_RVEROT - RV Corrn to Earth Centre</A>
+<LI><A NAME="tex2html532" HREF="node171.html#SECTION0004158000000000000000">
+SLA_RVGALC - RV Corrn to Galactic Centre</A>
+<LI><A NAME="tex2html533" HREF="node172.html#SECTION0004159000000000000000">
+SLA_RVLG - RV Corrn to Local Group</A>
+<LI><A NAME="tex2html534" HREF="node173.html#SECTION0004160000000000000000">
+SLA_RVLSRD - RV Corrn to Dynamical LSR</A>
+<LI><A NAME="tex2html535" HREF="node174.html#SECTION0004161000000000000000">
+SLA_RVLSRK - RV Corrn to Kinematical LSR</A>
+<LI><A NAME="tex2html536" HREF="node175.html#SECTION0004162000000000000000">
+SLA_S2TP - Spherical to Tangent Plane</A>
+<LI><A NAME="tex2html537" HREF="node176.html#SECTION0004163000000000000000">
+SLA_SEP - Angle Between 2 Points on Sphere</A>
+<LI><A NAME="tex2html538" HREF="node177.html#SECTION0004164000000000000000">
+SLA_SMAT - Solve Simultaneous Equations</A>
+<LI><A NAME="tex2html539" HREF="node178.html#SECTION0004165000000000000000">
+SLA_SUBET - Remove E-terms</A>
+<LI><A NAME="tex2html540" HREF="node179.html#SECTION0004166000000000000000">
+SLA_SUPGAL - Supergalactic to Galactic</A>
+<LI><A NAME="tex2html541" HREF="node180.html#SECTION0004167000000000000000">
+SLA_SVD - Singular Value Decomposition</A>
+<LI><A NAME="tex2html542" HREF="node181.html#SECTION0004168000000000000000">
+SLA_SVDCOV - Covariance Matrix from SVD</A>
+<LI><A NAME="tex2html543" HREF="node182.html#SECTION0004169000000000000000">
+SLA_SVDSOL - Solution Vector from SVD</A>
+<LI><A NAME="tex2html544" HREF="node183.html#SECTION0004170000000000000000">
+SLA_TP2S - Tangent Plane to Spherical</A>
+<LI><A NAME="tex2html545" HREF="node184.html#SECTION0004171000000000000000">
+SLA_TP2V - Tangent Plane to Direction Cosines</A>
+<LI><A NAME="tex2html546" HREF="node185.html#SECTION0004172000000000000000">
+SLA_TPS2C - Plate centre from <IMG WIDTH="26" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img90.gif"
+ ALT="$\xi,\eta$"> and <IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img91.gif"
+ ALT="$\alpha,\delta$"></A>
+<LI><A NAME="tex2html547" HREF="node186.html#SECTION0004173000000000000000">
+SLA_TPV2C - Plate centre from <IMG WIDTH="26" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img90.gif"
+ ALT="$\xi,\eta$"> and <I>x</I>,<I>y</I>,<I>z</I></A>
+<LI><A NAME="tex2html548" HREF="node187.html#SECTION0004174000000000000000">
+SLA_UE2EL - Universal to Conventional Elements</A>
+<LI><A NAME="tex2html549" HREF="node188.html#SECTION0004175000000000000000">
+SLA_UE2PV - Pos/Vel from Universal Elements</A>
+<LI><A NAME="tex2html550" HREF="node189.html#SECTION0004176000000000000000">
+SLA_UNPCD - Remove Radial Distortion</A>
+<LI><A NAME="tex2html551" HREF="node190.html#SECTION0004177000000000000000">
+SLA_V2TP - Direction Cosines to Tangent Plane</A>
+<LI><A NAME="tex2html552" HREF="node191.html#SECTION0004178000000000000000">
+SLA_VDV - Scalar Product</A>
+<LI><A NAME="tex2html553" HREF="node192.html#SECTION0004179000000000000000">
+SLA_VN - Normalize Vector</A>
+<LI><A NAME="tex2html554" HREF="node193.html#SECTION0004180000000000000000">
+SLA_VXV - Vector Product</A>
+<LI><A NAME="tex2html555" HREF="node194.html#SECTION0004181000000000000000">
+SLA_WAIT - Time Delay</A>
+<LI><A NAME="tex2html556" HREF="node195.html#SECTION0004182000000000000000">
+SLA_XY2XY - Apply Linear Model to an <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"></A>
+<LI><A NAME="tex2html557" HREF="node196.html#SECTION0004183000000000000000">
+SLA_ZD - <IMG WIDTH="27" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img65.gif"
+ ALT="$h,\delta$"> to Zenith Distance</A>
+</UL>
+<!--End of Table of Child-Links-->
+<BR> <HR>
+<A NAME="tex2html373" HREF="node14.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html371" HREF="sun67.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html365" HREF="node12.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html374" HREF="node14.html">SLA_ADDET - Add E-terms of Aberration</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html372" HREF="sun67.html">SLALIB   Positional Astronomy Library</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html366" HREF="node12.html">LINKING</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node130.html b/src/slalib/sun67.htx/node130.html
new file mode 100644
index 0000000..99d6086
--- /dev/null
+++ b/src/slalib/sun67.htx/node130.html
@@ -0,0 +1,140 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_MOON - Approx Moon Pos/Vel</TITLE>
+<META NAME="description" CONTENT="SLA_MOON - Approx Moon Pos/Vel">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node131.html">
+<LINK REL="previous" HREF="node129.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node131.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1726" HREF="node131.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1724" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1718" HREF="node129.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1727" HREF="node131.html">SLA_MXM - Multiply Matrices</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1725" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1719" HREF="node129.html">SLA_MAPQKZ - Quick Mean-Appt, no PM etc.</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004117000000000000000">SLA_MOON - Approx Moon Pos/Vel</A>
+<A NAME="xref_SLA_MOON">&#160;</A><A NAME="SLA_MOON">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Approximate geocentric position and velocity of the Moon
+(single precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_MOON (IY, ID, FD, PV)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IY</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>year</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ID</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>day in year (1 = Jan 1st)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>FD</EM></TD>
+<TD ALIGN="LEFT"><B>R </B></TD>
+<TD ALIGN="LEFT" NOWRAP>fraction of day</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PV</EM></TD>
+<TH ALIGN="LEFT"><B>R(6)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>Moon <IMG WIDTH="106" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img51.gif"
+ ALT="$[\,x,y,z,\dot{x},\dot{y},\dot{z}\,]$">, mean equator and equinox of
+date (AU, AU&nbsp;s<SUP>-1</SUP>)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The date and time is TDB (loosely ET) in a Julian calendar
+which has been aligned to the ordinary Gregorian
+calendar for the interval 1900 March 1 to 2100 February 28.
+        The year and day can be obtained by calling sla_CALYD or
+        sla_CLYD.
+  <DT>2.
+<DD>The position is accurate to better than 0.5&nbsp;arcminute
+        in direction and 1000&nbsp;km in distance.  The velocity
+        is accurate to better than 
+      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img83.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.5$">    per hour in direction
+        and 4&nbsp;metres per socond in distance.  (RMS figures with respect
+        to JPL DE200 for the interval 1960-2025 are <IMG WIDTH="25" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img126.gif"
+ ALT="$14\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> and
+<P>      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img76.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.2$">    per hour in longitude, <IMG WIDTH="17" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img127.gif"
+ ALT="$9\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> and 
+      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img76.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.2$"><P>
+per hour in latitude, 350&nbsp;km and 2&nbsp;metres per second in distance.)
+        Note that the distance accuracy is comparatively poor because this
+        routine is principally intended for computing topocentric direction.
+  <DT>3.
+<DD>This routine is only a partial implementation of the original
+        Meeus algorithm (reference below), which offers 4 times the
+        accuracy in direction and 20 times the accuracy in distance
+        when fully implemented (as it is in sla_DMOON).
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Meeus, <I>l'Astronomie</I>, June 1984, p348.
+</DL>
+<BR> <HR>
+<A NAME="tex2html1726" HREF="node131.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1724" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1718" HREF="node129.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1727" HREF="node131.html">SLA_MXM - Multiply Matrices</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1725" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1719" HREF="node129.html">SLA_MAPQKZ - Quick Mean-Appt, no PM etc.</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node131.html b/src/slalib/sun67.htx/node131.html
new file mode 100644
index 0000000..7ee2c74
--- /dev/null
+++ b/src/slalib/sun67.htx/node131.html
@@ -0,0 +1,106 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_MXM - Multiply Matrices</TITLE>
+<META NAME="description" CONTENT="SLA_MXM - Multiply Matrices">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node132.html">
+<LINK REL="previous" HREF="node130.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node132.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1736" HREF="node132.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1734" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1728" HREF="node130.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1737" HREF="node132.html">SLA_MXV - Apply 3D Rotation</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1735" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1729" HREF="node130.html">SLA_MOON - Approx Moon Pos/Vel</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004118000000000000000">&#160;</A><A NAME="xref_SLA_MXM">&#160;</A><A NAME="SLA_MXM">&#160;</A>
+<BR>
+SLA_MXM - Multiply <IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img18.gif"
+ ALT="$3\times3$"> Matrices
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Product of two <IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img18.gif"
+ ALT="$3\times3$"> matrices (single precision).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_MXM (A, B, C)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A</EM></TD>
+<TH ALIGN="LEFT"><B>R(3,3)</B></TH>
+<TH ALIGN="LEFT" NOWRAP>matrix <B>A</B></TH>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>B</EM></TD>
+<TD ALIGN="LEFT"><B>R(3,3)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>matrix <B>B</B></TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>C</EM></TD>
+<TH ALIGN="LEFT"><B>R(3,3)</B></TH>
+<TH ALIGN="LEFT" NOWRAP>matrix result: <B>A</B><IMG WIDTH="15" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img84.gif"
+ ALT="$\times$"><B>B</B></TH>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTE:</STRONG>
+<DD>To comply with the ANSI Fortran 77 standard, A, B and C must
+be different arrays.  The routine is, in fact, coded
+       so as to work properly on the VAX and many other systems even
+       if this rule is violated, something that is <B>not</B>, however,
+       recommended.
+      </DL>
+<BR> <HR>
+<A NAME="tex2html1736" HREF="node132.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1734" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1728" HREF="node130.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1737" HREF="node132.html">SLA_MXV - Apply 3D Rotation</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1735" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1729" HREF="node130.html">SLA_MOON - Approx Moon Pos/Vel</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node132.html b/src/slalib/sun67.htx/node132.html
new file mode 100644
index 0000000..5084d3d
--- /dev/null
+++ b/src/slalib/sun67.htx/node132.html
@@ -0,0 +1,117 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_MXV - Apply 3D Rotation</TITLE>
+<META NAME="description" CONTENT="SLA_MXV - Apply 3D Rotation">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node133.html">
+<LINK REL="previous" HREF="node131.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node133.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1746" HREF="node133.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1744" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1738" HREF="node131.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1747" HREF="node133.html">SLA_NUT - Nutation Matrix</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1745" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1739" HREF="node131.html">SLA_MXM - Multiply Matrices</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004119000000000000000">SLA_MXV - Apply 3D Rotation</A>
+<A NAME="xref_SLA_MXV">&#160;</A><A NAME="SLA_MXV">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Multiply a 3-vector by a rotation matrix (single precision).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_MXV (RM, VA, VB)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RM</EM></TD>
+<TH ALIGN="LEFT"><B>R(3,3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>rotation matrix</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>VA</EM></TD>
+<TD ALIGN="LEFT"><B>R(3)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>vector to be rotated</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>VB</EM></TD>
+<TH ALIGN="LEFT"><B>R(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>result vector</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>This routine performs the operation:
+<BLOCKQUOTE><B>b</B> = <B>M</B><IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"><B>a</B>
+</BLOCKQUOTE>
+        where <B>a</B> and <B>b</B> are the 3-vectors VA and VB
+        respectively, and <B>M</B> is the <IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img18.gif"
+ ALT="$3\times3$"> matrix RM.
+  <DT>2.
+<DD>The main function of this routine is apply a
+        rotation;  under these circumstances, <IMG WIDTH="20" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img122.gif"
+ ALT="${\bf M}$"> is a
+        <I>proper real orthogonal</I> matrix.
+  <DT>3.
+<DD>To comply with the ANSI Fortran 77 standard, VA and VB must
+        <B>not</B> be the same array.  The routine is, in fact, coded
+        so as to work properly on the VAX and many other systems even
+        if this rule is violated, something that is <B>not</B>, however,
+        recommended.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1746" HREF="node133.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1744" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1738" HREF="node131.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1747" HREF="node133.html">SLA_NUT - Nutation Matrix</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1745" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1739" HREF="node131.html">SLA_MXM - Multiply Matrices</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node133.html b/src/slalib/sun67.htx/node133.html
new file mode 100644
index 0000000..a849a15
--- /dev/null
+++ b/src/slalib/sun67.htx/node133.html
@@ -0,0 +1,111 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_NUT - Nutation Matrix</TITLE>
+<META NAME="description" CONTENT="SLA_NUT - Nutation Matrix">
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+ SRC="contents_motif.gif"></A>
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+<BR>
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+<BR>
+<B> Previous:</B> <A NAME="tex2html1749" HREF="node132.html">SLA_MXV - Apply 3D Rotation</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004120000000000000000">SLA_NUT - Nutation Matrix</A>
+<A NAME="xref_SLA_NUT">&#160;</A><A NAME="SLA_NUT">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Form the matrix of nutation (IAU 1980 theory) for a given date.
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_NUT (DATE, RMATN)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>TDB (formerly ET) as Modified Julian Date
+(JD-2400000.5)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RMATN</EM></TD>
+<TH ALIGN="LEFT"><B>D(3,3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>nutation matrix</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTE:</STRONG>
+<DD>The matrix is in the sense:
+<BLOCKQUOTE><B>v</B><SUB><I>true</I></SUB> =  <B>M</B><IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"><B>v</B><SUB><I>mean</I></SUB></BLOCKQUOTE>
+       where <B>v</B><SUB><I>true</I></SUB> is the star vector relative to the
+       true equator and equinox of date, <B>M</B> is the
+       <IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img18.gif"
+ ALT="$3\times3$"> matrix RMATN and
+       <B>v</B><SUB><I>mean</I></SUB> is the star vector relative to the
+       mean equator and equinox of date.
+      </DL>
+<P>     <DL>
+<DT><STRONG>REFERENCES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Final report of the IAU Working Group on Nutation,
+chairman P.K.Seidelmann, 1980.
+<DT>2.
+<DD>Kaplan, G.H., 1981. <I>USNO circular No. 163</I>, pA3-6.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1756" HREF="node134.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+<A NAME="tex2html1748" HREF="node132.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1757" HREF="node134.html">SLA_NUTC - Nutation Components</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1755" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1749" HREF="node132.html">SLA_MXV - Apply 3D Rotation</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node134.html b/src/slalib/sun67.htx/node134.html
new file mode 100644
index 0000000..a2b5df6
--- /dev/null
+++ b/src/slalib/sun67.htx/node134.html
@@ -0,0 +1,102 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_NUTC - Nutation Components</TITLE>
+<META NAME="description" CONTENT="SLA_NUTC - Nutation Components">
+<META NAME="keywords" CONTENT="sun67">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1767" HREF="node135.html">SLA_OAP - Observed to Apparent</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1765" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1759" HREF="node133.html">SLA_NUT - Nutation Matrix</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004121000000000000000">SLA_NUTC - Nutation Components</A>
+<A NAME="xref_SLA_NUTC">&#160;</A><A NAME="SLA_NUTC">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Nutation (IAU 1980 theory):  longitude &amp; obliquity
+components, and mean obliquity.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_NUTC (DATE, DPSI, DEPS, EPS0)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>TDB (formerly ET) as Modified Julian Date
+(JD-2400000.5)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DPSI,DEPS</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>nutation in longitude and obliquity (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EPS0</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>mean obliquity (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Final report of the IAU Working Group on Nutation,
+chairman P.K.Seidelmann, 1980.
+<DT>2.
+<DD>Kaplan, G.H., 1981. <I>USNO circular no. 163</I>, pA3-6.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1766" HREF="node135.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1764" HREF="node13.html">
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+<A NAME="tex2html1758" HREF="node133.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1767" HREF="node135.html">SLA_OAP - Observed to Apparent</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1765" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1759" HREF="node133.html">SLA_NUT - Nutation Matrix</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node135.html b/src/slalib/sun67.htx/node135.html
new file mode 100644
index 0000000..753bc4c
--- /dev/null
+++ b/src/slalib/sun67.htx/node135.html
@@ -0,0 +1,319 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_OAP - Observed to Apparent</TITLE>
+<META NAME="description" CONTENT="SLA_OAP - Observed to Apparent">
+<META NAME="keywords" CONTENT="sun67">
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+<A NAME="tex2html1774" HREF="node13.html">
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+<A NAME="tex2html1768" HREF="node134.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1777" HREF="node136.html">SLA_OAPQK - Quick Observed to Apparent</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1775" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1769" HREF="node134.html">SLA_NUTC - Nutation Components</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004122000000000000000">SLA_OAP - Observed to Apparent</A>
+<A NAME="xref_SLA_OAP">&#160;</A><A NAME="SLA_OAP">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Observed to apparent place.
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_OAP (
+         TYPE, OB1, OB2, DATE, DUT, ELONGM, PHIM,
+         HM, XP, YP, TDK, PMB, RH, WL, TLR, RAP, DAP)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>TYPE</EM></TD>
+<TH ALIGN="LEFT"><B>C*(*)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>type of coordinates - `R', `H' or `A' (see below)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>OB1</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>observed Az, HA or RA (radians; Az is N=0, E=<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img22.gif"
+ ALT="$90^{\circ}$">)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>OB2</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>observed zenith distance or <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TD ALIGN="LEFT"><B>D </B></TD>
+<TD ALIGN="LEFT" NOWRAP>UTC date/time (Modified Julian Date, JD-2400000.5)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DUT</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">UT:  UT1-UTC (UTC seconds)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ELONGM</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>observer's mean longitude (radians, east +ve)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PHIM</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>observer's mean geodetic latitude (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>HM</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>observer's height above sea level (metres)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>XP,YP</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>polar motion <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> coordinates (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>TDK</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>local ambient temperature (degrees K; std=273.155D0)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PMB</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>local atmospheric pressure (mB; std=1013.25D0)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>local relative humidity (in the range 0D0-1D0)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>WL</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>effective wavelength (<IMG WIDTH="26" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img21.gif"
+ ALT="$\mu{\rm m}$">, <I>e.g.</I> 0.55D0)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>TLR</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>tropospheric lapse rate (degrees K per metre,
+<I>e.g.</I> 0.0065D0)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RAP,DAP</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>geocentric apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"></TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>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 is <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img22.gif"
+ ALT="$90^{\circ}$">) 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.)
+  <DT>2.
+<DD>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 azimuth and elevation should be within about
+<P>      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img25.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.1$">    for <IMG WIDTH="56" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img26.gif"
+ ALT="$\zeta<70^{\circ}$">.  Even
+        at a topocentric zenith distance of
+        <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img22.gif"
+ ALT="$90^{\circ}$">, the accuracy in elevation should be better than
+        1&nbsp;arcminute;  useful results are available for a further
+        <IMG WIDTH="18" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img27.gif"
+ ALT="$3^{\circ}$">, beyond which the sla_REFRO routine returns a
+        fixed value of the refraction.  The complementary
+        routines sla_AOP (or sla_AOPQK) and sla_OAP (or sla_OAPQK)
+        are self-consistent to better than 1&nbsp;microarcsecond all over
+        the celestial sphere.
+  <DT>3.
+<DD>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.
+  <DT>4.
+<DD><I>Observed</I> <IMG WIDTH="66" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img28.gif"
+ ALT="$[\,Az,El~]$"> means the position that would be seen by a
+        perfect theodolite located at the observer.  This is
+        related to the observed <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$"> 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.  <I>Observed</I> <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> or <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$"> 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 (<I>n.b.</I> not to the refracted pole).
+        By removing from the observed place the effects of
+        atmospheric refraction and diurnal aberration, the
+        geocentric apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> is obtained.
+  <DT>5.
+<DD>Frequently, <I>mean</I> rather than <I>apparent</I>
+        <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> will be required,
+        in which case further transformations will be necessary.  The
+        sla_AMP <I>etc.</I> routines will convert
+        the apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> 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 B1950
+        coordinates be needed, the routines sla_FK524 <I>etc.</I> will also
+        need to be applied.
+  <DT>6.
+<DD>To convert to apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> 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.
+  <DT>7.
+<DD>The star-independent apparent-to-observed-place parameters
+        in AOPRMS may be computed by means of the sla_AOPPA routine.
+        If nothing has changed significantly except the time, the
+        sla_AOPPAT routine may be used to perform the requisite
+        partial recomputation of AOPRMS.
+  <DT>8.
+<DD>The DATE argument is UTC expressed as an MJD.  This is,
+        strictly speaking, wrong, because of leap seconds.  However,
+        as long as the <IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">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 <IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">UT should
+        continue to be used.  As the 61st second completes, the MJD
+        should revert to the start of the day as, simultaneously,
+        the <IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">UT changes by one second to its post-leap new value.
+  <DT>9.
+<DD>The <IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">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 <IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">UT
+        within <IMG WIDTH="15" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img30.gif"
+ ALT="$\pm$"><IMG WIDTH="24" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img31.gif"
+ ALT="$0^{\rm s}\hspace{-0.3em}.9$">.  <DT>10.
+<DD>IMPORTANT - TAKE CARE WITH THE LONGITUDE SIGN CONVENTION.  The
+        longitude required by the present routine is <B>east-positive</B>,
+        in accordance with geographical convention (and right-handed).
+        In particular, note that the longitudes returned by the
+        sla_OBS routine are west-positive (as in the <I>Astronomical
+        Almanac</I> before 1984) and must be reversed in sign before use
+        in the present routine.
+  <DT>11.
+<DD>The polar coordinates XP,YP can be obtained from IERS
+        circulars and equivalent publications.  The
+        maximum amplitude is about 
+      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img32.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.3$">   .  If XP,YP values
+        are unavailable, use XP=YP=0D0.  See page B60 of the 1988
+        <I>Astronomical Almanac</I> for a definition of the two angles.
+  <DT>12.
+<DD>The height above sea level of the observing station, HM,
+        can be obtained from the <I>Astronomical Almanac</I> (Section J
+        in the 1988 edition), or via the routine sla_OBS.  If P,
+        the pressure in mB, is available, an adequate
+        estimate of HM can be obtained from the following expression:
+        <BLOCKQUOTE><TT>HM=-29.3D0*TSL*LOG(P/1013.25D0)</TT>
+        </BLOCKQUOTE>
+        where TSL is the approximate sea-level air temperature in degrees K
+        (see <I>Astrophysical Quantities</I>, C.W.Allen, 3rd&nbsp;edition,
+        &#167;52).  Similarly, if the pressure P is not known,
+        it can be estimated from the height of the observing
+        station, HM as follows:
+        <BLOCKQUOTE><TT>P=1013.25D0*EXP(-HM/(29.3D0*TSL))</TT>
+        </BLOCKQUOTE>
+        Note, however, that the refraction is proportional to the
+        pressure and that an accurate P value is important for
+        precise work.
+  <DT>13.
+<DD>The azimuths <I>etc.</I> used by the present routine are with
+        respect to the celestial pole.  Corrections from the terrestrial pole
+        can be computed using sla_POLMO.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1776" HREF="node136.html">
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+<B> Next:</B> <A NAME="tex2html1777" HREF="node136.html">SLA_OAPQK - Quick Observed to Apparent</A>
+<BR>
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+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node136.html b/src/slalib/sun67.htx/node136.html
new file mode 100644
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+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
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+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004123000000000000000">SLA_OAPQK - Quick Observed to Apparent</A>
+<A NAME="xref_SLA_OAPQK">&#160;</A><A NAME="SLA_OAPQK">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Quick observed to apparent place.
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_OAPQK (TYPE, OB1, OB2, AOPRMS, RAP, DAP)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>TYPE</EM></TD>
+<TH ALIGN="LEFT"><B>C*(*)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>type of coordinates - `R', `H' or `A' (see below)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>OB1</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>observed Az, HA or RA (radians; Az is N=0, E=<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img22.gif"
+ ALT="$90^{\circ}$">)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>OB2</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>observed zenith distance or <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AOPRMS</EM></TD>
+<TD ALIGN="LEFT"><B>D(14)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>star-independent apparent-to-observed parameters:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(1)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>geodetic latitude (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(2,3)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>sine and cosine of geodetic latitude</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(4)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>magnitude of diurnal aberration vector</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(5)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>height (HM)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(6)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>ambient temperature (TDK)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(7)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>pressure (PMB)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(8)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>relative humidity (RH)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(9)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>wavelength (WL)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(10)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>lapse rate (TLR)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(11,12)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>refraction constants A and B (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(13)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>longitude + eqn of equinoxes +
+``sidereal <IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">UT'' (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(14)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>local apparent sidereal time (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RAP,DAP</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>geocentric apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"></TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>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 is <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img22.gif"
+ ALT="$90^{\circ}$">) 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.)
+  <DT>2.
+<DD>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 azimuth and elevation should be within about
+<P>      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img25.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.1$">    for <IMG WIDTH="56" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img26.gif"
+ ALT="$\zeta<70^{\circ}$">.  Even
+        at a topocentric zenith distance of
+        <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img22.gif"
+ ALT="$90^{\circ}$">, the accuracy in elevation should be better than
+        1&nbsp;arcminute;  useful results are available for a further
+        <IMG WIDTH="18" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img27.gif"
+ ALT="$3^{\circ}$">, beyond which the sla_REFRO routine returns a
+        fixed value of the refraction.  The complementary
+        routines sla_AOP (or sla_AOPQK) and sla_OAP (or sla_OAPQK)
+        are self-consistent to better than 1&nbsp;microarcsecond all over
+        the celestial sphere.
+  <DT>3.
+<DD>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.
+  <DT>4.
+<DD><I>Observed</I> <IMG WIDTH="66" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img28.gif"
+ ALT="$[\,Az,El~]$"> means the position that would be seen by a
+        perfect theodolite located at the observer.  This is
+        related to the observed <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$"> 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.  <I>Observed</I> <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> or <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$"> 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 (<I>n.b.</I> not to the refracted pole).
+        By removing from the observed place the effects of
+        atmospheric refraction and diurnal aberration, the
+        geocentric apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> is obtained.
+  <DT>5.
+<DD>Frequently, <I>mean</I> rather than <I>apparent</I>
+        <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> will be required,
+        in which case further transformations will be necessary.  The
+        sla_AMP <I>etc.</I> routines will convert
+        the apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> 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 B1950
+        coordinates be needed, the routines sla_FK524 <I>etc.</I> will also
+        need to be applied.
+  <DT>6.
+<DD>To convert to apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> 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.
+  <DT>7.
+<DD>The star-independent apparent-to-observed-place parameters
+        in AOPRMS may be computed by means of the sla_AOPPA routine.
+        If nothing has changed significantly except the time, the
+        sla_AOPPAT routine may be used to perform the requisite
+        partial recomputation of AOPRMS.
+  <DT>8.
+<DD>The azimuths <I>etc.</I> used by the present routine are with
+        respect to the celestial pole.  Corrections from the terrestrial pole
+        can be computed using sla_POLMO.
+ </DL></DL>
+<BR> <HR>
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+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
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diff --git a/src/slalib/sun67.htx/node137.html b/src/slalib/sun67.htx/node137.html
new file mode 100644
index 0000000..eda8158
--- /dev/null
+++ b/src/slalib/sun67.htx/node137.html
@@ -0,0 +1,247 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
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+<H2><A NAME="SECTION0004124000000000000000">SLA_OBS - Observatory Parameters</A>
+<A NAME="xref_SLA_OBS">&#160;</A><A NAME="SLA_OBS">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Look up an entry in a standard list of
+groundbased observing stations parameters.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_OBS (N, C, NAME, W, P, H)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>N</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>number specifying observing station</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>GIVEN or RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>C</EM></TD>
+<TH ALIGN="LEFT"><B>C*(*)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>identifier specifying observing station</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NAME</EM></TD>
+<TH ALIGN="LEFT"><B>C*(*)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>name of specified observing station</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>W</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>longitude (radians, west +ve)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>P</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>geodetic latitude (radians, north +ve)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>H</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>height above sea level (metres)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Station identifiers C may be up to 10 characters long,
+and station names NAME may be up to 40 characters long.
+<DT>2.
+<DD>C and N are <I>alternative</I> ways of specifying the observing
+        station.  The C option, which is the most generally useful,
+        may be selected by specifying an N value of zero or less.
+        If N is 1 or more, the parameters of the Nth station
+        in the currently supported list are interrogated, and
+        the station identifier C is returned as well as NAME, W,
+        P and H.
+  <DT>3.
+<DD>If the station parameters are not available, either because
+        the station identifier C is not recognized, or because an
+        N value greater than the number of stations supported is
+        given, a name of `?' is returned and W, P and H are left in
+        their current states.
+  <DT>4.
+<DD>Programs can obtain a list of all currently supported
+        stations by calling the routine repeatedly, with N=1,2,3...
+        When NAME=`?' is seen, the list of stations has been
+        exhausted.  The stations at the time of writing are listed
+        below.
+  <DT>5.
+<DD>Station numbers, identifiers, names and other details are
+        subject to change and should not be hardwired into
+        application programs.
+  <DT>6.
+<DD>All station identifiers C are uppercase only;  lower case
+        characters must be converted to uppercase by the calling
+        program.  The station names returned may contain both upper-
+        and lowercase.  All characters 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.
+  <DT>7.
+<DD>IMPORTANT - BEWARE OF THE LONGITUDE SIGN CONVENTION.  The
+        longitude returned by sla_OBS is
+        <B>west-positive</B>, following the pre-1984 <I>Astronomical
+        Almanac</I>.  However, this sign convention is left-handed and is
+        the opposite of the one now used; elsewhere in
+        SLALIB the preferable east-positive convention is used.  In
+        particular, note that for use in sla_AOP, sla_AOPPA and
+        sla_OAP the sign of the longitude must be reversed.
+  <DT>8.
+<DD>Users are urged to inform the author of any improvements
+        they would like to see made.  For example:
+        <UL>
+<LI> typographical corrections
+<LI> more accurate parameters
+<LI> better station identifiers or names
+<LI> additional stations
+        </UL></DL>
+Stations supported by sla_OBS at the time of writing:
+<PRE><TT>
+<I>ID</I> 		 <I>NAME</I> 
+&nbsp;
+AAT 		 Anglo-Australian 3.9m Telescope 
+ANU2.3 		 Siding Spring 2.3 metre 
+APO3.5 		 Apache Point 3.5m 
+ARECIBO 		 Arecibo 1000 foot 
+ATCA 		 Australia Telescope Compact Array 
+BLOEMF 		 Bloemfontein 1.52 metre 
+BOSQALEGRE 		 Bosque Alegre 1.54 metre 
+CAMB1MILE 		 Cambridge 1 mile 
+CAMB5KM 		 Cambridge 5km 
+CATALINA61 		 Catalina 61 inch 
+CFHT 		 Canada-France-Hawaii 3.6m Telescope 
+CSO 		 Caltech Sub-mm Observatory, Mauna Kea 
+DAO72 		 DAO Victoria BC 1.85 metre 
+DUNLAP74 		 David Dunlap 74 inch 
+DUPONT 		 Du Pont 2.5m Telescope, Las Campanas 
+EFFELSBERG 		 Effelsberg 100 metre 
+ESO3.6 		 ESO 3.6 metre 
+ESONTT 		 ESO 3.5 metre NTT 
+ESOSCHM 		 ESO 1 metre Schmidt, La Silla 
+FCRAO 		 Five College Radio Astronomy Obs 
+FLAGSTF61 		 USNO 61 inch astrograph, Flagstaff 
+GBVA140 		 Greenbank 140 foot 
+GBVA300 		 Greenbank 300 foot 
+GEMININ 		 Gemini North 8-m telescope 
+HARVARD 		 Harvard College Observatory 1.55m 
+HPROV1.52 		 Haute Provence 1.52 metre 
+HPROV1.93 		 Haute Provence 1.93 metre 
+IRTF 		 NASA IR Telescope Facility, Mauna Kea 
+JCMT 		 JCMT 15 metre 
+JODRELL1 		 Jodrell Bank 250 foot 
+KECK1 		 Keck 10m Telescope 1 
+KECK2 		 Keck 10m Telescope 2 
+KISO 		 Kiso 1.05 metre Schmidt, Japan 
+KOTTAMIA 		 Kottamia 74 inch 
+KPNO158 		 Kitt Peak 158 inch 
+KPNO36FT 		 Kitt Peak 36 foot 
+KPNO84 		 Kitt Peak 84 inch 
+KPNO90 		 Kitt Peak 90 inch 
+LICK120 		 Lick 120 inch 
+LOWELL72 		 Perkins 72 inch, Lowell 
+LPO1 		 Jacobus Kapteyn 1m Telescope 
+LPO2.5 		 Isaac Newton 2.5m Telescope 
+LPO4.2 		 William Herschel 4.2m Telescope 
+MAUNAK88 		 Mauna Kea 88 inch 
+MCDONLD2.1 		 McDonald 2.1 metre 
+MCDONLD2.7 		 McDonald 2.7 metre 
+MMT 		 MMT, Mt Hopkins 
+MOPRA 		 ATNF Mopra Observatory 
+MTEKAR 		 Mt Ekar 1.82 metre 
+MTHOP1.5 		 Mt Hopkins 1.5 metre 
+MTLEMMON60 		 Mt Lemmon 60 inch 
+NOBEYAMA 		 Nobeyama 45 metre 
+OKAYAMA 		 Okayama 1.88 metre 
+PALOMAR200 		 Palomar 200 inch 
+PALOMAR48 		 Palomar 48-inch Schmidt 
+PALOMAR60 		 Palomar 60 inch 
+PARKES 		 Parkes 64 metre 
+QUEBEC1.6 		 Quebec 1.6 metre 
+SAAO74 		 Sutherland 74 inch 
+SANPM83 		 San Pedro Martir 83 inch 
+ST.ANDREWS 		 St Andrews University Observatory 
+STEWARD90 		 Steward 90 inch 
+STROMLO74 		 Mount Stromlo 74 inch 
+SUBARU 		 Subaru 8 metre 
+SUGARGROVE 		 Sugar Grove 150 foot 
+TAUTNBG 		 Tautenburg 2 metre 
+TAUTSCHM 		 Tautenberg 1.34 metre Schmidt 
+TIDBINBLA 		 Tidbinbilla 64 metre 
+TOLOLO1.5M 		 Cerro Tololo 1.5 metre 
+TOLOLO4M 		 Cerro Tololo 4 metre 
+UKIRT 		 UK Infra Red Telescope 
+UKST 		 UK 1.2 metre Schmidt, Siding Spring 
+USSR6 		 USSR 6 metre 
+USSR600 		 USSR 600 foot 
+VLA 		 Very Large Array
+</TT></PRE></DL>
+<BR> <HR>
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+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node138.html b/src/slalib/sun67.htx/node138.html
new file mode 100644
index 0000000..d363298
--- /dev/null
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@@ -0,0 +1,116 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
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+<H2><A NAME="SECTION0004125000000000000000">&#160;</A><A NAME="xref_SLA_PA">&#160;</A><A NAME="SLA_PA">&#160;</A>
+<BR>
+SLA_PA - <IMG WIDTH="27" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img65.gif"
+ ALT="$h,\delta$"> to Parallactic Angle
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Hour angle and declination to parallactic angle
+(double precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>D&nbsp;=&nbsp;sla_PA (HA, DEC, PHI)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>HA</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>hour angle in radians (geocentric apparent)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DEC</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>declination in radians (geocentric apparent)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PHI</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>latitude in radians (geodetic)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_PA</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>parallactic angle (radians, in the range <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$">)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The parallactic angle at a point in the sky is the position
+angle of the vertical, <I>i.e.</I> the angle between the direction to
+the pole and to the zenith.  In precise applications care must
+        be taken only to use geocentric apparent <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$"> and to consider
+        separately the effects of atmospheric refraction and telescope
+        mount errors.
+  <DT>2.
+<DD>At the pole a zero result is returned.
+ </DL></DL>
+<BR> <HR>
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+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
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+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
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+<H2><A NAME="SECTION0004126000000000000000">SLA_PAV - Position-Angle Between Two Directions</A>
+<A NAME="xref_SLA_PAV">&#160;</A><A NAME="SLA_PAV">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Returns the bearing (position angle) of one celestial
+direction with respect to another (single precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>R&nbsp;=&nbsp;sla_PAV (V1, V2)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V1</EM></TD>
+<TH ALIGN="LEFT"><B>R(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>direction cosines of one point</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V2</EM></TD>
+<TD ALIGN="LEFT"><B>R(3)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>directions cosines of the other point</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_PAV</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>position-angle of 2nd point with respect to 1st</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The coordinate frames correspond to <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">,<IMG WIDTH="38" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img46.gif"
+ ALT="$[\lambda,\phi]$"> <I>etc.</I>.
+<DT>2.
+<DD>The result is the bearing (position angle), in radians,
+       of point V2 as seen
+       from point V1.  It is in the range <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$">.  The sense
+       is such that if V2
+       is a small distance due east of V1 the result
+       is about <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img14.gif"
+ ALT="$+\pi/2$">. Zero is returned
+       if the two points are coincident.
+ <DT>3.
+<DD>The routine sla_BEAR performs an equivalent function except
+       that the points are specified in the form of spherical coordinates.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1816" HREF="node140.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1814" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1808" HREF="node138.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1817" HREF="node140.html">SLA_PCD - Apply Radial Distortion</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1815" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1809" HREF="node138.html">SLA_PA - to Parallactic Angle</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node14.html b/src/slalib/sun67.htx/node14.html
new file mode 100644
index 0000000..9a2b861
--- /dev/null
+++ b/src/slalib/sun67.htx/node14.html
@@ -0,0 +1,112 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_ADDET - Add E-terms of Aberration</TITLE>
+<META NAME="description" CONTENT="SLA_ADDET - Add E-terms of Aberration">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node15.html">
+<LINK REL="previous" HREF="node13.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node15.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html566" HREF="node15.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html564" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html558" HREF="node13.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html567" HREF="node15.html">SLA_AFIN - Sexagesimal character string to angle</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html565" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html559" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION00041000000000000000">SLA_ADDET - Add E-terms of Aberration</A>
+<A NAME="xref_SLA_ADDET">&#160;</A><A NAME="SLA_ADDET">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Add the E-terms (elliptic component of annual aberration) to a
+pre IAU 1976 mean place to conform to the old catalogue convention.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_ADDET (RM, DM, EQ, RC, DC)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RM,DM</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> without E-terms (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EQ</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>Besselian epoch of mean equator and equinox</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RC,DC</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> with E-terms included (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTE:</STRONG>
+<DD>Most star positions from pre-1984 optical catalogues (or
+obtained by astrometry with respect to such stars) have the
+       E-terms built-in.  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 
+       <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> should be adjusted using this routine.
+      </DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD><I>Explanatory Supplement to the Astronomical Ephemeris</I>,
+section 2D, page 48.
+     </DL>
+<BR> <HR>
+<A NAME="tex2html566" HREF="node15.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html564" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html558" HREF="node13.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html567" HREF="node15.html">SLA_AFIN - Sexagesimal character string to angle</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html565" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html559" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node140.html b/src/slalib/sun67.htx/node140.html
new file mode 100644
index 0000000..aaf99dc
--- /dev/null
+++ b/src/slalib/sun67.htx/node140.html
@@ -0,0 +1,148 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_PCD - Apply Radial Distortion</TITLE>
+<META NAME="description" CONTENT="SLA_PCD - Apply Radial Distortion">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node141.html">
+<LINK REL="previous" HREF="node139.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node141.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1826" HREF="node141.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1824" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1818" HREF="node139.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1827" HREF="node141.html">SLA_PDA2H - H.A. for a Given Azimuth</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1825" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1819" HREF="node139.html">SLA_PAV - Position-Angle Between Two Directions</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004127000000000000000">SLA_PCD - Apply Radial Distortion</A>
+<A NAME="xref_SLA_PCD">&#160;</A><A NAME="SLA_PCD">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Apply pincushion/barrel distortion to a tangent-plane <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$">.<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_PCD (DISCO,X,Y)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DISCO</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>pincushion/barrel distortion coefficient</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>X,Y</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>tangent-plane <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"></TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>X,Y</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>distorted <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"></TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The distortion is of the form <IMG WIDTH="103" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img128.gif"
+ ALT="$\rho = r (1 + c r^{2})$">, where <I>r</I> is
+the radial distance from the tangent point, <I>c</I> is the DISCO
+argument, and <IMG WIDTH="11" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img129.gif"
+ ALT="$\rho$"> is the radial distance in the presence of
+        the distortion.
+  <DT>2.
+<DD>For <I>pincushion</I> distortion, C is +ve;  for
+        <I>barrel</I> distortion, C is -ve.
+  <DT>3.
+<DD>For X,Y in units of one projection radius (in the case of
+        a photographic plate, the focal length), the following
+        DISCO values apply:
+<P>        <BR>
+<BR>
+<BR>
+<P>        <TABLE CELLPADDING=3 BORDER="1">
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP>Geometry</TD>
+<TD ALIGN="CENTER" NOWRAP>DISCO</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP>astrograph</TD>
+<TD ALIGN="CENTER" NOWRAP>0.0</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP>Schmidt</TD>
+<TD ALIGN="CENTER" NOWRAP>-0.3333</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP>AAT PF doublet</TD>
+<TD ALIGN="CENTER" NOWRAP>+147.069</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP>AAT PF triplet</TD>
+<TD ALIGN="CENTER" NOWRAP>+178.585</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP>AAT f/8</TD>
+<TD ALIGN="CENTER" NOWRAP>+21.20</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP>JKT f/8</TD>
+<TD ALIGN="CENTER" NOWRAP>+14.6</TD>
+</TR>
+</TABLE>
+<P>        <BR>
+<BR>
+<BR>
+<P>  <DT>4.
+<DD>There is a companion routine, sla_UNPCD, which performs
+        an approximately inverse operation.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1826" HREF="node141.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1824" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1818" HREF="node139.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1827" HREF="node141.html">SLA_PDA2H - H.A. for a Given Azimuth</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1825" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1819" HREF="node139.html">SLA_PAV - Position-Angle Between Two Directions</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node141.html b/src/slalib/sun67.htx/node141.html
new file mode 100644
index 0000000..6e011b5
--- /dev/null
+++ b/src/slalib/sun67.htx/node141.html
@@ -0,0 +1,107 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_PDA2H - H.A. for a Given Azimuth</TITLE>
+<META NAME="description" CONTENT="SLA_PDA2H - H.A. for a Given Azimuth">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
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+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
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+<LINK REL="next" HREF="node142.html">
+<LINK REL="previous" HREF="node140.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node142.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1836" HREF="node142.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1834" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1828" HREF="node140.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1837" HREF="node142.html">SLA_PDQ2H - H.A. for a Given P.A.</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1835" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1829" HREF="node140.html">SLA_PCD - Apply Radial Distortion</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004128000000000000000">SLA_PDA2H - H.A. for a Given Azimuth</A>
+<A NAME="xref_SLA_PDA2H">&#160;</A><A NAME="SLA_PDA2H">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Hour Angle corresponding to a given azimuth (double precision).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_PDA2H (P, D, A, H1, J1, H2, J2)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>P</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>latitude</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>D</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>declination</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>azimuth</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>H1</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>hour angle:  first solution if any</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J1</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>flag: 0 = solution 1 is valid</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>H2</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>hour angle:  second solution if any</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J2</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>flag: 0 = solution 2 is valid</TD>
+</TR>
+</TABLE></DL>
+<BR> <HR>
+<A NAME="tex2html1836" HREF="node142.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1834" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1828" HREF="node140.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1837" HREF="node142.html">SLA_PDQ2H - H.A. for a Given P.A.</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1835" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1829" HREF="node140.html">SLA_PCD - Apply Radial Distortion</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node142.html b/src/slalib/sun67.htx/node142.html
new file mode 100644
index 0000000..f105cf4
--- /dev/null
+++ b/src/slalib/sun67.htx/node142.html
@@ -0,0 +1,108 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_PDQ2H - H.A. for a Given P.A.</TITLE>
+<META NAME="description" CONTENT="SLA_PDQ2H - H.A. for a Given P.A.">
+<META NAME="keywords" CONTENT="sun67">
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+<BODY >
+<BR> <HR>
+<A NAME="tex2html1846" HREF="node143.html">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1847" HREF="node143.html">SLA_PERMUT - Next Permutation</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1845" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1839" HREF="node141.html">SLA_PDA2H - H.A. for a Given Azimuth</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004129000000000000000">SLA_PDQ2H - H.A. for a Given P.A.</A>
+<A NAME="xref_SLA_PDQ2H">&#160;</A><A NAME="SLA_PDQ2H">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Hour Angle corresponding to a given parallactic angle
+(double precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_PDQ2H (P, D, Q, H1, J1, H2, J2)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>P</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>latitude</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>D</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>declination</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>Q</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>azimuth</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>H1</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>hour angle:  first solution if any</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J1</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>flag: 0 = solution 1 is valid</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>H2</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>hour angle:  second solution if any</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J2</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>flag: 0 = solution 2 is valid</TD>
+</TR>
+</TABLE></DL>
+<BR> <HR>
+<A NAME="tex2html1846" HREF="node143.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1844" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1838" HREF="node141.html">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1847" HREF="node143.html">SLA_PERMUT - Next Permutation</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1845" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1839" HREF="node141.html">SLA_PDA2H - H.A. for a Given Azimuth</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node143.html b/src/slalib/sun67.htx/node143.html
new file mode 100644
index 0000000..46f3e9e
--- /dev/null
+++ b/src/slalib/sun67.htx/node143.html
@@ -0,0 +1,133 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_PERMUT - Next Permutation</TITLE>
+<META NAME="description" CONTENT="SLA_PERMUT - Next Permutation">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
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+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1857" HREF="node144.html">SLA_PERTEL - Perturbed Orbital Elements</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1855" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1849" HREF="node142.html">SLA_PDQ2H - H.A. for a Given P.A.</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004130000000000000000">SLA_PERMUT - Next Permutation</A>
+<A NAME="xref_SLA_PERMUT">&#160;</A><A NAME="SLA_PERMUT">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Generate the next permutation of a specified number of items.
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_PERMUT (N, ISTATE, IORDER, J)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>N</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>number of items:  there will be N! permutations</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ISTATE</EM></TD>
+<TD ALIGN="LEFT"><B>I(N)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>state, ISTATE(1)=-1 to initialize</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ISTATE</EM></TD>
+<TH ALIGN="LEFT"><B>I(N)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>state, updated ready for next time</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IORDER</EM></TD>
+<TD ALIGN="LEFT"><B>I(N)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>next permutation of numbers 1,2,...,N</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -1 = illegal N (zero or less is illegal)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>     0 = OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  +1 = no more permutations available</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>This routine returns, in the IORDER array, the integers 1 to N
+inclusive, in an order that depends on the current contents of
+the ISTATE array.  Before calling the routine for the first
+        time, the caller must set the first element of the ISTATE array
+        to -1 (any negative number will do) to cause the ISTATE array
+        to be fully initialized.
+  <DT>2.
+<DD>The first permutation to be generated is:
+        <BLOCKQUOTE>IORDER(1)=N, IORDER(2)=N-1, ..., IORDER(N)=1
+        </BLOCKQUOTE>
+        This is also the permutation returned for the ``finished'' (J=1) case.
+        The final permutation to be generated is:
+        <BLOCKQUOTE>IORDER(1)=1, IORDER(2)=2, ..., IORDER(N)=N
+        </BLOCKQUOTE>
+  <DT>3.
+<DD>If the ``finished'' (J=1) status is ignored, the routine continues
+        to deliver permutations, the pattern repeating every&nbsp;N!&nbsp;calls.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1856" HREF="node144.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1854" HREF="node13.html">
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+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1857" HREF="node144.html">SLA_PERTEL - Perturbed Orbital Elements</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1855" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1849" HREF="node142.html">SLA_PDQ2H - H.A. for a Given P.A.</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node144.html b/src/slalib/sun67.htx/node144.html
new file mode 100644
index 0000000..eb511e6
--- /dev/null
+++ b/src/slalib/sun67.htx/node144.html
@@ -0,0 +1,310 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_PERTEL - Perturbed Orbital Elements</TITLE>
+<META NAME="description" CONTENT="SLA_PERTEL - Perturbed Orbital Elements">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
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+<LINK REL="previous" HREF="node143.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node145.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1866" HREF="node145.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1864" HREF="node13.html">
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+<A NAME="tex2html1858" HREF="node143.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1867" HREF="node145.html">SLA_PERTUE - Perturbed Universal Elements</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1865" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1859" HREF="node143.html">SLA_PERMUT - Next Permutation</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004131000000000000000">SLA_PERTEL - Perturbed Orbital Elements</A>
+<A NAME="xref_SLA_PERTEL">&#160;</A><A NAME="SLA_PERTEL">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Update the osculating elements of an asteroid or comet by
+applying planetary perturbations.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_PERTEL (
+         JFORM, DATE0, DATE1,
+         EPOCH0, ORBI0, ANODE0, PERIH0, AORQ0, E0, AM0,
+         EPOCH1, ORBI1, ANODE1, PERIH1, AORQ1, E1, AM1,
+         JSTAT)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN (format and dates):</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JFORM</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>choice of element set (2 or 3; Note&nbsp;1)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE0</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>date of osculation (TT MJD) for the given</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  elements</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE1</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>date of osculation (TT MJD) for the updated</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  elements</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>GIVEN (the unperturbed elements):</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EPOCH0</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>epoch of the given element set
+(<I>t<SUB>0</SUB></I> or <I>T</I>, TT MJD;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  Note&nbsp;2)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ORBI0</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>inclination (<I>i</I>, radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ANODE0</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>longitude of the ascending node (<IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$">, radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PERIH0</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>argument of perihelion
+(<IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$">, radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AORQ0</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>mean distance or perihelion distance (<I>a</I> or <I>q</I>, AU)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>E0</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>eccentricity (<I>e</I>)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AM0</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>mean anomaly (<I>M</I>, radians, JFORM=2 only)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED (the updated elements):</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EPOCH1</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>epoch of the updated element set
+(<I>t<SUB>0</SUB></I> or <I>T</I>,</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  TT MJD; Note&nbsp;2)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ORBI1</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>inclination (<I>i</I>, radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ANODE1</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>longitude of the ascending node (<IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$">, radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PERIH1</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>argument of perihelion
+(<IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$">, radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AORQ1</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>mean distance or perihelion distance (<I>a</I> or <I>q</I>, AU)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>E1</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>eccentricity (<I>e</I>)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AM1</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>mean anomaly (<I>M</I>, radians, JFORM=2 only)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED (status flag):</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JSTAT</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP> +102 = warning, distant epoch</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP> +101 = warning, large timespan
+(&gt;100 years)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP> +1 to +8 = coincident with major planet
+(Note&nbsp;6)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>        0 = OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>     -1 = illegal JFORM</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>     -2 = illegal E0</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>     -3 = illegal AORQ0</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>     -4 = internal error</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>     -5 = numerical error</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Two different element-format options are supported, as follows. <BR>
+JFORM=2, suitable for minor planets:
+<PRE><TT>
+ 		 EPOCH 		 = 		 epoch of elements <I>t<SUB>0</SUB></I> (TT MJD)
+		 ORBINC 		 = 		 inclination <I>i</I> (radians)
+		 ANODE 		 = 		 longitude of the ascending node <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> (radians)
+		 PERIH 		 = 		 argument of perihelion <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$"> (radians)
+		 AORQ 		 = 		 mean distance <I>a</I> (AU)
+		 E 		 = 		 eccentricity <I>e</I> <IMG WIDTH="83" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img106.gif"
+ ALT="$( 0 \leq e < 1 )$"> 
+		 AORL 		 = 		 mean anomaly <I>M</I> (radians)        
+</TT></PRE>
+<P>
+JFORM=3, suitable for comets:
+<P>        <PRE><TT>
+ 		 EPOCH 		 = 		 epoch of perihelion <I>T</I> (TT MJD)
+		 ORBINC 		 = 		 inclination <I>i</I> (radians)
+		 ANODE 		 = 		 longitude of the ascending node <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> (radians)
+		 PERIH 		 = 		 argument of perihelion <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$"> (radians)
+		 AORQ 		 = 		 perihelion distance <I>q</I> (AU)
+		 E 		 = 		 eccentricity <I>e</I> <IMG WIDTH="91" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img107.gif"
+ ALT="$( 0 \leq e \leq 10 )$"></TT></PRE>
+ <DT>2.
+<DD>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).
+       <UL>
+<LI> DATE0 is the instant at which the given
+             (<I>i.e.</I> unperturbed) osculating elements are correct.
+<LI> DATE1 is the specified instant at which the updated osculating
+             elements are correct.
+<LI> 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.
+       </UL>
+ <DT>3.
+<DD>The elements are with respect to the J2000 ecliptic and mean equinox.
+ <DT>4.
+<DD>Unused elements (AM0 and AM1 for JFORM=3) are not accessed.
+ <DT>5.
+<DD>See the sla_PERTUE routine for details of the algorithm used.
+ <DT>6.
+<DD>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&nbsp;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 (Mercury=1,...,Neptune=8) as a warning.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Sterne, Theodore E., <I>An Introduction to Celestial Mechanics,</I>
+Interscience Publishers, 1960.  Section 6.7, p199.
+     </DL>
+<BR> <HR>
+<A NAME="tex2html1866" HREF="node145.html">
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+<B> Next:</B> <A NAME="tex2html1867" HREF="node145.html">SLA_PERTUE - Perturbed Universal Elements</A>
+<BR>
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+<BR>
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+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node145.html b/src/slalib/sun67.htx/node145.html
new file mode 100644
index 0000000..8fbb853
--- /dev/null
+++ b/src/slalib/sun67.htx/node145.html
@@ -0,0 +1,279 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
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+<TITLE>SLA_PERTUE - Perturbed Universal Elements</TITLE>
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+<BR>
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+<BR>
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+<BR>
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+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004132000000000000000">SLA_PERTUE - Perturbed Universal Elements</A>
+<A NAME="xref_SLA_PERTUE">&#160;</A><A NAME="SLA_PERTUE">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Update the universal elements of an asteroid or comet by
+applying planetary perturbations.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_PERTUE (DATE, U, JSTAT)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE1</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>final epoch (TT MJD) for the updated elements</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>GIVEN and RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>U</EM></TD>
+<TH ALIGN="LEFT"><B>D(13)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>universal elements (updated in place)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(1)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>combined mass (<I>M</I>+<I>m</I>)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(2)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>total energy of the orbit (<IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$">)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(3)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>reference (osculating) epoch (<I>t<SUB>0</SUB></I>)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(4-6)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>position at reference epoch (<IMG WIDTH="17" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img102.gif"
+ ALT="${\rm \bf r}_0$">)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(7-9)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>velocity at reference epoch (<IMG WIDTH="19" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img103.gif"
+ ALT="${\rm \bf v}_0$">)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(10)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>heliocentric distance at reference epoch</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(11)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img104.gif"
+ ALT="${\rm \bf r}_0.{\rm \bf v}_0$"></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(12)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>date (<I>t</I>)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(13)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>universal eccentric anomaly (<IMG WIDTH="14" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img105.gif"
+ ALT="$\psi$">) of date, approx</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JSTAT</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP> +102 = warning, distant epoch</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP> +101 = warning, large timespan
+(&gt;100 years)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP> +1 to +8 = coincident with major planet
+(Note&nbsp;5)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>        0 = OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>     -1 = numerical error</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>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)&nbsp;<IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$">, which is proportional to the total energy of the
+        orbit, (ii)&nbsp;the heliocentric distance at epoch,
+        (iii)&nbsp;the outwards component of the velocity at the given epoch,
+        (iv)&nbsp;an estimate of <IMG WIDTH="14" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img105.gif"
+ ALT="$\psi$">, the ``universal eccentric anomaly'' at a
+        given date and (v)&nbsp;that date.
+  <DT>2.
+<DD>The universal elements are with respect to the J2000 equator and
+        equinox.
+  <DT>3.
+<DD>The epochs DATE, U(3) and U(12) are all Modified Julian Dates
+        (JD-2400000.5).
+  <DT>4.
+<DD>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.
+<P>
+The <I>f</I>(<I>q</I>) 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.
+<P>
+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.
+<P>
+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.
+<P>
+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.
+<P>
+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 sla_PLANET.  Two
+        levels of interpolation are used, to enhance speed without
+        significantly degrading accuracy.  At a low frequency, the routine
+        sla_PLANET is called to generate updated position+velocity ``state
+        vectors''.  The only task remaining to be carried out at the full
+        frequency (<I>i.e.</I> 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.
+<P>
+Various other approximations are made.  For example, perturbations
+        by Pluto and the minor planets are neglected, relativistic effects
+        are not taken into account and the Earth-Moon system is treated as
+        a single body.
+<P>
+In the interests of simplicity, the background calculations for
+        the major planets are carried out <I>en masse.</I>
+        The mean elements and
+        state vectors for all the planets are refreshed at the same time,
+        without regard for orbit curvature, mass or proximity.
+<P>  <DT>5.
+<DD>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&nbsp;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 (Mercury=1,...,Neptune=8) as a warning.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Sterne, Theodore E., <I>An Introduction to Celestial Mechanics,</I>
+Interscience Publishers, 1960.  Section 6.7, p199.
+<DT>2.
+<DD>Everhart, E. &amp; Pitkin, E.T., Am.&nbsp;J.&nbsp;Phys.&nbsp;51, 712, 1983.
+   </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1876" HREF="node146.html">
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+ SRC="contents_motif.gif"></A>
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+<B> Next:</B> <A NAME="tex2html1877" HREF="node146.html">SLA_PLANEL - Planet Position from Elements</A>
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+<BR>
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+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node146.html b/src/slalib/sun67.htx/node146.html
new file mode 100644
index 0000000..70b9139
--- /dev/null
+++ b/src/slalib/sun67.htx/node146.html
@@ -0,0 +1,255 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_PLANEL - Planet Position from Elements</TITLE>
+<META NAME="description" CONTENT="SLA_PLANEL - Planet Position from Elements">
+<META NAME="keywords" CONTENT="sun67">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1887" HREF="node147.html">SLA_PLANET - Planetary Ephemerides</A>
+<BR>
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+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004133000000000000000">SLA_PLANEL - Planet Position from Elements</A>
+<A NAME="xref_SLA_PLANEL">&#160;</A><A NAME="SLA_PLANEL">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Heliocentric position and velocity of a planet,
+asteroid or comet, starting from orbital elements.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_PLANEL (
+         DATE, JFORM, EPOCH, ORBINC, ANODE, PERIH,
+         AORQ, E, AORL, DM, PV, JSTAT)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>Modified Julian Date (JD-2400000.5)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JFORM</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>choice of element set (1-3, see Note&nbsp;3, below)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EPOCH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>epoch of elements (<I>t<SUB>0</SUB></I> or <I>T</I>, TT MJD)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ORBINC</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>inclination (<I>i</I>, radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ANODE</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>longitude of the ascending node (<IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$">, radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PERIH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>longitude or argument of perihelion
+(<IMG WIDTH="16" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img100.gif"
+ ALT="$\varpi$"> or <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$">,</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AORQ</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>mean distance or perihelion distance (<I>a</I> or <I>q</I>, AU)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>E</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>eccentricity (<I>e</I>)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AORL</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>mean anomaly or longitude
+(<I>M</I> or <I>L</I>, radians,</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  JFORM=1,2 only)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DM</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>daily motion (<I>n</I>, radians, JFORM=1 only)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PV</EM></TD>
+<TH ALIGN="LEFT"><B>D(6)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>heliocentric <IMG WIDTH="106" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img51.gif"
+ ALT="$[\,x,y,z,\dot{x},\dot{y},\dot{z}\,]$">, equatorial, J2000</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  (AU, AU/s)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JSTAT</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>     0 = OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -1 = illegal JFORM</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -2 = illegal E</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -3 = illegal AORQ</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -4 = illegal DM</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -5 = numerical error</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>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).
+  <DT>2.
+<DD>The elements are with respect to
+        the J2000 ecliptic and equinox.
+  <DT>3.
+<DD>Three different element-format options are available, as
+        follows. <BR>
+<P>
+JFORM=1, suitable for the major planets:
+<P>        <PRE><TT>
+ 		 EPOCH 		 = 		 epoch of elements <I>t<SUB>0</SUB></I> (TT MJD)
+		 ORBINC 		 = 		 inclination <I>i</I> (radians)
+		 ANODE 		 = 		 longitude of the ascending node <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> (radians)
+		 PERIH 		 = 		 longitude of perihelion <IMG WIDTH="16" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img100.gif"
+ ALT="$\varpi$"> (radians)
+		 AORQ 		 = 		 mean distance <I>a</I> (AU)
+		 E 		 = 		 eccentricity <I>e</I> <IMG WIDTH="83" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img106.gif"
+ ALT="$( 0 \leq e < 1 )$"> 
+		 AORL 		 = 		 mean longitude <I>L</I> (radians)
+		 DM 		 = 		 daily motion <I>n</I> (radians)        
+</TT></PRE>
+<P>
+JFORM=2, suitable for minor planets:
+<P>        <PRE><TT>
+ 		 EPOCH 		 = 		 epoch of elements <I>t<SUB>0</SUB></I> (TT MJD)
+		 ORBINC 		 = 		 inclination <I>i</I> (radians)
+		 ANODE 		 = 		 longitude of the ascending node <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> (radians)
+		 PERIH 		 = 		 argument of perihelion <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$"> (radians)
+		 AORQ 		 = 		 mean distance <I>a</I> (AU)
+		 E 		 = 		 eccentricity <I>e</I> <IMG WIDTH="83" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img106.gif"
+ ALT="$( 0 \leq e < 1 )$"> 
+		 AORL 		 = 		 mean anomaly <I>M</I> (radians)        
+</TT></PRE>
+<P>
+JFORM=3, suitable for comets:
+<P>        <PRE><TT>
+ 		 EPOCH 		 = 		 epoch of perihelion <I>T</I> (TT MJD)
+		 ORBINC 		 = 		 inclination <I>i</I> (radians)
+		 ANODE 		 = 		 longitude of the ascending node <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> (radians)
+		 PERIH 		 = 		 argument of perihelion <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$"> (radians)
+		 AORQ 		 = 		 perihelion distance <I>q</I> (AU)
+		 E 		 = 		 eccentricity <I>e</I> <IMG WIDTH="91" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img107.gif"
+ ALT="$( 0 \leq e \leq 10 )$"></TT></PRE>
+  <DT>4.
+<DD>Unused elements (DM for JFORM=2, AORL and DM for JFORM=3) are
+        not accessed.
+  <DT>5.
+<DD>The reference frame for the result is equatorial and is with
+        respect to the mean equinox and ecliptic of epoch J2000.
+  <DT>6.
+<DD>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.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Everhart, E. &amp; Pitkin, E.T., Am.&nbsp;J.&nbsp;Phys.&nbsp;51, 712, 1983.
+</DL>
+<BR> <HR>
+<A NAME="tex2html1886" HREF="node147.html">
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+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
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+<H2><A NAME="SECTION0004134000000000000000">SLA_PLANET - Planetary Ephemerides</A>
+<A NAME="xref_SLA_PLANET">&#160;</A><A NAME="SLA_PLANET">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Approximate heliocentric position and velocity of a planet.
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_PLANET (DATE, NP, PV, JSTAT)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>Modified Julian Date (JD-2400000.5)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NP</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>planet:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  1=Mercury</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  2=Venus</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  3=Earth-Moon Barycentre</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  4=Mars</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  5=Jupiter</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  6=Saturn</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  7=Uranus</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  8=Neptune</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  9=Pluto</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PV</EM></TD>
+<TH ALIGN="LEFT"><B>D(6)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>heliocentric <IMG WIDTH="106" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img51.gif"
+ ALT="$[\,x,y,z,\dot{x},\dot{y},\dot{z}\,]$">, equatorial, J2000</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  (AU, AU/s)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JSTAT</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  +1 = warning: date outside of range</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>     0 = OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -1 = illegal NP (outside 1-9)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -2 = solution didn't converge</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The epoch, DATE, is in the TDB timescale and is in the form
+of a Modified Julian Date (JD-2400000.5).
+<DT>2.
+<DD>The reference frame is equatorial and is with respect to
+        the mean equinox and ecliptic of epoch J2000.
+  <DT>3.
+<DD>If a planet number, NP, outside the range 1-9 is supplied, an error
+        status is returned (JSTAT&nbsp;=&nbsp;-1) and the PV vector
+        is set to zeroes.
+  <DT>4.
+<DD>The algorithm for obtaining the mean elements of the
+        planets from Mercury to Neptune is due to
+        J.L.Simon, P.Bretagnon, J.Chapront,
+        M.Chapront-Touze, G.Francou and J.Laskar (Bureau des
+        Longitudes, Paris, France).  The (completely different)
+        algorithm for calculating the ecliptic coordinates of
+        Pluto is by Meeus.
+  <DT>5.
+<DD>Comparisons of the present routine with the JPL DE200 ephemeris
+        give the following RMS errors over the interval 1960-2025:
+        <PRE><TT>
+ 		 		 <I>position (km)</I> 		 <I>speed (metre/sec)</I> 
+&nbsp;
+		 Mercury 		  334 		  0.437
+		 Venus 		  1060 		  0.855
+		 EMB 		  2010 		  0.815
+		 Mars 		  7690 		  1.98
+		 Jupiter 		  71700 		  7.70
+		 Saturn 		  199000 		  19.4
+		 Uranus 		  564000 		  16.4
+		 Neptune 		  158000 		  14.4
+		 Pluto 		  36400 		  0.137        
+</TT></PRE>
+        From comparisons with DE102, Simon <I>et al.</I> quote the following
+        longitude accuracies over the interval 1800-2200:
+        <PRE><TT>
+ 		 Mercury 		  <IMG WIDTH="17" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img130.gif"
+ ALT="$4\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> 
+		 Venus 		  <IMG WIDTH="17" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img131.gif"
+ ALT="$5\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> 
+		 EMB 		  <IMG WIDTH="17" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img132.gif"
+ ALT="$6\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> 
+		 Mars 		 <IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img133.gif"
+ ALT="$17\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> 
+		 Jupiter 		 <IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img134.gif"
+ ALT="$71\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> 
+		 Saturn 		 <IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img135.gif"
+ ALT="$81\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> 
+		 Uranus 		 <IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img136.gif"
+ ALT="$86\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> 
+		 Neptune 		 <IMG WIDTH="25" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img43.gif"
+ ALT="$11\hspace{-0.05em}^{'\hspace{-0.1em}'}$"></TT></PRE>
+        In the case of Pluto, Meeus quotes an accuracy of 
+      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img137.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.6$"><P>
+in longitude and 
+      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img76.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.2$">    in latitude for the period
+        1885-2099.
+<P>
+For all except Pluto, over the period 1000-3000,
+        the accuracy is better than 1.5
+        times that over 1800-2200.  Outside the interval 1000-3000 the
+        accuracy declines.  For Pluto the accuracy declines rapidly
+        outside the period 1885-2099.  Outside these ranges
+        (1885-2099 for Pluto, 1000-3000 for the rest) a ``date out
+        of range'' warning status (<TT>JSTAT=+1</TT>) is returned.
+  <DT>6.
+<DD>The algorithms for (i)&nbsp;Mercury through Neptune and
+        (ii)&nbsp;Pluto are completely independent.  In the Mercury
+        through Neptune case, the present SLALIB
+        implementation differs from the original
+        Simon <I>et al.</I> Fortran code in the following respects:
+        <UL>
+<LI> The date is supplied as a Modified Julian Date rather
+               a Julian Date (<IMG WIDTH="177" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img138.gif"
+ ALT="${\rm MJD} = ({\rm JD} - 2400000.5$">).
+<LI> The result is returned only in equatorial
+               Cartesian form;  the ecliptic
+               longitude, latitude and radius vector are not returned.
+<LI> The velocity is in AU per second, not AU per day.
+<LI> Different error/warning status values are used.
+<LI> Kepler's Equation is not solved inline.
+<LI> Polynomials in T are nested to minimize rounding errors.
+<LI> Explicit double-precision constants are used to avoid
+               mixed-mode expressions.
+<LI> There are other, cosmetic, changes to comply with
+               Starlink/SLALIB style guidelines.
+        </UL>
+        None of the above changes affects the result significantly.
+  <DT>7.
+<DD>NP=3 the result is for the Earth-Moon Barycentre.  To
+        obtain the heliocentric position and velocity of the Earth,
+        either use the SLALIB routine sla_EVP or call sla_DMOON and
+        subtract 0.012150581 times the geocentric Moon vector from
+        the EMB vector produced by the present routine.  (The Moon
+        vector should be precessed to J2000 first, but this can
+        be omitted for modern epochs without introducing significant
+        inaccuracy.)
+ </DL>
+<P>     <DL>
+<DT><STRONG>REFERENCES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Simon <I>et al.,</I>
+Astron. Astrophys. <B>282</B>, 663 (1994).
+<DT>2.
+<DD>Meeus, J.,
+        <I>Astronomical Algorithms,</I> Willmann-Bell (1991).
+ </DL></DL></DL>
+<BR> <HR>
+<A NAME="tex2html1896" HREF="node148.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1897" HREF="node148.html">SLA_PLANTE - of Planet from Elements</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1895" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1889" HREF="node146.html">SLA_PLANEL - Planet Position from Elements</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node148.html b/src/slalib/sun67.htx/node148.html
new file mode 100644
index 0000000..70ca411
--- /dev/null
+++ b/src/slalib/sun67.htx/node148.html
@@ -0,0 +1,256 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
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+<TITLE>SLA_PLANTE - of Planet from Elements</TITLE>
+<META NAME="description" CONTENT="SLA_PLANTE - of Planet from Elements">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1907" HREF="node149.html">SLA_PM - Proper Motion</A>
+<BR>
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+<BR>
+<B> Previous:</B> <A NAME="tex2html1899" HREF="node147.html">SLA_PLANET - Planetary Ephemerides</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004135000000000000000">&#160;</A><A NAME="xref_SLA_PLANTE">&#160;</A><A NAME="SLA_PLANTE">&#160;</A>
+<BR>
+SLA_PLANTE - <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> of Planet from Elements
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Topocentric apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> of a Solar-System object whose
+heliocentric orbital elements are known.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_PLANTE (
+         DATE, ELONG, PHI, JFORM, EPOCH, ORBINC, ANODE, PERIH,
+         AORQ, E, AORL, DM, RA, DEC, R, JSTAT)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>MJD of observation (JD-2400000.5)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ELONG,PHI</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>observer's longitude (east +ve) and latitude</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JFORM</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>choice of element set (1-3, see Note&nbsp;4, below)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EPOCH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>epoch of elements (<I>t<SUB>0</SUB></I> or <I>T</I>, TT MJD)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ORBINC</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>inclination (<I>i</I>, radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ANODE</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>longitude of the ascending node (<IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$">, radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PERIH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>longitude or argument of perihelion
+(<IMG WIDTH="16" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img100.gif"
+ ALT="$\varpi$"> or <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$">,</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AORQ</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>mean distance or perihelion distance (<I>a</I> or <I>q</I>, AU)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>E</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>eccentricity (<I>e</I>)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AORL</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>mean anomaly or longitude (<I>M</I> or <I>L</I>,</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  radians, JFORM=1,2 only)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DM</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>daily motion (<I>n</I>, radians, JFORM=1 only)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RA,DEC</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>topocentric apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>R</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>distance from observer (AU)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JSTAT</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>     0 = OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -1 = illegal JFORM</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -2 = illegal E</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -3 = illegal AORQ</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -4 = illegal DM</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -5 = numerical error</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>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).
+  <DT>2.
+<DD>The longitude and latitude allow correction for geocentric
+        parallax.  This is usually a small effect, but can become
+        important for Earth-crossing asteroids.  Geocentric positions
+        can be generated by appropriate use of the routines
+        sla_EVP and sla_PLANEL.
+  <DT>3.
+<DD>The elements are with respect to the J2000 ecliptic and equinox.
+  <DT>4.
+<DD>Three different element-format options are available, as
+        follows. <BR>
+<P>
+JFORM=1, suitable for the major planets:
+<P>        <PRE><TT>
+ 		 EPOCH 		 = 		 epoch of elements <I>t<SUB>0</SUB></I> (TT MJD)
+		 ORBINC 		 = 		 inclination <I>i</I> (radians)
+		 ANODE 		 = 		 longitude of the ascending node <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> (radians)
+		 PERIH 		 = 		 longitude of perihelion <IMG WIDTH="16" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img100.gif"
+ ALT="$\varpi$"> (radians)
+		 AORQ 		 = 		 mean distance <I>a</I> (AU)
+		 E 		 = 		 eccentricity <I>e</I> 
+		 AORL 		 = 		 mean longitude <I>L</I> (radians)
+		 DM 		 = 		 daily motion <I>n</I> (radians)        
+</TT></PRE>
+<P>
+JFORM=2, suitable for minor planets:
+<P>        <PRE><TT>
+ 		 EPOCH 		 = 		 epoch of elements <I>t<SUB>0</SUB></I> (TT MJD)
+		 ORBINC 		 = 		 inclination <I>i</I> (radians)
+		 ANODE 		 = 		 longitude of the ascending node <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> (radians)
+		 PERIH 		 = 		 argument of perihelion <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$"> (radians)
+		 AORQ 		 = 		 mean distance <I>a</I> (AU)
+		 E 		 = 		 eccentricity <I>e</I> 
+		 AORL 		 = 		 mean anomaly <I>M</I> (radians)        
+</TT></PRE>
+<P>
+JFORM=3, suitable for comets:
+<P>        <PRE><TT>
+ 		 EPOCH 		 = 		 epoch of perihelion <I>T</I> (TT MJD)
+		 ORBINC 		 = 		 inclination <I>i</I> (radians)
+		 ANODE 		 = 		 longitude of the ascending node <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> (radians)
+		 PERIH 		 = 		 argument of perihelion <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$"> (radians)
+		 AORQ 		 = 		 perihelion distance <I>q</I> (AU)
+		 E 		 = 		 eccentricity <I>e</I>
+</TT></PRE>
+  <DT>5.
+<DD>Unused elements (DM for JFORM=2, AORL and DM for JFORM=3) are
+        not accessed.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1906" HREF="node149.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1907" HREF="node149.html">SLA_PM - Proper Motion</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1905" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1899" HREF="node147.html">SLA_PLANET - Planetary Ephemerides</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node149.html b/src/slalib/sun67.htx/node149.html
new file mode 100644
index 0000000..999078a
--- /dev/null
+++ b/src/slalib/sun67.htx/node149.html
@@ -0,0 +1,135 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_PM - Proper Motion</TITLE>
+<META NAME="description" CONTENT="SLA_PM - Proper Motion">
+<META NAME="keywords" CONTENT="sun67">
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+<BR> <HR>
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+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1917" HREF="node150.html">SLA_POLMO - Polar Motion</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1915" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1909" HREF="node148.html">SLA_PLANTE - of Planet from Elements</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004136000000000000000">SLA_PM - Proper Motion</A>
+<A NAME="xref_SLA_PM">&#160;</A><A NAME="SLA_PM">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Apply corrections for proper motion to a star <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">.<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_PM (R0, D0, PR, PD, PX, RV, EP0, EP1, R1, D1)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>R0,D0</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> at epoch EP0 (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PR,PD</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>proper motions:  rate of change of 
+<IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">  (radians per year)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PX</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>parallax (arcsec)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RV</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>radial velocity (km&nbsp;s<SUP>-1</SUP>, +ve if receding)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EP0</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>start epoch in years (<I>e.g.</I> Julian epoch)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EP1</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>end epoch in years (same system as EP0)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>R1,D1</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> at epoch EP1 (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTE:</STRONG>
+<DD>The <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> proper motions are <IMG WIDTH="13" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img115.gif"
+ ALT="$\dot{\alpha}$"> rather than
+<IMG WIDTH="48" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img116.gif"
+ ALT="$\dot{\alpha}\cos\delta$">, and are in the same coordinate
+       system as R0,D0.
+      </DL>
+<P>     <DL>
+<DT><STRONG>REFERENCES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>1984 <I>Astronomical Almanac</I>, pp B39-B41.
+<DT>2.
+<DD>Lederle &amp; Schwan, 1984. <I>Astr. Astrophys.</I> <B>134</B>, 1-6.
+</DL></DL>
+<BR> <HR>
+<A NAME="tex2html1916" HREF="node150.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1914" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
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+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1917" HREF="node150.html">SLA_POLMO - Polar Motion</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1915" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1909" HREF="node148.html">SLA_PLANTE - of Planet from Elements</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node15.html b/src/slalib/sun67.htx/node15.html
new file mode 100644
index 0000000..45c1aeb
--- /dev/null
+++ b/src/slalib/sun67.htx/node15.html
@@ -0,0 +1,230 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_AFIN - Sexagesimal character string to angle</TITLE>
+<META NAME="description" CONTENT="SLA_AFIN - Sexagesimal character string to angle">
+<META NAME="keywords" CONTENT="sun67">
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+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION00042000000000000000">SLA_AFIN - Sexagesimal character string to angle</A>
+<A NAME="xref_SLA_AFIN">&#160;</A><A NAME="SLA_AFIN">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Decode a free-format sexagesimal string (degrees, arcminutes,
+arcseconds) into a single precision floating point
+         number (radians).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_AFIN (STRING, NSTRT, RESLT, JF)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>STRING</EM></TD>
+<TH ALIGN="LEFT"><B>C*(*)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>string containing deg, arcmin, arcsec fields</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NSTRT</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>pointer to start of decode (beginning of STRING = 1)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NSTRT</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>advanced past the decoded angle</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RESLT</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>angle in radians</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JF</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>    0 = OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  +1 = default, RESLT unchanged (note 2)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -1 = bad degrees (note 3)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -2 = bad arcminutes (note 3)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -3 = bad arcseconds (note 3)</TD>
+</TR>
+</TABLE></DL>
+<P><DL>
+<DT><STRONG>EXAMPLE:</STRONG>
+<DD>
+<BR>
+<BR>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TH ALIGN="LEFT"><I>argument</I></TH>
+<TH ALIGN="LEFT"><I>before</I></TH>
+<TH ALIGN="LEFT"><I>after</I></TH>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT">&nbsp;</TD>
+<TD ALIGN="LEFT">&nbsp;</TD>
+<TD ALIGN="LEFT">&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT">STRING</TD>
+<TD ALIGN="LEFT">'<code>-57 17 44.806  12 34 56.7</code>'</TD>
+<TD ALIGN="LEFT">unchanged</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT">NSTRT</TD>
+<TD ALIGN="LEFT">1</TD>
+<TD ALIGN="LEFT">16 (<I>i.e.</I> pointing to 12...)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT">RESLT</TD>
+<TD ALIGN="LEFT">-</TD>
+<TD ALIGN="LEFT">-1.00000</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT">JF</TD>
+<TD ALIGN="LEFT">-</TD>
+<TD ALIGN="LEFT">&nbsp;</TD>
+</TR>
+</TABLE>
+ <DT><DD> A further call to sla_AFIN, without adjustment of NSTRT, will
+       decode the second angle, <IMG WIDTH="90" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img4.gif"
+ ALT="$12^{\circ}\,34^{'}\,56^{''}.7$">.</DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>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 sla_DFLTIN routine and is free-format.
+  <DT>2.
+<DD>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 RESLT is
+   unchanged.  In all other cases RESLT is changed.
+  <DT>3.
+<DD>Range checking:
+   <UL>
+<LI> The degrees field is not range checked.  However, it is
+     expected to be integral unless the other two fields are absent.
+<LI> 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...
+<LI> The arcseconds field is expected to be 0-59.9999...
+<LI> Decoding continues even when a check has failed.  Under these
+     circumstances the field takes the supplied value, defaulting to
+     zero, and the result RESLT is computed and returned.
+   </UL>
+   <DT>4.
+<DD>Further fields after the three expected ones are not treated as
+    an error.  The pointer NSTRT is left in the correct state for
+    further decoding with the present routine or with sla_DFLTIN
+    <I>etc</I>.  See the example, above.
+   <DT>5.
+<DD>If STRING contains hours, minutes, seconds instead of
+    degrees <I>etc</I>,
+    or if the required units are turns (or days) instead of radians,
+    the result RESLT should be multiplied as follows: <BR>
+<BR>
+<BR>
+    <TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TH ALIGN="LEFT"><I>for STRING</I></TH>
+<TH ALIGN="LEFT"><I>to obtain</I></TH>
+<TH ALIGN="LEFT"><I>multiply RESLT by</I></TH>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT">&nbsp;</TD>
+<TD ALIGN="LEFT">&nbsp;</TD>
+<TD ALIGN="LEFT">&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><IMG WIDTH="10" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img5.gif"
+ ALT="${\circ}$">&nbsp;&nbsp;'&nbsp;&nbsp;''</TD>
+<TD ALIGN="LEFT">radians</TD>
+<TD ALIGN="LEFT">1.0</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><IMG WIDTH="10" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img5.gif"
+ ALT="${\circ}$">&nbsp;&nbsp;'&nbsp;&nbsp;''</TD>
+<TD ALIGN="LEFT">turns</TD>
+<TD ALIGN="LEFT"><IMG WIDTH="227" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img6.gif"
+ ALT="$1/{2 \pi} = 0.1591549430918953358$"></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT">h m s</TD>
+<TD ALIGN="LEFT">radians</TD>
+<TD ALIGN="LEFT">15.0</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT">h m s</TD>
+<TD ALIGN="LEFT">days</TD>
+<TD ALIGN="LEFT"><IMG WIDTH="235" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img7.gif"
+ ALT="$15/{2\pi} = 2.3873241463784300365$"></TD>
+</TR>
+</TABLE></DL></DL>
+<BR> <HR>
+<A NAME="tex2html576" HREF="node16.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html577" HREF="node16.html">SLA_AIRMAS - Air Mass</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html575" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
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+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node150.html b/src/slalib/sun67.htx/node150.html
new file mode 100644
index 0000000..4750c08
--- /dev/null
+++ b/src/slalib/sun67.htx/node150.html
@@ -0,0 +1,202 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_POLMO - Polar Motion</TITLE>
+<META NAME="description" CONTENT="SLA_POLMO - Polar Motion">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1927" HREF="node151.html">SLA_PREBN - Precession Matrix (FK4)</A>
+<BR>
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+<BR>
+<B> Previous:</B> <A NAME="tex2html1919" HREF="node149.html">SLA_PM - Proper Motion</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004137000000000000000">SLA_POLMO - Polar Motion</A>
+<A NAME="xref_SLA_POLMO">&#160;</A><A NAME="SLA_POLMO">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Polar motion:  correct site longitude and latitude for polar
+motion and calculate azimuth difference between celestial and
+         terrestrial poles.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_POLMO (ELONGM, PHIM, XP, YP, ELONG, PHI, DAZ)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ELONGM</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>mean longitude of the site (radians, east +ve)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PHIM</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>mean geodetic latitude of the site (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>XP</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>polar motion <I>x</I>-coordinate (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>YP</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>polar motion <I>y</I>-coordinate (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ELONG</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>true longitude of the site (radians, east +ve)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PHI</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>true geodetic latitude of the site (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DAZ</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>azimuth correction (terrestrial-celestial, radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>``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.
+<DT>2.
+<DD>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 <IMG WIDTH="18" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img1.gif"
+ ALT="$0^{\circ}$">,      and YP is positive along the meridian at longitude
+      <IMG WIDTH="34" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img139.gif"
+ ALT="$270^\circ$"> (<I>i.e.</I> <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img22.gif"
+ ALT="$90^{\circ}$"> west).  Values for XP,YP can
+      be obtained from IERS circulars and equivalent publications;
+      the maximum amplitude observed so far is about 
+      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img32.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.3$">   .
+<DT>3.
+<DD>``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 <I>etc</I>).
+<DT>4.
+<DD>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.
+<DT>5.
+<DD>The present routine is rigorous.  For most practical
+      purposes, the following simplified formulae provide an
+      adequate approximation: <BR>
+<BR>
+<BR>
+       <TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP><TT>ELONG</TT></TD>
+<TD ALIGN="LEFT" NOWRAP><TT>=</TT></TD>
+<TD ALIGN="LEFT" NOWRAP><TT>ELONGM+XP*COS(ELONGM)-YP*SIN(ELONGM)</TT></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP><TT>PHI  </TT></TD>
+<TD ALIGN="LEFT" NOWRAP><TT>=</TT></TD>
+<TD ALIGN="LEFT" NOWRAP><TT>PHIM+(XP*SIN(ELONGM)+YP*COS(ELONGM))*TAN(PHIM)</TT></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP><TT>DAZ  </TT></TD>
+<TD ALIGN="LEFT" NOWRAP><TT>=</TT></TD>
+<TD ALIGN="LEFT" NOWRAP><TT>-SQRT(XP*XP+YP*YP)*COS(ELONGM-ATAN2(XP,YP))/COS(PHIM)</TT></TD>
+</TR>
+</TABLE> <BR>
+<BR>
+<BR>
+An alternative formulation for DAZ is:
+<BR>
+<BR>
+<BR>
+       <TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP><TT>X  </TT></TD>
+<TD ALIGN="LEFT" NOWRAP><TT>=</TT></TD>
+<TD ALIGN="LEFT" NOWRAP><TT>COS(ELONGM)*COS(PHIM)</TT></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP><TT>Y  </TT></TD>
+<TD ALIGN="LEFT" NOWRAP><TT>=</TT></TD>
+<TD ALIGN="LEFT" NOWRAP><TT>SIN(ELONGM)*COS(PHIM)</TT></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP><TT>DAZ</TT></TD>
+<TD ALIGN="LEFT" NOWRAP><TT>=</TT></TD>
+<TD ALIGN="LEFT" NOWRAP><TT>ATAN2(-X*YP-Y*XP,X*X+Y*Y)</TT></TD>
+</TR>
+</TABLE></DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Seidelmann, P.K. (ed), 1992.  <I>Explanatory
+Supplement to the Astronomical Almanac,</I> ISBN&nbsp;0-935702-68-7,
+      sections 3.27, 4.25, 4.52.
+     </DL>
+<BR> <HR>
+<A NAME="tex2html1926" HREF="node151.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1927" HREF="node151.html">SLA_PREBN - Precession Matrix (FK4)</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1925" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1919" HREF="node149.html">SLA_PM - Proper Motion</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node151.html b/src/slalib/sun67.htx/node151.html
new file mode 100644
index 0000000..f7c9a66
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@@ -0,0 +1,111 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_PREBN - Precession Matrix (FK4)</TITLE>
+<META NAME="description" CONTENT="SLA_PREBN - Precession Matrix (FK4)">
+<META NAME="keywords" CONTENT="sun67">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1937" HREF="node152.html">SLA_PREC - Precession Matrix (FK5)</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1935" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1929" HREF="node150.html">SLA_POLMO - Polar Motion</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004138000000000000000">SLA_PREBN - Precession Matrix (FK4)</A>
+<A NAME="xref_SLA_PREBN">&#160;</A><A NAME="SLA_PREBN">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Generate the matrix of precession between two epochs,
+using the old, pre IAU&nbsp;1976, Bessel-Newcomb model, in
+         Andoyer's formulation.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_PREBN (BEP0, BEP1, RMATP)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>BEP0</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>beginning Besselian epoch</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>BEP1</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>ending Besselian epoch</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RMATP</EM></TD>
+<TH ALIGN="LEFT"><B>D(3,3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>precession matrix</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTE:</STRONG>
+<DD>The matrix is in the sense:
+<BLOCKQUOTE><B>v</B><SUB>1</SUB> =  <B>M</B><IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"><B>v</B><SUB>0</SUB></BLOCKQUOTE>
+       where <B>v</B><SUB>1</SUB> is the star vector relative to the
+       mean equator and equinox of epoch BEP1, <B>M</B> is the
+       <IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img18.gif"
+ ALT="$3\times3$"> matrix RMATP and
+       <B>v</B><SUB>0</SUB> is the star vector relative to the
+       mean equator and equinox of epoch BEP0.
+      </DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Smith <I>et al.</I>, 1989. <I>Astr.J.</I> <B>97</B>, 269.
+</DL>
+<BR> <HR>
+<A NAME="tex2html1936" HREF="node152.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1937" HREF="node152.html">SLA_PREC - Precession Matrix (FK5)</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1935" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1929" HREF="node150.html">SLA_POLMO - Polar Motion</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node152.html b/src/slalib/sun67.htx/node152.html
new file mode 100644
index 0000000..9e5ea39
--- /dev/null
+++ b/src/slalib/sun67.htx/node152.html
@@ -0,0 +1,145 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_PREC - Precession Matrix (FK5)</TITLE>
+<META NAME="description" CONTENT="SLA_PREC - Precession Matrix (FK5)">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
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+<BR> <HR>
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+<A NAME="tex2html1938" HREF="node151.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1947" HREF="node153.html">SLA_PRECES - Precession</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1945" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
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+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004139000000000000000">SLA_PREC - Precession Matrix (FK5)</A>
+<A NAME="xref_SLA_PREC">&#160;</A><A NAME="SLA_PREC">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Form the matrix of precession between two epochs (IAU 1976, FK5).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_PREC (EP0, EP1, RMATP)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EP0</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>beginning epoch</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EP1</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>ending epoch</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RMATP</EM></TD>
+<TH ALIGN="LEFT"><B>D(3,3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>precession matrix</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The epochs are TDB Julian epochs.
+<DT>2.
+<DD>The matrix is in the sense:
+<BLOCKQUOTE><B>v</B><SUB>1</SUB> =  <B>M</B><IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"><B>v</B><SUB>0</SUB></BLOCKQUOTE>
+        where <B>v</B><SUB>1</SUB> is the star vector relative to the
+        mean equator and equinox of epoch EP1, <B>M</B> is the
+        <IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img18.gif"
+ ALT="$3\times3$"> matrix RMATP and
+        <B>v</B><SUB>0</SUB> is the star vector relative to the
+        mean equator and equinox of epoch EP0.
+  <DT>3.
+<DD>Though the matrix method itself is rigorous, the precession
+        angles are expressed through canonical polynomials which are
+        valid only for a limited time span.  There are also known
+        errors in the IAU precession rate.  The absolute accuracy
+        of the present formulation is better than 
+      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img25.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.1$">    from
+        1960AD to 2040AD, better than <IMG WIDTH="17" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img140.gif"
+ ALT="$1\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> from 1640AD to 2360AD,
+        and remains below <IMG WIDTH="17" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img75.gif"
+ ALT="$3\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> for the whole of the period
+        500BC to 3000AD.  The errors exceed <IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img74.gif"
+ ALT="$10\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> outside the
+        range 1200BC to 3900AD, exceed <IMG WIDTH="33" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img141.gif"
+ ALT="$100\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> outside 4200BC to
+        5600AD and exceed <IMG WIDTH="41" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img142.gif"
+ ALT="$1000\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> outside 6800BC to 8200AD.
+        The SLALIB routine sla_PRECL implements a more elaborate
+        model which is suitable for problems spanning several
+        thousand years.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Lieske, J.H., 1979. <I>Astr.Astrophys.</I> <B>73</B>, 282;
+equations 6 &amp; 7, p283.
+<DT>2.
+<DD>Kaplan, G.H., 1981. <I>USNO circular no. 163</I>, pA2.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1946" HREF="node153.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1947" HREF="node153.html">SLA_PRECES - Precession</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1945" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1939" HREF="node151.html">SLA_PREBN - Precession Matrix (FK4)</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node153.html b/src/slalib/sun67.htx/node153.html
new file mode 100644
index 0000000..e63959a
--- /dev/null
+++ b/src/slalib/sun67.htx/node153.html
@@ -0,0 +1,120 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_PRECES - Precession</TITLE>
+<META NAME="description" CONTENT="SLA_PRECES - Precession">
+<META NAME="keywords" CONTENT="sun67">
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+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1957" HREF="node154.html">SLA_PRECL - Precession Matrix (latest)</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1955" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1949" HREF="node152.html">SLA_PREC - Precession Matrix (FK5)</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004140000000000000000">SLA_PRECES - Precession</A>
+<A NAME="xref_SLA_PRECES">&#160;</A><A NAME="SLA_PRECES">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Precession - either the old ``FK4'' (Bessel-Newcomb, pre&nbsp;IAU&nbsp;1976)
+or new ``FK5'' (Fricke, post&nbsp;IAU&nbsp;1976) as required.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_PRECES (SYSTEM, EP0, EP1, RA, DC)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>SYSTEM</EM></TD>
+<TH ALIGN="LEFT"><B>C</B></TH>
+<TD ALIGN="LEFT" NOWRAP>precession to be applied: `FK4' or `FK5'</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EP0,EP1</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>starting and ending epoch</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RA,DC</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">, mean equator &amp; equinox of epoch EP0</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RA,DC</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">, mean equator &amp; equinox of epoch EP1</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Lowercase characters in SYSTEM are acceptable.
+<DT>2.
+<DD>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:
+        <BLOCKQUOTE><TT>CALL sla_PRECES ('FK4', 1900D0, 1950D0, RA, DC)</TT>
+        </BLOCKQUOTE>
+  <DT>3.
+<DD>This routine will <B>NOT</B> correctly convert between the old and
+        the new systems - for example conversion from B1950 to J2000.
+        For these purposes see sla_FK425, sla_FK524, sla_FK45Z and
+        sla_FK54Z.
+  <DT>4.
+<DD>If an invalid SYSTEM is supplied, values of -99D0,-99D0 are
+        returned for both RA and DC.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1956" HREF="node154.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1957" HREF="node154.html">SLA_PRECL - Precession Matrix (latest)</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1955" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1949" HREF="node152.html">SLA_PREC - Precession Matrix (FK5)</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node154.html b/src/slalib/sun67.htx/node154.html
new file mode 100644
index 0000000..a20e26a
--- /dev/null
+++ b/src/slalib/sun67.htx/node154.html
@@ -0,0 +1,131 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_PRECL - Precession Matrix (latest)</TITLE>
+<META NAME="description" CONTENT="SLA_PRECL - Precession Matrix (latest)">
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+<B> Next:</B> <A NAME="tex2html1967" HREF="node155.html">SLA_PRENUT - Precession/Nutation Matrix</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1965" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1959" HREF="node153.html">SLA_PRECES - Precession</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004141000000000000000">SLA_PRECL - Precession Matrix (latest)</A>
+<A NAME="xref_SLA_PRECL">&#160;</A><A NAME="SLA_PRECL">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Form the matrix of precession between two epochs, using the
+model of Simon <I>et al</I>. (1994), which is suitable for long
+         periods of time.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_PRECL (EP0, EP1, RMATP)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EP0</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>beginning epoch</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EP1</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>ending epoch</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RMATP</EM></TD>
+<TH ALIGN="LEFT"><B>D(3,3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>precession matrix</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The epochs are TDB Julian epochs.
+<DT>2.
+<DD>The matrix is in the sense:
+<BLOCKQUOTE><B>v</B><SUB>1</SUB> =  <B>M</B><IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"><B>v</B><SUB>0</SUB></BLOCKQUOTE>
+        where <B>v</B><SUB>1</SUB> is the star vector relative to the
+        mean equator and equinox of epoch EP1, <B>M</B> is the
+        <IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img18.gif"
+ ALT="$3\times3$"> matrix RMATP and
+        <B>v</B><SUB>0</SUB> is the star vector relative to the
+        mean equator and equinox of epoch EP0.
+  <DT>3.
+<DD>The absolute accuracy of the model is limited by the
+        uncertainty in the general precession, about 
+      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img32.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.3$">    per
+        1000&nbsp;years.  The remainder of the formulation provides a
+        precision of 1&nbsp;milliarcsecond over the interval from 1000AD
+        to 3000AD, 
+      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img25.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.1$">    from 1000BC to 5000AD and
+        <IMG WIDTH="17" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img140.gif"
+ ALT="$1\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> from 4000BC to 8000AD.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Simon, J.L. <I>et al</I>., 1994. <I>Astr.Astrophys.</I> <B>282</B>,
+663.
+     </DL>
+<BR> <HR>
+<A NAME="tex2html1966" HREF="node155.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1964" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1958" HREF="node153.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1967" HREF="node155.html">SLA_PRENUT - Precession/Nutation Matrix</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1965" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1959" HREF="node153.html">SLA_PRECES - Precession</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node155.html b/src/slalib/sun67.htx/node155.html
new file mode 100644
index 0000000..e7dc899
--- /dev/null
+++ b/src/slalib/sun67.htx/node155.html
@@ -0,0 +1,110 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_PRENUT - Precession/Nutation Matrix</TITLE>
+<META NAME="description" CONTENT="SLA_PRENUT - Precession/Nutation Matrix">
+<META NAME="keywords" CONTENT="sun67">
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+<A NAME="tex2html1974" HREF="node13.html">
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+<A NAME="tex2html1968" HREF="node154.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1977" HREF="node156.html">SLA_PV2EL - Orbital Elements from Position/Velocity</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1975" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1969" HREF="node154.html">SLA_PRECL - Precession Matrix (latest)</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004142000000000000000">SLA_PRENUT - Precession/Nutation Matrix</A>
+<A NAME="xref_SLA_PRENUT">&#160;</A><A NAME="SLA_PRENUT">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Form the matrix of precession and nutation (IAU&nbsp;1976, FK5).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_PRENUT (EPOCH, DATE, RMATPN)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EPOCH</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>Julian Epoch for mean coordinates</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>Modified Julian Date (JD-2400000.5)
+for true coordinates</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RMATPN</EM></TD>
+<TH ALIGN="LEFT"><B>D(3,3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>combined precession/nutation matrix</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The epoch and date are TDB.
+<DT>2.
+<DD>The matrix is in the sense:
+<BLOCKQUOTE><B>v</B><SUB><I>true</I></SUB> =  <B>M</B><IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"><B>v</B><SUB><I>mean</I></SUB></BLOCKQUOTE>
+        where <B>v</B><SUB><I>true</I></SUB> is the star vector relative to the
+        true equator and equinox of epoch DATE, <B>M</B> is the
+        <IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img18.gif"
+ ALT="$3\times3$"> matrix RMATPN and
+        <B>v</B><SUB><I>mean</I></SUB> is the star vector relative to the
+        mean equator and equinox of epoch EPOCH.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1976" HREF="node156.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+<A NAME="tex2html1968" HREF="node154.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1977" HREF="node156.html">SLA_PV2EL - Orbital Elements from Position/Velocity</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1975" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1969" HREF="node154.html">SLA_PRECL - Precession Matrix (latest)</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node156.html b/src/slalib/sun67.htx/node156.html
new file mode 100644
index 0000000..ab897bc
--- /dev/null
+++ b/src/slalib/sun67.htx/node156.html
@@ -0,0 +1,323 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_PV2EL - Orbital Elements from Position/Velocity</TITLE>
+<META NAME="description" CONTENT="SLA_PV2EL - Orbital Elements from Position/Velocity">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node157.html">
+<LINK REL="previous" HREF="node155.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node157.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1986" HREF="node157.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1984" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1978" HREF="node155.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1987" HREF="node157.html">SLA_PV2UE - Position/Velocity to Universal Elements</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1985" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1979" HREF="node155.html">SLA_PRENUT - Precession/Nutation Matrix</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004143000000000000000">SLA_PV2EL - Orbital Elements from Position/Velocity</A>
+<A NAME="xref_SLA_PV2EL">&#160;</A><A NAME="SLA_PV2EL">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Heliocentric osculating elements obtained from instantaneous
+position and velocity.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_PV2EL (
+         PV, DATE, PMASS, JFORMR, JFORM, EPOCH, ORBINC,
+         ANODE, PERIH, AORQ, E, AORL, DM, JSTAT)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PV</EM></TD>
+<TH ALIGN="LEFT"><B>D(6)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>heliocentric <IMG WIDTH="106" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img51.gif"
+ ALT="$[\,x,y,z,\dot{x},\dot{y},\dot{z}\,]$">, equatorial, J2000</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  (AU, AU/s; Note&nbsp;1)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>date (TT Modified Julian Date = JD-2400000.5)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PMASS</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>mass of the planet (Sun = 1; Note&nbsp;2)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JFORMR</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>requested element set (1-3; Note&nbsp;3)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JFORM</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>element set actually returned (1-3; Note&nbsp;4)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EPOCH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>epoch of elements (<I>t<SUB>0</SUB></I> or <I>T</I>, TT MJD)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ORBINC</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>inclination (<I>i</I>, radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ANODE</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>longitude of the ascending node (<IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$">, radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PERIH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>longitude or argument of perihelion
+(<IMG WIDTH="16" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img100.gif"
+ ALT="$\varpi$"> or <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$">,</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AORQ</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>mean distance or perihelion distance (<I>a</I> or <I>q</I>, AU)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>E</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>eccentricity (<I>e</I>)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AORL</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>mean anomaly or longitude
+(<I>M</I> or <I>L</I>, radians,</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  JFORM=1,2 only)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DM</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>daily motion (<I>n</I>, radians, JFORM=1 only)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JSTAT</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>     0 = OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -1 = illegal PMASS</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -2 = illegal JFORMR</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -3 = position/velocity out of allowed range</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>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.
+  <DT>2.
+<DD>The mass, PMASS, is important only for the larger planets.  For
+        most purposes (<I>e.g.</I>&nbsp;asteroids) use 0D0.  Values less than zero
+        are illegal.
+  <DT>3.
+<DD>Three different element-format options are supported, as
+        follows. <BR>
+<P>
+JFORM=1, suitable for the major planets:
+<P>        <PRE><TT>
+ 		 EPOCH 		 = 		 epoch of elements <I>t<SUB>0</SUB></I> (TT MJD)
+		 ORBINC 		 = 		 inclination <I>i</I> (radians)
+		 ANODE 		 = 		 longitude of the ascending node <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> (radians)
+		 PERIH 		 = 		 longitude of perihelion <IMG WIDTH="16" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img100.gif"
+ ALT="$\varpi$"> (radians)
+		 AORQ 		 = 		 mean distance <I>a</I> (AU)
+		 E 		 = 		 eccentricity <I>e</I> <IMG WIDTH="83" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img106.gif"
+ ALT="$( 0 \leq e < 1 )$"> 
+		 AORL 		 = 		 mean longitude <I>L</I> (radians)
+		 DM 		 = 		 daily motion <I>n</I> (radians)        
+</TT></PRE>
+<P>
+JFORM=2, suitable for minor planets:
+<P>        <PRE><TT>
+ 		 EPOCH 		 = 		 epoch of elements <I>t<SUB>0</SUB></I> (TT MJD)
+		 ORBINC 		 = 		 inclination <I>i</I> (radians)
+		 ANODE 		 = 		 longitude of the ascending node <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> (radians)
+		 PERIH 		 = 		 argument of perihelion <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$"> (radians)
+		 AORQ 		 = 		 mean distance <I>a</I> (AU)
+		 E 		 = 		 eccentricity <I>e</I> <IMG WIDTH="83" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img106.gif"
+ ALT="$( 0 \leq e < 1 )$"> 
+		 AORL 		 = 		 mean anomaly <I>M</I> (radians)        
+</TT></PRE>
+<P>
+JFORM=3, suitable for comets:
+<P>        <PRE><TT>
+ 		 EPOCH 		 = 		 epoch of perihelion <I>T</I> (TT MJD)
+		 ORBINC 		 = 		 inclination <I>i</I> (radians)
+		 ANODE 		 = 		 longitude of the ascending node <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> (radians)
+		 PERIH 		 = 		 argument of perihelion <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$"> (radians)
+		 AORQ 		 = 		 perihelion distance <I>q</I> (AU)
+		 E 		 = 		 eccentricity <I>e</I> <IMG WIDTH="91" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img107.gif"
+ ALT="$( 0 \leq e \leq 10 )$"></TT></PRE>
+  <DT>4.
+<DD>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:
+<P>        <PRE><TT>
+ 		 JFORMR 		 JFORM 		 meaning 
+&nbsp;
+		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;1 		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;1 		 OK: elements are in the requested format
+		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;1 		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;2 		 never happens
+		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;1 		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;3 		 orbit not elliptical
+		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;2 		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;1 		 never happens
+		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;2 		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;2 		 OK: elements are in the requested format
+		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;2 		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;3 		 orbit not elliptical
+		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;3 		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;1 		 never happens
+		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;3 		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;2 		 never happens
+		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;3 		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;3 		 OK: elements are in the requested format        
+</TT></PRE>
+  <DT>5.
+<DD>The arguments returned for each value of JFORM (<I>cf</I> Note&nbsp;5:
+        JFORM may not be the same as JFORMR) are as follows:
+<P>        <PRE><TT>
+ 		 JFORM 		 1 		 2 		 3 
+&nbsp;
+		 EPOCH 		 <I>t<SUB>0</SUB></I> <I>t<SUB>0</SUB></I> <I>T</I> 
+		 ORBINC 		 <I>i</I> <I>i</I> <I>i</I> 
+		 ANODE 		 <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> 
+		 PERIH 		 <IMG WIDTH="16" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img100.gif"
+ ALT="$\varpi$"> <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$"> <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$"> 
+		 AORQ 		 <I>a</I> <I>a</I> <I>q</I> 
+		 E 		 <I>e</I> <I>e</I> <I>e</I> 
+		 AORL 		 <I>L</I> <I>M</I> -
+		 DM 		 <I>n</I> - 		 -        
+</TT></PRE>
+<P>
+where:
+        <PRE><TT>
+ 		 <I>t<SUB>0</SUB></I> is the epoch of the elements (MJD, TT)
+		 <I>T</I> is the epoch of perihelion (MJD, TT)
+		 <I>i</I> is the inclination (radians)
+		 <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> is the longitude of the ascending node (radians)
+		 <IMG WIDTH="16" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img100.gif"
+ ALT="$\varpi$"> is the longitude of perihelion (radians)
+		 <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$"> is the argument of perihelion (radians)
+		 <I>a</I> is the mean distance (AU)
+		 <I>q</I> is the perihelion distance (AU)
+		 <I>e</I> is the eccentricity
+		 <I>L</I> is the longitude (radians, <IMG WIDTH="48" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img143.gif"
+ ALT="$0-2\pi$">)		 <I>M</I> is the mean anomaly (radians, <IMG WIDTH="48" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img143.gif"
+ ALT="$0-2\pi$">)		 <I>n</I> is the daily motion (radians)
+		 - 		 means no value is set        
+</TT></PRE>
+  <DT>6.
+<DD>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.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Sterne, Theodore E., <I>An Introduction to Celestial Mechanics,</I>
+Interscience Publishers, 1960.
+     </DL>
+<BR> <HR>
+<A NAME="tex2html1986" HREF="node157.html">
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+<BR>
+<B> Next:</B> <A NAME="tex2html1987" HREF="node157.html">SLA_PV2UE - Position/Velocity to Universal Elements</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1985" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
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+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node157.html b/src/slalib/sun67.htx/node157.html
new file mode 100644
index 0000000..08c25e9
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+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
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+<H2><A NAME="SECTION0004144000000000000000">SLA_PV2UE - Position/Velocity to Universal Elements</A>
+<A NAME="xref_SLA_PV2UE">&#160;</A><A NAME="SLA_PV2UE">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Construct a universal element set based on an instantaneous
+position and velocity.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_PV2UE (PV, DATE, PMASS, U, JSTAT)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PV</EM></TD>
+<TH ALIGN="LEFT"><B>D(6)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>heliocentric <IMG WIDTH="106" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img51.gif"
+ ALT="$[\,x,y,z,\dot{x},\dot{y},\dot{z}\,]$">, equatorial, J2000</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  (AU, AU/s; Note&nbsp;1)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>date (TT Modified Julian Date = JD-2400000.5)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PMASS</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>mass of the planet (Sun = 1; Note&nbsp;2)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>U</EM></TD>
+<TH ALIGN="LEFT"><B>D(13)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>universal orbital elements (Note&nbsp;3)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(1)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>combined mass (<I>M</I>+<I>m</I>)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(2)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>total energy of the orbit (<IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$">)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(3)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>reference (osculating) epoch (<I>t<SUB>0</SUB></I>)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(4-6)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>position at reference epoch (<IMG WIDTH="17" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img102.gif"
+ ALT="${\rm \bf r}_0$">)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(7-9)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>velocity at reference epoch (<IMG WIDTH="19" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img103.gif"
+ ALT="${\rm \bf v}_0$">)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(10)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>heliocentric distance at reference epoch</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(11)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img104.gif"
+ ALT="${\rm \bf r}_0.{\rm \bf v}_0$"></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(12)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>date (<I>t</I>)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(13)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>universal eccentric anomaly (<IMG WIDTH="14" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img105.gif"
+ ALT="$\psi$">) of date, approx</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JSTAT</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>       0 = OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>     -1 = illegal PMASS</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>     -2 = too close to Sun</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>     -3 = too slow</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>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.
+  <DT>2.
+<DD>The mass, PMASS, is important only for the larger planets.  For
+        most purposes (<I>e.g.</I>&nbsp;asteroids) use 0D0.  Values less than zero
+        are illegal.
+  <DT>3.
+<DD>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)&nbsp;<IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$">, which is proportional to the total energy of the
+        orbit, (ii)&nbsp;the heliocentric distance at epoch,
+        (iii)&nbsp;the outwards component of the velocity at the given epoch,
+        (iv)&nbsp;an estimate of <IMG WIDTH="14" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img105.gif"
+ ALT="$\psi$">, the ``universal eccentric anomaly'' at a
+        given date and (v)&nbsp;that date.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Everhart, E. &amp; Pitkin, E.T., Am.&nbsp;J.&nbsp;Phys.&nbsp;51, 712, 1983.
+</DL>
+<BR> <HR>
+<A NAME="tex2html1996" HREF="node158.html">
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+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
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@@ -0,0 +1,102 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
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+<H2><A NAME="SECTION0004145000000000000000">SLA_PVOBS - Observatory Position &amp; Velocity</A>
+<A NAME="xref_SLA_PVOBS">&#160;</A><A NAME="SLA_PVOBS">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Position and velocity of an observing station.
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_PVOBS (P, H, STL, PV)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>P</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>latitude (geodetic, radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>H</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>height above reference spheroid (geodetic, metres)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>STL</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>local apparent sidereal time (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PV</EM></TD>
+<TH ALIGN="LEFT"><B>D(6)</B></TH>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="106" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img51.gif"
+ ALT="$[\,x,y,z,\dot{x},\dot{y},\dot{z}\,]$"> (AU, AU&nbsp;s<SUP>-1</SUP>, true equator and equinox
+of date)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTE:</STRONG>
+<DD>IAU 1976 constants are used.
+</DL>
+<BR> <HR>
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+<B> Next:</B> <A NAME="tex2html2007" HREF="node159.html">SLA_PXY - Apply Linear Model</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2005" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1999" HREF="node157.html">SLA_PV2UE - Position/Velocity to Universal Elements</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node159.html b/src/slalib/sun67.htx/node159.html
new file mode 100644
index 0000000..6cf76da
--- /dev/null
+++ b/src/slalib/sun67.htx/node159.html
@@ -0,0 +1,145 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_PXY - Apply Linear Model</TITLE>
+<META NAME="description" CONTENT="SLA_PXY - Apply Linear Model">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
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+<BR> <HR>
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+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2017" HREF="node160.html">SLA_RANDOM - Random Number</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2015" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2009" HREF="node158.html">SLA_PVOBS - Observatory Position &amp; Velocity</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004146000000000000000">SLA_PXY - Apply Linear Model</A>
+<A NAME="xref_SLA_PXY">&#160;</A><A NAME="SLA_PXY">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Given arrays of <I>expected</I> and <I>measured</I>
+<IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> coordinates, and a
+         linear model relating them (as produced by sla_FITXY), compute
+         the array of <I>predicted</I> coordinates and the RMS residuals.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_PXY (NP,XYE,XYM,COEFFS,XYP,XRMS,YRMS,RRMS)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NP</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>number of samples</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>XYE</EM></TD>
+<TD ALIGN="LEFT"><B>D(2,NP)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>expected <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> for each sample</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>XYM</EM></TD>
+<TD ALIGN="LEFT"><B>D(2,NP)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>measured <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> for each sample</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>COEFFS</EM></TD>
+<TD ALIGN="LEFT"><B>D(6)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>coefficients of model (see below)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>XYP</EM></TD>
+<TH ALIGN="LEFT"><B>D(2,NP)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>predicted <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> for each sample</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>XRMS</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>RMS in X</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>YRMS</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>RMS in Y</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RRMS</EM></TD>
+<TD ALIGN="LEFT"><B>D </B></TD>
+<TD ALIGN="LEFT" NOWRAP>total RMS (vector sum of XRMS and YRMS)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The model is supplied in the array COEFFS.  Naming the
+six elements of COEFFS <I>a</I>,<I>b</I>,<I>c</I>,<I>d</I>,<I>e</I> &amp; <I>f</I>,
+the model transforms <I>measured</I> coordinates
+        <IMG WIDTH="63" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img113.gif"
+ ALT="$[x_{m},y_{m}\,]$"> into <I>predicted</I> coordinates
+        <IMG WIDTH="53" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img144.gif"
+ ALT="$[x_{p},y_{p}\,]$"> as follows:
+        <BLOCKQUOTE><I>x</I><SUB><I>p</I></SUB> = <I>a</I> + <I>bx</I><SUB><I>m</I></SUB> + <I>cy</I><SUB><I>m</I></SUB> <BR>
+         <I>y</I><SUB><I>p</I></SUB> = <I>d</I> + <I>ex</I><SUB><I>m</I></SUB> + <I>fy</I><SUB><I>m</I></SUB></BLOCKQUOTE>
+  <DT>2.
+<DD>The residuals are (<I>x</I><SUB><I>p</I></SUB>-<I>x</I><SUB><I>e</I></SUB>) and (<I>y</I><SUB><I>p</I></SUB>-<I>y</I><SUB><I>e</I></SUB>).
+  <DT>3.
+<DD>If NP is less than or equal to zero, no coordinates are
+        transformed, and the RMS residuals are all zero.
+  <DT>4.
+<DD>See also sla_FITXY, sla_INVF, sla_XY2XY, sla_DCMPF
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html2016" HREF="node160.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2014" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2008" HREF="node158.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2017" HREF="node160.html">SLA_RANDOM - Random Number</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2015" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2009" HREF="node158.html">SLA_PVOBS - Observatory Position &amp; Velocity</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node16.html b/src/slalib/sun67.htx/node16.html
new file mode 100644
index 0000000..682e1dd
--- /dev/null
+++ b/src/slalib/sun67.htx/node16.html
@@ -0,0 +1,121 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_AIRMAS - Air Mass</TITLE>
+<META NAME="description" CONTENT="SLA_AIRMAS - Air Mass">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node17.html">
+<LINK REL="previous" HREF="node15.html">
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+<A NAME="tex2html578" HREF="node15.html">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html587" HREF="node17.html">SLA_ALTAZ - Velocities etc. for Altazimuth Mount</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html585" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html579" HREF="node15.html">SLA_AFIN - Sexagesimal character string to angle</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION00043000000000000000">SLA_AIRMAS - Air Mass</A>
+<A NAME="xref_SLA_AIRMAS">&#160;</A><A NAME="SLA_AIRMAS">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Air mass at given zenith distance (double precision).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>D&nbsp;=&nbsp;sla_AIRMAS (ZD)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ZD</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>observed zenith distance (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_AIRMAS</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>air mass (1 at zenith)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The <I>observed</I> zenith distance referred to above means
+``as affected by refraction''.
+<DT>2.
+<DD>The routine uses Hardie's (1962) polynomial fit to Bemporad's
+        data for the relative air mass, <I>X</I>, 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 <I>X</I> = 6.8 and better than 1% up to <I>X</I> = 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.
+  <DT>3.
+<DD>The sign of the ZD is ignored.
+  <DT>4.
+<DD>At zenith distances greater than about <IMG WIDTH="56" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img8.gif"
+ ALT="$\zeta = 87^{\circ}$"> the
+        air mass is held constant to avoid arithmetic overflows.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Hardie, R.H., 1962, in <I>Astronomical Techniques</I>
+ed. W.A. Hiltner, University of Chicago Press, p180.
+<DT>2.
+<DD>Schoenberg, E., 1929, Hdb. d. Ap.,
+        Berlin, Julius Springer, 2, 268.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html586" HREF="node17.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+<A NAME="tex2html578" HREF="node15.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html587" HREF="node17.html">SLA_ALTAZ - Velocities etc. for Altazimuth Mount</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html585" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html579" HREF="node15.html">SLA_AFIN - Sexagesimal character string to angle</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node160.html b/src/slalib/sun67.htx/node160.html
new file mode 100644
index 0000000..972237c
--- /dev/null
+++ b/src/slalib/sun67.htx/node160.html
@@ -0,0 +1,98 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_RANDOM - Random Number</TITLE>
+<META NAME="description" CONTENT="SLA_RANDOM - Random Number">
+<META NAME="keywords" CONTENT="sun67">
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+<A NAME="tex2html2026" HREF="node161.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2024" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2018" HREF="node159.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2027" HREF="node161.html">SLA_RANGE - Put Angle into Range</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2025" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2019" HREF="node159.html">SLA_PXY - Apply Linear Model</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004147000000000000000">SLA_RANDOM - Random Number</A>
+<A NAME="xref_SLA_RANDOM">&#160;</A><A NAME="SLA_RANDOM">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Generate pseudo-random real number in the range <IMG WIDTH="72" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img145.gif"
+ ALT="$0 \leq x < 1$">.<DT><STRONG>CALL:</STRONG>
+<DD><TT>R&nbsp;=&nbsp;sla_RANDOM (SEED)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>SEED</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>an arbitrary real number</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>SEED</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>a new arbitrary value</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_RANDOM</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>Pseudo-random real number <IMG WIDTH="72" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img145.gif"
+ ALT="$0 \leq x < 1$">.</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTE:</STRONG>
+<DD>The implementation is machine-dependent.
+</DL>
+<BR> <HR>
+<A NAME="tex2html2026" HREF="node161.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2024" HREF="node13.html">
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+<A NAME="tex2html2018" HREF="node159.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2027" HREF="node161.html">SLA_RANGE - Put Angle into Range</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2025" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2019" HREF="node159.html">SLA_PXY - Apply Linear Model</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node161.html b/src/slalib/sun67.htx/node161.html
new file mode 100644
index 0000000..b8c2cb4
--- /dev/null
+++ b/src/slalib/sun67.htx/node161.html
@@ -0,0 +1,93 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_RANGE - Put Angle into Range </TITLE>
+<META NAME="description" CONTENT="SLA_RANGE - Put Angle into Range ">
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+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2034" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2028" HREF="node160.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2037" HREF="node162.html">SLA_RANORM - Put Angle into Range</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2035" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2029" HREF="node160.html">SLA_RANDOM - Random Number</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004148000000000000000">&#160;</A><A NAME="xref_SLA_RANGE">&#160;</A><A NAME="SLA_RANGE">&#160;</A>
+<BR>
+SLA_RANGE - Put Angle into Range <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$"></H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Normalize an angle into the range <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$"> (single precision).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>R&nbsp;=&nbsp;sla_RANGE (ANGLE)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ANGLE</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>angle in radians</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_RANGE</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>ANGLE expressed in the range <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$">.</TD>
+</TR>
+</TABLE></DL>
+<BR> <HR>
+<A NAME="tex2html2036" HREF="node162.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2034" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2028" HREF="node160.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2037" HREF="node162.html">SLA_RANORM - Put Angle into Range</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2035" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2029" HREF="node160.html">SLA_RANDOM - Random Number</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node162.html b/src/slalib/sun67.htx/node162.html
new file mode 100644
index 0000000..3317041
--- /dev/null
+++ b/src/slalib/sun67.htx/node162.html
@@ -0,0 +1,93 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_RANORM - Put Angle into Range </TITLE>
+<META NAME="description" CONTENT="SLA_RANORM - Put Angle into Range ">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node163.html">
+<LINK REL="previous" HREF="node161.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node163.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html2046" HREF="node163.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2044" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2038" HREF="node161.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2047" HREF="node163.html">SLA_RCC - Barycentric Coordinate Time</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2045" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2039" HREF="node161.html">SLA_RANGE - Put Angle into Range</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004149000000000000000">&#160;</A><A NAME="xref_SLA_RANORM">&#160;</A><A NAME="SLA_RANORM">&#160;</A>
+<BR>
+SLA_RANORM - Put Angle into Range <IMG WIDTH="43" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img66.gif"
+ ALT="$0\!-\!2\pi$"></H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Normalize an angle into the range <IMG WIDTH="43" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img66.gif"
+ ALT="$0\!-\!2\pi$"> (single precision).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>R&nbsp;=&nbsp;sla_RANORM (ANGLE)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ANGLE</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>angle in radians</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_RANORM</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>ANGLE expressed in the range <IMG WIDTH="43" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img66.gif"
+ ALT="$0\!-\!2\pi$"></TD>
+</TR>
+</TABLE></DL>
+<BR> <HR>
+<A NAME="tex2html2046" HREF="node163.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2044" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2038" HREF="node161.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2047" HREF="node163.html">SLA_RCC - Barycentric Coordinate Time</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2045" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2039" HREF="node161.html">SLA_RANGE - Put Angle into Range</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node163.html b/src/slalib/sun67.htx/node163.html
new file mode 100644
index 0000000..4f6cf04
--- /dev/null
+++ b/src/slalib/sun67.htx/node163.html
@@ -0,0 +1,166 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_RCC - Barycentric Coordinate Time</TITLE>
+<META NAME="description" CONTENT="SLA_RCC - Barycentric Coordinate Time">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node164.html">
+<LINK REL="previous" HREF="node162.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node164.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html2056" HREF="node164.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2054" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2048" HREF="node162.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2057" HREF="node164.html">SLA_RDPLAN - Apparent of Planet</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2055" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2049" HREF="node162.html">SLA_RANORM - Put Angle into Range</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004150000000000000000">SLA_RCC - Barycentric Coordinate Time</A>
+<A NAME="xref_SLA_RCC">&#160;</A><A NAME="SLA_RCC">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>D&nbsp;=&nbsp;sla_RCC (TDB, UT1, WL, U, V)</TT>
+<DT><STRONG>ACTION:</STRONG>
+<DD>The relativistic clock correction TDB-TT, the
+         difference between <I>proper time</I>
+         on Earth and <I>coordinate time</I> in the solar system barycentric
+         space-time frame of reference.  The proper time is TT;  the
+         coordinate time is <I>an implementation</I> of TDB.
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>TDB</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>coordinate time (MJD: JD-2400000.5)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>UT1</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>universal time (fraction of one day)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>WL</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>clock longitude (radians west)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>U</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>clock distance from Earth spin axis (km)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>clock distance north of Earth equatorial plane (km)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_RCC</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>TDB-TT (sec)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>TDB may be considered to
+be the coordinate time in the solar system barycentre frame of
+reference, and TT is the proper time given by clocks at mean sea
+        level on the Earth.
+  <DT>2.
+<DD>The result has a main (annual) sinusoidal term of amplitude
+        approximately 1.66ms, plus planetary terms up to about
+        20<IMG WIDTH="12" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img146.gif"
+ ALT="$\mu$">s, and lunar and diurnal terms up to 2<IMG WIDTH="12" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img146.gif"
+ ALT="$\mu$">s.  The
+        variation arises from the transverse Doppler effect and the
+        gravitational red-shift as the observer varies in speed and
+        moves through different gravitational potentials.
+  <DT>3.
+<DD>The argument TDB is, strictly, the barycentric coordinate time;
+        however, the terrestrial proper time (TT) can in practice be used.
+  <DT>4.
+<DD>The geocentric model is that of Fairhead &amp; Bretagnon (1990),
+        in its full
+        form.  It was supplied by Fairhead (private communication)
+        as a Fortran subroutine.  A number of coding changes were made to
+        this subroutine in order
+        match the calling sequence of previous versions of the present
+        routine, to comply with Starlink programming standards and to
+        avoid compilation problems on certain machines.  On the supported
+        computer types,
+        the numerical results are essentially unaffected by the
+        changes.  The topocentric model is from Moyer (1981) and Murray (1983).
+        During the interval 1950-2050, the absolute accuracy of the
+        geocentric model is better than <IMG WIDTH="23" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img147.gif"
+ ALT="$\pm3$">&nbsp;nanoseconds
+        relative to direct numerical integrations using the JPL DE200/LE200
+        solar system ephemeris.
+  <DT>5.
+<DD>The IAU definition of TDB is that it must differ from TT only by
+        periodic terms.  Though practical, this is an imprecise definition
+        which ignores the existence of very long-period and secular effects
+        in the dynamics of the solar system.  As a consequence, different
+        implementations of TDB will, in general, differ in zero-point and
+        will drift linearly relative to one other.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Fairhead, L. &amp; 
+Bretagnon, P., 1990. <I>Astr.Astrophys.</I> <B>229</B>, 240-247.
+<DT>2.
+<DD>Moyer, T.D., 1981. <I>Cel.Mech.</I> <B>23</B>, 33.
+  <DT>3.
+<DD>Murray, C.A., 1983, <I>Vectorial Astrometry</I>, Adam Hilger.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html2056" HREF="node164.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2054" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2048" HREF="node162.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2057" HREF="node164.html">SLA_RDPLAN - Apparent of Planet</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2055" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2049" HREF="node162.html">SLA_RANORM - Put Angle into Range</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node164.html b/src/slalib/sun67.htx/node164.html
new file mode 100644
index 0000000..d45ee2f
--- /dev/null
+++ b/src/slalib/sun67.htx/node164.html
@@ -0,0 +1,184 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_RDPLAN - Apparent of Planet</TITLE>
+<META NAME="description" CONTENT="SLA_RDPLAN - Apparent of Planet">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node165.html">
+<LINK REL="previous" HREF="node163.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node165.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html2066" HREF="node165.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2064" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2058" HREF="node163.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2067" HREF="node165.html">SLA_REFCO - Refraction Constants</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2065" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2059" HREF="node163.html">SLA_RCC - Barycentric Coordinate Time</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004151000000000000000">&#160;</A><A NAME="xref_SLA_RDPLAN">&#160;</A><A NAME="SLA_RDPLAN">&#160;</A>
+<BR>
+SLA_RDPLAN - Apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> of Planet
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Approximate topocentric apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> and angular
+size of a planet.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_RDPLAN (DATE, NP, ELONG, PHI, RA, DEC, DIAM)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>MJD of observation (JD-2400000.5)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NP</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>planet:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  1=Mercury</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  2=Venus</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  3=Moon</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  4=Mars</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  5=Jupiter</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  6=Saturn</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  7=Uranus</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  8=Neptune</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  9=Pluto</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  else=Sun</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ELONG,PHI</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>observer's longitude (east +ve) and latitude
+(radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RA,DEC</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>topocentric apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DIAM</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>angular diameter (equatorial, radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The date is in a dynamical timescale (TDB, formerly ET)
+and is in the form of a Modified
+Julian Date (JD-2400000.5).  For all practical purposes, TT can
+        be used instead of TDB, and for many applications UT will do
+        (except for the Moon).
+  <DT>2.
+<DD>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 sla_DMOON and sla_PLANET.
+  <DT>3.
+<DD>The direction accuracy (arcsec, 1000-3000AD) is of order:
+        <PRE><TT>
+ 		 Sun 		   5
+		 Mercury 		   2
+		 Venus 		 10
+		 Moon 		 30
+		 Mars 		 50
+		 Jupiter 		 90
+		 Saturn 		 90
+		 Uranus 		 90
+		 Neptune 		 10
+		 Pluto 		  1&nbsp;&nbsp;&nbsp;(1885-2099AD only)        
+</TT></PRE>
+        The angular diameter accuracy is about 0.4% for the Moon,
+        and 0.01% or better for the Sun and planets.
+        For more information on accuracy,
+        refer to the routines sla_PLANET and sla_DMOON,
+        which the present routine uses.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html2066" HREF="node165.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+<BR>
+<B>Up:</B> <A NAME="tex2html2065" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2059" HREF="node163.html">SLA_RCC - Barycentric Coordinate Time</A>
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+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node165.html b/src/slalib/sun67.htx/node165.html
new file mode 100644
index 0000000..1fadca0
--- /dev/null
+++ b/src/slalib/sun67.htx/node165.html
@@ -0,0 +1,176 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
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+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004152000000000000000">SLA_REFCO - Refraction Constants</A>
+<A NAME="xref_SLA_REFCO">&#160;</A><A NAME="SLA_REFCO">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Determine the constants <I>a</I> and <I>b</I> in the
+atmospheric refraction model
+         <IMG WIDTH="164" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img148.gif"
+ ALT="$\Delta \zeta = a \tan \zeta + b \tan^{3} \zeta$">,         where <IMG WIDTH="11" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img149.gif"
+ ALT="$\zeta$"> is the <I>observed</I> zenith distance
+         (<I>i.e.</I> affected by refraction) and <IMG WIDTH="24" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img150.gif"
+ ALT="$\Delta \zeta$"> is
+         what to add to <IMG WIDTH="11" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img149.gif"
+ ALT="$\zeta$"> to give the <I>topocentric</I>
+         (<I>i.e. in vacuo</I>) zenith distance.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_REFCO (HM, TDK, PMB, RH, WL, PHI, TLR, EPS, REFA, REFB)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>HM</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>height of the observer above sea level (metre)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>TDK</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>ambient temperature at the observer (degrees K)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PMB</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>pressure at the observer (mB)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>relative humidity at the observer (range 0-1)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>WL</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>effective wavelength of the source (<IMG WIDTH="26" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img21.gif"
+ ALT="$\mu{\rm m}$">)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PHI</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>latitude of the observer (radian, astronomical)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>TLR</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>temperature lapse rate in the troposphere
+(degrees K per metre)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EPS</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>precision required to terminate iteration (radian)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>REFA</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="37" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img151.gif"
+ ALT="$\tan \zeta$"> coefficient (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>REFB</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="44" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img152.gif"
+ ALT="$\tan^{3} \zeta$"> coefficient (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Suggested values for the TLR and EPS arguments are 0.0065D0 and
+1D-8 respectively.
+<DT>2.
+<DD>The radio refraction is chosen by specifying WL &gt;100&nbsp;<IMG WIDTH="26" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img21.gif"
+ ALT="$\mu{\rm m}$">.  <DT>3.
+<DD>The routine is a slower but more accurate alternative to the
+        sla_REFCOQ routine.  The constants it produces give perfect
+        agreement with sla_REFRO at zenith distances
+        <IMG WIDTH="54" HEIGHT="16" ALIGN="BOTTOM" BORDER="0"
+ SRC="img153.gif"
+ ALT="$\tan^{-1} 1$"> (<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img154.gif"
+ ALT="$45^\circ$">) and <IMG WIDTH="54" HEIGHT="16" ALIGN="BOTTOM" BORDER="0"
+ SRC="img155.gif"
+ ALT="$\tan^{-1} 4$"> (<IMG WIDTH="43" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img156.gif"
+ ALT="$\sim 76^\circ$">).
+        At other zenith distances, the model achieves:
+<P>      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img83.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.5$">    accuracy for <IMG WIDTH="56" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img157.gif"
+ ALT="$\zeta<80^{\circ}$">,<P>      <IMG WIDTH="31" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img158.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.01$">    accuracy for <IMG WIDTH="56" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img159.gif"
+ ALT="$\zeta<60^{\circ}$">, and
+<P>      <IMG WIDTH="39" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img112.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.001$">    accuracy for <IMG WIDTH="56" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img160.gif"
+ ALT="$\zeta<45^{\circ}$">. </DL></DL>
+<BR> <HR>
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+<B> Next:</B> <A NAME="tex2html2077" HREF="node166.html">SLA_REFCOQ - Refraction Constants (fast)</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2075" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2069" HREF="node164.html">SLA_RDPLAN - Apparent of Planet</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node166.html b/src/slalib/sun67.htx/node166.html
new file mode 100644
index 0000000..4dd74d2
--- /dev/null
+++ b/src/slalib/sun67.htx/node166.html
@@ -0,0 +1,428 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_REFCOQ - Refraction Constants (fast)</TITLE>
+<META NAME="description" CONTENT="SLA_REFCOQ - Refraction Constants (fast)">
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+<B> Next:</B> <A NAME="tex2html2087" HREF="node167.html">SLA_REFRO - Refraction</A>
+<BR>
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+<BR>
+<B> Previous:</B> <A NAME="tex2html2079" HREF="node165.html">SLA_REFCO - Refraction Constants</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004153000000000000000">SLA_REFCOQ - Refraction Constants (fast)</A>
+<A NAME="xref_SLA_REFCOQ">&#160;</A><A NAME="SLA_REFCOQ">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Determine the constants <I>a</I> and <I>b</I> in the
+atmospheric refraction model
+         <IMG WIDTH="164" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img148.gif"
+ ALT="$\Delta \zeta = a \tan \zeta + b \tan^{3} \zeta$">,         where <IMG WIDTH="11" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img149.gif"
+ ALT="$\zeta$"> is the <I>observed</I> zenith distance
+         (<I>i.e.</I> affected by refraction) and <IMG WIDTH="24" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img150.gif"
+ ALT="$\Delta \zeta$"> is
+         what to add to <IMG WIDTH="11" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img149.gif"
+ ALT="$\zeta$"> to give the <I>topocentric</I>
+         (<I>i.e. in vacuo</I>) zenith distance. (This is a fast
+         alternative to the sla_REFCO routine - see notes.)
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_REFCOQ (TDK, PMB, RH, WL, REFA, REFB)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>TDK</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>ambient temperature at the observer (degrees K)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PMB</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>pressure at the observer (mB)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>relative humidity at the observer (range 0-1)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>WL</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>effective wavelength of the source (<IMG WIDTH="26" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img21.gif"
+ ALT="$\mu{\rm m}$">)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>REFA</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="37" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img151.gif"
+ ALT="$\tan \zeta$"> coefficient (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>REFB</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="44" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img152.gif"
+ ALT="$\tan^{3} \zeta$"> coefficient (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The radio refraction is chosen by specifying WL &gt;100&nbsp;<IMG WIDTH="26" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img21.gif"
+ ALT="$\mu{\rm m}$">.<DT>2.
+<DD>The model is an approximation, for moderate zenith distances,
+to the predictions of the sla_REFRO routine.  The approximation
+        is maintained across a range of conditions, and applies to
+        both optical/IR and radio.
+  <DT>3.
+<DD>The algorithm is a fast alternative to the sla_REFCO routine.
+        The latter calls the sla_REFRO routine itself:  this involves
+        integrations through a model atmosphere, and is costly in
+        processor time.  However, the model which is produced is precisely
+        correct for two zenith distances (<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img154.gif"
+ ALT="$45^\circ$"> and <IMG WIDTH="40" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img161.gif"
+ ALT="$\sim\!76^\circ$">)        and at other zenith distances is limited in accuracy only by the
+        <IMG WIDTH="164" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img148.gif"
+ ALT="$\Delta \zeta = a \tan \zeta + b \tan^{3} \zeta$"> formulation
+        itself.  The present routine is not as accurate, though it
+        satisfies most practical requirements.
+  <DT>4.
+<DD>The model omits the effects of (i)&nbsp;height above sea level (apart
+        from the reduced pressure itself), (ii)&nbsp;latitude (<I>i.e.</I> the
+        flattening of the Earth) and (iii)&nbsp;variations in tropospheric
+        lapse rate.
+  <DT>5.
+<DD>The model has been tested using the following range of conditions:
+        <DL COMPACT>
+<DT><IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"><DD>lapse rates 0.0055, 0.0065, 0.0075&nbsp;degrees K per metre
+<DT><IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"><DD>latitudes <IMG WIDTH="18" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img1.gif"
+ ALT="$0^{\circ}$">, <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img162.gif"
+ ALT="$25^\circ$">, <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img163.gif"
+ ALT="$50^\circ$">, <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img164.gif"
+ ALT="$75^\circ$">        <DT><IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"><DD>heights 0, 2500, 5000 metres above sea level
+        <DT><IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"><DD>pressures mean for height -10% to +5% in steps of 5%
+        <DT><IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"><DD>temperatures <IMG WIDTH="38" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img165.gif"
+ ALT="$-10^\circ$"> to <IMG WIDTH="38" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img166.gif"
+ ALT="$+20^\circ$"> with respect to
+              <IMG WIDTH="34" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img167.gif"
+ ALT="$280^\circ$">K at sea level
+        <DT><IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"><DD>relative humidity 0, 0.5, 1
+        <DT><IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"><DD>wavelength 0.4, 0.6, ... <IMG WIDTH="34" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img168.gif"
+ ALT="$2\mu{\rm m}$">, + radio
+        <DT><IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"><DD>zenith distances <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img39.gif"
+ ALT="$15^\circ$">, <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img154.gif"
+ ALT="$45^\circ$">, <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img164.gif"
+ ALT="$75^\circ$"></DL>
+        For the above conditions, the comparison with sla_REFRO
+        was as follows:
+<P>        <BR>
+<BR>
+<BR>
+<P>        &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;
+        <TABLE CELLPADDING=3 BORDER="1">
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>&nbsp;</TD>
+<TH ALIGN="RIGHT" NOWRAP><I>worst</I></TH>
+<TH ALIGN="RIGHT" NOWRAP><I>RMS</I></TH>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>optical/IR</TD>
+<TD ALIGN="RIGHT" NOWRAP>62</TD>
+<TD ALIGN="RIGHT" NOWRAP>8</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>radio</TD>
+<TD ALIGN="RIGHT" NOWRAP>319</TD>
+<TD ALIGN="RIGHT" NOWRAP>49</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP>mas</TD>
+<TD ALIGN="RIGHT" NOWRAP>mas</TD>
+</TR>
+</TABLE>
+<P>        <BR>
+<BR>
+<BR>
+<BR>
+<P>
+For this particular set of conditions:
+        <DL COMPACT>
+<DT><IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"><DD>lapse rate <IMG WIDTH="86" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img169.gif"
+ ALT="$6.5^\circ K km^{-1}$"><DT><IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"><DD>latitude <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img163.gif"
+ ALT="$50^\circ$">        <DT><IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"><DD>sea level
+        <DT><IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"><DD>pressure 1005mB
+        <DT><IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"><DD>temperature <IMG WIDTH="18" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img170.gif"
+ ALT="$7^\circ$">C
+        <DT><IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"><DD>humidity 80%
+        <DT><IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"><DD>wavelength 5740A
+        </DL>
+        the results were as follows:
+<P>        <BR>
+<BR>
+<BR>
+<P>        &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;
+        <TABLE CELLPADDING=3 BORDER="1">
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1><IMG WIDTH="11" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img149.gif"
+ ALT="$\zeta$"></TD>
+<TD ALIGN="CENTER" NOWRAP COLSPAN=1>sla_REFRO</TD>
+<TD ALIGN="CENTER" NOWRAP COLSPAN=1>sla_REFCOQ</TD>
+<TD ALIGN="CENTER" NOWRAP COLSPAN=1>Saastamoinen</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>10</TD>
+<TD ALIGN="RIGHT" NOWRAP>10.27</TD>
+<TD ALIGN="RIGHT" NOWRAP>10.27</TD>
+<TD ALIGN="RIGHT" NOWRAP>10.27</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>20</TD>
+<TD ALIGN="RIGHT" NOWRAP>21.19</TD>
+<TD ALIGN="RIGHT" NOWRAP>21.20</TD>
+<TD ALIGN="RIGHT" NOWRAP>21.19</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>30</TD>
+<TD ALIGN="RIGHT" NOWRAP>33.61</TD>
+<TD ALIGN="RIGHT" NOWRAP>33.61</TD>
+<TD ALIGN="RIGHT" NOWRAP>33.60</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>40</TD>
+<TD ALIGN="RIGHT" NOWRAP>48.82</TD>
+<TD ALIGN="RIGHT" NOWRAP>48.83</TD>
+<TD ALIGN="RIGHT" NOWRAP>48.81</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>45</TD>
+<TD ALIGN="RIGHT" NOWRAP>58.16</TD>
+<TD ALIGN="RIGHT" NOWRAP>58.18</TD>
+<TD ALIGN="RIGHT" NOWRAP>58.16</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>50</TD>
+<TD ALIGN="RIGHT" NOWRAP>69.28</TD>
+<TD ALIGN="RIGHT" NOWRAP>69.30</TD>
+<TD ALIGN="RIGHT" NOWRAP>69.27</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>55</TD>
+<TD ALIGN="RIGHT" NOWRAP>82.97</TD>
+<TD ALIGN="RIGHT" NOWRAP>82.99</TD>
+<TD ALIGN="RIGHT" NOWRAP>82.95</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>60</TD>
+<TD ALIGN="RIGHT" NOWRAP>100.51</TD>
+<TD ALIGN="RIGHT" NOWRAP>100.54</TD>
+<TD ALIGN="RIGHT" NOWRAP>100.50</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>65</TD>
+<TD ALIGN="RIGHT" NOWRAP>124.23</TD>
+<TD ALIGN="RIGHT" NOWRAP>124.26</TD>
+<TD ALIGN="RIGHT" NOWRAP>124.20</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>70</TD>
+<TD ALIGN="RIGHT" NOWRAP>158.63</TD>
+<TD ALIGN="RIGHT" NOWRAP>158.68</TD>
+<TD ALIGN="RIGHT" NOWRAP>158.61</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>72</TD>
+<TD ALIGN="RIGHT" NOWRAP>177.32</TD>
+<TD ALIGN="RIGHT" NOWRAP>177.37</TD>
+<TD ALIGN="RIGHT" NOWRAP>177.31</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>74</TD>
+<TD ALIGN="RIGHT" NOWRAP>200.35</TD>
+<TD ALIGN="RIGHT" NOWRAP>200.38</TD>
+<TD ALIGN="RIGHT" NOWRAP>200.32</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>76</TD>
+<TD ALIGN="RIGHT" NOWRAP>229.45</TD>
+<TD ALIGN="RIGHT" NOWRAP>229.43</TD>
+<TD ALIGN="RIGHT" NOWRAP>229.42</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>78</TD>
+<TD ALIGN="RIGHT" NOWRAP>267.44</TD>
+<TD ALIGN="RIGHT" NOWRAP>267.29</TD>
+<TD ALIGN="RIGHT" NOWRAP>267.41</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>80</TD>
+<TD ALIGN="RIGHT" NOWRAP>319.13</TD>
+<TD ALIGN="RIGHT" NOWRAP>318.55</TD>
+<TD ALIGN="RIGHT" NOWRAP>319.10</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>deg</TD>
+<TD ALIGN="RIGHT" NOWRAP>arcsec</TD>
+<TD ALIGN="RIGHT" NOWRAP>arcsec</TD>
+<TD ALIGN="RIGHT" NOWRAP>arcsec</TD>
+</TR>
+</TABLE>
+<P>        <BR>
+<BR>
+<BR>
+<BR>
+<P>
+The values for Saastamoinen's formula (which includes terms
+        up to <IMG WIDTH="33" HEIGHT="16" ALIGN="BOTTOM" BORDER="0"
+ SRC="img171.gif"
+ ALT="$\tan^5$">) are taken from Hohenkerk and Sinclair (1985).
+<P>
+The results from the much slower but more accurate sla_REFCO
+        routine have not been included in the tabulation as they are
+        identical to those in the sla_REFRO column to the 
+      <IMG WIDTH="31" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img158.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.01$"><P>
+resolution used.
+  <DT>6.
+<DD>Outlandish input parameters are silently limited
+        to mathematically safe values.  Zero pressure is permissible,
+        and causes zeroes to be returned.
+  <DT>7.
+<DD>The algorithm draws on several sources, as follows:
+        <UL>
+<LI> The formula for the saturation vapour pressure of water as
+              a function of temperature and temperature is taken from
+              expressions A4.5-A4.7 of Gill (1982).
+<LI> The formula for the water vapour pressure, given the
+              saturation pressure and the relative humidity is from
+              Crane (1976), expression 2.5.5.
+<LI> The refractivity of air is a function of temperature,
+              total pressure, water-vapour pressure and, in the case
+              of optical/IR but not radio, wavelength.  The formulae
+              for the two cases are developed from the Essen and Froome
+              expressions adopted in Resolution 1 of the 12th International
+              Geodesy Association General Assembly (1963).
+        </UL>
+        The above three items are as used in the sla_REFRO routine.
+        <UL>
+<LI> The formula for <IMG WIDTH="91" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img172.gif"
+ ALT="$\beta~(=H_0/r_0)$"> is
+              an adaption of expression 9 from Stone (1996).  The
+              adaptations, arrived at empirically, consist of (i)&nbsp;a
+              small adjustment to the coefficient and (ii)&nbsp;a humidity
+              term for the radio case only.
+<LI> The formulae for the refraction constants as a function of
+              <I>n</I>-1 and <IMG WIDTH="12" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img173.gif"
+ ALT="$\beta$"> are from Green (1987), expression 4.31.
+        </UL></DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Crane, R.K., Meeks, M.L. (ed), ``Refraction Effects in
+the Neutral Atmosphere'',
+<I>Methods of Experimental Physics: Astrophysics 12B,</I>
+        Academic Press, 1976.
+  <DT>2.
+<DD>Gill, Adrian E., <I>Atmosphere-Ocean Dynamics,</I>
+        Academic Press, 1982.
+  <DT>3.
+<DD>Hohenkerk, C.Y., &amp; Sinclair, A.T., NAO Technical Note
+        No.&nbsp;63, 1985.
+  <DT>4.
+<DD>International Geodesy Association General Assembly, Bulletin
+        G&#233;od&#233;sique <B>70</B> p390, 1963.
+  <DT>5.
+<DD>Stone, Ronald C., P.A.S.P.&nbsp;<B>108</B> 1051-1058, 1996.
+  <DT>6.
+<DD>Green, R.M., <I>Spherical Astronomy,</I> Cambridge
+        University Press, 1987.
+ </DL></DL>
+<BR> <HR>
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+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
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+<H2><A NAME="SECTION0004154000000000000000">SLA_REFRO - Refraction</A>
+<A NAME="xref_SLA_REFRO">&#160;</A><A NAME="SLA_REFRO">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Atmospheric refraction, for radio or optical/IR wavelengths.
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_REFRO (ZOBS, HM, TDK, PMB, RH, WL, PHI, TLR, EPS, REF)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ZOBS</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>observed zenith distance of the source (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>HM</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>height of the observer above sea level (metre)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>TDK</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>ambient temperature at the observer (degrees K)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PMB</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>pressure at the observer (mB)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>relative humidity at the observer (range 0-1)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>WL</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>effective wavelength of the source (<IMG WIDTH="26" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img21.gif"
+ ALT="$\mu{\rm m}$">)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PHI</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>latitude of the observer (radian, astronomical)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>TLR</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>temperature lapse rate in the troposphere
+(degrees K per metre)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EPS</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>precision required to terminate iteration (radian)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>REF</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TH ALIGN="LEFT" NOWRAP>refraction: <I>in vacuo</I> ZD minus observed ZD (radians)</TH>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>A suggested value for the TLR argument is 0.0065D0.  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.
+  <DT>2.
+<DD>A suggested value for the EPS argument is 1D-8.  The result is
+        usually at least two orders of magnitude more computationally
+        precise than the supplied EPS value.
+  <DT>3.
+<DD>The routine computes the refraction for zenith distances up
+        to and a little beyond <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img22.gif"
+ ALT="$90^{\circ}$"> using the method of Hohenkerk
+        &amp; Sinclair (NAO Technical Notes 59 and 63, subsequently adopted
+        in the <I>Explanatory Supplement to the Astronomical Almanac,</I>
+        1992 - see section 3.281).
+  <DT>4.
+<DD>The code is based on the AREF optical/IR refraction subroutine
+        of C.Hohenkerk (HMNAO, September 1984), with extensions to
+        support the radio case.  The modifications to the original HMNAO
+        optical/IR refraction code which affect the results are:
+        <UL>
+<LI> Murray's values for the gas constants have been used
+               (<I>Vectorial Astrometry,</I> Adam Hilger, 1983).
+<LI> A better model for <I>P</I><SUB><I>s</I></SUB>(<I>T</I>) has been adopted (taken from
+               Gill, <I>Atmosphere-Ocean Dynamics,</I> Academic Press, 1982).
+<LI> More accurate expressions for <I>Pw</I><SUB><I>o</I></SUB> have been adopted
+               (again from Gill 1982).
+<LI> Provision for radio wavelengths has been added using
+               expressions devised by A.T.Sinclair, RGO (private
+               communication 1989), based on the Essen &amp; Froome
+               refractivity formula adopted in Resolution&nbsp;1 of the
+               12th International Geodesy Association General Assembly
+               (Bulletin G&#233;od&#233;sique <B>70</B> p390, 1963).
+        </UL>
+        None of the changes significantly affects the optical/IR results
+        with respect to the algorithm given in the 1992 <I>Explanatory
+        Supplement.</I>  For example, at <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img174.gif"
+ ALT="$70^\circ$"> zenith distance the present
+        routine agrees with the ES algorithm to better than 
+      <IMG WIDTH="31" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img175.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.05$"><P>
+for any reasonable combination of parameters.  However, the
+        improved water-vapour expressions do make a significant difference
+        in the radio band, at <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img174.gif"
+ ALT="$70^\circ$"> zenith distance reaching almost
+        <IMG WIDTH="17" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img130.gif"
+ ALT="$4\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> for a hot, humid, low-altitude site during a period of
+        low pressure.
+  <DT>5.
+<DD>The radio refraction is chosen by specifying WL &gt;100&nbsp;<IMG WIDTH="26" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img21.gif"
+ ALT="$\mu{\rm m}$">.        Because the algorithm takes no account of the ionosphere, the
+        accuracy deteriorates at low frequencies, below about 30MHz.
+  <DT>6.
+<DD>Before use, the value of ZOBS is expressed in the range <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$">.        If this ranged ZOBS is negative, the result REF is computed from its
+        absolute value before being made negative to match.  In addition, if
+        it has an absolute value greater than <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img176.gif"
+ ALT="$93^\circ$">, a fixed REF value
+        equal to the result for ZOBS&nbsp;<IMG WIDTH="43" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img177.gif"
+ ALT="$=93^\circ$"> is returned, appropriately
+        signed.
+  <DT>7.
+<DD>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.
+  <DT>8.
+<DD>The radio refraction has been tested against work done by
+        Iain&nbsp;Coulson, JACH, (private communication 1995) for the
+        James Clerk Maxwell Telescope, Mauna Kea.  For typical conditions,
+        agreement at the 
+      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img25.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.1$">    level is achieved for moderate ZD,
+        worsening to perhaps 
+      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img83.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.5$">   -
+      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img178.gif"
+ ALT="$1\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.0$">    at ZD <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img179.gif"
+ ALT="$80^\circ$">.        At hot and humid sea-level sites the accuracy will not be as good.
+  <DT>9.
+<DD>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 familiar
+        <IMG WIDTH="75" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img180.gif"
+ ALT="$\nu=p_w/p_s$"> or <IMG WIDTH="75" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img181.gif"
+ ALT="$\nu=\rho_w/\rho_s$"> expressions can differ from
+        the formal definition by several percent, significant in the
+        radio case.
+  </DL></DL>
+<BR> <HR>
+<A NAME="tex2html2096" HREF="node168.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2094" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2088" HREF="node166.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2097" HREF="node168.html">SLA_REFV - Apply Refraction to Vector</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2095" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2089" HREF="node166.html">SLA_REFCOQ - Refraction Constants (fast)</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node168.html b/src/slalib/sun67.htx/node168.html
new file mode 100644
index 0000000..c695ed9
--- /dev/null
+++ b/src/slalib/sun67.htx/node168.html
@@ -0,0 +1,276 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_REFV - Apply Refraction to Vector</TITLE>
+<META NAME="description" CONTENT="SLA_REFV - Apply Refraction to Vector">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2107" HREF="node169.html">SLA_REFZ - Apply Refraction to ZD</A>
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+<B>Up:</B> <A NAME="tex2html2105" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2099" HREF="node167.html">SLA_REFRO - Refraction</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004155000000000000000">SLA_REFV - Apply Refraction to Vector</A>
+<A NAME="xref_SLA_REFV">&#160;</A><A NAME="SLA_REFV">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Adjust an unrefracted Cartesian vector to include the effect of
+atmospheric refraction, using the simple
+         <IMG WIDTH="164" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img148.gif"
+ ALT="$\Delta \zeta = a \tan \zeta + b \tan^{3} \zeta$"> model.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_REFV (VU, REFA, REFB, VR)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>VU</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>unrefracted position of the source (<IMG WIDTH="66" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img28.gif"
+ ALT="$[\,Az,El~]$"> 3-vector)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>REFA</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="37" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img151.gif"
+ ALT="$\tan \zeta$"> coefficient (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>REFB</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="44" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img152.gif"
+ ALT="$\tan^{3} \zeta$"> coefficient (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>VR</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>refracted position of the source (<IMG WIDTH="66" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img28.gif"
+ ALT="$[\,Az,El~]$"> 3-vector)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>This routine applies the adjustment for refraction in the
+opposite sense to the usual one - it takes an unrefracted
+(<I>in vacuo</I>) position and produces an observed (refracted)
+        position, whereas the
+        <IMG WIDTH="164" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img148.gif"
+ ALT="$\Delta \zeta = a \tan \zeta + b \tan^{3} \zeta$">        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.
+  <DT>2.
+<DD>Though optimized for speed rather than precision, the present
+        routine achieves consistency with the refracted-to-unrefracted
+        <IMG WIDTH="164" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img148.gif"
+ ALT="$\Delta \zeta = a \tan \zeta + b \tan^{3} \zeta$">        model at better than 1&nbsp;microarcsecond within
+        <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img182.gif"
+ ALT="$30^\circ$"> of the zenith and remains within 1&nbsp;milliarcsecond to
+        <IMG WIDTH="56" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img183.gif"
+ ALT="$\zeta=70^\circ$">.  The inherent accuracy of the model is, of
+        course, far worse than this - see the documentation for sla_REFCO
+        for more information.
+  <DT>3.
+<DD>At low elevations (below about <IMG WIDTH="18" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img27.gif"
+ ALT="$3^{\circ}$">) the refraction
+        correction is held back to prevent arithmetic problems and
+        wildly wrong results.  Over a wide range of observer heights
+        and corresponding temperatures and pressures, the following
+        levels of accuracy are achieved, relative to numerical
+        integration through a model atmosphere:
+<P>        <DIV ALIGN="CENTER">
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img184.gif"
+ ALT="$\zeta_{obs}$"></TD>
+<TH ALIGN="CENTER" NOWRAP><I>error</I></TH>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+<TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img179.gif"
+ ALT="$80^\circ$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img185.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.4$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img186.gif"
+ ALT="$81^\circ$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img187.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.8$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img188.gif"
+ ALT="$82^\circ$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img189.gif"
+ ALT="$1\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.6$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img190.gif"
+ ALT="$83^\circ$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="17" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img75.gif"
+ ALT="$3\hspace{-0.05em}^{'\hspace{-0.1em}'}$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img191.gif"
+ ALT="$84^\circ$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="17" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img192.gif"
+ ALT="$7\hspace{-0.05em}^{'\hspace{-0.1em}'}$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img193.gif"
+ ALT="$85^\circ$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img133.gif"
+ ALT="$17\hspace{-0.05em}^{'\hspace{-0.1em}'}$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img194.gif"
+ ALT="$86^\circ$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img195.gif"
+ ALT="$45\hspace{-0.05em}^{'\hspace{-0.1em}'}$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img196.gif"
+ ALT="$87^\circ$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="33" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img197.gif"
+ ALT="$150\hspace{-0.05em}^{'\hspace{-0.1em}'}$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img198.gif"
+ ALT="$88^\circ$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="33" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img199.gif"
+ ALT="$340\hspace{-0.05em}^{'\hspace{-0.1em}'}$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img200.gif"
+ ALT="$89^\circ$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="33" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img201.gif"
+ ALT="$620\hspace{-0.05em}^{'\hspace{-0.1em}'}$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img22.gif"
+ ALT="$90^{\circ}$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="41" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img202.gif"
+ ALT="$1100\hspace{-0.05em}^{'\hspace{-0.1em}'}$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img203.gif"
+ ALT="$91^\circ$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="41" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img204.gif"
+ ALT="$1900\hspace{-0.05em}^{'\hspace{-0.1em}'}$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&lt; high-altitude</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img205.gif"
+ ALT="$92^\circ$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="41" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img206.gif"
+ ALT="$3200\hspace{-0.05em}^{'\hspace{-0.1em}'}$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&lt; sites only</TD>
+</TR>
+</TABLE></DIV>
+  <DT>4.
+<DD>See also the routine sla_REFZ, which performs the adjustment to
+        the zenith distance rather than in <IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$">.        The present routine is faster than sla_REFZ and,
+        except very low down,
+        is equally accurate for all practical purposes.  However, beyond
+        about <IMG WIDTH="56" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img207.gif"
+ ALT="$\zeta=84^\circ$"> sla_REFZ should be used, and for the utmost
+        accuracy iterative use of sla_REFRO should be considered.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html2106" HREF="node169.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2107" HREF="node169.html">SLA_REFZ - Apply Refraction to ZD</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2105" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2099" HREF="node167.html">SLA_REFRO - Refraction</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node169.html b/src/slalib/sun67.htx/node169.html
new file mode 100644
index 0000000..6180ab0
--- /dev/null
+++ b/src/slalib/sun67.htx/node169.html
@@ -0,0 +1,275 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_REFZ - Apply Refraction to ZD</TITLE>
+<META NAME="description" CONTENT="SLA_REFZ - Apply Refraction to ZD">
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+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2114" HREF="node13.html">
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+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2117" HREF="node170.html">SLA_RVEROT - RV Corrn to Earth Centre</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2115" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2109" HREF="node168.html">SLA_REFV - Apply Refraction to Vector</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004156000000000000000">SLA_REFZ - Apply Refraction to ZD</A>
+<A NAME="xref_SLA_REFZ">&#160;</A><A NAME="SLA_REFZ">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Adjust an unrefracted zenith distance to include the effect of
+atmospheric refraction, using the simple
+         <IMG WIDTH="164" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img148.gif"
+ ALT="$\Delta \zeta = a \tan \zeta + b \tan^{3} \zeta$"> model.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_REFZ (ZU, REFA, REFB, ZR)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ZU</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>unrefracted zenith distance of the source (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>REFA</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="37" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img151.gif"
+ ALT="$\tan \zeta$"> coefficient (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>REFB</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="44" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img152.gif"
+ ALT="$\tan^{3} \zeta$"> coefficient (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ZR</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>refracted zenith distance (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>This routine applies the adjustment for refraction in the
+opposite sense to the usual one - it takes an unrefracted
+(<I>in vacuo</I>) position and produces an observed (refracted)
+        position, whereas the
+        <IMG WIDTH="164" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img148.gif"
+ ALT="$\Delta \zeta = a \tan \zeta + b \tan^{3} \zeta$">        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 10<SUP>-11</SUP>&nbsp;arcsecond level
+        for <IMG WIDTH="56" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img208.gif"
+ ALT="$\zeta=80^\circ$">.  The inherent accuracy of the model
+        is, of course, far worse than this - see the documentation for
+        sla_REFCO for more information.
+  <DT>2.
+<DD>At <IMG WIDTH="56" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img209.gif"
+ ALT="$\zeta=83^\circ$">, the rapidly-worsening
+        <IMG WIDTH="164" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img148.gif"
+ ALT="$\Delta \zeta = a \tan \zeta + b \tan^{3} \zeta$">        model is abandoned and an empirical formula takes over:
+<P>          
+<P ALIGN="CENTER"><IMG WIDTH="321" HEIGHT="49"
+ SRC="img210.gif"
+ ALT="\begin{displaymath}
+\Delta \zeta = F \left(
+ \frac{0^\circ\hspace{-0.37em}.\hspa...
+ ...hspace{0.02em}00202 E^2}
+ {1 + 0.28385 E +0.02390 E^2} \right) \end{displaymath}"></P>
+where <IMG WIDTH="113" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img211.gif"
+ ALT="$E=90^\circ-\zeta_{true}$">        and <I>F</I> is a factor chosen to meet the
+        <IMG WIDTH="164" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img148.gif"
+ ALT="$\Delta \zeta = a \tan \zeta + b \tan^{3} \zeta$">        formula at <IMG WIDTH="56" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img209.gif"
+ ALT="$\zeta=83^\circ$">.  Over a
+        wide range of observer heights and corresponding temperatures and
+        pressures, the following levels of accuracy are achieved,
+        relative to numerical integration through a model atmosphere:
+<P>        <DIV ALIGN="CENTER">
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img184.gif"
+ ALT="$\zeta_{obs}$"></TD>
+<TH ALIGN="CENTER" NOWRAP><I>error</I></TH>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+<TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img179.gif"
+ ALT="$80^\circ$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img185.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.4$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img186.gif"
+ ALT="$81^\circ$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img187.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.8$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img188.gif"
+ ALT="$82^\circ$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img212.gif"
+ ALT="$1\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.5$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img190.gif"
+ ALT="$83^\circ$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img213.gif"
+ ALT="$3\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.2$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img191.gif"
+ ALT="$84^\circ$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img214.gif"
+ ALT="$4\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.9$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img193.gif"
+ ALT="$85^\circ$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img215.gif"
+ ALT="$5\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.8$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img194.gif"
+ ALT="$86^\circ$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img216.gif"
+ ALT="$6\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.1$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img196.gif"
+ ALT="$87^\circ$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img217.gif"
+ ALT="$7\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.1$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img198.gif"
+ ALT="$88^\circ$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="25" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img43.gif"
+ ALT="$11\hspace{-0.05em}^{'\hspace{-0.1em}'}$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img200.gif"
+ ALT="$89^\circ$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="25" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img218.gif"
+ ALT="$21\hspace{-0.05em}^{'\hspace{-0.1em}'}$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img22.gif"
+ ALT="$90^{\circ}$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img219.gif"
+ ALT="$43\hspace{-0.05em}^{'\hspace{-0.1em}'}$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img203.gif"
+ ALT="$91^\circ$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img220.gif"
+ ALT="$92\hspace{-0.05em}^{'\hspace{-0.1em}'}$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&lt; high-altitude</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img205.gif"
+ ALT="$92^\circ$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="33" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img221.gif"
+ ALT="$220\hspace{-0.05em}^{'\hspace{-0.1em}'}$"></TD>
+<TD ALIGN="LEFT" NOWRAP>&lt; sites only</TD>
+</TR>
+</TABLE></DIV>
+  <DT>3.
+<DD>See also the routine sla_REFV, which performs the adjustment in
+        <IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$">, and with the emphasis on speed rather than numerical accuracy.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html2116" HREF="node170.html">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2117" HREF="node170.html">SLA_RVEROT - RV Corrn to Earth Centre</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2115" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
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+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
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+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
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+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
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+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
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+<HEAD>
+<TITLE>SLA_ALTAZ - Velocities etc. for Altazimuth Mount</TITLE>
+<META NAME="description" CONTENT="SLA_ALTAZ - Velocities etc. for Altazimuth Mount">
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+<H2><A NAME="SECTION00044000000000000000">SLA_ALTAZ - Velocities <I>etc.</I> for Altazimuth Mount</A>
+<A NAME="xref_SLA_ALTAZ">&#160;</A><A NAME="SLA_ALTAZ">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Positions, velocities and accelerations for an altazimuth
+telescope mount tracking a star (double precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_ALTAZ (
+         HA, DEC, PHI,
+         AZ, AZD, AZDD, EL, ELD, ELDD, PA, PAD, PADD)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>HA</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>hour angle</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DEC</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>declination</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PHI</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>observatory latitude</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AZ</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>azimuth</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AZD</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>azimuth velocity</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AZDD</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>azimuth acceleration</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EL</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>elevation</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ELD</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>elevation velocity</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ELDD</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>elevation acceleration</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PA</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>parallactic angle</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PAD</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>parallactic angle velocity</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PADD</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>parallactic angle acceleration</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>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:
+<P>        <DIV ALIGN="CENTER">
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>angles</TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="66" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img9.gif"
+ ALT="$\times 360/2\pi$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="19" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img10.gif"
+ ALT="$\rightarrow$"></TD>
+<TD ALIGN="LEFT" NOWRAP>degrees</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>velocities</TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="178" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img11.gif"
+ ALT="$\times (2\pi/86400) \times (360/2\pi)$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="19" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img10.gif"
+ ALT="$\rightarrow$"></TD>
+<TD ALIGN="LEFT" NOWRAP>degree/sec</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>accelerations</TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="186" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img12.gif"
+ ALT="$\times (2\pi/86400)^2 \times (360/2\pi)$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="19" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img10.gif"
+ ALT="$\rightarrow$"></TD>
+<TD ALIGN="LEFT" NOWRAP>degree/sec/sec</TD>
+</TR>
+</TABLE></DIV>
+<P>
+Note that the seconds here are sidereal rather than SI.  One
+        sidereal second is about 0.99727 SI seconds.
+<P>
+The velocity and acceleration factors assume the sidereal
+        tracking case.  Their respective numerical values are (exactly)
+        1/240 and (approximately) 1/3300236.9.
+  <DT>2.
+<DD>Azimuth is returned in the range <IMG WIDTH="50" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img13.gif"
+ ALT="$[\,0,2\pi\,]$">;  north is zero,
+        and east is <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img14.gif"
+ ALT="$+\pi/2$">.  Elevation and parallactic angle are
+        returned in the range <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img15.gif"
+ ALT="$\pm\pi/2$">.  Position angle is +ve
+        for a star west of the meridian and is the angle NP-star-zenith.
+  <DT>3.
+<DD>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.
+  <DT>4.
+<DD>No range checking of arguments is carried out.
+  <DT>5.
+<DD>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.
+ </DL></DL>
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+<A NAME="tex2html588" HREF="node16.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html597" HREF="node18.html">SLA_AMP - Apparent to Mean</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html595" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html589" HREF="node16.html">SLA_AIRMAS - Air Mass</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node170.html b/src/slalib/sun67.htx/node170.html
new file mode 100644
index 0000000..3f0f1a1
--- /dev/null
+++ b/src/slalib/sun67.htx/node170.html
@@ -0,0 +1,111 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_RVEROT - RV Corrn to Earth Centre</TITLE>
+<META NAME="description" CONTENT="SLA_RVEROT - RV Corrn to Earth Centre">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
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+<LINK REL="previous" HREF="node169.html">
+<LINK REL="up" HREF="node13.html">
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+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html2126" HREF="node171.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2124" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2118" HREF="node169.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2127" HREF="node171.html">SLA_RVGALC - RV Corrn to Galactic Centre</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2125" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2119" HREF="node169.html">SLA_REFZ - Apply Refraction to ZD</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004157000000000000000">SLA_RVEROT - RV Corrn to Earth Centre</A>
+<A NAME="xref_SLA_RVEROT">&#160;</A><A NAME="SLA_RVEROT">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Velocity component in a given direction due to Earth rotation.
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>R&nbsp;=&nbsp;sla_RVEROT (PHI, RA, DA, ST)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PHI</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>geodetic latitude of observing station (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RA,DA</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ST</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>local apparent sidereal time (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_RVEROT</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>Component of Earth rotation in
+direction RA,DA (km&nbsp;s<SUP>-1</SUP>)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Sign convention: the result is positive when the observatory
+is receding from the given point on the sky.
+<DT>2.
+<DD>Accuracy: the simple algorithm used assumes a spherical Earth and
+        an observing station at sea level;  for actual observing
+        sites, the error is unlikely to be greater than 0.0005&nbsp;km&nbsp;s<SUP>-1</SUP>.
+        For applications requiring greater precision, use the routine
+        sla_PVOBS.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html2126" HREF="node171.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2124" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2118" HREF="node169.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2127" HREF="node171.html">SLA_RVGALC - RV Corrn to Galactic Centre</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2125" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2119" HREF="node169.html">SLA_REFZ - Apply Refraction to ZD</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node171.html b/src/slalib/sun67.htx/node171.html
new file mode 100644
index 0000000..307d861
--- /dev/null
+++ b/src/slalib/sun67.htx/node171.html
@@ -0,0 +1,115 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_RVGALC - RV Corrn to Galactic Centre</TITLE>
+<META NAME="description" CONTENT="SLA_RVGALC - RV Corrn to Galactic Centre">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
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+<LINK REL="previous" HREF="node170.html">
+<LINK REL="up" HREF="node13.html">
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+</HEAD>
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+<BR> <HR>
+<A NAME="tex2html2136" HREF="node172.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2134" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2128" HREF="node170.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2137" HREF="node172.html">SLA_RVLG - RV Corrn to Local Group</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2135" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2129" HREF="node170.html">SLA_RVEROT - RV Corrn to Earth Centre</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004158000000000000000">SLA_RVGALC - RV Corrn to Galactic Centre</A>
+<A NAME="xref_SLA_RVGALC">&#160;</A><A NAME="SLA_RVGALC">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Velocity component in a given direction due to the rotation
+of the Galaxy.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>R&nbsp;=&nbsp;sla_RVGALC (R2000, D2000)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>R2000,D2000</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 mean <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_RVGALC</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>Component of dynamical LSR motion in direction
+R2000,D2000 (km&nbsp;s<SUP>-1</SUP>)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Sign convention: the result is positive when the LSR
+is receding from the given point on the sky.
+<DT>2.
+<DD>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 <I>dynamical</I> LSR,
+        it is not to be confused with a <I>kinematical</I> LSR, which
+        is the mean standard of rest of star catalogues or stellar
+        populations.
+  <DT>3.
+<DD>The dynamical LSR velocity due to Galactic rotation is assumed to
+        be 220&nbsp;km&nbsp;s<SUP>-1</SUP> towards <IMG WIDTH="64" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img222.gif"
+ ALT="$l^{I\!I}=90^{\circ}$">,                                   <IMG WIDTH="51" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img223.gif"
+ ALT="$b^{I\!I}=0$">. </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Kerr &amp; Lynden-Bell (1986), MNRAS, 221, p1023.
+</DL>
+<BR> <HR>
+<A NAME="tex2html2136" HREF="node172.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2134" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2128" HREF="node170.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2137" HREF="node172.html">SLA_RVLG - RV Corrn to Local Group</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2135" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2129" HREF="node170.html">SLA_RVEROT - RV Corrn to Earth Centre</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node172.html b/src/slalib/sun67.htx/node172.html
new file mode 100644
index 0000000..561680e
--- /dev/null
+++ b/src/slalib/sun67.htx/node172.html
@@ -0,0 +1,101 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_RVLG - RV Corrn to Local Group</TITLE>
+<META NAME="description" CONTENT="SLA_RVLG - RV Corrn to Local Group">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
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+<LINK REL="previous" HREF="node171.html">
+<LINK REL="up" HREF="node13.html">
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+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html2146" HREF="node173.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2144" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2138" HREF="node171.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2147" HREF="node173.html">SLA_RVLSRD - RV Corrn to Dynamical LSR</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2145" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2139" HREF="node171.html">SLA_RVGALC - RV Corrn to Galactic Centre</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004159000000000000000">SLA_RVLG - RV Corrn to Local Group</A>
+<A NAME="xref_SLA_RVLG">&#160;</A><A NAME="SLA_RVLG">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>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.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>R&nbsp;=&nbsp;sla_RVLG (R2000, D2000)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>R2000,D2000</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 mean <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_RVLG</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TH ALIGN="LEFT" NOWRAP>Component of <B>solar</B> (<I>n.b.</I>)
+motion in direction R2000,D2000 (km&nbsp;s<SUP>-1</SUP>)</TH>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTE:</STRONG>
+<DD>Sign convention: the result is positive when
+the Sun is receding from the given point on the sky.
+      </DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD><I>IAU Trans.</I> 1976. <B>16B</B>, p201.
+</DL>
+<BR> <HR>
+<A NAME="tex2html2146" HREF="node173.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2144" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2138" HREF="node171.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2147" HREF="node173.html">SLA_RVLSRD - RV Corrn to Dynamical LSR</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2145" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2139" HREF="node171.html">SLA_RVGALC - RV Corrn to Galactic Centre</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node173.html b/src/slalib/sun67.htx/node173.html
new file mode 100644
index 0000000..2ae01da
--- /dev/null
+++ b/src/slalib/sun67.htx/node173.html
@@ -0,0 +1,121 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_RVLSRD - RV Corrn to Dynamical LSR</TITLE>
+<META NAME="description" CONTENT="SLA_RVLSRD - RV Corrn to Dynamical LSR">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
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+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
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+<LINK REL="next" HREF="node174.html">
+<LINK REL="previous" HREF="node172.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node174.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html2156" HREF="node174.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2154" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2148" HREF="node172.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2157" HREF="node174.html">SLA_RVLSRK - RV Corrn to Kinematical LSR</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2155" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2149" HREF="node172.html">SLA_RVLG - RV Corrn to Local Group</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004160000000000000000">SLA_RVLSRD - RV Corrn to Dynamical LSR</A>
+<A NAME="xref_SLA_RVLSRD">&#160;</A><A NAME="SLA_RVLSRD">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Velocity component in a given direction due to the Sun's
+motion with respect to the ``dynamical'' Local Standard of Rest.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>R&nbsp;=&nbsp;sla_RVLSRD (R2000, D2000)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>R2000,D2000</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 mean <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_RVLSRD</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TH ALIGN="LEFT" NOWRAP>Component of <I>peculiar</I> solar motion
+in direction R2000,D2000 (km&nbsp;s<SUP>-1</SUP>)</TH>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Sign convention: the result is positive when
+the Sun is receding from the given point on the sky.
+<DT>2.
+<DD>The Local Standard of Rest used here is the <I>dynamical</I> 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 <I>peculiar</I> solar
+        motion.
+  <DT>3.
+<DD>There is another type of LSR, called a <I>kinematical</I> 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
+        <I>standard</I> solar motion.
+        The dynamical LSR is seldom used by observational astronomers,
+        who conventionally use a kinematical LSR such as the one implemented
+        in the routine sla_RVLSRK.
+  <DT>4.
+<DD>The peculiar solar motion is from Delhaye (1965), in <I>Stars
+        and Stellar Systems</I>, vol&nbsp;5, p73:  in Galactic Cartesian
+        coordinates (+9,+12,+7)&nbsp;km&nbsp;s<SUP>-1</SUP>.
+        This corresponds to about 16.6&nbsp;km&nbsp;s<SUP>-1</SUP>
+        towards Galactic coordinates <IMG WIDTH="148" HEIGHT="32" ALIGN="MIDDLE" BORDER="0"
+ SRC="img224.gif"
+ ALT="$l^{I\!I}=53^{\circ},b^{I\!I}=+25^{\circ}$">. </DL></DL>
+<BR> <HR>
+<A NAME="tex2html2156" HREF="node174.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2154" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2148" HREF="node172.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2157" HREF="node174.html">SLA_RVLSRK - RV Corrn to Kinematical LSR</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2155" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2149" HREF="node172.html">SLA_RVLG - RV Corrn to Local Group</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node174.html b/src/slalib/sun67.htx/node174.html
new file mode 100644
index 0000000..f243766
--- /dev/null
+++ b/src/slalib/sun67.htx/node174.html
@@ -0,0 +1,126 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_RVLSRK - RV Corrn to Kinematical LSR</TITLE>
+<META NAME="description" CONTENT="SLA_RVLSRK - RV Corrn to Kinematical LSR">
+<META NAME="keywords" CONTENT="sun67">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2167" HREF="node175.html">SLA_S2TP - Spherical to Tangent Plane</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2165" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2159" HREF="node173.html">SLA_RVLSRD - RV Corrn to Dynamical LSR</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004161000000000000000">SLA_RVLSRK - RV Corrn to Kinematical LSR</A>
+<A NAME="xref_SLA_RVLSRK">&#160;</A><A NAME="SLA_RVLSRK">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Velocity component in a given direction due to the Sun's
+motion with respect to a kinematical Local Standard of Rest.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>R&nbsp;=&nbsp;sla_RVLSRK (R2000, D2000)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>R2000,D2000</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 mean <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_RVLSRK</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TH ALIGN="LEFT" NOWRAP>Component of <I>standard</I> solar motion
+in direction R2000,D2000 (km&nbsp;s<SUP>-1</SUP>)</TH>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Sign convention: the result is positive when
+the Sun is receding from the given point on the sky.
+<DT>2.
+<DD>The Local Standard of Rest used here is one of several
+        <I>kinematical</I> 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 <I>standard</I> solar motion.
+  <DT>3.
+<DD>There is another sort of LSR, seldom used by observational
+        astronomers, called the <I>dynamical</I> LSR.  This 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 <I>peculiar</I> solar motion.  To
+        obtain a radial velocity correction with respect to the
+        dynamical LSR use the routine sla_RVLSRD.
+  <DT>4.
+<DD>The adopted standard solar motion is 20&nbsp;km&nbsp;s<SUP>-1</SUP>
+        towards <IMG WIDTH="132" HEIGHT="33" ALIGN="MIDDLE" BORDER="0"
+ SRC="img225.gif"
+ ALT="$\alpha=18^{\rm h},\delta=+30^{\circ}$"> (1900).
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Delhaye (1965), in <I>Stars and Stellar Systems</I>, vol&nbsp;5, p73.
+<DT>2.
+<DD><I>Methods of Experimental Physics</I> (ed Meeks), vol&nbsp;12,
+part&nbsp;C, sec&nbsp;6.1.5.2, p281.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html2166" HREF="node175.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2164" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2158" HREF="node173.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2167" HREF="node175.html">SLA_S2TP - Spherical to Tangent Plane</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2165" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2159" HREF="node173.html">SLA_RVLSRD - RV Corrn to Dynamical LSR</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node175.html b/src/slalib/sun67.htx/node175.html
new file mode 100644
index 0000000..5c3e6c7
--- /dev/null
+++ b/src/slalib/sun67.htx/node175.html
@@ -0,0 +1,129 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_S2TP - Spherical to Tangent Plane</TITLE>
+<META NAME="description" CONTENT="SLA_S2TP - Spherical to Tangent Plane">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
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+<LINK REL="up" HREF="node13.html">
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+<BODY >
+<BR> <HR>
+<A NAME="tex2html2176" HREF="node176.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2174" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2168" HREF="node174.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2177" HREF="node176.html">SLA_SEP - Angle Between 2 Points on Sphere</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2175" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2169" HREF="node174.html">SLA_RVLSRK - RV Corrn to Kinematical LSR</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004162000000000000000">SLA_S2TP - Spherical to Tangent Plane</A>
+<A NAME="xref_SLA_S2TP">&#160;</A><A NAME="SLA_S2TP">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Projection of spherical coordinates onto the tangent plane
+(single precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_S2TP (RA, DEC, RAZ, DECZ, XI, ETA, J)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RA,DEC</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>spherical coordinates of star (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RAZ,DECZ</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>spherical coordinates of tangent point (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>XI,ETA</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>tangent plane coordinates (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  0 = OK, star on tangent plane</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  1 = error, star too far from axis</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  2 = error, antistar on tangent plane</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  3 = error, antistar too far from axis</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The projection is called the <I>gnomonic</I> projection;  the
+Cartesian coordinates <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img85.gif"
+ ALT="$[\,\xi,\eta\,]$"> are called 
+<I>standard coordinates.</I>  The latter
+        are in units of the distance from the tangent plane to the projection
+        point, <I>i.e.</I> radians near the origin.
+  <DT>2.
+<DD>When working in <IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$"> rather than spherical coordinates, the
+        equivalent Cartesian routine sla_V2TP is available.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html2176" HREF="node176.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2174" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2168" HREF="node174.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2177" HREF="node176.html">SLA_SEP - Angle Between 2 Points on Sphere</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2175" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2169" HREF="node174.html">SLA_RVLSRK - RV Corrn to Kinematical LSR</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node176.html b/src/slalib/sun67.htx/node176.html
new file mode 100644
index 0000000..a12d2ab
--- /dev/null
+++ b/src/slalib/sun67.htx/node176.html
@@ -0,0 +1,100 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_SEP - Angle Between 2 Points on Sphere</TITLE>
+<META NAME="description" CONTENT="SLA_SEP - Angle Between 2 Points on Sphere">
+<META NAME="keywords" CONTENT="sun67">
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+<BODY >
+<BR> <HR>
+<A NAME="tex2html2186" HREF="node177.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2184" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2178" HREF="node175.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2187" HREF="node177.html">SLA_SMAT - Solve Simultaneous Equations</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2185" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2179" HREF="node175.html">SLA_S2TP - Spherical to Tangent Plane</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004163000000000000000">SLA_SEP - Angle Between 2 Points on Sphere</A>
+<A NAME="xref_SLA_SEP">&#160;</A><A NAME="SLA_SEP">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Angle between two points on a sphere (single precision).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>R&nbsp;=&nbsp;sla_SEP (A1, B1, A2, B2)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A1,B1</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>spherical coordinates of one point (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A2,B2</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>spherical coordinates of the other point (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_SEP</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>angle between [A1,B1] and [A2,B2] in radians</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The spherical coordinates are right ascension and declination,
+longitude and latitude, <I>etc.</I> in radians.
+<DT>2.
+<DD>The result is always positive.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html2186" HREF="node177.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2184" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2178" HREF="node175.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2187" HREF="node177.html">SLA_SMAT - Solve Simultaneous Equations</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2185" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2179" HREF="node175.html">SLA_S2TP - Spherical to Tangent Plane</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node177.html b/src/slalib/sun67.htx/node177.html
new file mode 100644
index 0000000..733a9c6
--- /dev/null
+++ b/src/slalib/sun67.htx/node177.html
@@ -0,0 +1,152 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_SMAT - Solve Simultaneous Equations</TITLE>
+<META NAME="description" CONTENT="SLA_SMAT - Solve Simultaneous Equations">
+<META NAME="keywords" CONTENT="sun67">
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+<META NAME="distribution" CONTENT="global">
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+<LINK REL="previous" HREF="node176.html">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2197" HREF="node178.html">SLA_SUBET - Remove E-terms</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2195" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2189" HREF="node176.html">SLA_SEP - Angle Between 2 Points on Sphere</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004164000000000000000">SLA_SMAT - Solve Simultaneous Equations</A>
+<A NAME="xref_SLA_SMAT">&#160;</A><A NAME="SLA_SMAT">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Matrix inversion and solution of simultaneous equations
+(single precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_SMAT (N, A, Y, D, JF, IW)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>N</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>number of unknowns</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A</EM></TD>
+<TD ALIGN="LEFT"><B>R(N,N)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>matrix</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>Y</EM></TD>
+<TD ALIGN="LEFT"><B>R(N)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>vector</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A</EM></TD>
+<TH ALIGN="LEFT"><B>R(N,N)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>matrix inverse</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>Y</EM></TD>
+<TD ALIGN="LEFT"><B>R(N)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>solution</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>D</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>determinant</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JF</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>singularity flag: 0=OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IW</EM></TD>
+<TD ALIGN="LEFT"><B>I(N)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>workspace</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>For the set of <I>n</I> simultaneous linear equations in <I>n</I> unknowns:
+<BLOCKQUOTE><B>A</B><IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"><B>y</B> = <B>x</B>
+</BLOCKQUOTE>
+        where:
+        <UL>
+<LI> <B>A</B> is a non-singular <IMG WIDTH="42" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img73.gif"
+ ALT="$n \times n$"> matrix,
+<LI> <B>y</B> is the vector of <I>n</I> unknowns, and
+<LI> <B>x</B> is the known vector,
+        </UL>
+        sla_SMAT computes:
+        <UL>
+<LI> the inverse of matrix <B>A</B>,
+<LI> the determinant of matrix <B>A</B>, and
+<LI> the vector of <I>n</I> unknowns <B>y</B>.
+        </UL>
+        Argument N is the order <I>n</I>, A (given) is the matrix <B>A</B>,
+        Y (given) is the vector <B>x</B> and Y (returned)
+        is the vector <B>y</B>.
+        The argument A (returned) is the inverse matrix <B>A</B><SUP>-1</SUP>,
+        and D is <I>det</I>(<B>A</B>).
+  <DT>2.
+<DD>JF is the singularity flag.  If the matrix is non-singular,
+        JF=0 is returned.  If the matrix is singular, JF=-1
+        and D=0.0 are returned.  In the latter case, the contents
+        of array A on return are undefined.
+  <DT>3.
+<DD>The algorithm is Gaussian elimination with partial pivoting.
+        This method is very fast;  some much slower algorithms can give
+        better accuracy, but only by a small factor.
+  <DT>4.
+<DD>This routine replaces the obsolete sla_SMATRX.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html2196" HREF="node178.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2194" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2188" HREF="node176.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2197" HREF="node178.html">SLA_SUBET - Remove E-terms</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2195" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2189" HREF="node176.html">SLA_SEP - Angle Between 2 Points on Sphere</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node178.html b/src/slalib/sun67.htx/node178.html
new file mode 100644
index 0000000..3d7a547
--- /dev/null
+++ b/src/slalib/sun67.htx/node178.html
@@ -0,0 +1,111 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_SUBET - Remove E-terms</TITLE>
+<META NAME="description" CONTENT="SLA_SUBET - Remove E-terms">
+<META NAME="keywords" CONTENT="sun67">
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+<META NAME="distribution" CONTENT="global">
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+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2204" HREF="node13.html">
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+<A NAME="tex2html2198" HREF="node177.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2207" HREF="node179.html">SLA_SUPGAL - Supergalactic to Galactic</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2205" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2199" HREF="node177.html">SLA_SMAT - Solve Simultaneous Equations</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004165000000000000000">SLA_SUBET - Remove E-terms</A>
+<A NAME="xref_SLA_SUBET">&#160;</A><A NAME="SLA_SUBET">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Remove the E-terms (elliptic component of annual aberration)
+from a pre IAU&nbsp;1976 catalogue <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> to give a mean place.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_SUBET (RC, DC, EQ, RM, DM)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RC,DC</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> with E-terms included (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EQ</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>Besselian epoch of mean equator and equinox</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RM,DM</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> without E-terms (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTE:</STRONG>
+<DD>Most star positions from pre-1984 optical catalogues (or
+obtained by astrometry with respect to such stars) have the
+       E-terms built-in.  This routine converts such a position to a
+       formal mean place (allowing, for example, comparison with a
+       pulsar timing position).
+      </DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD><I>Explanatory Supplement to the Astronomical Ephemeris</I>,
+section 2D, page 48.
+     </DL>
+<BR> <HR>
+<A NAME="tex2html2206" HREF="node179.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2204" HREF="node13.html">
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+<A NAME="tex2html2198" HREF="node177.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2207" HREF="node179.html">SLA_SUPGAL - Supergalactic to Galactic</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2205" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2199" HREF="node177.html">SLA_SMAT - Solve Simultaneous Equations</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node179.html b/src/slalib/sun67.htx/node179.html
new file mode 100644
index 0000000..1b5da60
--- /dev/null
+++ b/src/slalib/sun67.htx/node179.html
@@ -0,0 +1,107 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_SUPGAL - Supergalactic to Galactic</TITLE>
+<META NAME="description" CONTENT="SLA_SUPGAL - Supergalactic to Galactic">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node180.html">
+<LINK REL="previous" HREF="node178.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node180.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html2216" HREF="node180.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2214" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2208" HREF="node178.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2217" HREF="node180.html">SLA_SVD - Singular Value Decomposition</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2215" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2209" HREF="node178.html">SLA_SUBET - Remove E-terms</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004166000000000000000">SLA_SUPGAL - Supergalactic to Galactic</A>
+<A NAME="xref_SLA_SUPGAL">&#160;</A><A NAME="SLA_SUPGAL">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Transformation from de Vaucouleurs supergalactic coordinates
+to IAU 1958 galactic coordinates.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_GALSUP (DL, DB, DSL, DSB)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DSL,DSB</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>supergalactic longitude and latitude (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DL,DB</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>galactic longitude and latitude <IMG WIDTH="59" HEIGHT="32" ALIGN="MIDDLE" BORDER="0"
+ SRC="img98.gif"
+ ALT="$[\,l^{I\!I},b^{I\!I}\,]$"> (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>de Vaucouleurs, de Vaucouleurs, &amp; Corwin, <I>Second Reference
+Catalogue of Bright Galaxies</I>, U.Texas, p8.
+<DT>2.
+<DD>Systems &amp; Applied Sciences Corp., documentation for the
+        machine-readable version of the above catalogue,
+        Contract NAS 5-26490.
+ </DL>
+ (These two references give different values for the galactic
+ longitude of the supergalactic origin.  Both are wrong;  the
+ correct value is <IMG WIDTH="86" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img119.gif"
+ ALT="$l^{I\!I}=137.37$">.)
+<P>     </DL>
+<BR> <HR>
+<A NAME="tex2html2216" HREF="node180.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2214" HREF="node13.html">
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+<A NAME="tex2html2208" HREF="node178.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2217" HREF="node180.html">SLA_SVD - Singular Value Decomposition</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2215" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2209" HREF="node178.html">SLA_SUBET - Remove E-terms</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node18.html b/src/slalib/sun67.htx/node18.html
new file mode 100644
index 0000000..e3aee75
--- /dev/null
+++ b/src/slalib/sun67.htx/node18.html
@@ -0,0 +1,135 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_AMP - Apparent to Mean</TITLE>
+<META NAME="description" CONTENT="SLA_AMP - Apparent to Mean">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
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+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node19.html">
+<LINK REL="previous" HREF="node17.html">
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+<LINK REL="next" HREF="node19.html">
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+<A NAME="tex2html606" HREF="node19.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+<A NAME="tex2html598" HREF="node17.html">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html607" HREF="node19.html">SLA_AMPQK - Quick Apparent to Mean</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html605" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html599" HREF="node17.html">SLA_ALTAZ - Velocities etc. for Altazimuth Mount</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION00045000000000000000">SLA_AMP - Apparent to Mean</A>
+<A NAME="xref_SLA_AMP">&#160;</A><A NAME="SLA_AMP">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Convert star <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> from geocentric apparent to
+mean place (post IAU 1976).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_AMP (RA, DA, DATE, EQ, RM, DM)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RA,DA</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>TDB for apparent place (JD-2400000.5)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EQ</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>equinox:  Julian epoch of mean place</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RM,DM</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>mean <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The distinction between the required TDB and TT is
+always negligible.  Moreover, for all but the most
+critical applications UTC is adequate.
+  <DT>2.
+<DD>The accuracy is limited by the routine sla_EVP, called
+        by sla_MAPPA, which computes the Earth position and
+        velocity using the methods of Stumpff.  The maximum
+        error is about 0.3&nbsp;milliarcsecond.
+  <DT>3.
+<DD>Iterative techniques are used for the aberration and
+        light deflection corrections so that the routines
+        sla_AMP (or sla_AMPQK) and sla_MAP (or sla_MAPQK) are
+        accurate inverses;  even at the edge of the Sun's disc
+        the discrepancy is only about 1&nbsp;nanoarcsecond.
+  <DT>4.
+<DD>Where multiple apparent places are to be converted to
+        mean places, for a fixed date and equinox, it is more
+        efficient to use the sla_MAPPA routine to compute the
+        required parameters once, followed by one call to
+        sla_AMPQK per star.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>1984 <I>Astronomical Almanac</I>, pp B39-B41.
+<DT>2.
+<DD>Lederle &amp; Schwan, 1984. <I>Astr.Astrophys.</I> <B>134</B>, 1-6.
+</DL></DL>
+<BR> <HR>
+<A NAME="tex2html606" HREF="node19.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html607" HREF="node19.html">SLA_AMPQK - Quick Apparent to Mean</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html605" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html599" HREF="node17.html">SLA_ALTAZ - Velocities etc. for Altazimuth Mount</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node180.html b/src/slalib/sun67.htx/node180.html
new file mode 100644
index 0000000..2372b60
--- /dev/null
+++ b/src/slalib/sun67.htx/node180.html
@@ -0,0 +1,184 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_SVD - Singular Value Decomposition</TITLE>
+<META NAME="description" CONTENT="SLA_SVD - Singular Value Decomposition">
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+<BR>
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+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004167000000000000000">SLA_SVD - Singular Value Decomposition</A>
+<A NAME="xref_SLA_SVD">&#160;</A><A NAME="SLA_SVD">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Singular value decomposition.
+This routine expresses a given matrix <B>A</B> as the product of
+         three matrices <B>U</B>, <B>W</B>, <B>V</B><SUP><I>T</I></SUP>:
+         <PRE><TT>
+ 		 <B>A</B> = <B>U</B> <IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"> <B>W</B> <IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"> <B>V</B><SUP><I>T</I></SUP>
+</TT></PRE>
+         where:
+         <PRE><TT>
+ 		 <B>A</B> 		 is any <I>m</I> (rows) <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img226.gif"
+ ALT="$\times n$"> (columns) matrix,                       where <IMG WIDTH="48" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img227.gif"
+ ALT="$m \geq n$"> 
+		 <B>U</B> 		 is an <IMG WIDTH="46" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img228.gif"
+ ALT="$m \times n$"> column-orthogonal matrix
+		 <B>W</B> 		 is an <IMG WIDTH="42" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img73.gif"
+ ALT="$n \times n$"> diagonal matrix with                       <IMG WIDTH="54" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img229.gif"
+ ALT="$w_{ii} \geq 0$"> 
+		 <B>V</B><SUP><I>T</I></SUP> is the transpose of an <IMG WIDTH="42" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img73.gif"
+ ALT="$n \times n$">                             orthogonal matrix
+</TT></PRE>
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_SVD (M, N, MP, NP, A, W, V, WORK, JSTAT)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>M,N</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TH ALIGN="LEFT" NOWRAP><I>m</I>, <I>n</I>, the numbers of rows and columns in matrix <B>A</B></TH>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>MP,NP</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>physical dimensions of array containing matrix <B>A</B></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A</EM></TD>
+<TD ALIGN="LEFT"><B>D(MP,NP)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>array containing <IMG WIDTH="46" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img228.gif"
+ ALT="$m \times n$"> matrix <B>A</B></TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A</EM></TD>
+<TH ALIGN="LEFT"><B>D(MP,NP)</B></TH>
+<TH ALIGN="LEFT" NOWRAP>array containing <IMG WIDTH="46" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img228.gif"
+ ALT="$m \times n$"> column-orthogonal
+matrix <B>U</B></TH>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>W</EM></TD>
+<TD ALIGN="LEFT"><B>D(N)</B></TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="42" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img73.gif"
+ ALT="$n \times n$"> diagonal matrix <B>W</B>
+(diagonal elements only)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V</EM></TD>
+<TD ALIGN="LEFT"><B>D(NP,NP)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>array containing <IMG WIDTH="42" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img73.gif"
+ ALT="$n \times n$"> orthogonal
+matrix <B>V</B> (<I>n.b.</I> not <B>V</B><SUP><I>T</I></SUP>)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>WORK</EM></TD>
+<TD ALIGN="LEFT"><B>D(N)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>workspace</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JSTAT</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>0&nbsp;=&nbsp;OK, -1&nbsp;=&nbsp;array A wrong shape, &gt;0&nbsp;=&nbsp;index of W
+for which convergence failed (see note&nbsp;3, below)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>M and N are the <I>logical</I> dimensions of the
+matrices and vectors concerned, which can be located in
+arrays of larger <I>physical</I> dimensions, given by MP and NP.
+  <DT>2.
+<DD>V contains matrix V, not the transpose of matrix V.
+  <DT>3.
+<DD>If the status JSTAT is greater than zero, this need not
+        necessarily be treated as a failure.  It means that, due to
+        chance properties of the matrix A, the QR transformation
+        phase of the routine did not fully converge in a predefined
+        number of iterations, something that very seldom occurs.
+        When this condition does arise, it is possible that the
+        elements of the diagonal matrix W have not been correctly
+        found.  However, in practice the results are likely to
+        be trustworthy.  Applications should report the condition
+        as a warning, but then proceed normally.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCES:</STRONG>
+<DD>The algorithm is an adaptation of the routine SVD in the <I>EISPACK</I>
+library (Garbow&nbsp;<I>et&nbsp;al.</I> 1977, <I>EISPACK Guide Extension</I>,
+      Springer Verlag), which is a FORTRAN&nbsp;66 implementation of the Algol
+      routine SVD of Wilkinson &amp; Reinsch 1971 (<I>Handbook for Automatic
+      Computation</I>, vol&nbsp;2, ed Bauer&nbsp;<I>et&nbsp;al.</I>, Springer Verlag).  These
+      references give full details of the algorithm used here.
+      A good account of the use of SVD in least squares problems is given
+      in <I>Numerical Recipes</I> (Press&nbsp;<I>et&nbsp;al.</I> 1987, Cambridge
+      University Press), which includes another variant of the EISPACK code.
+     </DL>
+<BR> <HR>
+<A NAME="tex2html2226" HREF="node181.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2227" HREF="node181.html">SLA_SVDCOV - Covariance Matrix from SVD</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2225" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2219" HREF="node179.html">SLA_SUPGAL - Supergalactic to Galactic</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node181.html b/src/slalib/sun67.htx/node181.html
new file mode 100644
index 0000000..76e49b9
--- /dev/null
+++ b/src/slalib/sun67.htx/node181.html
@@ -0,0 +1,122 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_SVDCOV - Covariance Matrix from SVD</TITLE>
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+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004168000000000000000">SLA_SVDCOV - Covariance Matrix from SVD</A>
+<A NAME="xref_SLA_SVDCOV">&#160;</A><A NAME="SLA_SVDCOV">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>From the <B>W</B> and <B>V</B> matrices from the SVD
+factorization of a matrix
+         (as obtained from the sla_SVD routine), obtain
+         the covariance matrix.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_SVDCOV (N, NP, NC, W, V, WORK, CVM)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>N</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TH ALIGN="LEFT" NOWRAP><I>n</I>, the number of rows and columns in
+matrices <B>W</B> and <B>V</B></TH>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NP</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>first dimension of array containing <IMG WIDTH="42" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img73.gif"
+ ALT="$n \times n$">matrix <B>V</B></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NC</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>first dimension of array CVM</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>W</EM></TD>
+<TD ALIGN="LEFT"><B>D(N)</B></TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="42" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img73.gif"
+ ALT="$n \times n$"> diagonal matrix <B>W</B>
+(diagonal elements only)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V</EM></TD>
+<TD ALIGN="LEFT"><B>D(NP,NP)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>array containing <IMG WIDTH="42" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img73.gif"
+ ALT="$n \times n$"> orthogonal matrix <B>V</B></TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>WORK</EM></TD>
+<TH ALIGN="LEFT"><B>D(N)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>workspace</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>CVM</EM></TD>
+<TD ALIGN="LEFT"><B>D(NC,NC)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>array to receive covariance matrix</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD><I>Numerical Recipes</I>, section 14.3.
+</DL>
+<BR> <HR>
+<A NAME="tex2html2236" HREF="node182.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2237" HREF="node182.html">SLA_SVDSOL - Solution Vector from SVD</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2235" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2229" HREF="node180.html">SLA_SVD - Singular Value Decomposition</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node182.html b/src/slalib/sun67.htx/node182.html
new file mode 100644
index 0000000..f99ea3f
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@@ -0,0 +1,201 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
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+<BR>
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+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004169000000000000000">SLA_SVDSOL - Solution Vector from SVD</A>
+<A NAME="xref_SLA_SVDSOL">&#160;</A><A NAME="SLA_SVDSOL">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>From a given vector and the SVD of a matrix (as obtained from
+the sla_SVD routine), obtain the solution vector.
+         This routine solves the equation:
+         <PRE><TT>
+ 		 <B>A</B> <IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"> <B>x</B> = <B>b</B>         
+</TT></PRE>
+         where:
+         <PRE><TT>
+ 		 <B>A</B> 		 is a given <I>m</I> (rows) <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img226.gif"
+ ALT="$\times n$"> (columns)                       matrix, where <IMG WIDTH="48" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img227.gif"
+ ALT="$m \geq n$"> 
+		 <B>x</B> 		 is the <I>n</I>-vector we wish to find, and
+		 <B>b</B> 		 is a given <I>m</I>-vector         
+</TT></PRE>
+         by means of the <I>Singular Value Decomposition</I> method (SVD).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_SVDSOL (M, N, MP, NP, B, U, W, V, WORK, X)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>M,N</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TH ALIGN="LEFT" NOWRAP><I>m</I>, <I>n</I>, the numbers of rows and columns in matrix <B>A</B></TH>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>MP,NP</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>physical dimensions of array containing matrix <B>A</B></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>B</EM></TD>
+<TD ALIGN="LEFT"><B>D(M)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>known vector <B>b</B></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>U</EM></TD>
+<TD ALIGN="LEFT"><B>D(MP,NP)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>array containing <IMG WIDTH="46" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img228.gif"
+ ALT="$m \times n$"> matrix <B>U</B></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>W</EM></TD>
+<TD ALIGN="LEFT"><B>D(N)</B></TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="42" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img73.gif"
+ ALT="$n \times n$"> diagonal matrix <B>W</B>
+(diagonal elements only)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V</EM></TD>
+<TD ALIGN="LEFT"><B>D(NP,NP)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>array containing <IMG WIDTH="42" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img73.gif"
+ ALT="$n \times n$"> orthogonal matrix <B>V</B></TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>WORK</EM></TD>
+<TH ALIGN="LEFT"><B>D(N)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>workspace</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>X</EM></TD>
+<TD ALIGN="LEFT"><B>D(N)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>unknown vector <B>x</B></TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>In the Singular Value Decomposition method (SVD),
+the matrix <B>A</B> is first factorized (for example by
+the routine sla_SVD) into the following components:
+        <PRE><TT>
+ 		 <B>A</B> = <B>U</B> <IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"> <B>W</B> <IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"> <B>V</B><SUP><I>T</I></SUP>
+</TT></PRE>
+        where:
+        <PRE><TT>
+ 		 <B>A</B> 		 is any <I>m</I> (rows) <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img226.gif"
+ ALT="$\times n$"> (columns) matrix,                      where <I>m</I> &gt; <I>n</I> 
+		 <B>U</B> 		 is an <IMG WIDTH="46" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img228.gif"
+ ALT="$m \times n$"> column-orthogonal matrix
+		 <B>W</B> 		 is an <IMG WIDTH="42" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img73.gif"
+ ALT="$n \times n$"> diagonal matrix with                      <IMG WIDTH="54" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img229.gif"
+ ALT="$w_{ii} \geq 0$"> 
+		 <B>V</B><SUP><I>T</I></SUP> is the transpose of an <IMG WIDTH="42" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img73.gif"
+ ALT="$n \times n$">                            orthogonal matrix        
+</TT></PRE>
+        Note that <I>m</I> and <I>n</I> are the <I>logical</I> dimensions of the
+        matrices and vectors concerned, which can be located in
+        arrays of larger <I>physical</I> dimensions MP and NP.
+        The solution is then found from the expression:
+        <PRE><TT>
+ 		 <B>x</B> = <B>V</B> <IMG WIDTH="71" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img230.gif"
+ ALT="$\cdot~[diag(1/$"><B>W</B><IMG WIDTH="38" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img231.gif"
+ ALT="$_{j})]
+ \cdot ($"><B>U</B><IMG WIDTH="17" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img70.gif"
+ ALT="$^{T}\cdot$"><B>b</B>)        
+</TT></PRE>
+  <DT>2.
+<DD>If matrix <B>A</B> is square, and if the diagonal matrix <B>W</B> is not
+        altered, the method is equivalent to conventional solution
+        of simultaneous equations.
+  <DT>3.
+<DD>If <I>m</I> &gt; <I>n</I>, the result is a least-squares fit.
+  <DT>4.
+<DD>If the solution is poorly determined, this shows up in the
+        SVD factorization as very small or zero <B>W</B><SUB><I>j</I></SUB> values.  Where
+        a <B>W</B><SUB><I>j</I></SUB> value is small but non-zero it can be set to zero to
+        avoid ill effects.  The present routine detects such zero
+        <B>W</B><SUB><I>j</I></SUB> values and produces a sensible solution, with highly
+        correlated terms kept under control rather than being allowed
+        to elope to infinity, and with meaningful values for the
+       other terms.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD><I>Numerical Recipes</I>, section 2.9.
+</DL>
+<BR> <HR>
+<A NAME="tex2html2246" HREF="node183.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2244" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2238" HREF="node181.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2247" HREF="node183.html">SLA_TP2S - Tangent Plane to Spherical</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2245" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2239" HREF="node181.html">SLA_SVDCOV - Covariance Matrix from SVD</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node183.html b/src/slalib/sun67.htx/node183.html
new file mode 100644
index 0000000..ae3acd0
--- /dev/null
+++ b/src/slalib/sun67.htx/node183.html
@@ -0,0 +1,109 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_TP2S - Tangent Plane to Spherical</TITLE>
+<META NAME="description" CONTENT="SLA_TP2S - Tangent Plane to Spherical">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2257" HREF="node184.html">SLA_TP2V - Tangent Plane to Direction Cosines</A>
+<BR>
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+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004170000000000000000">SLA_TP2S - Tangent Plane to Spherical</A>
+<A NAME="xref_SLA_TP2S">&#160;</A><A NAME="SLA_TP2S">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Transform tangent plane coordinates into spherical
+coordinates (single precision)
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_TP2S (XI, ETA, RAZ, DECZ, RA, DEC)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>XI,ETA</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>tangent plane rectangular coordinates (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RAZ,DECZ</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>spherical coordinates of tangent point (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RA,DEC</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>spherical coordinates (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The projection is called the <I>gnomonic</I> projection;  the
+Cartesian coordinates <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img85.gif"
+ ALT="$[\,\xi,\eta\,]$"> are called 
+<I>standard coordinates.</I>  The latter
+        are in units of the distance from the tangent plane to the projection
+        point, <I>i.e.</I> radians near the origin.
+  <DT>2.
+<DD>When working in <IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$"> rather than spherical coordinates, the
+        equivalent Cartesian routine sla_TP2V is available.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html2256" HREF="node184.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2254" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2248" HREF="node182.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2257" HREF="node184.html">SLA_TP2V - Tangent Plane to Direction Cosines</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2255" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2249" HREF="node182.html">SLA_SVDSOL - Solution Vector from SVD</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node184.html b/src/slalib/sun67.htx/node184.html
new file mode 100644
index 0000000..f069a46
--- /dev/null
+++ b/src/slalib/sun67.htx/node184.html
@@ -0,0 +1,117 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_TP2V - Tangent Plane to Direction Cosines</TITLE>
+<META NAME="description" CONTENT="SLA_TP2V - Tangent Plane to Direction Cosines">
+<META NAME="keywords" CONTENT="sun67">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2267" HREF="node185.html">SLA_TPS2C - Plate centre from and</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2265" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2259" HREF="node183.html">SLA_TP2S - Tangent Plane to Spherical</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004171000000000000000">SLA_TP2V - Tangent Plane to Direction Cosines</A>
+<A NAME="xref_SLA_TP2V">&#160;</A><A NAME="SLA_TP2V">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Given the tangent-plane coordinates of a star and the direction
+cosines of the tangent point, determine the direction cosines
+         of the star
+         (single precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_TP2V (XI, ETA, V0, V)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>XI,ETA</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>tangent plane coordinates of star (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V0</EM></TD>
+<TD ALIGN="LEFT"><B>R(3)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>direction cosines of tangent point</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V</EM></TD>
+<TH ALIGN="LEFT"><B>R(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>direction cosines of star</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>If vector V0 is not of unit length, the returned vector V will
+be wrong.
+<DT>2.
+<DD>If vector V0 points at a pole, the returned vector V will be
+        based on the arbitrary assumption that <IMG WIDTH="43" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img89.gif"
+ ALT="$\alpha=0$"> at
+        the tangent point.
+  <DT>3.
+<DD>The projection is called the <I>gnomonic</I> projection;  the
+        Cartesian coordinates <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img85.gif"
+ ALT="$[\,\xi,\eta\,]$"> are called 
+        <I>standard coordinates.</I>  The latter
+        are in units of the distance from the tangent plane to the projection
+        point, <I>i.e.</I> radians near the origin.
+  <DT>4.
+<DD>This routine is the Cartesian equivalent of the routine sla_TP2S.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html2266" HREF="node185.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2264" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2258" HREF="node183.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2267" HREF="node185.html">SLA_TPS2C - Plate centre from and</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2265" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2259" HREF="node183.html">SLA_TP2S - Tangent Plane to Spherical</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node185.html b/src/slalib/sun67.htx/node185.html
new file mode 100644
index 0000000..0313e77
--- /dev/null
+++ b/src/slalib/sun67.htx/node185.html
@@ -0,0 +1,168 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_TPS2C - Plate centre from and </TITLE>
+<META NAME="description" CONTENT="SLA_TPS2C - Plate centre from and ">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node186.html">
+<LINK REL="previous" HREF="node184.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node186.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html2276" HREF="node186.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2274" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2268" HREF="node184.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2277" HREF="node186.html">SLA_TPV2C - Plate centre from and x,y,z</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2275" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2269" HREF="node184.html">SLA_TP2V - Tangent Plane to Direction Cosines</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004172000000000000000">&#160;</A><A NAME="xref_SLA_TPS2C">&#160;</A><A NAME="SLA_TPS2C">&#160;</A>
+<BR>
+SLA_TPS2C - Plate centre from <IMG WIDTH="26" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img90.gif"
+ ALT="$\xi,\eta$"> and <IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img91.gif"
+ ALT="$\alpha,\delta$"></H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>From the tangent plane coordinates of a star of known <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">,determine the <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> of the tangent point (single precision)
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_TPS2C (XI, ETA, RA, DEC, RAZ1, DECZ1, RAZ2, DECZ2, N)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>XI,ETA</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>tangent plane rectangular coordinates (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RA,DEC</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>spherical coordinates (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RAZ1,DECZ1</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>spherical coordinates of tangent point,
+solution 1</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RAZ2,DECZ2</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>spherical coordinates of tangent point,
+solution 2</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>N</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>number of solutions:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  0 = no solutions returned  (note 2)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  1 = only the first solution is useful (note 3)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  2 = there are two useful solutions (note 3)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The RAZ1 and RAZ2 values returned are in the range <IMG WIDTH="43" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img66.gif"
+ ALT="$0\!-\!2\pi$">.<DT>2.
+<DD>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 <IMG WIDTH="10" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img92.gif"
+ ALT="$\xi$"> value, and hence it is
+        meaningless to ask where the tangent point would have to be
+        to bring about this combination of <IMG WIDTH="10" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img92.gif"
+ ALT="$\xi$"> and <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$">.  <DT>3.
+<DD>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.
+  <DT>4.
+<DD>The DECZ1 and DECZ2 values returned are in the range <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$">,        but in the ordinary, non-pole-crossing, case, the range is
+        <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img15.gif"
+ ALT="$\pm\pi/2$">.  <DT>5.
+<DD>RA, DEC, RAZ1, DECZ1, RAZ2, DECZ2 are all in radians.
+  <DT>6.
+<DD>The projection is called the <I>gnomonic</I> projection;  the
+        Cartesian coordinates <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img85.gif"
+ ALT="$[\,\xi,\eta\,]$"> are called 
+        <I>standard coordinates.</I>  The latter
+        are in units of the distance from the tangent plane to the projection
+        point, <I>i.e.</I> radians near the origin.
+  <DT>7.
+<DD>When working in <IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$"> rather than spherical coordinates, the
+        equivalent Cartesian routine sla_TPV2C is available.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html2276" HREF="node186.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2274" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2268" HREF="node184.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2277" HREF="node186.html">SLA_TPV2C - Plate centre from and x,y,z</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2275" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2269" HREF="node184.html">SLA_TP2V - Tangent Plane to Direction Cosines</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node186.html b/src/slalib/sun67.htx/node186.html
new file mode 100644
index 0000000..32d0e60
--- /dev/null
+++ b/src/slalib/sun67.htx/node186.html
@@ -0,0 +1,144 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_TPV2C - Plate centre from and x,y,z</TITLE>
+<META NAME="description" CONTENT="SLA_TPV2C - Plate centre from and x,y,z">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node187.html">
+<LINK REL="previous" HREF="node185.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node187.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html2286" HREF="node187.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2284" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2278" HREF="node185.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2287" HREF="node187.html">SLA_UE2EL - Universal to Conventional Elements</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2285" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2279" HREF="node185.html">SLA_TPS2C - Plate centre from and</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004173000000000000000">&#160;</A><A NAME="xref_SLA_TPV2C">&#160;</A><A NAME="SLA_TPV2C">&#160;</A>
+<BR>
+SLA_TPV2C - Plate centre from <IMG WIDTH="26" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img90.gif"
+ ALT="$\xi,\eta$"> and <I>x</I>,<I>y</I>,<I>z</I>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>From the tangent plane coordinates of a star of known
+direction cosines, determine the direction cosines
+         of the tangent point (single precision)
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_TPV2C (XI, ETA, V, V01, V02, N)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>XI,ETA</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>tangent plane coordinates of star (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V</EM></TD>
+<TD ALIGN="LEFT"><B>R(3)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>direction cosines of star</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V01</EM></TD>
+<TH ALIGN="LEFT"><B>R(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>direction cosines of tangent point, solution 1</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V01</EM></TD>
+<TD ALIGN="LEFT"><B>R(3)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>direction cosines of tangent point, solution 2</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>N</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>number of solutions:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  0 = no solutions returned  (note 2)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  1 = only the first solution is useful (note 3)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  2 = there are two useful solutions (note 3)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The vector V must be of unit length or the result will be wrong.
+<DT>2.
+<DD>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.
+  <DT>3.
+<DD>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 can be regarded as valid if
+        the vector V02 is interpreted as the ``over-the-pole'' case.
+  <DT>4.
+<DD>The projection is called the <I>gnomonic</I> projection;  the
+        Cartesian coordinates <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img85.gif"
+ ALT="$[\,\xi,\eta\,]$"> are called 
+        <I>standard coordinates.</I>  The latter
+        are in units of the distance from the tangent plane to the projection
+        point, <I>i.e.</I> radians near the origin.
+  <DT>5.
+<DD>This routine is the Cartesian equivalent of the routine sla_TPS2C.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html2286" HREF="node187.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2284" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2278" HREF="node185.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2287" HREF="node187.html">SLA_UE2EL - Universal to Conventional Elements</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2285" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2279" HREF="node185.html">SLA_TPS2C - Plate centre from and</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node187.html b/src/slalib/sun67.htx/node187.html
new file mode 100644
index 0000000..9b71eb3
--- /dev/null
+++ b/src/slalib/sun67.htx/node187.html
@@ -0,0 +1,378 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_UE2EL - Universal to Conventional Elements</TITLE>
+<META NAME="description" CONTENT="SLA_UE2EL - Universal to Conventional Elements">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node188.html">
+<LINK REL="previous" HREF="node186.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node188.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html2296" HREF="node188.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2294" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2288" HREF="node186.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2297" HREF="node188.html">SLA_UE2PV - Pos/Vel from Universal Elements</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2295" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2289" HREF="node186.html">SLA_TPV2C - Plate centre from and x,y,z</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004174000000000000000">SLA_UE2EL - Universal to Conventional Elements</A>
+<A NAME="xref_SLA_UE2EL">&#160;</A><A NAME="SLA_UE2EL">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Transform universal elements into conventional heliocentric
+osculating elements.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_UE2EL (
+         U, JFORMR,
+         JFORM, EPOCH, ORBINC, ANODE, PERIH,
+         AORQ, E, AORL, DM, JSTAT)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>U</EM></TD>
+<TH ALIGN="LEFT"><B>D(13)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>universal orbital elements (updated; Note&nbsp;1)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(1)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>combined mass (<I>M</I>+<I>m</I>)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(2)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>total energy of the orbit (<IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$">)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(3)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>reference (osculating) epoch (<I>t<SUB>0</SUB></I>)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(4-6)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>position at reference epoch (<IMG WIDTH="17" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img102.gif"
+ ALT="${\rm \bf r}_0$">)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(7-9)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>velocity at reference epoch (<IMG WIDTH="19" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img103.gif"
+ ALT="${\rm \bf v}_0$">)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(10)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>heliocentric distance at reference epoch</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(11)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img104.gif"
+ ALT="${\rm \bf r}_0.{\rm \bf v}_0$"></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(12)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>date (<I>t</I>)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(13)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>universal eccentric anomaly (<IMG WIDTH="14" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img105.gif"
+ ALT="$\psi$">) of date, approx</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT">&nbsp;</TD>
+<TD ALIGN="LEFT">&nbsp;</TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JFORMR</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>requested element set (1-3; Note&nbsp;3)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JFORM</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>element set actually returned (1-3; Note&nbsp;4)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EPOCH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>epoch of elements (<I>t<SUB>0</SUB></I> or <I>T</I>, TT MJD)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ORBINC</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>inclination (<I>i</I>, radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ANODE</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>longitude of the ascending node (<IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$">, radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PERIH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>longitude or argument of perihelion
+(<IMG WIDTH="16" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img100.gif"
+ ALT="$\varpi$"> or <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$">,</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AORQ</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>mean distance or perihelion distance (<I>a</I> or <I>q</I>, AU)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>E</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>eccentricity (<I>e</I>)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AORL</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>mean anomaly or longitude
+(<I>M</I> or <I>L</I>, radians,</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  JFORM=1,2 only)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DM</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>daily motion (<I>n</I>, radians, JFORM=1 only)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JSTAT</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>     0 = OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -1 = illegal PMASS</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -2 = illegal JFORMR</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -3 = position/velocity out of allowed range</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>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)&nbsp;<IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$">, which is proportional to the total energy of the
+        orbit, (ii)&nbsp;the heliocentric distance at epoch,
+        (iii)&nbsp;the outwards component of the velocity at the given epoch,
+        (iv)&nbsp;an estimate of <IMG WIDTH="14" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img105.gif"
+ ALT="$\psi$">, the ``universal eccentric anomaly'' at a
+        given date and (v)&nbsp;that date.
+  <DT>2.
+<DD>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.
+  <DT>3.
+<DD>Three different element-format options are supported, as
+        follows. <BR>
+<P>
+JFORM=1, suitable for the major planets:
+<P>        <PRE><TT>
+ 		 EPOCH 		 = 		 epoch of elements <I>t<SUB>0</SUB></I> (TT MJD)
+		 ORBINC 		 = 		 inclination <I>i</I> (radians)
+		 ANODE 		 = 		 longitude of the ascending node <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> (radians)
+		 PERIH 		 = 		 longitude of perihelion <IMG WIDTH="16" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img100.gif"
+ ALT="$\varpi$"> (radians)
+		 AORQ 		 = 		 mean distance <I>a</I> (AU)
+		 E 		 = 		 eccentricity <I>e</I> <IMG WIDTH="83" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img106.gif"
+ ALT="$( 0 \leq e < 1 )$"> 
+		 AORL 		 = 		 mean longitude <I>L</I> (radians)
+		 DM 		 = 		 daily motion <I>n</I> (radians)        
+</TT></PRE>
+<P>
+JFORM=2, suitable for minor planets:
+<P>        <PRE><TT>
+ 		 EPOCH 		 = 		 epoch of elements <I>t<SUB>0</SUB></I> (TT MJD)
+		 ORBINC 		 = 		 inclination <I>i</I> (radians)
+		 ANODE 		 = 		 longitude of the ascending node <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> (radians)
+		 PERIH 		 = 		 argument of perihelion <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$"> (radians)
+		 AORQ 		 = 		 mean distance <I>a</I> (AU)
+		 E 		 = 		 eccentricity <I>e</I> <IMG WIDTH="83" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img106.gif"
+ ALT="$( 0 \leq e < 1 )$"> 
+		 AORL 		 = 		 mean anomaly <I>M</I> (radians)        
+</TT></PRE>
+<P>
+JFORM=3, suitable for comets:
+<P>        <PRE><TT>
+ 		 EPOCH 		 = 		 epoch of perihelion <I>T</I> (TT MJD)
+		 ORBINC 		 = 		 inclination <I>i</I> (radians)
+		 ANODE 		 = 		 longitude of the ascending node <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> (radians)
+		 PERIH 		 = 		 argument of perihelion <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$"> (radians)
+		 AORQ 		 = 		 perihelion distance <I>q</I> (AU)
+		 E 		 = 		 eccentricity <I>e</I> <IMG WIDTH="91" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img107.gif"
+ ALT="$( 0 \leq e \leq 10 )$"></TT></PRE>
+  <DT>4.
+<DD>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:
+<P>        <PRE><TT>
+ 		 JFORMR 		 JFORM 		 meaning 
+&nbsp;
+		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;1 		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;1 		 OK: elements are in the requested format
+		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;1 		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;2 		 never happens
+		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;1 		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;3 		 orbit not elliptical
+		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;2 		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;1 		 never happens
+		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;2 		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;2 		 OK: elements are in the requested format
+		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;2 		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;3 		 orbit not elliptical
+		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;3 		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;1 		 never happens
+		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;3 		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;2 		 never happens
+		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;3 		 &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;3 		 OK: elements are in the requested format        
+</TT></PRE>
+  <DT>5.
+<DD>The arguments returned for each value of JFORM (<I>cf</I> Note&nbsp;5:
+        JFORM may not be the same as JFORMR) are as follows:
+<P>        <PRE><TT>
+ 		 JFORM 		 1 		 2 		 3 
+&nbsp;
+		 EPOCH 		 <I>t<SUB>0</SUB></I> <I>t<SUB>0</SUB></I> <I>T</I> 
+		 ORBINC 		 <I>i</I> <I>i</I> <I>i</I> 
+		 ANODE 		 <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> 
+		 PERIH 		 <IMG WIDTH="16" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img100.gif"
+ ALT="$\varpi$"> <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$"> <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$"> 
+		 AORQ 		 <I>a</I> <I>a</I> <I>q</I> 
+		 E 		 <I>e</I> <I>e</I> <I>e</I> 
+		 AORL 		 <I>L</I> <I>M</I> -
+		 DM 		 <I>n</I> - 		 -        
+</TT></PRE>
+<P>
+where:
+        <PRE><TT>
+ 		 <I>t<SUB>0</SUB></I> is the epoch of the elements (MJD, TT)
+		 <I>T</I> is the epoch of perihelion (MJD, TT)
+		 <I>i</I> is the inclination (radians)
+		 <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> is the longitude of the ascending node (radians)
+		 <IMG WIDTH="16" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img100.gif"
+ ALT="$\varpi$"> is the longitude of perihelion (radians)
+		 <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$"> is the argument of perihelion (radians)
+		 <I>a</I> is the mean distance (AU)
+		 <I>q</I> is the perihelion distance (AU)
+		 <I>e</I> is the eccentricity
+		 <I>L</I> is the longitude (radians, <IMG WIDTH="48" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img143.gif"
+ ALT="$0-2\pi$">)		 <I>M</I> is the mean anomaly (radians, <IMG WIDTH="48" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img143.gif"
+ ALT="$0-2\pi$">)		 <I>n</I> is the daily motion (radians)
+		 - 		 means no value is set        
+</TT></PRE>
+  <DT>6.
+<DD>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.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Sterne, Theodore E., <I>An Introduction to Celestial Mechanics,</I>
+Interscience Publishers, 1960.  Section 6.7, p199.
+<DT>2.
+<DD>Everhart, E. &amp; Pitkin, E.T., Am.&nbsp;J.&nbsp;Phys.&nbsp;51, 712, 1983.
+   </DL></DL>
+<BR> <HR>
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+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
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+<H2><A NAME="SECTION0004175000000000000000">SLA_UE2PV - Pos/Vel from Universal Elements</A>
+<A NAME="xref_SLA_UE2PV">&#160;</A><A NAME="SLA_UE2PV">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Heliocentric position and velocity of a planet, asteroid or comet,
+starting from orbital elements in the ``universal variables'' form.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_UE2PV (DATE, U, PV, JSTAT)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>date (TT Modified Julian Date = JD-2400000.5)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>GIVEN and RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>U</EM></TD>
+<TH ALIGN="LEFT"><B>D(13)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>universal orbital elements (updated; Note&nbsp;1)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(1)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>combined mass (<I>M</I>+<I>m</I>)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(2)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>total energy of the orbit (<IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$">)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(3)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>reference (osculating) epoch (<I>t<SUB>0</SUB></I>)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(4-6)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>position at reference epoch (<IMG WIDTH="17" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img102.gif"
+ ALT="${\rm \bf r}_0$">)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(7-9)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>velocity at reference epoch (<IMG WIDTH="19" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img103.gif"
+ ALT="${\rm \bf v}_0$">)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(10)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>heliocentric distance at reference epoch</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(11)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img104.gif"
+ ALT="${\rm \bf r}_0.{\rm \bf v}_0$"></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(12)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>date (<I>t</I>)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(13)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>universal eccentric anomaly (<IMG WIDTH="14" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img105.gif"
+ ALT="$\psi$">) of date, approx</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PV</EM></TD>
+<TH ALIGN="LEFT"><B>D(6)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>heliocentric <IMG WIDTH="106" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img51.gif"
+ ALT="$[\,x,y,z,\dot{x},\dot{y},\dot{z}\,]$">, equatorial, J2000</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  (AU, AU/s; Note&nbsp;1)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JSTAT</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>       0 = OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>     -1 = radius vector zero</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>     -2 = failed to converge</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>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)&nbsp;<IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$">, which is proportional to the total energy of the
+        orbit, (ii)&nbsp;the heliocentric distance at epoch,
+        (iii)&nbsp;the outwards component of the velocity at the given epoch,
+        (iv)&nbsp;an estimate of <IMG WIDTH="14" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img105.gif"
+ ALT="$\psi$">, the ``universal eccentric anomaly'' at a
+        given date and (v)&nbsp;that date.
+  <DT>2.
+<DD>The companion routine is sla_EL2UE.  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 sla_EL2UE 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 sla_EL2UE once, but then calling the present routine
+        multiple times, which is faster than multiple calls to sla_PLANEL.
+<P>
+It is not obligatory to use sla_EL2UE to obtain the parameters.
+        However, it should be noted that because sla_EL2UE performs its
+        own validation, no checks on the contents of the array U are made
+        by the present routine.
+  <DT>3.
+<DD>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).
+  <DT>4.
+<DD>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
+        sla_EL2UE routine in fact produces coordinates with respect to the
+        J2000 equator and equinox.
+  <DT>5.
+<DD>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.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Everhart, E. &amp; Pitkin, E.T., Am.&nbsp;J.&nbsp;Phys.&nbsp;51, 712, 1983.
+</DL>
+<BR> <HR>
+<A NAME="tex2html2306" HREF="node189.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2307" HREF="node189.html">SLA_UNPCD - Remove Radial Distortion</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2305" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2299" HREF="node187.html">SLA_UE2EL - Universal to Conventional Elements</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node189.html b/src/slalib/sun67.htx/node189.html
new file mode 100644
index 0000000..a19516f
--- /dev/null
+++ b/src/slalib/sun67.htx/node189.html
@@ -0,0 +1,160 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_UNPCD - Remove Radial Distortion</TITLE>
+<META NAME="description" CONTENT="SLA_UNPCD - Remove Radial Distortion">
+<META NAME="keywords" CONTENT="sun67">
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+ SRC="contents_motif.gif"></A>
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+<BR>
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+<BR>
+<B> Previous:</B> <A NAME="tex2html2309" HREF="node188.html">SLA_UE2PV - Pos/Vel from Universal Elements</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004176000000000000000">SLA_UNPCD - Remove Radial Distortion</A>
+<A NAME="xref_SLA_UNPCD">&#160;</A><A NAME="SLA_UNPCD">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Remove pincushion/barrel distortion from a distorted 
+<IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$">  to give tangent-plane <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$">.<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_UNPCD (DISCO,X,Y)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DISCO</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>pincushion/barrel distortion coefficient</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>X,Y</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>distorted <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"></TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>X,Y</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>tangent-plane <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"></TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The distortion is of the form <IMG WIDTH="103" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img128.gif"
+ ALT="$\rho = r (1 + c r^{2})$">, where <I>r</I> is
+the radial distance from the tangent point, <I>c</I> is the DISCO
+argument, and <IMG WIDTH="11" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img129.gif"
+ ALT="$\rho$"> is the radial distance in the presence of
+        the distortion.
+  <DT>2.
+<DD>For <I>pincushion</I> distortion, C is +ve;  for
+        <I>barrel</I> distortion, C is -ve.
+  <DT>3.
+<DD>For X,Y in units of one projection radius (in the case of
+        a photographic plate, the focal length), the following
+        DISCO values apply:
+<P>        <BR>
+<BR>
+<BR>
+<P>        <TABLE CELLPADDING=3 BORDER="1">
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP>Geometry</TD>
+<TD ALIGN="CENTER" NOWRAP>DISCO</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP>astrograph</TD>
+<TD ALIGN="CENTER" NOWRAP>0.0</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP>Schmidt</TD>
+<TD ALIGN="CENTER" NOWRAP>-0.3333</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP>AAT PF doublet</TD>
+<TD ALIGN="CENTER" NOWRAP>+147.069</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP>AAT PF triplet</TD>
+<TD ALIGN="CENTER" NOWRAP>+178.585</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP>AAT f/8</TD>
+<TD ALIGN="CENTER" NOWRAP>+21.20</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP>JKT f/8</TD>
+<TD ALIGN="CENTER" NOWRAP>+14.6</TD>
+</TR>
+</TABLE>
+<P>        <BR>
+<BR>
+<BR>
+<P>  <DT>4.
+<DD>The present routine is an approximate inverse to the
+        companion routine sla_PCD, obtained from two iterations
+        of Newton's method.  The mismatch between the sla_PCD
+        and sla_UNPCD is negligible for astrometric applications;
+        to reach 1&nbsp;milliarcsec at the edge of the AAT triplet or
+        Schmidt field would require field diameters of <IMG WIDTH="25" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img232.gif"
+ ALT="$2^{\circ}
+ \hspace{-0.37em}.\hspace{0.02em}4$">        and <IMG WIDTH="26" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img233.gif"
+ ALT="$42^{\circ}$"> respectively.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html2316" HREF="node190.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2317" HREF="node190.html">SLA_V2TP - Direction Cosines to Tangent Plane</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2315" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2309" HREF="node188.html">SLA_UE2PV - Pos/Vel from Universal Elements</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node19.html b/src/slalib/sun67.htx/node19.html
new file mode 100644
index 0000000..3a52cd9
--- /dev/null
+++ b/src/slalib/sun67.htx/node19.html
@@ -0,0 +1,160 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_AMPQK - Quick Apparent to Mean</TITLE>
+<META NAME="description" CONTENT="SLA_AMPQK - Quick Apparent to Mean">
+<META NAME="keywords" CONTENT="sun67">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html617" HREF="node20.html">SLA_AOP - Apparent to Observed</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html615" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html609" HREF="node18.html">SLA_AMP - Apparent to Mean</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION00046000000000000000">SLA_AMPQK - Quick Apparent to Mean</A>
+<A NAME="xref_SLA_AMPQK">&#160;</A><A NAME="SLA_AMPQK">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Convert star <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> from geocentric apparent to mean place
+(post IAU 1976).  Use of this routine 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 sla_MAPPA routine.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_AMPQK (RA, DA, AMPRMS, RM, DM)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RA,DA</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AMPRMS</EM></TD>
+<TD ALIGN="LEFT"><B>D(21)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>star-independent mean-to-apparent parameters:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(1)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>time interval for proper motion (Julian years)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(2-4)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>barycentric position of the Earth (AU)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(5-7)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>heliocentric direction of the Earth (unit vector)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(8)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>(gravitational radius of
+Sun)<IMG WIDTH="31" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img16.gif"
+ ALT="$\times 2 / $">(Sun-Earth distance)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(9-11)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP><B>v</B>: barycentric Earth velocity in units of c</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(12)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="72" HEIGHT="45" ALIGN="MIDDLE" BORDER="0"
+ SRC="img17.gif"
+ ALT="$\sqrt{1-\left\vert\mbox{\bf v}\right\vert^2}$"></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(13-21)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>precession/nutation <IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img18.gif"
+ ALT="$3\times3$"> matrix</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RM,DM</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>mean <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The accuracy is limited by the routine sla_EVP, called
+by sla_MAPPA, which computes the Earth position and
+velocity using the methods of Stumpff.  The maximum
+        error is about 0.3&nbsp;milliarcsecond.
+  <DT>2.
+<DD>Iterative techniques are used for the aberration and
+        light deflection corrections so that the routines
+        sla_AMP (or sla_AMPQK) and sla_MAP (or sla_MAPQK) are
+        accurate inverses;  even at the edge of the Sun's disc
+        the discrepancy is only about 1&nbsp;nanoarcsecond.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>1984 <I>Astronomical Almanac</I>, pp B39-B41.
+<DT>2.
+<DD>Lederle &amp; Schwan, 1984. <I>Astr.Astrophys.</I> <B>134</B>, 1-6.
+</DL></DL>
+<BR> <HR>
+<A NAME="tex2html616" HREF="node20.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html617" HREF="node20.html">SLA_AOP - Apparent to Observed</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html615" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html609" HREF="node18.html">SLA_AMP - Apparent to Mean</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node190.html b/src/slalib/sun67.htx/node190.html
new file mode 100644
index 0000000..09def53
--- /dev/null
+++ b/src/slalib/sun67.htx/node190.html
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+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_V2TP - Direction Cosines to Tangent Plane</TITLE>
+<META NAME="description" CONTENT="SLA_V2TP - Direction Cosines to Tangent Plane">
+<META NAME="keywords" CONTENT="sun67">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2327" HREF="node191.html">SLA_VDV - Scalar Product</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2325" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2319" HREF="node189.html">SLA_UNPCD - Remove Radial Distortion</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004177000000000000000">SLA_V2TP - Direction Cosines to Tangent Plane</A>
+<A NAME="xref_SLA_V2TP">&#160;</A><A NAME="SLA_V2TP">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Given the direction cosines of a star and of the tangent point,
+determine the star's tangent-plane coordinates
+         (single precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_V2TP (V, V0, XI, ETA, J)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V</EM></TD>
+<TH ALIGN="LEFT"><B>R(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>direction cosines of star</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V0</EM></TD>
+<TD ALIGN="LEFT"><B>R(3)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>direction cosines of tangent point</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>XI,ETA</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>tangent plane coordinates (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  0 = OK, star on tangent plane</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  1 = error, star too far from axis</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  2 = error, antistar on tangent plane</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  3 = error, antistar too far from axis</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>If vector V0 is not of unit length, or if vector V is of zero
+length, the results will be wrong.
+<DT>2.
+<DD>If V0 points at a pole, the returned <IMG WIDTH="26" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img90.gif"
+ ALT="$\xi,\eta$">        will be based on the
+        arbitrary assumption that <IMG WIDTH="43" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img89.gif"
+ ALT="$\alpha=0$"> at the tangent point.
+  <DT>3.
+<DD>The projection is called the <I>gnomonic</I> projection;  the
+        Cartesian coordinates <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img85.gif"
+ ALT="$[\,\xi,\eta\,]$"> are called 
+        <I>standard coordinates.</I>  The latter
+        are in units of the distance from the tangent plane to the projection
+        point, <I>i.e.</I> radians near the origin.
+  <DT>4.
+<DD>This routine is the Cartesian equivalent of the routine sla_S2TP.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html2326" HREF="node191.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2324" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2318" HREF="node189.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2327" HREF="node191.html">SLA_VDV - Scalar Product</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2325" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2319" HREF="node189.html">SLA_UNPCD - Remove Radial Distortion</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node191.html b/src/slalib/sun67.htx/node191.html
new file mode 100644
index 0000000..427bf46
--- /dev/null
+++ b/src/slalib/sun67.htx/node191.html
@@ -0,0 +1,91 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_VDV - Scalar Product</TITLE>
+<META NAME="description" CONTENT="SLA_VDV - Scalar Product">
+<META NAME="keywords" CONTENT="sun67">
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+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2334" HREF="node13.html">
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+<A NAME="tex2html2328" HREF="node190.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2337" HREF="node192.html">SLA_VN - Normalize Vector</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2335" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2329" HREF="node190.html">SLA_V2TP - Direction Cosines to Tangent Plane</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004178000000000000000">SLA_VDV - Scalar Product</A>
+<A NAME="xref_SLA_VDV">&#160;</A><A NAME="SLA_VDV">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Scalar product of two 3-vectors (single precision).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>R&nbsp;=&nbsp;sla_VDV (VA, VB)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>VA</EM></TD>
+<TH ALIGN="LEFT"><B>R(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>first vector</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>VB</EM></TD>
+<TD ALIGN="LEFT"><B>R(3)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>second vector</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_VDV</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>scalar product VA.VB</TD>
+</TR>
+</TABLE></DL>
+<BR> <HR>
+<A NAME="tex2html2336" HREF="node192.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2334" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2328" HREF="node190.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2337" HREF="node192.html">SLA_VN - Normalize Vector</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2335" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2329" HREF="node190.html">SLA_V2TP - Direction Cosines to Tangent Plane</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node192.html b/src/slalib/sun67.htx/node192.html
new file mode 100644
index 0000000..dd4d9b6
--- /dev/null
+++ b/src/slalib/sun67.htx/node192.html
@@ -0,0 +1,95 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_VN - Normalize Vector</TITLE>
+<META NAME="description" CONTENT="SLA_VN - Normalize Vector">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
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+<LINK REL="previous" HREF="node191.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node193.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html2346" HREF="node193.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2344" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2338" HREF="node191.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2347" HREF="node193.html">SLA_VXV - Vector Product</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2345" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2339" HREF="node191.html">SLA_VDV - Scalar Product</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004179000000000000000">SLA_VN - Normalize Vector</A>
+<A NAME="xref_SLA_VN">&#160;</A><A NAME="SLA_VN">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Normalize a 3-vector, also giving the modulus (single precision).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_VN (V, UV, VM)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V</EM></TD>
+<TH ALIGN="LEFT"><B>R(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>vector</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>UV</EM></TD>
+<TH ALIGN="LEFT"><B>R(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>unit vector in direction of V</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>VM</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>modulus of V</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTE:</STRONG>
+<DD>If the modulus of V is zero, UV is set to zero as well.
+</DL>
+<BR> <HR>
+<A NAME="tex2html2346" HREF="node193.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2344" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2338" HREF="node191.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2347" HREF="node193.html">SLA_VXV - Vector Product</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2345" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2339" HREF="node191.html">SLA_VDV - Scalar Product</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node193.html b/src/slalib/sun67.htx/node193.html
new file mode 100644
index 0000000..8f27978
--- /dev/null
+++ b/src/slalib/sun67.htx/node193.html
@@ -0,0 +1,93 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_VXV - Vector Product</TITLE>
+<META NAME="description" CONTENT="SLA_VXV - Vector Product">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node194.html">
+<LINK REL="previous" HREF="node192.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node194.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html2356" HREF="node194.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2354" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2348" HREF="node192.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2357" HREF="node194.html">SLA_WAIT - Time Delay</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2355" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2349" HREF="node192.html">SLA_VN - Normalize Vector</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004180000000000000000">SLA_VXV - Vector Product</A>
+<A NAME="xref_SLA_VXV">&#160;</A><A NAME="SLA_VXV">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Vector product of two 3-vectors (single precision).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_VXV (VA, VB, VC)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>VA</EM></TD>
+<TH ALIGN="LEFT"><B>R(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>first vector</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>VB</EM></TD>
+<TD ALIGN="LEFT"><B>R(3)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>second vector</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>VC</EM></TD>
+<TH ALIGN="LEFT"><B>R(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>vector product VA<IMG WIDTH="15" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img84.gif"
+ ALT="$\times$">VB</TD>
+</TR>
+</TABLE></DL>
+<BR> <HR>
+<A NAME="tex2html2356" HREF="node194.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2354" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2348" HREF="node192.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2357" HREF="node194.html">SLA_WAIT - Time Delay</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2355" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2349" HREF="node192.html">SLA_VN - Normalize Vector</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node194.html b/src/slalib/sun67.htx/node194.html
new file mode 100644
index 0000000..55a0ed7
--- /dev/null
+++ b/src/slalib/sun67.htx/node194.html
@@ -0,0 +1,91 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_WAIT - Time Delay</TITLE>
+<META NAME="description" CONTENT="SLA_WAIT - Time Delay">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
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+<BR> <HR>
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+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+<A NAME="tex2html2358" HREF="node193.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2367" HREF="node195.html">SLA_XY2XY - Apply Linear Model to an</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2365" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2359" HREF="node193.html">SLA_VXV - Vector Product</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004181000000000000000">SLA_WAIT - Time Delay</A>
+<A NAME="xref_SLA_WAIT">&#160;</A><A NAME="SLA_WAIT">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Wait for a specified interval.
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_WAIT (DELAY)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DELAY</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>delay in seconds</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The implementation is machine-specific.
+<DT>2.
+<DD>The delay actually requested is restricted to the range
+100ns-200s in the present implementation.
+  <DT>3.
+<DD>There is no guarantee of accuracy, though on almost all
+        types of computer the program will certainly not
+        resume execution <I>before</I> the stated interval has
+        elapsed.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html2366" HREF="node195.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2364" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2358" HREF="node193.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2367" HREF="node195.html">SLA_XY2XY - Apply Linear Model to an</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2365" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2359" HREF="node193.html">SLA_VXV - Vector Product</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node195.html b/src/slalib/sun67.htx/node195.html
new file mode 100644
index 0000000..2b33ece
--- /dev/null
+++ b/src/slalib/sun67.htx/node195.html
@@ -0,0 +1,114 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_XY2XY - Apply Linear Model to an </TITLE>
+<META NAME="description" CONTENT="SLA_XY2XY - Apply Linear Model to an ">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node196.html">
+<LINK REL="previous" HREF="node194.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node196.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html2376" HREF="node196.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2374" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2368" HREF="node194.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2377" HREF="node196.html">SLA_ZD - to Zenith Distance</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2375" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2369" HREF="node194.html">SLA_WAIT - Time Delay</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004182000000000000000">&#160;</A><A NAME="xref_SLA_XY2XY">&#160;</A><A NAME="SLA_XY2XY">&#160;</A>
+<BR>
+SLA_XY2XY - Apply Linear Model to an <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"></H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Transform one <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> into another using a linear model of the type
+produced by the sla_FITXY routine.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_XY2XY (X1,Y1,COEFFS,X2,Y2)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>X1,Y1</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> before transformation</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>COEFFS</EM></TD>
+<TD ALIGN="LEFT"><B>D(6)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>transformation coefficients (see note)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>X2,Y2</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> after transformation</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The model relates two sets of <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> coordinates as follows.
+Naming the six elements of COEFFS <I>a</I>,<I>b</I>,<I>c</I>,<I>d</I>,<I>e</I> &amp; <I>f</I>,
+the present routine performs the transformation:
+        <BLOCKQUOTE><I>x<SUB>2</SUB></I> = <I>a</I> + <I>bx<SUB>1</SUB></I> + <I>cy<SUB>1</SUB></I> <BR>
+          <I>y<SUB>2</SUB></I> = <I>d</I> + <I>ex<SUB>1</SUB></I> + <I>fy<SUB>1</SUB></I></BLOCKQUOTE>
+  <DT>2.
+<DD>See also sla_FITXY, sla_PXY, sla_INVF, sla_DCMPF.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html2376" HREF="node196.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2374" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2368" HREF="node194.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2377" HREF="node196.html">SLA_ZD - to Zenith Distance</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2375" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2369" HREF="node194.html">SLA_WAIT - Time Delay</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node196.html b/src/slalib/sun67.htx/node196.html
new file mode 100644
index 0000000..0dc168b
--- /dev/null
+++ b/src/slalib/sun67.htx/node196.html
@@ -0,0 +1,137 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_ZD - to Zenith Distance</TITLE>
+<META NAME="description" CONTENT="SLA_ZD - to Zenith Distance">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
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+<LINK REL="previous" HREF="node195.html">
+<LINK REL="up" HREF="node13.html">
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+</HEAD>
+<BODY >
+<BR> <HR>
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+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2382" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2378" HREF="node195.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2385" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2383" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2379" HREF="node195.html">SLA_XY2XY - Apply Linear Model to an</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION0004183000000000000000">&#160;</A><A NAME="xref_SLA_ZD">&#160;</A><A NAME="SLA_ZD">&#160;</A>
+<BR>
+SLA_ZD - <IMG WIDTH="27" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img65.gif"
+ ALT="$h,\delta$"> to Zenith Distance
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Hour angle and declination to zenith distance
+(double precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>D&nbsp;=&nbsp;sla_ZD (HA, DEC, PHI)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>HA</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>hour angle in radians</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DEC</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>declination in radians</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PHI</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>latitude in radians</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_ZD</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>zenith distance (radians, <IMG WIDTH="35" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img234.gif"
+ ALT="$0\!-\!\pi$">)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The latitude must be geodetic.  In critical applications,
+corrections for polar motion should be applied (see sla_POLMO).
+<DT>2.
+<DD>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 zenith distance.  In particular, it may be
+        important to distinguish between the zenith distance
+        as affected by refraction, which would require the
+        <I>observed</I> <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$">, and the zenith distance <I>in vacuo</I>,
+        which would require the <I>topocentric</I> <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$">.  If
+        the effects of diurnal aberration can be neglected, the
+        <I>apparent</I> <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$"> may be used instead of the
+        <I>topocentric</I> <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$">.  <DT>3.
+<DD>No range checking of arguments is done.
+  <DT>4.
+<DD>In applications which involve many zenith distance 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 perhaps sine and
+        cosine of declination.
+ </DL></DL>
+<P>
+<BR>
+<P>
+<BR> <HR>
+<A NAME="tex2html2384" HREF="node197.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2382" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2378" HREF="node195.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2385" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2383" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2379" HREF="node195.html">SLA_XY2XY - Apply Linear Model to an</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node197.html b/src/slalib/sun67.htx/node197.html
new file mode 100644
index 0000000..ae8cd55
--- /dev/null
+++ b/src/slalib/sun67.htx/node197.html
@@ -0,0 +1,171 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>EXPLANATION AND EXAMPLES</TITLE>
+<META NAME="description" CONTENT="EXPLANATION AND EXAMPLES">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node228.html">
+<LINK REL="previous" HREF="node13.html">
+<LINK REL="up" HREF="sun67.html">
+<LINK REL="next" HREF="node198.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html2394" HREF="node198.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2392" HREF="sun67.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2386" HREF="node196.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2395" HREF="node198.html">Spherical Trigonometry</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2393" HREF="sun67.html">SLALIB   Positional Astronomy Library</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2387" HREF="node196.html">SLA_ZD - to Zenith Distance</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H1><A NAME="SECTION00050000000000000000">
+EXPLANATION AND EXAMPLES</A>
+</H1>
+To guide the writer of positional-astronomy applications software,
+this final chapter puts the SLALIB routines into the context of
+astronomical phenomena and techniques, and presents a few
+``cookbook'' examples
+of the SLALIB calls in action.  The astronomical content of the chapter
+is not, of course, intended to be a substitute for specialist text-books on
+positional astronomy, but may help bridge the gap between
+such books and the SLALIB routines.  For further reading, the following
+cover a wide range of material and styles:
+<UL>
+<LI> <I>Explanatory Supplement to the Astronomical Almanac</I>,
+      ed. P.Kenneth&nbsp;Seidelmann (1992), University Science Books.
+<LI> <I>Vectorial Astrometry</I>, C.A.Murray (1983), Adam Hilger.
+<LI> <I>Spherical Astronomy</I>, Robin&nbsp;M.Green (1985), Cambridge
+      University Press.
+<LI> <I>Spacecraft Attitude Determination and Control</I>,
+      ed. James&nbsp;R.Wertz (1986), Reidel.
+<LI> <I>Practical Astronomy with your Calculator</I>,
+      Peter&nbsp;Duffett-Smith (1981), Cambridge University Press.
+</UL>
+Also of considerable value, though out of date in places, are:
+<UL>
+<LI> <I>Explanatory Supplement to the Astronomical Ephemeris
+      and the American Ephemeris and Nautical Almanac</I>, RGO/USNO (1974),
+      HMSO.
+<LI> <I>Textbook on Spherical Astronomy</I>, W.M.Smart (1977),
+      Cambridge University Press.
+</UL>
+Only brief details of individual SLALIB routines are given here, and
+readers will find it useful to refer to the subprogram specifications
+elsewhere in this document.  The source code for the SLALIB routines
+(available in both Fortran and C) is also intended to be used as
+documentation.
+<P>
+<BR><HR>
+<!--Table of Child-Links-->
+<A NAME="CHILD_LINKS">&#160;</A>
+<UL>
+<LI><A NAME="tex2html2396" HREF="node198.html#SECTION00051000000000000000">
+Spherical Trigonometry</A>
+<UL>
+<LI><A NAME="tex2html2397" HREF="node199.html#SECTION00051100000000000000">
+Formatting angles</A>
+</UL>
+<LI><A NAME="tex2html2398" HREF="node200.html#SECTION00052000000000000000">
+Vectors and Matrices</A>
+<UL>
+<LI><A NAME="tex2html2399" HREF="node201.html#SECTION00052100000000000000">
+Using vectors</A>
+</UL>
+<LI><A NAME="tex2html2400" HREF="node202.html#SECTION00053000000000000000">
+Celestial Coordinate Systems</A>
+<LI><A NAME="tex2html2401" HREF="node203.html#SECTION00054000000000000000">
+Precession and Nutation</A>
+<UL>
+<LI><A NAME="tex2html2402" HREF="node204.html#SECTION00054100000000000000">
+SLALIB support for precession and nutation</A>
+</UL>
+<LI><A NAME="tex2html2403" HREF="node205.html#SECTION00055000000000000000">
+Mean Places</A>
+<LI><A NAME="tex2html2404" HREF="node206.html#SECTION00056000000000000000">
+Epoch</A>
+<LI><A NAME="tex2html2405" HREF="node207.html#SECTION00057000000000000000">
+Proper Motion</A>
+<LI><A NAME="tex2html2406" HREF="node208.html#SECTION00058000000000000000">
+Parallax and Radial Velocity</A>
+<LI><A NAME="tex2html2407" HREF="node209.html#SECTION00059000000000000000">
+Aberration</A>
+<LI><A NAME="tex2html2408" HREF="node210.html#SECTION000510000000000000000">
+Different Sorts of Mean Place</A>
+<LI><A NAME="tex2html2409" HREF="node211.html#SECTION000511000000000000000">
+Mean Place Transformations</A>
+<LI><A NAME="tex2html2410" HREF="node212.html#SECTION000512000000000000000">
+Mean Place to Apparent Place</A>
+<LI><A NAME="tex2html2411" HREF="node213.html#SECTION000513000000000000000">
+Apparent Place to Observed Place</A>
+<UL>
+<LI><A NAME="tex2html2412" HREF="node214.html#SECTION000513100000000000000">
+Refraction</A>
+<LI><A NAME="tex2html2413" HREF="node215.html#SECTION000513200000000000000">
+Efficiency considerations</A>
+</UL>
+<LI><A NAME="tex2html2414" HREF="node216.html#SECTION000514000000000000000">
+The Hipparcos Catalogue and the ICRS</A>
+<LI><A NAME="tex2html2415" HREF="node217.html#SECTION000515000000000000000">
+Timescales</A>
+<UL>
+<LI><A NAME="tex2html2416" HREF="node218.html#SECTION000515100000000000000">
+Atomic Time: TAI</A>
+<LI><A NAME="tex2html2417" HREF="node219.html#SECTION000515200000000000000">
+Universal Time: UTC, UT1</A>
+<LI><A NAME="tex2html2418" HREF="node220.html#SECTION000515300000000000000">
+Sidereal Time: GMST, LAST</A>
+<LI><A NAME="tex2html2419" HREF="node221.html#SECTION000515400000000000000">
+Dynamical Time: TT, TDB</A>
+</UL>
+<LI><A NAME="tex2html2420" HREF="node222.html#SECTION000516000000000000000">
+Calendars</A>
+<LI><A NAME="tex2html2421" HREF="node223.html#SECTION000517000000000000000">
+Geocentric Coordinates</A>
+<LI><A NAME="tex2html2422" HREF="node224.html#SECTION000518000000000000000">
+Ephemerides</A>
+<LI><A NAME="tex2html2423" HREF="node225.html#SECTION000519000000000000000">
+Radial Velocity and Light-Time Corrections</A>
+<LI><A NAME="tex2html2424" HREF="node226.html#SECTION000520000000000000000">
+Focal-Plane Astrometry</A>
+<LI><A NAME="tex2html2425" HREF="node227.html#SECTION000521000000000000000">
+Numerical Methods</A>
+</UL>
+<!--End of Table of Child-Links-->
+<BR> <HR>
+<A NAME="tex2html2394" HREF="node198.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2392" HREF="sun67.html">
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+<A NAME="tex2html2386" HREF="node196.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2395" HREF="node198.html">Spherical Trigonometry</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2393" HREF="sun67.html">SLALIB   Positional Astronomy Library</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2387" HREF="node196.html">SLA_ZD - to Zenith Distance</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node198.html b/src/slalib/sun67.htx/node198.html
new file mode 100644
index 0000000..30aa3e8
--- /dev/null
+++ b/src/slalib/sun67.htx/node198.html
@@ -0,0 +1,167 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Spherical Trigonometry</TITLE>
+<META NAME="description" CONTENT="Spherical Trigonometry">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
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+<A NAME="tex2html2426" HREF="node197.html">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2435" HREF="node199.html">Formatting angles</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2433" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2427" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION00051000000000000000">
+Spherical Trigonometry</A>
+</H2>
+Celestial phenomena occur at such vast distances from the
+observer that for most practical purposes there is no need to
+work in 3D;  only the direction
+of a source matters, not how far away it is.  Things can
+therefore be viewed as if they were happening
+on the inside of sphere with the observer at the centre -
+the <I>celestial sphere</I>.  Problems involving
+positions and orientations in the sky can then be solved by
+using the formulae of <I>spherical trigonometry</I>, which
+apply to <I>spherical triangles</I>, the sides of which are
+<I>great circles</I>.
+<P>
+Positions on the celestial sphere may be specified by using
+a spherical polar coordinate system, defined in terms of
+some fundamental plane and a line in that plane chosen to
+represent zero longitude.  Mathematicians usually work with the
+co-latitude, with zero at the principal pole, whereas most
+astronomical coordinate systems use latitude, reckoned plus and
+minus from the equator.
+Astronomical coordinate systems may be either right-handed
+(<I>e.g.</I> right ascension and declination <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">,Galactic longitude and latitude <IMG WIDTH="59" HEIGHT="32" ALIGN="MIDDLE" BORDER="0"
+ SRC="img98.gif"
+ ALT="$[\,l^{I\!I},b^{I\!I}\,]$">)or left-handed (<I>e.g.</I> hour angle and
+declination <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$">).  In some cases
+different conventions have been used in the past, a fruitful source of
+mistakes.  Azimuth and geographical longitude are examples;  azimuth
+is now generally reckoned north through east
+(making a left-handed system);  geographical longitude is now usually
+taken to increase eastwards (a right-handed system) but astronomers
+used to employ a west-positive convention.  In reports
+and program comments it is wise to spell out what convention
+is being used, if there is any possibility of confusion.
+<P>
+When applying spherical trigonometry formulae, attention must be
+paid to
+rounding errors (for example it is a bad idea to find a
+small angle through its cosine) and to the possibility of
+problems close to poles.
+Also, if a formulation relies on inspection to establish
+the quadrant of the result, it is an indication that a vector-related
+method might be preferable.
+<P>
+As well as providing many routines which work in terms of specific
+spherical coordinates such as <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">, SLALIB provides
+two routines which operate directly on generic spherical
+coordinates:
+sla_SEP
+computes the separation between
+two points (the distance along a great circle) and
+sla_BEAR
+computes the bearing (or <I>position angle</I>)
+of one point seen from the other.  The routines
+sla_DSEP
+and
+sla_DBEAR
+are double precision equivalents.  As a simple demonstration
+of SLALIB, we will use these facilities to estimate the distance from
+London to Sydney and the initial compass heading:
+<P><PRE>
+            IMPLICIT NONE
+
+      *  Degrees to radians
+            REAL D2R
+            PARAMETER (D2R=0.01745329252)
+
+      *  Longitudes and latitudes (radians) for London and Sydney
+            REAL AL,BL,AS,BS
+            PARAMETER (AL=-0.2*D2R,BL=51.5*D2R,AS=151.2*D2R,BS=-33.9*D2R)
+
+      *  Earth radius in km (spherical approximation)
+            REAL RKM
+            PARAMETER (RKM=6375.0)
+
+            REAL sla_SEP,sla_BEAR
+
+
+      *  Distance and initial heading (N=0, E=90)
+            WRITE (*,'(1X,I5,'' km,'',I4,'' deg'')')
+           :    NINT(sla_SEP(AL,BL,AS,BS)*RKM),NINT(sla_BEAR(AL,BL,AS,BS)/D2R)
+
+            END
+</PRE>
+<P>(The result is 17011&nbsp;km, <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img235.gif"
+ ALT="$61^\circ$">.)
+<P>
+The routines
+sla_PAV and
+sla_DPAV
+are equivalents of sla_BEAR and sla_DBEAR but starting from
+direction-cosines instead of spherical coordinates.
+<P>
+<BR><HR>
+<!--Table of Child-Links-->
+<A NAME="CHILD_LINKS">&#160;</A>
+<UL>
+<LI><A NAME="tex2html2436" HREF="node199.html#SECTION00051100000000000000">
+Formatting angles</A>
+</UL>
+<!--End of Table of Child-Links-->
+<BR> <HR>
+<A NAME="tex2html2434" HREF="node199.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2432" HREF="node197.html">
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+<A NAME="tex2html2426" HREF="node197.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2435" HREF="node199.html">Formatting angles</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2433" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2427" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node199.html b/src/slalib/sun67.htx/node199.html
new file mode 100644
index 0000000..93a4839
--- /dev/null
+++ b/src/slalib/sun67.htx/node199.html
@@ -0,0 +1,174 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Formatting angles</TITLE>
+<META NAME="description" CONTENT="Formatting angles">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
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+<BODY >
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+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2441" HREF="node198.html">
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+<A NAME="tex2html2437" HREF="node198.html">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2444" HREF="node200.html">Vectors and Matrices</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2442" HREF="node198.html">Spherical Trigonometry</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2438" HREF="node198.html">Spherical Trigonometry</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H3><A NAME="SECTION00051100000000000000">
+Formatting angles</A>
+</H3>
+SLALIB has routines for decoding decimal numbers
+from character form and for converting angles to and from
+sexagesimal form (hours, minutes, seconds or degrees,
+arcminutes, arcseconds).  These apparently straightforward
+operations contain hidden traps which the SLALIB routines
+avoid.
+<P>
+There are five routines for decoding numbers from a character
+string, such as might be entered using a keyboard.
+They all work in the same style, and successive calls
+can work their way along a single string decoding
+a sequence of numbers of assorted types.  Number
+fields can be separated by spaces or commas, and can be defaulted
+to previous values or to preset defaults.
+<P>
+Three of the routines decode single numbers:
+sla_INTIN
+(integer),
+sla_FLOTIN
+(single precision floating point) and
+sla_DFLTIN
+(double precision).  A minus sign can be
+detected even when the number is zero;  this avoids
+the frequently-encountered ``minus zero'' bug, where
+declinations <I>etc.</I> in
+the range <IMG WIDTH="18" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img1.gif"
+ ALT="$0^{\circ}$"> to <IMG WIDTH="30" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img2.gif"
+ ALT="$-1^{\circ}$"> mysteriously migrate to
+the range <IMG WIDTH="18" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img1.gif"
+ ALT="$0^{\circ}$"> to <IMG WIDTH="30" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img236.gif"
+ ALT="$+1^{\circ}$">.Here is an example (in Fortran) where we wish to
+read two numbers, and integer <TT>IX</TT> and a real, <TT>Y</TT>,
+with <TT>X</TT> defaulting to zero and <TT>Y</TT> defaulting to
+<TT>X</TT>:
+<P><PRE>
+            DOUBLE PRECISION Y
+            CHARACTER*80 A
+            INTEGER IX,I,J
+
+      *  Input the string to be decoded
+            READ (*,'(A)') A
+
+      *  Preset IX to its default value
+            IX = 0
+
+      *  Point to the start of the string
+            I = 1
+
+      *  Decode an integer
+            CALL sla_INTIN(A,I,IX,J)
+            IF (J.GT.1) GO TO ... (bad IX)
+
+      *  Preset Y to its default value
+            Y = DBLE(IX)
+
+      *  Decode a double precision number
+            CALL sla_DFLTIN(A,I,Y,J)
+            IF (J.GT.1) GO TO ... (bad Y)
+</PRE>
+<P>
+Two additional routines decode a 3-field sexagesimal number:
+sla_AFIN
+(degrees, arcminutes, arcseconds to single
+precision radians) and
+sla_DAFIN
+(the same but double precision).  They also
+work using other units such as hours <I>etc</I>. if
+you multiply the result by the appropriate factor.  An example
+Fortran program which uses
+sla_DAFIN
+was given earlier, in section 1.2.
+<P>
+SLALIB provides four routines for expressing an angle in radians
+in a preferred range.  The function
+sla_RANGE
+expresses an angle
+in the range <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$">;sla_RANORM
+expresses an angle in the range
+<IMG WIDTH="48" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img143.gif"
+ ALT="$0-2\pi$">.  The functions
+sla_DRANGE
+and
+sla_DRANRM
+are double precision versions.
+<P>
+Several routines
+(sla_CTF2D,
+sla_CR2AF
+<I>etc.</I>) are provided to convert
+angles to and from
+sexagesimal form (hours, minute, seconds or degrees,
+arcminutes and arcseconds).
+They avoid the common
+``converting from integer to real at the wrong time''
+bug, which produces angles like <IMG WIDTH="113" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img237.gif"
+ ALT="$24^{h}\,59^{m}\,59^{s}.999$">.Here is a program which displays an hour angle
+stored in radians:
+<P><PRE>
+            DOUBLE PRECISION HA
+            CHARACTER SIGN
+            INTEGER IHMSF(4)
+            :
+            CALL sla_DR2TF(3,HA,SIGN,IHMSF)
+            WRITE (*,'(1X,A,3I3.2,''.'',I3.3)') SIGN,IHMSF
+</PRE>
+<P>
+<BR> <HR>
+<A NAME="tex2html2443" HREF="node200.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2444" HREF="node200.html">Vectors and Matrices</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2442" HREF="node198.html">Spherical Trigonometry</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2438" HREF="node198.html">Spherical Trigonometry</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node2.html b/src/slalib/sun67.htx/node2.html
new file mode 100644
index 0000000..2e1859d
--- /dev/null
+++ b/src/slalib/sun67.htx/node2.html
@@ -0,0 +1,85 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>INTRODUCTION</TITLE>
+<META NAME="description" CONTENT="INTRODUCTION">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node12.html">
+<LINK REL="previous" HREF="node1.html">
+<LINK REL="up" HREF="sun67.html">
+<LINK REL="next" HREF="node3.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html256" HREF="node3.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html254" HREF="sun67.html">
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+<H1><A NAME="SECTION00020000000000000000">
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+<!--Table of Child-Links-->
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+Purpose</A>
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+Example Application</A>
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+C Version</A>
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+Future Versions</A>
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+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node20.html b/src/slalib/sun67.htx/node20.html
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+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
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+<TITLE>SLA_AOP - Apparent to Observed</TITLE>
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+<H2><A NAME="SECTION00047000000000000000">SLA_AOP - Apparent to Observed</A>
+<A NAME="xref_SLA_AOP">&#160;</A><A NAME="SLA_AOP">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Apparent to observed place, for optical sources distant from
+the solar system.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_AOP (
+         RAP, DAP, DATE, DUT, ELONGM, PHIM, HM, XP, YP,
+         TDK, PMB, RH, WL, TLR, AOB, ZOB, HOB, DOB, ROB)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RAP,DAP</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>geocentric apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>UTC date/time (Modified Julian Date, JD-2400000.5)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DUT</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">UT:  UT1-UTC (UTC seconds)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ELONGM</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>observer's mean longitude (radians, east +ve)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PHIM</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>observer's mean geodetic latitude (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>HM</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>observer's height above sea level (metres)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>XP,YP</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>polar motion <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> coordinates (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>TDK</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>local ambient temperature (degrees K; std=273.155D0)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PMB</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>local atmospheric pressure (mB; std=1013.25D0)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>local relative humidity (in the range 0D0-1D0)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>WL</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>effective wavelength (<IMG WIDTH="26" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img21.gif"
+ ALT="$\mu{\rm m}$">, <I>e.g.</I> 0.55D0)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>TLR</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>tropospheric lapse rate (degrees K per metre,
+<I>e.g.</I> 0.0065D0)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AOB</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>observed azimuth (radians: N=0, E=<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img22.gif"
+ ALT="$90^{\circ}$">)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ZOB</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>observed zenith distance (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>HOB</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>observed Hour Angle (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DOB</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>observed <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ROB</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>observed <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>This routine returns zenith distance rather than elevation
+in order to reflect the fact that no allowance is made for
+depression of the horizon.
+  <DT>2.
+<DD>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 azimuth and elevation should be within about
+<P>      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img25.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.1$">    for <IMG WIDTH="56" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img26.gif"
+ ALT="$\zeta<70^{\circ}$">.  Even
+        at a topocentric zenith distance of
+        <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img22.gif"
+ ALT="$90^{\circ}$">, the accuracy in elevation should be better than
+        1&nbsp;arcminute;  useful results are available for a further
+        <IMG WIDTH="18" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img27.gif"
+ ALT="$3^{\circ}$">, beyond which the sla_REFRO routine returns a
+        fixed value of the refraction.  The complementary
+        routines sla_AOP (or sla_AOPQK) and sla_OAP (or sla_OAPQK)
+        are self-consistent to better than 1&nbsp;microarcsecond all over
+        the celestial sphere.
+  <DT>3.
+<DD>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.
+  <DT>4.
+<DD><I>Apparent</I> <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> 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>i.e.</I> J2000), these effects can
+        be applied by means of the sla_MAP <I>etc.</I> routines.  Starting from
+        other mean place systems, additional transformations will be
+        needed;  for example, FK4 (<I>i.e.</I> B1950) mean places would first
+        have to be converted to FK5, which can be done with the
+        sla_FK425 <I>etc.</I> routines.
+  <DT>5.
+<DD><I>Observed</I> <IMG WIDTH="66" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img28.gif"
+ ALT="$[\,Az,El~]$"> means the position that would be seen by a
+        perfect theodolite located at the observer.  This is obtained
+        from the geocentric apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> by allowing for Earth
+        orientation and diurnal aberration, rotating from equator
+        to horizon coordinates, and then adjusting for refraction.
+        The <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$"> 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 (<I>n.b.</I> not to the
+        refracted pole).  Finally, the <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> is obtained by subtracting
+        the <I>h</I> from the local apparent ST.
+  <DT>6.
+<DD>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.
+  <DT>7.
+<DD>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 sla_AOPPA once followed by one call per star to sla_AOPQK.
+        Where a range of times within a limited period of a few hours
+        is involved, and the highest precision is not required, call
+        sla_AOPPA once, followed by a call to sla_AOPPAT each time the
+        time changes, followed by one call per star to sla_AOPQK.
+  <DT>8.
+<DD>The DATE argument is UTC expressed as an MJD.  This is,
+        strictly speaking, wrong, because of leap seconds.  However,
+        as long as the <IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">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 <IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">UT should
+        continue to be used.  As the 61st second completes, the MJD
+        should revert to the start of the day as, simultaneously,
+        the <IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">UT changes by one second to its post-leap new value.
+  <DT>9.
+<DD>The <IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">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 <IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">UT
+        within <IMG WIDTH="15" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img30.gif"
+ ALT="$\pm$"><IMG WIDTH="24" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img31.gif"
+ ALT="$0^{\rm s}\hspace{-0.3em}.9$">.  <DT>10.
+<DD>IMPORTANT - TAKE CARE WITH THE LONGITUDE SIGN CONVENTION.  The
+        longitude required by the present routine is <B>east-positive</B>,
+        in accordance with geographical convention (and right-handed).
+        In particular, note that the longitudes returned by the
+        sla_OBS routine are west-positive (as in the <I>Astronomical
+        Almanac</I> before 1984) and must be reversed in sign before use
+        in the present routine.
+  <DT>11.
+<DD>The polar coordinates XP,YP can be obtained from IERS
+        circulars and equivalent publications.  The
+        maximum amplitude is about 
+      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img32.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.3$">   .  If XP,YP values
+        are unavailable, use XP=YP=0D0.  See page B60 of the 1988
+        <I>Astronomical Almanac</I> for a definition of the two angles.
+  <DT>12.
+<DD>The height above sea level of the observing station, HM,
+        can be obtained from the <I>Astronomical Almanac</I> (Section J
+        in the 1988 edition), or via the routine sla_OBS.  If P,
+        the pressure in mB, is available, an adequate
+        estimate of HM can be obtained from the following expression:
+        <BLOCKQUOTE><TT>HM=-29.3D0*TSL*LOG(P/1013.25D0)</TT>
+        </BLOCKQUOTE>
+        where TSL is the approximate sea-level air temperature in degrees K
+        (see <I>Astrophysical Quantities</I>, C.W.Allen, 3rd&nbsp;edition,
+        &#167;52).  Similarly, if the pressure P is not known,
+        it can be estimated from the height of the observing
+        station, HM as follows:
+        <BLOCKQUOTE><TT>P=1013.25D0*EXP(-HM/(29.3D0*TSL))</TT>
+        </BLOCKQUOTE>
+        Note, however, that the refraction is proportional to the
+        pressure and that an accurate P value is important for
+        precise work.
+  <DT>13.
+<DD>The azimuths <I>etc.</I> used by the present routine are with
+        respect to the celestial pole.  Corrections to the terrestrial pole
+        can be computed using sla_POLMO.
+ </DL></DL>
+<BR> <HR>
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+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
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+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
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+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION00052000000000000000">
+Vectors and Matrices</A>
+</H2>
+As an alternative to employing a spherical polar coordinate system,
+the direction of an object can be defined in terms of the sum of any
+three vectors as long as they are different and
+not coplanar.  In practice, three vectors at right angles are
+usually chosen, forming a system
+of <I>Cartesian coordinates</I>.  The <I>x</I>- and <I>y</I>-axes
+lie in the fundamental plane (<I>e.g.</I> the equator in the
+case of <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">), with the <I>x</I>-axis pointing to zero longitude.
+The <I>z</I>-axis is normal to the fundamental plane and points
+towards positive latitudes.  The <I>y</I>-axis can lie in either
+of the two possible directions, depending on whether the
+coordinate system is right-handed or left-handed.
+The three axes are sometimes called
+a <I>triad</I>.  For most applications involving arbitrarily
+distant objects such as stars, the vector which defines
+the direction concerned is constrained to have unit length.
+The <I>x</I>-, <I>y-</I> and <I>z-</I>components
+can be regarded as the scalar (dot) product of this vector
+onto the three axes of the triad in turn.  Because the vector
+is a unit vector,
+each of the three dot-products is simply the cosine of the angle
+between the unit vector and the axis concerned, and the
+<I>x</I>-, <I>y-</I> and <I>z-</I>components are sometimes
+called <I>direction cosines</I>.
+<P>
+For some applications involving objects
+with the Solar System, unit vectors are inappropriate, and
+it is necessary to use vectors scaled in length-units such as
+AU, km <I>etc.</I>
+In these cases the origin of the coordinate system may not be
+the observer, but instead might be the Sun, the Solar-System
+barycentre, the centre of the Earth <I>etc.</I>  But whatever the application,
+the final direction in which the observer sees the object can be
+expressed as direction cosines.
+<P>
+But where has this got us?  Instead of two numbers - a longitude and
+a latitude - we now have three numbers to look after
+- the <I>x</I>-, <I>y-</I> and
+<I>z-</I>components - whose quadratic sum we have somehow to contrive to
+be unity.  And, in addition to this apparent redundancy,
+most people find it harder to visualize
+problems in terms of <IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$"> than in <IMG WIDTH="45" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img238.gif"
+ ALT="$[\,\theta,\phi~]$">.Despite these objections, the vector approach turns out to have
+significant advantages over the spherical trigonometry approach:
+<UL>
+<LI> Vector formulae tend to be much more succinct;  one vector
+      operation is the equivalent of strings of sines and cosines.
+<LI> The formulae are as a rule rigorous, even at the poles.
+<LI> Accuracy is maintained all over the celestial sphere.
+      When one Cartesian component is nearly unity and
+      therefore insensitive to direction, the others become small
+      and therefore more precise.
+<LI> Formulations usually deliver the quadrant of the result
+      without the need for any inspection (except within the
+      library function ATAN2).
+</UL>
+A number of important transformations in positional
+astronomy turn out to be nothing more than changes of coordinate
+system, something which is especially convenient if
+the vector approach is used.  A direction with respect
+to one triad can be expressed relative to another triad simply
+by multiplying the <IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$"> column vector by the appropriate
+<IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img18.gif"
+ ALT="$3\times3$"> orthogonal matrix
+(a tensor of Rank&nbsp;2, or <I>dyadic</I>).  The three rows of this
+<I>rotation matrix</I>
+are the vectors in the old coordinate system of the three
+new axes, and the transformation amounts to obtaining the
+dot-product of the direction-vector with each of the three
+new axes.  Precession, nutation, <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$"> to <IMG WIDTH="66" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img28.gif"
+ ALT="$[\,Az,El~]$">,<IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> to <IMG WIDTH="59" HEIGHT="32" ALIGN="MIDDLE" BORDER="0"
+ SRC="img98.gif"
+ ALT="$[\,l^{I\!I},b^{I\!I}\,]$"> and so on are typical examples of the
+technique.  A useful property of the rotation matrices
+is that they can be inverted simply by taking the transpose.
+<P>
+The elements of these vectors and matrices are assorted combinations of
+the sines and cosines of the various angles involved (hour angle,
+declination and so on, depending on which transformation is
+being applied).  If you write out the matrix multiplications
+in full you get expressions which are essentially the same as the
+equivalent spherical trigonometry formulae.  Indeed, many of the
+standard formulae of spherical trigonometry are most easily
+derived by expressing the problem initially in
+terms of vectors.
+<P>
+<BR><HR>
+<!--Table of Child-Links-->
+<A NAME="CHILD_LINKS">&#160;</A>
+<UL>
+<LI><A NAME="tex2html2455" HREF="node201.html#SECTION00052100000000000000">
+Using vectors</A>
+</UL>
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+<B> Next:</B> <A NAME="tex2html2454" HREF="node201.html">Using vectors</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2452" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2446" HREF="node199.html">Formatting angles</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node201.html b/src/slalib/sun67.htx/node201.html
new file mode 100644
index 0000000..4613125
--- /dev/null
+++ b/src/slalib/sun67.htx/node201.html
@@ -0,0 +1,215 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Using vectors</TITLE>
+<META NAME="description" CONTENT="Using vectors">
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+<BR>
+<B> Previous:</B> <A NAME="tex2html2457" HREF="node200.html">Vectors and Matrices</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H3><A NAME="SECTION00052100000000000000">
+Using vectors</A>
+</H3>
+SLALIB provides conversions between spherical and vector
+form
+(sla_CS2C,
+sla_CC2S
+<I>etc.</I>), plus an assortment
+of standard vector and matrix operations
+(sla_VDV,
+sla_MXV
+<I>etc.</I>).
+There are also routines
+(sla_EULER
+<I>etc.</I>) for creating a rotation matrix
+from three <I>Euler angles</I> (successive rotations about
+specified Cartesian axes).  Instead of Euler angles, a rotation
+matrix can be expressed as an <I>axial vector</I> (the pole of the rotation,
+and the amount of rotation), and routines are provided for this
+(sla_AV2M,
+sla_M2AV
+<I>etc.</I>).
+<P>
+Here is an example where spherical coordinates <TT>P1</TT> and <TT>Q1</TT>
+undergo a coordinate transformation and become <TT>P2</TT> and <TT>Q2</TT>;
+the transformation consists of a rotation of the coordinate system
+through angles <TT>A</TT>, <TT>B</TT> and <TT>C</TT> about the
+<I>z</I>, new <I>y</I> and new <I>z</I> axes respectively:
+<P><PRE>
+            REAL A,B,C,R(3,3),P1,Q1,V1(3),V2(3),P2,Q2
+             :
+      *  Create rotation matrix
+            CALL sla_EULER('ZYZ',A,B,C,R)
+
+      *  Transform position (P,Q) from spherical to Cartesian
+            CALL sla_CS2C(P1,Q1,V1)
+
+      *  Multiply by rotation matrix
+            CALL sla_MXV(R,V1,V2)
+
+      *  Back to spherical
+            CALL sla_CC2S(V2,P2,Q2)
+</PRE>
+<P>
+Small adjustments to the direction of a position
+vector are often most conveniently described in terms of
+<IMG WIDTH="99" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img239.gif"
+ ALT="$[\,\Delta x,\Delta y, \Delta z\,]$">.  Adding the correction
+vector needs careful handling if the position
+vector is to remain of length unity, an advisable precaution which
+ensures that
+the <IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$"> components are always available to mean the cosines of
+the angles between the vector and the axis concerned.  Two types
+of shifts are commonly used,
+the first where a small vector of arbitrary direction is
+added to the unit vector, and the second where there is a displacement
+in the latitude coordinate (declination, elevation <I>etc.</I>) alone.
+<P>
+For a shift produced by adding a small <IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$"> vector <IMG WIDTH="17" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img240.gif"
+ ALT="${\bf D}$"> to a
+unit vector <IMG WIDTH="26" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img241.gif"
+ ALT="${\bf V1}$">, the resulting vector <IMG WIDTH="26" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img242.gif"
+ ALT="${\bf V2}$"> has direction
+<IMG WIDTH="95" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img243.gif"
+ ALT="$<{\bf V1}+{\bf D}\gt$"> but is no longer of unit length.  A better approximation
+is available if the result is multiplied by a scaling factor of
+<IMG WIDTH="93" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img244.gif"
+ ALT="$(1-{\bf D}\cdot{\bf V1})$">, where the dot
+means scalar product.  In Fortran:
+<P><PRE>
+            F = (1D0-(DX*V1X+DY*V1Y+DZ*V1Z))
+            V2X = F*(V1X+DX)
+            V2Y = F*(V1Y+DY)
+            V2Z = F*(V1Z+DZ)
+</PRE>
+<P>
+The correction for diurnal aberration (discussed later) is
+an example of this form of shift.
+<P>
+As an example of the second kind of displacement
+we will apply a small change in elevation <IMG WIDTH="23" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img245.gif"
+ ALT="$\delta E$"> to an
+<IMG WIDTH="66" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img28.gif"
+ ALT="$[\,Az,El~]$"> direction vector.  The direction of the
+result can be obtained by making the allowable approximation
+<IMG WIDTH="92" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img246.gif"
+ ALT="${\tan \delta E\approx\delta E}$"> and adding a adjustment
+vector of length <IMG WIDTH="23" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img245.gif"
+ ALT="$\delta E$"> normal
+to the direction vector in the vertical plane containing the direction
+vector.  The <I>z</I>-component of the adjustment vector is
+<IMG WIDTH="64" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img247.gif"
+ ALT="$\delta E \cos E$">,and the horizontal component is
+<IMG WIDTH="62" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img248.gif"
+ ALT="$\delta E \sin E$"> which has then to be
+resolved into <I>x</I> and <I>y</I> in proportion to their current sizes. To
+approximate a unit vector more closely, a correction factor of
+<IMG WIDTH="48" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img249.gif"
+ ALT="$\cos \delta E$"> can then be applied, which is nearly
+<IMG WIDTH="88" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img250.gif"
+ ALT="$(1-\delta E^2 /2)$"> for
+small <IMG WIDTH="23" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img245.gif"
+ ALT="$\delta E$">.  Expressed in Fortran, for initial vector
+<TT>V1X,V1Y,V1Z</TT>, change in elevation <TT>DEL</TT>
+(+ve <IMG WIDTH="15" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img251.gif"
+ ALT="$\equiv$"> upwards), and result
+vector <TT>V2X,V2Y,V2Z</TT>:
+<P><PRE>
+            COSDEL = 1D0-DEL*DEL/2D0
+            R1 = SQRT(V1X*V1X+V1Y*V1Y)
+            F = COSDEL*(R1-DEL*V1Z)/R1
+            V2X = F*V1X
+            V2Y = F*V1Y
+            V2Z = COSDEL*(V1Z+DEL*R1)
+</PRE>
+<P>
+An example of this type of shift is the correction for atmospheric
+refraction (see later).
+Depending on the relationship between <IMG WIDTH="23" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img245.gif"
+ ALT="$\delta E$"> and <I>E</I>, special
+handling at the pole (the zenith for our example) may be required.
+<P>
+SLALIB includes routines for the case where both a position
+and a velocity are involved.  The routines
+sla_CS2C6
+and
+sla_CC62S
+convert from <IMG WIDTH="69" HEIGHT="35" ALIGN="MIDDLE" BORDER="0"
+ SRC="img252.gif"
+ ALT="$[\theta,\phi,\dot{\theta},\dot{\phi}]$">to <IMG WIDTH="106" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img51.gif"
+ ALT="$[\,x,y,z,\dot{x},\dot{y},\dot{z}\,]$"> and back;
+sla_DCS26
+and
+sla_DC62S
+are double precision equivalents.
+<P>
+<BR> <HR>
+<A NAME="tex2html2462" HREF="node202.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2463" HREF="node202.html">Celestial Coordinate Systems</A>
+<BR>
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+<BR>
+<B> Previous:</B> <A NAME="tex2html2457" HREF="node200.html">Vectors and Matrices</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node202.html b/src/slalib/sun67.htx/node202.html
new file mode 100644
index 0000000..a161c65
--- /dev/null
+++ b/src/slalib/sun67.htx/node202.html
@@ -0,0 +1,254 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Celestial Coordinate Systems</TITLE>
+<META NAME="description" CONTENT="Celestial Coordinate Systems">
+<META NAME="keywords" CONTENT="sun67">
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+<B> Next:</B> <A NAME="tex2html2473" HREF="node203.html">Precession and Nutation</A>
+<BR>
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+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION00053000000000000000">
+Celestial Coordinate Systems</A>
+</H2>
+SLALIB has routines to perform transformations
+of celestial positions between different spherical
+coordinate systems, including those shown in the following table:
+<P>
+<DIV ALIGN="CENTER">
+<TABLE CELLPADDING=3 BORDER="1">
+<TR VALIGN="TOP"><TH ALIGN="LEFT" NOWRAP><I>system</I></TH>
+<TH ALIGN="CENTER" NOWRAP><I>symbols</I></TH>
+<TH ALIGN="CENTER" NOWRAP><I>longitude</I></TH>
+<TH ALIGN="CENTER" NOWRAP><I>latitude</I></TH>
+<TH ALIGN="CENTER" NOWRAP><I>x-y plane</I></TH>
+<TH ALIGN="CENTER" NOWRAP><I>long. zero</I></TH>
+<TH ALIGN="CENTER" NOWRAP><I>RH/LH</I></TH>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP>horizon</TD>
+<TD ALIGN="CENTER" NOWRAP>-</TD>
+<TD ALIGN="CENTER" NOWRAP>azimuth</TD>
+<TD ALIGN="CENTER" NOWRAP>elevation</TD>
+<TD ALIGN="CENTER" NOWRAP>horizontal</TD>
+<TD ALIGN="CENTER" NOWRAP>north</TD>
+<TD ALIGN="CENTER" NOWRAP>L</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP>equatorial</TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img91.gif"
+ ALT="$\alpha,\delta$"></TD>
+<TD ALIGN="CENTER" NOWRAP>R.A.</TD>
+<TD ALIGN="CENTER" NOWRAP>Dec.</TD>
+<TD ALIGN="CENTER" NOWRAP>equator</TD>
+<TD ALIGN="CENTER" NOWRAP>equinox</TD>
+<TD ALIGN="CENTER" NOWRAP>R</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP>local equ.</TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="27" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img65.gif"
+ ALT="$h,\delta$"></TD>
+<TD ALIGN="CENTER" NOWRAP>H.A.</TD>
+<TD ALIGN="CENTER" NOWRAP>Dec.</TD>
+<TD ALIGN="CENTER" NOWRAP>equator</TD>
+<TD ALIGN="CENTER" NOWRAP>meridian</TD>
+<TD ALIGN="CENTER" NOWRAP>L</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP>ecliptic</TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="29" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img253.gif"
+ ALT="$\lambda,\beta$"></TD>
+<TD ALIGN="CENTER" NOWRAP>ecl. long.</TD>
+<TD ALIGN="CENTER" NOWRAP>ecl. lat.</TD>
+<TD ALIGN="CENTER" NOWRAP>ecliptic</TD>
+<TD ALIGN="CENTER" NOWRAP>equinox</TD>
+<TD ALIGN="CENTER" NOWRAP>R</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP>galactic</TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="45" HEIGHT="32" ALIGN="MIDDLE" BORDER="0"
+ SRC="img254.gif"
+ ALT="$l^{I\!I},b^{I\!I}$"></TD>
+<TD ALIGN="CENTER" NOWRAP>gal. long.</TD>
+<TD ALIGN="CENTER" NOWRAP>gal. lat.</TD>
+<TD ALIGN="CENTER" NOWRAP>gal. equator</TD>
+<TD ALIGN="CENTER" NOWRAP>gal. centre</TD>
+<TD ALIGN="CENTER" NOWRAP>R</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT" NOWRAP>supergalactic</TD>
+<TD ALIGN="CENTER" NOWRAP>SGL,SGB</TD>
+<TD ALIGN="CENTER" NOWRAP>SG long.</TD>
+<TD ALIGN="CENTER" NOWRAP>SG lat.</TD>
+<TD ALIGN="CENTER" NOWRAP>SG equator</TD>
+<TD ALIGN="CENTER" NOWRAP>node w. gal. equ.</TD>
+<TD ALIGN="CENTER" NOWRAP>R</TD>
+</TR>
+</TABLE></DIV>
+Transformations between <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$"> and <IMG WIDTH="66" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img28.gif"
+ ALT="$[\,Az,El~]$"> can be performed by
+calling
+sla_E2H
+and
+sla_H2E,
+or, in double precision,
+sla_DE2H
+and
+sla_DH2E.
+There is also a routine for obtaining
+zenith distance alone for a given <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$">,sla_ZD,
+and one for determining the parallactic angle,
+sla_PA.
+Three routines are included which relate to altazimuth telescope
+mountings.  For a given <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$"> and latitude,
+sla_ALTAZ
+returns the azimuth, elevation and parallactic angle, plus
+velocities and accelerations for sidereal tracking.
+The routines
+sla_PDA2H
+and
+sla_PDQ2H
+predict at what hour angle a given azimuth or
+parallactic angle will be reached.
+<P>
+The routines
+sla_EQECL
+and
+sla_ECLEQ
+transform between ecliptic
+coordinates and <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">; there is also a routine for generating the
+equatorial to ecliptic rotation matrix for a given date:
+sla_ECMAT.
+<P>
+For conversion between Galactic coordinates and <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> there are
+two sets of routines, depending on whether the <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> is
+old-style, B1950, or new-style, J2000;
+sla_EG50
+and
+sla_GE50
+are <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> to <IMG WIDTH="59" HEIGHT="32" ALIGN="MIDDLE" BORDER="0"
+ SRC="img98.gif"
+ ALT="$[\,l^{I\!I},b^{I\!I}\,]$"> and <I>vice versa</I> for the B1950 case, while
+sla_EQGAL
+and
+sla_GALEQ
+are the J2000 equivalents.
+<P>
+Finally, the routines
+sla_GALSUP
+and
+sla_SUPGAL
+transform <IMG WIDTH="59" HEIGHT="32" ALIGN="MIDDLE" BORDER="0"
+ SRC="img98.gif"
+ ALT="$[\,l^{I\!I},b^{I\!I}\,]$"> to de&nbsp;Vaucouleurs supergalactic longitude and latitude
+and <I>vice versa.</I>
+<P>
+It should be appreciated that the table, above, constitutes
+a gross oversimplification.   Apparently
+simple concepts such as equator, equinox <I>etc.</I> are apt to be very hard to
+pin down precisely (polar motion, orbital perturbations ...) and
+some have several interpretations, all subtly different.  The various
+frames move in complicated ways with respect to one another or to
+the stars (themselves in motion).  And in some instances the
+coordinate system is slightly distorted, so that the
+ordinary rules of spherical trigonometry no longer strictly apply.
+<P>
+These <I>caveats</I>
+apply particularly to the bewildering variety of different
+<IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> systems that are in use.  Figure&nbsp;1 shows how
+some of these systems are related, to one another and
+to the direction in which a celestial source actually
+appears in the sky.  At the top of the diagram are
+the various sorts of <I>mean place</I>
+found in star catalogues and papers;<A NAME="tex2html3" HREF="footnode.html#27724"><SUP><IMG  ALIGN="BOTTOM" BORDER="1" ALT="[*]" SRC="foot_motif.gif"></SUP></A> at the bottom is the
+<I>observed</I> <IMG WIDTH="66" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img28.gif"
+ ALT="$[\,Az,El~]$">, where a perfect theodolite would
+be pointed to see the source;  and in the body of
+the diagram are
+the intermediate processing steps and coordinate
+systems.  To help
+understand this diagram, and the SLALIB routines that can
+be used to carry out the various calculations, we will look at the coordinate
+systems involved, and the astronomical phenomena that
+affect them.
+<P>
+<BR>
+<DIV ALIGN="CENTER"><A NAME="27722">&#160;</A>
+<TABLE>
+<CAPTION><STRONG>Figure 1:</STRONG>
+Relationship Between Celestial Coordinates</CAPTION>
+<TR><TD><IMG WIDTH="450" HEIGHT="642"
+ SRC="img255.gif"
+ ALT="\begin{figure}
+\begin{center}
+\begin{tabular}
+{\vert cccccc\vert} \hline
+& & & &...
+ ...2000, all of the precession and E-terms corrections
+are superfluous.\end{figure}"></TD></TR>
+</TABLE>
+</DIV>
+<BR>
+<BR> <HR>
+<A NAME="tex2html2472" HREF="node203.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2473" HREF="node203.html">Precession and Nutation</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2471" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2465" HREF="node201.html">Using vectors</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node203.html b/src/slalib/sun67.htx/node203.html
new file mode 100644
index 0000000..fd18b48
--- /dev/null
+++ b/src/slalib/sun67.htx/node203.html
@@ -0,0 +1,187 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
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+<BR>
+<B> Previous:</B> <A NAME="tex2html2475" HREF="node202.html">Celestial Coordinate Systems</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION00054000000000000000">
+Precession and Nutation</A>
+</H2>
+<I>Right ascension and declination</I>, (<IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">), are the names
+of the longitude and latitude in a spherical
+polar coordinate system based on the Earth's axis of rotation.
+The zero point of <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> is the point of intersection of
+the <I>celestial
+equator</I> and the <I>ecliptic</I> (the apparent path of the Sun
+through the year) where the Sun moves into the northern
+hemisphere.  This point is called the
+<I>first point of Aries</I>,
+the <I>vernal equinox</I> (with apologies to
+southern-hemisphere readers) or simply the <I>equinox</I>.<A NAME="tex2html4" HREF="footnode.html#27833"><SUP><IMG  ALIGN="BOTTOM" BORDER="1" ALT="[*]" SRC="foot_motif.gif"></SUP></A>
+<P>
+This simple picture is unfortunately
+complicated by the difficulty of defining
+a suitable equator and equinox.  One problem is that the
+Sun's apparent motion is not completely regular, due to the
+ellipticity of the Earth's orbit and its continuous disturbance
+by the Moon and planets.  This is dealt with by
+separating the motion into (i)&nbsp;a smooth and steady <I>mean Sun</I>
+and (ii)&nbsp;a set of periodic corrections and perturbations; only the former
+is involved in establishing reference frames and timescales.
+A second, far larger problem, is that
+the celestial equator and the ecliptic
+are both moving with respect to the stars.
+These motions arise because of the gravitational
+interactions between the Earth and the other solar-system bodies.
+<P>
+By far the largest effect is the
+so-called ``precession of the equinoxes'', where the Earth's
+rotation axis sweeps out a cone centred on the ecliptic
+pole, completing one revolution in about 26,000 years.  The
+cause of the motion is the torque exerted on the distorted and
+spinning Earth by the Sun and the Moon.  Consider the effect of the
+Sun alone, at or near the northern summer solstice.  The Sun
+`sees' the top (north pole) of the Earth tilted towards it
+(by about <IMG WIDTH="33" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img256.gif"
+ ALT="$23^{\circ}
+ \hspace{-0.37em}.\hspace{0.02em}5$">, the <I>obliquity of the
+ecliptic</I>),
+and sees the nearer part of the Earth's equatorial bulge
+below centre and the further part above centre.
+Although the Earth is in free fall,
+the gravitational force on the nearer part of the
+equatorial bulge is greater than that on the further part, and
+so there is a net torque acting
+as if to eliminate the tilt.  Six months later the same thing
+is happening in reverse, except that the torque is still
+trying to eliminate the tilt.  In between (at the equinoxes) the
+torque shrinks to zero.  A torque acting on a spinning body
+is gyroscopically translated
+into a precessional motion of the spin axis at right-angles to the torque,
+and this happens to the Earth.
+The motion varies during the
+year, going through two maxima, but always acts in the
+same direction.  The Moon produces the same effect,
+adding a contribution to the precession which peaks twice
+per month.  The Moon's proximity to the Earth more than compensates
+for its smaller mass and gravitational attraction, so that it
+in fact contributes most of the precessional effect.
+<P>
+The complex interactions between the three bodies produce a
+precessional motion that is wobbly rather than completely smooth.
+However, the main 26,000-year component is on such a grand scale that
+it dwarfs the remaining terms, the biggest of
+which has an amplitude of only <IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img133.gif"
+ ALT="$17\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> and a period of
+about 18.6&nbsp;years.  This difference of scale makes it convenient to treat
+these two components of the motion separately.  The main 26,000-year
+effect is called <I>luni-solar precession</I>;  the smaller,
+faster, periodic terms are called the <I>nutation</I>.
+<P>
+Note that precession and nutation are simply
+different frequency components of the same physical effect.  It is
+a common misconception that precession is caused
+by the Sun and nutation is caused by the Moon.  In fact
+the Moon is responsible for two-thirds of the precession, and,
+while it is true that much of the complex detail of the nutation is
+a reflection of the intricacies of the lunar orbit, there are
+nonetheless important solar terms in the nutation.
+<P>
+In addition to and quite separate
+from the precession/nutation effect, the orbit of the Earth-Moon system
+is not fixed in orientation, a result of the attractions of the
+planets.  This slow (about 
+      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img83.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.5$">   &nbsp;per&nbsp;year)
+secular rotation of the ecliptic about a slowly-moving diameter is called,
+confusingly, <I>planetary
+precession</I> and, along with the luni-solar precession is
+included in the <I>general precession</I>.  The equator and
+ecliptic as affected by general precession
+are what define the various ``mean'' <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> reference frames.
+<P>
+The models for precession and nutation come from a combination
+of observation and theory, and are subject to continuous
+refinement.  Nutation models in particular have reached a high
+degree of sophistication, taking into account such things as
+the non-rigidity of the Earth and the effects of
+the planets; SLALIB's nutation
+model (IAU&nbsp;1980) involves 106 terms in each of <IMG WIDTH="14" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img105.gif"
+ ALT="$\psi$"> (longitude)
+and <IMG WIDTH="9" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img257.gif"
+ ALT="$\epsilon$"> (obliquity), some as small as 
+      <IMG WIDTH="47" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img258.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.0001$">   .
+<P>
+<BR><HR>
+<!--Table of Child-Links-->
+<A NAME="CHILD_LINKS">&#160;</A>
+<UL>
+<LI><A NAME="tex2html2484" HREF="node204.html#SECTION00054100000000000000">
+SLALIB support for precession and nutation</A>
+</UL>
+<!--End of Table of Child-Links-->
+<BR> <HR>
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+ SRC="contents_motif.gif"></A>
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+<B> Next:</B> <A NAME="tex2html2483" HREF="node204.html">SLALIB support for precession and nutation</A>
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+<BR>
+<B> Previous:</B> <A NAME="tex2html2475" HREF="node202.html">Celestial Coordinate Systems</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node204.html b/src/slalib/sun67.htx/node204.html
new file mode 100644
index 0000000..cc880e2
--- /dev/null
+++ b/src/slalib/sun67.htx/node204.html
@@ -0,0 +1,127 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLALIB support for precession and nutation</TITLE>
+<META NAME="description" CONTENT="SLALIB support for precession and nutation">
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+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H3><A NAME="SECTION00054100000000000000">
+SLALIB support for precession and nutation</A>
+</H3>
+SLALIB offers a choice of three precession models:
+<UL>
+<LI> The old Bessel-Newcomb, pre IAU&nbsp;1976, ``FK4'' model, used for B1950
+      star positions and other pre-1984.0 purposes
+(sla_PREBN).
+<LI> The new Fricke, IAU&nbsp;1976, ``FK5'' model, used for J2000 star
+      positions and other post-1984.0 purposes
+(sla_PREC).
+<LI> A model published by Simon <I>et al.</I> which is more accurate than
+      the IAU&nbsp;1976 model and which is suitable for long
+      periods of time
+(sla_PRECL).
+</UL>
+In each case, the named SLALIB routine generates the <IMG WIDTH="51" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img259.gif"
+ ALT="$(3\times3)$"><I>precession
+matrix</I> for a given start and finish time.  For example,
+here is the Fortran code for generating the rotation
+matrix which describes the precession between the epochs
+J2000 and J1985.372 (IAU 1976 model):
+<P><PRE>
+            DOUBLE PRECISION PMAT(3,3)
+             :
+            CALL sla_PREC(2000D0,1985.372D0,PMAT)
+</PRE>
+<P>
+It is instructive to examine the resulting matrix:
+<P><PRE>
+            +0.9999936402  +0.0032709208  +0.0014214694
+            -0.0032709208  +0.9999946505  -0.0000023247
+            -0.0014214694  -0.0000023248  +0.9999989897
+</PRE>
+<P>
+Note that the diagonal elements are close to unity, and the
+other elements are small.  This shows that over an interval as
+short as 15&nbsp;years the precession isn't going to move a
+position vector very far (in this case about <IMG WIDTH="25" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img260.gif"
+ ALT="$0^{\circ}
+ \hspace{-0.37em}.\hspace{0.02em}2$">).
+<P>
+For convenience, a direct <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> to <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> precession routine is
+also provided
+(sla_PRECES),
+suitable for either the old or the new system (but not a
+mixture of the two).
+<P>
+SLALIB provides only one nutation model, the new, IAU&nbsp;1980 model,
+implemented in the routine
+sla_NUTC.
+This returns the components of nutation
+in longitude and latitude (and also provides the obliquity) from
+which a nutation matrix can be generated by calling
+sla_DEULER
+(and from which the <I>equation of the equinoxes</I>, described
+later, can be found).  Alternatively,
+the nutation matrix can be generated in a single call by using
+sla_NUT.
+<P>
+A rotation matrix for applying the entire precession/nutation
+transformation in one go can be generated by calling
+sla_PRENUT.
+<P>
+<BR> <HR>
+<A NAME="tex2html2491" HREF="node205.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2492" HREF="node205.html">Mean Places</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2490" HREF="node203.html">Precession and Nutation</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2486" HREF="node203.html">Precession and Nutation</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node205.html b/src/slalib/sun67.htx/node205.html
new file mode 100644
index 0000000..6da5021
--- /dev/null
+++ b/src/slalib/sun67.htx/node205.html
@@ -0,0 +1,92 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Mean Places</TITLE>
+<META NAME="description" CONTENT="Mean Places">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node206.html">
+<LINK REL="previous" HREF="node203.html">
+<LINK REL="up" HREF="node197.html">
+<LINK REL="next" HREF="node206.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html2501" HREF="node206.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2499" HREF="node197.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2493" HREF="node204.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2502" HREF="node206.html">Epoch</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2500" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2494" HREF="node204.html">SLALIB support for precession and nutation</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION00055000000000000000">
+Mean Places</A>
+</H2>
+The main effect of the precession/nutation is a steady increase of about
+<IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img261.gif"
+ ALT="$50\hspace{-0.05em}^{'\hspace{-0.1em}'}$">/year in the ecliptic longitudes of the stars.  It is therefore
+essential, when reporting the position of an astronomical target, to
+qualify the coordinates with a date, or <I>epoch</I>.
+Specifying the epoch ties down the equator and
+equinox which define the <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> coordinate system that is
+being used.
+<A NAME="tex2html5" HREF="footnode.html#27903"><SUP><IMG  ALIGN="BOTTOM" BORDER="1" ALT="[*]" SRC="foot_motif.gif"></SUP></A>  For simplicity, only
+the smooth and steady ``general
+precession'' part of the complete precession/nutation effect is
+included, thereby defining what is called the <I>mean</I>
+equator and equinox for the epoch concerned.  We say a star
+has a mean place of (for example)
+<IMG WIDTH="104" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img262.gif"
+ ALT="$12^{h}\,07^{m}\,58^{s}.09$">&nbsp;<IMG WIDTH="102" HEIGHT="35" ALIGN="MIDDLE" BORDER="0"
+ SRC="img263.gif"
+ ALT="$-19^{\circ}\,44^{'}\,37^{''}.1$"> ``with respect to the mean equator
+and equinox of epoch J2000''.  The short way of saying
+this is ``<IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> equinox J2000'' (<B>not</B> ``<IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> epoch J2000'', 
+which means something different to do with
+proper motion).
+<P>
+<BR> <HR>
+<A NAME="tex2html2501" HREF="node206.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2499" HREF="node197.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2493" HREF="node204.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2502" HREF="node206.html">Epoch</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2500" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2494" HREF="node204.html">SLALIB support for precession and nutation</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node206.html b/src/slalib/sun67.htx/node206.html
new file mode 100644
index 0000000..9a94a3d
--- /dev/null
+++ b/src/slalib/sun67.htx/node206.html
@@ -0,0 +1,125 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Epoch</TITLE>
+<META NAME="description" CONTENT="Epoch">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node207.html">
+<LINK REL="previous" HREF="node205.html">
+<LINK REL="up" HREF="node197.html">
+<LINK REL="next" HREF="node207.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html2511" HREF="node207.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2509" HREF="node197.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2503" HREF="node205.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2512" HREF="node207.html">Proper Motion</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2510" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2504" HREF="node205.html">Mean Places</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION00056000000000000000">
+Epoch</A>
+</H2>
+The word ``epoch'' just means a moment in time, and can be supplied
+in a variety of forms, using different calendar systems and timescales.
+<P>
+For the purpose of specifying the epochs associated with the
+mean place of a star, two conventions exist.  Both sorts of epoch
+superficially resemble years AD but are not tied to the civil
+(Gregorian) calendar;  to distinguish them from ordinary calendar-years
+there is often
+a ``.0'' suffix (as in ``1950.0''), although any other fractional
+part is perfectly legal (<I>e.g.</I> 1987.5).
+<P>
+The older system,
+<I>Besselian epoch</I>, is defined in such a way that its units are
+tropical years of about 365.2422&nbsp;days and its timescale is the
+obsolete <I>Ephemeris Time</I>.
+The start of the Besselian year is the moment
+when the ecliptic longitude of the mean Sun is
+<IMG WIDTH="34" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img167.gif"
+ ALT="$280^\circ$">;  this happens near the start of the
+calendar year (which is why <IMG WIDTH="34" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img167.gif"
+ ALT="$280^\circ$"> was chosen).
+<P>
+The new system, <I>Julian epoch</I>, was adopted as
+part of the IAU&nbsp;1976 revisions (about which more will be said
+in due course) and came formally into use at the
+beginning of 1984.  It uses the Julian year of exactly
+365.25&nbsp;days; Julian epoch 2000 is defined to be 2000&nbsp;January&nbsp;1.5 in the
+TT timescale.
+<P>
+For specifying mean places, various standard epochs are in use, the
+most common ones being Besselian epoch 1950.0 and Julian epoch 2000.0.
+To distinguish the two systems, Besselian epochs
+are now prefixed ``B'' and Julian epochs are prefixed ``J''.
+Epochs without an initial letter can be assumed to be Besselian
+if before 1984.0, otherwise Julian.  These details are supported by
+the SLALIB routines
+sla_DBJIN
+(decodes numbers from a
+character string, accepting an optional leading B or J),
+sla_KBJ
+(decides whether B or J depending on prefix or range) and
+sla_EPCO
+(converts one epoch to match another).
+<P>
+SLALIB has four routines for converting
+Besselian and Julian epochs into other forms.
+The functions
+sla_EPB2D
+and
+sla_EPJ2D
+convert Besselian and Julian epochs into MJD; the functions
+sla_EPB
+and
+sla_EPJ
+do the reverse.  For example, to express B1950 as a Julian epoch:
+<P><PRE>
+            DOUBLE PRECISION sla_EPJ,sla_EPB2D
+             :
+            WRITE (*,'(1X,''J'',F10.5)') sla_EPJ(sla_EPB2D(1950D0))
+</PRE>
+<P>(The answer is J1949.99979.)
+<P>
+<BR> <HR>
+<A NAME="tex2html2511" HREF="node207.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2509" HREF="node197.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2503" HREF="node205.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2512" HREF="node207.html">Proper Motion</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2510" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2504" HREF="node205.html">Mean Places</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node207.html b/src/slalib/sun67.htx/node207.html
new file mode 100644
index 0000000..6c74c4e
--- /dev/null
+++ b/src/slalib/sun67.htx/node207.html
@@ -0,0 +1,119 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Proper Motion</TITLE>
+<META NAME="description" CONTENT="Proper Motion">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node208.html">
+<LINK REL="previous" HREF="node206.html">
+<LINK REL="up" HREF="node197.html">
+<LINK REL="next" HREF="node208.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html2521" HREF="node208.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2519" HREF="node197.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2513" HREF="node206.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2522" HREF="node208.html">Parallax and Radial Velocity</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2520" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2514" HREF="node206.html">Epoch</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION00057000000000000000">
+Proper Motion</A>
+</H2>
+Stars in catalogues usually have, in addition to the 
+<IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">  coordinates, a <I>proper motion</I> <IMG WIDTH="54" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img264.gif"
+ ALT="$[\mu_\alpha,\mu_\delta]$">.This is an intrinsic motion
+of the star across the background.  Very few stars have a
+proper motion which exceeds <IMG WIDTH="17" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img140.gif"
+ ALT="$1\hspace{-0.05em}^{'\hspace{-0.1em}'}$">/year, and most are
+far below this level.  A star observed as part of normal
+astronomy research will, as a rule, have a proper motion
+which is unknown.
+<P>
+Mean <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> and rate of change are not sufficient to pin
+down a star;  the epoch at which the <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> was or will
+be correct is also needed.  Note the distinction
+between the epoch which specifies the
+coordinate system and the epoch at which the star passed
+through the given <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">.  The full specification for a star
+is <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">, proper motions, equinox and epoch (plus something to
+identify which set of models for the precession <I>etc.</I> is 
+being used - see the next section).
+For convenience, coordinates given in star catalogues are almost
+always adjusted to make the equinox and epoch the same - for
+example B1950 in the case of the SAO&nbsp;catalogue.
+<P>
+SLALIB provides one routine to handle proper motion on its own,
+sla_PM.
+Proper motion is also allowed for in various other
+routines as appropriate, for example
+sla_MAP
+and
+sla_FK425.
+Note that in all SLALIB routines which involve proper motion
+the units are radians per year and the
+<IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> component is in the form <IMG WIDTH="13" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img115.gif"
+ ALT="$\dot{\alpha}$"> (<I>i.e.</I> big
+numbers near the poles).
+Some star catalogues have proper motion per century, and
+in some catalogues the <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> component is in the form
+<IMG WIDTH="48" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img116.gif"
+ ALT="$\dot{\alpha}\cos\delta$"> (<I>i.e.</I> angle on the sky).
+<P>
+<BR> <HR>
+<A NAME="tex2html2521" HREF="node208.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2519" HREF="node197.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2513" HREF="node206.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2522" HREF="node208.html">Parallax and Radial Velocity</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2520" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2514" HREF="node206.html">Epoch</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node208.html b/src/slalib/sun67.htx/node208.html
new file mode 100644
index 0000000..cc2b337
--- /dev/null
+++ b/src/slalib/sun67.htx/node208.html
@@ -0,0 +1,92 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Parallax and Radial Velocity</TITLE>
+<META NAME="description" CONTENT="Parallax and Radial Velocity">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node209.html">
+<LINK REL="previous" HREF="node207.html">
+<LINK REL="up" HREF="node197.html">
+<LINK REL="next" HREF="node209.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html2531" HREF="node209.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2529" HREF="node197.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2523" HREF="node207.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2532" HREF="node209.html">Aberration</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2530" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2524" HREF="node207.html">Proper Motion</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION00058000000000000000">
+Parallax and Radial Velocity</A>
+</H2>
+For the utmost accuracy and the nearest stars, allowance can
+be made for <I>annual parallax</I> and for the effects of perspective
+on the proper motion.
+<P>
+Parallax is appreciable only for nearby stars;  even
+the nearest, Proxima Centauri, is displaced from its average
+position by less than
+an arcsecond as the Earth revolves in its orbit.
+<P>
+For stars with a known parallax, knowledge of the radial velocity
+allows the proper motion to be expressed as an actual space
+motion in 3&nbsp;dimensions.  The proper motion is,
+in fact, a snapshot of the transverse component of the
+space motion, and in the case of nearby stars will
+change with time due to perspective.
+<P>
+SLALIB does not provide facilities for handling parallax
+and radial-velocity on their own, but their contribution is
+allowed for in such routines as
+sla_PM,
+sla_MAP
+and
+sla_FK425.
+Catalogue mean
+places do not include the effects of parallax and are therefore
+<I>barycentric</I>;  when pointing telescopes <I>etc.</I> it is 
+usually most efficient to apply the slowly-changing
+parallax correction to the mean place of the target early on
+and to work with the <I>geocentric</I> mean place.  This latter
+approach is implied in Figure&nbsp;1.
+<P>
+<BR> <HR>
+<A NAME="tex2html2531" HREF="node209.html">
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+<B> Next:</B> <A NAME="tex2html2532" HREF="node209.html">Aberration</A>
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+<BR>
+<B> Previous:</B> <A NAME="tex2html2524" HREF="node207.html">Proper Motion</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node209.html b/src/slalib/sun67.htx/node209.html
new file mode 100644
index 0000000..4790dda
--- /dev/null
+++ b/src/slalib/sun67.htx/node209.html
@@ -0,0 +1,147 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Aberration</TITLE>
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+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION00059000000000000000">
+Aberration</A>
+</H2>
+The finite speed of light combined with the motion of the observer
+around the Sun during the year causes apparent displacements of
+the positions of the stars.  The effect is called
+the <I>annual aberration</I> (or ``stellar''
+aberration).  Its maximum size, about 
+      <IMG WIDTH="31" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img265.gif"
+ ALT="$20\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.5$">   ,
+occurs for stars <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img22.gif"
+ ALT="$90^{\circ}$"> from the point towards which
+the Earth is headed as it orbits the Sun;  a star exactly in line with
+the Earth's motion is not displaced.  To receive the light of
+a star, the telescope has to be offset slightly in the direction of
+the Earth's motion.  A familiar analogy is the need to tilt your
+umbrella forward when on the move, to avoid getting wet.  This
+Newtonian model is,
+in fact, highly misleading in the context of light as opposed
+to rain, but happens to give the same answer as a relativistic
+treatment to first order (better than 1&nbsp;milliarcsecond).
+<P>
+Before the IAU 1976 resolutions, different
+values for the approximately
+<P>      <IMG WIDTH="31" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img265.gif"
+ ALT="$20\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.5$">    <I>aberration constant</I> were employed
+at different times, and this can complicate comparisons
+between different catalogues.  Another complication comes from
+the so-called <I>E-terms of aberration</I>,
+that small part of the annual aberration correction that is a
+function of the eccentricity of the Earth's orbit.  The E-terms,
+maximum amplitude about 
+      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img32.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.3$">   ,
+happen to be approximately constant for a given star, and so they
+used to be incorporated in the catalogue <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">to reduce the labour of converting to and from apparent place.
+The E-terms can be removed from a catalogue <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> by
+calling
+sla_SUBET
+or applied (for example to allow a pulsar
+timing-position to be plotted on a B1950 finding chart)
+by calling
+sla_ADDET;
+the E-terms vector itself can be obtained by calling
+sla_ETRMS.
+Star positions post IAU 1976 are free of these distortions, and to
+apply corrections for annual aberration involves the actual
+barycentric velocity of the Earth rather than the use of
+canonical circular-orbit models.
+<P>
+The annual aberration is the aberration correction for
+an imaginary observer at the Earth's centre.
+The motion of a real observer around the Earth's rotation axis in
+the course of the day makes a small extra contribution to the total
+aberration effect called the <I>diurnal aberration</I>.  Its
+maximum amplitude is about 
+      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img76.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.2$">   .
+<P>
+No SLALIB routine is provided for calculating the aberration on
+its own, though the required velocity vectors can be
+generated using
+sla_EVP
+and
+sla_GEOC.
+Annual and diurnal aberration are allowed for where required, for example in
+sla_MAP
+<I>etc</I>. and
+sla_AOP
+<I>etc</I>.  Note that this sort
+of aberration is different from the <I>planetary
+aberration</I>, which is the apparent displacement of a solar-system
+body, with respect to the ephemeris position, as a consequence
+of the motion of <I>both</I> the Earth and the source.  The
+planetary aberration can be computed either by correcting the
+position of the solar-system body for light-time, followed by
+the ordinary stellar aberration correction, or more
+directly by expressing the position and velocity of the source
+in the observer's frame and correcting for light-time alone.
+<P>
+<BR> <HR>
+<A NAME="tex2html2541" HREF="node210.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
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+<B> Next:</B> <A NAME="tex2html2542" HREF="node210.html">Different Sorts of Mean Place</A>
+<BR>
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+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node21.html b/src/slalib/sun67.htx/node21.html
new file mode 100644
index 0000000..13ef3e2
--- /dev/null
+++ b/src/slalib/sun67.htx/node21.html
@@ -0,0 +1,264 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
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+<TITLE>SLA_AOPPA - Appt-to-Obs Parameters</TITLE>
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+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION00048000000000000000">SLA_AOPPA - Appt-to-Obs Parameters</A>
+<A NAME="xref_SLA_AOPPA">&#160;</A><A NAME="SLA_AOPPA">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Pre-compute the set of apparent to observed place parameters
+required by the ``quick'' routines sla_AOPQK and sla_OAPQK.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_AOPPA (
+          DATE, DUT, ELONGM, PHIM, HM, XP, YP,
+          TDK, PMB, RH, WL, TLR, AOPRMS)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>UTC date/time (Modified Julian Date, JD-2400000.5)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DUT</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">UT:  UT1-UTC (UTC seconds)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ELONGM</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>observer's mean longitude (radians, east +ve)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PHIM</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>observer's mean geodetic latitude (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>HM</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>observer's height above sea level (metres)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>XP,YP</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>polar motion <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> coordinates (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>TDK</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>local ambient temperature (degrees K; std=273.155D0)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PMB</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>local atmospheric pressure (mB; std=1013.25D0)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>local relative humidity (in the range 0D0-1D0)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>WL</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>effective wavelength (<IMG WIDTH="26" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img21.gif"
+ ALT="$\mu{\rm m}$">, <I>e.g.</I> 0.55D0)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>TLR</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>tropospheric lapse rate (degrees K per metre,
+<I>e.g.</I> 0.0065D0)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AOPRMS</EM></TD>
+<TH ALIGN="LEFT"><B>D(14)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>star-independent apparent-to-observed parameters:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(1)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>geodetic latitude (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(2,3)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>sine and cosine of geodetic latitude</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(4)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>magnitude of diurnal aberration vector</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(5)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>height (HM)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(6)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>ambient temperature (TDK)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(7)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>pressure (PMB)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(8)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>relative humidity (RH)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(9)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>wavelength (WL)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(10)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>lapse rate (TLR)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(11,12)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>refraction constants A and B (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(13)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>longitude + eqn of equinoxes +
+``sidereal <IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">UT'' (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(14)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>local apparent sidereal time (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>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.
+  <DT>2.
+<DD>The DATE argument is UTC expressed as an MJD.  This is,
+        strictly speaking, wrong, because of leap seconds.  However,
+        as long as the <IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">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 <IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">UT should
+        continue to be used.  As the 61st second completes, the MJD
+        should revert to the start of the day as, simultaneously,
+        the <IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">UT changes by one second to its post-leap new value.
+  <DT>3.
+<DD>The <IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">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 <IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">UT
+        within <IMG WIDTH="15" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img30.gif"
+ ALT="$\pm$"><IMG WIDTH="24" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img31.gif"
+ ALT="$0^{\rm s}\hspace{-0.3em}.9$">.  The ``sidereal <IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">UT'' which forms
+        part of AOPRMS(13) is the same quantity, but converted from solar
+        to sidereal seconds and expressed in radians.
+  <DT>4.
+<DD>IMPORTANT - TAKE CARE WITH THE LONGITUDE SIGN CONVENTION.  The
+        longitude required by the present routine is <B>east-positive</B>,
+        in accordance with geographical convention (and right-handed).
+        In particular, note that the longitudes returned by the
+        sla_OBS routine are west-positive (as in the <I>Astronomical
+        Almanac</I> before 1984) and must be reversed in sign before use in
+        the present routine.
+  <DT>5.
+<DD>The polar coordinates XP,YP can be obtained from IERS
+        circulars and equivalent publications.  The
+        maximum amplitude is about 
+      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img32.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.3$">   .  If XP,YP values
+        are unavailable, use XP=YP=0D0.  See page B60 of the 1988
+        <I>Astronomical Almanac</I> for a definition of the two angles.
+  <DT>6.
+<DD>The height above sea level of the observing station, HM,
+        can be obtained from the <I>Astronomical Almanac</I> (Section J
+        in the 1988 edition), or via the routine sla_OBS.  If P,
+        the pressure in mB, is available, an adequate
+        estimate of HM can be obtained from the following expression:
+        <BLOCKQUOTE><TT>HM=-29.3D0*TSL*LOG(P/1013.25D0)</TT>
+        </BLOCKQUOTE>
+        where TSL is the approximate sea-level air temperature in degrees K
+        (see <I>Astrophysical Quantities</I>, C.W.Allen, 3rd&nbsp;edition,
+        &#167;52).  Similarly, if the pressure P is not known,
+        it can be estimated from the height of the observing
+        station, HM as follows:
+        <BLOCKQUOTE><TT>P=1013.25D0*EXP(-HM/(29.3D0*TSL))</TT>
+        </BLOCKQUOTE>
+        Note, however, that the refraction is proportional to the
+        pressure and that an accurate P value is important for
+        precise work.
+ </DL></DL>
+<BR> <HR>
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+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
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diff --git a/src/slalib/sun67.htx/node210.html b/src/slalib/sun67.htx/node210.html
new file mode 100644
index 0000000..1a8e19e
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+++ b/src/slalib/sun67.htx/node210.html
@@ -0,0 +1,177 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
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+<H2><A NAME="SECTION000510000000000000000">
+Different Sorts of Mean Place</A>
+</H2>
+A particularly confusing aspect of published mean places is that they
+are sensitive to the precise way they were determined.  A mean
+place is not directly observable, even with fundamental
+instruments such as transit circles, and to produce a mean
+place will involve relying on some existing star catalogue,
+for example the fundamental catalogues FK4 and FK5,
+and applying given mathematical models of precession, nutation,
+aberration and so on.
+Note in particular that no star catalogue,
+even a fundamental catalogue such as FK4 or
+FK5, defines a coordinate system, strictly speaking;
+it is merely a list of star positions and proper motions.
+However, once the stars from a given catalogue
+are used as position calibrators, <I>e.g.</I> for
+transit-circle observations or for plate reductions, then a
+broader sense of there being a coordinate grid naturally
+arises, and such phrases as ``in the system of
+the FK4'' can legitimately be employed.  However,
+there is no formal link between the
+two concepts - no ``standard least squares fit'' between
+reality and the inevitably flawed catalogues.<A NAME="tex2html6" HREF="footnode.html#28038"><SUP><IMG  ALIGN="BOTTOM" BORDER="1" ALT="[*]" SRC="foot_motif.gif"></SUP></A>  All such
+catalogues suffer at some level from systematic, zonal distortions
+of both the star positions and of the proper motions,
+and include measurement errors peculiar to individual
+stars.
+<P>
+Many of these complications are of little significance except to
+specialists.  However, observational astronomers cannot
+escape exposure to at least the two main varieties of
+mean place, loosely called
+FK4 and FK5, and should be aware of
+certain pitfalls.  For most practical purposes the more recent
+system, FK5, is free of surprises and tolerates naive
+use well.  FK4, in contrast, contains two important traps:
+<UL>
+<LI> The FK4 system rotates at about
+<P>      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img83.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.5$">    per century relative to distant galaxies.
+      This is manifested as a systematic distortion in the
+      proper motions of all FK4-derived catalogues, which will
+      in turn pollute any astrometry done using those catalogues.
+      For example, FK4-based astrometry of a QSO using plates
+      taken decades apart will reveal a non-zero <I>fictitious proper
+      motion</I>, and any FK4 star which happens to have zero proper
+      motion is, in fact, slowly moving against the distant
+      background.  The FK4 frame rotates because it was
+      established before the nature of the Milky Way, and hence the
+      existence of systematic motions of nearby stars, had been
+      recognized.
+<LI> Star positions in the FK4 system are part-corrected for
+      annual aberration (see above) and embody the so-called
+      E-terms of aberration.
+</UL>
+The change from the old FK4-based system to FK5
+occurred at the beginning
+of 1984 as part of a package of resolutions made by the IAU in 1976,
+along with the adoption of J2000 as the reference epoch.  Star
+positions in the newer, FK5, system are free from the E-terms, and
+the system is a much better approximation to an
+inertial frame (about five times better).
+<P>
+It may occasionally be convenient to specify the FK4 fictitious proper
+motion directly.  In FK4, the centennial proper motion of (for example)
+a QSO is:
+<P><IMG WIDTH="56" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img266.gif"
+ ALT="$\mu_\alpha=-$"><IMG WIDTH="65" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img267.gif"
+ ALT="$0^{\rm s}\hspace{-0.3em}.015869$">+((<IMG WIDTH="65" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img268.gif"
+ ALT="$0^{\rm s}\hspace{-0.3em}.029032$"><IMG WIDTH="56" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
+ SRC="img269.gif"
+ ALT="$~\sin \alpha
+ +$"><IMG WIDTH="65" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img270.gif"
+ ALT="$0^{\rm s}\hspace{-0.3em}.000340$"><IMG WIDTH="98" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img271.gif"
+ ALT="$~\cos \alpha ) \sin \delta
+ -$"><IMG WIDTH="65" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img272.gif"
+ ALT="$0^{\rm s}\hspace{-0.3em}.000105$"><IMG WIDTH="58" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img273.gif"
+ ALT="$~\cos \alpha
+ -$"><IMG WIDTH="65" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img274.gif"
+ ALT="$0^{\rm s}\hspace{-0.3em}.000083$"><IMG WIDTH="84" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img275.gif"
+ ALT="$~\sin \alpha ) \sec \delta $"> <BR>
+<IMG WIDTH="56" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img276.gif"
+ ALT="$\mu_\delta\,=+$">      <IMG WIDTH="56" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img277.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.43549$">   <IMG WIDTH="58" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img273.gif"
+ ALT="$~\cos \alpha
+ -$">      <IMG WIDTH="56" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img278.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.00510$">   <IMG WIDTH="70" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img279.gif"
+ ALT="$~\sin \alpha +
+ ($">      <IMG WIDTH="56" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img280.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.00158$">   <IMG WIDTH="56" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
+ SRC="img281.gif"
+ ALT="$~\sin \alpha
+ -$">      <IMG WIDTH="56" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img282.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.00125$">   <IMG WIDTH="98" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img271.gif"
+ ALT="$~\cos \alpha ) \sin \delta
+ -$">      <IMG WIDTH="56" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img283.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.00066$">   <IMG WIDTH="43" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img284.gif"
+ ALT="$~\cos \delta $">
+<BR> <HR>
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+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node211.html b/src/slalib/sun67.htx/node211.html
new file mode 100644
index 0000000..2a8cbee
--- /dev/null
+++ b/src/slalib/sun67.htx/node211.html
@@ -0,0 +1,232 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Mean Place Transformations</TITLE>
+<META NAME="description" CONTENT="Mean Place Transformations">
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+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000511000000000000000">
+Mean Place Transformations</A>
+</H2>
+Figure&nbsp;1 is based upon three varieties of mean <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> all of which are
+of practical significance to observing astronomers in the present era:
+<UL>
+<LI> Old style (FK4) with known proper motion in the FK4
+         system, and with parallax and radial velocity either
+         known or assumed zero.
+<LI> Old style (FK4) with zero proper motion in FK5,
+         and with parallax and radial velocity assumed zero.
+<LI> New style (FK5) with proper motion, parallax and
+         radial velocity either known or assumed zero.
+</UL>
+The figure outlines the steps required to convert positions in
+any of these systems to a J2000 <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> for the current
+epoch, as might be required in a telescope-control
+program for example.
+Most of the steps can be carried out by calling a single
+SLALIB routines;  there are other SLALIB routines which
+offer set-piece end-to-end transformation routines for common cases.
+Note, however, that SLALIB does not set out to provide the capability
+for arbitrary transformations of star-catalogue data
+between all possible systems of mean <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">.Only in the (common) cases of FK4, equinox and epoch B1950,
+to FK5, equinox and epoch J2000, and <I>vice versa</I> are
+proper motion, parallax and radial velocity transformed
+along with the star position itself, the
+focus of SLALIB support.
+<P>
+As an example of using SLALIB to transform mean places, here is
+a program which implements the top-left path of Figure&nbsp;1.
+An FK4 <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> of arbitrary equinox and epoch and with
+known proper motion and
+parallax is transformed into an FK5 J2000 <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> for the current
+epoch.  As a test star we will use <IMG WIDTH="30" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img285.gif"
+ ALT="$\alpha=$"><IMG WIDTH="104" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img286.gif"
+ ALT="$16^{h}\,09^{m}\,55^{s}.13$">,<IMG WIDTH="28" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img287.gif"
+ ALT="$\delta=$"><IMG WIDTH="102" HEIGHT="35" ALIGN="MIDDLE" BORDER="0"
+ SRC="img288.gif"
+ ALT="$-75^{\circ}\,59^{'}\,27^{''}.2$">, equinox 1900, epoch 1963.087,
+<IMG WIDTH="38" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img289.gif"
+ ALT="$\mu_\alpha=$"><IMG WIDTH="61" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
+ SRC="img290.gif"
+ ALT="$-0^{\rm s}\hspace{-0.3em}.0312$">/<I>y</I>, <IMG WIDTH="36" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img291.gif"
+ ALT="$\mu_\delta=$">      <IMG WIDTH="52" HEIGHT="35" ALIGN="MIDDLE" BORDER="0"
+ SRC="img292.gif"
+ ALT="$+0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.103$">   /<I>y</I>,
+parallax = 
+      <IMG WIDTH="39" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img293.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.062$">   , radial velocity = -34.22&nbsp;km/s.  The
+epoch of observation is 1994.35.
+<P><PRE>
+            IMPLICIT NONE
+            DOUBLE PRECISION AS2R,S2R
+            PARAMETER (AS2R=4.8481368110953599D-6,S2R=7.2722052166430399D-5)
+            INTEGER J,I
+            DOUBLE PRECISION R0,D0,EQ0,EP0,PR,PD,PX,RV,EP1,R1,D1,R2,D2,R3,D3,
+           :                 R4,D4,R5,D5,R6,D6,EP1D,EP1B,W(3),EB(3),PXR,V(3)
+            DOUBLE PRECISION sla_EPB,sla_EPJ2D
+
+      *  RA, Dec etc of example star
+            CALL sla_DTF2R(16,09,55.13D0,R0,J)
+            CALL sla_DAF2R(75,59,27.2D0,D0,J)
+            D0=-D0
+            EQ0=1900D0
+            EP0=1963.087D0
+            PR=-0.0312D0*S2R
+            PD=+0.103D0*AS2R
+            PX=0.062D0
+            RV=-34.22D0
+            EP1=1994.35D0
+
+      *  Epoch of observation as MJD and Besselian epoch
+            EP1D=sla_EPJ2D(EP1)
+            EP1B=sla_EPB(EP1D)
+
+      *  Space motion to the current epoch
+            CALL sla_PM(R0,D0,PR,PD,PX,RV,EP0,EP1B,R1,D1)
+
+      *  Remove E-terms of aberration for the original equinox
+            CALL sla_SUBET(R1,D1,EQ0,R2,D2)
+
+      *  Precess to B1950
+            R3=R2
+            D3=D2
+            CALL sla_PRECES('FK4',EQ0,1950D0,R3,D3)
+
+      *  Add E-terms for the standard equinox B1950
+            CALL sla_ADDET(R3,D3,1950D0,R4,D4)
+
+      *  Transform to J2000, no proper motion
+            CALL sla_FK45Z(R4,D4,EP1B,R5,D5)
+
+      *  Parallax
+            CALL sla_EVP(sla_EPJ2D(EP1),2000D0,W,EB,W,W)
+            PXR=PX*AS2R
+            CALL sla_DCS2C(R5,D5,V)
+            DO I=1,3
+               V(I)=V(I)-PXR*EB(I)
+            END DO
+            CALL sla_DCC2S(V,R6,D6)
+             :
+</PRE>
+<P>
+It is interesting to look at how the <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> changes during the
+course of the calculation:
+<PRE><TT>
+		 <TT>16 09 55.130 -75 59 27.20</TT> 		 		 <I>original equinox and epoch</I>
+		 <TT>16 09 54.155 -75 59 23.98</TT> 		 		 <I>with space motion</I>
+		 <TT>16 09 54.229 -75 59 24.18</TT> 		 		 <I>with old E-terms removed</I>
+		 <TT>16 16 28.213 -76 06 54.57</TT> 		 		 <I>precessed to 1950.0</I>
+		 <TT>16 16 28.138 -76 06 54.37</TT> 		 		 <I>with new E-terms</I>
+		 <TT>16 23 07.901 -76 13 58.87</TT> 		 		 <I>J2000, current epoch</I>
+		 <TT>16 23 07.907 -76 13 58.92</TT> 		 		 <I>including parallax</I>
+</TT></PRE>
+<P>
+Other remarks about the above (unusually complicated) example:
+<UL>
+<LI> If the original equinox and epoch were B1950, as is quite
+      likely, then it would be unnecessary to treat space motions
+      and E-terms explicitly.  Transformation to FK5 J2000 could
+      be accomplished simply by calling
+sla_FK425, after which
+      a call to
+sla_PM and the parallax code would complete the
+      work.
+<LI> The rigorous treatment of the E-terms
+      has only a small effect on the result.  Such refinements
+      are, nevertheless, worthwhile in order to facilitate comparisons and
+      to increase the chances that star positions from different
+      suppliers are compatible.
+<LI> The FK4 to FK5 transformations,
+sla_FK425
+      and
+sla_FK45Z,
+      are not as is sometimes assumed simply 50 years of precession,
+      though this indeed accounts for most of the change.  The
+      transformations also include adjustments
+      to the equinox, a revised precession model, elimination of the
+      E-terms, a change to the proper-motion time unit and so on.
+      The reason there are two routines rather than just one
+      is that the FK4 frame rotates relative to the background, whereas
+      the FK5 frame is a much better approximation to an
+      inertial frame, and zero proper
+      motion in FK4 does not, therefore, mean zero proper motion in FK5.
+      SLALIB also provides two routines,
+sla_FK524
+      and
+sla_FK54Z,
+      to perform the inverse transformations.
+<LI> Some star catalogues (FK4 itself is one) were constructed using slightly
+      different procedures for the polar regions compared with
+      elsewhere.  SLALIB ignores this inhomogeneity and always
+      applies the standard
+      transformations irrespective of location on the celestial sphere.
+</UL>
+<BR> <HR>
+<A NAME="tex2html2561" HREF="node212.html">
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+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
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+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Mean Place to Apparent Place</TITLE>
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+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000512000000000000000">
+Mean Place to Apparent Place</A>
+</H2>
+The <I>geocentric apparent place</I> of a source, or <I>apparent place</I>
+for short,
+is the <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> if viewed from the centre of the Earth,
+with respect to the true equator and equinox of date.
+Transformation of an FK5 mean <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">, equinox J2000,
+current epoch, to apparent place involves the following effects:
+<P><UL>
+<LI> Light deflection - the gravitational lens effect of
+         the sun.
+<LI> Annual aberration.
+<LI> Precession/nutation.
+</UL>
+The <I>light deflection</I> is seldom significant.  Its value
+at the limb of the Sun is about
+<P>      <IMG WIDTH="31" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img294.gif"
+ ALT="$1\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.74$">   ;  it falls off rapidly with distance from the
+Sun and has shrunk to about
+<P>      <IMG WIDTH="31" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img295.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.02$">    at an elongation of <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img296.gif"
+ ALT="$20^\circ$">.<P>
+As already described, the <I>annual aberration</I>
+is a function of the Earth's velocity
+relative to the solar system barycentre (available through the
+SLALIB routine
+sla_EVP)
+and produces shifts of up to about 
+      <IMG WIDTH="31" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img265.gif"
+ ALT="$20\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.5$">   .
+<P>
+The <I>precession/nutation</I>, from J2000 to the current epoch, is
+expressed by a rotation matrix which is available through the
+SLALIB routine
+sla_PRENUT.
+<P>
+The whole mean-to-apparent transformation can be done using the SLALIB
+routine
+sla_MAP.  As a demonstration, here is a program which lists the
+<I>North Polar Distance</I> (<IMG WIDTH="54" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img297.gif"
+ ALT="$90^\circ-\delta$">) of Polaris for
+the decade of closest approach to the Pole:
+<P><PRE>
+            IMPLICIT NONE
+            DOUBLE PRECISION PI,PIBY2,D2R,S2R,AS2R
+            PARAMETER (PI=3.141592653589793238462643D0)
+            PARAMETER (D2R=PI/180D0,
+           :           PIBY2=PI/2D0,
+           :           S2R=PI/(12D0*3600D0),
+           :           AS2R=PI/(180D0*3600D0))
+            DOUBLE PRECISION RM,DM,PR,PD,DATE,RA,DA
+            INTEGER J,IDS,IDE,ID,IYMDF(4),I
+            DOUBLE PRECISION sla_EPJ2D
+
+            CALL sla_DTF2R(02,31,49.8131D0,RM,J)
+            CALL sla_DAF2R(89,15,50.661D0,DM,J)
+            PR=+21.7272D0*S2R/100D0
+            PD=-1.571D0*AS2R/100D0
+            WRITE (*,'(1X,'//
+           :            '''Polaris north polar distance (deg) 2096-2105''/)')
+            WRITE (*,'(4X,''Date'',7X''NPD''/)')
+            CALL sla_CLDJ(2096,1,1,DATE,J)
+            IDS=NINT(DATE)
+            CALL sla_CLDJ(2105,12,31,DATE,J)
+            IDE=NINT(DATE)
+            DO ID=IDS,IDE,10
+               DATE=DBLE(ID)
+               CALL sla_DJCAL(0,DATE,IYMDF,J)
+               CALL sla_MAP(RM,DM,PR,PD,0D0,0D0,2000D0,DATE,RA,DA)
+               WRITE (*,'(1X,I4,2I3.2,F9.5)') (IYMDF(I),I=1,3),(PIBY2-DA)/D2R
+            END DO
+
+            END
+</PRE>
+<P>
+For cases where the transformation has to be repeated for different
+times or for more than one star, the straightforward
+sla_MAP
+approach is apt to be
+wasteful as both the Earth velocity and the
+precession/nutation matrix can be re-calculated relatively
+infrequently without ill effect.  A more efficient method is to
+perform the target-independent calculations only when necessary,
+by calling
+sla_MAPPA,
+and then to use either
+sla_MAPQKZ,
+when only the <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> is known, or
+sla_MAPQK,
+when full catalogue positions, including proper motion, parallax and
+radial velocity, are available.  How frequently to call
+sla_MAPPA
+depends on the accuracy objectives;  once per
+night will deliver sub-arcsecond accuracy for example.
+<P>
+The routines
+sla_AMP
+and
+sla_AMPQK
+allow the reverse transformation, from apparent to mean place.
+<P>
+<BR> <HR>
+<A NAME="tex2html2571" HREF="node213.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2572" HREF="node213.html">Apparent Place to Observed Place</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2570" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2564" HREF="node211.html">Mean Place Transformations</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node213.html b/src/slalib/sun67.htx/node213.html
new file mode 100644
index 0000000..4d2a0e1
--- /dev/null
+++ b/src/slalib/sun67.htx/node213.html
@@ -0,0 +1,181 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Apparent Place to Observed Place</TITLE>
+<META NAME="description" CONTENT="Apparent Place to Observed Place">
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+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000513000000000000000">
+Apparent Place to Observed Place</A>
+</H2>
+The <I>observed place</I> of a source is its position as
+seen by a perfect theodolite at the location of the
+observer.  Transformation of an apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> to observed 
+place involves the following effects:
+<P><UL>
+<LI> <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> to <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$">.<LI> Diurnal aberration.
+<LI> <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$"> to <IMG WIDTH="66" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img28.gif"
+ ALT="$[\,Az,El~]$">.<LI> Refraction.
+</UL>
+The transformation from apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> to
+apparent <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$"> is made by allowing for
+<I>Earth rotation</I> through the <I>sidereal time</I>, <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img298.gif"
+ ALT="$\theta$">:
+<P ALIGN="CENTER"><IMG WIDTH="70" HEIGHT="25"
+ SRC="img299.gif"
+ ALT="\begin{displaymath}
+h = \theta - \alpha \end{displaymath}"></P>
+For this equation to work, <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> must be the apparent right
+ascension for the time of observation, and <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img298.gif"
+ ALT="$\theta$"> must be
+the <I>local apparent sidereal time</I>.  The latter is obtained
+as follows:
+<DL COMPACT>
+<DT>1.
+<DD>from civil time obtain the coordinated universal time, UTC
+(more later on this);
+<DT>2.
+<DD>add the UT1-UTC (typically a few tenths of a second) to
+      give the UT;
+<DT>3.
+<DD>from the UT compute the Greenwich mean sidereal time (using
+sla_GMST);
+<DT>4.
+<DD>add the observer's (east) longitude, giving the local mean
+      sidereal time;
+<DT>5.
+<DD>add the equation of the equinoxes (using
+sla_EQEQX).
+</DL>
+The <I>equation of the equinoxes</I>&nbsp;(<IMG WIDTH="78" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img300.gif"
+ ALT="$=\Delta\psi\cos\epsilon$"> plus
+small terms)
+is the effect of nutation on the sidereal time.
+Its value is typically a second or less.  It is
+interesting to note that if the object of the exercise is to
+transform a mean place all the way into an observed place (very
+often the case),
+then the equation of the
+equinoxes and the longitude component of nutation can both be
+omitted, removing a great deal of computation.  However, SLALIB
+follows the normal convention and  works <I>via</I> the apparent place.
+<P>
+Note that for very precise work the observer's longitude should
+be corrected for <I>polar motion</I>.  This can be done with
+sla_POLMO.
+The corrections are always less than about 
+      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img32.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.3$">   , and
+are futile unless the position of the observer's telescope is known
+to better than a few metres.
+<P>
+Tables of observed and
+predicted UT1-UTC corrections and polar motion data
+are published every few weeks by the International Earth Rotation Service.
+<P>
+The transformation from apparent <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$"> to <I>topocentric</I>
+<IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$"> consists of allowing for
+<I>diurnal aberration</I>.  This effect, maximum amplitude 
+      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img76.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.2$">   ,
+was described earlier.  There is no specific SLALIB routine
+for computing the diurnal aberration,
+though the routines
+sla_AOP <I>etc.</I> include it, and the required velocity vector can be
+determined by calling
+sla_GEOC.
+<P>
+The next stage is the major coordinate rotation from local equatorial
+coordinates <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$"> into horizon coordinates.  The SLALIB routines
+sla_E2H
+<I>etc.</I> can be used for this.  For high-precision
+applications the mean geodetic latitude should be corrected for polar
+motion.
+<P>
+<BR><HR>
+<!--Table of Child-Links-->
+<A NAME="CHILD_LINKS">&#160;</A>
+<UL>
+<LI><A NAME="tex2html2583" HREF="node214.html#SECTION000513100000000000000">
+Refraction</A>
+<LI><A NAME="tex2html2584" HREF="node215.html#SECTION000513200000000000000">
+Efficiency considerations</A>
+</UL>
+<!--End of Table of Child-Links-->
+<BR> <HR>
+<A NAME="tex2html2581" HREF="node214.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+<A NAME="tex2html2573" HREF="node212.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2582" HREF="node214.html">Refraction</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2580" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2574" HREF="node212.html">Mean Place to Apparent Place</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node214.html b/src/slalib/sun67.htx/node214.html
new file mode 100644
index 0000000..41b8d99
--- /dev/null
+++ b/src/slalib/sun67.htx/node214.html
@@ -0,0 +1,189 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Refraction</TITLE>
+<META NAME="description" CONTENT="Refraction">
+<META NAME="keywords" CONTENT="sun67">
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+<META NAME="distribution" CONTENT="global">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2594" HREF="node215.html">Efficiency considerations</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2592" HREF="node213.html">Apparent Place to Observed Place</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2586" HREF="node213.html">Apparent Place to Observed Place</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H3><A NAME="SECTION000513100000000000000">
+Refraction</A>
+</H3>
+The final correction is for atmospheric refraction.
+This effect, which depends on local meteorological conditions and
+the effective colour of the source/detector combination,
+increases the observed elevation of the source by a
+significant effect even at moderate zenith distances, and near the
+horizon by over <IMG WIDTH="25" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img301.gif"
+ ALT="$0^{\circ}
+ \hspace{-0.37em}.\hspace{0.02em}5$">.  The amount of refraction can by
+computed by calling the SLALIB routine
+sla_REFRO;
+however,
+this requires as input the observed zenith distance, which is what
+we are trying to predict.  For high precision it is
+therefore necessary to iterate, using the topocentric
+zenith distance as the initial estimate of the
+observed zenith distance.
+<P>
+The full
+sla_REFRO refraction calculation is onerous, and for
+zenith distances of less than, say, <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img164.gif"
+ ALT="$75^\circ$"> the following
+model can be used instead:
+<P>
+<P ALIGN="CENTER"><IMG WIDTH="255" HEIGHT="27"
+ SRC="img302.gif"
+ ALT="\begin{displaymath}
+\zeta _{vac} \approx \zeta _{obs}
+ + A \tan \zeta _{obs}
+ + B \tan ^{3}\zeta _{obs} \end{displaymath}"></P>
+where <IMG WIDTH="29" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img303.gif"
+ ALT="$\zeta _{vac}$"> is the topocentric
+zenith distance (i.e. <I>in vacuo</I>),
+<IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img184.gif"
+ ALT="$\zeta_{obs}$"> is the observed
+zenith distance (i.e. affected by refraction), and <I>A</I> and <I>B</I> are
+constants, about <IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img304.gif"
+ ALT="$60\hspace{-0.05em}^{'\hspace{-0.1em}'}$">and 
+      <IMG WIDTH="44" HEIGHT="35" ALIGN="MIDDLE" BORDER="0"
+ SRC="img305.gif"
+ ALT="$-0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.06$">    respectively for a sea-level site.
+The two constants can be calculated for a given set of conditions
+by calling either
+sla_REFCO or
+sla_REFCOQ.
+<P>
+sla_REFCO works by calling
+sla_REFRO for two zenith distances and fitting <I>A</I> and <I>B</I>
+to match.  The calculation is onerous, but delivers accurate
+results whatever the conditions.
+sla_REFCOQ uses a direct formulation of <I>A</I> and <I>B</I> and
+is much faster;  it is slightly less accurate than
+sla_REFCO but more than adequate for most practical purposes.
+<P>
+Like the full refraction model, the two-term formulation works in the wrong
+direction for our purposes, predicting
+the <I>in vacuo</I> (topocentric) zenith distance
+given the refracted (observed) zenith distance,
+rather than <I>vice versa</I>.  The obvious approach of
+interchanging <IMG WIDTH="29" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img303.gif"
+ ALT="$\zeta _{vac}$"> and <IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img184.gif"
+ ALT="$\zeta_{obs}$"> and
+reversing the signs, though approximately
+correct, gives avoidable errors which are just significant in
+some applications;  for
+example about 
+      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img76.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.2$">    at <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img174.gif"
+ ALT="$70^\circ$"> zenith distance.  A
+much better result can easily be obtained, by using one Newton-Raphson
+iteration as follows:
+<P>
+<P ALIGN="CENTER"><IMG WIDTH="313" HEIGHT="45"
+ SRC="img306.gif"
+ ALT="\begin{displaymath}
+\zeta _{obs} \approx \zeta _{vac}
+ - \frac{A \tan \zeta _{va...
+ ...
+ {1 + ( A + 3 B \tan ^{2}\zeta _{vac} ) \sec ^{2}\zeta _{vac}}\end{displaymath}"></P>
+<P>
+The effect of refraction can be applied to an unrefracted
+zenith distance by calling
+sla_REFZ or to an unrefracted
+<IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$"> by calling
+sla_REFV.
+Over most of the sky these two routines deliver almost identical
+results, but beyond <IMG WIDTH="56" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img209.gif"
+ ALT="$\zeta=83^\circ$">sla_REFV
+becomes unacceptably inaccurate while
+sla_REFZ
+remains usable.  (However
+sla_REFV
+is significantly faster, which may be important in some applications.)
+SLALIB also provides a routine for computing the airmass, the function
+sla_AIRMAS.
+<P>
+The refraction ``constants'' returned by
+sla_REFCO and
+sla_REFCOQ
+are slightly affected by colour, especially at the blue end
+of the spectrum.  Where values for more than one
+wavelength are needed, rather than calling
+sla_REFCO
+several times it is more efficient to call
+sla_REFCO
+just once, for a selected ``base'' wavelength, and then to call
+sla_ATMDSP
+once for each wavelength of interest.
+<P>
+All the SLALIB refraction routines work for radio wavelengths as well
+as the optical/IR band.  The radio refraction is very dependent on
+humidity, and an accurate value must be supplied.  There is no
+wavelength dependence, however.  The choice of optical/IR or
+radio is made by specifying a wavelength greater than <IMG WIDTH="51" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img307.gif"
+ ALT="$100\mu m$">for the radio case.
+<P>
+<BR> <HR>
+<A NAME="tex2html2593" HREF="node215.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2591" HREF="node213.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2585" HREF="node213.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2594" HREF="node215.html">Efficiency considerations</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2592" HREF="node213.html">Apparent Place to Observed Place</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2586" HREF="node213.html">Apparent Place to Observed Place</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node215.html b/src/slalib/sun67.htx/node215.html
new file mode 100644
index 0000000..020487b
--- /dev/null
+++ b/src/slalib/sun67.htx/node215.html
@@ -0,0 +1,87 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Efficiency considerations</TITLE>
+<META NAME="description" CONTENT="Efficiency considerations">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="previous" HREF="node214.html">
+<LINK REL="up" HREF="node213.html">
+<LINK REL="next" HREF="node216.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html2601" HREF="node216.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2599" HREF="node213.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2595" HREF="node214.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2602" HREF="node216.html">The Hipparcos Catalogue and the ICRS</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2600" HREF="node213.html">Apparent Place to Observed Place</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2596" HREF="node214.html">Refraction</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H3><A NAME="SECTION000513200000000000000">
+Efficiency considerations</A>
+</H3>
+The complete apparent place to observed place transformation
+can be carried out by calling
+sla_AOP.
+For improved efficiency
+in cases of more than one star or a sequence of times, the
+target-independent calculations can be done once by
+calling
+sla_AOPPA,
+the time can be updated by calling
+sla_AOPPAT,
+and
+sla_AOPQK
+can then be used to perform the
+apparent-to-observed transformation.  The reverse transformation
+is available through
+sla_OAP
+and
+sla_OAPQK.
+(<I>n.b.</I> These routines use accurate but computationally-expensive
+refraction algorithms for zenith distances beyond about <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img33.gif"
+ ALT="$76^\circ$">.For many purposes, in-line code tailored to the accuracy requirements
+of the application will be preferable, for example ignoring UT1-UTC,
+omitting diurnal aberration and using
+sla_REFZ
+to apply the refraction.)
+<P>
+<BR> <HR>
+<A NAME="tex2html2601" HREF="node216.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2599" HREF="node213.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2595" HREF="node214.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2602" HREF="node216.html">The Hipparcos Catalogue and the ICRS</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2600" HREF="node213.html">Apparent Place to Observed Place</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2596" HREF="node214.html">Refraction</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node216.html b/src/slalib/sun67.htx/node216.html
new file mode 100644
index 0000000..ab75104
--- /dev/null
+++ b/src/slalib/sun67.htx/node216.html
@@ -0,0 +1,110 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>The Hipparcos Catalogue and the ICRS</TITLE>
+<META NAME="description" CONTENT="The Hipparcos Catalogue and the ICRS">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node217.html">
+<LINK REL="previous" HREF="node213.html">
+<LINK REL="up" HREF="node197.html">
+<LINK REL="next" HREF="node217.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html2611" HREF="node217.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2609" HREF="node197.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2603" HREF="node215.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2612" HREF="node217.html">Timescales</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2610" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2604" HREF="node215.html">Efficiency considerations</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000514000000000000000">
+The Hipparcos Catalogue and the ICRS</A>
+</H2>
+With effect from the beginning of 1998, the IAU adopted a new
+reference system to replace FK5 J2000.  The new system, called the
+International Celestial Reference System (ICRS), differs profoundly
+from all predecessors in that the link with solar-system dynamics
+was broken;  the ICRS axes are defined in terms of the directions
+of a set of extragalactic sources, not in terms of the mean equator and
+equinox at a given reference epoch.  Although the ICRS and FK5 coordinates
+of any given object are almost the same, the orientation of the new frame
+was essentially arbitrary, and the close match to FK5 J2000 was contrived
+purely for reasons of continuity and convenience.
+<P>
+A distinction is made between the reference <I>system</I> (the ICRS)
+and <I>frame</I> (ICRF).  The ICRS is the set of prescriptions and
+conventions together with the modelling required to define, at any
+time, a triad of axes.  The ICRF is a practical realization, and
+currently consists of a catalogue of equatorial coordinates for 608
+extragalactic radio sources observed by VLBI.
+<P>
+The best optical realization of the ICRF currently available is the
+Hipparcos catalogue.  The extragalactic sources were not directly
+observable by the Hipparcos satellite and so the link from Hipparcos
+to ICRF was established through a variety of indirect techniques: VLBI and
+conventional interferometry of radio stars, photographic astrometry
+and so on.  The Hipparcos frame is aligned to the ICRF to within about
+0.5&nbsp;mas and 0.5&nbsp;mas/year (at epoch 1991.25).
+<P>
+The Hipparcos catalogue includes all of the FK5 stars, which has enabled
+the orientation and spin of the latter to be studied.  At epoch J2000,
+the misalignment of the FK5 frame with respect to Hipparcos
+(and hence ICRS) are about 32&nbsp;mas and 1&nbsp;mas/year respectively.
+Consequently, for many practical purposes, including pointing
+telescopes, the IAU 1976-1982 conventions on reference frames and
+Earth orientation remain adequate and there is no need to change to
+Hipparcos coordinates, new precession/nutation models and so on.
+However, for the most exacting astrometric applications, SLALIB
+provides some support for Hipparcos coordinates in the form of
+four new routines:
+sla_FK52H and
+sla_H2FK5,
+which transform FK5 positions and proper motions to the Hipparcos frame
+and <I>vice versa,</I> and
+sla_FK5HZ and
+sla_HFK5Z,
+where the transformations are for stars whose Hipparcos proper motion is
+zero.
+<P>
+Further information on the ICRS can be found in the paper by M.Feissel
+and F.Mignard, Astron.Astrophys. 331, L33-L36 (1988).
+<P>
+<BR> <HR>
+<A NAME="tex2html2611" HREF="node217.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2609" HREF="node197.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2603" HREF="node215.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2612" HREF="node217.html">Timescales</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2610" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2604" HREF="node215.html">Efficiency considerations</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node217.html b/src/slalib/sun67.htx/node217.html
new file mode 100644
index 0000000..b6fbe6c
--- /dev/null
+++ b/src/slalib/sun67.htx/node217.html
@@ -0,0 +1,92 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Timescales</TITLE>
+<META NAME="description" CONTENT="Timescales">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node222.html">
+<LINK REL="previous" HREF="node216.html">
+<LINK REL="up" HREF="node197.html">
+<LINK REL="next" HREF="node218.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html2621" HREF="node218.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2619" HREF="node197.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2613" HREF="node216.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2622" HREF="node218.html">Atomic Time: TAI</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2620" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2614" HREF="node216.html">The Hipparcos Catalogue and the ICRS</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000515000000000000000">
+Timescales</A>
+</H2>
+SLALIB provides for conversion between several timescales, and involves
+use of one or two others.  The full list is as follows:
+<UL>
+<LI> TAI: International Atomic Time
+<LI> UTC: Coordinated Universal Time
+<LI> UT: Universal Time
+<LI> GMST: Greenwich Mean Sidereal Time
+<LI> LAST: Local Apparent Sidereal Time
+<LI> TT: Terrestrial Time
+<LI> TDB: Barycentric Dynamical Time.
+</UL>
+Three obsolete timescales should be mentioned here to avoid confusion.
+<UL>
+<LI> GMT: Greenwich Mean Time - can mean either UTC or UT.
+<LI> ET: Ephemeris Time - more or less the same as either TT or TDB.
+<LI> TDT: Terrestrial Dynamical Time - former name of TT.
+</UL>
+<BR><HR>
+<!--Table of Child-Links-->
+<A NAME="CHILD_LINKS">&#160;</A>
+<UL>
+<LI><A NAME="tex2html2623" HREF="node218.html#SECTION000515100000000000000">
+Atomic Time: TAI</A>
+<LI><A NAME="tex2html2624" HREF="node219.html#SECTION000515200000000000000">
+Universal Time: UTC, UT1</A>
+<LI><A NAME="tex2html2625" HREF="node220.html#SECTION000515300000000000000">
+Sidereal Time: GMST, LAST</A>
+<LI><A NAME="tex2html2626" HREF="node221.html#SECTION000515400000000000000">
+Dynamical Time: TT, TDB</A>
+</UL>
+<!--End of Table of Child-Links-->
+<BR> <HR>
+<A NAME="tex2html2621" HREF="node218.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2619" HREF="node197.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2613" HREF="node216.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2622" HREF="node218.html">Atomic Time: TAI</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2620" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2614" HREF="node216.html">The Hipparcos Catalogue and the ICRS</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node218.html b/src/slalib/sun67.htx/node218.html
new file mode 100644
index 0000000..106412e
--- /dev/null
+++ b/src/slalib/sun67.htx/node218.html
@@ -0,0 +1,91 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Atomic Time: TAI</TITLE>
+<META NAME="description" CONTENT="Atomic Time: TAI">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node219.html">
+<LINK REL="previous" HREF="node217.html">
+<LINK REL="up" HREF="node217.html">
+<LINK REL="next" HREF="node219.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html2635" HREF="node219.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2633" HREF="node217.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2627" HREF="node217.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2636" HREF="node219.html">Universal Time: UTC, UT1</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2634" HREF="node217.html">Timescales</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2628" HREF="node217.html">Timescales</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H3><A NAME="SECTION000515100000000000000">
+Atomic Time: TAI</A>
+</H3>
+<I>International Atomic Time</I> TAI is a laboratory timescale.  Its
+unit is the SI second, which is defined in terms of a
+defined number
+of wavelengths of the radiation produced by a certain electronic
+transition in the caesium 133 atom.  It
+is realized through a changing
+population of high-precision atomic clocks held
+at standards institutes in various countries.  There is an
+elaborate process of continuous intercomparison, leading to
+a weighted average of all the clocks involved.
+<P>
+Though TAI shares the same second as the more familiar UTC, the
+two timescales are noticeably separated in epoch because of the
+build-up of leap seconds.  At the time of writing, UTC
+lags about half a minute behind TAI.
+<P>
+For any given date, the difference TAI-UTC
+can be obtained by calling the SLALIB routine
+sla_DAT.
+Note, however, that an up-to-date copy of the routine must be used if
+the most recent leap seconds are required.  For applications
+where this is critical, mechanisms independent of SLALIB
+and under local control must
+be set up;  in such cases
+sla_DAT
+can be useful as an
+independent check, for test dates within the range of the
+available version.  Up-to-date information on TAI-UTC is available
+from <TT>ftp://maia.usno.navy.mil/ser7/tai-utc.dat</TT>.
+<P>
+<BR> <HR>
+<A NAME="tex2html2635" HREF="node219.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2633" HREF="node217.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2627" HREF="node217.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2636" HREF="node219.html">Universal Time: UTC, UT1</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2634" HREF="node217.html">Timescales</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2628" HREF="node217.html">Timescales</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node219.html b/src/slalib/sun67.htx/node219.html
new file mode 100644
index 0000000..4214aaa
--- /dev/null
+++ b/src/slalib/sun67.htx/node219.html
@@ -0,0 +1,184 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Universal Time: UTC, UT1</TITLE>
+<META NAME="description" CONTENT="Universal Time: UTC, UT1">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node220.html">
+<LINK REL="previous" HREF="node218.html">
+<LINK REL="up" HREF="node217.html">
+<LINK REL="next" HREF="node220.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html2645" HREF="node220.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2643" HREF="node217.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2637" HREF="node218.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2646" HREF="node220.html">Sidereal Time: GMST, LAST</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2644" HREF="node217.html">Timescales</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2638" HREF="node218.html">Atomic Time: TAI</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H3><A NAME="SECTION000515200000000000000">
+Universal Time: UTC, UT1</A>
+</H3>
+<I>Coordinated Universal Time</I> UTC is the basis of civil timekeeping.
+Most time zones differ from UTC by an integer number
+of hours, though a few (<I>e.g.</I> parts of Canada and Australia) differ
+by <I>n</I>+0.5&nbsp;hours.  The UTC second is the same as the SI second,
+as for TAI.  In the long term, UTC keeps in step with the
+Sun.  It does so even though the Earth's rotation is slightly
+variable (due to large scale movements of water and atmosphere
+among other things) by occasionally introducing a <I>leap
+second</I>.
+<P><I>Universal Time</I> UT, or more specifically UT1,
+is in effect the mean solar time.  It is continuous
+(<I>i.e.</I> there are no leap seconds) but has a variable
+rate because of the Earth's non-uniform rotation period.  It is
+needed for computing the sidereal time, an essential part of
+pointing a telescope at a celestial source.  To obtain UT1, you
+have to look up the value of UT1-UTC for the date concerned
+in tables published by the International Earth Rotation
+Service;  this quantity, kept in the range
+<IMG WIDTH="15" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img30.gif"
+ ALT="$\pm$"><IMG WIDTH="24" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img31.gif"
+ ALT="$0^{\rm s}\hspace{-0.3em}.9$"> by means of UTC leap
+seconds, is then added to the UTC.  The quantity UT1-UTC,
+which typically changes by 1 or 2&nbsp;ms per day,
+can only be obtained by observation, though seasonal trends
+are known and the IERS listings are able to predict some way into
+the future with adequate accuracy for pointing telescopes.
+<P>
+UTC leap seconds are introduced as necessary,
+usually at the end of December or June.
+On the average the solar day is slightly longer
+than the nominal 86,400&nbsp;SI&nbsp;seconds and so leap seconds are always positive;
+however, provision exists for negative leap seconds if needed.
+The form of a leap second can be seen from the
+following description of the end of June&nbsp;1994:
+<P><A NAME="27722">&#160;</A>
+<TABLE CELLPADDING=3>
+<CAPTION><STRONG>Figure 1:</STRONG>
+Relationship Between Celestial Coordinates</CAPTION>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP>&nbsp;</TD>
+<TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+<TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+<TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP>&nbsp;</TD>
+<TD ALIGN="CENTER" NOWRAP>UTC</TD>
+<TD ALIGN="CENTER" NOWRAP>UT1-UTC</TD>
+<TD ALIGN="CENTER" NOWRAP>UT1</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP>&nbsp;</TD>
+<TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+<TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+<TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP>1994</TD>
+<TD ALIGN="LEFT" NOWRAP>June</TD>
+<TD ALIGN="RIGHT" NOWRAP>30</TD>
+<TD ALIGN="CENTER" NOWRAP>23 59 58</TD>
+<TD ALIGN="CENTER" NOWRAP>-0.218</TD>
+<TD ALIGN="CENTER" NOWRAP>23 59 57.782</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP>&nbsp;</TD>
+<TD ALIGN="CENTER" NOWRAP>23 59 59</TD>
+<TD ALIGN="CENTER" NOWRAP>-0.218</TD>
+<TD ALIGN="CENTER" NOWRAP>23 59 58.782</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP>&nbsp;</TD>
+<TD ALIGN="CENTER" NOWRAP>23 59 60</TD>
+<TD ALIGN="CENTER" NOWRAP>-0.218</TD>
+<TD ALIGN="CENTER" NOWRAP>23 59 59.782</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+<TD ALIGN="LEFT" NOWRAP>July</TD>
+<TD ALIGN="RIGHT" NOWRAP>1</TD>
+<TD ALIGN="CENTER" NOWRAP>00 00 00</TD>
+<TD ALIGN="CENTER" NOWRAP>+0.782</TD>
+<TD ALIGN="CENTER" NOWRAP>00 00 00.782</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+<TD ALIGN="RIGHT" NOWRAP>&nbsp;</TD>
+<TD ALIGN="CENTER" NOWRAP>00 00 01</TD>
+<TD ALIGN="CENTER" NOWRAP>+0.782</TD>
+<TD ALIGN="CENTER" NOWRAP>00 00 01.782</TD>
+</TR>
+</TABLE>
+<P>
+Note that UTC has to be expressed as hours, minutes and
+seconds (or at least in seconds for a given date) if leap seconds
+are to be taken into account.  It is improper to express a UTC as a
+Julian Date, for example, because there will be an ambiguity
+during a leap second (in the above example,
+1994&nbsp;June&nbsp;30 <IMG WIDTH="96" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img308.gif"
+ ALT="$23^{h}\,59^{m}\,60^{s}.0$"> and
+1994&nbsp;July&nbsp;1 <IMG WIDTH="96" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img309.gif"
+ ALT="$00^{h}\,00^{m}\,00^{s}.0$"> would <I>both</I> come out as
+MJD&nbsp;49534.00000).  Although in the vast majority of
+cases this won't matter, there are potential problems in
+on-line data acquisition systems and in applications involving
+taking the difference between two times.  Note that although the routines
+sla_DAT
+and
+sla_DTT
+expect UTC in the form of an MJD, the meaning here is really a
+whole-number <I>date</I> rather than a time.  Though the routines will accept
+a fractional part and will almost always function correctly, on a day
+which ends with a leap
+second incorrect results would be obtained during the leap second
+itself because by then the MJD would have moved into the next day.
+<P>
+<BR> <HR>
+<A NAME="tex2html2645" HREF="node220.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2643" HREF="node217.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2637" HREF="node218.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2646" HREF="node220.html">Sidereal Time: GMST, LAST</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2644" HREF="node217.html">Timescales</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2638" HREF="node218.html">Atomic Time: TAI</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node22.html b/src/slalib/sun67.htx/node22.html
new file mode 100644
index 0000000..4e96061
--- /dev/null
+++ b/src/slalib/sun67.htx/node22.html
@@ -0,0 +1,119 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_AOPPAT - Update Appt-to-Obs Parameters</TITLE>
+<META NAME="description" CONTENT="SLA_AOPPAT - Update Appt-to-Obs Parameters">
+<META NAME="keywords" CONTENT="sun67">
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+<LINK REL="previous" HREF="node21.html">
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+<A NAME="tex2html638" HREF="node21.html">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html647" HREF="node23.html">SLA_AOPQK - Quick Appt-to-Observed</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html645" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html639" HREF="node21.html">SLA_AOPPA - Appt-to-Obs Parameters</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION00049000000000000000">SLA_AOPPAT - Update Appt-to-Obs Parameters</A>
+<A NAME="xref_SLA_AOPPAT">&#160;</A><A NAME="SLA_AOPPAT">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Recompute the sidereal time in the apparent to observed place
+star-independent parameter block.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_AOPPAT (DATE, AOPRMS)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>UTC date/time (Modified Julian Date, JD-2400000.5)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AOPRMS</EM></TD>
+<TD ALIGN="LEFT"><B>D(14)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>star-independent apparent-to-observed parameters:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(1-12)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>not required</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(13)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>longitude + eqn of equinoxes +
+``sidereal <IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">UT'' (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(14)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>not required</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AOPRMS</EM></TD>
+<TH ALIGN="LEFT"><B>D(14)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>star-independent apparent-to-observed parameters:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(1-13)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>not changed</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(14)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>local apparent sidereal time (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTE:</STRONG>
+<DD>For more information, see sla_AOPPA.
+</DL>
+<BR> <HR>
+<A NAME="tex2html646" HREF="node23.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html644" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html638" HREF="node21.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html647" HREF="node23.html">SLA_AOPQK - Quick Appt-to-Observed</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html645" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html639" HREF="node21.html">SLA_AOPPA - Appt-to-Obs Parameters</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node220.html b/src/slalib/sun67.htx/node220.html
new file mode 100644
index 0000000..84db99f
--- /dev/null
+++ b/src/slalib/sun67.htx/node220.html
@@ -0,0 +1,96 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Sidereal Time: GMST, LAST</TITLE>
+<META NAME="description" CONTENT="Sidereal Time: GMST, LAST">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
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+<LINK REL="next" HREF="node221.html">
+<LINK REL="previous" HREF="node219.html">
+<LINK REL="up" HREF="node217.html">
+<LINK REL="next" HREF="node221.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html2655" HREF="node221.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2653" HREF="node217.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2647" HREF="node219.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2656" HREF="node221.html">Dynamical Time: TT, TDB</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2654" HREF="node217.html">Timescales</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2648" HREF="node219.html">Universal Time: UTC, UT1</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H3><A NAME="SECTION000515300000000000000">
+Sidereal Time: GMST, LAST</A>
+</H3>
+Sidereal Time is the ``time of day'' relative to the
+stars rather than to the Sun.  After
+one sidereal day the stars come back to the same place in the
+sky, apart from sub-arcsecond precession effects.  Because the Earth
+rotates faster relative to the stars than to the Sun by one day
+per year, the sidereal second is shorter than the solar
+second; the ratio is about 0.9973.
+<P>
+The <I>Greenwich Mean Sidereal Time</I> GMST is
+linked to UT1 by a numerical formula which
+is implemented in the SLALIB routines
+sla_GMST
+and
+sla_GMSTA.
+There are, of course, no leap seconds in GMST, but the second
+changes in length along with the UT1 second, and also varies
+over long periods of time because of slow changes in the Earth's
+orbit.  This makes the timescale unsuitable for everything except
+predicting the apparent directions of celestial sources.
+<P>
+The <I>Local Apparent Sidereal Time</I> LAST is the apparent right
+ascension of the local meridian, from which the hour angle of any
+star can be determined knowing its <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$">.  It can be obtained from the
+GMST by adding the east longitude (corrected for polar motion
+in precise work) and the <I>equation of the equinoxes</I>.  The
+latter, already described, is an aspect of the nutation effect
+and can be predicted by calling the SLALIB routine
+sla_EQEQX
+or, neglecting certain very small terms, by calling
+sla_NUTC
+and using the expression <IMG WIDTH="61" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img310.gif"
+ ALT="$\Delta\psi\cos\epsilon$">.<P>
+<BR> <HR>
+<A NAME="tex2html2655" HREF="node221.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2653" HREF="node217.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2647" HREF="node219.html">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2656" HREF="node221.html">Dynamical Time: TT, TDB</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2654" HREF="node217.html">Timescales</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2648" HREF="node219.html">Universal Time: UTC, UT1</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node221.html b/src/slalib/sun67.htx/node221.html
new file mode 100644
index 0000000..926f2ce
--- /dev/null
+++ b/src/slalib/sun67.htx/node221.html
@@ -0,0 +1,158 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Dynamical Time: TT, TDB</TITLE>
+<META NAME="description" CONTENT="Dynamical Time: TT, TDB">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
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+<A NAME="tex2html2657" HREF="node220.html">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2664" HREF="node222.html">Calendars</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2662" HREF="node217.html">Timescales</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2658" HREF="node220.html">Sidereal Time: GMST, LAST</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H3><A NAME="SECTION000515400000000000000">
+Dynamical Time: TT, TDB</A>
+</H3>
+Dynamical time is the independent variable in the theories
+which describe the motions of bodies in the solar system.  When
+you use published formulae which model the position of the
+Earth in its orbit, for example, or look up
+the Moon's position in a precomputed ephemeris, the date and time
+you use must be in terms of one of the dynamical timescales.  It
+is a common but understandable mistake to use UT directly, in which
+case the results will be about 1&nbsp;minute out (in the present
+era).
+<P>
+It is not hard to see why such timescales are necessary.
+UTC would clearly be unsuitable as the argument of an
+ephemeris because of leap seconds.
+A solar-system ephemeris based on UT1 or sidereal time would somehow
+have to include the unpredictable variations of the Earth's rotation.
+TAI would work, but eventually
+the ephemeris and the ensemble of atomic clocks would drift apart.
+In effect, the ephemeris <I>is</I> a clock, with the bodies of
+the solar system the hands.
+<P>
+Only two of the dynamical timescales are of any great importance to
+observational astronomers, TT and TDB.  (The obsolete
+timescale ET, ephemeris time, was more or less the same as TT.)
+<P><I>Terrestrial Time</I> TT is
+the theoretical timescale of apparent geocentric ephemerides of solar
+system bodies.  It applies, in principle,
+to an Earthbound clock, at sea-level, and for practical purposes
+it is tied to
+Atomic Time TAI through the formula TT&nbsp;=&nbsp;TAI&nbsp;+&nbsp;<IMG WIDTH="48" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img311.gif"
+ ALT="$32^{\rm s}\hspace{-0.3em}.184$">.In practice, therefore, the units of TT are ordinary SI seconds, and
+the offset of <IMG WIDTH="48" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img311.gif"
+ ALT="$32^{\rm s}\hspace{-0.3em}.184$"> with respect to TAI is fixed.
+The SLALIB routine
+sla_DTT
+returns TT-UTC for a given UTC 
+(<I>n.b.</I>  sla_DTT
+calls
+sla_DAT,
+and the latter must be an up-to-date version if recent leap seconds are
+to be taken into account).
+<P><I>Barycentric Dynamical Time</I> TDB differs from TT by an amount which
+cycles back and forth by a millisecond or two due to
+relativistic effects.  The variation is
+negligible for most purposes, but unless taken into
+account would swamp
+long-term analysis of pulse arrival times from the
+millisecond pulsars.  It is a consequence of
+the TT clock being on the Earth rather than in empty
+space:  the ellipticity of
+the Earth's orbit means that the TT clock's speed and
+gravitational potential vary slightly
+during the course of the year, and as a consequence
+its rate as seen from an outside observer
+varies due to transverse Doppler effect and gravitational
+redshift.  By definition, TDB and TT differ only
+by periodic terms, and the main effect
+is a sinusoidal variation of amplitude <IMG WIDTH="48" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img312.gif"
+ ALT="$0^{\rm s}\hspace{-0.3em}.0016$">;  the
+largest planetary terms are nearly two orders of magnitude
+smaller.  The SLALIB routine
+sla_RCC
+provides a model of
+TDB-TT accurate to a few nanoseconds.
+There are other dynamical timescales, not supported by
+SLALIB routines, which include allowance also for the secular terms.
+These timescales gain on TT and TDB by about <IMG WIDTH="48" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img313.gif"
+ ALT="$0^{\rm s}\hspace{-0.3em}.0013$">/day.
+<P>
+For most purposes the more accessible TT is the timescale to use,
+for example when calling
+sla_PRENUT
+to generate a precession/nutation matrix or when calling
+sla_EVP
+to predict the
+Earth's position and velocity.  For some purposes TDB is the
+correct timescale, for example when interrogating the JPL planetary
+ephemeris (see <I>Starlink User Note&nbsp;87</I>), though in most cases
+TT will be near enough and will involve less computation.
+<P>
+Investigations of topocentric solar-system phenomena such as
+occultations and eclipses require solar time as well as dynamical
+time.  TT/TDB/ET is all that is required in order to compute the geocentric
+circumstances, but if horizon coordinates or geocentric parallax
+are to be tackled UT is also needed.  A rough estimate
+of <IMG WIDTH="117" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img314.gif"
+ ALT="$\Delta {\rm T} = {\rm ET} - {\rm UT}$"> is
+available via the routine
+sla_DT.
+For a given epoch (<I>e.g.</I> 1650) this returns an approximation
+to <IMG WIDTH="28" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img315.gif"
+ ALT="$\Delta {\rm T}$"> in seconds.
+<P>
+<BR> <HR>
+<A NAME="tex2html2663" HREF="node222.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2661" HREF="node217.html">
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+<A NAME="tex2html2657" HREF="node220.html">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2664" HREF="node222.html">Calendars</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2662" HREF="node217.html">Timescales</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2658" HREF="node220.html">Sidereal Time: GMST, LAST</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node222.html b/src/slalib/sun67.htx/node222.html
new file mode 100644
index 0000000..7cc8f58
--- /dev/null
+++ b/src/slalib/sun67.htx/node222.html
@@ -0,0 +1,113 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Calendars</TITLE>
+<META NAME="description" CONTENT="Calendars">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
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+<LINK REL="previous" HREF="node217.html">
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+<BODY >
+<BR> <HR>
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+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2671" HREF="node197.html">
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+<A NAME="tex2html2665" HREF="node221.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2674" HREF="node223.html">Geocentric Coordinates</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2672" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2666" HREF="node221.html">Dynamical Time: TT, TDB</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000516000000000000000">
+Calendars</A>
+</H2>
+The ordinary <I>Gregorian Calendar Date</I>,
+together with a time of day, can be
+used to express an epoch in any desired timescale.  For many purposes,
+however, a continuous count of days is more convenient, and for
+this purpose the system of <I>Julian Day Number</I> can be used.
+JD zero is located about 7000&nbsp;years ago, well before the
+historical era, and is formally defined in terms of Greenwich noon;
+Julian Day Number 2449444 began at noon on 1994 April&nbsp;1.  <I>Julian Date</I>
+is the same system but with a fractional part appended;
+Julian Date 2449443.5 was the midnight on which 1994 April&nbsp;1
+commenced.  Because of the unwieldy size of Julian Dates
+and the awkwardness of the half-day offset, it is
+accepted practice to remove the leading `24' and the trailing `.5',
+producing what is called the <I>Modified Julian Date</I>:
+MJD&nbsp;=&nbsp;JD-2400000.5.  SLALIB routines use MJD, as opposed to
+JD, throughout, largely to avoid loss of precision.
+1994 April&nbsp;1 commenced at MJD&nbsp;49443.0.
+<P>
+Despite JD (and hence MJD) being defined in terms of (in effect)
+UT, the system can be used in conjunction with other timescales
+such as TAI, TT and TDB (and even sidereal time through the
+concept of <I>Greenwich Sidereal Date</I>).  However, it is improper
+to express a UTC as a JD or MJD because of leap seconds.
+<P>
+SLALIB has six routines for converting to and from dates in
+the Gregorian calendar.  The routines
+sla_CLDJ
+and
+sla_CALDJ
+both convert a calendar date into an MJD, the former interpreting
+years between 0 and 99 as 1st century and the latter as late 20th or
+early 21st century.  The routines sla_DJCL
+and
+sla_DJCAL
+both convert an MJD into calendar year, month, day and fraction of a day;
+the latter performs rounding to a specified precision, important
+to avoid dates like `<TT>94 04 01.***</TT>' appearing in messages.
+Some of SLALIB's low-precision ephemeris routines
+(sla_EARTH,
+sla_MOON
+and
+sla_ECOR)
+work in terms of year plus day-in-year (where
+day&nbsp;1&nbsp;=&nbsp;January&nbsp;1st, at least for the modern era).
+This form of date can be generated by
+calling
+sla_CALYD
+(which defaults years 0-99 into 1950-2049)
+or
+sla_CLYD
+(which covers the full range from prehistoric times).
+<P>
+<BR> <HR>
+<A NAME="tex2html2673" HREF="node223.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2671" HREF="node197.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2665" HREF="node221.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2674" HREF="node223.html">Geocentric Coordinates</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2672" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2666" HREF="node221.html">Dynamical Time: TT, TDB</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node223.html b/src/slalib/sun67.htx/node223.html
new file mode 100644
index 0000000..497a385
--- /dev/null
+++ b/src/slalib/sun67.htx/node223.html
@@ -0,0 +1,139 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Geocentric Coordinates</TITLE>
+<META NAME="description" CONTENT="Geocentric Coordinates">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
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+<LINK REL="previous" HREF="node222.html">
+<LINK REL="up" HREF="node197.html">
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+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html2683" HREF="node224.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2681" HREF="node197.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2675" HREF="node222.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2684" HREF="node224.html">Ephemerides</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2682" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2676" HREF="node222.html">Calendars</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000517000000000000000">
+Geocentric Coordinates</A>
+</H2>
+The location of the observer on the Earth is significant in a
+number of ways.  The most obvious, of course, is the effect of latitude
+on the observed <IMG WIDTH="66" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img28.gif"
+ ALT="$[\,Az,El~]$"> of a star.  Less obvious is the need to
+allow for geocentric parallax when finding the Moon with a
+telescope (and when doing high-precision work involving the
+Sun or planets), and the need to correct observed radial
+velocities and apparent pulsar periods for the effects
+of the Earth's rotation.
+<P>
+The SLALIB routine
+sla_OBS
+supplies details of groundbased observatories from an internal
+list.  This is useful when writing applications that apply to
+more than one observatory;  the user can enter a brief name,
+or browse through a list, and be spared the trouble of typing
+in the full latitude, longitude <I>etc</I>.  The following
+Fortran code returns the full name, longitude and latitude
+of a specified observatory:
+<P><PRE>
+            CHARACTER IDENT*10,NAME*40
+            DOUBLE PRECISION W,P,H
+             :
+            CALL sla_OBS(0,IDENT,NAME,W,P,H)
+            IF (NAME.EQ.'?') ...             (not recognized)
+</PRE>
+<P>(Beware of the longitude sign convention, which is west +ve
+for historical reasons.)  The following lists all
+the supported observatories:
+<P><PRE>
+             :
+            INTEGER N
+             :
+            N=1
+            NAME=' '
+            DO WHILE (NAME.NE.'?')
+               CALL sla_OBS(N,IDENT,NAME,W,P,H)
+               IF (NAME.NE.'?') THEN
+                  WRITE (*,'(1X,I3,4X,A,4X,A)') N,IDENT,NAME
+                  N=N+1
+               END IF
+            END DO
+</PRE>
+<P>
+The routine
+sla_GEOC
+converts a <I>geodetic latitude</I>
+(one referred to the local horizon) to a geocentric position,
+taking into account the Earth's oblateness and also the height
+above sea level of the observer.  The results are expressed in
+vector form, namely as the distance of the observer from
+the spin axis and equator respectively.  The <I>geocentric
+latitude</I> can be found be evaluating ATAN2 of the
+two numbers.  A full 3-D vector description of the position
+and velocity of the observer is available through the routine
+sla_PVOBS.
+For a specified geodetic latitude, height above
+sea level, and local sidereal time,
+sla_PVOBS
+generates a 6-element vector containing the position and
+velocity with respect to the true equator and equinox of
+date (<I>i.e.</I> compatible with apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">).  For
+some applications it will be necessary to convert to a
+mean <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> frame (notably FK5, J2000) by multiplying
+elements 1-3 and 4-6 respectively with the appropriate
+precession matrix.  (In theory an additional correction to the
+velocity vector is needed to allow for differential precession,
+but this correction is always negligible.)
+<P>
+See also the discussion of the routine
+sla_RVEROT,
+later.
+<P>
+<BR> <HR>
+<A NAME="tex2html2683" HREF="node224.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2681" HREF="node197.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2675" HREF="node222.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2684" HREF="node224.html">Ephemerides</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2682" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2676" HREF="node222.html">Calendars</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node224.html b/src/slalib/sun67.htx/node224.html
new file mode 100644
index 0000000..4cb8678
--- /dev/null
+++ b/src/slalib/sun67.htx/node224.html
@@ -0,0 +1,617 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Ephemerides</TITLE>
+<META NAME="description" CONTENT="Ephemerides">
+<META NAME="keywords" CONTENT="sun67">
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+<META NAME="distribution" CONTENT="global">
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+<H2><A NAME="SECTION000518000000000000000">
+Ephemerides</A>
+</H2>
+SLALIB includes routines for generating positions and
+velocities of Solar-System bodies.  The accuracy objectives are
+modest, and the SLALIB facilities do not attempt
+to compete with precomputed ephemerides such as
+those provided by JPL, or with models containing
+thousands of terms.  It is also worth noting
+that SLALIB's very accurate star coordinate conversion
+routines are not strictly applicable to solar-system cases,
+though they are adequate for most practical purposes.
+<P>
+Earth/Sun ephemerides can be generated using the routine
+sla_EVP,
+which predicts Earth position and velocity with respect to both the
+solar-system barycentre and the
+Sun.  Maximum velocity error is 0.42&nbsp;metres per second;  maximum
+heliocentric position error is 1600&nbsp;km (about <IMG WIDTH="17" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img316.gif"
+ ALT="$2\hspace{-0.05em}^{'\hspace{-0.1em}'}$">), with
+barycentric position errors about 4 times worse.
+(The Sun's position as
+seen from the Earth can, of course, be obtained simply by
+reversing the signs of the Cartesian components of the
+Earth:Sun vector.)
+<P>
+Geocentric Moon ephemerides are available from
+sla_DMOON,
+which predicts the Moon's position and velocity with respect to
+the Earth's centre.  Direction accuracy is usually better than
+10&nbsp;km (<IMG WIDTH="17" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img131.gif"
+ ALT="$5\hspace{-0.05em}^{'\hspace{-0.1em}'}$">) and distance accuracy a little worse.
+<P>
+Lower-precision but faster predictions for the Sun and Moon
+can be made by calling
+sla_EARTH
+and
+sla_MOON.
+Both are single precision and accept dates in the form of
+year, day-in-year and fraction of day
+(starting from a calendar date you need to call
+sla_CLYD
+or
+sla_CALYD
+to get the required year and day).
+The
+sla_EARTH
+routine returns the heliocentric position and velocity
+of the Earth's centre for the mean equator and
+equinox of date.  The accuracy is better than 20,000&nbsp;km in position
+and 10&nbsp;metres per second in speed.
+The
+position and velocity of the Moon with respect to the
+Earth's centre for the mean equator and ecliptic of date
+can be obtained by calling
+sla_MOON.
+The positional accuracy is better than <IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img82.gif"
+ ALT="$30\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> in direction
+and 1000&nbsp;km in distance.
+<P>
+Approximate ephemerides for all the major planets
+can be generated by calling
+sla_PLANET
+or
+sla_RDPLAN.  These routines offer arcminute accuracy (much
+better for the inner planets and for Pluto) over a span of several
+millennia (but only <IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img317.gif"
+ ALT="$\pm100$"> years for Pluto).
+The routine
+sla_PLANET produces heliocentric position and
+velocity in the form of equatorial <IMG WIDTH="106" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img51.gif"
+ ALT="$[\,x,y,z,\dot{x},\dot{y},\dot{z}\,]$"> for the
+mean equator and equinox of J2000.  The vectors
+produced by
+sla_PLANET
+can be used in a variety of ways according to the
+requirements of the application concerned.  The routine
+sla_RDPLAN
+uses
+sla_PLANET
+and
+sla_DMOON
+to deal with the common case of predicting
+a planet's apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> and angular size as seen by a
+terrestrial observer.
+<P>
+Note that in predicting the position in the sky of a solar-system body
+it is necessary to allow for geocentric parallax.  This correction
+is <I>essential</I> in the case of the Moon, where the observer's
+position on the Earth can affect the Moon's <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> by up to
+<IMG WIDTH="18" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img318.gif"
+ ALT="$1^\circ$">.  The calculation can most conveniently be done by calling
+sla_PVOBS and subtracting the resulting 6-vector from the
+one produced by
+sla_DMOON, as is demonstrated by the following example:
+<P><PRE>
+      *  Demonstrate the size of the geocentric parallax correction
+      *  in the case of the Moon.  The test example is for the AAT,
+      *  before midnight, in summer, near first quarter.
+
+            IMPLICIT NONE
+            CHARACTER NAME*40,SH,SD
+            INTEGER J,I,IHMSF(4),IDMSF(4)
+            DOUBLE PRECISION SLONGW,SLAT,H,DJUTC,FDUTC,DJUT1,DJTT,STL,
+           :                 RMATN(3,3),PMM(6),PMT(6),RM,DM,PVO(6),TL
+            DOUBLE PRECISION sla_DTT,sla_GMST,sla_EQEQX,sla_DRANRM
+
+      *  Get AAT longitude and latitude in radians and height in metres
+            CALL sla_OBS(0,'AAT',NAME,SLONGW,SLAT,H)
+
+      *  UTC (1992 January 13, 11 13 59) to MJD
+            CALL sla_CLDJ(1992,1,13,DJUTC,J)
+            CALL sla_DTF2D(11,13,59.0D0,FDUTC,J)
+            DJUTC=DJUTC+FDUTC
+
+      *  UT1 (UT1-UTC value of -0.152 sec is from IERS Bulletin B)
+            DJUT1=DJUTC+(-0.152D0)/86400D0
+
+      *  TT
+            DJTT=DJUTC+sla_DTT(DJUTC)/86400D0
+
+      *  Local apparent sidereal time
+            STL=sla_GMST(DJUT1)-SLONGW+sla_EQEQX(DJTT)
+
+      *  Geocentric position/velocity of Moon (mean of date)
+            CALL sla_DMOON(DJTT,PMM)
+
+      *  Nutation to true equinox of date
+            CALL sla_NUT(DJTT,RMATN)
+            CALL sla_DMXV(RMATN,PMM,PMT)
+            CALL sla_DMXV(RMATN,PMM(4),PMT(4))
+
+      *  Report geocentric HA,Dec
+            CALL sla_DCC2S(PMT,RM,DM)
+            CALL sla_DR2TF(2,sla_DRANRM(STL-RM),SH,IHMSF)
+            CALL sla_DR2AF(1,DM,SD,IDMSF)
+            WRITE (*,'(1X,'' geocentric:'',2X,A,I2.2,2I3.2,''.'',I2.2,'//
+           :                              '1X,A,I2.2,2I3.2,''.'',I1)')
+           :                                                SH,IHMSF,SD,IDMSF
+
+      *  Geocentric position of observer (true equator and equinox of date)
+            CALL sla_PVOBS(SLAT,H,STL,PVO)
+
+      *  Place origin at observer
+            DO I=1,6
+               PMT(I)=PMT(I)-PVO(I)
+            END DO
+
+      *  Allow for planetary aberration
+            TL=499.004782D0*SQRT(PMT(1)**2+PMT(2)**2+PMT(3)**2)
+            DO I=1,3
+               PMT(I)=PMT(I)-TL*PMT(I+3)
+            END DO
+
+      *  Report topocentric HA,Dec
+            CALL sla_DCC2S(PMT,RM,DM)
+            CALL sla_DR2TF(2,sla_DRANRM(STL-RM),SH,IHMSF)
+            CALL sla_DR2AF(1,DM,SD,IDMSF)
+            WRITE (*,'(1X,''topocentric:'',2X,A,I2.2,2I3.2,''.'',I2.2,'//
+           :                              '1X,A,I2.2,2I3.2,''.'',I1)')
+           :                                                SH,IHMSF,SD,IDMSF
+            END
+</PRE>
+<P>
+The output produced is as follows:
+<P><PRE>
+       geocentric:  +03 06 55.59 +15 03 39.0
+      topocentric:  +03 09 23.79 +15 40 51.5
+</PRE>
+<P>(An easier but
+less instructive method of estimating the topocentric apparent place of the
+Moon is to call the routine
+sla_RDPLAN.)
+<P>
+As an example of using
+sla_PLANET,
+the following program estimates the geocentric separation
+between Venus and Jupiter during a close conjunction
+in 2BC, which is a star-of-Bethlehem candidate:
+<P><PRE>
+      *  Compute time and minimum geocentric apparent separation
+      *  between Venus and Jupiter during the close conjunction of 2 BC.
+
+            IMPLICIT NONE
+
+            DOUBLE PRECISION SEPMIN,DJD0,FD,DJD,DJDM,DF,PV(6),RMATP(3,3),
+           :                 PVM(6),PVE(6),TL,RV,DV,RJ,DJ,SEP
+            INTEGER IHOUR,IMIN,J,I,IHMIN,IMMIN
+            DOUBLE PRECISION sla_EPJ,sla_DSEP
+
+
+      *  Search for closest approach on the given day
+            DJD0=1720859.5D0
+            SEPMIN=1D10
+            DO IHOUR=20,22
+               DO IMIN=0,59
+                  CALL sla_DTF2D(IHOUR,IMIN,0D0,FD,J)
+
+      *        Julian date and MJD
+                  DJD=DJD0+FD
+                  DJDM=DJD-2400000.5D0
+
+      *        Earth to Moon (mean of date)
+                  CALL sla_DMOON(DJDM,PV)
+
+      *        Precess Moon position to J2000
+                  CALL sla_PRECL(sla_EPJ(DJDM),2000D0,RMATP)
+                  CALL sla_DMXV(RMATP,PV,PVM)
+
+      *        Sun to Earth-Moon Barycentre (mean J2000)
+                  CALL sla_PLANET(DJDM,3,PVE,J)
+
+      *        Correct from EMB to Earth
+                  DO I=1,3
+                     PV(I)=PVE(I)-0.012150581D0*PVM(I)
+                  END DO
+
+      *        Sun to Venus
+                  CALL sla_PLANET(DJDM,2,PV,J)
+
+      *        Earth to Venus
+                  DO I=1,6
+                     PV(I)=PV(I)-PVE(I)
+                  END DO
+
+      *        Light time to Venus (sec)
+                  TL=499.004782D0*SQRT((PV(1)-PVE(1))**2+
+           :                           (PV(2)-PVE(2))**2+
+           :                           (PV(3)-PVE(3))**2)
+
+      *        Extrapolate backwards in time by that much
+                  DO I=1,3
+                     PV(I)=PV(I)-TL*PV(I+3)
+                  END DO
+
+      *       To RA,Dec
+                  CALL sla_DCC2S(PV,RV,DV)
+
+      *        Same for Jupiter
+                  CALL sla_PLANET(DJDM,5,PV,J)
+                  DO I=1,6
+                     PV(I)=PV(I)-PVE(I)
+                  END DO
+                  TL=499.004782D0*SQRT((PV(1)-PVE(1))**2+
+           :                           (PV(2)-PVE(2))**2+
+           :                           (PV(3)-PVE(3))**2)
+                  DO I=1,3
+                     PV(I)=PV(I)-TL*PV(I+3)
+                  END DO
+                  CALL sla_DCC2S(PV,RJ,DJ)
+
+      *        Separation (arcsec)
+                  SEP=sla_DSEP(RV,DV,RJ,DJ)
+
+      *        Keep if smallest so far
+                  IF (SEP.LT.SEPMIN) THEN
+                     IHMIN=IHOUR
+                     IMMIN=IMIN
+                     SEPMIN=SEP
+                  END IF
+               END DO
+            END DO
+
+      *  Report
+            WRITE (*,'(1X,I2.2,'':'',I2.2,F6.1)') IHMIN,IMMIN,
+           :                                      206264.8062D0*SEPMIN
+
+            END
+</PRE>
+<P>
+The output produced (the Ephemeris Time on the day in question, and
+the closest approach in arcseconds) is as follows:
+<P><PRE>
+      21:19  33.7
+</PRE>
+<P>
+For comparison, accurate predictions based on the JPL DE102 ephemeris
+give a separation about <IMG WIDTH="17" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img319.gif"
+ ALT="$8\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> less than
+the above estimate, occurring about half an hour earlier
+(see <I>Sky and Telescope,</I> April&nbsp;1987, p357).
+<P>
+The following program demonstrates
+sla_RDPLAN.
+<PRE>
+      *  For a given date, time and geographical location, output
+      *  a table of planetary positions and diameters.
+
+            IMPLICIT NONE
+            CHARACTER PNAMES(0:9)*7,B*80,S
+            INTEGER I,NP,IY,J,IM,ID,IHMSF(4),IDMSF(4)
+            DOUBLE PRECISION R2AS,FD,DJM,ELONG,PHI,RA,DEC,DIAM
+            PARAMETER (R2AS=206264.80625D0)
+            DATA PNAMES / 'Sun','Mercury','Venus','Moon','Mars','Jupiter',
+           :              'Saturn','Uranus','Neptune', 'Pluto' /
+
+
+      *  Loop until 'end' typed
+            B=' '
+            DO WHILE (B.NE.'END'.AND.B.NE.'end')
+
+      *     Get date, time and observer's location
+               PRINT *,'Date? (Y,M,D, Gregorian)'
+               READ (*,'(A)') B
+               IF (B.NE.'END'.AND.B.NE.'end') THEN
+                  I=1
+                  CALL sla_INTIN(B,I,IY,J)
+                  CALL sla_INTIN(B,I,IM,J)
+                  CALL sla_INTIN(B,I,ID,J)
+                  PRINT *,'Time? (H,M,S, dynamical)'
+                  READ (*,'(A)') B
+                  I=1
+                  CALL sla_DAFIN(B,I,FD,J)
+                  FD=FD*2.3873241463784300365D0
+                  CALL sla_CLDJ(IY,IM,ID,DJM,J)
+                  DJM=DJM+FD
+                  PRINT *,'Longitude? (D,M,S, east +ve)'
+                  READ (*,'(A)') B
+                  I=1
+                  CALL sla_DAFIN(B,I,ELONG,J)
+                  PRINT *,'Latitude? (D,M,S, (geodetic)'
+                  READ (*,'(A)') B
+                  I=1
+                  CALL sla_DAFIN(B,I,PHI,J)
+
+      *        Loop planet by planet
+                  DO NP=0,8
+
+      *           Get RA,Dec and diameter
+                     CALL sla_RDPLAN(DJM,NP,ELONG,PHI,RA,DEC,DIAM)
+
+      *           One line of report
+                     CALL sla_DR2TF(2,RA,S,IHMSF)
+                     CALL sla_DR2AF(1,DEC,S,IDMSF)
+                     WRITE (*,
+           : '(1X,A,2X,3I3.2,''.'',I2.2,2X,A,I2.2,2I3.2,''.'',I1,F8.1)')
+           :                          PNAMES(NP),IHMSF,S,IDMSF,R2AS*DIAM
+
+      *           Next planet
+                  END DO
+                  PRINT *,' '
+               END IF
+
+      *     Next case
+            END DO
+
+            END
+</PRE>
+Entering the following data (for 1927&nbsp;June&nbsp;29 at <IMG WIDTH="49" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img320.gif"
+ ALT="$5^{\rm h}\,25^{\rm m}$">&nbsp;ET
+and the position of Preston, UK.):
+<PRE>
+      1927 6 29
+      5 25
+      -2 42
+      53 46
+</PRE>
+produces the following report:
+<PRE>
+      Sun       06 28 14.03  +23 17 17.5  1887.8
+      Mercury   08 08 58.62  +19 20 57.3     9.3
+      Venus     09 38 53.64  +15 35 32.9    22.8
+      Moon      06 28 18.30  +23 18 37.3  1903.9
+      Mars      09 06 49.34  +17 52 26.7     4.0
+      Jupiter   00 11 12.06  -00 10 57.5    41.1
+      Saturn    16 01 43.34  -18 36 55.9    18.2
+      Uranus    00 13 33.53  +00 39 36.0     3.5
+      Neptune   09 49 35.75  +13 38 40.8     2.2
+      Pluto     07 05 29.50  +21 25 04.2      .1
+</PRE>
+Inspection of the Sun and Moon data reveals that
+a total solar eclipse is in progress.
+<P>
+SLALIB also provides for the case where orbital elements (with respect
+to the J2000 equinox and ecliptic)
+are available.  This allows predictions to be made for minor-planets and
+(if you ignore non-gravitational effects)
+comets.  Furthermore, if major-planet elements for an epoch close to the date
+in question are available, more accurate predictions can be made than
+are offered by
+sla_RDPLAN and
+sla_PLANET.
+<P>
+The SLALIB planetary-prediction
+routines that work with orbital elements are
+sla_PLANTE (the orbital-elements equivalent of
+sla_RDPLAN), which predicts the topocentric <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">, and
+sla_PLANEL (the orbital-elements equivalent of
+sla_PLANET), which predicts the heliocentric <IMG WIDTH="106" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img51.gif"
+ ALT="$[\,x,y,z,\dot{x},\dot{y},\dot{z}\,]$"> with respect to the
+J2000 equinox and equator.  In addition, the routine
+sla_PV2EL does the inverse of
+sla_PLANEL, transforming <IMG WIDTH="106" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img51.gif"
+ ALT="$[\,x,y,z,\dot{x},\dot{y},\dot{z}\,]$"> into <I>osculating elements.</I>
+<P>
+Osculating elements describe the unperturbed 2-body orbit.  This is
+a good approximation to the actual orbit for a few weeks either
+side of the specified epoch, outside which perturbations due to
+the other bodies of the Solar System lead to
+increasing errors.  Given a minor planet's osculating elements for
+a particular date, predictions for a date even just
+100 days earlier or later
+are likely to be in error by several arcseconds.
+These errors can
+be reduced if new elements are generated which take account of
+the perturbations of the major planets, and this is what the routine
+sla_PERTEL does.  Once
+sla_PERTEL has been called, to provide osculating elements
+close to the required date, the elements can be passed to
+sla_PLANEL or
+sla_PLANTE in the normal way.  Predictions of arcsecond accuracy
+over a span of a decade or more are available using this
+technique.
+<P>
+Three different combinations of orbital elements are
+provided for, matching the usual conventions
+for major planets, minor planets and
+comets respectively.  The choice is made through the
+argument <TT>JFORM</TT>:
+<BR>
+<P><TABLE CELLPADDING=3 BORDER="1">
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><TT>JFORM=1</TT></TD>
+<TD ALIGN="CENTER" NOWRAP><TT>JFORM=2</TT></TD>
+<TD ALIGN="CENTER" NOWRAP><TT>JFORM=3</TT></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><I>t<SUB>0</SUB></I></TD>
+<TD ALIGN="CENTER" NOWRAP><I>t<SUB>0</SUB></I></TD>
+<TD ALIGN="CENTER" NOWRAP><I>T</I></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><I>i</I></TD>
+<TD ALIGN="CENTER" NOWRAP><I>i</I></TD>
+<TD ALIGN="CENTER" NOWRAP><I>i</I></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><IMG WIDTH="16" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img100.gif"
+ ALT="$\varpi$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$"></TD>
+<TD ALIGN="CENTER" NOWRAP><IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$"></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><I>a</I></TD>
+<TD ALIGN="CENTER" NOWRAP><I>a</I></TD>
+<TD ALIGN="CENTER" NOWRAP><I>q</I></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><I>e</I></TD>
+<TD ALIGN="CENTER" NOWRAP><I>e</I></TD>
+<TD ALIGN="CENTER" NOWRAP><I>e</I></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><I>L</I></TD>
+<TD ALIGN="CENTER" NOWRAP><I>M</I></TD>
+<TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP><I>n</I></TD>
+<TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+<TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+</TR>
+</TABLE>
+<BR>
+<BR>
+<BR>
+<BR>
+<BR>
+<BR>
+The symbols have the following meanings:
+<PRE><TT>
+		 <I>t<SUB>0</SUB></I> epoch at which the elements were correct
+		 <I>T</I> epoch of perihelion passage
+		 <I>i</I> inclination of the orbit
+		 <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> longitude of the ascending node
+		 <IMG WIDTH="16" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img100.gif"
+ ALT="$\varpi$"> longitude of perihelion (<IMG WIDTH="81" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img321.gif"
+ ALT="$\varpi = \Omega + \omega$">)		 <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$"> argument of perihelion
+		 <I>a</I> semi-major axis of the orbital ellipse
+		 <I>q</I> perihelion distance
+		 <I>e</I> orbital eccentricity
+		 <I>L</I> mean longitude (<IMG WIDTH="87" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img322.gif"
+ ALT="$L = \varpi + M$">)		 <I>M</I> mean anomaly
+		 <I>n</I> mean motion 
+</TT></PRE>
+<P>
+The mean motion, <I>n</I>, tells sla_PLANEL the mass of the planet.
+If it is not available, it should be claculated
+from <I>n<SUP>2</SUP></I> <I>a<SUP>3</SUP></I> = <I>k<SUP>2</SUP></I> (1+<I>m</I>), where <I>k</I> = 0.01720209895 and
+m is the mass of the planet (<IMG WIDTH="59" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img323.gif"
+ ALT="$M_\odot = 1$">); <I>a</I> is in AU.
+<P>
+Conventional elements are not the only way of specifying an orbit.
+The <IMG WIDTH="106" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img51.gif"
+ ALT="$[\,x,y,z,\dot{x},\dot{y},\dot{z}\,]$"> state vector is an equally valid specification,
+and the so-called <I>method of universal variables</I> allows
+orbital calculations to be made directly, bypassing angular
+quantities and avoiding Kepler's Equation.  The universal-variables
+approach has various advantages, including better handling of
+near-parabolic cases and greater efficiency.
+SLALIB uses universal variables for its internal
+calculations and also offers a number of routines which
+applications can call.
+<P>
+The universal elements are the <IMG WIDTH="106" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img51.gif"
+ ALT="$[\,x,y,z,\dot{x},\dot{y},\dot{z}\,]$"> and its epoch, plus the mass
+of the body.  The SLALIB routines supplement these elements with
+certain redundant values in order to
+avoid unnecessary recomputation when the elements are next used.
+<P>
+The routines
+sla_EL2UE and
+sla_UE2EL transform conventional elements into the
+universal form and <I>vice versa.</I>
+The routine
+sla_PV2UE takes an <IMG WIDTH="106" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img51.gif"
+ ALT="$[\,x,y,z,\dot{x},\dot{y},\dot{z}\,]$"> and forms the set of universal
+elements;
+sla_UE2PV takes a set of universal elements and predicts the <IMG WIDTH="106" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img51.gif"
+ ALT="$[\,x,y,z,\dot{x},\dot{y},\dot{z}\,]$"> for a specified epoch.
+The routine
+sla_PERTUE provides updated universal elements,
+taking into account perturbations from the major planets.
+<P>
+<BR> <HR>
+<A NAME="tex2html2693" HREF="node225.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2691" HREF="node197.html">
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+<A NAME="tex2html2685" HREF="node223.html">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2694" HREF="node225.html">Radial Velocity and Light-Time Corrections</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2692" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2686" HREF="node223.html">Geocentric Coordinates</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node225.html b/src/slalib/sun67.htx/node225.html
new file mode 100644
index 0000000..ce716c7
--- /dev/null
+++ b/src/slalib/sun67.htx/node225.html
@@ -0,0 +1,143 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Radial Velocity and Light-Time Corrections</TITLE>
+<META NAME="description" CONTENT="Radial Velocity and Light-Time Corrections">
+<META NAME="keywords" CONTENT="sun67">
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+<A NAME="tex2html2695" HREF="node224.html">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2704" HREF="node226.html">Focal-Plane Astrometry</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2702" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2696" HREF="node224.html">Ephemerides</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000519000000000000000">
+Radial Velocity and Light-Time Corrections</A>
+</H2>
+When publishing high-resolution spectral observations
+it is necessary to refer them to a specified standard of rest.
+This involves knowing the component in the direction of the
+source of the velocity of the observer.  SLALIB provides a number
+of routines for this purpose, allowing observations to be
+referred to the Earth's centre, the Sun, a Local Standard of Rest
+(either dynamical or kinematical), the centre of the Galaxy, and
+the mean motion of the Local Group.
+<P>
+The routine
+sla_RVEROT
+corrects for the diurnal rotation of
+the observer around the Earth's axis.  This is always less than 0.5&nbsp;km/s.
+<P>
+No specific routine is provided to correct a radial velocity
+from geocentric to heliocentric, but this can easily be done by calling
+sla_EVP
+as follows (array declarations <I>etc</I>. omitted):
+<P><PRE>
+             :
+      *  Star vector, J2000
+            CALL sla_DCS2C(RM,DM,V)
+
+      *  Earth/Sun velocity and position, J2000
+            CALL sla_EVP(TDB,2000D0,DVB,DPB,DVH,DPH)
+
+      *  Radial velocity correction due to Earth orbit (km/s)
+            VCORB = -sla_DVDV(V,DVH)*149.597870D6
+             :
+</PRE>
+<P>
+The maximum value of this correction is the Earth's orbital speed
+of about 30&nbsp;km/s.  A related routine,
+sla_ECOR,
+computes the light-time correction with respect to the Sun.  It
+would be used when reducing observations of a rapid variable-star
+for instance.
+Note, however, that the accuracy objectives for pulsar work are
+beyond the scope of these SLALIB routines, and even the superior
+sla_EVP
+routine is unsuitable for arrival-time calculations of better
+than 25&nbsp;millisecond accuracy.
+<P>
+To remove the intrinsic <IMG WIDTH="36" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img324.gif"
+ ALT="$\sim20$">&nbsp;km/s motion of the Sun relative
+to other stars in the solar neighbourhood,
+a velocity correction to a
+<I>local standard of rest</I> (LSR) is required.  There are
+opportunities for mistakes here.  There are two sorts of LSR,
+<I>dynamical</I> and <I>kinematical</I>, and
+multiple definitions exist for the latter.  The
+dynamical LSR is a point near the Sun which is in a circular
+orbit around the Galactic centre;  the Sun has a ``peculiar''
+motion relative to the dynamical LSR.  A kinematical LSR is
+the mean standard of rest of specified star catalogues or stellar
+populations, and its precise definition depends on which
+catalogues or populations were used and how the analysis was
+carried out.  The Sun's motion with respect to a kinematical
+LSR is called the ``standard'' solar motion.  Radial
+velocity corrections to the dynamical LSR are produced by the routine
+sla_RVLSRD
+and to the adopted kinematical LSR by
+sla_RVLSRK.
+See the individual specifications for these routines for the
+precise definition of the LSR in each case.
+<P>
+For extragalactic sources, the centre of the Galaxy can be used as
+a standard of rest.  The radial velocity correction from the
+dynamical LSR to the Galactic centre can be obtained by calling
+sla_RVGALC.
+Its maximum value is 220&nbsp;km/s.
+<P>
+For very distant sources it is appropriate to work relative
+to the mean motion of the Local Group.  The routine for
+computing the radial velocity correction in this case is
+sla_RVLG.
+Note that in this case the correction is with respect to the
+dynamical LSR, not the Galactic centre as might be expected.
+This conforms to the IAU definition, and confers immunity from
+revisions of the Galactic rotation speed.
+<P>
+<BR> <HR>
+<A NAME="tex2html2703" HREF="node226.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html2701" HREF="node197.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html2695" HREF="node224.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2704" HREF="node226.html">Focal-Plane Astrometry</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2702" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2696" HREF="node224.html">Ephemerides</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node226.html b/src/slalib/sun67.htx/node226.html
new file mode 100644
index 0000000..41baa89
--- /dev/null
+++ b/src/slalib/sun67.htx/node226.html
@@ -0,0 +1,212 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Focal-Plane Astrometry</TITLE>
+<META NAME="description" CONTENT="Focal-Plane Astrometry">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
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+<A NAME="tex2html2705" HREF="node225.html">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2714" HREF="node227.html">Numerical Methods</A>
+<BR>
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+<BR>
+<B> Previous:</B> <A NAME="tex2html2706" HREF="node225.html">Radial Velocity and Light-Time Corrections</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000520000000000000000">
+Focal-Plane Astrometry</A>
+</H2>
+The relationship between the position of a star image in
+the focal plane of a telescope and the star's celestial
+coordinates is usually described in terms of the <I>tangent plane</I>
+or <I>gnomonic</I> projection.  This is the projection produced
+by a pin-hole camera and is a good approximation to the projection
+geometry of a traditional large <I>f</I>-ratio astrographic refractor.
+SLALIB includes a group of routines which transform
+star positions between their observed places on the celestial
+sphere and their <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> coordinates in the tangent plane.  The
+spherical coordinate system does not have to be <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> but
+usually is.  The so-called <I>standard coordinates</I> of a star
+are the tangent plane <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$">, in radians, with respect to an origin
+at the tangent point, with the <I>y</I>-axis pointing north and
+the <I>x</I>-axis pointing east (in the direction of increasing <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$">).
+The factor relating the standard coordinates to
+the actual <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> coordinates in, say, millimetres is simply
+the focal length of the telescope.
+<P>
+Given the <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> of the <I>plate centre</I> (the tangent point)
+and the <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> of a star within the field, the standard
+coordinates can be determined by calling
+sla_S2TP
+(single precision) or
+sla_DS2TP
+(double precision).  The reverse transformation, where the
+<IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> is known and we wish to find the <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">, is carried out by calling
+sla_TP2S
+or
+sla_DTP2S.
+Occasionally we know the both the <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> and the <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> of a 
+star and need to deduce the <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> of the tangent point;  
+this can be done by calling
+sla_TPS2C
+or
+sla_DTPS2C.
+(All of these transformations apply not just to <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> but to
+other spherical coordinate systems, of course.)
+Equivalent (and faster)
+routines are provided which work directly in <IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$"> instead of
+spherical coordinates:
+sla_V2TP and
+sla_DV2TP,
+sla_TP2V and
+sla_DTP2V,
+sla_TPV2C and
+sla_DTPV2C.
+<P>
+Even at the best of times, the tangent plane projection is merely an
+approximation.  Some telescopes and cameras exhibit considerable pincushion
+or barrel distortion and some have a curved focal surface.
+For example, neither Schmidt cameras nor (especially)
+large reflecting telescopes with wide-field corrector lenses
+are adequately modelled by tangent-plane geometry.  In such
+cases, however, it is still possible to do most of the work
+using the (mathematically convenient) tangent-plane
+projection by inserting an extra step which applies or
+removes the distortion peculiar to the system concerned.
+A simple <I>r<SUB>1</SUB></I>=<I>r<SUB>0</SUB></I>(1+<I>Kr<SUB>0</SUB></I><SUP>2</SUP>) law works well in the
+majority of cases; <I>r<SUB>0</SUB></I> is the radial distance in the
+tangent plane, <I>r<SUB>1</SUB></I> is the radial distance after adding
+the distortion, and <I>K</I> is a constant which depends on the
+telescope (<IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img298.gif"
+ ALT="$\theta$"> is unaffected).  The routine
+sla_PCD
+applies the distortion to an <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> and
+sla_UNPCD
+removes it.  For <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> in radians, <I>K</I> values range from -1/3 for the
+tiny amount of barrel distortion in Schmidt geometry to several
+hundred for the serious pincushion distortion
+produced by wide-field correctors in big reflecting telescopes
+(the AAT prime focus triplet corrector is about <I>K</I>=+178.6).
+<P>
+SLALIB includes a group of routines which can be put together
+to build a simple plate-reduction program.  The heart of the group is
+sla_FITXY,
+which fits a linear model to relate two sets of <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> coordinates,
+in the case of a plate reduction the measured positions of the
+images of a set of
+reference stars and the standard
+coordinates derived from their catalogue positions.  The
+model is of the form:
+
+<P ALIGN="CENTER">
+<I>x</I><SUB><I>p</I></SUB> = <I>a</I> + <I>bx</I><SUB><I>m</I></SUB> + <I>cy</I><SUB><I>m</I></SUB>
+</P>
+
+<P ALIGN="CENTER">
+<I>y</I><SUB><I>p</I></SUB> = <I>d</I> + <I>ex</I><SUB><I>m</I></SUB> + <I>fy</I><SUB><I>m</I></SUB>
+</P>
+<P>
+where the <I>p</I> subscript indicates ``predicted'' coordinates
+(the model's approximation to the ideal ``expected'' coordinates) and the
+<I>m</I> subscript indicates ``measured coordinates''.  The
+six coefficients <I>a-f</I> can optionally be
+constrained to represent a ``solid body rotation'' free of
+any squash or shear distortions.  Without this constraint
+the model can, to some extent, accommodate effects like refraction,
+allowing mean places to be used directly and
+avoiding the extra complications of a
+full mean-apparent-observed transformation for each star.
+Having obtained the linear model,
+sla_PXY
+can be used to process the set of measured and expected
+coordinates, giving the predicted coordinates and determining
+the RMS residuals in <I>x</I> and <I>y</I>.
+The routine
+sla_XY2XY
+transforms one <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> into another using the linear model.  A model
+can be inverted by calling
+sla_INVF,
+and decomposed into zero points, scales, <I>x</I>/<I>y</I> nonperpendicularity
+and orientation by calling
+sla_DCMPF.
+<P>
+<BR> <HR>
+<A NAME="tex2html2713" HREF="node227.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html2714" HREF="node227.html">Numerical Methods</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html2712" HREF="node197.html">EXPLANATION AND EXAMPLES</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html2706" HREF="node225.html">Radial Velocity and Light-Time Corrections</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node227.html b/src/slalib/sun67.htx/node227.html
new file mode 100644
index 0000000..9ed563a
--- /dev/null
+++ b/src/slalib/sun67.htx/node227.html
@@ -0,0 +1,230 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Numerical Methods</TITLE>
+<META NAME="description" CONTENT="Numerical Methods">
+<META NAME="keywords" CONTENT="sun67">
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+<META NAME="distribution" CONTENT="global">
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+<H2><A NAME="SECTION000521000000000000000">
+Numerical Methods</A>
+</H2>
+SLALIB contains a small number of simple, general-purpose
+numerical-methods routines.  They have no specific
+connection with positional astronomy but have proved useful in
+applications to do with simulation and fitting.
+<P>
+At the heart of many simulation programs is the generation of
+pseudo-random numbers, evenly distributed in a given range:
+sla_RANDOM
+does this.  Pseudo-random normal deviates, or ``Gaussian
+residuals'', are often required to simulate noise and
+can be generated by means of the function
+sla_GRESID.
+Neither routine will pass super-sophisticated
+statistical tests, but they work adequately for most
+practical purposes and avoid the need to call non-standard
+library routines peculiar to one sort of computer.
+<P>
+Applications which perform a least-squares fit using a traditional
+normal-equations methods can accomplish the required matrix-inversion
+by calling either
+sla_SMAT
+(single precision) or
+sla_DMAT
+(double).  A generally better way to perform such fits is
+to use singular value decomposition.  SLALIB provides a routine
+to do the decomposition itself,
+sla_SVD,
+and two routines to use the results:
+sla_SVDSOL
+generates the solution, and
+sla_SVDCOV
+produces the covariance matrix.
+A simple demonstration of the use of the SLALIB SVD
+routines is given below.  It generates 500 simulated data
+points and fits them to a model which has 4 unknown coefficients.
+(The arrays in the example are sized to accept up to 1000
+points and 20 unknowns.)  The model is:
+
+<P ALIGN="CENTER">
+<I>y</I> = <I>C<SUB>1</SUB></I> +<I>C<SUB>2</SUB>x</I> +<I>C<SUB>3</SUB>sin</I><I>x</I> +<I>C<SUB>4</SUB>cos</I><I>x</I> 
+</P>
+The test values for the four coefficients are
+<IMG WIDTH="79" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img325.gif"
+ ALT="$C_1\!=\!+50.0$">,<IMG WIDTH="71" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img326.gif"
+ ALT="$C_2\!=\!-2.0$">,<IMG WIDTH="79" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img327.gif"
+ ALT="$C_3\!=\!-10.0$"> and
+<IMG WIDTH="79" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img328.gif"
+ ALT="$C_4\!=\!+25.0$">.Gaussian noise, <IMG WIDTH="55" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img329.gif"
+ ALT="$\sigma=5.0$">, is added to each ``observation''.
+<P><PRE>
+            IMPLICIT NONE
+
+      *  Sizes of arrays, physical and logical
+            INTEGER MP,NP,NC,M,N
+            PARAMETER (MP=1000,NP=10,NC=20,M=500,N=4)
+
+      *  The unknowns we are going to solve for
+            DOUBLE PRECISION C1,C2,C3,C4
+            PARAMETER (C1=50D0,C2=-2D0,C3=-10D0,C4=25D0)
+
+      *  Arrays
+            DOUBLE PRECISION A(MP,NP),W(NP),V(NP,NP),
+           :                 WORK(NP),B(MP),X(NP),CVM(NC,NC)
+
+            DOUBLE PRECISION VAL,BF1,BF2,BF3,BF4,SD2,D,VAR
+            REAL sla_GRESID
+            INTEGER I,J
+
+      *  Fill the design matrix
+            DO I=1,M
+
+      *     Dummy independent variable
+               VAL=DBLE(I)/10D0
+
+      *     The basis functions
+               BF1=1D0
+               BF2=VAL
+               BF3=SIN(VAL)
+               BF4=COS(VAL)
+
+      *     The observed value, including deliberate Gaussian noise
+               B(I)=C1*BF1+C2*BF2+C3*BF3+C4*BF4+DBLE(sla_GRESID(5.0))
+
+      *     Fill one row of the design matrix
+               A(I,1)=BF1
+               A(I,2)=BF2
+               A(I,3)=BF3
+               A(I,4)=BF4
+            END DO
+
+      *  Factorize the design matrix, solve and generate covariance matrix
+            CALL sla_SVD(M,N,MP,NP,A,W,V,WORK,J)
+            CALL sla_SVDSOL(M,N,MP,NP,B,A,W,V,WORK,X)
+            CALL sla_SVDCOV(N,NP,NC,W,V,WORK,CVM)
+
+      *  Compute the variance
+            SD2=0D0
+            DO I=1,M
+               VAL=DBLE(I)/10D0
+               BF1=1D0
+               BF2=VAL
+               BF3=SIN(VAL)
+               BF4=COS(VAL)
+               D=B(I)-(X(1)*BF1+X(2)*BF2+X(3)*BF3+X(4)*BF4)
+               SD2=SD2+D*D
+            END DO
+            VAR=SD2/DBLE(M)
+
+      *  Report the RMS and the solution
+            WRITE (*,'(1X,''RMS ='',F5.2/)') SQRT(VAR)
+            DO I=1,N
+               WRITE (*,'(1X,''C'',I1,'' ='',F7.3,'' +/-'',F6.3)')
+           :                                         I,X(I),SQRT(VAR*CVM(I,I))
+            END DO
+            END
+</PRE>
+<P>
+The program produces the following output:
+<P><PRE>
+            RMS = 4.88
+
+            C1 = 50.192 +/- 0.439
+            C2 = -2.002 +/- 0.015
+            C3 = -9.771 +/- 0.310
+            C4 = 25.275 +/- 0.310
+</PRE>
+<P>
+In this above example, essentially
+identical results would be obtained if the more
+commonplace normal-equations method had been used, and the large
+<IMG WIDTH="72" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img330.gif"
+ ALT="$1000\times20$"> array would have been avoided.  However, the SVD method
+comes into its own when the opportunity is taken to edit the W-matrix
+(the so-called ``singular values'') in order to control
+possible ill-conditioning.  The procedure involves replacing with
+zeroes any W-elements smaller than a nominated value, for example
+0.001 times the largest W-element.  Small W-elements indicate
+ill-conditioning, which in the case of the normal-equations
+method would produce spurious large coefficient values and
+possible arithmetic overflows.  Using SVD, the effect on the solution
+of setting suspiciously small W-elements to zero is to restrain
+the offending coefficients from moving very far.  The
+fact that action was taken can be reported to show the program user that
+something is amiss.  Furthermore, if element W(J) was set to zero,
+the row numbers of the two biggest elements in the Jth column of the
+V-matrix identify the pair of solution coefficients that are
+dependent.
+<P>
+A more detailed description of SVD and its use in least-squares
+problems would be out of place here, and the reader is urged
+to refer to the relevant sections of the book <I>Numerical Recipes</I>
+(Press <I>et al.</I>, Cambridge University Press, 1987).
+<P>
+The routines
+sla_COMBN
+and
+sla_PERMUT
+are useful for problems which involve combinations (different subsets)
+and permutations (different orders).
+Both return the next in a sequence of results, cycling through all the
+possible results as the routine is called repeatedly.
+<P>
+<BR>
+<P>
+<BR> <HR>
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+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
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+<H1><A NAME="SECTION00060000000000000000">
+SUMMARY OF CALLS</A>
+</H1>
+The basic trigonometrical and numerical facilities are supplied in both single
+and double precision versions.
+Most of the more esoteric position and time routines use double precision
+arguments only, even in cases where single precision would normally be adequate
+in practice.
+Certain routines with modest accuracy objectives are supplied in
+single precision versions only.
+In the calling sequences which follow, no attempt has been made
+to distinguish between single and double precision argument names,
+and frequently the same name is used on different occasions to
+mean different things.
+However, none of the routines uses a mixture of single and
+double precision arguments;  each routine is either wholly
+single precision or wholly double precision.
+<P>
+In the classified list, below,
+<I>subroutine</I> subprograms are those whose names and argument lists
+are preceded by `CALL', whereas <I>function</I> subprograms are
+those beginning `R=' (when the result is REAL) or `D=' (when
+the result is DOUBLE&nbsp;PRECISION).
+<P>
+The list is, of course, merely for quick reference;  inexperienced
+users <B>must</B> refer to the detailed specifications given later.
+In particular, <B>don't guess</B> whether arguments are single or
+double precision; the result could be a program that happens to
+works on one sort of machine but not on another.
+<P>
+<BR><BIG><B>String Decoding</BIG></B><UL>
+<LI> CALL sla_INTIN (STRING, NSTRT, IRESLT, JFLAG)
+<BR>
+Convert free-format string into integer
+<LI> CALL sla_FLOTIN (STRING, NSTRT, RESLT, JFLAG)
+<BR>
+CALL sla_DFLTIN (STRING, NSTRT, DRESLT, JFLAG)
+<BR>
+Convert free-format string into floating-point number
+<LI> CALL sla_AFIN (STRING, NSTRT, RESLT, JFLAG)
+<BR>
+CALL sla_DAFIN (STRING, NSTRT, DRESLT, JFLAG)
+<BR>
+Convert free-format string from deg,arcmin,arcsec to radians</UL>
+<BR><BIG><B>Sexagesimal Conversions</BIG></B><UL>
+<LI> CALL sla_CTF2D (IHOUR, IMIN, SEC, DAYS, J)
+<BR>
+CALL sla_DTF2D (IHOUR, IMIN, SEC, DAYS, J)
+<BR>
+Hours, minutes, seconds to days
+<LI> CALL sla_CD2TF (NDP, DAYS, SIGN, IHMSF)
+<BR>
+CALL sla_DD2TF (NDP, DAYS, SIGN, IHMSF)
+<BR>
+Days to hours, minutes, seconds
+<LI> CALL sla_CTF2R (IHOUR, IMIN, SEC, RAD, J)
+<BR>
+CALL sla_DTF2R (IHOUR, IMIN, SEC, RAD, J)
+<BR>
+Hours, minutes, seconds to radians
+<LI> CALL sla_CR2TF (NDP, ANGLE, SIGN, IHMSF)
+<BR>
+CALL sla_DR2TF (NDP, ANGLE, SIGN, IHMSF)
+<BR>
+Radians to hours, minutes, seconds
+<LI> CALL sla_CAF2R (IDEG, IAMIN, ASEC, RAD, J)
+<BR>
+CALL sla_DAF2R (IDEG, IAMIN, ASEC, RAD, J)
+<BR>
+Degrees, arcminutes, arcseconds to radians
+<LI> CALL sla_CR2AF (NDP, ANGLE, SIGN, IDMSF)
+<BR>
+CALL sla_DR2AF (NDP, ANGLE, SIGN, IDMSF)
+<BR>
+Radians to degrees, arcminutes, arcseconds</UL>
+<BR><BIG><B>Angles, Vectors and Rotation Matrices</BIG></B><UL>
+<LI> R&nbsp;=&nbsp;sla_RANGE (ANGLE)
+<BR>
+D&nbsp;=&nbsp;sla_DRANGE (ANGLE)
+<BR>
+Normalize angle into range <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$"><LI> R&nbsp;=&nbsp;sla_RANORM (ANGLE)
+<BR>
+D&nbsp;=&nbsp;sla_DRANRM (ANGLE)
+<BR>
+Normalize angle into range <IMG WIDTH="43" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img66.gif"
+ ALT="$0\!-\!2\pi$"><LI> CALL sla_CS2C (A, B, V)
+<BR>
+CALL sla_DCS2C (A, B, V)
+<BR>
+Spherical coordinates to <IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$"><LI> CALL sla_CC2S (V, A, B)
+<BR>
+CALL sla_DCC2S (V, A, B)
+<BR>
+   <IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$"> to spherical coordinates
+<LI> R&nbsp;=&nbsp;sla_VDV (VA, VB)
+<BR>
+D&nbsp;=&nbsp;sla_DVDV (VA, VB)
+<BR>
+Scalar product of two 3-vectors
+<LI> CALL sla_VXV (VA, VB, VC)
+<BR>
+CALL sla_DVXV (VA, VB, VC)
+<BR>
+Vector product of two 3-vectors
+<LI> CALL sla_VN (V, UV, VM)
+<BR>
+CALL sla_DVN (V, UV, VM)
+<BR>
+Normalize a 3-vector also giving the modulus
+<LI> R&nbsp;=&nbsp;sla_SEP (A1, B1, A2, B2)
+<BR>
+D&nbsp;=&nbsp;sla_DSEP (A1, B1, A2, B2)
+<BR>
+Angle between two points on a sphere
+<LI> R&nbsp;=&nbsp;sla_BEAR (A1, B1, A2, B2)
+<BR>
+D&nbsp;=&nbsp;sla_DBEAR (A1, B1, A2, B2)
+<BR>
+Direction of one point on a sphere seen from another
+<LI> R&nbsp;=&nbsp;sla_PAV (V1, V2)
+<BR>
+D&nbsp;=&nbsp;sla_DPAV (V1, V2)
+<BR>
+Position-angle of one <IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$"> with respect to another
+<LI> CALL sla_EULER (ORDER, PHI, THETA, PSI, RMAT)
+<BR>
+CALL sla_DEULER (ORDER, PHI, THETA, PSI, RMAT)
+<BR>
+Form rotation matrix from three Euler angles
+<LI> CALL sla_AV2M (AXVEC, RMAT)
+<BR>
+CALL sla_DAV2M (AXVEC, RMAT)
+<BR>
+Form rotation matrix from axial vector
+<LI> CALL sla_M2AV (RMAT, AXVEC)
+<BR>
+CALL sla_DM2AV (RMAT, AXVEC)
+<BR>
+Determine axial vector from rotation matrix
+<LI> CALL sla_MXV (RM, VA, VB)
+<BR>
+CALL sla_DMXV (DM, VA, VB)
+<BR>
+Rotate vector forwards
+<LI> CALL sla_IMXV (RM, VA, VB)
+<BR>
+CALL sla_DIMXV (DM, VA, VB)
+<BR>
+Rotate vector backwards
+<LI> CALL sla_MXM (A, B, C)
+<BR>
+CALL sla_DMXM (A, B, C)
+<BR>
+Product of two 3x3 matrices
+<LI> CALL sla_CS2C6 (A, B, R, AD, BD, RD, V)
+<BR>
+CALL sla_DS2C6 (A, B, R, AD, BD, RD, V)
+<BR>
+Conversion of position and velocity in spherical
+     coordinates to Cartesian coordinates
+<LI> CALL sla_CC62S (V, A, B, R, AD, BD, RD)
+<BR>
+CALL sla_DC62S (V, A, B, R, AD, BD, RD)
+<BR>
+Conversion of position and velocity in Cartesian
+     coordinates to spherical coordinates</UL>
+<BR><BIG><B>Calendars</BIG></B><UL>
+<LI> CALL sla_CLDJ (IY, IM, ID, DJM, J)
+<BR>
+Gregorian Calendar to Modified Julian Date
+<LI> CALL sla_CALDJ (IY, IM, ID, DJM, J)
+<BR>
+Gregorian Calendar to Modified Julian Date,
+     permitting century default
+<LI> CALL sla_DJCAL (NDP, DJM, IYMDF, J)
+<BR>
+Modified Julian Date to Gregorian Calendar,
+     in a form convenient for formatted output
+<LI> CALL sla_DJCL (DJM, IY, IM, ID, FD, J)
+<BR>
+Modified Julian Date to Gregorian Year, Month, Day, Fraction
+<LI> CALL sla_CALYD (IY, IM, ID, NY, ND, J)
+<BR>
+Calendar to year and day in year, permitting century default
+<LI> CALL sla_CLYD (IY, IM, ID, NY, ND, J)
+<BR>
+Calendar to year and day in year
+<LI> D&nbsp;=&nbsp;sla_EPB (DATE)
+<BR>
+Modified Julian Date to Besselian Epoch
+<LI> D&nbsp;=&nbsp;sla_EPB2D (EPB)
+<BR>
+Besselian Epoch to Modified Julian Date
+<LI> D&nbsp;=&nbsp;sla_EPJ (DATE)
+<BR>
+Modified Julian Date to Julian Epoch
+<LI> D&nbsp;=&nbsp;sla_EPJ2D (EPJ)
+<BR>
+Julian Epoch to Modified Julian Date</UL>
+<BR><BIG><B>Timescales</BIG></B><UL>
+<LI> D&nbsp;=&nbsp;sla_GMST (UT1)
+<BR>
+Conversion from Universal Time to sidereal time
+<LI> D&nbsp;=&nbsp;sla_GMSTA (DATE, UT1)
+<BR>
+Conversion from Universal Time to sidereal time, rounding errors minimized
+<LI> D&nbsp;=&nbsp;sla_EQEQX (DATE)
+<BR>
+Equation of the equinoxes
+<LI> D&nbsp;=&nbsp;sla_DAT (DJU)
+<BR>
+Offset of Atomic Time from Coordinated Universal Time: TAI-UTC
+<LI> D&nbsp;=&nbsp;sla_DT (EPOCH)
+<BR>
+Approximate offset between dynamical time and universal time
+<LI> D&nbsp;=&nbsp;sla_DTT (DJU)
+<BR>
+Offset of Terrestrial Time from Coordinated Universal Time: TT-UTC
+<LI> D&nbsp;=&nbsp;sla_RCC (TDB, UT1, WL, U, V)
+<BR>
+Relativistic clock correction: TDB-TT</UL>
+<BR><BIG><B>Precession and Nutation</BIG></B><UL>
+<LI> CALL sla_NUT (DATE, RMATN)
+<BR>
+Nutation matrix
+<LI> CALL sla_NUTC (DATE, DPSI, DEPS, EPS0)
+<BR>
+Longitude and obliquity components of nutation, and
+     mean obliquity
+<LI> CALL sla_PREC (EP0, EP1, RMATP)
+<BR>
+Precession matrix (IAU)
+<LI> CALL sla_PRECL (EP0, EP1, RMATP)
+<BR>
+Precession matrix (suitable for long periods)
+<LI> CALL sla_PRENUT (EPOCH, DATE, RMATPN)
+<BR>
+Combined precession/nutation matrix
+<LI> CALL sla_PREBN (BEP0, BEP1, RMATP)
+<BR>
+Precession matrix, old system
+<LI> CALL sla_PRECES (SYSTEM, EP0, EP1, RA, DC)
+<BR>
+Precession, in either the old or the new system</UL>
+<BR><BIG><B>Proper Motion</BIG></B><UL>
+<LI> CALL sla_PM (R0, D0, PR, PD, PX, RV, EP0, EP1, R1, D1)
+<BR>
+Adjust for proper motion</UL>
+<BR><BIG><B>FK4/FK5/Hipparcos Conversions</BIG></B><UL>
+<LI> CALL sla_FK425 (
+                       R1950, D1950, DR1950, DD1950, P1950, V1950,
+                        R2000, D2000, DR2000, DD2000, P2000, V2000)
+<BR>
+Convert B1950.0 FK4 star data to J2000.0 FK5
+<LI> CALL sla_FK45Z (R1950, D1950, EPOCH, R2000, D2000)
+<BR>
+Convert B1950.0 FK4 position to J2000.0 FK5 assuming zero
+   FK5 proper motion and no parallax
+<LI> CALL sla_FK524 (
+                       R2000, D2000, DR2000, DD2000, P2000, V2000,
+                        R1950, D1950, DR1950, DD1950, P1950, V1950)
+<BR>
+Convert J2000.0 FK5 star data to B1950.0 FK4
+<LI> CALL sla_FK54Z (R2000, D2000, BEPOCH,
+               R1950, D1950, DR1950, DD1950)
+<BR>
+Convert J2000.0 FK5 position to B1950.0 FK4 assuming zero
+   FK5 proper motion and no parallax
+<LI> CALL sla_FK52H (R5, D5, DR5, DD5, RH, DH, DRH, DDH)
+<BR>
+Convert J2000.0 FK5 star data to Hipparcos
+<LI> CALL sla_FK5HZ (R5, D5, EPOCH, RH, DH )
+<BR>
+Convert J2000.0 FK5 position to Hipparcos assuming zero Hipparcos
+   proper motion
+<LI> CALL sla_H2FK5 (RH, DH, DRH, DDH, R5, D5, DR5, DD5)
+<BR>
+Convert Hipparcos star data to J2000.0 FK5
+<LI> CALL sla_HFK5Z (RH, DH, EPOCH, R5, D5, DR5, DD5)
+<BR>
+Convert Hipparcos position to J2000.0 FK5 assuming zero Hipparcos
+   proper motion
+<LI> CALL sla_DBJIN (STRING, NSTRT, DRESLT, J1, J2)
+<BR>
+Like sla_DFLTIN but with extensions to accept leading `B' and `J'
+<LI> CALL sla_KBJ (JB, E, K, J)
+<BR>
+Select epoch prefix `B' or `J'
+<LI> D&nbsp;=&nbsp;sla_EPCO (K0, K, E)
+<BR>
+Convert an epoch into the appropriate form - `B' or `J'</UL>
+<BR><BIG><B>Elliptic Aberration</BIG></B><UL>
+<LI> CALL sla_ETRMS (EP, EV)
+<BR>
+E-terms
+<LI> CALL sla_SUBET (RC, DC, EQ, RM, DM)
+<BR>
+Remove the E-terms
+<LI> CALL sla_ADDET (RM, DM, EQ, RC, DC)
+<BR>
+Add the E-terms</UL>
+<BR><BIG><B>Geographical and Geocentric Coordinates</BIG></B><UL>
+<LI> CALL sla_OBS (NUMBER, ID, NAME, WLONG, PHI, HEIGHT)
+<BR>
+Interrogate list of observatory parameters
+<LI> CALL sla_GEOC (P, H, R, Z)
+<BR>
+Convert geodetic position to geocentric
+<LI> CALL sla_POLMO (ELONGM, PHIM, XP, YP, ELONG, PHI, DAZ)
+<BR>
+Polar motion
+<LI> CALL sla_PVOBS (P, H, STL, PV)
+<BR>
+Position and velocity of observatory</UL>
+<BR><BIG><B>Apparent and Observed Place</BIG></B><UL>
+<LI> CALL sla_MAP (RM, DM, PR, PD, PX, RV, EQ, DATE, RA, DA)
+<BR>
+Mean place to geocentric apparent place
+<LI> CALL sla_MAPPA (EQ, DATE, AMPRMS)
+<BR>
+Precompute mean to apparent parameters
+<LI> CALL sla_MAPQK (RM, DM, PR, PD, PX, RV, AMPRMS, RA, DA)
+<BR>
+Mean to apparent using precomputed parameters
+<LI> CALL sla_MAPQKZ (RM, DM, AMPRMS, RA, DA)
+<BR>
+Mean to apparent using precomputed parameters, for zero proper
+     motion, parallax and radial velocity
+<LI> CALL sla_AMP (RA, DA, DATE, EQ, RM, DM)
+<BR>
+Geocentric apparent place to mean place
+<LI> CALL sla_AMPQK (RA, DA, AOPRMS, RM, DM)
+<BR>
+Apparent to mean using precomputed parameters
+<LI> CALL sla_AOP (
+                      RAP, DAP, UTC, DUT, ELONGM, PHIM, HM, XP, YP,
+                       TDK, PMB, RH, WL, TLR, AOB, ZOB, HOB, DOB, ROB)
+<BR>
+Apparent place to observed place
+<LI> CALL sla_AOPPA (
+                        UTC, DUT, ELONGM, PHIM, HM, XP, YP,
+                         TDK, PMB, RH, WL, TLR, AOPRMS)
+<BR>
+Precompute apparent to observed parameters
+<LI> CALL sla_AOPPAT (UTC, AOPRMS)
+<BR>
+Update sidereal time in apparent to observed parameters
+<LI> CALL sla_AOPQK (RAP, DAP, AOPRMS, AOB, ZOB, HOB, DOB, ROB)
+<BR>
+Apparent to observed using precomputed parameters
+<LI> CALL sla_OAP (
+                     TYPE, OB1, OB2, UTC, DUT, ELONGM, PHIM, HM, XP, YP,
+                      TDK, PMB, RH, WL, TLR, RAP, DAP)
+<BR>
+Observed to apparent
+<LI> CALL sla_OAPQK (TYPE, OB1, OB2, AOPRMS, RA, DA)
+<BR>
+Observed to apparent using precomputed parameters</UL>
+<BR><BIG><B>Azimuth and Elevation</BIG></B><UL>
+<LI> CALL sla_ALTAZ (
+               HA, DEC, PHI,
+                AZ, AZD, AZDD, EL, ELD, ELDD, PA, PAD, PADD)
+<BR>
+Positions, velocities <I>etc.</I> for an altazimuth mount
+<LI> CALL sla_E2H (HA, DEC, PHI, AZ, EL)
+<BR>
+CALL sla_DE2H (HA, DEC, PHI, AZ, EL)
+<BR>
+   <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$"> to <IMG WIDTH="66" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img28.gif"
+ ALT="$[\,Az,El~]$"><LI> CALL sla_H2E (AZ, EL, PHI, HA, DEC)
+<BR>
+CALL sla_DH2E (AZ, EL, PHI, HA, DEC)
+<BR>
+   <IMG WIDTH="66" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img28.gif"
+ ALT="$[\,Az,El~]$"> to <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$"><LI> CALL sla_PDA2H (P, D, A, H1, J1, H2, J2)
+<BR>
+Hour Angle corresponding to a given azimuth
+<LI> CALL sla_PDQ2H (P, D, Q, H1, J1, H2, J2)
+<BR>
+Hour Angle corresponding to a given parallactic angle
+<LI> D&nbsp;=&nbsp;sla_PA (HA, DEC, PHI)
+<BR>
+   <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$"> to parallactic angle
+<LI> D&nbsp;=&nbsp;sla_ZD (HA, DEC, PHI)
+<BR>
+   <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$"> to zenith distance</UL>
+<BR><BIG><B>Refraction and Air Mass</BIG></B><UL>
+<LI> CALL sla_REFRO (ZOBS, HM, TDK, PMB, RH, WL, PHI, TLR, EPS, REF)
+<BR>
+Change in zenith distance due to refraction
+<LI> CALL sla_REFCO (HM, TDK, PMB, RH, WL, PHI, TLR, EPS, REFA, REFB)
+<BR>
+Constants for simple refraction model (accurate)
+<LI> CALL sla_REFCOQ (TDK, PMB, RH, WL, REFA, REFB)
+<BR>
+Constants for simple refraction model (fast)
+<LI> CALL sla_ATMDSP ( TDK, PMB, RH, WL1, REFA1, REFB1, WL2, REFA2, REFB2 )
+<BR>
+Adjust refraction constants for colour
+<LI> CALL sla_REFZ (ZU, REFA, REFB, ZR)
+<BR>
+Unrefracted to refracted ZD, simple model
+<LI> CALL sla_REFV (VU, REFA, REFB, VR)
+<BR>
+Unrefracted to refracted <IMG WIDTH="66" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img28.gif"
+ ALT="$[\,Az,El~]$"> vector, simple model
+<LI> D&nbsp;=&nbsp;sla_AIRMAS (ZD)
+<BR>
+Air mass</UL>
+<BR><BIG><B>Ecliptic Coordinates</BIG></B><UL>
+<LI> CALL sla_ECMAT (DATE, RMAT)
+<BR>
+Equatorial to ecliptic rotation matrix
+<LI> CALL sla_EQECL (DR, DD, DATE, DL, DB)
+<BR>
+J2000.0 `FK5' to ecliptic coordinates
+<LI> CALL sla_ECLEQ (DL, DB, DATE, DR, DD)
+<BR>
+Ecliptic coordinates to J2000.0 `FK5'</UL>
+<BR><BIG><B>Galactic Coordinates</BIG></B><UL>
+<LI> CALL sla_EG50 (DR, DD, DL, DB)
+<BR>
+B1950.0 `FK4' to galactic
+<LI> CALL sla_GE50 (DL, DB, DR, DD)
+<BR>
+Galactic to B1950.0 `FK4'
+<LI> CALL sla_EQGAL (DR, DD, DL, DB)
+<BR>
+J2000.0 `FK5' to galactic
+<LI> CALL sla_GALEQ (DL, DB, DR, DD)
+<BR>
+Galactic to J2000.0 `FK5'</UL>
+<BR><BIG><B>Supergalactic Coordinates</BIG></B><UL>
+<LI> CALL sla_GALSUP (DL, DB, DSL, DSB)
+<BR>
+Galactic to supergalactic
+<LI> CALL sla_SUPGAL (DSL, DSB, DL, DB)
+<BR>
+Supergalactic to galactic</UL>
+<BR><BIG><B>Ephemerides</BIG></B><UL>
+<LI> CALL sla_DMOON (DATE, PV)
+<BR>
+Approximate geocentric position and velocity of the Moon
+<LI> CALL sla_EARTH (IY, ID, FD, PV)
+<BR>
+Approximate heliocentric position and velocity of the Earth
+<LI> CALL sla_EVP (DATE, DEQX, DVB, DPB, DVH, DPH)
+<BR>
+Barycentric and heliocentric velocity and position of the Earth
+<LI> CALL sla_MOON (IY, ID, FD, PV)
+<BR>
+Approximate geocentric position and velocity of the Moon
+<LI> CALL sla_PLANET (DATE, NP, PV, JSTAT)
+<BR>
+Approximate heliocentric position and velocity of a planet
+<LI> CALL sla_RDPLAN (DATE, NP, ELONG, PHI, RA, DEC, DIAM)
+<BR>
+Approximate topocentric apparent place of a planet
+<LI> CALL sla_PLANEL (
+                       DATE, JFORM, EPOCH, ORBINC, ANODE, PERIH,
+                      AORQ, E, AORL, DM, PV, JSTAT)
+<BR>
+Heliocentric position and velocity of a planet, asteroid or
+   comet, starting from orbital elements
+<LI> CALL sla_PLANTE (
+                       DATE, ELONG, PHI, JFORM, EPOCH, ORBINC, ANODE,
+                      PERIH, AORQ, E, AORL, DM, RA, DEC, R, JSTAT)
+<BR>
+Topocentric apparent place of a Solar-System object whose
+   heliocentric orbital elements are known
+<LI> CALL sla_PV2EL (
+                      PV, DATE, PMASS, JFORMR, JFORM, EPOCH, ORBINC,
+                     ANODE, PERIH, AORQ, E, AORL, DM, JSTAT)
+<BR>
+Orbital elements of a planet from instantaneous position and velocity
+<LI> CALL sla_PERTEL (
+                       JFORM, DATE0, DATE1,
+                     EPOCH0, ORBI0, ANODE0, PERIH0, AORQ0, E0, AM0,
+                     EPOCH1, ORBI1, ANODE1, PERIH1, AORQ1, E1, AM1,
+                     JSTAT)
+<BR>
+Update elements by applying perturbations
+<LI> CALL sla_EL2UE (
+                      DATE, JFORM, EPOCH, ORBINC, ANODE,
+                     PERIH, AORQ, E, AORL, DM,
+                     U, JSTAT)
+<BR>
+Transform conventional elements to universal elements
+<LI> CALL sla_UE2EL (
+                      U, JFORMR,
+                     JFORM, EPOCH, ORBINC, ANODE, PERIH,
+                     AORQ, E, AORL, DM, JSTAT)
+<BR>
+Transform universal elements to conventional elements
+<LI> CALL sla_PV2UE (PV, DATE, PMASS, U, JSTAT)
+<BR>
+Package a position and velocity for use as universal elements
+<LI> CALL sla_UE2PV (DATE, U, PV, JSTAT)
+<BR>
+Extract the position and velocity from universal elements
+<LI> CALL sla_PERTUE (DATE, U, JSTAT)
+<BR>
+Update universal elements by applying perturbations
+<LI> R&nbsp;=&nbsp;sla_RVEROT (PHI, RA, DA, ST)
+<BR>
+Velocity component due to rotation of the Earth
+<LI> CALL sla_ECOR (RM, DM, IY, ID, FD, RV, TL)
+<BR>
+Components of velocity and light time due to Earth orbital motion
+<LI> R&nbsp;=&nbsp;sla_RVLSRD (R2000, D2000)
+<BR>
+Velocity component due to solar motion wrt dynamical LSR
+<LI> R&nbsp;=&nbsp;sla_RVLSRK (R2000, D2000)
+<BR>
+Velocity component due to solar motion wrt kinematical LSR
+<LI> R&nbsp;=&nbsp;sla_RVGALC (R2000, D2000)
+<BR>
+Velocity component due to rotation of the Galaxy
+<LI> R&nbsp;=&nbsp;sla_RVLG (R2000, D2000)
+<BR>
+Velocity component due to rotation and translation of the
+   Galaxy, relative to the mean motion of the local group</UL>
+<BR><BIG><B>Astrometry</BIG></B><UL>
+<LI> CALL sla_S2TP (RA, DEC, RAZ, DECZ, XI, ETA, J)
+<BR>
+CALL sla_DS2TP (RA, DEC, RAZ, DECZ, XI, ETA, J)
+<BR>
+Transform spherical coordinates into tangent plane
+<LI> CALL sla_V2TP (V, V0, XI, ETA, J)
+<BR>
+CALL sla_DV2TP (V, V0, XI, ETA, J)
+<BR>
+Transform <IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$"> into tangent plane coordinates
+<LI> CALL sla_DTP2S (XI, ETA, RAZ, DECZ, RA, DEC)
+<BR>
+CALL sla_TP2S (XI, ETA, RAZ, DECZ, RA, DEC)
+<BR>
+Transform tangent plane coordinates into spherical coordinates
+<LI> CALL sla_DTP2V (XI, ETA, V0, V)
+<BR>
+CALL sla_TP2V (XI, ETA, V0, V)
+<BR>
+Transform tangent plane coordinates into <IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$"><LI> CALL sla_DTPS2C (XI, ETA, RA, DEC, RAZ1, DECZ1, RAZ2, DECZ2, N)
+<BR>
+CALL sla_TPS2C (XI, ETA, RA, DEC, RAZ1, DECZ1, RAZ2, DECZ2, N)
+<BR>
+Get plate centre from star <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> and tangent plane coordinates
+<LI> CALL sla_DTPV2C (XI, ETA, V, V01, V02, N)
+<BR>
+CALL sla_TPV2C (XI, ETA, V, V01, V02, N)
+<BR>
+Get plate centre from star <IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$"> and tangent plane coordinates
+<LI> CALL sla_PCD (DISCO, X, Y)
+<BR>
+Apply pincushion/barrel distortion
+<LI> CALL sla_UNPCD (DISCO, X, Y)
+<BR>
+Remove pincushion/barrel distortion
+<LI> CALL sla_FITXY (ITYPE, NP, XYE, XYM, COEFFS, J)
+<BR>
+Fit a linear model to relate two sets of <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> coordinates
+<LI> CALL sla_PXY (NP, XYE, XYM, COEFFS, XYP, XRMS, YRMS, RRMS)
+<BR>
+Compute predicted coordinates and residuals
+<LI> CALL sla_INVF (FWDS, BKWDS, J)
+<BR>
+Invert a linear model
+<LI> CALL sla_XY2XY (X1, Y1, COEFFS, X2, Y2)
+<BR>
+Transform one <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"><LI> CALL sla_DCMPF (COEFFS, XZ, YZ, XS, YS, PERP, ORIENT)
+<BR>
+Decompose a linear fit into scales <I>etc.</I></UL>
+<BR><BIG><B>Numerical Methods</BIG></B><UL>
+<LI> CALL sla_COMBN (NSEL, NCAND, LIST, J)
+<BR>
+Next combination (subset from a specified number of items)
+<LI> CALL sla_PERMUT (N, ISTATE, IORDER, J)
+<BR>
+Next permutation of a specified number of items
+<LI> CALL sla_SMAT (N, A, Y, D, JF, IW)
+<BR>
+CALL sla_DMAT (N, A, Y, D, JF, IW)
+<BR>
+Matrix inversion and solution of simultaneous equations
+<LI> CALL sla_SVD (M, N, MP, NP, A, W, V, WORK, JSTAT)
+<BR>
+Singular value decomposition of a matrix
+<LI> CALL sla_SVDSOL (M, N, MP, NP, B, U, W, V, WORK, X)
+<BR>
+Solution from given vector plus SVD
+<LI> CALL sla_SVDCOV (N, NP, NC, W, V, WORK, CVM)
+<BR>
+Covariance matrix from SVD
+<LI> R&nbsp;=&nbsp;sla_RANDOM (SEED)
+<BR>
+Generate pseudo-random real number in the range <IMG WIDTH="72" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img145.gif"
+ ALT="$0 \leq x < 1$"><LI> R&nbsp;=&nbsp;sla_GRESID (S)
+<BR>
+Generate pseudo-random normal deviate (<IMG WIDTH="15" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img251.gif"
+ ALT="$\equiv$"> `Gaussian residual')</UL>
+<BR><BIG><B>Real-time</BIG></B><UL>
+<LI> CALL sla_WAIT (DELAY)
+<BR>
+Interval wait</UL>
+<BR> <HR>
+<A NAME="tex2html2731" HREF="node229.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
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+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
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+About this document ... </A>
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+ <STRONG></STRONG><P>
+This document was generated using the
+<A HREF="http://www-dsed.llnl.gov/files/programs/unix/latex2html/manual/"><STRONG>LaTeX</STRONG>2<tt>HTML</tt></A> translator Version 97.1 (release) (July 13th, 1997)
+<P>
+Copyright &#169; 1993, 1994, 1995, 1996, 1997,
+<A HREF="http://cbl.leeds.ac.uk/nikos/personal.html">Nikos Drakos</A>, 
+Computer Based Learning Unit, University of Leeds.
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+The command line arguments were: <BR>
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+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
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+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
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+<H2><A NAME="SECTION000410000000000000000">SLA_AOPQK - Quick Appt-to-Observed</A>
+<A NAME="xref_SLA_AOPQK">&#160;</A><A NAME="SLA_AOPQK">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Quick apparent to observed place (but see Note&nbsp;8, below).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_AOPQK (RAP, DAP, AOPRMS, AOB, ZOB, HOB, DOB, ROB)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RAP,DAP</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>geocentric apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AOPRMS</EM></TD>
+<TD ALIGN="LEFT"><B>D(14)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>star-independent apparent-to-observed parameters:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(1)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>geodetic latitude (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(2,3)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>sine and cosine of geodetic latitude</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(4)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>magnitude of diurnal aberration vector</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(5)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>height (metres)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(6)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>ambient temperature (degrees K)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(7)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>pressure (mB)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(8)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>relative humidity (0-1)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(9)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>wavelength (<IMG WIDTH="26" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img21.gif"
+ ALT="$\mu{\rm m}$">)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(10)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>lapse rate (degrees K per metre)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(11,12)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>refraction constants A and B (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(13)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>longitude + eqn of equinoxes +
+``sidereal <IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">UT'' (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(14)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>local apparent sidereal time (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AOB</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>observed azimuth (radians: N=0, E=<IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img22.gif"
+ ALT="$90^{\circ}$">)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ZOB</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>observed zenith distance (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>HOB</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>observed Hour Angle (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DOB</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>observed Declination (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ROB</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>observed Right Ascension (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>This routine returns zenith distance rather than elevation
+in order to reflect the fact that no allowance is made for
+depression of the horizon.
+  <DT>2.
+<DD>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 azimuth and elevation should be within about
+<P>      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img25.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.1$">    for <IMG WIDTH="56" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img26.gif"
+ ALT="$\zeta<70^{\circ}$">.  Even
+        at a topocentric zenith distance of
+        <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img22.gif"
+ ALT="$90^{\circ}$">, the accuracy in elevation should be better than
+        1&nbsp;arcminute;  useful results are available for a further
+        <IMG WIDTH="18" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img27.gif"
+ ALT="$3^{\circ}$">, beyond which the sla_REFRO routine returns a
+        fixed value of the refraction.  The complementary
+        routines sla_AOP (or sla_AOPQK) and sla_OAP (or sla_OAPQK)
+        are self-consistent to better than 1&nbsp;microarcsecond all over
+        the celestial sphere.
+  <DT>3.
+<DD>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.
+  <DT>4.
+<DD><I>Apparent</I> <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> 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>i.e.</I> J2000), these effects can
+        be applied by means of the sla_MAP <I>etc.</I> routines.  Starting from
+        other mean place systems, additional transformations will be
+        needed;  for example, FK4 (<I>i.e.</I> B1950) mean places would first
+        have to be converted to FK5, which can be done with the
+        sla_FK425 <I>etc.</I> routines.
+  <DT>5.
+<DD><I>Observed</I> <IMG WIDTH="66" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img28.gif"
+ ALT="$[\,Az,El~]$"> means the position that would be seen by a
+        perfect theodolite located at the observer.  This is obtained
+        from the geocentric apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> by allowing for Earth
+        orientation and diurnal aberration, rotating from equator
+        to horizon coordinates, and then adjusting for refraction.
+        The <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$"> 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 (<I>n.b.</I> not to the
+        refracted pole).  Finally, the <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"> is obtained by subtracting
+        the <I>h</I> from the local apparent ST.
+  <DT>6.
+<DD>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.
+  <DT>7.
+<DD>The star-independent apparent-to-observed-place parameters
+        in AOPRMS may be computed by means of the sla_AOPPA routine.
+        If nothing has changed significantly except the time, the
+        sla_AOPPAT routine may be used to perform the requisite
+        partial recomputation of AOPRMS.
+  <DT>8.
+<DD>The  ``sidereal <IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">UT'' which forms part of AOPRMS(13)
+        is UT1-UTC converted from solar to
+        sidereal seconds and expressed in radians.
+  <DT>9.
+<DD>At zenith distances beyond about <IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img33.gif"
+ ALT="$76^\circ$">, 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.
+  <DT>10.
+<DD>The azimuths <I>etc.</I> used by the present routine are with
+        respect to the celestial pole.  Corrections to the terrestrial pole
+        can be computed using sla_POLMO.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html656" HREF="node24.html">
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+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node24.html b/src/slalib/sun67.htx/node24.html
new file mode 100644
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--- /dev/null
+++ b/src/slalib/sun67.htx/node24.html
@@ -0,0 +1,213 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
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+<TITLE>SLA_ATMDSP - Atmospheric Dispersion</TITLE>
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+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000411000000000000000">SLA_ATMDSP - Atmospheric Dispersion</A>
+<A NAME="xref_SLA_ATMDSP">&#160;</A><A NAME="SLA_ATMDSP">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Apply atmospheric-dispersion adjustments to refraction coefficients.
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_ATMDSP (TDK, PMB, RH, WL1, A1, B1, WL2, A2, B2)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>TDK</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>ambient temperature at the observer (degrees K)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PMB</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>pressure at the observer (mB)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>relative humidity at the observer (range 0-1)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>WL1</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>base wavelength (<IMG WIDTH="26" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img21.gif"
+ ALT="$\mu{\rm m}$">)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A1</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>refraction coefficient A for wavelength WL1 (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>B1</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>refraction coefficient B for wavelength WL1 (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>WL2</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>wavelength for which adjusted A,B required (<IMG WIDTH="26" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img21.gif"
+ ALT="$\mu{\rm m}$">)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A2</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>refraction coefficient A for wavelength WL2 (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>B2</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>refraction coefficient B for wavelength WL2 (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>To use this routine, first call sla_REFCO specifying WL1 as the
+wavelength.  This yields refraction coefficients A1, B1, correct
+for that wavelength.  Subsequently, calls to sla_ATMDSP specifying
+        different wavelengths will produce new, slightly adjusted
+        refraction coefficients A2, B2, which apply to the specified wavelength.
+  <DT>2.
+<DD>Most of the atmospheric dispersion happens between <IMG WIDTH="50" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img34.gif"
+ ALT="$0.7\,\mu{\rm m}$">        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 <IMG WIDTH="50" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img35.gif"
+ ALT="$0.4\,\mu{\rm m}$">.  <DT>3.
+<DD>The accuracy, for this set of conditions: <BR>
+<BR>
+     <TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>height above sea level</TD>
+<TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+<TD ALIGN="LEFT" NOWRAP>2000m</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>latitude</TD>
+<TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img36.gif"
+ ALT="$29^\circ$"></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>pressure</TD>
+<TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+<TD ALIGN="LEFT" NOWRAP>793mB</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>temperature</TD>
+<TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="34" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img37.gif"
+ ALT="$290^\circ$">K</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>humidity</TD>
+<TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+<TD ALIGN="LEFT" NOWRAP>0.5 (50%)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>lapse rate</TD>
+<TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="86" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img38.gif"
+ ALT="$0.0065^\circ m^{-1}$"></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>reference wavelength</TD>
+<TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="50" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img35.gif"
+ ALT="$0.4\,\mu{\rm m}$"></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="RIGHT" NOWRAP>star elevation</TD>
+<TD ALIGN="CENTER" NOWRAP>&nbsp;</TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="26" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img39.gif"
+ ALT="$15^\circ$"></TD>
+</TR>
+</TABLE>
+<BR>
+<BR>
+is about 2.5mas RMS between 0.3 and <IMG WIDTH="50" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img40.gif"
+ ALT="$1.0\,\mu{\rm m}$">, and stays
+        within 4mas for the whole range longward of <IMG WIDTH="50" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img41.gif"
+ ALT="$0.3\,\mu{\rm m}$">        (compared with a total dispersion from 0.3 to <IMG WIDTH="45" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img42.gif"
+ ALT="$20\,\mu{\rm m}$">        of about <IMG WIDTH="25" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img43.gif"
+ ALT="$11\hspace{-0.05em}^{'\hspace{-0.1em}'}$">).  These errors are typical for ordinary
+        conditions;  in extreme conditions values a few times this size
+        may occur.
+  <DT>4.
+<DD>If either wavelength exceeds <IMG WIDTH="53" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img44.gif"
+ ALT="$100\,\mu{\rm m}$">, the radio case
+        is assumed and the returned refraction coefficients are the
+        same as the given ones.
+  <DT>5.
+<DD>The algorithm consists of calculation of the refractivity of the
+        air at the observer for the two wavelengths, using the methods
+        of the sla_REFRO routine, and then scaling of the two refraction
+        coefficients according to classical refraction theory.  This
+        amounts to scaling the A coefficient in proportion to <IMG WIDTH="53" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img45.gif"
+ ALT="$(\mu-1)$"> and
+        the B coefficient almost in the same ratio (see R.M.Green,
+        <I>Spherical Astronomy,</I> Cambridge University Press, 1985).
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html666" HREF="node25.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html664" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html658" HREF="node23.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html667" HREF="node25.html">SLA_AV2M - Rotation Matrix from Axial Vector</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html665" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html659" HREF="node23.html">SLA_AOPQK - Quick Appt-to-Observed</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node25.html b/src/slalib/sun67.htx/node25.html
new file mode 100644
index 0000000..f557394
--- /dev/null
+++ b/src/slalib/sun67.htx/node25.html
@@ -0,0 +1,103 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_AV2M - Rotation Matrix from Axial Vector</TITLE>
+<META NAME="description" CONTENT="SLA_AV2M - Rotation Matrix from Axial Vector">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
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+<A NAME="tex2html668" HREF="node24.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html677" HREF="node26.html">SLA_BEAR - Direction Between Points on a Sphere</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html675" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html669" HREF="node24.html">SLA_ATMDSP - Atmospheric Dispersion</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000412000000000000000">SLA_AV2M - Rotation Matrix from Axial Vector</A>
+<A NAME="xref_SLA_AV2M">&#160;</A><A NAME="SLA_AV2M">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Form the rotation matrix corresponding to a given axial vector
+(single precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_AV2M (AXVEC, RMAT)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AXVEC</EM></TD>
+<TH ALIGN="LEFT"><B>R(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>axial vector (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RMAT</EM></TD>
+<TH ALIGN="LEFT"><B>R(3,3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>rotation matrix</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>A rotation matrix describes a rotation about some arbitrary axis.
+The axis is called the <I>Euler axis</I>, and the angle through which the
+reference frame rotates is called the Euler angle.  The axial
+        vector supplied to this routine has the same direction as the
+        Euler axis, and its magnitude is the Euler angle in radians.
+  <DT>2.
+<DD>If AXVEC is null, the unit matrix is returned.
+  <DT>3.
+<DD>The reference frame rotates clockwise as seen looking along
+        the axial vector from the origin.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html676" HREF="node26.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html674" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html668" HREF="node24.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html677" HREF="node26.html">SLA_BEAR - Direction Between Points on a Sphere</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html675" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html669" HREF="node24.html">SLA_ATMDSP - Atmospheric Dispersion</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node26.html b/src/slalib/sun67.htx/node26.html
new file mode 100644
index 0000000..8296b32
--- /dev/null
+++ b/src/slalib/sun67.htx/node26.html
@@ -0,0 +1,123 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_BEAR - Direction Between Points on a Sphere</TITLE>
+<META NAME="description" CONTENT="SLA_BEAR - Direction Between Points on a Sphere">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node27.html">
+<LINK REL="previous" HREF="node25.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node27.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html686" HREF="node27.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html684" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html678" HREF="node25.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html687" HREF="node27.html">SLA_CAF2R - Deg,Arcmin,Arcsec to Radians</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html685" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html679" HREF="node25.html">SLA_AV2M - Rotation Matrix from Axial Vector</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000413000000000000000">SLA_BEAR - Direction Between Points on a Sphere</A>
+<A NAME="xref_SLA_BEAR">&#160;</A><A NAME="SLA_BEAR">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Returns the bearing (position angle) of one point on a
+sphere seen from another (single precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>R&nbsp;=&nbsp;sla_BEAR (A1, B1, A2, B2)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A1,B1</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>spherical coordinates of one point</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A2,B2</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>spherical coordinates of the other point</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_BEAR</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>bearing from first point to second</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The spherical coordinates are <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">,<IMG WIDTH="38" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img46.gif"
+ ALT="$[\lambda,\phi]$"> <I>etc.</I>, in radians.
+<DT>2.
+<DD>The result is the bearing (position angle), in radians,
+       of point [A2,B2] as seen
+       from point [A1,B1].  It is in the range <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$">.  The sense
+       is such that if [A2,B2]
+       is a small distance due east of [A1,B1] the result
+       is about <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img14.gif"
+ ALT="$+\pi/2$">. Zero is returned
+       if the two points are coincident.
+ <DT>3.
+<DD>If either B-coordinate is outside the range <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img15.gif"
+ ALT="$\pm\pi/2$">, the
+       result may correspond to ``the long way round''.
+ <DT>4.
+<DD>The routine sla_PAV performs an equivalent function except
+       that the points are specified in the form of Cartesian unit
+       vectors.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html686" HREF="node27.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html684" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html678" HREF="node25.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html687" HREF="node27.html">SLA_CAF2R - Deg,Arcmin,Arcsec to Radians</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html685" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html679" HREF="node25.html">SLA_AV2M - Rotation Matrix from Axial Vector</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node27.html b/src/slalib/sun67.htx/node27.html
new file mode 100644
index 0000000..6c176b5
--- /dev/null
+++ b/src/slalib/sun67.htx/node27.html
@@ -0,0 +1,122 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_CAF2R - Deg,Arcmin,Arcsec to Radians</TITLE>
+<META NAME="description" CONTENT="SLA_CAF2R - Deg,Arcmin,Arcsec to Radians">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node28.html">
+<LINK REL="previous" HREF="node26.html">
+<LINK REL="up" HREF="node13.html">
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+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html696" HREF="node28.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html694" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html688" HREF="node26.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html697" HREF="node28.html">SLA_CALDJ - Calendar Date to MJD</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html695" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html689" HREF="node26.html">SLA_BEAR - Direction Between Points on a Sphere</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000414000000000000000">SLA_CAF2R - Deg,Arcmin,Arcsec to Radians</A>
+<A NAME="xref_SLA_CAF2R">&#160;</A><A NAME="SLA_CAF2R">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Convert degrees, arcminutes, arcseconds to radians
+(single precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_CAF2R (IDEG, IAMIN, ASEC, RAD, J)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IDEG</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>degrees</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IAMIN</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>arcminutes</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ASEC</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>arcseconds</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RAD</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>angle in radians</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  1 = IDEG outside range 0-359</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  2 = IAMIN outside range 0-59</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  3 = ASEC outside range 0-59.999<IMG WIDTH="21" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img48.gif"
+ ALT="$\cdots$"></TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The result is computed even if any of the range checks fail.
+<DT>2.
+<DD>The sign must be dealt with outside this routine.
+</DL></DL>
+<BR> <HR>
+<A NAME="tex2html696" HREF="node28.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html694" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html688" HREF="node26.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html697" HREF="node28.html">SLA_CALDJ - Calendar Date to MJD</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html695" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html689" HREF="node26.html">SLA_BEAR - Direction Between Points on a Sphere</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node28.html b/src/slalib/sun67.htx/node28.html
new file mode 100644
index 0000000..33bc93d
--- /dev/null
+++ b/src/slalib/sun67.htx/node28.html
@@ -0,0 +1,128 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_CALDJ - Calendar Date to MJD</TITLE>
+<META NAME="description" CONTENT="SLA_CALDJ - Calendar Date to MJD">
+<META NAME="keywords" CONTENT="sun67">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html707" HREF="node29.html">SLA_CALYD - Calendar to Year, Day</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html705" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html699" HREF="node27.html">SLA_CAF2R - Deg,Arcmin,Arcsec to Radians</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000415000000000000000">SLA_CALDJ - Calendar Date to MJD</A>
+<A NAME="xref_SLA_CALDJ">&#160;</A><A NAME="SLA_CALDJ">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Gregorian Calendar to Modified Julian Date, with century default.
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_CALDJ (IY, IM, ID, DJM, J)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IY,IM,ID</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>year, month, day in Gregorian calendar</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DJM</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>modified Julian Date (JD-2400000.5) for <IMG WIDTH="18" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img49.gif"
+ ALT="$0^{\rm h}$"></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  0 = OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  1 = bad year   (MJD not computed)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  2 = bad month  (MJD not computed)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  3 = bad day    (MJD computed)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>This routine supports the <I>century default</I> feature.
+Acceptable years are:
+<UL>
+<LI> 00-49, interpreted as 2000-2049,
+<LI> 50-99, interpreted as 1950-1999, and
+<LI> 100 upwards, interpreted literally.
+        </UL>
+        For 1-100AD use the routine sla_CLDJ instead.
+  <DT>2.
+<DD>For year <I>n</I>BC use IY = -(<I>n</I>-1).
+  <DT>3.
+<DD>When an invalid year or month is supplied (status J&nbsp;=&nbsp;1&nbsp;or&nbsp;2)
+        the MJD is <B>not</B> computed.  When an invalid day is supplied
+        (status J&nbsp;=&nbsp;3) the MJD <B>is</B> computed.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html706" HREF="node29.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html704" HREF="node13.html">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html707" HREF="node29.html">SLA_CALYD - Calendar to Year, Day</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html705" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html699" HREF="node27.html">SLA_CAF2R - Deg,Arcmin,Arcsec to Radians</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node29.html b/src/slalib/sun67.htx/node29.html
new file mode 100644
index 0000000..f831e5a
--- /dev/null
+++ b/src/slalib/sun67.htx/node29.html
@@ -0,0 +1,140 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_CALYD - Calendar to Year, Day</TITLE>
+<META NAME="description" CONTENT="SLA_CALYD - Calendar to Year, Day">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html717" HREF="node30.html">SLA_CC2S - Cartesian to Spherical</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html715" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html709" HREF="node28.html">SLA_CALDJ - Calendar Date to MJD</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000416000000000000000">SLA_CALYD - Calendar to Year, Day</A>
+<A NAME="xref_SLA_CALYD">&#160;</A><A NAME="SLA_CALYD">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Gregorian calendar date to year and day in year, in a Julian
+calendar aligned to the 20th/21st century Gregorian calendar,
+         with century default.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_CALYD (IY, IM, ID, NY, ND, J)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IY,IM,ID</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>year, month, day in Gregorian calendar:
+year may optionally omit the century</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NY</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>year (re-aligned Julian calendar)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ND</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>day in year (1 = January 1st)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>   0 = OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>   1 = bad year (before -4711)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>   2 = bad month</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>   3 = bad day</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>This routine supports the <I>century default</I> feature.
+Acceptable years are:
+<UL>
+<LI> 00-49, interpreted as 2000-2049,
+<LI> 50-99, interpreted as 1950-1999, and
+<LI> other years after -4712 , interpreted literally.
+        </UL>
+        Use sla_CLYD for years before 100AD.
+  <DT>2.
+<DD>The purpose of sla_CALDJ is to support
+        sla_EARTH, sla_MOON and sla_ECOR.
+  <DT>3.
+<DD>Between 1900&nbsp;March&nbsp;1 and 2100&nbsp;February&nbsp;28 it returns answers
+        which are consistent with the ordinary Gregorian calendar.
+        Outside this range there will be a discrepancy which increases
+        by one day for every non-leap century year.
+  <DT>4.
+<DD>When an invalid year or month is supplied (status J&nbsp;=&nbsp;1 or J&nbsp;=&nbsp;2)
+        the results are <B>not</B> computed.  When a day is
+        supplied which is outside the conventional range (status J&nbsp;=&nbsp;3)
+        the results <B>are</B> computed.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html716" HREF="node30.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html714" HREF="node13.html">
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+<A NAME="tex2html708" HREF="node28.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html717" HREF="node30.html">SLA_CC2S - Cartesian to Spherical</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html715" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html709" HREF="node28.html">SLA_CALDJ - Calendar Date to MJD</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node3.html b/src/slalib/sun67.htx/node3.html
new file mode 100644
index 0000000..886a149
--- /dev/null
+++ b/src/slalib/sun67.htx/node3.html
@@ -0,0 +1,76 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Purpose</TITLE>
+<META NAME="description" CONTENT="Purpose">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node4.html">
+<LINK REL="previous" HREF="node2.html">
+<LINK REL="up" HREF="node2.html">
+<LINK REL="next" HREF="node4.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html275" HREF="node4.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html273" HREF="node2.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html267" HREF="node2.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html276" HREF="node4.html">Example Application</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html274" HREF="node2.html">INTRODUCTION</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html268" HREF="node2.html">INTRODUCTION</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION00021000000000000000">
+Purpose</A>
+</H2>
+SLALIB<A NAME="tex2html1" HREF="footnode.html#412"><SUP><IMG  ALIGN="BOTTOM" BORDER="1" ALT="[*]" SRC="foot_motif.gif"></SUP></A>
+is a library of routines
+intended to make accurate and reliable positional-astronomy
+applications easier to write.
+Most SLALIB routines are concerned with astronomical position and time, but a
+number have wider trigonometrical, numerical or general applications.
+The applications ASTROM, COCO, RV and TPOINT
+all make extensive use of the SLALIB
+routines, as do a number of telescope control systems around the world.
+The SLALIB versions currently in service are written in
+Fortran&nbsp;77 and run on VAX/VMS, several Unix platforms and PC.
+A generic ANSI&nbsp;C version is also available from the author;  it is
+functionally similar to the Fortran version upon which the present
+document concentrates.
+<P>
+<BR> <HR>
+<A NAME="tex2html275" HREF="node4.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html273" HREF="node2.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html267" HREF="node2.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html276" HREF="node4.html">Example Application</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html274" HREF="node2.html">INTRODUCTION</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html268" HREF="node2.html">INTRODUCTION</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node30.html b/src/slalib/sun67.htx/node30.html
new file mode 100644
index 0000000..21b121e
--- /dev/null
+++ b/src/slalib/sun67.htx/node30.html
@@ -0,0 +1,103 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_CC2S - Cartesian to Spherical</TITLE>
+<META NAME="description" CONTENT="SLA_CC2S - Cartesian to Spherical">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node31.html">
+<LINK REL="previous" HREF="node29.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node31.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html726" HREF="node31.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html724" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html718" HREF="node29.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html727" HREF="node31.html">SLA_CC62S - Cartesian 6-Vector to Spherical</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html725" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html719" HREF="node29.html">SLA_CALYD - Calendar to Year, Day</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000417000000000000000">SLA_CC2S - Cartesian to Spherical</A>
+<A NAME="xref_SLA_CC2S">&#160;</A><A NAME="SLA_CC2S">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Cartesian coordinates to spherical coordinates (single precision).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_CC2S (V, A, B)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V</EM></TD>
+<TH ALIGN="LEFT"><B>R(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$"> vector</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A,B</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>spherical coordinates in radians</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The spherical coordinates are longitude (+ve anticlockwise
+looking from the +ve latitude pole) and latitude.  The
+Cartesian coordinates are right handed, with the <I>x</I>-axis
+        at zero longitude and latitude, and the <I>z</I>-axis at the
+        +ve latitude pole.
+  <DT>2.
+<DD>If V is null, zero A and B are returned.
+  <DT>3.
+<DD>At either pole, zero A is returned.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html726" HREF="node31.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html724" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html718" HREF="node29.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html727" HREF="node31.html">SLA_CC62S - Cartesian 6-Vector to Spherical</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html725" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html719" HREF="node29.html">SLA_CALYD - Calendar to Year, Day</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node31.html b/src/slalib/sun67.htx/node31.html
new file mode 100644
index 0000000..1877958
--- /dev/null
+++ b/src/slalib/sun67.htx/node31.html
@@ -0,0 +1,114 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_CC62S - Cartesian 6-Vector to Spherical</TITLE>
+<META NAME="description" CONTENT="SLA_CC62S - Cartesian 6-Vector to Spherical">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node32.html">
+<LINK REL="previous" HREF="node30.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node32.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html736" HREF="node32.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html734" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html728" HREF="node30.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html737" HREF="node32.html">SLA_CD2TF - Days to Hour,Min,Sec</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html735" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html729" HREF="node30.html">SLA_CC2S - Cartesian to Spherical</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000418000000000000000">SLA_CC62S - Cartesian 6-Vector to Spherical</A>
+<A NAME="xref_SLA_CC62S">&#160;</A><A NAME="SLA_CC62S">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Conversion of position &amp; velocity in Cartesian coordinates
+to spherical coordinates (single precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_CC62S (V, A, B, R, AD, BD, RD)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V</EM></TD>
+<TH ALIGN="LEFT"><B>R(6)</B></TH>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="106" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img51.gif"
+ ALT="$[\,x,y,z,\dot{x},\dot{y},\dot{z}\,]$"></TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>longitude (radians) - for example <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>B</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>latitude (radians) - for example <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$"></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>R</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>radial coordinate</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AD</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>longitude derivative (radians per unit time)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>BD</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>latitude derivative (radians per unit time)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RD</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>radial derivative</TD>
+</TR>
+</TABLE></DL>
+<BR> <HR>
+<A NAME="tex2html736" HREF="node32.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html734" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html728" HREF="node30.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html737" HREF="node32.html">SLA_CD2TF - Days to Hour,Min,Sec</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html735" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html729" HREF="node30.html">SLA_CC2S - Cartesian to Spherical</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node32.html b/src/slalib/sun67.htx/node32.html
new file mode 100644
index 0000000..9d7f8ab
--- /dev/null
+++ b/src/slalib/sun67.htx/node32.html
@@ -0,0 +1,115 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_CD2TF - Days to Hour,Min,Sec</TITLE>
+<META NAME="description" CONTENT="SLA_CD2TF - Days to Hour,Min,Sec">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node33.html">
+<LINK REL="previous" HREF="node31.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node33.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html746" HREF="node33.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html744" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html738" HREF="node31.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html747" HREF="node33.html">SLA_CLDJ - Calendar to MJD</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html745" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html739" HREF="node31.html">SLA_CC62S - Cartesian 6-Vector to Spherical</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000419000000000000000">SLA_CD2TF - Days to Hour,Min,Sec</A>
+<A NAME="xref_SLA_CD2TF">&#160;</A><A NAME="SLA_CD2TF">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Convert an interval in days to hours, minutes, seconds
+(single precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_CD2TF (NDP, DAYS, SIGN, IHMSF)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NDP</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>number of decimal places of seconds</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DAYS</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>interval in days</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>SIGN</EM></TD>
+<TH ALIGN="LEFT"><B>C</B></TH>
+<TD ALIGN="LEFT" NOWRAP>`+' or `-'</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IHMSF</EM></TD>
+<TD ALIGN="LEFT"><B>I(4)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>hours, minutes, seconds, fraction</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>NDP less than zero is interpreted as zero.
+<DT>2.
+<DD>The largest useful value for NDP is determined by the size of
+DAYS, the format of REAL floating-point numbers on the target
+        machine, and the risk of overflowing IHMSF(4).  For example,
+        on a VAX computer, for DAYS up to 1.0, the available floating-point
+        precision corresponds roughly to NDP=3.  This is well below
+        the ultimate limit of NDP=9 set by the capacity of the 32-bit
+        integer IHMSF(4).
+  <DT>3.
+<DD>The absolute value of DAYS may exceed 1.0.  In cases where it
+        does not, it is up to the caller to test for and handle the
+        case where DAYS is very nearly 1.0 and rounds up to 24&nbsp;hours,
+        by testing for IHMSF(1)=24 and setting IHMSF(1-4) to zero.
+</DL></DL>
+<BR> <HR>
+<A NAME="tex2html746" HREF="node33.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html744" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html738" HREF="node31.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html747" HREF="node33.html">SLA_CLDJ - Calendar to MJD</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html745" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html739" HREF="node31.html">SLA_CC62S - Cartesian 6-Vector to Spherical</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node33.html b/src/slalib/sun67.htx/node33.html
new file mode 100644
index 0000000..556eb23
--- /dev/null
+++ b/src/slalib/sun67.htx/node33.html
@@ -0,0 +1,128 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_CLDJ - Calendar to MJD</TITLE>
+<META NAME="description" CONTENT="SLA_CLDJ - Calendar to MJD">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node34.html">
+<LINK REL="previous" HREF="node32.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node34.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html756" HREF="node34.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html754" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html748" HREF="node32.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html757" HREF="node34.html">SLA_CLYD - Calendar to Year, Day</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html755" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html749" HREF="node32.html">SLA_CD2TF - Days to Hour,Min,Sec</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000420000000000000000">SLA_CLDJ - Calendar to MJD</A>
+<A NAME="xref_SLA_CLDJ">&#160;</A><A NAME="SLA_CLDJ">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Gregorian Calendar to Modified Julian Date.
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_CLDJ (IY, IM, ID, DJM, J)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IY,IM,ID</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>year, month, day in Gregorian calendar</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DJM</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>modified Julian Date (JD-2400000.5) for <IMG WIDTH="18" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img49.gif"
+ ALT="$0^{\rm h}$"></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  0 = OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  1 = bad year</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  2 = bad month</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  3 = bad day</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>When an invalid year or month is supplied (status J&nbsp;=&nbsp;1&nbsp;or&nbsp;2)
+the MJD is <B>not</B> computed.  When an invalid day is supplied
+(status J&nbsp;=&nbsp;3) the MJD <B>is</B> computed.
+  <DT>2.
+<DD>The year must be -4699 (<I>i.e.</I> 4700BC) or later.
+        For year <I>n</I>BC use IY = -(<I>n</I>-1).
+  <DT>3.
+<DD>An alternative to the present routine is sla_CALDJ, which
+        accepts a year with the century missing.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>The algorithm is derived from that of Hatcher,
+<I>Q.Jl.R.astr.Soc.</I> (1984) <B>25</B>, 53-55.
+     </DL>
+<BR> <HR>
+<A NAME="tex2html756" HREF="node34.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html754" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html748" HREF="node32.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html757" HREF="node34.html">SLA_CLYD - Calendar to Year, Day</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html755" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html749" HREF="node32.html">SLA_CD2TF - Days to Hour,Min,Sec</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node34.html b/src/slalib/sun67.htx/node34.html
new file mode 100644
index 0000000..266f38a
--- /dev/null
+++ b/src/slalib/sun67.htx/node34.html
@@ -0,0 +1,129 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_CLYD - Calendar to Year, Day</TITLE>
+<META NAME="description" CONTENT="SLA_CLYD - Calendar to Year, Day">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node35.html">
+<LINK REL="previous" HREF="node33.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node35.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html766" HREF="node35.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html764" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html758" HREF="node33.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html767" HREF="node35.html">SLA_COMBN - Next Combination</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html765" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html759" HREF="node33.html">SLA_CLDJ - Calendar to MJD</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000421000000000000000">SLA_CLYD - Calendar to Year, Day</A>
+<A NAME="xref_SLA_CLYD">&#160;</A><A NAME="SLA_CLYD">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Gregorian calendar date to year and day in year, in a Julian
+calendar aligned to the 20th/21st century Gregorian calendar.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_CLYD (IY, IM, ID, NY, ND, J)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IY,IM,ID</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>year, month, day in Gregorian calendar</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NY</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>year (re-aligned Julian calendar)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ND</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>day in year (1 = January 1st)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>   0 = OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>   1 = bad year (before -4711)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>   2 = bad month</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>   3 = bad day</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The purpose of sla_CLYD is to support sla_EARTH,
+sla_MOON and sla_ECOR.
+<DT>2.
+<DD>Between 1900&nbsp;March&nbsp;1 and 2100&nbsp;February&nbsp;28 it returns answers
+        which are consistent with the ordinary Gregorian calendar.
+        Outside this range there will be a discrepancy which increases
+        by one day for every non-leap century year.
+  <DT>3.
+<DD>When an invalid year or month is supplied (status J&nbsp;=&nbsp;1 or J&nbsp;=&nbsp;2)
+        the results are <B>not</B> computed.  When a day is
+        supplied which is outside the conventional range (status J&nbsp;=&nbsp;3)
+        the results <B>are</B> computed.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html766" HREF="node35.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html764" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html758" HREF="node33.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html767" HREF="node35.html">SLA_COMBN - Next Combination</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html765" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html759" HREF="node33.html">SLA_CLDJ - Calendar to MJD</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node35.html b/src/slalib/sun67.htx/node35.html
new file mode 100644
index 0000000..8723385
--- /dev/null
+++ b/src/slalib/sun67.htx/node35.html
@@ -0,0 +1,142 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_COMBN - Next Combination</TITLE>
+<META NAME="description" CONTENT="SLA_COMBN - Next Combination">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node36.html">
+<LINK REL="previous" HREF="node34.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node36.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html776" HREF="node36.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html774" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html768" HREF="node34.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html777" HREF="node36.html">SLA_CR2AF - Radians to Deg,Arcmin,Arcsec</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html775" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html769" HREF="node34.html">SLA_CLYD - Calendar to Year, Day</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000422000000000000000">SLA_COMBN - Next Combination</A>
+<A NAME="xref_SLA_COMBN">&#160;</A><A NAME="SLA_COMBN">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Generate the next combination, a subset of a specified size chosen
+from a specified number of items.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_COMBN (NSEL, NCAND, LIST, J)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NSEL</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>number of items (subset size)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NCAND</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>number of candidates (set size)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>GIVEN and RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>LIST</EM></TD>
+<TH ALIGN="LEFT"><B>I(NSEL)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>latest combination, LIST(1)=0 to initialize</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -1 = illegal NSEL or NCAND</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>     0 = OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  +1 = no more combinations available</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>NSEL and NCAND must both be at least 1, and NSEL must be less
+than or equal to NCAND.
+<DT>2.
+<DD>This routine returns, in the LIST array, a subset of NSEL integers
+        chosen from the range 1 to NCAND inclusive, in ascending order.
+        Before calling the routine for the first time, the caller must set
+        the first element of the LIST array to zero (any value less than 1
+        will do) to cause initialization.
+  <DT>3.
+<DD>The first combination to be generated is:
+        <BLOCKQUOTE>LIST(1)=1, LIST(2)=2, ..., LIST(NSEL)=NSEL
+        </BLOCKQUOTE>
+        This is also the combination returned for the ``finished'' (J=1) case.
+        The final permutation to be generated is:
+        <BLOCKQUOTE>LIST(1)=NCAND, LIST(2)=NCAND-1, ..., <BR>
+           &nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;LIST(NSEL)=NCAND-NSEL+1
+        </BLOCKQUOTE>
+  <DT>4.
+<DD>If the ``finished'' (J=1) status is ignored, the routine
+        continues to deliver combinations, the pattern repeating
+        every NCAND!/(NSEL!(NCAND-NSEL)!) calls.
+  <DT>5.
+<DD>The algorithm is by R.F.Warren-Smith (private communication).
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html776" HREF="node36.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html774" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html768" HREF="node34.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html777" HREF="node36.html">SLA_CR2AF - Radians to Deg,Arcmin,Arcsec</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html775" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html769" HREF="node34.html">SLA_CLYD - Calendar to Year, Day</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node36.html b/src/slalib/sun67.htx/node36.html
new file mode 100644
index 0000000..0932642
--- /dev/null
+++ b/src/slalib/sun67.htx/node36.html
@@ -0,0 +1,122 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_CR2AF - Radians to Deg,Arcmin,Arcsec</TITLE>
+<META NAME="description" CONTENT="SLA_CR2AF - Radians to Deg,Arcmin,Arcsec">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node37.html">
+<LINK REL="previous" HREF="node35.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node37.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html786" HREF="node37.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html784" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html778" HREF="node35.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html787" HREF="node37.html">SLA_CR2TF - Radians to Hour,Min,Sec</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html785" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html779" HREF="node35.html">SLA_COMBN - Next Combination</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000423000000000000000">SLA_CR2AF - Radians to Deg,Arcmin,Arcsec</A>
+<A NAME="xref_SLA_CR2AF">&#160;</A><A NAME="SLA_CR2AF">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Convert an angle in radians to degrees, arcminutes,
+arcseconds (single precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_CR2AF (NDP, ANGLE, SIGN, IDMSF)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NDP</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>number of decimal places of arcseconds</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ANGLE</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>angle in radians</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>SIGN</EM></TD>
+<TH ALIGN="LEFT"><B>C</B></TH>
+<TD ALIGN="LEFT" NOWRAP>`+' or `-'</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IDMSF</EM></TD>
+<TD ALIGN="LEFT"><B>I(4)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>degrees, arcminutes, arcseconds, fraction</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>NDP less than zero is interpreted as zero.
+<DT>2.
+<DD>The largest useful value for NDP is determined by the size of
+ANGLE, the format of REAL floating-point numbers on the target
+        machine, and the risk of overflowing IDMSF(4).  For example,
+        on a VAX computer, for ANGLE up to <IMG WIDTH="20" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img52.gif"
+ ALT="$2\pi$">, the available floating-point
+        precision corresponds roughly to NDP=3.  This is well below
+        the ultimate limit of NDP=9 set by the capacity of the 32-bit
+        integer IHMSF(4).
+  <DT>3.
+<DD>The absolute value of ANGLE may exceed <IMG WIDTH="20" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img52.gif"
+ ALT="$2\pi$">.  In cases where it
+        does not, it is up to the caller to test for and handle the
+        case where ANGLE is very nearly <IMG WIDTH="20" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img52.gif"
+ ALT="$2\pi$"> and rounds up to <IMG WIDTH="34" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img53.gif"
+ ALT="$360^{\circ}$">,        by testing for IDMSF(1)=360 and setting IDMSF(1-4) to zero.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html786" HREF="node37.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html784" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html778" HREF="node35.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html787" HREF="node37.html">SLA_CR2TF - Radians to Hour,Min,Sec</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html785" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html779" HREF="node35.html">SLA_COMBN - Next Combination</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node37.html b/src/slalib/sun67.htx/node37.html
new file mode 100644
index 0000000..cd25af4
--- /dev/null
+++ b/src/slalib/sun67.htx/node37.html
@@ -0,0 +1,121 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_CR2TF - Radians to Hour,Min,Sec</TITLE>
+<META NAME="description" CONTENT="SLA_CR2TF - Radians to Hour,Min,Sec">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node38.html">
+<LINK REL="previous" HREF="node36.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node38.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html796" HREF="node38.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html794" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html788" HREF="node36.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html797" HREF="node38.html">SLA_CS2C - Spherical to Cartesian</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html795" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html789" HREF="node36.html">SLA_CR2AF - Radians to Deg,Arcmin,Arcsec</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000424000000000000000">SLA_CR2TF - Radians to Hour,Min,Sec</A>
+<A NAME="xref_SLA_CR2TF">&#160;</A><A NAME="SLA_CR2TF">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Convert an angle in radians to hours, minutes, seconds
+(single precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_CR2TF (NDP, ANGLE, SIGN, IHMSF)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NDP</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>number of decimal places of seconds</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ANGLE</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>angle in radians</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>SIGN</EM></TD>
+<TH ALIGN="LEFT"><B>C</B></TH>
+<TD ALIGN="LEFT" NOWRAP>`+' or `-'</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IHMSF</EM></TD>
+<TD ALIGN="LEFT"><B>I(4)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>hours, minutes, seconds, fraction</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>NDP less than zero is interpreted as zero.
+<DT>2.
+<DD>The largest useful value for NDP is determined by the size of
+ANGLE, the format of REAL floating-point numbers on the target
+        machine, and the risk of overflowing IHMSF(4).  For example,
+        on a VAX computer, for ANGLE up to <IMG WIDTH="20" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img52.gif"
+ ALT="$2\pi$">, the available floating-point
+        precision corresponds roughly to NDP=3.  This is well below
+        the ultimate limit of NDP=9 set by the capacity of the 32-bit
+        integer IHMSF(4).
+  <DT>3.
+<DD>The absolute value of ANGLE may exceed <IMG WIDTH="20" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img52.gif"
+ ALT="$2\pi$">.  In cases where it
+        does not, it is up to the caller to test for and handle the
+        case where ANGLE is very nearly <IMG WIDTH="20" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img52.gif"
+ ALT="$2\pi$"> and rounds up to 24&nbsp;hours,
+        by testing for IHMSF(1)=24 and setting IHMSF(1-4) to zero.
+</DL></DL>
+<BR> <HR>
+<A NAME="tex2html796" HREF="node38.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html794" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html788" HREF="node36.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html797" HREF="node38.html">SLA_CS2C - Spherical to Cartesian</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html795" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html789" HREF="node36.html">SLA_CR2AF - Radians to Deg,Arcmin,Arcsec</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node38.html b/src/slalib/sun67.htx/node38.html
new file mode 100644
index 0000000..93d4f63
--- /dev/null
+++ b/src/slalib/sun67.htx/node38.html
@@ -0,0 +1,99 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_CS2C - Spherical to Cartesian</TITLE>
+<META NAME="description" CONTENT="SLA_CS2C - Spherical to Cartesian">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node39.html">
+<LINK REL="previous" HREF="node37.html">
+<LINK REL="up" HREF="node13.html">
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+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html806" HREF="node39.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html804" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html798" HREF="node37.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html807" HREF="node39.html">SLA_CS2C6 - Spherical Pos/Vel to Cartesian</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html805" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html799" HREF="node37.html">SLA_CR2TF - Radians to Hour,Min,Sec</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000425000000000000000">SLA_CS2C - Spherical to Cartesian</A>
+<A NAME="xref_SLA_CS2C">&#160;</A><A NAME="SLA_CS2C">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Spherical coordinates to Cartesian coordinates (single precision).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_CS2C (A, B, V)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A,B</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TH ALIGN="LEFT" NOWRAP>spherical coordinates in radians: <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> <I>etc.</I></TH>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V</EM></TD>
+<TH ALIGN="LEFT"><B>R(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$"> unit vector</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTE:</STRONG>
+<DD>The spherical coordinates are longitude (+ve anticlockwise
+looking from the +ve latitude pole) and latitude.  The
+       Cartesian coordinates are right handed, with the <I>x</I>-axis
+       at zero longitude and latitude, and the <I>z</I>-axis at the
+       +ve latitude pole.
+      </DL>
+<BR> <HR>
+<A NAME="tex2html806" HREF="node39.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html804" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html798" HREF="node37.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html807" HREF="node39.html">SLA_CS2C6 - Spherical Pos/Vel to Cartesian</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html805" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html799" HREF="node37.html">SLA_CR2TF - Radians to Hour,Min,Sec</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node39.html b/src/slalib/sun67.htx/node39.html
new file mode 100644
index 0000000..51bbf4f
--- /dev/null
+++ b/src/slalib/sun67.htx/node39.html
@@ -0,0 +1,114 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_CS2C6 - Spherical Pos/Vel to Cartesian</TITLE>
+<META NAME="description" CONTENT="SLA_CS2C6 - Spherical Pos/Vel to Cartesian">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node40.html">
+<LINK REL="previous" HREF="node38.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node40.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html816" HREF="node40.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html814" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html808" HREF="node38.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html817" HREF="node40.html">SLA_CTF2D - Hour,Min,Sec to Days</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html815" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html809" HREF="node38.html">SLA_CS2C - Spherical to Cartesian</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000426000000000000000">SLA_CS2C6 - Spherical Pos/Vel to Cartesian</A>
+<A NAME="xref_SLA_CS2C6">&#160;</A><A NAME="SLA_CS2C6">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Conversion of position &amp; velocity in spherical coordinates
+to Cartesian coordinates (single precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_CS2C6 (A, B, R, AD, BD, RD, V)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>longitude (radians) - for example <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>B</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>latitude (radians) - for example <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$"></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>R</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>radial coordinate</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AD</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>longitude derivative (radians per unit time)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>BD</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>latitude derivative (radians per unit time)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RD</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>radial derivative</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V</EM></TD>
+<TH ALIGN="LEFT"><B>R(6)</B></TH>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="106" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img51.gif"
+ ALT="$[\,x,y,z,\dot{x},\dot{y},\dot{z}\,]$"></TD>
+</TR>
+</TABLE></DL>
+<BR> <HR>
+<A NAME="tex2html816" HREF="node40.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html814" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html808" HREF="node38.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html817" HREF="node40.html">SLA_CTF2D - Hour,Min,Sec to Days</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html815" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html809" HREF="node38.html">SLA_CS2C - Spherical to Cartesian</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node4.html b/src/slalib/sun67.htx/node4.html
new file mode 100644
index 0000000..81c9586
--- /dev/null
+++ b/src/slalib/sun67.htx/node4.html
@@ -0,0 +1,131 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Example Application</TITLE>
+<META NAME="description" CONTENT="Example Application">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node5.html">
+<LINK REL="previous" HREF="node3.html">
+<LINK REL="up" HREF="node2.html">
+<LINK REL="next" HREF="node5.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html285" HREF="node5.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html283" HREF="node2.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html277" HREF="node3.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html286" HREF="node5.html">Scope</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html284" HREF="node2.html">INTRODUCTION</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html278" HREF="node3.html">Purpose</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION00022000000000000000">
+Example Application</A>
+</H2>
+Here is a simple example of an application program written
+using SLALIB calls:
+<P><PRE>
+         PROGRAM FK4FK5
+   *
+   *  Read a B1950 position from I/O unit 5 and reply on I/O unit 6
+   *  with the J2000 equivalent.  Enter a period to quit.
+   *
+         IMPLICIT NONE
+         CHARACTER C*80,S
+         INTEGER I,J,IHMSF(4),IDMSF(4)
+         DOUBLE PRECISION R4,D4,R5,D5
+         LOGICAL BAD
+
+   *   Loop until a period is entered
+         C = ' '
+         DO WHILE (C(:1).NE.'.')
+
+   *     Read h m s d ' &quot;
+            READ (5,'(A)') C
+            IF (C(:1).NE.'.') THEN
+               BAD = .TRUE.
+
+   *        Decode the RA
+               I = 1
+               CALL sla_DAFIN(C,I,R4,J)
+               IF (J.EQ.0) THEN
+                  R4 = 15D0*R4
+
+   *           Decode the Dec
+                  CALL sla_DAFIN(C,I,D4,J)
+                  IF (J.EQ.0) THEN
+
+   *              FK4 to FK5
+                     CALL sla_FK45Z(R4,D4,1950D0,R5,D5)
+
+   *              Format and output the result
+                     CALL sla_DR2TF(2,R5,S,IHMSF)
+                     CALL sla_DR2AF(1,D5,S,IDMSF)
+                     WRITE (6,
+        :       '(1X,I2.2,2I3.2,''.'',I2.2,2X,A,I2.2,2I3.2,''.'',I1)')
+        :                                                     IHMSF,S,IDMSF
+                     BAD = .FALSE.
+                  END IF
+               END IF
+               IF (BAD) WRITE (6,'(1X,''?'')')
+            END IF
+         END DO
+
+         END
+</PRE>
+In this example, SLALIB not only provides the complicated FK4 to
+FK5 transformation but also
+simplifies the tedious and error-prone tasks
+of decoding and formatting angles
+expressed as hours, minutes <I>etc</I>.  The
+example incorporates range checking, and avoids the
+notorious ``minus zero'' problem (an often-perpetrated bug where
+declinations between <IMG WIDTH="18" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img1.gif"
+ ALT="$0^{\circ}$"> and <IMG WIDTH="30" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img2.gif"
+ ALT="$-1^{\circ}$"> lose their minus
+sign).
+With a little extra elaboration and a few more calls to SLALIB,
+defaulting can be provided (enabling unused fields to
+be replaced with commas to avoid retyping), proper motions
+can be handled, different epochs can be specified, and
+so on.  See the program COCO (SUN/56) for further ideas.
+<P>
+<BR> <HR>
+<A NAME="tex2html285" HREF="node5.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html283" HREF="node2.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html277" HREF="node3.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html286" HREF="node5.html">Scope</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html284" HREF="node2.html">INTRODUCTION</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html278" HREF="node3.html">Purpose</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node40.html b/src/slalib/sun67.htx/node40.html
new file mode 100644
index 0000000..438541e
--- /dev/null
+++ b/src/slalib/sun67.htx/node40.html
@@ -0,0 +1,125 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_CTF2D - Hour,Min,Sec to Days</TITLE>
+<META NAME="description" CONTENT="SLA_CTF2D - Hour,Min,Sec to Days">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node41.html">
+<LINK REL="previous" HREF="node39.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node41.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html826" HREF="node41.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html824" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html818" HREF="node39.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html827" HREF="node41.html">SLA_CTF2R - Hour,Min,Sec to Radians</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html825" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html819" HREF="node39.html">SLA_CS2C6 - Spherical Pos/Vel to Cartesian</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000427000000000000000">SLA_CTF2D - Hour,Min,Sec to Days</A>
+<A NAME="xref_SLA_CTF2D">&#160;</A><A NAME="SLA_CTF2D">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Convert hours, minutes, seconds to days (single precision).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_CTF2D (IHOUR, IMIN, SEC, DAYS, J)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IHOUR</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>hours</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IMIN</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>minutes</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>SEC</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>seconds</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DAYS</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>interval in days</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  0 = OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  1 = IHOUR outside range 0-23</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  2 = IMIN outside range 0-59</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  3 = SEC outside range 0-59.999<IMG WIDTH="21" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img48.gif"
+ ALT="$\cdots$"></TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The result is computed even if any of the range checks fail.
+<DT>2.
+<DD>The sign must be dealt with outside this routine.
+</DL></DL>
+<BR> <HR>
+<A NAME="tex2html826" HREF="node41.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html824" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html818" HREF="node39.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html827" HREF="node41.html">SLA_CTF2R - Hour,Min,Sec to Radians</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html825" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html819" HREF="node39.html">SLA_CS2C6 - Spherical Pos/Vel to Cartesian</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node41.html b/src/slalib/sun67.htx/node41.html
new file mode 100644
index 0000000..bf3cf62
--- /dev/null
+++ b/src/slalib/sun67.htx/node41.html
@@ -0,0 +1,125 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_CTF2R - Hour,Min,Sec to Radians</TITLE>
+<META NAME="description" CONTENT="SLA_CTF2R - Hour,Min,Sec to Radians">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node42.html">
+<LINK REL="previous" HREF="node40.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node42.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html836" HREF="node42.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html834" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html828" HREF="node40.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html837" HREF="node42.html">SLA_DAF2R - Deg,Arcmin,Arcsec to Radians</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html835" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html829" HREF="node40.html">SLA_CTF2D - Hour,Min,Sec to Days</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000428000000000000000">SLA_CTF2R - Hour,Min,Sec to Radians</A>
+<A NAME="xref_SLA_CTF2R">&#160;</A><A NAME="SLA_CTF2R">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Convert hours, minutes, seconds to radians (single precision).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_CTF2R (IHOUR, IMIN, SEC, RAD, J)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IHOUR</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>hours</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IMIN</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>minutes</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>SEC</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>seconds</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RAD</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>angle in radians</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  0 = OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  1 = IHOUR outside range 0-23</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  2 = IMIN outside range 0-59</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  3 = SEC outside range 0-59.999<IMG WIDTH="21" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img48.gif"
+ ALT="$\cdots$"></TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The result is computed even if any of the range checks fail.
+<DT>2.
+<DD>The sign must be dealt with outside this routine.
+</DL></DL>
+<BR> <HR>
+<A NAME="tex2html836" HREF="node42.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html834" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html828" HREF="node40.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html837" HREF="node42.html">SLA_DAF2R - Deg,Arcmin,Arcsec to Radians</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html835" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html829" HREF="node40.html">SLA_CTF2D - Hour,Min,Sec to Days</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node42.html b/src/slalib/sun67.htx/node42.html
new file mode 100644
index 0000000..faed2a4
--- /dev/null
+++ b/src/slalib/sun67.htx/node42.html
@@ -0,0 +1,122 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DAF2R - Deg,Arcmin,Arcsec to Radians</TITLE>
+<META NAME="description" CONTENT="SLA_DAF2R - Deg,Arcmin,Arcsec to Radians">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node43.html">
+<LINK REL="previous" HREF="node41.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node43.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html846" HREF="node43.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html844" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html838" HREF="node41.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html847" HREF="node43.html">SLA_DAFIN - Sexagesimal character string to angle</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html845" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html839" HREF="node41.html">SLA_CTF2R - Hour,Min,Sec to Radians</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000429000000000000000">SLA_DAF2R - Deg,Arcmin,Arcsec to Radians</A>
+<A NAME="xref_SLA_DAF2R">&#160;</A><A NAME="SLA_DAF2R">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Convert degrees, arcminutes, arcseconds to radians
+(double precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DAF2R (IDEG, IAMIN, ASEC, RAD, J)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IDEG</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>degrees</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IAMIN</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>arcminutes</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ASEC</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>arcseconds</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RAD</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>angle in radians</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  1 = IDEG outside range 0-359</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  2 = IAMIN outside range 0-59</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  3 = ASEC outside range 0-59.999<IMG WIDTH="21" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img48.gif"
+ ALT="$\cdots$"></TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The result is computed even if any of the range checks fail.
+<DT>2.
+<DD>The sign must be dealt with outside this routine.
+</DL></DL>
+<BR> <HR>
+<A NAME="tex2html846" HREF="node43.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html844" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html838" HREF="node41.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html847" HREF="node43.html">SLA_DAFIN - Sexagesimal character string to angle</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html845" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html839" HREF="node41.html">SLA_CTF2R - Hour,Min,Sec to Radians</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node43.html b/src/slalib/sun67.htx/node43.html
new file mode 100644
index 0000000..8559153
--- /dev/null
+++ b/src/slalib/sun67.htx/node43.html
@@ -0,0 +1,229 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DAFIN - Sexagesimal character string to angle</TITLE>
+<META NAME="description" CONTENT="SLA_DAFIN - Sexagesimal character string to angle">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node44.html">
+<LINK REL="previous" HREF="node42.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node44.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html856" HREF="node44.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html854" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html848" HREF="node42.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html857" HREF="node44.html">SLA_DAT - TAI-UTC</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html855" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html849" HREF="node42.html">SLA_DAF2R - Deg,Arcmin,Arcsec to Radians</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000430000000000000000">SLA_DAFIN - Sexagesimal character string to angle</A>
+<A NAME="xref_SLA_DAFIN">&#160;</A><A NAME="SLA_DAFIN">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Decode a free-format sexagesimal string (degrees, arcminutes,
+arcseconds) into a double precision floating point
+         number (radians).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DAFIN (STRING, NSTRT, DRESLT, JF)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>STRING</EM></TD>
+<TH ALIGN="LEFT"><B>C*(*)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>string containing deg, arcmin, arcsec fields</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NSTRT</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>pointer to start of decode (beginning of STRING = 1)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NSTRT</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>advanced past the decoded angle</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DRESLT</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>angle in radians</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JF</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>    0 = OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  +1 = default, DRESLT unchanged (note 2)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -1 = bad degrees (note 3)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -2 = bad arcminutes (note 3)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -3 = bad arcseconds (note 3)</TD>
+</TR>
+</TABLE></DL>
+<P><DL>
+<DT><STRONG>EXAMPLE</STRONG>
+<DD>: <BR>
+<BR>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TH ALIGN="LEFT"><I>argument</I></TH>
+<TH ALIGN="LEFT"><I>before</I></TH>
+<TH ALIGN="LEFT"><I>after</I></TH>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT">&nbsp;</TD>
+<TD ALIGN="LEFT">&nbsp;</TD>
+<TD ALIGN="LEFT">&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT">STRING</TD>
+<TD ALIGN="LEFT">'<code>-57 17 44.806  12 34 56.7</code>'</TD>
+<TD ALIGN="LEFT">unchanged</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT">NSTRT</TD>
+<TD ALIGN="LEFT">1</TD>
+<TD ALIGN="LEFT">16 (<I>i.e.</I> pointing to 12...)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT">RESLT</TD>
+<TD ALIGN="LEFT">-</TD>
+<TD ALIGN="LEFT">-1.00000<TT>D0</TT></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT">JF</TD>
+<TD ALIGN="LEFT">-</TD>
+<TD ALIGN="LEFT">&nbsp;</TD>
+</TR>
+</TABLE>
+ <DT><DD> A further call to sla_DAFIN, without adjustment of NSTRT, will
+       decode the second angle, <IMG WIDTH="90" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img4.gif"
+ ALT="$12^{\circ}\,34^{'}\,56^{''}.7$">.</DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>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 sla_DFLTIN routine and is free-format.
+  <DT>2.
+<DD>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 DRESLT is
+   unchanged.  In all other cases DRESLT is changed.
+  <DT>3.
+<DD>Range checking:
+   <UL>
+<LI> The degrees field is not range checked.  However, it is
+     expected to be integral unless the other two fields are absent.
+<LI> 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...
+<LI> The arcseconds field is expected to be 0-59.9999...
+<LI> Decoding continues even when a check has failed.  Under these
+     circumstances the field takes the supplied value, defaulting to
+     zero, and the result DRESLT is computed and returned.
+   </UL>
+   <DT>4.
+<DD>Further fields after the three expected ones are not treated as
+    an error.  The pointer NSTRT is left in the correct state for
+    further decoding with the present routine or with sla_DFLTIN
+    <I>etc</I>.  See the example, above.
+   <DT>5.
+<DD>If STRING contains hours, minutes, seconds instead of
+    degrees <I>etc</I>,
+    or if the required units are turns (or days) instead of radians,
+    the result DRESLT should be multiplied as follows: <BR>
+<BR>
+<BR>
+    <TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TH ALIGN="LEFT"><I>for STRING</I></TH>
+<TH ALIGN="LEFT"><I>to obtain</I></TH>
+<TH ALIGN="LEFT"><I>multiply DRESLT by</I></TH>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT">&nbsp;</TD>
+<TD ALIGN="LEFT">&nbsp;</TD>
+<TD ALIGN="LEFT">&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><IMG WIDTH="10" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img5.gif"
+ ALT="${\circ}$">&nbsp;&nbsp;'&nbsp;&nbsp;''</TD>
+<TD ALIGN="LEFT">radians</TD>
+<TD ALIGN="LEFT">1.0<TT>D0</TT></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><IMG WIDTH="10" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img5.gif"
+ ALT="${\circ}$">&nbsp;&nbsp;'&nbsp;&nbsp;''</TD>
+<TD ALIGN="LEFT">turns</TD>
+<TD ALIGN="LEFT"><IMG WIDTH="227" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img6.gif"
+ ALT="$1/{2 \pi} = 0.1591549430918953358$"><TT>D0</TT></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT">h m s</TD>
+<TD ALIGN="LEFT">radians</TD>
+<TD ALIGN="LEFT">15.0<TT>D0</TT></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT">h m s</TD>
+<TD ALIGN="LEFT">days</TD>
+<TD ALIGN="LEFT"><IMG WIDTH="235" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img7.gif"
+ ALT="$15/{2\pi} = 2.3873241463784300365$"><TT>D0</TT></TD>
+</TR>
+</TABLE></DL></DL>
+<BR> <HR>
+<A NAME="tex2html856" HREF="node44.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html854" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html848" HREF="node42.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html857" HREF="node44.html">SLA_DAT - TAI-UTC</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html855" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html849" HREF="node42.html">SLA_DAF2R - Deg,Arcmin,Arcsec to Radians</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node44.html b/src/slalib/sun67.htx/node44.html
new file mode 100644
index 0000000..791aba6
--- /dev/null
+++ b/src/slalib/sun67.htx/node44.html
@@ -0,0 +1,109 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DAT - TAI-UTC</TITLE>
+<META NAME="description" CONTENT="SLA_DAT - TAI-UTC">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html867" HREF="node45.html">SLA_DAV2M - Rotation Matrix from Axial Vector</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html865" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html859" HREF="node43.html">SLA_DAFIN - Sexagesimal character string to angle</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000431000000000000000">SLA_DAT - TAI-UTC</A>
+<A NAME="xref_SLA_DAT">&#160;</A><A NAME="SLA_DAT">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Increment to be applied to Coordinated Universal Time UTC to give
+International Atomic Time TAI.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>D&nbsp;=&nbsp;sla_DAT (UTC)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>UTC</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>UTC date as a modified JD (JD-2400000.5)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_DAT</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>TAI-UTC in seconds</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The UTC is specified to be a date rather than a time to indicate
+that care needs to be taken not to specify an instant which lies
+within a leap second.  Though in most cases UTC can include the
+       fractional part, correct behaviour on the day of a leap second
+       can be guaranteed only up to the end of the second
+       <IMG WIDTH="82" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img54.gif"
+ ALT="$23^{\rm h}\,59^{\rm m}\,59^{\rm s}$">. <DT>2.
+<DD>UTC began at 1960 January 1.  To specify a UTC prior to this
+       date would be meaningless;  in such cases the parameters
+       for the year 1960 are used by default.
+ <DT>3.
+<DD>This routine has to be updated on each occasion that a
+       leap second is announced, and programs using it relinked.
+       Refer to the program source code for information on when the
+       most recent leap second was added.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html866" HREF="node45.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html867" HREF="node45.html">SLA_DAV2M - Rotation Matrix from Axial Vector</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html865" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html859" HREF="node43.html">SLA_DAFIN - Sexagesimal character string to angle</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node45.html b/src/slalib/sun67.htx/node45.html
new file mode 100644
index 0000000..4e11c46
--- /dev/null
+++ b/src/slalib/sun67.htx/node45.html
@@ -0,0 +1,103 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DAV2M - Rotation Matrix from Axial Vector</TITLE>
+<META NAME="description" CONTENT="SLA_DAV2M - Rotation Matrix from Axial Vector">
+<META NAME="keywords" CONTENT="sun67">
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+<A NAME="tex2html874" HREF="node13.html">
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+<A NAME="tex2html868" HREF="node44.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html877" HREF="node46.html">SLA_DBEAR - Direction Between Points on a Sphere</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html875" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html869" HREF="node44.html">SLA_DAT - TAI-UTC</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000432000000000000000">SLA_DAV2M - Rotation Matrix from Axial Vector</A>
+<A NAME="xref_SLA_DAV2M">&#160;</A><A NAME="SLA_DAV2M">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Form the rotation matrix corresponding to a given axial vector
+(double precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DAV2M (AXVEC, RMAT)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AXVEC</EM></TD>
+<TH ALIGN="LEFT"><B>D(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>axial vector (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RMAT</EM></TD>
+<TH ALIGN="LEFT"><B>D(3,3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>rotation matrix</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>A rotation matrix describes a rotation about some arbitrary axis.
+The axis is called the <I>Euler axis</I>, and the angle through which the
+reference frame rotates is called the <I>Euler angle</I>.  The axial
+        vector supplied to this routine has the same direction as the
+        Euler axis, and its magnitude is the Euler angle in radians.
+  <DT>2.
+<DD>If AXVEC is null, the unit matrix is returned.
+  <DT>3.
+<DD>The reference frame rotates clockwise as seen looking along
+        the axial vector from the origin.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html876" HREF="node46.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html874" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html868" HREF="node44.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html877" HREF="node46.html">SLA_DBEAR - Direction Between Points on a Sphere</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html875" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html869" HREF="node44.html">SLA_DAT - TAI-UTC</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node46.html b/src/slalib/sun67.htx/node46.html
new file mode 100644
index 0000000..39a1ffd
--- /dev/null
+++ b/src/slalib/sun67.htx/node46.html
@@ -0,0 +1,123 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DBEAR - Direction Between Points on a Sphere</TITLE>
+<META NAME="description" CONTENT="SLA_DBEAR - Direction Between Points on a Sphere">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node47.html">
+<LINK REL="previous" HREF="node45.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node47.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html886" HREF="node47.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html884" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html878" HREF="node45.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html887" HREF="node47.html">SLA_DBJIN - Decode String to B/J Epoch (DP)</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html885" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html879" HREF="node45.html">SLA_DAV2M - Rotation Matrix from Axial Vector</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000433000000000000000">SLA_DBEAR - Direction Between Points on a Sphere</A>
+<A NAME="xref_SLA_DBEAR">&#160;</A><A NAME="SLA_DBEAR">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Returns the bearing (position angle) of one point on a
+sphere relative to another (double precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>D&nbsp;=&nbsp;sla_DBEAR (A1, B1, A2, B2)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A1,B1</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>spherical coordinates of one point</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A2,B2</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>spherical coordinates of the other point</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_DBEAR</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>bearing from first point to second</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The spherical coordinates are <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">,<IMG WIDTH="38" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img46.gif"
+ ALT="$[\lambda,\phi]$"> <I>etc.</I>, in radians.
+<DT>2.
+<DD>The result is the bearing (position angle), in radians,
+       of point [A2,B2] as seen
+       from point [A1,B1].  It is in the range <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$">.  The sense
+       is such that if [A2,B2]
+       is a small distance due east of [A1,B1] the result
+       is about <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img14.gif"
+ ALT="$+\pi/2$">. Zero is returned
+       if the two points are coincident.
+ <DT>3.
+<DD>If either B-coordinate is outside the range <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img15.gif"
+ ALT="$\pm\pi/2$">, the
+       result may correspond to ``the long way round''.
+ <DT>4.
+<DD>The routine sla_DPAV performs an equivalent function except
+       that the points are specified in the form of Cartesian unit
+       vectors.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html886" HREF="node47.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html884" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html878" HREF="node45.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html887" HREF="node47.html">SLA_DBJIN - Decode String to B/J Epoch (DP)</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html885" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html879" HREF="node45.html">SLA_DAV2M - Rotation Matrix from Axial Vector</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node47.html b/src/slalib/sun67.htx/node47.html
new file mode 100644
index 0000000..5d8e877
--- /dev/null
+++ b/src/slalib/sun67.htx/node47.html
@@ -0,0 +1,157 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DBJIN - Decode String to B/J Epoch (DP)</TITLE>
+<META NAME="description" CONTENT="SLA_DBJIN - Decode String to B/J Epoch (DP)">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node48.html">
+<LINK REL="previous" HREF="node46.html">
+<LINK REL="up" HREF="node13.html">
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+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html896" HREF="node48.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html894" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html888" HREF="node46.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html897" HREF="node48.html">SLA_DC62S - Cartesian 6-Vector to Spherical</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html895" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html889" HREF="node46.html">SLA_DBEAR - Direction Between Points on a Sphere</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000434000000000000000">SLA_DBJIN - Decode String to B/J Epoch (DP)</A>
+<A NAME="xref_SLA_DBJIN">&#160;</A><A NAME="SLA_DBJIN">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Decode a character string into a DOUBLE PRECISION number,
+with special provision for Besselian and Julian epochs.
+         The string syntax is as for sla_DFLTIN, prefixed by
+         an optional `B' or `J'.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DBJIN (STRING, NSTRT, DRESLT, J1, J2)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>STRING</EM></TD>
+<TH ALIGN="LEFT"><B>C</B></TH>
+<TD ALIGN="LEFT" NOWRAP>string containing field to be decoded</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NSTRT</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>pointer to first character of field in string</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NSTRT</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>incremented past the decoded field</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DRESLT</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>result</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J1</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>DFLTIN status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -1 = -OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>    0 = +OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>    1 = null field</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>    2 = error</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J2</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>syntax flag:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>    0 = normal DFLTIN syntax</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>    1 = `B' or `b'</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>    2 = `J' or `j'</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The purpose of the syntax extensions is to help cope with mixed
+FK4 and FK5 data, allowing fields such as `B1950' or `J2000'
+to be decoded.
+  <DT>2.
+<DD>In addition to the syntax accepted by sla_DFLTIN,
+        the following two extensions are recognized by sla_DBJIN:
+        <DL COMPACT>
+<DT>(a)
+<DD>A valid non-null field preceded by the character `B'
+(or `b') is accepted.
+         <DT>(b)
+<DD>A valid non-null field preceded by the character `J'
+               (or `j') is accepted.
+         </DL>
+  <DT>3.
+<DD>The calling program is told of the `B' or `J' through an
+        supplementary status argument.  The rest of
+        the arguments are as for sla_DFLTIN.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html896" HREF="node48.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html894" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html888" HREF="node46.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html897" HREF="node48.html">SLA_DC62S - Cartesian 6-Vector to Spherical</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html895" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html889" HREF="node46.html">SLA_DBEAR - Direction Between Points on a Sphere</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node48.html b/src/slalib/sun67.htx/node48.html
new file mode 100644
index 0000000..95057e4
--- /dev/null
+++ b/src/slalib/sun67.htx/node48.html
@@ -0,0 +1,110 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DC62S - Cartesian 6-Vector to Spherical</TITLE>
+<META NAME="description" CONTENT="SLA_DC62S - Cartesian 6-Vector to Spherical">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
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+<A NAME="tex2html904" HREF="node13.html">
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+<A NAME="tex2html898" HREF="node47.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html907" HREF="node49.html">SLA_DCC2S - Cartesian to Spherical</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html905" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html899" HREF="node47.html">SLA_DBJIN - Decode String to B/J Epoch (DP)</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000435000000000000000">SLA_DC62S - Cartesian 6-Vector to Spherical</A>
+<A NAME="xref_SLA_DC62S">&#160;</A><A NAME="SLA_DC62S">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Conversion of position &amp; velocity in Cartesian coordinates
+to spherical coordinates (double precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DC62S (V, A, B, R, AD, BD, RD)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V</EM></TD>
+<TH ALIGN="LEFT"><B>D(6)</B></TH>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="106" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img51.gif"
+ ALT="$[\,x,y,z,\dot{x},\dot{y},\dot{z}\,]$"></TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>longitude (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>B</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>latitude (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>R</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>radial coordinate</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AD</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>longitude derivative (radians per unit time)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>BD</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>latitude derivative (radians per unit time)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RD</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>radial derivative</TD>
+</TR>
+</TABLE></DL>
+<BR> <HR>
+<A NAME="tex2html906" HREF="node49.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html904" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html898" HREF="node47.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html907" HREF="node49.html">SLA_DCC2S - Cartesian to Spherical</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html905" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html899" HREF="node47.html">SLA_DBJIN - Decode String to B/J Epoch (DP)</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node49.html b/src/slalib/sun67.htx/node49.html
new file mode 100644
index 0000000..86f582e
--- /dev/null
+++ b/src/slalib/sun67.htx/node49.html
@@ -0,0 +1,103 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DCC2S - Cartesian to Spherical</TITLE>
+<META NAME="description" CONTENT="SLA_DCC2S - Cartesian to Spherical">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
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+<LINK REL="previous" HREF="node48.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node50.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html916" HREF="node50.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html914" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html908" HREF="node48.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html917" HREF="node50.html">SLA_DCMPF - Interpret Linear Fit</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html915" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html909" HREF="node48.html">SLA_DC62S - Cartesian 6-Vector to Spherical</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000436000000000000000">SLA_DCC2S - Cartesian to Spherical</A>
+<A NAME="xref_SLA_DCC2S">&#160;</A><A NAME="SLA_DCC2S">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Cartesian coordinates to spherical coordinates (double precision).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DCC2S (V, A, B)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V</EM></TD>
+<TH ALIGN="LEFT"><B>D(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$"> vector</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A,B</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>spherical coordinates in radians</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The spherical coordinates are longitude (+ve anticlockwise
+looking from the +ve latitude pole) and latitude.  The
+Cartesian coordinates are right handed, with the <I>x</I>-axis
+        at zero longitude and latitude, and the <I>z</I>-axis at the
+        +ve latitude pole.
+  <DT>2.
+<DD>If V is null, zero A and B are returned.
+  <DT>3.
+<DD>At either pole, zero A is returned.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html916" HREF="node50.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html914" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html908" HREF="node48.html">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html917" HREF="node50.html">SLA_DCMPF - Interpret Linear Fit</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html915" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html909" HREF="node48.html">SLA_DC62S - Cartesian 6-Vector to Spherical</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node5.html b/src/slalib/sun67.htx/node5.html
new file mode 100644
index 0000000..3920866
--- /dev/null
+++ b/src/slalib/sun67.htx/node5.html
@@ -0,0 +1,83 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Scope</TITLE>
+<META NAME="description" CONTENT="Scope">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node6.html">
+<LINK REL="previous" HREF="node4.html">
+<LINK REL="up" HREF="node2.html">
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+</HEAD>
+<BODY >
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+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html296" HREF="node6.html">Objectives</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html294" HREF="node2.html">INTRODUCTION</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html288" HREF="node4.html">Example Application</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION00023000000000000000">
+Scope</A>
+</H2>
+SLALIB contains 183 routines covering the following topics:
+<UL>
+<LI> String Decoding,
+      Sexagesimal Conversions
+<LI> Angles, Vectors &amp; Rotation Matrices
+<LI> Calendars,
+      Timescales
+<LI> Precession &amp; Nutation
+<LI> Proper Motion
+<LI> FK4/FK5/Hipparcos,
+      Elliptic Aberration
+<LI> Geocentric Coordinates
+<LI> Apparent &amp; Observed Place
+<LI> Azimuth &amp; Elevation
+<LI> Refraction &amp; Air Mass
+<LI> Ecliptic,
+      Galactic,
+      Supergalactic Coordinates
+<LI> Ephemerides
+<LI> Astrometry
+<LI> Numerical Methods
+</UL>
+<BR> <HR>
+<A NAME="tex2html295" HREF="node6.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html293" HREF="node2.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html287" HREF="node4.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html296" HREF="node6.html">Objectives</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html294" HREF="node2.html">INTRODUCTION</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html288" HREF="node4.html">Example Application</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node50.html b/src/slalib/sun67.htx/node50.html
new file mode 100644
index 0000000..555de30
--- /dev/null
+++ b/src/slalib/sun67.htx/node50.html
@@ -0,0 +1,166 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DCMPF - Interpret Linear Fit</TITLE>
+<META NAME="description" CONTENT="SLA_DCMPF - Interpret Linear Fit">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node51.html">
+<LINK REL="previous" HREF="node49.html">
+<LINK REL="up" HREF="node13.html">
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+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html927" HREF="node51.html">SLA_DCS2C - Spherical to Cartesian</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html925" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html919" HREF="node49.html">SLA_DCC2S - Cartesian to Spherical</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000437000000000000000">SLA_DCMPF - Interpret Linear Fit</A>
+<A NAME="xref_SLA_DCMPF">&#160;</A><A NAME="SLA_DCMPF">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Decompose an <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> linear fit into its constituent parameters:
+zero points, scales, nonperpendicularity and orientation.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DCMPF (COEFFS,XZ,YZ,XS,YS,PERP,ORIENT)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>COEFFS</EM></TD>
+<TH ALIGN="LEFT"><B>D(6)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>transformation coefficients (see note)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>XZ</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TH ALIGN="LEFT" NOWRAP><I>x</I> zero point</TH>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>YZ</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP><I>y</I> zero point</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>XS</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP><I>x</I> scale</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>YS</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP><I>y</I> scale</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PERP</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>nonperpendicularity (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ORIENT</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>orientation (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The model relates two sets of <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> coordinates as follows.
+Naming the six elements of COEFFS <I>a</I>,<I>b</I>,<I>c</I>,<I>d</I>,<I>e</I> &amp; <I>f</I>,
+the model transforms coordinates <IMG WIDTH="53" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img55.gif"
+ ALT="$[x_{1},y_{1}\,]$"> into coordinates
+        <IMG WIDTH="53" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img56.gif"
+ ALT="$[x_{2},y_{2}\,]$"> as follows:
+        <BLOCKQUOTE><I>x<SUB>2</SUB></I> = <I>a</I> + <I>bx<SUB>1</SUB></I> + <I>cy<SUB>1</SUB></I> <BR>
+         <I>y<SUB>2</SUB></I> = <I>d</I> + <I>ex<SUB>1</SUB></I> + <I>fy<SUB>1</SUB></I></BLOCKQUOTE>
+        The sla_DCMPF routine decomposes this transformation
+        into four steps:
+        <DL COMPACT>
+<DT>(a)
+<DD>Zero points:
+<BLOCKQUOTE><IMG WIDTH="96" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
+ SRC="img57.gif"
+ ALT="$x' = x_{1} + {\rm XZ}$"> <BR>
+               <IMG WIDTH="94" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
+ SRC="img58.gif"
+ ALT="$y' = y_{1} + {\rm YZ}$"></BLOCKQUOTE>
+        <DT>(b)
+<DD>Scales:
+              <BLOCKQUOTE><IMG WIDTH="76" HEIGHT="16" ALIGN="BOTTOM" BORDER="0"
+ SRC="img59.gif"
+ ALT="$x'' = x' {\rm XS}$"> <BR>
+               <IMG WIDTH="74" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
+ SRC="img60.gif"
+ ALT="$y'' = y' {\rm YS}$"></BLOCKQUOTE>
+        <DT>(c)
+<DD>Nonperpendicularity:
+              <BLOCKQUOTE><IMG WIDTH="287" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
+ SRC="img61.gif"
+ ALT="$x''' = + x'' \cos {\rm PERP}/2 + y'' \sin {\rm PERP}/2$"> <BR>
+               <IMG WIDTH="286" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
+ SRC="img62.gif"
+ ALT="$y''' = + x'' \sin {\rm PERP}/2 + y'' \cos {\rm PERP}/2$"></BLOCKQUOTE>
+        <DT>(d)
+<DD>Orientation:
+              <BLOCKQUOTE><IMG WIDTH="298" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
+ SRC="img63.gif"
+ ALT="$x_{2} = + x''' \cos {\rm ORIENT} +
+ y''' \sin {\rm ORIENT}$"> <BR>
+               <IMG WIDTH="297" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
+ SRC="img64.gif"
+ ALT="$y_{2} = - x''' \sin {\rm ORIENT} +
+ y''' \cos {\rm ORIENT}$"></BLOCKQUOTE></DL>
+  <DT>2.
+<DD>See also sla_FITXY, sla_PXY, sla_INVF, sla_XY2XY.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html926" HREF="node51.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html924" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html918" HREF="node49.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html927" HREF="node51.html">SLA_DCS2C - Spherical to Cartesian</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html925" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html919" HREF="node49.html">SLA_DCC2S - Cartesian to Spherical</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node51.html b/src/slalib/sun67.htx/node51.html
new file mode 100644
index 0000000..1a8cb1b
--- /dev/null
+++ b/src/slalib/sun67.htx/node51.html
@@ -0,0 +1,99 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DCS2C - Spherical to Cartesian</TITLE>
+<META NAME="description" CONTENT="SLA_DCS2C - Spherical to Cartesian">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
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+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html934" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html928" HREF="node50.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html937" HREF="node52.html">SLA_DD2TF - Days to Hour,Min,Sec</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html935" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html929" HREF="node50.html">SLA_DCMPF - Interpret Linear Fit</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000438000000000000000">SLA_DCS2C - Spherical to Cartesian</A>
+<A NAME="xref_SLA_DCS2C">&#160;</A><A NAME="SLA_DCS2C">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Spherical coordinates to Cartesian coordinates (double precision).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DCS2C (A, B, V)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A,B</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TH ALIGN="LEFT" NOWRAP>spherical coordinates in radians: <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> <I>etc.</I></TH>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V</EM></TD>
+<TH ALIGN="LEFT"><B>D(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$"> unit vector</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTE:</STRONG>
+<DD>The spherical coordinates are longitude (+ve anticlockwise
+looking from the +ve latitude pole) and latitude.  The
+       Cartesian coordinates are right handed, with the <I>x</I>-axis
+       at zero longitude and latitude, and the <I>z</I>-axis at the
+       +ve latitude pole.
+      </DL>
+<BR> <HR>
+<A NAME="tex2html936" HREF="node52.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html937" HREF="node52.html">SLA_DD2TF - Days to Hour,Min,Sec</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html935" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html929" HREF="node50.html">SLA_DCMPF - Interpret Linear Fit</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node52.html b/src/slalib/sun67.htx/node52.html
new file mode 100644
index 0000000..52cca63
--- /dev/null
+++ b/src/slalib/sun67.htx/node52.html
@@ -0,0 +1,115 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DD2TF - Days to Hour,Min,Sec</TITLE>
+<META NAME="description" CONTENT="SLA_DD2TF - Days to Hour,Min,Sec">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html947" HREF="node53.html">SLA_DE2H - to Az,El</A>
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+<B>Up:</B> <A NAME="tex2html945" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html939" HREF="node51.html">SLA_DCS2C - Spherical to Cartesian</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000439000000000000000">SLA_DD2TF - Days to Hour,Min,Sec</A>
+<A NAME="xref_SLA_DD2TF">&#160;</A><A NAME="SLA_DD2TF">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Convert an interval in days into hours, minutes, seconds
+(double precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DD2TF (NDP, DAYS, SIGN, IHMSF)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NDP</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>number of decimal places of seconds</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DAYS</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>interval in days</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>SIGN</EM></TD>
+<TH ALIGN="LEFT"><B>C</B></TH>
+<TD ALIGN="LEFT" NOWRAP>`+' or `-'</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IHMSF</EM></TD>
+<TD ALIGN="LEFT"><B>I(4)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>hours, minutes, seconds, fraction</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>NDP less than zero is interpreted as zero.
+<DT>2.
+<DD>The largest useful value for NDP is determined by the size
+of DAYS, the format of DOUBLE PRECISION floating-point numbers
+        on the target machine, and the risk of overflowing IHMSF(4).
+        For example, on a VAX computer, for DAYS up to 1D0, the available
+        floating-point precision corresponds roughly to NDP=12.  However,
+        the practical limit is NDP=9, set by the capacity of the 32-bit
+        integer IHMSF(4).
+  <DT>3.
+<DD>The absolute value of DAYS may exceed 1D0.  In cases where it
+        does not, it is up to the caller to test for and handle the
+        case where DAYS is very nearly 1D0 and rounds up to 24&nbsp;hours,
+        by testing for IHMSF(1)=24 and setting IHMSF(1-4) to zero.
+</DL></DL>
+<BR> <HR>
+<A NAME="tex2html946" HREF="node53.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html944" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html938" HREF="node51.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html947" HREF="node53.html">SLA_DE2H - to Az,El</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html945" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html939" HREF="node51.html">SLA_DCS2C - Spherical to Cartesian</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node53.html b/src/slalib/sun67.htx/node53.html
new file mode 100644
index 0000000..05a6c56
--- /dev/null
+++ b/src/slalib/sun67.htx/node53.html
@@ -0,0 +1,145 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DE2H - to Az,El</TITLE>
+<META NAME="description" CONTENT="SLA_DE2H - to Az,El">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node54.html">
+<LINK REL="previous" HREF="node52.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node54.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html956" HREF="node54.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html954" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html948" HREF="node52.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html957" HREF="node54.html">SLA_DEULER - Euler Angles to Rotation Matrix</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html955" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html949" HREF="node52.html">SLA_DD2TF - Days to Hour,Min,Sec</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000440000000000000000">&#160;</A><A NAME="xref_SLA_DE2H">&#160;</A><A NAME="SLA_DE2H">&#160;</A>
+<BR>
+SLA_DE2H - <IMG WIDTH="27" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img65.gif"
+ ALT="$h,\delta$"> to Az,El
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Equatorial to horizon coordinates
+(double precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DE2H (HA, DEC, PHI, AZ, EL)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>HA</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>hour angle (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DEC</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>declination (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PHI</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>latitude (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AZ</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>azimuth (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EL</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>elevation (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Azimuth is returned in the range <IMG WIDTH="43" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img66.gif"
+ ALT="$0\!-\!2\pi$">;  north is zero,
+and east is <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img14.gif"
+ ALT="$+\pi/2$">.  Elevation is returned in the range
+<IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$">.  <DT>2.
+<DD>The latitude must be geodetic.  In critical applications,
+        corrections for polar motion should be applied.
+  <DT>3.
+<DD>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 <I>observed</I> <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$">, and the elevation
+        <I>in vacuo</I>, which would require the <I>topocentric</I>
+        <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$">.        If the effects of diurnal aberration can be neglected, the
+        <I>apparent</I> <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$"> may be used instead of the topocentric
+        <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$">.  <DT>4.
+<DD>No range checking of arguments is carried out.
+  <DT>5.
+<DD>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.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html956" HREF="node54.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html954" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html948" HREF="node52.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html957" HREF="node54.html">SLA_DEULER - Euler Angles to Rotation Matrix</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html955" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html949" HREF="node52.html">SLA_DD2TF - Days to Hour,Min,Sec</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node54.html b/src/slalib/sun67.htx/node54.html
new file mode 100644
index 0000000..1fc9a2a
--- /dev/null
+++ b/src/slalib/sun67.htx/node54.html
@@ -0,0 +1,127 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DEULER - Euler Angles to Rotation Matrix</TITLE>
+<META NAME="description" CONTENT="SLA_DEULER - Euler Angles to Rotation Matrix">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
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+<LINK REL="next" HREF="node55.html">
+<LINK REL="previous" HREF="node53.html">
+<LINK REL="up" HREF="node13.html">
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+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html966" HREF="node55.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html964" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html958" HREF="node53.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html967" HREF="node55.html">SLA_DFLTIN - Decode a Double Precision Number</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html965" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html959" HREF="node53.html">SLA_DE2H - to Az,El</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000441000000000000000">SLA_DEULER - Euler Angles to Rotation Matrix</A>
+<A NAME="xref_SLA_DEULER">&#160;</A><A NAME="SLA_DEULER">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Form a rotation matrix from the Euler angles - three
+successive rotations about specified Cartesian axes
+         (double precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DEULER (ORDER, PHI, THETA, PSI, RMAT)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ORDER</EM></TD>
+<TH ALIGN="LEFT"><B>C</B></TH>
+<TD ALIGN="LEFT" NOWRAP>specifies about which axes the rotations occur</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PHI</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>1st rotation (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>THETA</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>2nd rotation (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PSI</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>3rd rotation (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RMAT</EM></TD>
+<TH ALIGN="LEFT"><B>D(3,3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>rotation matrix</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>A rotation is positive when the reference frame rotates
+anticlockwise as seen looking towards the origin from the
+positive region of the specified axis.
+ <DT>2.
+<DD>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 <I>z</I>-axis, followed by THETA radians about the resulting
+       <I>x</I>-axis,
+       then PSI radians about the resulting <I>z</I>-axis.
+ <DT>3.
+<DD>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 <I>xyz</I> (<IMG WIDTH="44" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img67.gif"
+ ALT="$\equiv123$">)       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.  Zero rotations produces a unit RMAT.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html966" HREF="node55.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html964" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html958" HREF="node53.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html967" HREF="node55.html">SLA_DFLTIN - Decode a Double Precision Number</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html965" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html959" HREF="node53.html">SLA_DE2H - to Az,El</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node55.html b/src/slalib/sun67.htx/node55.html
new file mode 100644
index 0000000..390f876
--- /dev/null
+++ b/src/slalib/sun67.htx/node55.html
@@ -0,0 +1,200 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DFLTIN - Decode a Double Precision Number</TITLE>
+<META NAME="description" CONTENT="SLA_DFLTIN - Decode a Double Precision Number">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node56.html">
+<LINK REL="previous" HREF="node54.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node56.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html976" HREF="node56.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html974" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html968" HREF="node54.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html977" HREF="node56.html">SLA_DH2E - Az,El to</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html975" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html969" HREF="node54.html">SLA_DEULER - Euler Angles to Rotation Matrix</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000442000000000000000">SLA_DFLTIN - Decode a Double Precision Number</A>
+<A NAME="xref_SLA_DFLTIN">&#160;</A><A NAME="SLA_DFLTIN">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Convert free-format input into double precision floating point.
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DFLTIN (STRING, NSTRT, DRESLT, JFLAG)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>STRING</EM></TD>
+<TH ALIGN="LEFT"><B>C</B></TH>
+<TD ALIGN="LEFT" NOWRAP>string containing number to be decoded</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NSTRT</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>pointer to where decoding is to commence</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DRESLT</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>current value of result</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NSTRT</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>advanced to next number</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DRESLT</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>result</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JFLAG</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status: -1&nbsp;=&nbsp;-OK, 0&nbsp;=&nbsp;+OK, 1&nbsp;=&nbsp;null result, 2&nbsp;=&nbsp;error</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The reason sla_DFLTIN has separate `OK' status values
+for + and - is to enable minus zero to be detected.
+This is of crucial importance
+       when decoding mixed-radix numbers.  For example, an angle
+       expressed as degrees, arcminutes and arcseconds may have a
+       leading minus sign but a zero degrees field.
+ <DT>2.
+<DD>A TAB is interpreted as a space, and lowercase characters are
+       interpreted as uppercase.  <I>n.b.</I> The test for TAB is
+       ASCII-specific.
+ <DT>3.
+<DD>The basic format is the sequence of fields <IMG WIDTH="78" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img68.gif"
+ ALT="$\pm n.n x \pm n$">,       where <IMG WIDTH="15" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img30.gif"
+ ALT="$\pm$"> is a sign
+       character `+' or `-', <I>n</I> means a string of decimal digits,
+       `.' is a decimal point, and <I>x</I>, which indicates an exponent,
+       means `D' or `E'.  Various combinations of these fields can be
+       omitted, and embedded blanks are permissible in certain places.
+ <DT>4.
+<DD>Spaces:
+       <UL>
+<LI> Leading spaces are ignored.
+<LI> Embedded spaces are allowed only after +, -, D or E,
+             and after the decimal point if the first sequence of
+             digits is absent.
+<LI> Trailing spaces are ignored;  the first signifies
+             end of decoding and subsequent ones are skipped.
+       </UL>
+ <DT>5.
+<DD>Delimiters:
+       <UL>
+<LI> Any character other than +,-,0-9,.,D,E or space may be
+             used to signal the end of the number and terminate decoding.
+<LI> Comma is recognized by sla_DFLTIN as a special case; it
+             is skipped, leaving the pointer on the next character.  See
+             13, below.
+<LI> Decoding will in all cases terminate if end of string
+             is reached.
+       </UL>
+ <DT>6.
+<DD>Both signs are optional.  The default is +.
+ <DT>7.
+<DD>The mantissa <I>n</I>.<I>n</I> defaults to unity.
+ <DT>8.
+<DD>The exponent <IMG WIDTH="36" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img69.gif"
+ ALT="$x\!\pm\!n$"> defaults to `D0'.
+ <DT>9.
+<DD>The strings of decimal digits may be of any length.
+ <DT>10.
+<DD>The decimal point is optional for whole numbers.
+ <DT>11.
+<DD>A <I>null result</I> occurs when the string of characters
+       being decoded does not begin with +,-,0-9,.,D or E, or
+       consists entirely of spaces.  When this condition is
+       detected, JFLAG is set to 1 and DRESLT is left untouched.
+ <DT>12.
+<DD>NSTRT = 1 for the first character in the string.
+ <DT>13.
+<DD>On return from sla_DFLTIN, NSTRT is set ready for the next
+       decode - following trailing blanks and any comma.  If a
+       delimiter other than comma is being used, NSTRT must be
+       incremented before the next call to sla_DFLTIN, otherwise
+       all subsequent calls will return a null result.
+ <DT>14.
+<DD>Errors (JFLAG=2) occur when:
+       <UL>
+<LI> a +, -, D or E is left unsatisfied; or
+<LI> the decimal point is present without at least
+             one decimal digit before or after it; or
+<LI> an exponent more than 100 has been presented.
+       </UL>
+ <DT>15.
+<DD>When an error has been detected, NSTRT is left
+       pointing to the character following the last
+       one used before the error came to light.  This
+       may be after the point at which a more sophisticated
+       program could have detected the error.  For example,
+       sla_DFLTIN does not detect that `1D999' is unacceptable
+       (on a computer where this is so) until the entire number
+       has been decoded.
+ <DT>16.
+<DD>Certain highly unlikely combinations of mantissa and
+       exponent can cause arithmetic faults during the
+       decode, in some cases despite the fact that they
+       together could be construed as a valid number.
+ <DT>17.
+<DD>Decoding is left to right, one pass.
+ <DT>18.
+<DD>See also sla_FLOTIN and sla_INTIN.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html976" HREF="node56.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html977" HREF="node56.html">SLA_DH2E - Az,El to</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html975" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html969" HREF="node54.html">SLA_DEULER - Euler Angles to Rotation Matrix</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node56.html b/src/slalib/sun67.htx/node56.html
new file mode 100644
index 0000000..e71b073
--- /dev/null
+++ b/src/slalib/sun67.htx/node56.html
@@ -0,0 +1,146 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DH2E - Az,El to </TITLE>
+<META NAME="description" CONTENT="SLA_DH2E - Az,El to ">
+<META NAME="keywords" CONTENT="sun67">
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+ SRC="contents_motif.gif"></A>
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+<BR>
+<B> Previous:</B> <A NAME="tex2html979" HREF="node55.html">SLA_DFLTIN - Decode a Double Precision Number</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000443000000000000000">&#160;</A><A NAME="xref_SLA_DH2E">&#160;</A><A NAME="SLA_DH2E">&#160;</A>
+<BR>
+SLA_DH2E - Az,El to <IMG WIDTH="27" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img65.gif"
+ ALT="$h,\delta$"></H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Horizon to equatorial coordinates
+(double precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DH2E (AZ, EL, PHI, HA, DEC)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AZ</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>azimuth (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EL</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>elevation (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PHI</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>latitude (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>HA</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>hour angle (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DEC</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>declination (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The sign convention for azimuth is north zero, east <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img14.gif"
+ ALT="$+\pi/2$">.<DT>2.
+<DD>HA is returned in the range <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$">.  Declination is returned
+in the range <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$">.  <DT>3.
+<DD>The latitude is (in principle) geodetic.  In critical
+        applications, corrections for polar motion should be applied
+        (see sla_POLMO).
+  <DT>4.
+<DD>In some applications it will be important to specify the
+        correct type of elevation in order to produce the required
+        type of <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$">.  In particular, it may be important to
+        distinguish between the elevation as affected by refraction,
+        which will yield the <I>observed</I> <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$">, and the elevation
+        <I>in vacuo</I>, which will yield the <I>topocentric</I>
+        <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$">.  If the
+        effects of diurnal aberration can be neglected, the
+        topocentric <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$"> may be used as an approximation to the
+        <I>apparent</I> <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$">.  <DT>5.
+<DD>No range checking of arguments is carried out.
+  <DT>6.
+<DD>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.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html986" HREF="node57.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html987" HREF="node57.html">SLA_DIMXV - Apply 3D Reverse Rotation</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html985" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html979" HREF="node55.html">SLA_DFLTIN - Decode a Double Precision Number</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node57.html b/src/slalib/sun67.htx/node57.html
new file mode 100644
index 0000000..df5870d
--- /dev/null
+++ b/src/slalib/sun67.htx/node57.html
@@ -0,0 +1,118 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DIMXV - Apply 3D Reverse Rotation</TITLE>
+<META NAME="description" CONTENT="SLA_DIMXV - Apply 3D Reverse Rotation">
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+<BR>
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+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000444000000000000000">SLA_DIMXV - Apply 3D Reverse Rotation</A>
+<A NAME="xref_SLA_DIMXV">&#160;</A><A NAME="SLA_DIMXV">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Multiply a 3-vector by the inverse of a rotation
+matrix (double precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DIMXV (DM, VA, VB)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DM</EM></TD>
+<TH ALIGN="LEFT"><B>D(3,3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>rotation matrix</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>VA</EM></TD>
+<TD ALIGN="LEFT"><B>D(3)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>vector to be rotated</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>VB</EM></TD>
+<TH ALIGN="LEFT"><B>D(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>result vector</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>This routine performs the operation:
+<BLOCKQUOTE><B>b</B> = <B>M</B><IMG WIDTH="17" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img70.gif"
+ ALT="$^{T}\cdot$"><B>a</B>
+</BLOCKQUOTE>
+        where <B>a</B> and <B>b</B> are the 3-vectors VA and VB
+        respectively, and  <B>M</B> is the <IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img18.gif"
+ ALT="$3\times3$"> matrix DM.
+  <DT>2.
+<DD>The main function of this routine is apply an inverse
+        rotation;  under these circumstances, <IMG WIDTH="17" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img71.gif"
+ ALT="${\bf \rm M}$"> is
+        <I>orthogonal</I>, with its inverse the same as its transpose.
+  <DT>3.
+<DD>To comply with the ANSI Fortran 77 standard, VA and VB must
+        <B>not</B> be the same array.  The routine is, in fact, coded
+        so as to work properly on the VAX and many other systems even
+        if this rule is violated, something that is <B>not</B>, however,
+        recommended.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html996" HREF="node58.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+<BR>
+<B> Next:</B> <A NAME="tex2html997" HREF="node58.html">SLA_DJCAL - MJD to Gregorian for Output</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html995" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html989" HREF="node56.html">SLA_DH2E - Az,El to</A>
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+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node58.html b/src/slalib/sun67.htx/node58.html
new file mode 100644
index 0000000..78f70fa
--- /dev/null
+++ b/src/slalib/sun67.htx/node58.html
@@ -0,0 +1,112 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DJCAL - MJD to Gregorian for Output</TITLE>
+<META NAME="description" CONTENT="SLA_DJCAL - MJD to Gregorian for Output">
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+<BR>
+<B> Previous:</B> <A NAME="tex2html999" HREF="node57.html">SLA_DIMXV - Apply 3D Reverse Rotation</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000445000000000000000">SLA_DJCAL - MJD to Gregorian for Output</A>
+<A NAME="xref_SLA_DJCAL">&#160;</A><A NAME="SLA_DJCAL">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Modified Julian Date to Gregorian Calendar Date, expressed
+in a form convenient for formatting messages (namely
+         rounded to a specified precision, and with the fields
+         stored in a single array).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DJCAL (NDP, DJM, IYMDF, J)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NDP</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>number of decimal places of days in fraction</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DJM</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>modified Julian Date (JD-2400000.5)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IYMDF</EM></TD>
+<TH ALIGN="LEFT"><B>I(4)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>year, month, day, fraction in Gregorian calendar</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:  nonzero = out of range</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Any date after 4701BC March 1 is accepted.
+<DT>2.
+<DD>NDP should be 4 or less to avoid overflow on machines which
+use 32-bit integers.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>The algorithm is derived from that of Hatcher,
+<I>Q.Jl.R.astr.Soc.</I> (1984) <B>25</B>, 53-55.
+     </DL>
+<BR> <HR>
+<A NAME="tex2html1006" HREF="node59.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1004" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html998" HREF="node57.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1007" HREF="node59.html">SLA_DJCL - MJD to Year,Month,Day,Frac</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1005" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html999" HREF="node57.html">SLA_DIMXV - Apply 3D Reverse Rotation</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node59.html b/src/slalib/sun67.htx/node59.html
new file mode 100644
index 0000000..1d0b789
--- /dev/null
+++ b/src/slalib/sun67.htx/node59.html
@@ -0,0 +1,117 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DJCL - MJD to Year,Month,Day,Frac</TITLE>
+<META NAME="description" CONTENT="SLA_DJCL - MJD to Year,Month,Day,Frac">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node60.html">
+<LINK REL="previous" HREF="node58.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node60.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1016" HREF="node60.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1014" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1008" HREF="node58.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1017" HREF="node60.html">SLA_DM2AV - Rotation Matrix to Axial Vector</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1015" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1009" HREF="node58.html">SLA_DJCAL - MJD to Gregorian for Output</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000446000000000000000">SLA_DJCL - MJD to Year,Month,Day,Frac</A>
+<A NAME="xref_SLA_DJCL">&#160;</A><A NAME="SLA_DJCL">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Modified Julian Date to Gregorian year, month, day,
+and fraction of a day.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DJCL (DJM, IY, IM, ID, FD, J)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DJM</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>modified Julian Date (JD-2400000.5)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IY</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>year</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IM</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>month</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ID</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>day</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>FD</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>fraction of day</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  0 = OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  -1 = unacceptable date (before 4701BC March 1)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>The algorithm is derived from that of Hatcher,
+<I>Q.Jl.R.astr.Soc.</I> (1984) <B>25</B>, 53-55.
+     </DL>
+<BR> <HR>
+<A NAME="tex2html1016" HREF="node60.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1014" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1008" HREF="node58.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1017" HREF="node60.html">SLA_DM2AV - Rotation Matrix to Axial Vector</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1015" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1009" HREF="node58.html">SLA_DJCAL - MJD to Gregorian for Output</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node6.html b/src/slalib/sun67.htx/node6.html
new file mode 100644
index 0000000..c90fd51
--- /dev/null
+++ b/src/slalib/sun67.htx/node6.html
@@ -0,0 +1,116 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Objectives</TITLE>
+<META NAME="description" CONTENT="Objectives">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node7.html">
+<LINK REL="previous" HREF="node5.html">
+<LINK REL="up" HREF="node2.html">
+<LINK REL="next" HREF="node7.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html305" HREF="node7.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html303" HREF="node2.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html297" HREF="node5.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html306" HREF="node7.html">Fortran Version</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html304" HREF="node2.html">INTRODUCTION</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html298" HREF="node5.html">Scope</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION00024000000000000000">
+Objectives</A>
+</H2>
+SLALIB was designed to give application programmers
+a basic set of positional-astronomy tools which were
+accurate and easy to use.  To this end, the library is:
+<UL>
+<LI> Readily available, including source code and documentation.
+<LI> Supported and maintained.
+<LI> Portable - coded in standard languages and available for
+multiple computers and operating systems.
+<LI> Thoroughly commented, both for maintainability and to
+assist those wishing to cannibalize the code.
+<LI> Stable.
+<LI> Trustworthy - some care has gone into
+testing SLALIB, both by comparison with published data and
+by checks for internal consistency.
+<LI> Rigorous - corners are not cut,
+even where the practical consequences would, as a rule, be
+negligible.
+<LI> Comprehensive, without including too many esoteric features
+required only by specialists.
+<LI> Practical - almost all the routines have been written to
+satisfy real needs encountered during the development of
+real-life applications.
+<LI> Environment-independent - the package is
+completely free of pauses, stops, I/O <I>etc</I>.
+<LI> Self-contained - SLALIB calls no other libraries.
+</UL>
+A few <I>caveats</I>:
+<UL>
+<LI> SLALIB does not pretend to be canonical.  It is in essence
+an anthology, and the adopted algorithms are liable
+to change as more up-to-date ones become available.
+<LI> The functions aren't orthogonal - there are several
+cases of different
+routines doing similar things, and many examples where
+sequences of SLALIB calls have simply been packaged, all to
+make applications less trouble to write.
+<LI> There are omissions - for example there are no
+routines for calculating physical ephemerides of
+Solar-System bodies.
+<LI> SLALIB is not homogeneous, though important subsets
+(for example the FK4/FK5 routines) are.
+<LI> The library is not foolproof.  You have to know what
+you are trying to do (<I>e.g.</I> by reading textbooks on positional
+astronomy), and it is the caller's responsibility to supply
+sensible arguments (although enough internal validation is done to
+avoid arithmetic errors).
+<LI> Without being written in a wasteful
+manner, SLALIB is nonetheless optimized for maintainability
+rather than speed.  In addition, there are many places
+where considerable simplification would be possible if some
+specified amount of accuracy could be sacrificed;  such
+compromises are left to the individual programmer and
+are not allowed to limit SLALIB's value as a source
+of comparison results.
+</UL>
+<BR> <HR>
+<A NAME="tex2html305" HREF="node7.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html303" HREF="node2.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html297" HREF="node5.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html306" HREF="node7.html">Fortran Version</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html304" HREF="node2.html">INTRODUCTION</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html298" HREF="node5.html">Scope</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node60.html b/src/slalib/sun67.htx/node60.html
new file mode 100644
index 0000000..db12402
--- /dev/null
+++ b/src/slalib/sun67.htx/node60.html
@@ -0,0 +1,107 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DM2AV - Rotation Matrix to Axial Vector</TITLE>
+<META NAME="description" CONTENT="SLA_DM2AV - Rotation Matrix to Axial Vector">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
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+<LINK REL="previous" HREF="node59.html">
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+<BR> <HR>
+<A NAME="tex2html1026" HREF="node61.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1024" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1018" HREF="node59.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1027" HREF="node61.html">SLA_DMAT - Solve Simultaneous Equations</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1025" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1019" HREF="node59.html">SLA_DJCL - MJD to Year,Month,Day,Frac</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000447000000000000000">SLA_DM2AV - Rotation Matrix to Axial Vector</A>
+<A NAME="xref_SLA_DM2AV">&#160;</A><A NAME="SLA_DM2AV">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>From a rotation matrix, determine the corresponding axial vector
+(double precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DM2AV (RMAT, AXVEC)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RMAT</EM></TD>
+<TH ALIGN="LEFT"><B>D(3,3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>rotation matrix</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AXVEC</EM></TD>
+<TH ALIGN="LEFT"><B>D(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>axial vector (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>A rotation matrix describes a rotation about some arbitrary axis.
+The axis is called the <I>Euler axis</I>, and the angle through
+which the reference frame rotates is called the <I>Euler angle</I>.
+        The <I>axial vector</I> returned by this routine has the same
+        direction as the Euler axis, and its magnitude is the Euler angle
+        in radians.
+  <DT>2.
+<DD>The magnitude and direction of the axial vector can be separated
+        by means of the routine sla_DVN.
+  <DT>3.
+<DD>The reference frame rotates clockwise as seen looking along
+        the axial vector from the origin.
+  <DT>4.
+<DD>If RMAT is null, so is the result.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1026" HREF="node61.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1024" HREF="node13.html">
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+<A NAME="tex2html1018" HREF="node59.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1027" HREF="node61.html">SLA_DMAT - Solve Simultaneous Equations</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1025" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1019" HREF="node59.html">SLA_DJCL - MJD to Year,Month,Day,Frac</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node61.html b/src/slalib/sun67.htx/node61.html
new file mode 100644
index 0000000..b72e3ac
--- /dev/null
+++ b/src/slalib/sun67.htx/node61.html
@@ -0,0 +1,152 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DMAT - Solve Simultaneous Equations</TITLE>
+<META NAME="description" CONTENT="SLA_DMAT - Solve Simultaneous Equations">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node62.html">
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+<LINK REL="up" HREF="node13.html">
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+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1036" HREF="node62.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1037" HREF="node62.html">SLA_DMOON - Approx Moon Pos/Vel</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1035" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1029" HREF="node60.html">SLA_DM2AV - Rotation Matrix to Axial Vector</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000448000000000000000">SLA_DMAT - Solve Simultaneous Equations</A>
+<A NAME="xref_SLA_DMAT">&#160;</A><A NAME="SLA_DMAT">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Matrix inversion and solution of simultaneous equations
+(double precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DMAT (N, A, Y, D, JF, IW)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>N</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>number of unknowns</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A</EM></TD>
+<TD ALIGN="LEFT"><B>D(N,N)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>matrix</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>Y</EM></TD>
+<TD ALIGN="LEFT"><B>D(N)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>vector</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A</EM></TD>
+<TH ALIGN="LEFT"><B>D(N,N)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>matrix inverse</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>Y</EM></TD>
+<TD ALIGN="LEFT"><B>D(N)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>solution</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>D</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>determinant</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JF</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>singularity flag: 0=OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IW</EM></TD>
+<TD ALIGN="LEFT"><B>I(N)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>workspace</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>For the set of <I>n</I> simultaneous linear equations in <I>n</I> unknowns:
+<BLOCKQUOTE><B>A</B><IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"><B>y</B> = <B>x</B>
+</BLOCKQUOTE>
+        where:
+        <UL>
+<LI> <B>A</B> is a non-singular <IMG WIDTH="42" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img73.gif"
+ ALT="$n \times n$"> matrix,
+<LI> <B>y</B> is the vector of <I>n</I> unknowns, and
+<LI> <B>x</B> is the known vector,
+        </UL>
+        sla_DMAT computes:
+        <UL>
+<LI> the inverse of matrix <B>A</B>,
+<LI> the determinant of matrix <B>A</B>, and
+<LI> the vector of <I>n</I> unknowns <B>y</B>.
+        </UL>
+        Argument N is the order <I>n</I>, A (given) is the matrix <B>A</B>,
+        Y (given) is the vector <B>x</B> and Y (returned)
+        is the vector <B>y</B>.
+        The argument A (returned) is the inverse matrix <B>A</B><SUP>-1</SUP>,
+        and D is <I>det</I>(<B>A</B>).
+  <DT>2.
+<DD>JF is the singularity flag.  If the matrix is non-singular,
+        JF=0 is returned.  If the matrix is singular, JF=-1
+        and D=0D0 are returned.  In the latter case, the contents
+        of array A on return are undefined.
+  <DT>3.
+<DD>The algorithm is Gaussian elimination with partial pivoting.
+        This method is very fast;  some much slower algorithms can give
+        better accuracy, but only by a small factor.
+  <DT>4.
+<DD>This routine replaces the obsolete sla_DMATRX.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1036" HREF="node62.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1034" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1028" HREF="node60.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1037" HREF="node62.html">SLA_DMOON - Approx Moon Pos/Vel</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1035" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1029" HREF="node60.html">SLA_DM2AV - Rotation Matrix to Axial Vector</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node62.html b/src/slalib/sun67.htx/node62.html
new file mode 100644
index 0000000..dedceda
--- /dev/null
+++ b/src/slalib/sun67.htx/node62.html
@@ -0,0 +1,154 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DMOON - Approx Moon Pos/Vel</TITLE>
+<META NAME="description" CONTENT="SLA_DMOON - Approx Moon Pos/Vel">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
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+<LINK REL="previous" HREF="node61.html">
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+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1044" HREF="node13.html">
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+<A NAME="tex2html1038" HREF="node61.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1047" HREF="node63.html">SLA_DMXM - Multiply Matrices</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1045" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1039" HREF="node61.html">SLA_DMAT - Solve Simultaneous Equations</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000449000000000000000">SLA_DMOON - Approx Moon Pos/Vel</A>
+<A NAME="xref_SLA_DMOON">&#160;</A><A NAME="SLA_DMOON">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Approximate geocentric position and velocity of the Moon
+(double precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DMOON (DATE, PV)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>TDB (loosely ET) as a Modified Julian Date (JD-2400000.5)
+</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PV</EM></TD>
+<TH ALIGN="LEFT"><B>D(6)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>Moon <IMG WIDTH="106" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img51.gif"
+ ALT="$[\,x,y,z,\dot{x},\dot{y},\dot{z}\,]$">, mean equator and equinox
+of date (AU, AU&nbsp;s<SUP>-1</SUP>)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>This routine is a full implementation of the algorithm
+published by Meeus (see reference).
+<DT>2.
+<DD>Meeus quotes accuracies of <IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img74.gif"
+ ALT="$10\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> in longitude,
+        <IMG WIDTH="17" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img75.gif"
+ ALT="$3\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> in latitude and 
+      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img76.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.2$">    arcsec in HP
+        (equivalent to about 20&nbsp;km in distance).  Comparison with
+        JPL&nbsp;DE200 over the interval 1960-2025 gives RMS errors of
+<P>      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img77.gif"
+ ALT="$3\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.7$">    and 83&nbsp;mas/hour in longitude,
+<P>      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img78.gif"
+ ALT="$2\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.3$">    arcsec and 48&nbsp;mas/hour in latitude,
+        11&nbsp;km and 81&nbsp;mm/s in distance.
+        The maximum errors over the same interval are
+        <IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img79.gif"
+ ALT="$18\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> and 
+      <IMG WIDTH="31" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img80.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.50$">   /hour in longitude,
+        <IMG WIDTH="25" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img43.gif"
+ ALT="$11\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> and 
+      <IMG WIDTH="31" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img81.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.24$">   /hour in latitude,
+        40&nbsp;km and 0.29&nbsp;m/s in distance.
+  <DT>3.
+<DD>The original algorithm is expressed in terms of the obsolete
+        timescale <I>Ephemeris Time</I>.  Either TDB or TT can be used,
+        but not UT without incurring significant errors (<IMG WIDTH="25" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img82.gif"
+ ALT="$30\hspace{-0.05em}^{'\hspace{-0.1em}'}$"> at
+        the present time) due to the Moon's 
+      <IMG WIDTH="23" HEIGHT="18" ALIGN="BOTTOM" BORDER="0"
+ SRC="img83.gif"
+ ALT="$0\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.5$">   /s movement.
+  <DT>4.
+<DD>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.
+  <DT>5.
+<DD>Velocity is obtained by a complete analytical differentiation
+        of the Meeus model.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Meeus, <I>l'Astronomie</I>, June 1984, p348.
+</DL>
+<BR> <HR>
+<A NAME="tex2html1046" HREF="node63.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1044" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1038" HREF="node61.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1047" HREF="node63.html">SLA_DMXM - Multiply Matrices</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1045" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1039" HREF="node61.html">SLA_DMAT - Solve Simultaneous Equations</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node63.html b/src/slalib/sun67.htx/node63.html
new file mode 100644
index 0000000..9d19b4d
--- /dev/null
+++ b/src/slalib/sun67.htx/node63.html
@@ -0,0 +1,106 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DMXM - Multiply Matrices</TITLE>
+<META NAME="description" CONTENT="SLA_DMXM - Multiply Matrices">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
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+<LINK REL="previous" HREF="node62.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node64.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1056" HREF="node64.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1054" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1048" HREF="node62.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1057" HREF="node64.html">SLA_DMXV - Apply 3D Rotation</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1055" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1049" HREF="node62.html">SLA_DMOON - Approx Moon Pos/Vel</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000450000000000000000">&#160;</A><A NAME="xref_SLA_DMXM">&#160;</A><A NAME="SLA_DMXM">&#160;</A>
+<BR>
+SLA_DMXM - Multiply <IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img18.gif"
+ ALT="$3\times3$"> Matrices
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Product of two <IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img18.gif"
+ ALT="$3\times3$"> matrices (double precision).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DMXM (A, B, C)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A</EM></TD>
+<TH ALIGN="LEFT"><B>D(3,3)</B></TH>
+<TH ALIGN="LEFT" NOWRAP>matrix <B>A</B></TH>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>B</EM></TD>
+<TD ALIGN="LEFT"><B>D(3,3)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>matrix <B>B</B></TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>C</EM></TD>
+<TH ALIGN="LEFT"><B>D(3,3)</B></TH>
+<TH ALIGN="LEFT" NOWRAP>matrix result: <B>A</B><IMG WIDTH="15" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img84.gif"
+ ALT="$\times$"><B>B</B></TH>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTE:</STRONG>
+<DD>To comply with the ANSI Fortran 77 standard, A, B and C must
+be different arrays.  The routine is, in fact, coded
+       so as to work properly on the VAX and many other systems even
+       if this rule is violated, something that is <B>not</B>, however,
+       recommended.
+      </DL>
+<BR> <HR>
+<A NAME="tex2html1056" HREF="node64.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1054" HREF="node13.html">
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+<A NAME="tex2html1048" HREF="node62.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1057" HREF="node64.html">SLA_DMXV - Apply 3D Rotation</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1055" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1049" HREF="node62.html">SLA_DMOON - Approx Moon Pos/Vel</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node64.html b/src/slalib/sun67.htx/node64.html
new file mode 100644
index 0000000..b6a0e15
--- /dev/null
+++ b/src/slalib/sun67.htx/node64.html
@@ -0,0 +1,115 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DMXV - Apply 3D Rotation</TITLE>
+<META NAME="description" CONTENT="SLA_DMXV - Apply 3D Rotation">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node65.html">
+<LINK REL="previous" HREF="node63.html">
+<LINK REL="up" HREF="node13.html">
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+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1066" HREF="node65.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1064" HREF="node13.html">
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+<A NAME="tex2html1058" HREF="node63.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1067" HREF="node65.html">SLA_DPAV - Position-Angle Between Two Directions</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1065" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1059" HREF="node63.html">SLA_DMXM - Multiply Matrices</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000451000000000000000">SLA_DMXV - Apply 3D Rotation</A>
+<A NAME="xref_SLA_DMXV">&#160;</A><A NAME="SLA_DMXV">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Multiply a 3-vector by a rotation matrix (double precision).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DMXV (DM, VA, VB)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DM</EM></TD>
+<TH ALIGN="LEFT"><B>D(3,3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>rotation matrix</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>VA</EM></TD>
+<TD ALIGN="LEFT"><B>D(3)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>vector to be rotated</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>VB</EM></TD>
+<TH ALIGN="LEFT"><B>D(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>result vector</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>This routine performs the operation:
+<BLOCKQUOTE><B>b</B> = <B>M</B><IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"><B>a</B>
+</BLOCKQUOTE>
+        where <B>a</B> and <B>b</B> are the 3-vectors VA and VB
+        respectively, and <B>M</B> is the <IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img18.gif"
+ ALT="$3\times3$"> matrix DM.
+  <DT>2.
+<DD>The main function of this routine is apply a
+        rotation;  under these circumstances, <B>M</B> is a
+        <I>proper real orthogonal</I> matrix.
+  <DT>3.
+<DD>To comply with the ANSI Fortran 77 standard, VA and VB must
+        <B>not</B> be the same array.  The routine is, in fact, coded
+        so as to work properly on the VAX and many other systems even
+        if this rule is violated, something that is <B>not</B>, however,
+        recommended.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1066" HREF="node65.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1064" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1058" HREF="node63.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1067" HREF="node65.html">SLA_DPAV - Position-Angle Between Two Directions</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1065" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1059" HREF="node63.html">SLA_DMXM - Multiply Matrices</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node65.html b/src/slalib/sun67.htx/node65.html
new file mode 100644
index 0000000..de89921
--- /dev/null
+++ b/src/slalib/sun67.htx/node65.html
@@ -0,0 +1,117 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DPAV - Position-Angle Between Two Directions</TITLE>
+<META NAME="description" CONTENT="SLA_DPAV - Position-Angle Between Two Directions">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
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+<LINK REL="next" HREF="node66.html">
+<LINK REL="previous" HREF="node64.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node66.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1076" HREF="node66.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1074" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1068" HREF="node64.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1077" HREF="node66.html">SLA_DR2AF - Radians to Deg,Min,Sec,Frac</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1075" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1069" HREF="node64.html">SLA_DMXV - Apply 3D Rotation</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000452000000000000000">SLA_DPAV - Position-Angle Between Two Directions</A>
+<A NAME="xref_SLA_DPAV">&#160;</A><A NAME="SLA_DPAV">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Returns the bearing (position angle) of one celestial
+direction with respect to another (double precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>D&nbsp;=&nbsp;sla_DPAV (V1, V2)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V1</EM></TD>
+<TH ALIGN="LEFT"><B>D(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>direction cosines of one point</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V2</EM></TD>
+<TD ALIGN="LEFT"><B>D(3)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>directions cosines of the other point</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_DPAV</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>position-angle of 2nd point with respect to 1st</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The coordinate frames correspond to <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">,<IMG WIDTH="38" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img46.gif"
+ ALT="$[\lambda,\phi]$"> <I>etc.</I>.
+<DT>2.
+<DD>The result is the bearing (position angle), in radians,
+       of point V2 as seen
+       from point V1.  It is in the range <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$">.  The sense
+       is such that if V2
+       is a small distance due east of V1 the result
+       is about <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img14.gif"
+ ALT="$+\pi/2$">. Zero is returned
+       if the two points are coincident.
+ <DT>3.
+<DD>The routine sla_DBEAR performs an equivalent function except
+       that the points are specified in the form of spherical coordinates.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1076" HREF="node66.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1074" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1068" HREF="node64.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1077" HREF="node66.html">SLA_DR2AF - Radians to Deg,Min,Sec,Frac</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1075" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1069" HREF="node64.html">SLA_DMXV - Apply 3D Rotation</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node66.html b/src/slalib/sun67.htx/node66.html
new file mode 100644
index 0000000..c4b2639
--- /dev/null
+++ b/src/slalib/sun67.htx/node66.html
@@ -0,0 +1,122 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DR2AF - Radians to Deg,Min,Sec,Frac</TITLE>
+<META NAME="description" CONTENT="SLA_DR2AF - Radians to Deg,Min,Sec,Frac">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node67.html">
+<LINK REL="previous" HREF="node65.html">
+<LINK REL="up" HREF="node13.html">
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+</HEAD>
+<BODY >
+<BR> <HR>
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+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1084" HREF="node13.html">
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+<A NAME="tex2html1078" HREF="node65.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1087" HREF="node67.html">SLA_DR2TF - Radians to Hour,Min,Sec,Frac</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1085" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1079" HREF="node65.html">SLA_DPAV - Position-Angle Between Two Directions</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000453000000000000000">SLA_DR2AF - Radians to Deg,Min,Sec,Frac</A>
+<A NAME="xref_SLA_DR2AF">&#160;</A><A NAME="SLA_DR2AF">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Convert an angle in radians to degrees, arcminutes, arcseconds,
+fraction (double precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DR2AF (NDP, ANGLE, SIGN, IDMSF)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NDP</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>number of decimal places of arcseconds</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ANGLE</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>angle in radians</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>SIGN</EM></TD>
+<TH ALIGN="LEFT"><B>C</B></TH>
+<TD ALIGN="LEFT" NOWRAP>`+' or `-'</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IDMSF</EM></TD>
+<TD ALIGN="LEFT"><B>I(4)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>degrees, arcminutes, arcseconds, fraction</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>NDP less than zero is interpreted as zero.
+<DT>2.
+<DD>The largest useful value for NDP is determined by the size
+of ANGLE, the format of DOUBLE&nbsp;PRECISION floating-point numbers
+        on the target machine, and the risk of overflowing IDMSF(4).
+        For example, on a VAX computer, for ANGLE up to <IMG WIDTH="20" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img52.gif"
+ ALT="$2\pi$">, the available
+        floating-point precision corresponds roughly to NDP=12.  However,
+        the practical limit is NDP=9, set by the capacity of the 32-bit
+        integer IDMSF(4).
+  <DT>3.
+<DD>The absolute value of ANGLE may exceed <IMG WIDTH="20" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img52.gif"
+ ALT="$2\pi$">.  In cases where it
+        does not, it is up to the caller to test for and handle the
+        case where ANGLE is very nearly <IMG WIDTH="20" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img52.gif"
+ ALT="$2\pi$"> and rounds up to <IMG WIDTH="34" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img53.gif"
+ ALT="$360^{\circ}$">,        by testing for IDMSF(1)=360 and setting IDMSF(1-4) to zero.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1086" HREF="node67.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1084" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1078" HREF="node65.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1087" HREF="node67.html">SLA_DR2TF - Radians to Hour,Min,Sec,Frac</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1085" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1079" HREF="node65.html">SLA_DPAV - Position-Angle Between Two Directions</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node67.html b/src/slalib/sun67.htx/node67.html
new file mode 100644
index 0000000..f5e0648
--- /dev/null
+++ b/src/slalib/sun67.htx/node67.html
@@ -0,0 +1,121 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DR2TF - Radians to Hour,Min,Sec,Frac</TITLE>
+<META NAME="description" CONTENT="SLA_DR2TF - Radians to Hour,Min,Sec,Frac">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node68.html">
+<LINK REL="previous" HREF="node66.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node68.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1096" HREF="node68.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1094" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1088" HREF="node66.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1097" HREF="node68.html">SLA_DRANGE - Put Angle into Range</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1095" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1089" HREF="node66.html">SLA_DR2AF - Radians to Deg,Min,Sec,Frac</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000454000000000000000">SLA_DR2TF - Radians to Hour,Min,Sec,Frac</A>
+<A NAME="xref_SLA_DR2TF">&#160;</A><A NAME="SLA_DR2TF">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Convert an angle in radians to hours, minutes, seconds,
+fraction (double precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DR2TF (NDP, ANGLE, SIGN, IHMSF)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>NDP</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>number of decimal places of seconds</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ANGLE</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>angle in radians</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>SIGN</EM></TD>
+<TH ALIGN="LEFT"><B>C</B></TH>
+<TD ALIGN="LEFT" NOWRAP>`+' or `-'</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IHMSF</EM></TD>
+<TD ALIGN="LEFT"><B>I(4)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>hours, minutes, seconds, fraction</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>NDP less than zero is interpreted as zero.
+<DT>2.
+<DD>The largest useful value for NDP is determined by the size
+of ANGLE, the format of DOUBLE PRECISION floating-point numbers
+        on the target machine, and the risk of overflowing IHMSF(4).
+        For example, on a VAX computer, for ANGLE up to <IMG WIDTH="20" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img52.gif"
+ ALT="$2\pi$">, the available
+        floating-point precision corresponds roughly to NDP=12.  However,
+        the practical limit is NDP=9, set by the capacity of the 32-bit
+        integer IHMSF(4).
+  <DT>3.
+<DD>The absolute value of ANGLE may exceed <IMG WIDTH="20" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img52.gif"
+ ALT="$2\pi$">.  In cases where it
+        does not, it is up to the caller to test for and handle the
+        case where ANGLE is very nearly <IMG WIDTH="20" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img52.gif"
+ ALT="$2\pi$"> and rounds up to 24&nbsp;hours,
+        by testing for IHMSF(1)=24 and setting IHMSF(1-4) to zero.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1096" HREF="node68.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1094" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1088" HREF="node66.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1097" HREF="node68.html">SLA_DRANGE - Put Angle into Range</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1095" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1089" HREF="node66.html">SLA_DR2AF - Radians to Deg,Min,Sec,Frac</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node68.html b/src/slalib/sun67.htx/node68.html
new file mode 100644
index 0000000..477164f
--- /dev/null
+++ b/src/slalib/sun67.htx/node68.html
@@ -0,0 +1,93 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DRANGE - Put Angle into Range </TITLE>
+<META NAME="description" CONTENT="SLA_DRANGE - Put Angle into Range ">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node69.html">
+<LINK REL="previous" HREF="node67.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node69.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1106" HREF="node69.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1104" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1098" HREF="node67.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1107" HREF="node69.html">SLA_DRANRM - Put Angle into Range</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1105" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1099" HREF="node67.html">SLA_DR2TF - Radians to Hour,Min,Sec,Frac</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000455000000000000000">&#160;</A><A NAME="xref_SLA_DRANGE">&#160;</A><A NAME="SLA_DRANGE">&#160;</A>
+<BR>
+SLA_DRANGE - Put Angle into Range <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$"></H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Normalize an angle into the range <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$"> (double precision).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>D&nbsp;=&nbsp;sla_DRANGE (ANGLE)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ANGLE</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>angle in radians</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_DRANGE</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>ANGLE expressed in the range <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$">.</TD>
+</TR>
+</TABLE></DL>
+<BR> <HR>
+<A NAME="tex2html1106" HREF="node69.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1104" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1098" HREF="node67.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1107" HREF="node69.html">SLA_DRANRM - Put Angle into Range</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1105" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1099" HREF="node67.html">SLA_DR2TF - Radians to Hour,Min,Sec,Frac</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node69.html b/src/slalib/sun67.htx/node69.html
new file mode 100644
index 0000000..02f5415
--- /dev/null
+++ b/src/slalib/sun67.htx/node69.html
@@ -0,0 +1,93 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DRANRM - Put Angle into Range </TITLE>
+<META NAME="description" CONTENT="SLA_DRANRM - Put Angle into Range ">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node70.html">
+<LINK REL="previous" HREF="node68.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node70.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1116" HREF="node70.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1114" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1108" HREF="node68.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1117" HREF="node70.html">SLA_DS2C6 - Spherical Pos/Vel to Cartesian</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1115" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1109" HREF="node68.html">SLA_DRANGE - Put Angle into Range</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000456000000000000000">&#160;</A><A NAME="xref_SLA_DRANRM">&#160;</A><A NAME="SLA_DRANRM">&#160;</A>
+<BR>
+SLA_DRANRM - Put Angle into Range <IMG WIDTH="43" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img66.gif"
+ ALT="$0\!-\!2\pi$"></H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Normalize an angle into the range <IMG WIDTH="43" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img66.gif"
+ ALT="$0\!-\!2\pi$">(double precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>D&nbsp;=&nbsp;sla_DRANRM (ANGLE)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ANGLE</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>angle in radians</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_DRANRM</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>ANGLE expressed in the range <IMG WIDTH="43" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img66.gif"
+ ALT="$0\!-\!2\pi$"></TD>
+</TR>
+</TABLE></DL>
+<BR> <HR>
+<A NAME="tex2html1116" HREF="node70.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1114" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1108" HREF="node68.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1117" HREF="node70.html">SLA_DS2C6 - Spherical Pos/Vel to Cartesian</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1115" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1109" HREF="node68.html">SLA_DRANGE - Put Angle into Range</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node7.html b/src/slalib/sun67.htx/node7.html
new file mode 100644
index 0000000..e75fbed
--- /dev/null
+++ b/src/slalib/sun67.htx/node7.html
@@ -0,0 +1,76 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Fortran Version</TITLE>
+<META NAME="description" CONTENT="Fortran Version">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node8.html">
+<LINK REL="previous" HREF="node6.html">
+<LINK REL="up" HREF="node2.html">
+<LINK REL="next" HREF="node8.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html315" HREF="node8.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html313" HREF="node2.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html307" HREF="node6.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html316" HREF="node8.html">C Version</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html314" HREF="node2.html">INTRODUCTION</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html308" HREF="node6.html">Objectives</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION00025000000000000000">
+Fortran Version</A>
+</H2>
+The Fortran versions of SLALIB use ANSI Fortran&nbsp;77 with a few
+commonplace extensions.  Just three out of the 183 routines require
+platform-specific techniques and accordingly are supplied
+in different forms.
+SLALIB has been implemented on the following platforms:
+VAX/VMS,
+PC (Microsoft Fortran, Linux),
+DECstation (Ultrix),
+DEC Alpha (DEC Unix),
+Sun (SunOS, Solaris),
+Hewlett Packard (HP-UX),
+CONVEX,
+Perkin-Elmer and
+Fujitsu.
+<P>
+<BR> <HR>
+<A NAME="tex2html315" HREF="node8.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html313" HREF="node2.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html307" HREF="node6.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html316" HREF="node8.html">C Version</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html314" HREF="node2.html">INTRODUCTION</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html308" HREF="node6.html">Objectives</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node70.html b/src/slalib/sun67.htx/node70.html
new file mode 100644
index 0000000..b1ebf8a
--- /dev/null
+++ b/src/slalib/sun67.htx/node70.html
@@ -0,0 +1,114 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DS2C6 - Spherical Pos/Vel to Cartesian</TITLE>
+<META NAME="description" CONTENT="SLA_DS2C6 - Spherical Pos/Vel to Cartesian">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node71.html">
+<LINK REL="previous" HREF="node69.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node71.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1126" HREF="node71.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1124" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1118" HREF="node69.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1127" HREF="node71.html">SLA_DS2TP - Spherical to Tangent Plane</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1125" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1119" HREF="node69.html">SLA_DRANRM - Put Angle into Range</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000457000000000000000">SLA_DS2C6 - Spherical Pos/Vel to Cartesian</A>
+<A NAME="xref_SLA_DS2C6">&#160;</A><A NAME="SLA_DS2C6">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Conversion of position &amp; velocity in spherical coordinates
+to Cartesian coordinates (double precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DS2C6 (A, B, R, AD, BD, RD, V)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>longitude (radians) - for example <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$"></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>B</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>latitude (radians) - for example <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$"></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>R</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>radial coordinate</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AD</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>longitude derivative (radians per unit time)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>BD</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>latitude derivative (radians per unit time)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RD</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>radial derivative</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V</EM></TD>
+<TH ALIGN="LEFT"><B>D(6)</B></TH>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="106" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img51.gif"
+ ALT="$[\,x,y,z,\dot{x},\dot{y},\dot{z}\,]$"></TD>
+</TR>
+</TABLE></DL>
+<BR> <HR>
+<A NAME="tex2html1126" HREF="node71.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1124" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1118" HREF="node69.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1127" HREF="node71.html">SLA_DS2TP - Spherical to Tangent Plane</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1125" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1119" HREF="node69.html">SLA_DRANRM - Put Angle into Range</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node71.html b/src/slalib/sun67.htx/node71.html
new file mode 100644
index 0000000..8703383
--- /dev/null
+++ b/src/slalib/sun67.htx/node71.html
@@ -0,0 +1,129 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DS2TP - Spherical to Tangent Plane</TITLE>
+<META NAME="description" CONTENT="SLA_DS2TP - Spherical to Tangent Plane">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
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+</HEAD>
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+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1134" HREF="node13.html">
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+<A NAME="tex2html1128" HREF="node70.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1137" HREF="node72.html">SLA_DSEP - Angle Between 2 Points on Sphere</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1135" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1129" HREF="node70.html">SLA_DS2C6 - Spherical Pos/Vel to Cartesian</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000458000000000000000">SLA_DS2TP - Spherical to Tangent Plane</A>
+<A NAME="xref_SLA_DS2TP">&#160;</A><A NAME="SLA_DS2TP">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Projection of spherical coordinates onto the tangent plane
+(double precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DS2TP (RA, DEC, RAZ, DECZ, XI, ETA, J)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RA,DEC</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>spherical coordinates of star (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RAZ,DECZ</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>spherical coordinates of tangent point (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>XI,ETA</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>tangent plane coordinates (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  0 = OK, star on tangent plane</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  1 = error, star too far from axis</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  2 = error, antistar on tangent plane</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  3 = error, antistar too far from axis</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The projection is called the <I>gnomonic</I> projection;  the
+Cartesian coordinates <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img85.gif"
+ ALT="$[\,\xi,\eta\,]$"> are called 
+<I>standard coordinates.</I>  The latter
+        are in units of the distance from the tangent plane to the projection
+        point, <I>i.e.</I> radians near the origin.
+  <DT>2.
+<DD>When working in <IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$"> rather than spherical coordinates, the
+        equivalent Cartesian routine sla_DV2TP is available.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1136" HREF="node72.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1134" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1128" HREF="node70.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1137" HREF="node72.html">SLA_DSEP - Angle Between 2 Points on Sphere</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1135" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1129" HREF="node70.html">SLA_DS2C6 - Spherical Pos/Vel to Cartesian</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node72.html b/src/slalib/sun67.htx/node72.html
new file mode 100644
index 0000000..b127b82
--- /dev/null
+++ b/src/slalib/sun67.htx/node72.html
@@ -0,0 +1,100 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DSEP - Angle Between 2 Points on Sphere</TITLE>
+<META NAME="description" CONTENT="SLA_DSEP - Angle Between 2 Points on Sphere">
+<META NAME="keywords" CONTENT="sun67">
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+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1144" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1138" HREF="node71.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1147" HREF="node73.html">SLA_DT - Approximate ET minus UT</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1145" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1139" HREF="node71.html">SLA_DS2TP - Spherical to Tangent Plane</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000459000000000000000">SLA_DSEP - Angle Between 2 Points on Sphere</A>
+<A NAME="xref_SLA_DSEP">&#160;</A><A NAME="SLA_DSEP">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Angle between two points on a sphere (double precision).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>D&nbsp;=&nbsp;sla_DSEP (A1, B1, A2, B2)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A1,B1</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>spherical coordinates of one point (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>A2,B2</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>spherical coordinates of the other point (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_DSEP</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>angle between [A1,B1] and [A2,B2] in radians</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The spherical coordinates are right ascension and declination,
+longitude and latitude, <I>etc.</I>, in radians.
+<DT>2.
+<DD>The result is always positive.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1146" HREF="node73.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1144" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1138" HREF="node71.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1147" HREF="node73.html">SLA_DT - Approximate ET minus UT</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1145" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1139" HREF="node71.html">SLA_DS2TP - Spherical to Tangent Plane</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node73.html b/src/slalib/sun67.htx/node73.html
new file mode 100644
index 0000000..fca730c
--- /dev/null
+++ b/src/slalib/sun67.htx/node73.html
@@ -0,0 +1,131 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DT - Approximate ET minus UT</TITLE>
+<META NAME="description" CONTENT="SLA_DT - Approximate ET minus UT">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
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+<LINK REL="next" HREF="node74.html">
+<LINK REL="previous" HREF="node72.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node74.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1156" HREF="node74.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1154" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1148" HREF="node72.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1157" HREF="node74.html">SLA_DTF2D - Hour,Min,Sec to Days</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1155" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1149" HREF="node72.html">SLA_DSEP - Angle Between 2 Points on Sphere</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000460000000000000000">SLA_DT - Approximate ET minus UT</A>
+<A NAME="xref_SLA_DT">&#160;</A><A NAME="SLA_DT">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Estimate <IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">T, the offset between dynamical time
+and Universal Time, for a given historical epoch.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>D&nbsp;=&nbsp;sla_DT (EPOCH)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EPOCH</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TH ALIGN="LEFT" NOWRAP>(Julian) epoch (<I>e.g.</I> 1850D0)</TH>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_DT</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>approximate ET-UT (after 1984, TT-UT1) in seconds</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Depending on the epoch, one of three parabolic approximations
+is used:
+<PRE><TT>
+before AD 979 		 Stephenson &amp; Morrison's 390 BC to AD 948 model
+		 AD 979 to AD 1708 		 Stephenson &amp; Morrison's AD 948 to AD 1600 model
+		 after AD 1708 		 McCarthy &amp; Babcock's post-1650 model
+</TT></PRE>
+        The breakpoints are chosen to ensure continuity:  they occur
+        at places where the adjacent models give the same answer as
+        each other.
+  <DT>2.
+<DD>The accuracy is modest, with errors of up to <IMG WIDTH="24" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img86.gif"
+ ALT="$20^{\rm s}$"> during
+        the interval since 1650, rising to perhaps <IMG WIDTH="30" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img87.gif"
+ ALT="$30^{\rm m}$">        by 1000&nbsp;BC.  Comparatively accurate values from AD&nbsp;1600
+        are tabulated in
+        the <I>Astronomical Almanac</I> (see section K8 of the 1995
+        edition).
+  <DT>3.
+<DD>The use of <TT>DOUBLE PRECISION</TT> for both argument and result is
+        simply for compatibility with other SLALIB time routines.
+  <DT>4.
+<DD>The models used are based on a lunar tidal acceleration value
+        of 
+      <IMG WIDTH="52" HEIGHT="35" ALIGN="MIDDLE" BORDER="0"
+ SRC="img88.gif"
+ ALT="$-26\hspace{-0.05em}^{'\hspace{-0.1em}'}\hspace{-0.4em}.00$">    per century.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Seidelmann, P.K. (ed), 1992.  <I>Explanatory
+Supplement to the Astronomical Almanac,</I> ISBN&nbsp;0-935702-68-7.
+      This contains references to the papers by Stephenson &amp; Morrison
+      and by McCarthy &amp; Babcock which describe the models used here.
+     </DL>
+<BR> <HR>
+<A NAME="tex2html1156" HREF="node74.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1154" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1148" HREF="node72.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1157" HREF="node74.html">SLA_DTF2D - Hour,Min,Sec to Days</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1155" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1149" HREF="node72.html">SLA_DSEP - Angle Between 2 Points on Sphere</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node74.html b/src/slalib/sun67.htx/node74.html
new file mode 100644
index 0000000..88700cd
--- /dev/null
+++ b/src/slalib/sun67.htx/node74.html
@@ -0,0 +1,125 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DTF2D - Hour,Min,Sec to Days</TITLE>
+<META NAME="description" CONTENT="SLA_DTF2D - Hour,Min,Sec to Days">
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+<LINK REL="previous" HREF="node73.html">
+<LINK REL="up" HREF="node13.html">
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+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1166" HREF="node75.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1164" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1158" HREF="node73.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1167" HREF="node75.html">SLA_DTF2R - Hour,Min,Sec to Radians</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1165" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1159" HREF="node73.html">SLA_DT - Approximate ET minus UT</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000461000000000000000">SLA_DTF2D - Hour,Min,Sec to Days</A>
+<A NAME="xref_SLA_DTF2D">&#160;</A><A NAME="SLA_DTF2D">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Convert hours, minutes, seconds to days (double precision).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DTF2D (IHOUR, IMIN, SEC, DAYS, J)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IHOUR</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>hours</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IMIN</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>minutes</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>SEC</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>seconds</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DAYS</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>interval in days</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  0 = OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  1 = IHOUR outside range 0-23</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  2 = IMIN outside range 0-59</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  3 = SEC outside range 0-59.999<IMG WIDTH="21" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img48.gif"
+ ALT="$\cdots$"></TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The result is computed even if any of the range checks fail.
+<DT>2.
+<DD>The sign must be dealt with outside this routine.
+</DL></DL>
+<BR> <HR>
+<A NAME="tex2html1166" HREF="node75.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1164" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1158" HREF="node73.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1167" HREF="node75.html">SLA_DTF2R - Hour,Min,Sec to Radians</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1165" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1159" HREF="node73.html">SLA_DT - Approximate ET minus UT</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node75.html b/src/slalib/sun67.htx/node75.html
new file mode 100644
index 0000000..535d444
--- /dev/null
+++ b/src/slalib/sun67.htx/node75.html
@@ -0,0 +1,125 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DTF2R - Hour,Min,Sec to Radians</TITLE>
+<META NAME="description" CONTENT="SLA_DTF2R - Hour,Min,Sec to Radians">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node76.html">
+<LINK REL="previous" HREF="node74.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node76.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1176" HREF="node76.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1174" HREF="node13.html">
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+<A NAME="tex2html1168" HREF="node74.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1177" HREF="node76.html">SLA_DTP2S - Tangent Plane to Spherical</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1175" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1169" HREF="node74.html">SLA_DTF2D - Hour,Min,Sec to Days</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000462000000000000000">SLA_DTF2R - Hour,Min,Sec to Radians</A>
+<A NAME="xref_SLA_DTF2R">&#160;</A><A NAME="SLA_DTF2R">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Convert hours, minutes, seconds to radians (double precision).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DTF2R (IHOUR, IMIN, SEC, RAD, J)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IHOUR</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>hours</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IMIN</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>minutes</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>SEC</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>seconds</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RAD</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>angle in radians</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  0 = OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  1 = IHOUR outside range 0-23</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  2 = IMIN outside range 0-59</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  3 = SEC outside range 0-59.999<IMG WIDTH="21" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img48.gif"
+ ALT="$\cdots$"></TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The result is computed even if any of the range checks fail.
+<DT>2.
+<DD>The sign must be dealt with outside this routine.
+</DL></DL>
+<BR> <HR>
+<A NAME="tex2html1176" HREF="node76.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1174" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1168" HREF="node74.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1177" HREF="node76.html">SLA_DTP2S - Tangent Plane to Spherical</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1175" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1169" HREF="node74.html">SLA_DTF2D - Hour,Min,Sec to Days</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node76.html b/src/slalib/sun67.htx/node76.html
new file mode 100644
index 0000000..46c4f7a
--- /dev/null
+++ b/src/slalib/sun67.htx/node76.html
@@ -0,0 +1,109 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DTP2S - Tangent Plane to Spherical</TITLE>
+<META NAME="description" CONTENT="SLA_DTP2S - Tangent Plane to Spherical">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node77.html">
+<LINK REL="previous" HREF="node75.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node77.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1186" HREF="node77.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1184" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1178" HREF="node75.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1187" HREF="node77.html">SLA_DTP2V - Tangent Plane to Direction Cosines</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1185" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1179" HREF="node75.html">SLA_DTF2R - Hour,Min,Sec to Radians</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000463000000000000000">SLA_DTP2S - Tangent Plane to Spherical</A>
+<A NAME="xref_SLA_DTP2S">&#160;</A><A NAME="SLA_DTP2S">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Transform tangent plane coordinates into spherical
+coordinates (double precision)
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DTP2S (XI, ETA, RAZ, DECZ, RA, DEC)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>XI,ETA</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>tangent plane rectangular coordinates (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RAZ,DECZ</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>spherical coordinates of tangent point (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RA,DEC</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>spherical coordinates (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The projection is called the <I>gnomonic</I> projection;  the
+Cartesian coordinates <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img85.gif"
+ ALT="$[\,\xi,\eta\,]$"> are called 
+<I>standard coordinates.</I>  The latter
+        are in units of the distance from the tangent plane to the projection
+        point, <I>i.e.</I> radians near the origin.
+  <DT>2.
+<DD>When working in <IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$"> rather than spherical coordinates, the
+        equivalent Cartesian routine sla_DTP2V is available.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1186" HREF="node77.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1184" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1178" HREF="node75.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1187" HREF="node77.html">SLA_DTP2V - Tangent Plane to Direction Cosines</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1185" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1179" HREF="node75.html">SLA_DTF2R - Hour,Min,Sec to Radians</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node77.html b/src/slalib/sun67.htx/node77.html
new file mode 100644
index 0000000..522e009
--- /dev/null
+++ b/src/slalib/sun67.htx/node77.html
@@ -0,0 +1,117 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DTP2V - Tangent Plane to Direction Cosines</TITLE>
+<META NAME="description" CONTENT="SLA_DTP2V - Tangent Plane to Direction Cosines">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node78.html">
+<LINK REL="previous" HREF="node76.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node78.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1196" HREF="node78.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1194" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1188" HREF="node76.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1197" HREF="node78.html">SLA_DTPS2C - Plate centre from and</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1195" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1189" HREF="node76.html">SLA_DTP2S - Tangent Plane to Spherical</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000464000000000000000">SLA_DTP2V - Tangent Plane to Direction Cosines</A>
+<A NAME="xref_SLA_DTP2V">&#160;</A><A NAME="SLA_DTP2V">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Given the tangent-plane coordinates of a star and the direction
+cosines of the tangent point, determine the direction cosines
+         of the star
+         (double precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DTP2V (XI, ETA, V0, V)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>XI,ETA</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>tangent plane coordinates of star (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V0</EM></TD>
+<TD ALIGN="LEFT"><B>D(3)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>direction cosines of tangent point</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V</EM></TD>
+<TH ALIGN="LEFT"><B>D(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>direction cosines of star</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>If vector V0 is not of unit length, the returned vector V will
+be wrong.
+<DT>2.
+<DD>If vector V0 points at a pole, the returned vector V will be
+        based on the arbitrary assumption that <IMG WIDTH="43" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img89.gif"
+ ALT="$\alpha=0$"> at
+        the tangent point.
+  <DT>3.
+<DD>The projection is called the <I>gnomonic</I> projection;  the
+        Cartesian coordinates <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img85.gif"
+ ALT="$[\,\xi,\eta\,]$"> are called 
+        <I>standard coordinates.</I>  The latter
+        are in units of the distance from the tangent plane to the projection
+        point, <I>i.e.</I> radians near the origin.
+  <DT>4.
+<DD>This routine is the Cartesian equivalent of the routine sla_DTP2S.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1196" HREF="node78.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1194" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1188" HREF="node76.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1197" HREF="node78.html">SLA_DTPS2C - Plate centre from and</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1195" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1189" HREF="node76.html">SLA_DTP2S - Tangent Plane to Spherical</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node78.html b/src/slalib/sun67.htx/node78.html
new file mode 100644
index 0000000..61458ac
--- /dev/null
+++ b/src/slalib/sun67.htx/node78.html
@@ -0,0 +1,168 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DTPS2C - Plate centre from and </TITLE>
+<META NAME="description" CONTENT="SLA_DTPS2C - Plate centre from and ">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node79.html">
+<LINK REL="previous" HREF="node77.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node79.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1206" HREF="node79.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1204" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1198" HREF="node77.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1207" HREF="node79.html">SLA_DTPV2C - Plate centre from and x,y,z</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1205" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1199" HREF="node77.html">SLA_DTP2V - Tangent Plane to Direction Cosines</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000465000000000000000">&#160;</A><A NAME="xref_SLA_DTPS2C">&#160;</A><A NAME="SLA_DTPS2C">&#160;</A>
+<BR>
+SLA_DTPS2C - Plate centre from <IMG WIDTH="26" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img90.gif"
+ ALT="$\xi,\eta$"> and <IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img91.gif"
+ ALT="$\alpha,\delta$"></H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>From the tangent plane coordinates of a star of known <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">,determine the <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> of the tangent point (double precision)
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DTPS2C (XI, ETA, RA, DEC, RAZ1, DECZ1, RAZ2, DECZ2, N)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>XI,ETA</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>tangent plane rectangular coordinates (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RA,DEC</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>spherical coordinates (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RAZ1,DECZ1</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>spherical coordinates of tangent point,
+solution 1</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RAZ2,DECZ2</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>spherical coordinates of tangent point,
+solution 2</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>N</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>number of solutions:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  0 = no solutions returned  (note 2)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  1 = only the first solution is useful (note 3)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  2 = there are two useful solutions (note 3)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The RAZ1 and RAZ2 values returned are in the range <IMG WIDTH="43" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img66.gif"
+ ALT="$0\!-\!2\pi$">.<DT>2.
+<DD>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 <IMG WIDTH="10" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img92.gif"
+ ALT="$\xi$"> value, and hence it is
+        meaningless to ask where the tangent point would have to be
+        to bring about this combination of <IMG WIDTH="10" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img92.gif"
+ ALT="$\xi$"> and <IMG WIDTH="10" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img23.gif"
+ ALT="$\delta$">.  <DT>3.
+<DD>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.
+  <DT>4.
+<DD>The DECZ1 and DECZ2 values returned are in the range <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$">,        but in the ordinary, non-pole-crossing, case, the range is
+        <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img15.gif"
+ ALT="$\pm\pi/2$">.  <DT>5.
+<DD>RA, DEC, RAZ1, DECZ1, RAZ2, DECZ2 are all in radians.
+  <DT>6.
+<DD>The projection is called the <I>gnomonic</I> projection;  the
+        Cartesian coordinates <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img85.gif"
+ ALT="$[\,\xi,\eta\,]$"> are called 
+        <I>standard coordinates.</I>  The latter
+        are in units of the distance from the tangent plane to the projection
+        point, <I>i.e.</I> radians near the origin.
+  <DT>7.
+<DD>When working in <IMG WIDTH="58" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img50.gif"
+ ALT="$[\,x,y,z\,]$"> rather than spherical coordinates, the
+        equivalent Cartesian routine sla_DTPV2C is available.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1206" HREF="node79.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1204" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1198" HREF="node77.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1207" HREF="node79.html">SLA_DTPV2C - Plate centre from and x,y,z</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1205" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1199" HREF="node77.html">SLA_DTP2V - Tangent Plane to Direction Cosines</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node79.html b/src/slalib/sun67.htx/node79.html
new file mode 100644
index 0000000..de0194d
--- /dev/null
+++ b/src/slalib/sun67.htx/node79.html
@@ -0,0 +1,144 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DTPV2C - Plate centre from and x,y,z</TITLE>
+<META NAME="description" CONTENT="SLA_DTPV2C - Plate centre from and x,y,z">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node80.html">
+<LINK REL="previous" HREF="node78.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node80.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1216" HREF="node80.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1214" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1208" HREF="node78.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1217" HREF="node80.html">SLA_DTT - TT minus UTC</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1215" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1209" HREF="node78.html">SLA_DTPS2C - Plate centre from and</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000466000000000000000">&#160;</A><A NAME="xref_SLA_DTPV2C">&#160;</A><A NAME="SLA_DTPV2C">&#160;</A>
+<BR>
+SLA_DTPV2C - Plate centre from <IMG WIDTH="26" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img90.gif"
+ ALT="$\xi,\eta$"> and <I>x</I>,<I>y</I>,<I>z</I>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>From the tangent plane coordinates of a star of known
+direction cosines, determine the direction cosines
+         of the tangent point (double precision)
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DTPV2C (XI, ETA, V, V01, V02, N)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>XI,ETA</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>tangent plane coordinates of star (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V</EM></TD>
+<TD ALIGN="LEFT"><B>D(3)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>direction cosines of star</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V01</EM></TD>
+<TH ALIGN="LEFT"><B>D(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>direction cosines of tangent point, solution 1</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V01</EM></TD>
+<TD ALIGN="LEFT"><B>D(3)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>direction cosines of tangent point, solution 2</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>N</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>number of solutions:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  0 = no solutions returned  (note 2)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  1 = only the first solution is useful (note 3)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  2 = there are two useful solutions (note 3)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The vector V must be of unit length or the result will be wrong.
+<DT>2.
+<DD>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.
+  <DT>3.
+<DD>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 can be regarded as valid if
+        the vector V02 is interpreted as the ``over-the-pole'' case.
+  <DT>4.
+<DD>The projection is called the <I>gnomonic</I> projection;  the
+        Cartesian coordinates <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img85.gif"
+ ALT="$[\,\xi,\eta\,]$"> are called 
+        <I>standard coordinates.</I>  The latter
+        are in units of the distance from the tangent plane to the projection
+        point, <I>i.e.</I> radians near the origin.
+  <DT>5.
+<DD>This routine is the Cartesian equivalent of the routine sla_DTPS2C.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1216" HREF="node80.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1214" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1208" HREF="node78.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1217" HREF="node80.html">SLA_DTT - TT minus UTC</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1215" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1209" HREF="node78.html">SLA_DTPS2C - Plate centre from and</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node8.html b/src/slalib/sun67.htx/node8.html
new file mode 100644
index 0000000..81261d2
--- /dev/null
+++ b/src/slalib/sun67.htx/node8.html
@@ -0,0 +1,85 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>C Version</TITLE>
+<META NAME="description" CONTENT="C Version">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node9.html">
+<LINK REL="previous" HREF="node7.html">
+<LINK REL="up" HREF="node2.html">
+<LINK REL="next" HREF="node9.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html325" HREF="node9.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html323" HREF="node2.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html317" HREF="node7.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html326" HREF="node9.html">Future Versions</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html324" HREF="node2.html">INTRODUCTION</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html318" HREF="node7.html">Fortran Version</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION00026000000000000000">
+C Version</A>
+</H2>
+An ANSI C version of SLALIB is available from the author
+but is not part of the Starlink release.
+The functionality of this (proprietary) C version closely matches
+that of the Starlink Fortran SLALIB, partly for the convenience of
+existing users of the Fortran version, some of whom have in the past
+implemented C ``wrappers''.  The function names
+cannot be the same as the Fortran versions because of potential
+linking problems when
+both forms of the library are present; the C routine which
+is the equivalent of (for example) <TT>SLA_REFRO</TT> is <TT>slaRefro</TT>.
+The types of arguments follow the Fortran version, except
+that integers are <TT>int</TT> rather than <TT>long</TT>.
+Argument passing is by value
+(except for arrays and strings of course)
+for given arguments and by pointer for returned arguments.
+All the C functions are re-entrant.
+<P>
+The Fortran routines <TT>sla_GRESID</TT>, <TT>sla_RANDOM</TT> and
+<TT>sla_WAIT</TT> have no C counterparts.
+<P>
+Further details of the C version of SLALIB are available
+from the author.  The definitive guide to
+the calling sequences is the file <TT>slalib.h</TT>.
+<P>
+<BR> <HR>
+<A NAME="tex2html325" HREF="node9.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html323" HREF="node2.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html317" HREF="node7.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html326" HREF="node9.html">Future Versions</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html324" HREF="node2.html">INTRODUCTION</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html318" HREF="node7.html">Fortran Version</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node80.html b/src/slalib/sun67.htx/node80.html
new file mode 100644
index 0000000..e7704f5
--- /dev/null
+++ b/src/slalib/sun67.htx/node80.html
@@ -0,0 +1,111 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DTT - TT minus UTC</TITLE>
+<META NAME="description" CONTENT="SLA_DTT - TT minus UTC">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node81.html">
+<LINK REL="previous" HREF="node79.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node81.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1226" HREF="node81.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1224" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1218" HREF="node79.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1227" HREF="node81.html">SLA_DV2TP - Direction Cosines to Tangent Plane</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1225" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1219" HREF="node79.html">SLA_DTPV2C - Plate centre from and x,y,z</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000467000000000000000">SLA_DTT - TT minus UTC</A>
+<A NAME="xref_SLA_DTT">&#160;</A><A NAME="SLA_DTT">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Compute <IMG WIDTH="16" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img19.gif"
+ ALT="$\Delta$">TT, the increment to be applied to
+Coordinated Universal Time UTC to give
+         Terrestrial Time TT.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>D&nbsp;=&nbsp;sla_DTT (DJU)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DJU</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>UTC date as a modified JD (JD-2400000.5)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_DTT</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>TT-UTC in seconds</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The UTC is specified to be a date rather than a time to indicate
+that care needs to be taken not to specify an instant which lies
+within a leap second.  Though in most cases UTC can include the
+        fractional part, correct behaviour on the day of a leap second
+        can be guaranteed only up to the end of the second
+        <IMG WIDTH="82" HEIGHT="17" ALIGN="BOTTOM" BORDER="0"
+ SRC="img54.gif"
+ ALT="$23^{\rm h}\,59^{\rm m}\,59^{\rm s}$">.  <DT>2.
+<DD>Pre 1972 January 1 a fixed value of 10 + ET-TAI is returned.
+  <DT>3.
+<DD>TT is one interpretation of the defunct timescale
+        <I>Ephemeris Time</I>, ET.
+  <DT>4.
+<DD>See also the routine sla_DT, which roughly estimates ET-UT for
+        historical epochs.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1226" HREF="node81.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1224" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1218" HREF="node79.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1227" HREF="node81.html">SLA_DV2TP - Direction Cosines to Tangent Plane</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1225" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1219" HREF="node79.html">SLA_DTPV2C - Plate centre from and x,y,z</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node81.html b/src/slalib/sun67.htx/node81.html
new file mode 100644
index 0000000..eba8ed9
--- /dev/null
+++ b/src/slalib/sun67.htx/node81.html
@@ -0,0 +1,137 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DV2TP - Direction Cosines to Tangent Plane</TITLE>
+<META NAME="description" CONTENT="SLA_DV2TP - Direction Cosines to Tangent Plane">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node82.html">
+<LINK REL="previous" HREF="node80.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node82.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1236" HREF="node82.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1234" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1228" HREF="node80.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1237" HREF="node82.html">SLA_DVDV - Scalar Product</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1235" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1229" HREF="node80.html">SLA_DTT - TT minus UTC</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000468000000000000000">SLA_DV2TP - Direction Cosines to Tangent Plane</A>
+<A NAME="xref_SLA_DV2TP">&#160;</A><A NAME="SLA_DV2TP">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Given the direction cosines of a star and of the tangent point,
+determine the star's tangent-plane coordinates
+         (double precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DV2TP (V, V0, XI, ETA, J)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V</EM></TD>
+<TH ALIGN="LEFT"><B>D(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>direction cosines of star</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V0</EM></TD>
+<TD ALIGN="LEFT"><B>D(3)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>direction cosines of tangent point</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>XI,ETA</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>tangent plane coordinates (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>J</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  0 = OK, star on tangent plane</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  1 = error, star too far from axis</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  2 = error, antistar on tangent plane</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  3 = error, antistar too far from axis</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>If vector V0 is not of unit length, or if vector V is of zero
+length, the results will be wrong.
+<DT>2.
+<DD>If V0 points at a pole, the returned <IMG WIDTH="26" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img90.gif"
+ ALT="$\xi,\eta$">        will be based on the
+        arbitrary assumption that <IMG WIDTH="43" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img89.gif"
+ ALT="$\alpha=0$"> at the tangent point.
+  <DT>3.
+<DD>The projection is called the <I>gnomonic</I> projection;  the
+        Cartesian coordinates <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img85.gif"
+ ALT="$[\,\xi,\eta\,]$"> are called 
+        <I>standard coordinates.</I>  The latter
+        are in units of the distance from the tangent plane to the projection
+        point, <I>i.e.</I> radians near the origin.
+  <DT>4.
+<DD>This routine is the Cartesian equivalent of the routine sla_DS2TP.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1236" HREF="node82.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1234" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1228" HREF="node80.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1237" HREF="node82.html">SLA_DVDV - Scalar Product</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1235" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1229" HREF="node80.html">SLA_DTT - TT minus UTC</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node82.html b/src/slalib/sun67.htx/node82.html
new file mode 100644
index 0000000..024100b
--- /dev/null
+++ b/src/slalib/sun67.htx/node82.html
@@ -0,0 +1,91 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DVDV - Scalar Product</TITLE>
+<META NAME="description" CONTENT="SLA_DVDV - Scalar Product">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node83.html">
+<LINK REL="previous" HREF="node81.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node83.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1246" HREF="node83.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1244" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1238" HREF="node81.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1247" HREF="node83.html">SLA_DVN - Normalize Vector</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1245" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1239" HREF="node81.html">SLA_DV2TP - Direction Cosines to Tangent Plane</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000469000000000000000">SLA_DVDV - Scalar Product</A>
+<A NAME="xref_SLA_DVDV">&#160;</A><A NAME="SLA_DVDV">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Scalar product of two 3-vectors (double precision).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>D&nbsp;=&nbsp;sla_DVDV (VA, VB)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>VA</EM></TD>
+<TH ALIGN="LEFT"><B>D(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>first vector</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>VB</EM></TD>
+<TD ALIGN="LEFT"><B>D(3)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>second vector</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_DVDV</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>scalar product VA.VB</TD>
+</TR>
+</TABLE></DL>
+<BR> <HR>
+<A NAME="tex2html1246" HREF="node83.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1244" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1238" HREF="node81.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1247" HREF="node83.html">SLA_DVN - Normalize Vector</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1245" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1239" HREF="node81.html">SLA_DV2TP - Direction Cosines to Tangent Plane</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node83.html b/src/slalib/sun67.htx/node83.html
new file mode 100644
index 0000000..073d4ef
--- /dev/null
+++ b/src/slalib/sun67.htx/node83.html
@@ -0,0 +1,95 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DVN - Normalize Vector</TITLE>
+<META NAME="description" CONTENT="SLA_DVN - Normalize Vector">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node84.html">
+<LINK REL="previous" HREF="node82.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node84.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1256" HREF="node84.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1254" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1248" HREF="node82.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1257" HREF="node84.html">SLA_DVXV - Vector Product</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1255" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1249" HREF="node82.html">SLA_DVDV - Scalar Product</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000470000000000000000">SLA_DVN - Normalize Vector</A>
+<A NAME="xref_SLA_DVN">&#160;</A><A NAME="SLA_DVN">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Normalize a 3-vector, also giving the modulus (double precision).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DVN (V, UV, VM)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>V</EM></TD>
+<TH ALIGN="LEFT"><B>D(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>vector</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>UV</EM></TD>
+<TH ALIGN="LEFT"><B>D(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>unit vector in direction of V</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>VM</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>modulus of V</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTE:</STRONG>
+<DD>If the modulus of V is zero, UV is set to zero as well.
+</DL>
+<BR> <HR>
+<A NAME="tex2html1256" HREF="node84.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1254" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1248" HREF="node82.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1257" HREF="node84.html">SLA_DVXV - Vector Product</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1255" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1249" HREF="node82.html">SLA_DVDV - Scalar Product</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node84.html b/src/slalib/sun67.htx/node84.html
new file mode 100644
index 0000000..745d1f0
--- /dev/null
+++ b/src/slalib/sun67.htx/node84.html
@@ -0,0 +1,93 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_DVXV - Vector Product</TITLE>
+<META NAME="description" CONTENT="SLA_DVXV - Vector Product">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node85.html">
+<LINK REL="previous" HREF="node83.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node85.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1266" HREF="node85.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1264" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1258" HREF="node83.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1267" HREF="node85.html">SLA_E2H - to Az,El</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1265" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1259" HREF="node83.html">SLA_DVN - Normalize Vector</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000471000000000000000">SLA_DVXV - Vector Product</A>
+<A NAME="xref_SLA_DVXV">&#160;</A><A NAME="SLA_DVXV">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Vector product of two 3-vectors (double precision).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DVXV (VA, VB, VC)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>VA</EM></TD>
+<TH ALIGN="LEFT"><B>D(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>first vector</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>VB</EM></TD>
+<TD ALIGN="LEFT"><B>D(3)</B></TD>
+<TD ALIGN="LEFT" NOWRAP>second vector</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>VC</EM></TD>
+<TH ALIGN="LEFT"><B>D(3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>vector product VA<IMG WIDTH="15" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img84.gif"
+ ALT="$\times$">VB</TD>
+</TR>
+</TABLE></DL>
+<BR> <HR>
+<A NAME="tex2html1266" HREF="node85.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1264" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1258" HREF="node83.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1267" HREF="node85.html">SLA_E2H - to Az,El</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1265" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1259" HREF="node83.html">SLA_DVN - Normalize Vector</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node85.html b/src/slalib/sun67.htx/node85.html
new file mode 100644
index 0000000..3c589df
--- /dev/null
+++ b/src/slalib/sun67.htx/node85.html
@@ -0,0 +1,145 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_E2H - to Az,El</TITLE>
+<META NAME="description" CONTENT="SLA_E2H - to Az,El">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node86.html">
+<LINK REL="previous" HREF="node84.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node86.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1276" HREF="node86.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1274" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1268" HREF="node84.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1277" HREF="node86.html">SLA_EARTH - Approx Earth Pos/Vel</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1275" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1269" HREF="node84.html">SLA_DVXV - Vector Product</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000472000000000000000">&#160;</A><A NAME="xref_SLA_E2H">&#160;</A><A NAME="SLA_E2H">&#160;</A>
+<BR>
+SLA_E2H - <IMG WIDTH="27" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img65.gif"
+ ALT="$h,\delta$"> to Az,El
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Equatorial to horizon coordinates
+(single precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_DE2H (HA, DEC, PHI, AZ, EL)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>HA</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>hour angle (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DEC</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>declination (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PHI</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>latitude (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AZ</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>azimuth (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EL</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>elevation (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>Azimuth is returned in the range <IMG WIDTH="43" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img66.gif"
+ ALT="$0\!-\!2\pi$">;  north is zero,
+and east is <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img14.gif"
+ ALT="$+\pi/2$">.  Elevation is returned in the range
+<IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$">.  <DT>2.
+<DD>The latitude must be geodetic.  In critical applications,
+        corrections for polar motion should be applied.
+  <DT>3.
+<DD>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 <I>observed</I> <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$">, and the elevation
+        <I>in vacuo</I>, which would require the <I>topocentric</I>
+        <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$">.        If the effects of diurnal aberration can be neglected, the
+        <I>apparent</I> <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$"> may be used instead of the topocentric
+        <IMG WIDTH="41" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img29.gif"
+ ALT="$[\,h,\delta\,]$">.  <DT>4.
+<DD>No range checking of arguments is carried out.
+  <DT>5.
+<DD>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.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1276" HREF="node86.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1274" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1268" HREF="node84.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1277" HREF="node86.html">SLA_EARTH - Approx Earth Pos/Vel</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1275" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1269" HREF="node84.html">SLA_DVXV - Vector Product</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node86.html b/src/slalib/sun67.htx/node86.html
new file mode 100644
index 0000000..6507524
--- /dev/null
+++ b/src/slalib/sun67.htx/node86.html
@@ -0,0 +1,124 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_EARTH - Approx Earth Pos/Vel</TITLE>
+<META NAME="description" CONTENT="SLA_EARTH - Approx Earth Pos/Vel">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node87.html">
+<LINK REL="previous" HREF="node85.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node87.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1286" HREF="node87.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1284" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1278" HREF="node85.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1287" HREF="node87.html">SLA_ECLEQ - Ecliptic to Equatorial</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1285" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1279" HREF="node85.html">SLA_E2H - to Az,El</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000473000000000000000">SLA_EARTH - Approx Earth Pos/Vel</A>
+<A NAME="xref_SLA_EARTH">&#160;</A><A NAME="SLA_EARTH">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Approximate heliocentric position and velocity of the Earth
+(single precision).
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_EARTH (IY, ID, FD, PV)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IY</EM></TD>
+<TH ALIGN="LEFT"><B>I</B></TH>
+<TD ALIGN="LEFT" NOWRAP>year</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ID</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>day in year (1 = Jan 1st)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>FD</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>fraction of day</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PV</EM></TD>
+<TH ALIGN="LEFT"><B>R(6)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>Earth <IMG WIDTH="106" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img51.gif"
+ ALT="$[\,x,y,z,\dot{x},\dot{y},\dot{z}\,]$"> (AU, AU&nbsp;s<SUP>-1</SUP>)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The date and time is TDB (loosely ET) in a Julian calendar
+which has been aligned to the ordinary Gregorian
+calendar for the interval 1900&nbsp;March&nbsp;1 to 2100&nbsp;February&nbsp;28.
+        The year and day can be obtained by calling sla_CALYD or
+        sla_CLYD.
+  <DT>2.
+<DD>The Earth heliocentric 6-vector is referred to the
+        FK4 mean equator and equinox of date.
+  <DT>3.
+<DD>Maximum/RMS errors 1950-2050:
+        <UL>
+<LI> 13/5&nbsp;<IMG WIDTH="48" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img93.gif"
+ ALT="$\times10^{-5}$">&nbsp;AU = 19200/7600&nbsp;km in position
+<LI> 47/26&nbsp;<IMG WIDTH="55" HEIGHT="31" ALIGN="MIDDLE" BORDER="0"
+ SRC="img94.gif"
+ ALT="$\times10^{-10}$">&nbsp;AU&nbsp;s<SUP>-1</SUP> =
+               0.0070/0.0039&nbsp;km&nbsp;s<SUP>-1</SUP> in speed
+        </UL>
+  <DT>4.
+<DD>More accurate results are obtainable with the routine sla_EVP.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1286" HREF="node87.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1284" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1278" HREF="node85.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1287" HREF="node87.html">SLA_ECLEQ - Ecliptic to Equatorial</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1285" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1279" HREF="node85.html">SLA_E2H - to Az,El</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node87.html b/src/slalib/sun67.htx/node87.html
new file mode 100644
index 0000000..5935487
--- /dev/null
+++ b/src/slalib/sun67.htx/node87.html
@@ -0,0 +1,97 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_ECLEQ - Ecliptic to Equatorial</TITLE>
+<META NAME="description" CONTENT="SLA_ECLEQ - Ecliptic to Equatorial">
+<META NAME="keywords" CONTENT="sun67">
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+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1288" HREF="node86.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1297" HREF="node88.html">SLA_ECMAT - Form Matrix</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1295" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1289" HREF="node86.html">SLA_EARTH - Approx Earth Pos/Vel</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000474000000000000000">SLA_ECLEQ - Ecliptic to Equatorial</A>
+<A NAME="xref_SLA_ECLEQ">&#160;</A><A NAME="SLA_ECLEQ">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Transformation from ecliptic longitude and latitude to
+J2000.0 <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$">.<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_ECLEQ (DL, DB, DATE, DR, DD)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DL,DB</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>ecliptic longitude and latitude
+(mean of date, IAU 1980 theory, radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>TDB (formerly ET) as Modified Julian Date
+(JD-2400000.5)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DR,DD</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 mean <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> (radians)</TD>
+</TR>
+</TABLE></DL>
+<BR> <HR>
+<A NAME="tex2html1296" HREF="node88.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1294" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1288" HREF="node86.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1297" HREF="node88.html">SLA_ECMAT - Form Matrix</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1295" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1289" HREF="node86.html">SLA_EARTH - Approx Earth Pos/Vel</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node88.html b/src/slalib/sun67.htx/node88.html
new file mode 100644
index 0000000..895c629
--- /dev/null
+++ b/src/slalib/sun67.htx/node88.html
@@ -0,0 +1,106 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_ECMAT - Form Matrix</TITLE>
+<META NAME="description" CONTENT="SLA_ECMAT - Form Matrix">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node89.html">
+<LINK REL="previous" HREF="node87.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node89.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1306" HREF="node89.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1304" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1298" HREF="node87.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1307" HREF="node89.html">SLA_ECOR - RV &amp; Time Corrns to Sun</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1305" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1299" HREF="node87.html">SLA_ECLEQ - Ecliptic to Equatorial</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000475000000000000000">&#160;</A><A NAME="xref_SLA_ECMAT">&#160;</A><A NAME="SLA_ECMAT">&#160;</A>
+<BR>
+SLA_ECMAT - Form <IMG WIDTH="81" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img95.gif"
+ ALT="$\alpha,\delta\rightarrow\lambda,\beta$"> Matrix
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Form the equatorial to ecliptic rotation matrix (IAU 1980 theory).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_ECMAT (DATE, RMAT)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>TDB (formerly ET) as Modified Julian Date
+(JD-2400000.5)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RMAT</EM></TD>
+<TH ALIGN="LEFT"><B>D(3,3)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>rotation matrix</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>RMAT is matrix <B>M</B> in the expression
+<B>v</B><SUB><I>ecl</I></SUB>&nbsp;=&nbsp;<B>M</B><IMG WIDTH="7" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img72.gif"
+ ALT="$\cdot$"><B>v</B><SUB><I>equ</I></SUB>.
+<DT>2.
+<DD>The equator, equinox and ecliptic are mean of date.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Murray, C.A., <I>Vectorial Astrometry</I>, section 4.3.
+</DL>
+<BR> <HR>
+<A NAME="tex2html1306" HREF="node89.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1304" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1298" HREF="node87.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1307" HREF="node89.html">SLA_ECOR - RV &amp; Time Corrns to Sun</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1305" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1299" HREF="node87.html">SLA_ECLEQ - Ecliptic to Equatorial</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node89.html b/src/slalib/sun67.htx/node89.html
new file mode 100644
index 0000000..990df2a
--- /dev/null
+++ b/src/slalib/sun67.htx/node89.html
@@ -0,0 +1,140 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_ECOR - RV &amp; Time Corrns to Sun</TITLE>
+<META NAME="description" CONTENT="SLA_ECOR - RV &amp; Time Corrns to Sun">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node90.html">
+<LINK REL="previous" HREF="node88.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node90.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1316" HREF="node90.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1314" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1308" HREF="node88.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1317" HREF="node90.html">SLA_EG50 - B1950 to Galactic</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1315" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1309" HREF="node88.html">SLA_ECMAT - Form Matrix</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000476000000000000000">SLA_ECOR - RV &amp; Time Corrns to Sun</A>
+<A NAME="xref_SLA_ECOR">&#160;</A><A NAME="SLA_ECOR">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Component of Earth orbit velocity and heliocentric
+light time in a given direction.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_ECOR (RM, DM, IY, ID, FD, RV, TL)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RM,DM</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>mean <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> of date (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>IY</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>year</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ID</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>day in year (1 = Jan 1st)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>FD</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>fraction of day</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>RV</EM></TD>
+<TH ALIGN="LEFT"><B>R</B></TH>
+<TD ALIGN="LEFT" NOWRAP>component of Earth orbital velocity (km&nbsp;s<SUP>-1</SUP>)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>TL</EM></TD>
+<TD ALIGN="LEFT"><B>R</B></TD>
+<TD ALIGN="LEFT" NOWRAP>component of heliocentric light time (s)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The date and time is TDB (loosely ET) in a Julian calendar
+which has been aligned to the ordinary Gregorian
+calendar for the interval 1900 March 1 to 2100 February 28.
+        The year and day can be obtained by calling sla_CALYD or
+        sla_CLYD.
+  <DT>2.
+<DD>Sign convention:
+        <UL>
+<LI> The velocity component is +ve when the
+               Earth is receding from
+               the given point on the sky.
+<LI> The light time component is +ve
+               when the Earth lies between the Sun and
+               the given point on the sky.
+        </UL>
+ <DT>3.
+<DD>Accuracy:
+       <UL>
+<LI> The velocity component is usually within 0.004&nbsp;km&nbsp;s<SUP>-1</SUP>
+              of the correct value and is never in error by more than
+              0.007&nbsp;km&nbsp;s<SUP>-1</SUP>.
+<LI> The error in light time correction is about
+              <IMG WIDTH="32" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img96.gif"
+ ALT="$0^{\rm s}\hspace{-0.3em}.03$"> at worst,
+              but is usually better than <IMG WIDTH="32" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img97.gif"
+ ALT="$0^{\rm s}\hspace{-0.3em}.01$">.       </UL>
+       For applications requiring higher accuracy, see the sla_EVP routine.
+ </DL></DL>
+<BR> <HR>
+<A NAME="tex2html1316" HREF="node90.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1314" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1308" HREF="node88.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1317" HREF="node90.html">SLA_EG50 - B1950 to Galactic</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1315" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1309" HREF="node88.html">SLA_ECMAT - Form Matrix</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node9.html b/src/slalib/sun67.htx/node9.html
new file mode 100644
index 0000000..a9d8058
--- /dev/null
+++ b/src/slalib/sun67.htx/node9.html
@@ -0,0 +1,75 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>Future Versions</TITLE>
+<META NAME="description" CONTENT="Future Versions">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node10.html">
+<LINK REL="previous" HREF="node8.html">
+<LINK REL="up" HREF="node2.html">
+<LINK REL="next" HREF="node10.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html335" HREF="node10.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html333" HREF="node2.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html327" HREF="node8.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html336" HREF="node10.html">New Functions</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html334" HREF="node2.html">INTRODUCTION</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html328" HREF="node8.html">C Version</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION00027000000000000000">
+Future Versions</A>
+</H2>
+The homogeneity and ease of use of SLALIB could perhaps be improved
+in the future
+by turning to C++ and object-oriented techniques.  For example ``celestial
+position'' could be a class and many of the transformations
+could happen automatically.  This requires further study and
+would almost certainly result in a complete redesign.
+Similarly,
+the impact of Fortran&nbsp;90 has yet to be assessed.  Once compilers
+become widely available, some internal recoding may be worthwhile
+in order to simplify parts of the code.  However, as with C++,
+a redesign of the
+application interfaces will be needed if the capabilities of the
+new language are to be exploited to the full.
+<P>
+<BR> <HR>
+<A NAME="tex2html335" HREF="node10.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html333" HREF="node2.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html327" HREF="node8.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html336" HREF="node10.html">New Functions</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html334" HREF="node2.html">INTRODUCTION</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html328" HREF="node8.html">C Version</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node90.html b/src/slalib/sun67.htx/node90.html
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@@ -0,0 +1,106 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_EG50 - B1950 to Galactic</TITLE>
+<META NAME="description" CONTENT="SLA_EG50 - B1950 to Galactic">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1327" HREF="node91.html">SLA_EL2UE - Conventional to Universal Elements</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1325" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1319" HREF="node89.html">SLA_ECOR - RV &amp; Time Corrns to Sun</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000477000000000000000">&#160;</A><A NAME="xref_SLA_EG50">&#160;</A><A NAME="SLA_EG50">&#160;</A>
+<BR>
+SLA_EG50 - B1950 <IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img91.gif"
+ ALT="$\alpha,\delta$"> to Galactic
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Transformation from B1950.0 FK4 equatorial coordinates to
+IAU 1958 galactic coordinates.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_EG50 (DR, DD, DL, DB)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DR,DD</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>B1950.0 <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DL,DB</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>galactic longitude and latitude <IMG WIDTH="59" HEIGHT="32" ALIGN="MIDDLE" BORDER="0"
+ SRC="img98.gif"
+ ALT="$[\,l^{I\!I},b^{I\!I}\,]$"> (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTE:</STRONG>
+<DD>The equatorial coordinates are B1950.0 FK4.  Use the
+routine sla_EQGAL if conversion from J2000.0 FK5 coordinates
+       is required.
+      </DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Blaauw <I>et al.</I>, 1960, <I>Mon.Not.R.astr.Soc.</I>,
+<B>121</B>, 123.
+     </DL>
+<BR> <HR>
+<A NAME="tex2html1326" HREF="node91.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1324" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1318" HREF="node89.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1327" HREF="node91.html">SLA_EL2UE - Conventional to Universal Elements</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1325" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1319" HREF="node89.html">SLA_ECOR - RV &amp; Time Corrns to Sun</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node91.html b/src/slalib/sun67.htx/node91.html
new file mode 100644
index 0000000..2beedff
--- /dev/null
+++ b/src/slalib/sun67.htx/node91.html
@@ -0,0 +1,330 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_EL2UE - Conventional to Universal Elements</TITLE>
+<META NAME="description" CONTENT="SLA_EL2UE - Conventional to Universal Elements">
+<META NAME="keywords" CONTENT="sun67">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1337" HREF="node92.html">SLA_EPB - MJD to Besselian Epoch</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1335" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1329" HREF="node90.html">SLA_EG50 - B1950 to Galactic</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000478000000000000000">SLA_EL2UE - Conventional to Universal Elements</A>
+<A NAME="xref_SLA_EL2UE">&#160;</A><A NAME="SLA_EL2UE">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Transform conventional osculating orbital elements
+into ``universal'' form.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_EL2UE (
+         DATE, JFORM, EPOCH, ORBINC, ANODE,
+         PERIH, AORQ, E, AORL, DM,
+         U, JSTAT)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>epoch (TT MJD) of osculation (Note&nbsp;3)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JFORM</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>choice of element set (1-3; Note&nbsp;6)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EPOCH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>epoch of elements (<I>t<SUB>0</SUB></I> or <I>T</I>, TT MJD)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ORBINC</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>inclination (<I>i</I>, radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>ANODE</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>longitude of the ascending node (<IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$">, radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>PERIH</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>longitude or argument of perihelion
+(<IMG WIDTH="16" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img100.gif"
+ ALT="$\varpi$"> or <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$">,</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AORQ</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>mean distance or perihelion distance (<I>a</I> or <I>q</I>, AU)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>E</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>eccentricity (<I>e</I>)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>AORL</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>mean anomaly or longitude
+(<I>M</I> or <I>L</I>, radians,</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>  JFORM=1,2 only)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DM</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>daily motion (<I>n</I>, radians, JFORM=1 only)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>U</EM></TD>
+<TH ALIGN="LEFT"><B>D(13)</B></TH>
+<TD ALIGN="LEFT" NOWRAP>universal orbital elements (Note&nbsp;1)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(1)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>combined mass (<I>M</I>+<I>m</I>)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(2)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>total energy of the orbit (<IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$">)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(3)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>reference (osculating) epoch (<I>t<SUB>0</SUB></I>)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(4-6)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>position at reference epoch (<IMG WIDTH="17" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img102.gif"
+ ALT="${\rm \bf r}_0$">)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(7-9)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>velocity at reference epoch (<IMG WIDTH="19" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img103.gif"
+ ALT="${\rm \bf v}_0$">)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(10)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>heliocentric distance at reference epoch</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(11)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP><IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img104.gif"
+ ALT="${\rm \bf r}_0.{\rm \bf v}_0$"></TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(12)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>date (<I>t</I>)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="CENTER" NOWRAP COLSPAN=1>(13)</TD>
+<TD></TD>
+<TD ALIGN="LEFT" NOWRAP>universal eccentric anomaly (<IMG WIDTH="14" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img105.gif"
+ ALT="$\psi$">) of date,
+approx</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT">&nbsp;</TD>
+<TD ALIGN="LEFT">&nbsp;</TD>
+<TD ALIGN="LEFT" NOWRAP>&nbsp;</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>JSTAT</EM></TD>
+<TD ALIGN="LEFT"><B>I</B></TD>
+<TD ALIGN="LEFT" NOWRAP>status:</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>        0 = OK</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>   -1 = illegal JFORM</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>    -2 = illegal E</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>    -3 = illegal AORQ</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>    -4 = illegal DM</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM></EM></TD>
+<TD ALIGN="LEFT"><B></B></TD>
+<TD ALIGN="LEFT" NOWRAP>    -5 = numerical error</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>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)&nbsp;<IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img24.gif"
+ ALT="$\alpha$">, which is proportional to the total energy of the
+        orbit, (ii)&nbsp;the heliocentric distance at epoch,
+        (iii)&nbsp;the outwards component of the velocity at the given epoch,
+        (iv)&nbsp;an estimate of <IMG WIDTH="14" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img105.gif"
+ ALT="$\psi$">, the ``universal eccentric anomaly'' at a
+        given date and (v)&nbsp;that date.
+  <DT>2.
+<DD>The companion routine is sla_UE2PV.  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 sla_UE2PV;
+        for convenience, the two calls are packaged as the routine
+        sla_PLANEL.  Multiple predictions may be made by again calling the
+        present routine once, but then calling sla_UE2PV multiple times,
+        which is faster than multiple calls to sla_PLANEL.
+  <DT>3.
+<DD>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).
+  <DT>4.
+<DD>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.
+  <DT>5.
+<DD>The universal elements returned in the array U are in canonical
+        units (solar masses, AU and canonical days).
+  <DT>6.
+<DD>Three different element-format options are supported, as
+        follows. <BR>
+<P>
+JFORM=1, suitable for the major planets:
+<P>        <PRE><TT>
+ 		 EPOCH 		 = 		 epoch of elements <I>t<SUB>0</SUB></I> (TT MJD)
+		 ORBINC 		 = 		 inclination <I>i</I> (radians)
+		 ANODE 		 = 		 longitude of the ascending node <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> (radians)
+		 PERIH 		 = 		 longitude of perihelion <IMG WIDTH="16" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img100.gif"
+ ALT="$\varpi$"> (radians)
+		 AORQ 		 = 		 mean distance <I>a</I> (AU)
+		 E 		 = 		 eccentricity <I>e</I> <IMG WIDTH="83" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img106.gif"
+ ALT="$( 0 \leq e < 1 )$"> 
+		 AORL 		 = 		 mean longitude <I>L</I> (radians)
+		 DM 		 = 		 daily motion <I>n</I> (radians)        
+</TT></PRE>
+<P>
+JFORM=2, suitable for minor planets:
+<P>        <PRE><TT>
+ 		 EPOCH 		 = 		 epoch of elements <I>t<SUB>0</SUB></I> (TT MJD)
+		 ORBINC 		 = 		 inclination <I>i</I> (radians)
+		 ANODE 		 = 		 longitude of the ascending node <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> (radians)
+		 PERIH 		 = 		 argument of perihelion <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$"> (radians)
+		 AORQ 		 = 		 mean distance <I>a</I> (AU)
+		 E 		 = 		 eccentricity <I>e</I> <IMG WIDTH="83" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img106.gif"
+ ALT="$( 0 \leq e < 1 )$"> 
+		 AORL 		 = 		 mean anomaly <I>M</I> (radians)        
+</TT></PRE>
+<P>
+JFORM=3, suitable for comets:
+<P>        <PRE><TT>
+ 		 EPOCH 		 = 		 epoch of perihelion <I>T</I> (TT MJD)
+		 ORBINC 		 = 		 inclination <I>i</I> (radians)
+		 ANODE 		 = 		 longitude of the ascending node <IMG WIDTH="14" HEIGHT="13" ALIGN="BOTTOM" BORDER="0"
+ SRC="img99.gif"
+ ALT="$\Omega$"> (radians)
+		 PERIH 		 = 		 argument of perihelion <IMG WIDTH="13" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
+ SRC="img101.gif"
+ ALT="$\omega$"> (radians)
+		 AORQ 		 = 		 perihelion distance <I>q</I> (AU)
+		 E 		 = 		 eccentricity <I>e</I> <IMG WIDTH="91" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img107.gif"
+ ALT="$( 0 \leq e \leq 10 )$"></TT></PRE>
+  <DT>7.
+<DD>Unused elements (DM for JFORM=2, AORL and DM for JFORM=3) are
+        not accessed.
+  <DT>8.
+<DD>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.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Everhart, E. &amp; Pitkin, E.T., Am.&nbsp;J.&nbsp;Phys.&nbsp;51, 712, 1983.
+</DL>
+<BR> <HR>
+<A NAME="tex2html1336" HREF="node92.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1334" HREF="node13.html">
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1337" HREF="node92.html">SLA_EPB - MJD to Besselian Epoch</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1335" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1329" HREF="node90.html">SLA_EG50 - B1950 to Galactic</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node92.html b/src/slalib/sun67.htx/node92.html
new file mode 100644
index 0000000..854488f
--- /dev/null
+++ b/src/slalib/sun67.htx/node92.html
@@ -0,0 +1,91 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_EPB - MJD to Besselian Epoch</TITLE>
+<META NAME="description" CONTENT="SLA_EPB - MJD to Besselian Epoch">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node93.html">
+<LINK REL="previous" HREF="node91.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node93.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1346" HREF="node93.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1344" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1338" HREF="node91.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1347" HREF="node93.html">SLA_EPB2D - Besselian Epoch to MJD</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1345" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1339" HREF="node91.html">SLA_EL2UE - Conventional to Universal Elements</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000479000000000000000">SLA_EPB - MJD to Besselian Epoch</A>
+<A NAME="xref_SLA_EPB">&#160;</A><A NAME="SLA_EPB">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Conversion of Modified Julian Date to Besselian Epoch.
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>D&nbsp;=&nbsp;sla_EPB (DATE)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>Modified Julian Date (JD-2400000.5)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_EPB</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>Besselian Epoch</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Lieske, J.H., 1979, <I>Astr.Astrophys.</I> <B>73</B>, 282.
+</DL>
+<BR> <HR>
+<A NAME="tex2html1346" HREF="node93.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1344" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1338" HREF="node91.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1347" HREF="node93.html">SLA_EPB2D - Besselian Epoch to MJD</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1345" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1339" HREF="node91.html">SLA_EL2UE - Conventional to Universal Elements</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node93.html b/src/slalib/sun67.htx/node93.html
new file mode 100644
index 0000000..c142fe7
--- /dev/null
+++ b/src/slalib/sun67.htx/node93.html
@@ -0,0 +1,91 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_EPB2D - Besselian Epoch to MJD</TITLE>
+<META NAME="description" CONTENT="SLA_EPB2D - Besselian Epoch to MJD">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node94.html">
+<LINK REL="previous" HREF="node92.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node94.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1356" HREF="node94.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1354" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1348" HREF="node92.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1357" HREF="node94.html">SLA_EPCO - Convert Epoch to B or J</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1355" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1349" HREF="node92.html">SLA_EPB - MJD to Besselian Epoch</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000480000000000000000">SLA_EPB2D - Besselian Epoch to MJD</A>
+<A NAME="xref_SLA_EPB2D">&#160;</A><A NAME="SLA_EPB2D">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Conversion of Besselian Epoch to Modified Julian Date.
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>D&nbsp;=&nbsp;sla_EPB2D (EPB)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EPB</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>Besselian Epoch</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_EPB2D</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>Modified Julian Date (JD-2400000.5)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Lieske, J.H., 1979. <I>Astr.Astrophys.</I> <B>73</B>, 282.
+</DL>
+<BR> <HR>
+<A NAME="tex2html1356" HREF="node94.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1354" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1348" HREF="node92.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1357" HREF="node94.html">SLA_EPCO - Convert Epoch to B or J</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1355" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1349" HREF="node92.html">SLA_EPB - MJD to Besselian Epoch</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node94.html b/src/slalib/sun67.htx/node94.html
new file mode 100644
index 0000000..e71fda8
--- /dev/null
+++ b/src/slalib/sun67.htx/node94.html
@@ -0,0 +1,110 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_EPCO - Convert Epoch to B or J</TITLE>
+<META NAME="description" CONTENT="SLA_EPCO - Convert Epoch to B or J">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node95.html">
+<LINK REL="previous" HREF="node93.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node95.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1366" HREF="node95.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1364" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1358" HREF="node93.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1367" HREF="node95.html">SLA_EPJ - MJD to Julian Epoch</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1365" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1359" HREF="node93.html">SLA_EPB2D - Besselian Epoch to MJD</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000481000000000000000">SLA_EPCO - Convert Epoch to B or J</A>
+<A NAME="xref_SLA_EPCO">&#160;</A><A NAME="SLA_EPCO">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Convert an epoch to Besselian or Julian to match another one.
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>D&nbsp;=&nbsp;sla_EPCO (K0, K, E)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>K0</EM></TD>
+<TH ALIGN="LEFT"><B>C</B></TH>
+<TD ALIGN="LEFT" NOWRAP>form of result:  `B'=Besselian, `J'=Julian</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>K</EM></TD>
+<TD ALIGN="LEFT"><B>C</B></TD>
+<TD ALIGN="LEFT" NOWRAP>form of given epoch:  `B' or `J'</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>E</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>epoch</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_EPCO</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>the given epoch converted as necessary</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>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.
+  <DT>2.
+<DD>K0 and K are not validated.  They are interpreted as follows:
+        <UL>
+<LI> If K0 and K are the same, the result is E.
+<LI> If K0 is `B' and K isn't, the conversion is J to B.
+<LI> In all other cases, the conversion is B to J.
+        </UL></DL></DL>
+<BR> <HR>
+<A NAME="tex2html1366" HREF="node95.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1364" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1358" HREF="node93.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1367" HREF="node95.html">SLA_EPJ - MJD to Julian Epoch</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1365" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1359" HREF="node93.html">SLA_EPB2D - Besselian Epoch to MJD</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node95.html b/src/slalib/sun67.htx/node95.html
new file mode 100644
index 0000000..aefb9d6
--- /dev/null
+++ b/src/slalib/sun67.htx/node95.html
@@ -0,0 +1,91 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_EPJ - MJD to Julian Epoch</TITLE>
+<META NAME="description" CONTENT="SLA_EPJ - MJD to Julian Epoch">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node96.html">
+<LINK REL="previous" HREF="node94.html">
+<LINK REL="up" HREF="node13.html">
+<LINK REL="next" HREF="node96.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html1376" HREF="node96.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1374" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1368" HREF="node94.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1377" HREF="node96.html">SLA_EPJ2D - Julian Epoch to MJD</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1375" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1369" HREF="node94.html">SLA_EPCO - Convert Epoch to B or J</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000482000000000000000">SLA_EPJ - MJD to Julian Epoch</A>
+<A NAME="xref_SLA_EPJ">&#160;</A><A NAME="SLA_EPJ">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Convert Modified Julian Date to Julian Epoch.
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>D&nbsp;=&nbsp;sla_EPJ (DATE)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>Modified Julian Date (JD-2400000.5)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_EPJ</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>Julian Epoch</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Lieske, J.H., 1979. <I>Astr.Astrophys.</I>, <B>73</B>, 282.
+</DL>
+<BR> <HR>
+<A NAME="tex2html1376" HREF="node96.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1374" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1368" HREF="node94.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1377" HREF="node96.html">SLA_EPJ2D - Julian Epoch to MJD</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1375" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1369" HREF="node94.html">SLA_EPCO - Convert Epoch to B or J</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node96.html b/src/slalib/sun67.htx/node96.html
new file mode 100644
index 0000000..c0f38a9
--- /dev/null
+++ b/src/slalib/sun67.htx/node96.html
@@ -0,0 +1,91 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_EPJ2D - Julian Epoch to MJD</TITLE>
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+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1387" HREF="node97.html">SLA_EQECL - J2000 to Ecliptic</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1385" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1379" HREF="node95.html">SLA_EPJ - MJD to Julian Epoch</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000483000000000000000">SLA_EPJ2D - Julian Epoch to MJD</A>
+<A NAME="xref_SLA_EPJ2D">&#160;</A><A NAME="SLA_EPJ2D">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Convert Julian Epoch to Modified Julian Date.
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>D&nbsp;=&nbsp;sla_EPJ2D (EPJ)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>EPJ</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>Julian Epoch</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_EPJ2D</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>Modified Julian Date (JD-2400000.5)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Lieske, J.H., 1979. <I>Astr.Astrophys.</I>, <B>73</B>, 282.
+</DL>
+<BR> <HR>
+<A NAME="tex2html1386" HREF="node97.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1387" HREF="node97.html">SLA_EQECL - J2000 to Ecliptic</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1385" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1379" HREF="node95.html">SLA_EPJ - MJD to Julian Epoch</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node97.html b/src/slalib/sun67.htx/node97.html
new file mode 100644
index 0000000..a386ad5
--- /dev/null
+++ b/src/slalib/sun67.htx/node97.html
@@ -0,0 +1,98 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_EQECL - J2000 to Ecliptic</TITLE>
+<META NAME="description" CONTENT="SLA_EQECL - J2000 to Ecliptic">
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+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1394" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1388" HREF="node96.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1397" HREF="node98.html">SLA_EQEQX - Equation of the Equinoxes</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1395" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1389" HREF="node96.html">SLA_EPJ2D - Julian Epoch to MJD</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000484000000000000000">&#160;</A><A NAME="xref_SLA_EQECL">&#160;</A><A NAME="SLA_EQECL">&#160;</A>
+<BR>
+SLA_EQECL - J2000 <IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img91.gif"
+ ALT="$\alpha,\delta$"> to Ecliptic
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Transformation from J2000.0 equatorial coordinates to
+ecliptic longitude and latitude.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_EQECL (DR, DD, DATE, DL, DB)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DR,DD</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 mean <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> (radians)</TD>
+</TR>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TD ALIGN="LEFT"><B>D</B></TD>
+<TD ALIGN="LEFT" NOWRAP>TDB (formerly ET) as Modified Julian Date (JD-2400000.5)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DL,DB</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>ecliptic longitude and latitude
+(mean of date, IAU 1980 theory, radians)</TD>
+</TR>
+</TABLE></DL>
+<BR> <HR>
+<A NAME="tex2html1396" HREF="node98.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
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+<A NAME="tex2html1388" HREF="node96.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1397" HREF="node98.html">SLA_EQEQX - Equation of the Equinoxes</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1395" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1389" HREF="node96.html">SLA_EPJ2D - Julian Epoch to MJD</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node98.html b/src/slalib/sun67.htx/node98.html
new file mode 100644
index 0000000..e5a2cc7
--- /dev/null
+++ b/src/slalib/sun67.htx/node98.html
@@ -0,0 +1,111 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_EQEQX - Equation of the Equinoxes</TITLE>
+<META NAME="description" CONTENT="SLA_EQEQX - Equation of the Equinoxes">
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+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1407" HREF="node99.html">SLA_EQGAL - J2000 to Galactic</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1405" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1399" HREF="node97.html">SLA_EQECL - J2000 to Ecliptic</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000485000000000000000">SLA_EQEQX - Equation of the Equinoxes</A>
+<A NAME="xref_SLA_EQEQX">&#160;</A><A NAME="SLA_EQEQX">&#160;</A>
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Equation of the equinoxes (IAU 1994).
+<DT><STRONG>CALL:</STRONG>
+<DD><TT>D&nbsp;=&nbsp;sla_EQEQX (DATE)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DATE</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>TDB (formerly ET) as Modified Julian Date (JD-2400000.5)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>sla_EQEQX</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>The equation of the equinoxes (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTES:</STRONG>
+<DD><DL COMPACT>
+<DT>1.
+<DD>The equation of the equinoxes is defined here as GAST&nbsp;-&nbsp;GMST:
+it is added to a <I>mean</I> sidereal time to give the
+<I>apparent</I> sidereal time.
+  <DT>2.
+<DD>The change from the classic ``textbook'' expression
+        <IMG WIDTH="62" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img108.gif"
+ ALT="$\Delta\psi\,cos\,\epsilon$"> occurred with IAU Resolution C7,
+        Recommendation&nbsp;3 (1994).  The new formulation takes into
+        account cross-terms between the various precession and
+        nutation quantities, amounting to about 3&nbsp;milliarcsec.
+        The transition from the old to the new model officially
+        takes place on 1997 February&nbsp;27.
+ </DL></DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Capitaine, N. &amp; Gontier, A.-M. (1993),
+<I>Astron. Astrophys.</I>,
+      <B>275</B>, 645-650.
+     </DL>
+<BR> <HR>
+<A NAME="tex2html1406" HREF="node99.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1404" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1398" HREF="node97.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1407" HREF="node99.html">SLA_EQGAL - J2000 to Galactic</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1405" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1399" HREF="node97.html">SLA_EQECL - J2000 to Ecliptic</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/node99.html b/src/slalib/sun67.htx/node99.html
new file mode 100644
index 0000000..1e4582a
--- /dev/null
+++ b/src/slalib/sun67.htx/node99.html
@@ -0,0 +1,105 @@
+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLA_EQGAL - J2000 to Galactic</TITLE>
+<META NAME="description" CONTENT="SLA_EQGAL - J2000 to Galactic">
+<META NAME="keywords" CONTENT="sun67">
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+</HEAD>
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+<BR> <HR>
+<A NAME="tex2html1416" HREF="node100.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1414" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1408" HREF="node98.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1417" HREF="node100.html">SLA_ETRMS - E-terms of Aberration</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1415" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1409" HREF="node98.html">SLA_EQEQX - Equation of the Equinoxes</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<H2><A NAME="SECTION000486000000000000000">&#160;</A><A NAME="xref_SLA_EQGAL">&#160;</A><A NAME="SLA_EQGAL">&#160;</A>
+<BR>
+SLA_EQGAL - J2000 <IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img91.gif"
+ ALT="$\alpha,\delta$"> to Galactic
+</H2>
+       <DL>
+<DT><STRONG>ACTION:</STRONG>
+<DD>Transformation from J2000.0 FK5 equatorial coordinates to
+IAU 1958 galactic coordinates.
+<P>    <DT><STRONG>CALL:</STRONG>
+<DD><TT>CALL sla_EQGAL (DR, DD, DL, DB)</TT>
+<P>       </DL>
+<P>     <DL>
+<DT><STRONG>GIVEN:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DR,DD</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>J2000.0 <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>     <DL>
+<DT><STRONG>RETURNED:</STRONG>
+<DD>
+<BR>
+<TABLE CELLPADDING=3>
+<TR VALIGN="TOP"><TD ALIGN="LEFT"><EM>DL,DB</EM></TD>
+<TH ALIGN="LEFT"><B>D</B></TH>
+<TD ALIGN="LEFT" NOWRAP>galactic longitude and latitude <IMG WIDTH="59" HEIGHT="32" ALIGN="MIDDLE" BORDER="0"
+ SRC="img98.gif"
+ ALT="$[\,l^{I\!I},b^{I\!I}\,]$"> (radians)</TD>
+</TR>
+</TABLE></DL>
+<P>      <DL>
+<DT><STRONG>NOTE:</STRONG>
+<DD>The equatorial coordinates are J2000.0 FK5.  Use the routine
+sla_EG50 if conversion from B1950.0 FK4 coordinates is required.
+      </DL>
+<P>     <DL>
+<DT><STRONG>REFERENCE:</STRONG>
+<DD>Blaauw <I>et al.</I>, 1960, <I>Mon.Not.R.astr.Soc.</I>,
+<B>121</B>, 123.
+     </DL>
+<BR> <HR>
+<A NAME="tex2html1416" HREF="node100.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<A NAME="tex2html1414" HREF="node13.html">
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif.gif"></A> 
+<A NAME="tex2html1408" HREF="node98.html">
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif.gif"></A>   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html1417" HREF="node100.html">SLA_ETRMS - E-terms of Aberration</A>
+<BR>
+<B>Up:</B> <A NAME="tex2html1415" HREF="node13.html">SUBPROGRAM SPECIFICATIONS</A>
+<BR>
+<B> Previous:</B> <A NAME="tex2html1409" HREF="node98.html">SLA_EQEQX - Equation of the Equinoxes</A>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/orangeball.gif b/src/slalib/sun67.htx/orangeball.gif
new file mode 100644
index 0000000..e757cd0
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+
+SMALL.TINY		{ font-size : xx-small }
+SMALL.SCRIPTSIZE	{ font-size : xx-small }
+SMALL.FOOTNOTESIZE	{ font-size : x-small  }
+SMALL.SMALL		{ font-size : small    }
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+<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 3.2//EN">
+<!--Converted with LaTeX2HTML 97.1 (release) (July 13th, 1997)
+ by Nikos Drakos (nikos@cbl.leeds.ac.uk), CBLU, University of Leeds
+* revised and updated by:  Marcus Hennecke, Ross Moore, Herb Swan
+* with significant contributions from:
+  Jens Lippman, Marek Rouchal, Martin Wilck and others -->
+<HTML>
+<HEAD>
+<TITLE>SLALIB -- Positional Astronomy Library</TITLE>
+<META NAME="description" CONTENT="SLALIB -- Positional Astronomy Library">
+<META NAME="keywords" CONTENT="sun67">
+<META NAME="resource-type" CONTENT="document">
+<META NAME="distribution" CONTENT="global">
+<META HTTP-EQUIV="Content-Type" CONTENT="text/html; charset=iso_8859_1">
+<LINK REL="STYLESHEET" HREF="sun67.css">
+<LINK REL="next" HREF="node1.html">
+</HEAD>
+<BODY >
+<BR> <HR>
+<A NAME="tex2html7" HREF="node1.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif_gr.gif"> 
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif_gr.gif">   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html8" HREF="node1.html">Abstract</A>
+<BR>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<P><A NAME="xref_">&#160;</A>
+    <H1>
+      SLALIB -- Positional Astronomy Library
+<BR>
+2.4-0
+<BR>
+Programmer's Manual
+    </H1>
+<P>    <P> <I>
+   Starlink User Note67.45
+<BR>
+P.T.Wallace
+<BR>
+12 October 1999
+    </I> </P> <H3>
+      <A NAME="tex2html1" HREF="http://www.cclrc.ac.uk">CCLRC</A>
+/
+      <A NAME="tex2html1" HREF="http://www.cclrc.ac.uk/ral">Rutherford Appleton Laboratory</A>
+<BR>
+      <A NAME="tex2html1" HREF="http://www.pparc.ac.uk">Particle Physics &amp; Astronomy Research Council</A>
+<BR>
+    </H3> <H2>
+      <A NAME="tex2html1" HREF="http://star-www.rl.ac.uk/">Starlink Project</A>
+ </H2>
+   <A NAME="tex2html1" HREF="http://star-www.rl.ac.uk/cgi-bin/hcserver?sun67.45"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="source.gif"> Retrieve hardcopy</A>
+<BR>
+<A NAME="stardoccontents">&#160;</A>      <HR>
+    <H2>Contents</H2>
+<P>  <BR><HR>
+<!--Table of Child-Links-->
+<A NAME="CHILD_LINKS">&#160;</A>
+<UL>
+<LI><A NAME="tex2html9" HREF="node1.html#SECTION00010000000000000000">
+Abstract</A>
+<LI><A NAME="tex2html10" HREF="node2.html#SECTION00020000000000000000">
+INTRODUCTION</A>
+<UL>
+<LI><A NAME="tex2html11" HREF="node3.html#SECTION00021000000000000000">
+Purpose</A>
+<LI><A NAME="tex2html12" HREF="node4.html#SECTION00022000000000000000">
+Example Application</A>
+<LI><A NAME="tex2html13" HREF="node5.html#SECTION00023000000000000000">
+Scope</A>
+<LI><A NAME="tex2html14" HREF="node6.html#SECTION00024000000000000000">
+Objectives</A>
+<LI><A NAME="tex2html15" HREF="node7.html#SECTION00025000000000000000">
+Fortran Version</A>
+<LI><A NAME="tex2html16" HREF="node8.html#SECTION00026000000000000000">
+C Version</A>
+<LI><A NAME="tex2html17" HREF="node9.html#SECTION00027000000000000000">
+Future Versions</A>
+<LI><A NAME="tex2html18" HREF="node10.html#SECTION00028000000000000000">
+New Functions</A>
+<LI><A NAME="tex2html19" HREF="node11.html#SECTION00029000000000000000">
+Acknowledgements</A>
+</UL>
+<LI><A NAME="tex2html20" HREF="node12.html#SECTION00030000000000000000">
+LINKING</A>
+<LI><A NAME="tex2html21" HREF="node13.html#SECTION00040000000000000000">
+SUBPROGRAM SPECIFICATIONS</A>
+<UL>
+<LI><A NAME="tex2html22" HREF="node14.html#SECTION00041000000000000000">
+SLA_ADDET - Add E-terms of Aberration</A>
+<LI><A NAME="tex2html23" HREF="node15.html#SECTION00042000000000000000">
+SLA_AFIN - Sexagesimal character string to angle</A>
+<LI><A NAME="tex2html24" HREF="node16.html#SECTION00043000000000000000">
+SLA_AIRMAS - Air Mass</A>
+<LI><A NAME="tex2html25" HREF="node17.html#SECTION00044000000000000000">
+SLA_ALTAZ - Velocities <I>etc.</I> for Altazimuth Mount</A>
+<LI><A NAME="tex2html26" HREF="node18.html#SECTION00045000000000000000">
+SLA_AMP - Apparent to Mean</A>
+<LI><A NAME="tex2html27" HREF="node19.html#SECTION00046000000000000000">
+SLA_AMPQK - Quick Apparent to Mean</A>
+<LI><A NAME="tex2html28" HREF="node20.html#SECTION00047000000000000000">
+SLA_AOP - Apparent to Observed</A>
+<LI><A NAME="tex2html29" HREF="node21.html#SECTION00048000000000000000">
+SLA_AOPPA - Appt-to-Obs Parameters</A>
+<LI><A NAME="tex2html30" HREF="node22.html#SECTION00049000000000000000">
+SLA_AOPPAT - Update Appt-to-Obs Parameters</A>
+<LI><A NAME="tex2html31" HREF="node23.html#SECTION000410000000000000000">
+SLA_AOPQK - Quick Appt-to-Observed</A>
+<LI><A NAME="tex2html32" HREF="node24.html#SECTION000411000000000000000">
+SLA_ATMDSP - Atmospheric Dispersion</A>
+<LI><A NAME="tex2html33" HREF="node25.html#SECTION000412000000000000000">
+SLA_AV2M - Rotation Matrix from Axial Vector</A>
+<LI><A NAME="tex2html34" HREF="node26.html#SECTION000413000000000000000">
+SLA_BEAR - Direction Between Points on a Sphere</A>
+<LI><A NAME="tex2html35" HREF="node27.html#SECTION000414000000000000000">
+SLA_CAF2R - Deg,Arcmin,Arcsec to Radians</A>
+<LI><A NAME="tex2html36" HREF="node28.html#SECTION000415000000000000000">
+SLA_CALDJ - Calendar Date to MJD</A>
+<LI><A NAME="tex2html37" HREF="node29.html#SECTION000416000000000000000">
+SLA_CALYD - Calendar to Year, Day</A>
+<LI><A NAME="tex2html38" HREF="node30.html#SECTION000417000000000000000">
+SLA_CC2S - Cartesian to Spherical</A>
+<LI><A NAME="tex2html39" HREF="node31.html#SECTION000418000000000000000">
+SLA_CC62S - Cartesian 6-Vector to Spherical</A>
+<LI><A NAME="tex2html40" HREF="node32.html#SECTION000419000000000000000">
+SLA_CD2TF - Days to Hour,Min,Sec</A>
+<LI><A NAME="tex2html41" HREF="node33.html#SECTION000420000000000000000">
+SLA_CLDJ - Calendar to MJD</A>
+<LI><A NAME="tex2html42" HREF="node34.html#SECTION000421000000000000000">
+SLA_CLYD - Calendar to Year, Day</A>
+<LI><A NAME="tex2html43" HREF="node35.html#SECTION000422000000000000000">
+SLA_COMBN - Next Combination</A>
+<LI><A NAME="tex2html44" HREF="node36.html#SECTION000423000000000000000">
+SLA_CR2AF - Radians to Deg,Arcmin,Arcsec</A>
+<LI><A NAME="tex2html45" HREF="node37.html#SECTION000424000000000000000">
+SLA_CR2TF - Radians to Hour,Min,Sec</A>
+<LI><A NAME="tex2html46" HREF="node38.html#SECTION000425000000000000000">
+SLA_CS2C - Spherical to Cartesian</A>
+<LI><A NAME="tex2html47" HREF="node39.html#SECTION000426000000000000000">
+SLA_CS2C6 - Spherical Pos/Vel to Cartesian</A>
+<LI><A NAME="tex2html48" HREF="node40.html#SECTION000427000000000000000">
+SLA_CTF2D - Hour,Min,Sec to Days</A>
+<LI><A NAME="tex2html49" HREF="node41.html#SECTION000428000000000000000">
+SLA_CTF2R - Hour,Min,Sec to Radians</A>
+<LI><A NAME="tex2html50" HREF="node42.html#SECTION000429000000000000000">
+SLA_DAF2R - Deg,Arcmin,Arcsec to Radians</A>
+<LI><A NAME="tex2html51" HREF="node43.html#SECTION000430000000000000000">
+SLA_DAFIN - Sexagesimal character string to angle</A>
+<LI><A NAME="tex2html52" HREF="node44.html#SECTION000431000000000000000">
+SLA_DAT - TAI-UTC</A>
+<LI><A NAME="tex2html53" HREF="node45.html#SECTION000432000000000000000">
+SLA_DAV2M - Rotation Matrix from Axial Vector</A>
+<LI><A NAME="tex2html54" HREF="node46.html#SECTION000433000000000000000">
+SLA_DBEAR - Direction Between Points on a Sphere</A>
+<LI><A NAME="tex2html55" HREF="node47.html#SECTION000434000000000000000">
+SLA_DBJIN - Decode String to B/J Epoch (DP)</A>
+<LI><A NAME="tex2html56" HREF="node48.html#SECTION000435000000000000000">
+SLA_DC62S - Cartesian 6-Vector to Spherical</A>
+<LI><A NAME="tex2html57" HREF="node49.html#SECTION000436000000000000000">
+SLA_DCC2S - Cartesian to Spherical</A>
+<LI><A NAME="tex2html58" HREF="node50.html#SECTION000437000000000000000">
+SLA_DCMPF - Interpret Linear Fit</A>
+<LI><A NAME="tex2html59" HREF="node51.html#SECTION000438000000000000000">
+SLA_DCS2C - Spherical to Cartesian</A>
+<LI><A NAME="tex2html60" HREF="node52.html#SECTION000439000000000000000">
+SLA_DD2TF - Days to Hour,Min,Sec</A>
+<LI><A NAME="tex2html61" HREF="node53.html#SECTION000440000000000000000">
+SLA_DE2H - <IMG WIDTH="27" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img65.gif"
+ ALT="$h,\delta$"> to Az,El</A>
+<LI><A NAME="tex2html62" HREF="node54.html#SECTION000441000000000000000">
+SLA_DEULER - Euler Angles to Rotation Matrix</A>
+<LI><A NAME="tex2html63" HREF="node55.html#SECTION000442000000000000000">
+SLA_DFLTIN - Decode a Double Precision Number</A>
+<LI><A NAME="tex2html64" HREF="node56.html#SECTION000443000000000000000">
+SLA_DH2E - Az,El to <IMG WIDTH="27" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img65.gif"
+ ALT="$h,\delta$"></A>
+<LI><A NAME="tex2html65" HREF="node57.html#SECTION000444000000000000000">
+SLA_DIMXV - Apply 3D Reverse Rotation</A>
+<LI><A NAME="tex2html66" HREF="node58.html#SECTION000445000000000000000">
+SLA_DJCAL - MJD to Gregorian for Output</A>
+<LI><A NAME="tex2html67" HREF="node59.html#SECTION000446000000000000000">
+SLA_DJCL - MJD to Year,Month,Day,Frac</A>
+<LI><A NAME="tex2html68" HREF="node60.html#SECTION000447000000000000000">
+SLA_DM2AV - Rotation Matrix to Axial Vector</A>
+<LI><A NAME="tex2html69" HREF="node61.html#SECTION000448000000000000000">
+SLA_DMAT - Solve Simultaneous Equations</A>
+<LI><A NAME="tex2html70" HREF="node62.html#SECTION000449000000000000000">
+SLA_DMOON - Approx Moon Pos/Vel</A>
+<LI><A NAME="tex2html71" HREF="node63.html#SECTION000450000000000000000">
+SLA_DMXM - Multiply <IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img18.gif"
+ ALT="$3\times3$"> Matrices</A>
+<LI><A NAME="tex2html72" HREF="node64.html#SECTION000451000000000000000">
+SLA_DMXV - Apply 3D Rotation</A>
+<LI><A NAME="tex2html73" HREF="node65.html#SECTION000452000000000000000">
+SLA_DPAV - Position-Angle Between Two Directions</A>
+<LI><A NAME="tex2html74" HREF="node66.html#SECTION000453000000000000000">
+SLA_DR2AF - Radians to Deg,Min,Sec,Frac</A>
+<LI><A NAME="tex2html75" HREF="node67.html#SECTION000454000000000000000">
+SLA_DR2TF - Radians to Hour,Min,Sec,Frac</A>
+<LI><A NAME="tex2html76" HREF="node68.html#SECTION000455000000000000000">
+SLA_DRANGE - Put Angle into Range <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$"></A>
+<LI><A NAME="tex2html77" HREF="node69.html#SECTION000456000000000000000">
+SLA_DRANRM - Put Angle into Range <IMG WIDTH="43" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img66.gif"
+ ALT="$0\!-\!2\pi$"></A>
+<LI><A NAME="tex2html78" HREF="node70.html#SECTION000457000000000000000">
+SLA_DS2C6 - Spherical Pos/Vel to Cartesian</A>
+<LI><A NAME="tex2html79" HREF="node71.html#SECTION000458000000000000000">
+SLA_DS2TP - Spherical to Tangent Plane</A>
+<LI><A NAME="tex2html80" HREF="node72.html#SECTION000459000000000000000">
+SLA_DSEP - Angle Between 2 Points on Sphere</A>
+<LI><A NAME="tex2html81" HREF="node73.html#SECTION000460000000000000000">
+SLA_DT - Approximate ET minus UT</A>
+<LI><A NAME="tex2html82" HREF="node74.html#SECTION000461000000000000000">
+SLA_DTF2D - Hour,Min,Sec to Days</A>
+<LI><A NAME="tex2html83" HREF="node75.html#SECTION000462000000000000000">
+SLA_DTF2R - Hour,Min,Sec to Radians</A>
+<LI><A NAME="tex2html84" HREF="node76.html#SECTION000463000000000000000">
+SLA_DTP2S - Tangent Plane to Spherical</A>
+<LI><A NAME="tex2html85" HREF="node77.html#SECTION000464000000000000000">
+SLA_DTP2V - Tangent Plane to Direction Cosines</A>
+<LI><A NAME="tex2html86" HREF="node78.html#SECTION000465000000000000000">
+SLA_DTPS2C - Plate centre from <IMG WIDTH="26" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img90.gif"
+ ALT="$\xi,\eta$"> and <IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img91.gif"
+ ALT="$\alpha,\delta$"></A>
+<LI><A NAME="tex2html87" HREF="node79.html#SECTION000466000000000000000">
+SLA_DTPV2C - Plate centre from <IMG WIDTH="26" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img90.gif"
+ ALT="$\xi,\eta$"> and <I>x</I>,<I>y</I>,<I>z</I></A>
+<LI><A NAME="tex2html88" HREF="node80.html#SECTION000467000000000000000">
+SLA_DTT - TT minus UTC</A>
+<LI><A NAME="tex2html89" HREF="node81.html#SECTION000468000000000000000">
+SLA_DV2TP - Direction Cosines to Tangent Plane</A>
+<LI><A NAME="tex2html90" HREF="node82.html#SECTION000469000000000000000">
+SLA_DVDV - Scalar Product</A>
+<LI><A NAME="tex2html91" HREF="node83.html#SECTION000470000000000000000">
+SLA_DVN - Normalize Vector</A>
+<LI><A NAME="tex2html92" HREF="node84.html#SECTION000471000000000000000">
+SLA_DVXV - Vector Product</A>
+<LI><A NAME="tex2html93" HREF="node85.html#SECTION000472000000000000000">
+SLA_E2H - <IMG WIDTH="27" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img65.gif"
+ ALT="$h,\delta$"> to Az,El</A>
+<LI><A NAME="tex2html94" HREF="node86.html#SECTION000473000000000000000">
+SLA_EARTH - Approx Earth Pos/Vel</A>
+<LI><A NAME="tex2html95" HREF="node87.html#SECTION000474000000000000000">
+SLA_ECLEQ - Ecliptic to Equatorial</A>
+<LI><A NAME="tex2html96" HREF="node88.html#SECTION000475000000000000000">
+SLA_ECMAT - Form <IMG WIDTH="81" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img95.gif"
+ ALT="$\alpha,\delta\rightarrow\lambda,\beta$"> Matrix</A>
+<LI><A NAME="tex2html97" HREF="node89.html#SECTION000476000000000000000">
+SLA_ECOR - RV &amp; Time Corrns to Sun</A>
+<LI><A NAME="tex2html98" HREF="node90.html#SECTION000477000000000000000">
+SLA_EG50 - B1950 <IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img91.gif"
+ ALT="$\alpha,\delta$"> to Galactic</A>
+<LI><A NAME="tex2html99" HREF="node91.html#SECTION000478000000000000000">
+SLA_EL2UE - Conventional to Universal Elements</A>
+<LI><A NAME="tex2html100" HREF="node92.html#SECTION000479000000000000000">
+SLA_EPB - MJD to Besselian Epoch</A>
+<LI><A NAME="tex2html101" HREF="node93.html#SECTION000480000000000000000">
+SLA_EPB2D - Besselian Epoch to MJD</A>
+<LI><A NAME="tex2html102" HREF="node94.html#SECTION000481000000000000000">
+SLA_EPCO - Convert Epoch to B or J</A>
+<LI><A NAME="tex2html103" HREF="node95.html#SECTION000482000000000000000">
+SLA_EPJ - MJD to Julian Epoch</A>
+<LI><A NAME="tex2html104" HREF="node96.html#SECTION000483000000000000000">
+SLA_EPJ2D - Julian Epoch to MJD</A>
+<LI><A NAME="tex2html105" HREF="node97.html#SECTION000484000000000000000">
+SLA_EQECL - J2000 <IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img91.gif"
+ ALT="$\alpha,\delta$"> to Ecliptic</A>
+<LI><A NAME="tex2html106" HREF="node98.html#SECTION000485000000000000000">
+SLA_EQEQX - Equation of the Equinoxes</A>
+<LI><A NAME="tex2html107" HREF="node99.html#SECTION000486000000000000000">
+SLA_EQGAL - J2000 <IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img91.gif"
+ ALT="$\alpha,\delta$"> to Galactic</A>
+<LI><A NAME="tex2html108" HREF="node100.html#SECTION000487000000000000000">
+SLA_ETRMS - E-terms of Aberration</A>
+<LI><A NAME="tex2html109" HREF="node101.html#SECTION000488000000000000000">
+SLA_EULER - Rotation Matrix from Euler Angles</A>
+<LI><A NAME="tex2html110" HREF="node102.html#SECTION000489000000000000000">
+SLA_EVP - Earth Position &amp; Velocity</A>
+<LI><A NAME="tex2html111" HREF="node103.html#SECTION000490000000000000000">
+SLA_FITXY - Fit Linear Model to Two <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"> Sets</A>
+<LI><A NAME="tex2html112" HREF="node104.html#SECTION000491000000000000000">
+SLA_FK425 - FK4 to FK5</A>
+<LI><A NAME="tex2html113" HREF="node105.html#SECTION000492000000000000000">
+SLA_FK45Z - FK4 to FK5, no P.M. or Parallax</A>
+<LI><A NAME="tex2html114" HREF="node106.html#SECTION000493000000000000000">
+SLA_FK524 - FK5 to FK4</A>
+<LI><A NAME="tex2html115" HREF="node107.html#SECTION000494000000000000000">
+SLA_FK52H - FK5 to Hipparcos</A>
+<LI><A NAME="tex2html116" HREF="node108.html#SECTION000495000000000000000">
+SLA_FK54Z - FK5 to FK4, no P.M. or Parallax</A>
+<LI><A NAME="tex2html117" HREF="node109.html#SECTION000496000000000000000">
+SLA_FK5HZ - FK5 to Hipparcos, no P.M.</A>
+<LI><A NAME="tex2html118" HREF="node110.html#SECTION000497000000000000000">
+SLA_FLOTIN - Decode a Real Number</A>
+<LI><A NAME="tex2html119" HREF="node111.html#SECTION000498000000000000000">
+SLA_GALEQ - Galactic to J2000 <IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img91.gif"
+ ALT="$\alpha,\delta$"></A>
+<LI><A NAME="tex2html120" HREF="node112.html#SECTION000499000000000000000">
+SLA_GALSUP - Galactic to Supergalactic</A>
+<LI><A NAME="tex2html121" HREF="node113.html#SECTION0004100000000000000000">
+SLA_GE50 - Galactic to B1950 <IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img91.gif"
+ ALT="$\alpha,\delta$"></A>
+<LI><A NAME="tex2html122" HREF="node114.html#SECTION0004101000000000000000">
+SLA_GEOC - Geodetic to Geocentric</A>
+<LI><A NAME="tex2html123" HREF="node115.html#SECTION0004102000000000000000">
+SLA_GMST - UT to GMST</A>
+<LI><A NAME="tex2html124" HREF="node116.html#SECTION0004103000000000000000">
+SLA_GMSTA - UT to GMST (extra precision)</A>
+<LI><A NAME="tex2html125" HREF="node117.html#SECTION0004104000000000000000">
+SLA_GRESID - Gaussian Residual</A>
+<LI><A NAME="tex2html126" HREF="node118.html#SECTION0004105000000000000000">
+SLA_H2E - Az,El to <IMG WIDTH="27" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img65.gif"
+ ALT="$h,\delta$"></A>
+<LI><A NAME="tex2html127" HREF="node119.html#SECTION0004106000000000000000">
+SLA_H2FK5 - Hipparcos to FK5</A>
+<LI><A NAME="tex2html128" HREF="node120.html#SECTION0004107000000000000000">
+SLA_HFK5Z - Hipparcos to FK5, no P.M.</A>
+<LI><A NAME="tex2html129" HREF="node121.html#SECTION0004108000000000000000">
+SLA_IMXV - Apply 3D Reverse Rotation</A>
+<LI><A NAME="tex2html130" HREF="node122.html#SECTION0004109000000000000000">
+SLA_INTIN - Decode an Integer Number</A>
+<LI><A NAME="tex2html131" HREF="node123.html#SECTION0004110000000000000000">
+SLA_INVF - Invert Linear Model</A>
+<LI><A NAME="tex2html132" HREF="node124.html#SECTION0004111000000000000000">
+SLA_KBJ - Select Epoch Prefix</A>
+<LI><A NAME="tex2html133" HREF="node125.html#SECTION0004112000000000000000">
+SLA_M2AV - Rotation Matrix to Axial Vector</A>
+<LI><A NAME="tex2html134" HREF="node126.html#SECTION0004113000000000000000">
+SLA_MAP - Mean to Apparent</A>
+<LI><A NAME="tex2html135" HREF="node127.html#SECTION0004114000000000000000">
+SLA_MAPPA - Mean to Apparent Parameters</A>
+<LI><A NAME="tex2html136" HREF="node128.html#SECTION0004115000000000000000">
+SLA_MAPQK - Quick Mean to Apparent</A>
+<LI><A NAME="tex2html137" HREF="node129.html#SECTION0004116000000000000000">
+SLA_MAPQKZ - Quick Mean-Appt, no PM <I>etc.</I></A>
+<LI><A NAME="tex2html138" HREF="node130.html#SECTION0004117000000000000000">
+SLA_MOON - Approx Moon Pos/Vel</A>
+<LI><A NAME="tex2html139" HREF="node131.html#SECTION0004118000000000000000">
+SLA_MXM - Multiply <IMG WIDTH="39" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img18.gif"
+ ALT="$3\times3$"> Matrices</A>
+<LI><A NAME="tex2html140" HREF="node132.html#SECTION0004119000000000000000">
+SLA_MXV - Apply 3D Rotation</A>
+<LI><A NAME="tex2html141" HREF="node133.html#SECTION0004120000000000000000">
+SLA_NUT - Nutation Matrix</A>
+<LI><A NAME="tex2html142" HREF="node134.html#SECTION0004121000000000000000">
+SLA_NUTC - Nutation Components</A>
+<LI><A NAME="tex2html143" HREF="node135.html#SECTION0004122000000000000000">
+SLA_OAP - Observed to Apparent</A>
+<LI><A NAME="tex2html144" HREF="node136.html#SECTION0004123000000000000000">
+SLA_OAPQK - Quick Observed to Apparent</A>
+<LI><A NAME="tex2html145" HREF="node137.html#SECTION0004124000000000000000">
+SLA_OBS - Observatory Parameters</A>
+<LI><A NAME="tex2html146" HREF="node138.html#SECTION0004125000000000000000">
+SLA_PA - <IMG WIDTH="27" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img65.gif"
+ ALT="$h,\delta$"> to Parallactic Angle</A>
+<LI><A NAME="tex2html147" HREF="node139.html#SECTION0004126000000000000000">
+SLA_PAV - Position-Angle Between Two Directions</A>
+<LI><A NAME="tex2html148" HREF="node140.html#SECTION0004127000000000000000">
+SLA_PCD - Apply Radial Distortion</A>
+<LI><A NAME="tex2html149" HREF="node141.html#SECTION0004128000000000000000">
+SLA_PDA2H - H.A. for a Given Azimuth</A>
+<LI><A NAME="tex2html150" HREF="node142.html#SECTION0004129000000000000000">
+SLA_PDQ2H - H.A. for a Given P.A.</A>
+<LI><A NAME="tex2html151" HREF="node143.html#SECTION0004130000000000000000">
+SLA_PERMUT - Next Permutation</A>
+<LI><A NAME="tex2html152" HREF="node144.html#SECTION0004131000000000000000">
+SLA_PERTEL - Perturbed Orbital Elements</A>
+<LI><A NAME="tex2html153" HREF="node145.html#SECTION0004132000000000000000">
+SLA_PERTUE - Perturbed Universal Elements</A>
+<LI><A NAME="tex2html154" HREF="node146.html#SECTION0004133000000000000000">
+SLA_PLANEL - Planet Position from Elements</A>
+<LI><A NAME="tex2html155" HREF="node147.html#SECTION0004134000000000000000">
+SLA_PLANET - Planetary Ephemerides</A>
+<LI><A NAME="tex2html156" HREF="node148.html#SECTION0004135000000000000000">
+SLA_PLANTE - <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> of Planet from Elements</A>
+<LI><A NAME="tex2html157" HREF="node149.html#SECTION0004136000000000000000">
+SLA_PM - Proper Motion</A>
+<LI><A NAME="tex2html158" HREF="node150.html#SECTION0004137000000000000000">
+SLA_POLMO - Polar Motion</A>
+<LI><A NAME="tex2html159" HREF="node151.html#SECTION0004138000000000000000">
+SLA_PREBN - Precession Matrix (FK4)</A>
+<LI><A NAME="tex2html160" HREF="node152.html#SECTION0004139000000000000000">
+SLA_PREC - Precession Matrix (FK5)</A>
+<LI><A NAME="tex2html161" HREF="node153.html#SECTION0004140000000000000000">
+SLA_PRECES - Precession</A>
+<LI><A NAME="tex2html162" HREF="node154.html#SECTION0004141000000000000000">
+SLA_PRECL - Precession Matrix (latest)</A>
+<LI><A NAME="tex2html163" HREF="node155.html#SECTION0004142000000000000000">
+SLA_PRENUT - Precession/Nutation Matrix</A>
+<LI><A NAME="tex2html164" HREF="node156.html#SECTION0004143000000000000000">
+SLA_PV2EL - Orbital Elements from Position/Velocity</A>
+<LI><A NAME="tex2html165" HREF="node157.html#SECTION0004144000000000000000">
+SLA_PV2UE - Position/Velocity to Universal Elements</A>
+<LI><A NAME="tex2html166" HREF="node158.html#SECTION0004145000000000000000">
+SLA_PVOBS - Observatory Position &amp; Velocity</A>
+<LI><A NAME="tex2html167" HREF="node159.html#SECTION0004146000000000000000">
+SLA_PXY - Apply Linear Model</A>
+<LI><A NAME="tex2html168" HREF="node160.html#SECTION0004147000000000000000">
+SLA_RANDOM - Random Number</A>
+<LI><A NAME="tex2html169" HREF="node161.html#SECTION0004148000000000000000">
+SLA_RANGE - Put Angle into Range <IMG WIDTH="25" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img47.gif"
+ ALT="$\pm \pi$"></A>
+<LI><A NAME="tex2html170" HREF="node162.html#SECTION0004149000000000000000">
+SLA_RANORM - Put Angle into Range <IMG WIDTH="43" HEIGHT="25" ALIGN="MIDDLE" BORDER="0"
+ SRC="img66.gif"
+ ALT="$0\!-\!2\pi$"></A>
+<LI><A NAME="tex2html171" HREF="node163.html#SECTION0004150000000000000000">
+SLA_RCC - Barycentric Coordinate Time</A>
+<LI><A NAME="tex2html172" HREF="node164.html#SECTION0004151000000000000000">
+SLA_RDPLAN - Apparent <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img3.gif"
+ ALT="$[\,\alpha,\delta\,]$"> of Planet</A>
+<LI><A NAME="tex2html173" HREF="node165.html#SECTION0004152000000000000000">
+SLA_REFCO - Refraction Constants</A>
+<LI><A NAME="tex2html174" HREF="node166.html#SECTION0004153000000000000000">
+SLA_REFCOQ - Refraction Constants (fast)</A>
+<LI><A NAME="tex2html175" HREF="node167.html#SECTION0004154000000000000000">
+SLA_REFRO - Refraction</A>
+<LI><A NAME="tex2html176" HREF="node168.html#SECTION0004155000000000000000">
+SLA_REFV - Apply Refraction to Vector</A>
+<LI><A NAME="tex2html177" HREF="node169.html#SECTION0004156000000000000000">
+SLA_REFZ - Apply Refraction to ZD</A>
+<LI><A NAME="tex2html178" HREF="node170.html#SECTION0004157000000000000000">
+SLA_RVEROT - RV Corrn to Earth Centre</A>
+<LI><A NAME="tex2html179" HREF="node171.html#SECTION0004158000000000000000">
+SLA_RVGALC - RV Corrn to Galactic Centre</A>
+<LI><A NAME="tex2html180" HREF="node172.html#SECTION0004159000000000000000">
+SLA_RVLG - RV Corrn to Local Group</A>
+<LI><A NAME="tex2html181" HREF="node173.html#SECTION0004160000000000000000">
+SLA_RVLSRD - RV Corrn to Dynamical LSR</A>
+<LI><A NAME="tex2html182" HREF="node174.html#SECTION0004161000000000000000">
+SLA_RVLSRK - RV Corrn to Kinematical LSR</A>
+<LI><A NAME="tex2html183" HREF="node175.html#SECTION0004162000000000000000">
+SLA_S2TP - Spherical to Tangent Plane</A>
+<LI><A NAME="tex2html184" HREF="node176.html#SECTION0004163000000000000000">
+SLA_SEP - Angle Between 2 Points on Sphere</A>
+<LI><A NAME="tex2html185" HREF="node177.html#SECTION0004164000000000000000">
+SLA_SMAT - Solve Simultaneous Equations</A>
+<LI><A NAME="tex2html186" HREF="node178.html#SECTION0004165000000000000000">
+SLA_SUBET - Remove E-terms</A>
+<LI><A NAME="tex2html187" HREF="node179.html#SECTION0004166000000000000000">
+SLA_SUPGAL - Supergalactic to Galactic</A>
+<LI><A NAME="tex2html188" HREF="node180.html#SECTION0004167000000000000000">
+SLA_SVD - Singular Value Decomposition</A>
+<LI><A NAME="tex2html189" HREF="node181.html#SECTION0004168000000000000000">
+SLA_SVDCOV - Covariance Matrix from SVD</A>
+<LI><A NAME="tex2html190" HREF="node182.html#SECTION0004169000000000000000">
+SLA_SVDSOL - Solution Vector from SVD</A>
+<LI><A NAME="tex2html191" HREF="node183.html#SECTION0004170000000000000000">
+SLA_TP2S - Tangent Plane to Spherical</A>
+<LI><A NAME="tex2html192" HREF="node184.html#SECTION0004171000000000000000">
+SLA_TP2V - Tangent Plane to Direction Cosines</A>
+<LI><A NAME="tex2html193" HREF="node185.html#SECTION0004172000000000000000">
+SLA_TPS2C - Plate centre from <IMG WIDTH="26" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img90.gif"
+ ALT="$\xi,\eta$"> and <IMG WIDTH="28" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img91.gif"
+ ALT="$\alpha,\delta$"></A>
+<LI><A NAME="tex2html194" HREF="node186.html#SECTION0004173000000000000000">
+SLA_TPV2C - Plate centre from <IMG WIDTH="26" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img90.gif"
+ ALT="$\xi,\eta$"> and <I>x</I>,<I>y</I>,<I>z</I></A>
+<LI><A NAME="tex2html195" HREF="node187.html#SECTION0004174000000000000000">
+SLA_UE2EL - Universal to Conventional Elements</A>
+<LI><A NAME="tex2html196" HREF="node188.html#SECTION0004175000000000000000">
+SLA_UE2PV - Pos/Vel from Universal Elements</A>
+<LI><A NAME="tex2html197" HREF="node189.html#SECTION0004176000000000000000">
+SLA_UNPCD - Remove Radial Distortion</A>
+<LI><A NAME="tex2html198" HREF="node190.html#SECTION0004177000000000000000">
+SLA_V2TP - Direction Cosines to Tangent Plane</A>
+<LI><A NAME="tex2html199" HREF="node191.html#SECTION0004178000000000000000">
+SLA_VDV - Scalar Product</A>
+<LI><A NAME="tex2html200" HREF="node192.html#SECTION0004179000000000000000">
+SLA_VN - Normalize Vector</A>
+<LI><A NAME="tex2html201" HREF="node193.html#SECTION0004180000000000000000">
+SLA_VXV - Vector Product</A>
+<LI><A NAME="tex2html202" HREF="node194.html#SECTION0004181000000000000000">
+SLA_WAIT - Time Delay</A>
+<LI><A NAME="tex2html203" HREF="node195.html#SECTION0004182000000000000000">
+SLA_XY2XY - Apply Linear Model to an <IMG WIDTH="42" HEIGHT="29" ALIGN="MIDDLE" BORDER="0"
+ SRC="img20.gif"
+ ALT="$[\,x,y\,]$"></A>
+<LI><A NAME="tex2html204" HREF="node196.html#SECTION0004183000000000000000">
+SLA_ZD - <IMG WIDTH="27" HEIGHT="27" ALIGN="MIDDLE" BORDER="0"
+ SRC="img65.gif"
+ ALT="$h,\delta$"> to Zenith Distance</A>
+</UL>
+<LI><A NAME="tex2html205" HREF="node197.html#SECTION00050000000000000000">
+EXPLANATION AND EXAMPLES</A>
+<UL>
+<LI><A NAME="tex2html206" HREF="node198.html#SECTION00051000000000000000">
+Spherical Trigonometry</A>
+<UL>
+<LI><A NAME="tex2html207" HREF="node199.html#SECTION00051100000000000000">
+Formatting angles</A>
+</UL>
+<LI><A NAME="tex2html208" HREF="node200.html#SECTION00052000000000000000">
+Vectors and Matrices</A>
+<UL>
+<LI><A NAME="tex2html209" HREF="node201.html#SECTION00052100000000000000">
+Using vectors</A>
+</UL>
+<LI><A NAME="tex2html210" HREF="node202.html#SECTION00053000000000000000">
+Celestial Coordinate Systems</A>
+<LI><A NAME="tex2html211" HREF="node203.html#SECTION00054000000000000000">
+Precession and Nutation</A>
+<UL>
+<LI><A NAME="tex2html212" HREF="node204.html#SECTION00054100000000000000">
+SLALIB support for precession and nutation</A>
+</UL>
+<LI><A NAME="tex2html213" HREF="node205.html#SECTION00055000000000000000">
+Mean Places</A>
+<LI><A NAME="tex2html214" HREF="node206.html#SECTION00056000000000000000">
+Epoch</A>
+<LI><A NAME="tex2html215" HREF="node207.html#SECTION00057000000000000000">
+Proper Motion</A>
+<LI><A NAME="tex2html216" HREF="node208.html#SECTION00058000000000000000">
+Parallax and Radial Velocity</A>
+<LI><A NAME="tex2html217" HREF="node209.html#SECTION00059000000000000000">
+Aberration</A>
+<LI><A NAME="tex2html218" HREF="node210.html#SECTION000510000000000000000">
+Different Sorts of Mean Place</A>
+<LI><A NAME="tex2html219" HREF="node211.html#SECTION000511000000000000000">
+Mean Place Transformations</A>
+<LI><A NAME="tex2html220" HREF="node212.html#SECTION000512000000000000000">
+Mean Place to Apparent Place</A>
+<LI><A NAME="tex2html221" HREF="node213.html#SECTION000513000000000000000">
+Apparent Place to Observed Place</A>
+<UL>
+<LI><A NAME="tex2html222" HREF="node214.html#SECTION000513100000000000000">
+Refraction</A>
+<LI><A NAME="tex2html223" HREF="node215.html#SECTION000513200000000000000">
+Efficiency considerations</A>
+</UL>
+<LI><A NAME="tex2html224" HREF="node216.html#SECTION000514000000000000000">
+The Hipparcos Catalogue and the ICRS</A>
+<LI><A NAME="tex2html225" HREF="node217.html#SECTION000515000000000000000">
+Timescales</A>
+<UL>
+<LI><A NAME="tex2html226" HREF="node218.html#SECTION000515100000000000000">
+Atomic Time: TAI</A>
+<LI><A NAME="tex2html227" HREF="node219.html#SECTION000515200000000000000">
+Universal Time: UTC, UT1</A>
+<LI><A NAME="tex2html228" HREF="node220.html#SECTION000515300000000000000">
+Sidereal Time: GMST, LAST</A>
+<LI><A NAME="tex2html229" HREF="node221.html#SECTION000515400000000000000">
+Dynamical Time: TT, TDB</A>
+</UL>
+<LI><A NAME="tex2html230" HREF="node222.html#SECTION000516000000000000000">
+Calendars</A>
+<LI><A NAME="tex2html231" HREF="node223.html#SECTION000517000000000000000">
+Geocentric Coordinates</A>
+<LI><A NAME="tex2html232" HREF="node224.html#SECTION000518000000000000000">
+Ephemerides</A>
+<LI><A NAME="tex2html233" HREF="node225.html#SECTION000519000000000000000">
+Radial Velocity and Light-Time Corrections</A>
+<LI><A NAME="tex2html234" HREF="node226.html#SECTION000520000000000000000">
+Focal-Plane Astrometry</A>
+<LI><A NAME="tex2html235" HREF="node227.html#SECTION000521000000000000000">
+Numerical Methods</A>
+</UL>
+<LI><A NAME="tex2html236" HREF="node228.html#SECTION00060000000000000000">
+SUMMARY OF CALLS</A>
+<LI><A NAME="tex2html237" HREF="node229.html#SECTION00070000000000000000">
+About this document ... </A>
+</UL>
+<!--End of Table of Child-Links-->
+<BR> <HR>
+<A NAME="tex2html7" HREF="node1.html">
+<IMG WIDTH="37" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="next" SRC="next_motif.gif"></A> 
+<IMG WIDTH="26" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="up" SRC="up_motif_gr.gif"> 
+<IMG WIDTH="63" HEIGHT="24" ALIGN="BOTTOM" BORDER="0" ALT="previous" SRC="previous_motif_gr.gif">   <A HREF="sun67.html#stardoccontents"><IMG  ALIGN="BOTTOM" BORDER="0"
+ SRC="contents_motif.gif"></A>
+<BR>
+<B> Next:</B> <A NAME="tex2html8" HREF="node1.html">Abstract</A>
+<BR>
+<BR> <HR> <P>
+<P><!--End of Navigation Panel-->
+<ADDRESS>
+<I>SLALIB --- Positional Astronomy Library<BR>Starlink User Note 67<BR>P. T. Wallace<BR>12 October 1999<BR>E-mail:ptw@star.rl.ac.uk</I>
+</ADDRESS>
+</BODY>
+</HTML>
diff --git a/src/slalib/sun67.htx/up_motif.gif b/src/slalib/sun67.htx/up_motif.gif
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diff --git a/src/slalib/sun67.htx/yellowball.gif b/src/slalib/sun67.htx/yellowball.gif
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diff --git a/src/slalib/sun67.htx_tar b/src/slalib/sun67.htx_tar
new file mode 100644
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diff --git a/src/slalib/sun67.tex b/src/slalib/sun67.tex
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--- /dev/null
+++ b/src/slalib/sun67.tex
@@ -0,0 +1,12430 @@
+\documentclass[11pt,twoside]{article}
+\setcounter{tocdepth}{2}
+\pagestyle{myheadings}
+
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+% ? Document identification
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+\newcommand{\stardocsource}    {sun67.45}
+\newcommand{\stardocnumber}    {67.45}
+\newcommand{\stardocauthors}   {P.\,T.\,Wallace}
+\newcommand{\stardocdate}      {12 October 1999}
+\newcommand{\stardoctitle}     {SLALIB --- Positional Astronomy Library}
+\newcommand{\stardocversion}   {2.4-0}
+\newcommand{\stardocmanual}    {Programmer's Manual}
+% ? End of document identification
+
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+
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+
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+%\setlength{\topmargin}{-10mm}       %
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+
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+%  These are used by the LaTeX2HTML translator in conjunction with star2html.
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+%  Comment.sty: version 2.0, 19 June 1992
+%  Selectively in/exclude pieces of text.
+%
+%  Author
+%    Victor Eijkhout                                      <eijkhout@cs.utk.edu>
+%    Department of Computer Science
+%    University Tennessee at Knoxville
+%    104 Ayres Hall
+%    Knoxville, TN 37996
+%    USA
+
+%  Do not remove the %\begin{rawtex} and %\end{rawtex} lines (used by
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+      \fi \fi \html@next}
+}
+\makeatother
+
+\def\includecomment
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+
+%  Define environments that ignore their contents.
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+%\end{rawtex}
+
+%  Hypertext commands etc. This is a condensed version of the html.sty
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+
+%  Latex document header.
+%  ======================
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+   CCLRC / {\sc Rutherford Appleton Laboratory} \hfill {\bf \stardocname}\\
+   {\large Particle Physics \& Astronomy Research Council}\\
+   {\large Starlink Project\\}
+   {\large \stardoccategory\ \stardocnumber}
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+      {\Large\bf Abstract}
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+%  ==========================
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+      \htmladdnormallink{CCLRC}{http://www.cclrc.ac.uk} /
+      \htmladdnormallink{Rutherford Appleton Laboratory}
+                        {http://www.cclrc.ac.uk/ral} \\
+      \htmladdnormallink{Particle Physics \& Astronomy Research Council}
+                        {http://www.pparc.ac.uk} \\
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+\end{htmlonly}
+
+% -----------------------------------------------------------------------------
+% ? Document Abstract. (if used)
+%   ==================
+SLALIB is a library used by writers of positional-astronomy applications.
+Most of the \nroutines\ routines are concerned with astronomical position and time,
+but a number have wider trigonometrical, numerical or general applications.
+% ? End of document abstract
+% -----------------------------------------------------------------------------
+% ? Latex document Table of Contents (if used).
+%  ===========================================
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+\newpage
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+
+\section{INTRODUCTION}
+\subsection{Purpose}
+SLALIB\footnote{The name isn't an acronym;
+it just stands for ``Subprogram Library~A''.}
+is a library of routines
+intended to make accurate and reliable positional-astronomy
+applications easier to write.
+Most SLALIB routines are concerned with astronomical position and time, but a
+number have wider trigonometrical, numerical or general applications.
+The applications ASTROM, COCO, RV and TPOINT
+all make extensive use of the SLALIB
+routines, as do a number of telescope control systems around the world.
+The SLALIB versions currently in service are written in
+Fortran~77 and run on VAX/VMS, several Unix platforms and PC.
+A generic ANSI~C version is also available from the author;  it is
+functionally similar to the Fortran version upon which the present
+document concentrates.
+
+\subsection{Example Application}
+Here is a simple example of an application program written
+using SLALIB calls:
+
+\begin{verbatim}
+         PROGRAM FK4FK5
+   *
+   *  Read a B1950 position from I/O unit 5 and reply on I/O unit 6
+   *  with the J2000 equivalent.  Enter a period to quit.
+   *
+         IMPLICIT NONE
+         CHARACTER C*80,S
+         INTEGER I,J,IHMSF(4),IDMSF(4)
+         DOUBLE PRECISION R4,D4,R5,D5
+         LOGICAL BAD
+
+   *   Loop until a period is entered
+         C = ' '
+         DO WHILE (C(:1).NE.'.')
+
+   *     Read h m s d ' "
+            READ (5,'(A)') C
+            IF (C(:1).NE.'.') THEN
+               BAD = .TRUE.
+
+   *        Decode the RA
+               I = 1
+               CALL sla_DAFIN(C,I,R4,J)
+               IF (J.EQ.0) THEN
+                  R4 = 15D0*R4
+
+   *           Decode the Dec
+                  CALL sla_DAFIN(C,I,D4,J)
+                  IF (J.EQ.0) THEN
+
+   *              FK4 to FK5
+                     CALL sla_FK45Z(R4,D4,1950D0,R5,D5)
+
+   *              Format and output the result
+                     CALL sla_DR2TF(2,R5,S,IHMSF)
+                     CALL sla_DR2AF(1,D5,S,IDMSF)
+                     WRITE (6,
+        :       '(1X,I2.2,2I3.2,''.'',I2.2,2X,A,I2.2,2I3.2,''.'',I1)')
+        :                                                     IHMSF,S,IDMSF
+                     BAD = .FALSE.
+                  END IF
+               END IF
+               IF (BAD) WRITE (6,'(1X,''?'')')
+            END IF
+         END DO
+
+         END
+\end{verbatim}
+In this example, SLALIB not only provides the complicated FK4 to
+FK5 transformation but also
+simplifies the tedious and error-prone tasks
+of decoding and formatting angles
+expressed as hours, minutes {\it etc}.  The
+example incorporates range checking, and avoids the
+notorious ``minus zero'' problem (an often-perpetrated bug where
+declinations between $0^{\circ}$ and $-1^{\circ}$ lose their minus
+sign).
+With a little extra elaboration and a few more calls to SLALIB,
+defaulting can be provided (enabling unused fields to
+be replaced with commas to avoid retyping), proper motions
+can be handled, different epochs can be specified, and
+so on.  See the program COCO (SUN/56) for further ideas.
+
+\subsection{Scope}
+SLALIB contains \nroutines\ routines covering the following topics:
+\begin{itemize}
+\item String Decoding,
+      Sexagesimal Conversions
+\item Angles, Vectors \& Rotation Matrices
+\item Calendars,
+      Timescales
+\item Precession \& Nutation
+\item Proper Motion
+\item FK4/FK5/Hipparcos,
+      Elliptic Aberration
+\item Geocentric Coordinates
+\item Apparent \& Observed Place
+\item Azimuth \& Elevation
+\item Refraction \& Air Mass
+\item Ecliptic,
+      Galactic,
+      Supergalactic Coordinates
+\item Ephemerides
+\item Astrometry
+\item Numerical Methods
+\end{itemize}
+
+\subsection{Objectives}
+SLALIB was designed to give application programmers
+a basic set of positional-astronomy tools which were
+accurate and easy to use.  To this end, the library is:
+\begin{itemize}
+\item Readily available, including source code and documentation.
+\item Supported and maintained.
+\item Portable -- coded in standard languages and available for
+multiple computers and operating systems.
+\item Thoroughly commented, both for maintainability and to
+assist those wishing to cannibalize the code.
+\item Stable.
+\item Trustworthy -- some care has gone into
+testing SLALIB, both by comparison with published data and
+by checks for internal consistency.
+\item Rigorous -- corners are not cut,
+even where the practical consequences would, as a rule, be
+negligible.
+\item Comprehensive, without including too many esoteric features
+required only by specialists.
+\item Practical -- almost all the routines have been written to
+satisfy real needs encountered during the development of
+real-life applications.
+\item Environment-independent -- the package is
+completely free of pauses, stops, I/O {\it etc}.
+\item Self-contained -- SLALIB calls no other libraries.
+\end{itemize}
+A few {\it caveats}:
+\begin{itemize}
+\item SLALIB does not pretend to be canonical.  It is in essence
+an anthology, and the adopted algorithms are liable
+to change as more up-to-date ones become available.
+\item The functions aren't orthogonal -- there are several
+cases of different
+routines doing similar things, and many examples where
+sequences of SLALIB calls have simply been packaged, all to
+make applications less trouble to write.
+\item There are omissions -- for example there are no
+routines for calculating physical ephemerides of
+Solar-System bodies.
+\item SLALIB is not homogeneous, though important subsets
+(for example the FK4/FK5 routines) are.
+\item The library is not foolproof.  You have to know what
+you are trying to do ({\it e.g.}\ by reading textbooks on positional
+astronomy), and it is the caller's responsibility to supply
+sensible arguments (although enough internal validation is done to
+avoid arithmetic errors).
+\item Without being written in a wasteful
+manner, SLALIB is nonetheless optimized for maintainability
+rather than speed.  In addition, there are many places
+where considerable simplification would be possible if some
+specified amount of accuracy could be sacrificed;  such
+compromises are left to the individual programmer and
+are not allowed to limit SLALIB's value as a source
+of comparison results.
+\end{itemize}
+
+\subsection{Fortran Version}
+The Fortran versions of SLALIB use ANSI Fortran~77 with a few
+commonplace extensions.  Just three out of the \nroutines\ routines require
+platform-specific techniques and accordingly are supplied
+in different forms.
+SLALIB has been implemented on the following platforms:
+VAX/VMS,
+PC (Microsoft Fortran, Linux),
+DECstation (Ultrix),
+DEC Alpha (DEC Unix),
+Sun (SunOS, Solaris),
+Hewlett Packard (HP-UX),
+CONVEX,
+Perkin-Elmer and
+Fujitsu.
+
+\subsection{C Version}
+An ANSI C version of SLALIB is available from the author
+but is not part of the Starlink release.
+The functionality of this (proprietary) C version closely matches
+that of the Starlink Fortran SLALIB, partly for the convenience of
+existing users of the Fortran version, some of whom have in the past
+implemented C ``wrappers''.  The function names
+cannot be the same as the Fortran versions because of potential
+linking problems when
+both forms of the library are present; the C routine which
+is the equivalent of (for example) {\tt SLA\_REFRO} is {\tt slaRefro}.
+The types of arguments follow the Fortran version, except
+that integers are {\tt int} rather than {\tt long}.
+Argument passing is by value
+(except for arrays and strings of course)
+for given arguments and by pointer for returned arguments.
+All the C functions are re-entrant.
+
+The Fortran routines {\tt sla\_GRESID}, {\tt sla\_RANDOM} and
+{\tt sla\_WAIT} have no C counterparts.
+
+Further details of the C version of SLALIB are available
+from the author.  The definitive guide to
+the calling sequences is the file {\tt slalib.h}.
+
+\subsection{Future Versions}
+The homogeneity and ease of use of SLALIB could perhaps be improved
+in the future
+by turning to C++ and object-oriented techniques.  For example ``celestial
+position'' could be a class and many of the transformations
+could happen automatically.  This requires further study and
+would almost certainly result in a complete redesign.
+Similarly,
+the impact of Fortran~90 has yet to be assessed.  Once compilers
+become widely available, some internal recoding may be worthwhile
+in order to simplify parts of the code.  However, as with C++,
+a redesign of the
+application interfaces will be needed if the capabilities of the
+new language are to be exploited to the full.
+
+\subsection{New Functions}
+In a package like SLALIB it is difficult to know how far to go.  Is it
+enough to provide the primitive operations, or should more
+complicated functions be packaged?  Is it worth encroaching on
+specialist areas, where individual experts have all written their
+own software already?  To what extent should CPU efficiency be
+an issue?  How much support of different numerical precisions is
+required?  And so on.
+
+In practice, almost all the routines in SLALIB are there because they were
+needed for some specific application, and this is likely to remain the
+pattern for any enhancements in the future.
+Suggestions for additional SLALIB routines should be addressed to the
+author.
+
+\subsection{Acknowledgements}
+SLALIB is descended from a package of routines written
+for the AAO 16-bit minicomputers
+in the mid-1970s.  The coming of the VAX
+allowed a much more comprehensive and thorough package
+to be designed for Starlink, especially important
+at a time when the adoption
+of the IAU 1976 resolutions meant that astronomers
+would have to cope with a mixture of reference frames,
+timescales and nomenclature.
+
+Much of the preparatory work on SLALIB was done by
+Althea~Wilkinson of Manchester University.
+During its development,
+Andrew~Murray,
+Catherine~Hohenkerk,
+Andrew~Sinclair,
+Bernard~Yallop
+and
+Brian~Emerson of Her Majesty's Nautical Almanac Office were consulted
+on many occasions; their advice was indispensable.
+I am especially grateful to
+Catherine~Hohenkerk
+for supplying preprints of papers, and test data. A number of
+enhancements to SLALIB were at the suggestion of
+Russell~Owen, University of Washington,
+the late Phil~Hill, St~Andrews University,
+Bill~Vacca, JILA, Boulder and
+Ron~Maddalena, NRAO.
+Mark~Calabretta, CSIRO Radiophysics, Sydney supplied changes to suit Convex.
+I am indebted to Derek~Jones (RGO) for introducing me to the
+``universal variables'' method of calculating orbits.
+
+The first C version of SLALIB was a hand-coded transcription
+of the Starlink Fortran version carried out by
+Steve~Eaton (University of Leeds) in the course of
+MSc work.  This was later
+enhanced by John~Straede (AAO) and Martin~Shepherd (Caltech).
+The current C SLALIB is a complete rewrite by the present author and
+includes a comprehensive validation suite.
+Additional comments on the C version came from Bob~Payne (NRAO) and
+Jeremy~Bailey (AAO).
+
+\section{LINKING}
+
+On Unix systems (Sun, DEC Alpha {\it etc.}):
+\begin{verse}
+{\tt \%~~f77 progname.o -L/star/lib `sla\_link` -o progname}
+\end{verse}
+(The above assumes that all Starlink directories have been added to
+the {\tt LD\_LIBRARY\_PATH} and {\tt PATH} environment variables
+as described in SUN/202.)
+
+On VAX/VMS:
+\begin{verse}
+{\tt \$~~LINK progname,SLALIB\_DIR:SLALIB/LIB}
+\end{verse}
+
+\pagebreak
+
+\section{SUBPROGRAM SPECIFICATIONS}
+%-----------------------------------------------------------------------
+\routine{SLA\_ADDET}{Add E-terms of Aberration}
+{
+ \action{Add the E-terms (elliptic component of annual aberration) to a
+  pre IAU 1976 mean place to conform to the old catalogue convention.}
+ \call{CALL sla\_ADDET (RM, DM, EQ, RC, DC)}
+}
+\args{GIVEN}
+{
+ \spec{RM,DM}{D}{\radec\ without E-terms (radians)} \\
+ \spec{EQ}{D}{Besselian epoch of mean equator and equinox}
+}
+\args{RETURNED}
+{
+ \spec{RC,DC}{D}{\radec\ with E-terms included (radians)}
+}
+\anote{Most star positions from pre-1984 optical catalogues (or
+       obtained by astrometry with respect to such stars) have the
+       E-terms built-in.  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 
+       \radec\ should be adjusted using this routine.}
+\aref{{\it Explanatory Supplement to the Astronomical Ephemeris},
+ section 2D, page 48.}
+%-----------------------------------------------------------------------
+\routine{SLA\_AFIN}{Sexagesimal character string to angle}
+{
+ \action{Decode a free-format sexagesimal string (degrees, arcminutes,
+         arcseconds) into a single precision floating point
+         number (radians).}
+ \call{CALL sla\_AFIN (STRING, NSTRT, RESLT, JF)}
+}
+\args{GIVEN}
+{
+ \spec{STRING}{C*(*)}{string containing deg, arcmin, arcsec fields} \\
+ \spec{NSTRT}{I}{pointer to start of decode (beginning of STRING = 1)}
+}
+\args{RETURNED}
+{
+ \spec{NSTRT}{I}{advanced past the decoded angle} \\
+ \spec{RESLT}{R}{angle in radians} \\
+ \spec{JF}{I}{status:} \\
+ \spec{}{}{\hspace{1.5em}   0 = OK} \\
+ \spec{}{}{\hspace{0.7em} $+1$ = default, RESLT unchanged (note 2)} \\
+ \spec{}{}{\hspace{0.7em} $-1$ = bad degrees (note 3)} \\
+ \spec{}{}{\hspace{0.7em} $-2$ = bad arcminutes (note 3)} \\
+ \spec{}{}{\hspace{0.7em} $-3$ = bad arcseconds (note 3)} \\
+}
+\goodbreak
+\setlength{\oldspacing}{\topsep}
+\setlength{\topsep}{0.3ex}
+\begin{description}
+ \exampleitem \\ [1.5ex]
+  \begin{tabular}{p{7em}p{15em}p{12em}}
+   {\it argument} & {\it before} & {\it after} \\ \\
+   STRING & $'$\verb*}-57 17 44.806  12 34 56.7}$'$ & unchanged \\
+   NSTRT & 1 & 16 ({\it i.e.}\ pointing to 12...) \\
+   RESLT & - & $-1.00000$ \\
+   JF & - & 0
+  \end{tabular}
+ \item A further call to sla\_AFIN, without adjustment of NSTRT, will
+       decode the second angle, \dms{12}{34}{56}{7}.
+\end{description}
+\setlength{\topsep}{\oldspacing}
+\notes
+{
+ \begin{enumerate}
+  \item 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 sla\_DFLTIN routine and is free-format.
+  \item 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 RESLT is
+   unchanged.  In all other cases RESLT is changed.
+  \item Range checking:
+   \begin{itemize}
+    \item The degrees field is not range checked.  However, it is
+     expected to be integral unless the other two fields are absent.
+    \item 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...
+    \item The arcseconds field is expected to be 0-59.9999...
+    \item Decoding continues even when a check has failed.  Under these
+     circumstances the field takes the supplied value, defaulting to
+     zero, and the result RESLT is computed and returned.
+   \end{itemize}
+   \item Further fields after the three expected ones are not treated as
+    an error.  The pointer NSTRT is left in the correct state for
+    further decoding with the present routine or with sla\_DFLTIN
+    {\it etc}.  See the example, above.
+   \item If STRING contains hours, minutes, seconds instead of
+    degrees {\it etc},
+    or if the required units are turns (or days) instead of radians,
+    the result RESLT should be multiplied as follows: \\ [1.5ex]
+    \begin{tabular}{p{6em}p{5em}p{15em}}
+    {\it for STRING} & {\it to obtain} & {\it multiply RESLT by} \\ \\
+    ${\circ}$~~\raisebox{-0.7ex}{$'$}~~\raisebox{-0.7ex}{$''$}
+     & radians & $1.0$ \\
+    ${\circ}$~~\raisebox{-0.7ex}{$'$}~~\raisebox{-0.7ex}{$''$}
+     & turns & $1/{2 \pi} = 0.1591549430918953358$ \\
+    h m s & radians & $15.0$ \\
+    h m s & days & $15/{2\pi} = 2.3873241463784300365$ \\
+   \end{tabular}
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_AIRMAS}{Air Mass}
+{
+ \action{Air mass at given zenith distance (double precision).}
+ \call{D~=~sla\_AIRMAS (ZD)}
+}
+\args{GIVEN}
+{
+ \spec{ZD}{D}{observed zenith distance (radians)}
+}
+\args{RETURNED}
+{
+ \spec{sla\_AIRMAS}{D}{air mass (1 at zenith)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The {\it observed}\/ zenith distance referred to above means
+        ``as affected by refraction''.
+  \item The routine 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.
+  \item The sign of the ZD is ignored.
+  \item At zenith distances greater than about $\zeta = 87^{\circ}$ the
+        air mass is held constant to avoid arithmetic overflows.
+ \end{enumerate}
+}
+\refs
+{
+ \begin{enumerate}
+  \item Hardie, R.H., 1962, in {\it Astronomical Techniques}\,
+        ed. W.A.\ Hiltner, University of Chicago Press, p180.
+  \item Schoenberg, E., 1929, Hdb.\ d.\ Ap.,
+        Berlin, Julius Springer, 2, 268.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_ALTAZ}{Velocities {\it etc.}\ for Altazimuth Mount}
+{
+ \action{Positions, velocities and accelerations for an altazimuth
+         telescope mount tracking a star (double precision).}
+ \call{CALL sla\_ALTAZ (\vtop{
+         \hbox{HA, DEC, PHI,}
+         \hbox{AZ, AZD, AZDD, EL, ELD, ELDD, PA, PAD, PADD)}}}
+}
+\args{GIVEN}
+{
+ \spec{HA}{D}{hour angle} \\
+ \spec{DEC}{D}{declination} \\
+ \spec{PHI}{D}{observatory latitude}
+}
+\args{RETURNED}
+{
+ \spec{AZ}{D}{azimuth} \\
+ \spec{AZD}{D}{azimuth velocity} \\
+ \spec{AZDD}{D}{azimuth acceleration} \\
+ \spec{EL}{D}{elevation} \\
+ \spec{ELD}{D}{elevation velocity} \\
+ \spec{ELDD}{D}{elevation acceleration} \\
+ \spec{PA}{D}{parallactic angle} \\
+ \spec{PAD}{D}{parallactic angle velocity} \\
+ \spec{PADD}{D}{parallactic angle acceleration}
+}
+\notes
+{
+ \begin{enumerate}
+  \setlength{\parskip}{\medskipamount}
+  \item 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:
+
+        \begin{center}
+        \begin{tabular}{rlcl}
+                  angles & $\times 360/2\pi$ & $\rightarrow$ & degrees \\
+              velocities & $\times (2\pi/86400) \times (360/2\pi)$
+                                             & $\rightarrow$ & degree/sec \\
+           accelerations & $\times (2\pi/86400)^2 \times (360/2\pi)$
+                                             & $\rightarrow$ & degree/sec/sec \\
+        \end{tabular}
+        \end{center}
+
+        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.
+  \item Azimuth is returned in the range $[\,0,2\pi\,]$;  north is zero,
+        and east is $+\pi/2$.  Elevation and parallactic angle are
+        returned in the range $\pm\pi/2$.  Position angle is +ve
+        for a star west of the meridian and is the angle NP--star--zenith.
+  \item 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.
+  \item No range checking of arguments is carried out.
+  \item 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.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_AMP}{Apparent to Mean}
+{
+ \action{Convert star \radec\ from geocentric apparent to
+         mean place (post IAU 1976).}
+ \call{CALL sla\_AMP (RA, DA, DATE, EQ, RM, DM)}
+}
+\args{GIVEN}
+{
+ \spec{RA,DA}{D}{apparent \radec\ (radians)} \\
+ \spec{DATE}{D}{TDB for apparent place (JD$-$2400000.5)} \\
+ \spec{EQ}{D}{equinox:  Julian epoch of mean place}
+}
+\args{RETURNED}
+{
+ \spec{RM,DM}{D}{mean \radec\ (radians)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The distinction between the required TDB and TT is
+        always negligible.  Moreover, for all but the most
+        critical applications UTC is adequate.
+  \item The accuracy is limited by the routine sla\_EVP, called
+        by sla\_MAPPA, which computes the Earth position and
+        velocity using the methods of Stumpff.  The maximum
+        error is about 0.3~milliarcsecond.
+  \item Iterative techniques are used for the aberration and
+        light deflection corrections so that the routines
+        sla\_AMP (or sla\_AMPQK) and sla\_MAP (or sla\_MAPQK) are
+        accurate inverses;  even at the edge of the Sun's disc
+        the discrepancy is only about 1~nanoarcsecond.
+  \item Where multiple apparent places are to be converted to
+        mean places, for a fixed date and equinox, it is more
+        efficient to use the sla\_MAPPA routine to compute the
+        required parameters once, followed by one call to
+        sla\_AMPQK per star.
+ \end{enumerate}
+}
+\refs
+{
+ \begin{enumerate}
+  \item 1984 {\it Astronomical Almanac}, pp B39-B41.
+  \item Lederle \& Schwan, 1984.\ {\it Astr.Astrophys.}\ {\bf 134}, 1-6.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_AMPQK}{Quick Apparent to Mean}
+{
+ \action{Convert star \radec\ from geocentric apparent to mean place
+         (post IAU 1976).  Use of this routine 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 sla\_MAPPA routine.}
+ \call{CALL sla\_AMPQK (RA, DA, AMPRMS, RM, DM)}
+}
+\args{GIVEN}
+{
+ \spec{RA,DA}{D}{apparent \radec\ (radians)} \\
+ \spec{AMPRMS}{D(21)}{star-independent mean-to-apparent parameters:} \\
+ \specel   {(1)}     {time interval for proper motion (Julian years)} \\
+ \specel   {(2-4)}   {barycentric position of the Earth (AU)} \\
+ \specel   {(5-7)}   {heliocentric direction of the Earth (unit vector)} \\
+ \specel   {(8)}     {(gravitational radius of
+                      Sun)$\times 2 / $(Sun-Earth distance)} \\
+ \specel   {(9-11)}  {{\bf v}: barycentric Earth velocity in units of c} \\
+ \specel   {(12)}    {$\sqrt{1-\left|\mbox{\bf v}\right|^2}$} \\
+ \specel   {(13-21)} {precession/nutation $3\times3$ matrix}
+}
+\args{RETURNED}
+{
+ \spec{RM,DM}{D}{mean \radec\ (radians)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The accuracy is limited by the routine sla\_EVP, called
+        by sla\_MAPPA, which computes the Earth position and
+        velocity using the methods of Stumpff.  The maximum
+        error is about 0.3~milliarcsecond.
+  \item Iterative techniques are used for the aberration and
+        light deflection corrections so that the routines
+        sla\_AMP (or sla\_AMPQK) and sla\_MAP (or sla\_MAPQK) are
+        accurate inverses;  even at the edge of the Sun's disc
+        the discrepancy is only about 1~nanoarcsecond.
+ \end{enumerate}
+}
+\refs
+{
+ \begin{enumerate}
+  \item 1984 {\it Astronomical Almanac}, pp B39-B41.
+  \item Lederle \& Schwan, 1984.\ {\it Astr.Astrophys.}\ {\bf 134}, 1-6.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_AOP}{Apparent to Observed}
+{
+ \action{Apparent to observed place, for optical sources distant from
+         the solar system.}
+ \call{CALL sla\_AOP (\vtop{
+         \hbox{RAP, DAP, DATE, DUT, ELONGM, PHIM, HM, XP, YP,}
+         \hbox{TDK, PMB, RH, WL, TLR, AOB, ZOB, HOB, DOB, ROB)}}}
+}
+\args{GIVEN}
+{
+ \spec{RAP,DAP}{D}{geocentric apparent \radec\ (radians)} \\
+ \spec{DATE}{D}{UTC date/time (Modified Julian Date, JD$-$2400000.5)} \\
+ \spec{DUT}{D}{$\Delta$UT:  UT1$-$UTC (UTC seconds)} \\
+ \spec{ELONGM}{D}{observer's mean longitude (radians, east +ve)} \\
+ \spec{PHIM}{D}{observer's mean geodetic latitude (radians)} \\
+ \spec{HM}{D}{observer's height above sea level (metres)} \\
+ \spec{XP,YP}{D}{polar motion \xy\ coordinates (radians)} \\
+ \spec{TDK}{D}{local ambient temperature (degrees K; std=273.155D0)} \\
+ \spec{PMB}{D}{local atmospheric pressure (mB; std=1013.25D0)} \\
+ \spec{RH}{D}{local relative humidity (in the range 0D0\,--\,1D0)} \\
+ \spec{WL}{D}{effective wavelength ($\mu{\rm m}$, {\it e.g.}\ 0.55D0)} \\
+ \spec{TLR}{D}{tropospheric lapse rate (degrees K per metre,
+                                              {\it e.g.}\ 0.0065D0)}
+}
+\args{RETURNED}
+{
+ \spec{AOB}{D}{observed azimuth (radians: N=0, E=$90^{\circ}$)} \\
+ \spec{ZOB}{D}{observed zenith distance (radians)} \\
+ \spec{HOB}{D}{observed Hour Angle (radians)} \\
+ \spec{DOB}{D}{observed $\delta$ (radians)} \\
+ \spec{ROB}{D}{observed $\alpha$ (radians)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item This routine returns zenith distance rather than elevation
+        in order to reflect the fact that no allowance is made for
+        depression of the horizon.
+  \item 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 azimuth and elevation should be within about
+        \arcsec{0}{1} for $\zeta<70^{\circ}$.  Even
+        at a topocentric zenith distance of
+        $90^{\circ}$, the accuracy in elevation should be better than
+        1~arcminute;  useful results are available for a further
+        $3^{\circ}$, beyond which the sla\_REFRO routine returns a
+        fixed value of the refraction.  The complementary
+        routines sla\_AOP (or sla\_AOPQK) and sla\_OAP (or sla\_OAPQK)
+        are self-consistent to better than 1~microarcsecond all over
+        the celestial sphere.
+  \item 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.
+  \item {\it Apparent}\/ \radec\ 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 ({\it i.e.}\ J2000), these effects can
+        be applied by means of the sla\_MAP {\it etc.}\ routines.  Starting from
+        other mean place systems, additional transformations will be
+        needed;  for example, FK4 ({\it i.e.}\ B1950) mean places would first
+        have to be converted to FK5, which can be done with the
+        sla\_FK425 {\it etc.}\ routines.
+  \item {\it Observed}\/ \azel\ means the position that would be seen by a
+        perfect theodolite located at the observer.  This is obtained
+        from the geocentric apparent \radec\ by allowing for Earth
+        orientation and diurnal aberration, rotating from equator
+        to horizon coordinates, and then adjusting for refraction.
+        The \hadec\ 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 ({\it n.b.}\ not to the
+        refracted pole).  Finally, the $\alpha$ is obtained by subtracting
+        the {\it h}\/ from the local apparent ST.
+  \item 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.
+  \item 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 sla\_AOPPA once followed by one call per star to sla\_AOPQK.
+        Where a range of times within a limited period of a few hours
+        is involved, and the highest precision is not required, call
+        sla\_AOPPA once, followed by a call to sla\_AOPPAT each time the
+        time changes, followed by one call per star to sla\_AOPQK.
+  \item 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 $\Delta$UT changes by one second to its post-leap new value.
+  \item 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 $\pm$\tsec{0}{9}.
+  \item IMPORTANT -- TAKE CARE WITH THE LONGITUDE SIGN CONVENTION.  The
+        longitude required by the present routine is {\bf 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 (as in the {\it Astronomical
+        Almanac}\/ before 1984) and must be reversed in sign before use
+        in the present routine.
+  \item The polar coordinates XP,YP can be obtained from IERS
+        circulars and equivalent publications.  The
+        maximum amplitude is about \arcsec{0}{3}.  If XP,YP values
+        are unavailable, use XP=YP=0D0.  See page B60 of the 1988
+        {\it Astronomical Almanac}\/ for a definition of the two angles.
+  \item The height above sea level of the observing station, HM,
+        can be obtained from the {\it Astronomical Almanac}\/ (Section J
+        in the 1988 edition), or via the routine sla\_OBS.  If P,
+        the pressure in mB, is available, an adequate
+        estimate of HM can be obtained from the following expression:
+        \begin{quote}
+         {\tt HM=-29.3D0*TSL*LOG(P/1013.25D0)}
+        \end{quote}
+        where TSL is the approximate sea-level air temperature in degrees K
+        (see {\it Astrophysical Quantities}, C.W.Allen, 3rd~edition,
+        \S 52).  Similarly, if the pressure P is not known,
+        it can be estimated from the height of the observing
+        station, HM as follows:
+        \begin{quote}
+         {\tt P=1013.25D0*EXP(-HM/(29.3D0*TSL))}
+        \end{quote}
+        Note, however, that the refraction is proportional to the
+        pressure and that an accurate P value is important for
+        precise work.
+  \item The azimuths {\it etc.}\ used by the present routine are with
+        respect to the celestial pole.  Corrections to the terrestrial pole
+        can be computed using sla\_POLMO.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_AOPPA}{Appt-to-Obs Parameters}
+{
+ \action{Pre-compute the set of apparent to observed place parameters
+         required by the ``quick'' routines sla\_AOPQK and sla\_OAPQK.}
+ \call{CALL sla\_AOPPA (\vtop{
+          \hbox{DATE, DUT, ELONGM, PHIM, HM, XP, YP,}
+          \hbox{TDK, PMB, RH, WL, TLR, AOPRMS)}}}
+}
+\args{GIVEN}
+{
+ \spec{DATE}{D}{UTC date/time (Modified Julian Date, JD$-$2400000.5)} \\
+ \spec{DUT}{D}{$\Delta$UT:  UT1$-$UTC (UTC seconds)} \\
+ \spec{ELONGM}{D}{observer's mean longitude (radians, east +ve)} \\
+ \spec{PHIM}{D}{observer's mean geodetic latitude (radians)} \\
+ \spec{HM}{D}{observer's height above sea level (metres)} \\
+ \spec{XP,YP}{D}{polar motion \xy\ coordinates (radians)} \\
+ \spec{TDK}{D}{local ambient temperature (degrees K; std=273.155D0)} \\
+ \spec{PMB}{D}{local atmospheric pressure (mB; std=1013.25D0)} \\
+ \spec{RH}{D}{local relative humidity (in the range 0D0\,--\,1D0)} \\
+ \spec{WL}{D}{effective wavelength ($\mu{\rm m}$, {\it e.g.}\ 0.55D0)} \\
+ \spec{TLR}{D}{tropospheric lapse rate (degrees K per metre,
+                                              {\it e.g.}\ 0.0065D0)}
+}
+\args{RETURNED}
+{
+ \spec{AOPRMS}{D(14)}{star-independent apparent-to-observed parameters:} \\
+ \specel   {(1)}     {geodetic latitude (radians)} \\
+ \specel   {(2,3)}   {sine and cosine of geodetic latitude} \\
+ \specel   {(4)}     {magnitude of diurnal aberration vector} \\
+ \specel   {(5)}     {height (HM)} \\
+ \specel   {(6)}     {ambient temperature (TDK)} \\
+ \specel   {(7)}     {pressure (PMB)} \\
+ \specel   {(8)}     {relative humidity (RH)} \\
+ \specel   {(9)}     {wavelength (WL)} \\
+ \specel   {(10)}    {lapse rate (TLR)} \\
+ \specel   {(11,12)} {refraction constants A and B (radians)} \\
+ \specel   {(13)}    {longitude + eqn of equinoxes +
+                       ``sidereal $\Delta$UT'' (radians)} \\
+ \specel   {(14)}    {local apparent sidereal time (radians)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item 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.
+  \item 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 $\Delta$UT changes by one second to its post-leap new value.
+  \item 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 $\pm$\tsec{0}{9}.  The ``sidereal $\Delta$UT'' which forms
+        part of AOPRMS(13) is the same quantity, but converted from solar
+        to sidereal seconds and expressed in radians.
+  \item IMPORTANT -- TAKE CARE WITH THE LONGITUDE SIGN CONVENTION.  The
+        longitude required by the present routine is {\bf 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 (as in the {\it Astronomical
+        Almanac}\/ before 1984) and must be reversed in sign before use in
+        the present routine.
+  \item The polar coordinates XP,YP can be obtained from IERS
+        circulars and equivalent publications.  The
+        maximum amplitude is about \arcsec{0}{3}.  If XP,YP values
+        are unavailable, use XP=YP=0D0.  See page B60 of the 1988
+        {\it Astronomical Almanac}\/ for a definition of the two angles.
+  \item The height above sea level of the observing station, HM,
+        can be obtained from the {\it Astronomical Almanac}\/ (Section J
+        in the 1988 edition), or via the routine sla\_OBS.  If P,
+        the pressure in mB, is available, an adequate
+        estimate of HM can be obtained from the following expression:
+        \begin{quote}
+         {\tt HM=-29.3D0*TSL*LOG(P/1013.25D0)}
+        \end{quote}
+        where TSL is the approximate sea-level air temperature in degrees K
+        (see {\it Astrophysical Quantities}, C.W.Allen, 3rd~edition,
+        \S 52).  Similarly, if the pressure P is not known,
+        it can be estimated from the height of the observing
+        station, HM as follows:
+        \begin{quote}
+         {\tt P=1013.25D0*EXP(-HM/(29.3D0*TSL))}
+        \end{quote}
+        Note, however, that the refraction is proportional to the
+        pressure and that an accurate P value is important for
+        precise work.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_AOPPAT}{Update Appt-to-Obs Parameters}
+{
+ \action{Recompute the sidereal time in the apparent to observed place
+         star-independent parameter block.}
+ \call{CALL sla\_AOPPAT (DATE, AOPRMS)}
+}
+\args{GIVEN}
+{
+ \spec{DATE}{D}{UTC date/time (Modified Julian Date, JD$-$2400000.5)} \\
+ \spec{AOPRMS}{D(14)}{star-independent apparent-to-observed parameters:} \\
+ \specel{(1-12)}{not required} \\
+ \specel{(13)}{longitude + eqn of equinoxes +
+               ``sidereal $\Delta$UT'' (radians)} \\
+ \specel{(14)}{not required}
+}
+\args{RETURNED}
+{
+ \spec{AOPRMS}{D(14)}{star-independent apparent-to-observed parameters:} \\
+ \specel{(1-13)}{not changed} \\
+ \specel{(14)}{local apparent sidereal time (radians)}
+}
+\anote{For more information, see sla\_AOPPA.}
+%-----------------------------------------------------------------------
+\routine{SLA\_AOPQK}{Quick Appt-to-Observed}
+{
+ \action{Quick apparent to observed place (but see Note~8, below).}
+ \call{CALL sla\_AOPQK (RAP, DAP, AOPRMS, AOB, ZOB, HOB, DOB, ROB)}
+}
+\args{GIVEN}
+{
+ \spec{RAP,DAP}{D}{geocentric apparent \radec\ (radians)} \\
+ \spec{AOPRMS}{D(14)}{star-independent apparent-to-observed parameters:} \\
+ \specel{(1)}{geodetic latitude (radians)} \\
+ \specel{(2,3)}{sine and cosine of geodetic latitude} \\
+ \specel{(4)}{magnitude of diurnal aberration vector} \\
+ \specel{(5)}{height (metres)} \\
+ \specel{(6)}{ambient temperature (degrees K)} \\
+ \specel{(7)}{pressure (mB)} \\
+ \specel{(8)}{relative humidity (0\,--\,1)} \\
+ \specel{(9)}{wavelength ($\mu{\rm m}$)} \\
+ \specel{(10)}{lapse rate (degrees K per metre)} \\
+ \specel{(11,12)}{refraction constants A and B (radians)} \\
+ \specel{(13)}{longitude + eqn of equinoxes +
+               ``sidereal $\Delta$UT'' (radians)} \\
+ \specel{(14)}{local apparent sidereal time (radians)}
+}
+\args{RETURNED}
+{
+ \spec{AOB}{D}{observed azimuth (radians: N=0, E=$90^{\circ}$)} \\
+ \spec{ZOB}{D}{observed zenith distance (radians)} \\
+ \spec{HOB}{D}{observed Hour Angle (radians)} \\
+ \spec{DOB}{D}{observed Declination (radians)} \\
+ \spec{ROB}{D}{observed Right Ascension (radians)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item This routine returns zenith distance rather than elevation
+        in order to reflect the fact that no allowance is made for
+        depression of the horizon.
+  \item 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 azimuth and elevation should be within about
+        \arcsec{0}{1} for $\zeta<70^{\circ}$.  Even
+        at a topocentric zenith distance of
+        $90^{\circ}$, the accuracy in elevation should be better than
+        1~arcminute;  useful results are available for a further
+        $3^{\circ}$, beyond which the sla\_REFRO routine returns a
+        fixed value of the refraction.  The complementary
+        routines sla\_AOP (or sla\_AOPQK) and sla\_OAP (or sla\_OAPQK)
+        are self-consistent to better than 1~microarcsecond all over
+        the celestial sphere.
+  \item 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.
+  \item {\it Apparent}\/ \radec\ 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 ({\it i.e.}\ J2000), these effects can
+        be applied by means of the sla\_MAP {\it etc.}\ routines.  Starting from
+        other mean place systems, additional transformations will be
+        needed;  for example, FK4 ({\it i.e.}\ B1950) mean places would first
+        have to be converted to FK5, which can be done with the
+        sla\_FK425 {\it etc.}\ routines.
+  \item {\it Observed}\/ \azel\ means the position that would be seen by a
+        perfect theodolite located at the observer.  This is obtained
+        from the geocentric apparent \radec\ by allowing for Earth
+        orientation and diurnal aberration, rotating from equator
+        to horizon coordinates, and then adjusting for refraction.
+        The \hadec\ 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 ({\it n.b.}\ not to the
+        refracted pole).  Finally, the $\alpha$ is obtained by subtracting
+        the {\it h}\/ from the local apparent ST.
+  \item 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.
+  \item The star-independent apparent-to-observed-place parameters
+        in AOPRMS may be computed by means of the sla\_AOPPA routine.
+        If nothing has changed significantly except the time, the
+        sla\_AOPPAT routine may be used to perform the requisite
+        partial recomputation of AOPRMS.
+  \item The  ``sidereal $\Delta$UT'' which forms part of AOPRMS(13)
+        is UT1$-$UTC converted from solar to
+        sidereal seconds and expressed in radians.
+  \item At zenith distances beyond about $76^\circ$, 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.
+  \item The azimuths {\it etc.}\ used by the present routine are with
+        respect to the celestial pole.  Corrections to the terrestrial pole
+        can be computed using sla\_POLMO.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_ATMDSP}{Atmospheric Dispersion}
+{
+ \action{Apply atmospheric-dispersion adjustments to refraction coefficients.}
+ \call{CALL sla\_ATMDSP (TDK, PMB, RH, WL1, A1, B1, WL2, A2, B2)}
+}
+\args{GIVEN}
+{
+ \spec{TDK}{D}{ambient temperature at the observer (degrees K)} \\
+ \spec{PMB}{D}{pressure at the observer (mB)} \\
+ \spec{RH}{D}{relative humidity at the observer (range 0\,--\,1)} \\
+ \spec{WL1}{D}{base wavelength ($\mu{\rm m}$)} \\
+ \spec{A1}{D}{refraction coefficient A for wavelength WL1 (radians)} \\
+ \spec{B1}{D}{refraction coefficient B for wavelength WL1 (radians)} \\
+ \spec{WL2}{D}{wavelength for which adjusted A,B required ($\mu{\rm m}$)}
+}
+\args{RETURNED}
+{
+ \spec{A2}{D}{refraction coefficient A for wavelength WL2 (radians)} \\
+ \spec{B2}{D}{refraction coefficient B for wavelength WL2 (radians)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item To use this routine, first call sla\_REFCO specifying WL1 as the
+        wavelength.  This yields refraction coefficients A1, B1, correct
+        for that wavelength.  Subsequently, calls to sla\_ATMDSP specifying
+        different wavelengths will produce new, slightly adjusted
+        refraction coefficients A2, B2, which apply to the specified wavelength.
+  \item Most of the atmospheric dispersion happens between $0.7\,\mu{\rm m}$
+        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 $0.4\,\mu{\rm m}$.
+  \item The accuracy, for this set of conditions: \\[1pc]
+   \hspace*{5ex} \begin{tabular}{rcl}
+        height above sea level & ~ & 2000\,m \\
+                      latitude & ~ & $29^\circ$ \\
+                      pressure & ~ & 793\,mB \\
+                   temperature & ~ & $290^\circ$\,K \\
+                      humidity & ~ & 0.5 (50\%) \\
+                    lapse rate & ~ & $0.0065^\circ m^{-1}$ \\
+          reference wavelength & ~ & $0.4\,\mu{\rm m}$ \\
+                star elevation & ~ & $15^\circ$ \\
+                  \end{tabular}\\[1pc]
+        is about 2.5\,mas RMS between 0.3 and $1.0\,\mu{\rm m}$, and stays
+        within 4\,mas for the whole range longward of $0.3\,\mu{\rm m}$
+        (compared with a total dispersion from 0.3 to $20\,\mu{\rm m}$
+        of about \arcseci{11}).  These errors are typical for ordinary
+        conditions;  in extreme conditions values a few times this size
+        may occur.
+  \item If either wavelength exceeds $100\,\mu{\rm m}$, the radio case
+        is assumed and the returned refraction coefficients are the
+        same as the given ones.
+  \item The algorithm consists of calculation of the refractivity of the
+        air at the observer for the two wavelengths, using the methods
+        of the sla\_REFRO routine, and then scaling of the two refraction
+        coefficients according to classical refraction theory.  This
+        amounts to scaling the A coefficient in proportion to $(\mu-1)$ and
+        the B coefficient almost in the same ratio (see R.M.Green,
+        {\it Spherical Astronomy,}\/ Cambridge University Press, 1985).
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_AV2M}{Rotation Matrix from Axial Vector}
+{
+ \action{Form the rotation matrix corresponding to a given axial vector
+         (single precision).}
+ \call{CALL sla\_AV2M (AXVEC, RMAT)}
+}
+\args{GIVEN}
+{
+ \spec{AXVEC}{R(3)}{axial vector (radians)}
+}
+\args{RETURNED}
+{
+ \spec{RMAT}{R(3,3)}{rotation matrix}
+}
+\notes
+{
+ \begin{enumerate}
+  \item A rotation matrix describes a rotation about some arbitrary axis.
+        The axis is called the {\it Euler axis}, and the angle through which the
+        reference frame rotates is called the Euler angle.  The axial
+        vector supplied to this routine has the same direction as the
+        Euler axis, and its magnitude is the Euler angle in radians.
+  \item If AXVEC is null, the unit matrix is returned.
+  \item The reference frame rotates clockwise as seen looking along
+        the axial vector from the origin.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_BEAR}{Direction Between Points on a Sphere}
+{
+ \action{Returns the bearing (position angle) of one point on a
+         sphere seen from another (single precision).}
+ \call{R~=~sla\_BEAR (A1, B1, A2, B2)}
+}
+\args{GIVEN}
+{
+ \spec{A1,B1}{R}{spherical coordinates of one point} \\
+ \spec{A2,B2}{R}{spherical coordinates of the other point}
+}
+\args{RETURNED}
+{
+ \spec{sla\_BEAR}{R}{bearing from first point to second}
+}
+\notes
+{
+ \begin{enumerate}
+ \item The spherical coordinates are \radec,
+       $[\lambda,\phi]$ {\it etc.}, in radians.
+ \item The result is the bearing (position angle), in radians,
+       of point [A2,B2] as seen
+       from point [A1,B1].  It is in the range $\pm \pi$.  The sense
+       is such that if [A2,B2]
+       is a small distance due east of [A1,B1] the result
+       is about $+\pi/2$. Zero is returned
+       if the two points are coincident.
+ \item If either B-coordinate is outside the range $\pm\pi/2$, the
+       result may correspond to ``the long way round''.
+ \item The routine sla\_PAV performs an equivalent function except
+       that the points are specified in the form of Cartesian unit
+       vectors.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_CAF2R}{Deg,Arcmin,Arcsec to Radians}
+{
+ \action{Convert degrees, arcminutes, arcseconds to radians
+         (single precision).}
+ \call{CALL sla\_CAF2R (IDEG, IAMIN, ASEC, RAD, J)}
+}
+\args{GIVEN}
+{
+ \spec{IDEG}{I}{degrees} \\
+ \spec{IAMIN}{I}{arcminutes} \\
+ \spec{ASEC}{R}{arcseconds}
+}
+\args{RETURNED}
+{
+ \spec{RAD}{R}{angle in radians} \\
+ \spec{J}{I}{status:} \\
+ \spec{}{}{\hspace{1.5em} 1 = IDEG outside range 0$-$359} \\
+ \spec{}{}{\hspace{1.5em} 2 = IAMIN outside range 0$-$59} \\
+ \spec{}{}{\hspace{1.5em} 3 = ASEC outside range 0$-$59.999$\cdots$}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The result is computed even if any of the range checks fail.
+  \item The sign must be dealt with outside this routine.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_CALDJ}{Calendar Date to MJD}
+{
+ \action{Gregorian Calendar to Modified Julian Date, with century default.}
+ \call{CALL sla\_CALDJ (IY, IM, ID, DJM, J)}
+}
+\args{GIVEN}
+{
+ \spec{IY,IM,ID}{I}{year, month, day in Gregorian calendar}
+}
+\args{RETURNED}
+{
+ \spec{DJM}{D}{modified Julian Date (JD$-$2400000.5) for $0^{\rm h}$} \\
+ \spec{J}{I}{status:} \\
+ \spec{}{}{\hspace{1.5em} 0 = OK} \\
+ \spec{}{}{\hspace{1.5em} 1 = bad year   (MJD not computed)} \\
+ \spec{}{}{\hspace{1.5em} 2 = bad month  (MJD not computed)} \\
+ \spec{}{}{\hspace{1.5em} 3 = bad day    (MJD computed)} \\
+}
+\notes
+{
+ \begin{enumerate}
+  \item This routine supports the {\it century default}\/ feature.
+        Acceptable years are:
+        \begin{itemize}
+         \item 00-49, interpreted as 2000\,--\,2049,
+         \item 50-99, interpreted as 1950\,--\,1999, and
+         \item 100 upwards, interpreted literally.
+        \end{itemize}
+        For 1-100AD use the routine sla\_CLDJ instead.
+  \item For year $n$BC use IY = $-(n-1)$.
+  \item When an invalid year or month is supplied (status J~=~1~or~2)
+        the MJD is {\bf not} computed.  When an invalid day is supplied
+        (status J~=~3) the MJD {\bf is} computed.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_CALYD}{Calendar to Year, Day}
+{
+ \action{Gregorian calendar date to year and day in year, in a Julian
+         calendar aligned to the 20th/21st century Gregorian calendar,
+         with century default.}
+ \call{CALL sla\_CALYD (IY, IM, ID, NY, ND, J)}
+}
+\args{GIVEN}
+{
+ \spec{IY,IM,ID}{I}{year, month, day in Gregorian calendar:
+                    year may optionally omit the century}
+}
+\args{RETURNED}
+{
+ \spec{NY}{I}{year (re-aligned Julian calendar)} \\
+ \spec{ND}{I}{day in year (1 = January 1st)} \\
+ \spec{J}{I}{status:} \\
+ \spec{}{}{\hspace{1.5em}  0 = OK} \\
+ \spec{}{}{\hspace{1.5em}  1 = bad year (before $-4711$)} \\
+ \spec{}{}{\hspace{1.5em}  2 = bad month} \\
+ \spec{}{}{\hspace{1.5em}  3 = bad day}
+}
+\notes
+{
+ \begin{enumerate}
+  \item This routine supports the {\it century default}\/ feature.
+        Acceptable years are:
+        \begin{itemize}
+         \item 00-49, interpreted as 2000\,--\,2049,
+         \item 50-99, interpreted as 1950\,--\,1999, and
+         \item other years after -4712 , interpreted literally.
+        \end{itemize}
+        Use sla\_CLYD for years before 100AD.
+  \item The purpose of sla\_CALDJ is to support
+        sla\_EARTH, sla\_MOON and sla\_ECOR.
+  \item Between 1900~March~1 and 2100~February~28 it returns answers
+        which are consistent with the ordinary Gregorian calendar.
+        Outside this range there will be a discrepancy which increases
+        by one day for every non-leap century year.
+  \item When an invalid year or month is supplied (status J~=~1 or J~=~2)
+        the results are {\bf not} computed.  When a day is
+        supplied which is outside the conventional range (status J~=~3)
+        the results {\bf are} computed.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_CC2S}{Cartesian to Spherical}
+{
+ \action{Cartesian coordinates to spherical coordinates (single precision).}
+ \call{CALL sla\_CC2S (V, A, B)}
+}
+\args{GIVEN}
+{
+ \spec{V}{R(3)}{\xyz\ vector}
+}
+\args{RETURNED}
+{
+ \spec{A,B}{R}{spherical coordinates in radians}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The spherical coordinates are longitude (+ve anticlockwise
+        looking from the +ve latitude pole) and latitude.  The
+        Cartesian coordinates are right handed, with the {\it x}-axis
+        at zero longitude and latitude, and the {\it z}-axis at the
+        +ve latitude pole.
+  \item If V is null, zero A and B are returned.
+  \item At either pole, zero A is returned.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_CC62S}{Cartesian 6-Vector to Spherical}
+{
+ \action{Conversion of position \& velocity in Cartesian coordinates
+         to spherical coordinates (single precision).}
+ \call{CALL sla\_CC62S (V, A, B, R, AD, BD, RD)}
+}
+\args{GIVEN}
+{
+ \spec{V}{R(6)}{\xyzxyzd}
+}
+\args{RETURNED}
+{
+ \spec{A}{R}{longitude (radians) -- for example $\alpha$} \\
+ \spec{B}{R}{latitude (radians) -- for example $\delta$} \\
+ \spec{R}{R}{radial coordinate} \\
+ \spec{AD}{R}{longitude derivative (radians per unit time)} \\
+ \spec{BD}{R}{latitude derivative (radians per unit time)} \\
+ \spec{RD}{R}{radial derivative}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_CD2TF}{Days to Hour,Min,Sec}
+{
+ \action{Convert an interval in days to hours, minutes, seconds
+         (single precision).}
+ \call{CALL sla\_CD2TF (NDP, DAYS, SIGN, IHMSF)}
+}
+\args{GIVEN}
+{
+ \spec{NDP}{I}{number of decimal places of seconds} \\
+ \spec{DAYS}{R}{interval in days}
+}
+\args{RETURNED}
+{
+ \spec{SIGN}{C}{`+' or `$-$'} \\
+ \spec{IHMSF}{I(4)}{hours, minutes, seconds, fraction}
+}
+\notes
+{
+ \begin{enumerate}
+  \item NDP less than zero is interpreted as zero.
+  \item The largest useful value for NDP is determined by the size of
+        DAYS, the format of REAL floating-point numbers on the target
+        machine, and the risk of overflowing IHMSF(4).  For example,
+        on a VAX computer, for DAYS up to 1.0, the available floating-point
+        precision corresponds roughly to NDP=3.  This is well below
+        the ultimate limit of NDP=9 set by the capacity of the 32-bit
+        integer IHMSF(4).
+  \item The absolute value of DAYS may exceed 1.0.  In cases where it
+        does not, it is up to the caller to test for and handle the
+        case where DAYS is very nearly 1.0 and rounds up to 24~hours,
+        by testing for IHMSF(1)=24 and setting IHMSF(1-4) to zero.
+\end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_CLDJ}{Calendar to MJD}
+{
+ \action{Gregorian Calendar to Modified Julian Date.}
+ \call{CALL sla\_CLDJ (IY, IM, ID, DJM, J)}
+}
+\args{GIVEN}
+{
+ \spec{IY,IM,ID}{I}{year, month, day in Gregorian calendar}
+}
+\args{RETURNED}
+{
+ \spec{DJM}{D}{modified Julian Date (JD$-$2400000.5) for $0^{\rm h}$} \\
+ \spec{J}{I}{status:} \\
+ \spec{}{}{\hspace{1.5em} 0 = OK} \\
+ \spec{}{}{\hspace{1.5em} 1 = bad year} \\
+ \spec{}{}{\hspace{1.5em} 2 = bad month} \\
+ \spec{}{}{\hspace{1.5em} 3 = bad day}
+}
+\notes
+{
+ \begin{enumerate}
+  \item When an invalid year or month is supplied (status J~=~1~or~2)
+        the MJD is {\bf not} computed.  When an invalid day is supplied
+        (status J~=~3) the MJD {\bf is} computed.
+  \item The year must be $-$4699 ({\it i.e.}\ 4700BC) or later.
+        For year $n$BC use IY = $-(n-1)$.
+  \item An alternative to the present routine is sla\_CALDJ, which
+        accepts a year with the century missing.
+ \end{enumerate}
+}
+\aref{The algorithm is derived from that of Hatcher,
+      {\it Q.\,Jl.\,R.\,astr.\,Soc.}\ (1984) {\bf 25}, 53-55.}
+%-----------------------------------------------------------------------
+\routine{SLA\_CLYD}{Calendar to Year, Day}
+{
+ \action{Gregorian calendar date to year and day in year, in a Julian
+         calendar aligned to the 20th/21st century Gregorian calendar.}
+ \call{CALL sla\_CLYD (IY, IM, ID, NY, ND, J)}
+}
+\args{GIVEN}
+{
+ \spec{IY,IM,ID}{I}{year, month, day in Gregorian calendar}
+}
+\args{RETURNED}
+{
+ \spec{NY}{I}{year (re-aligned Julian calendar)} \\
+ \spec{ND}{I}{day in year (1 = January 1st)} \\
+ \spec{J}{I}{status:} \\
+ \spec{}{}{\hspace{1.5em}  0 = OK} \\
+ \spec{}{}{\hspace{1.5em}  1 = bad year (before $-4711$)} \\
+ \spec{}{}{\hspace{1.5em}  2 = bad month} \\
+ \spec{}{}{\hspace{1.5em}  3 = bad day}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The purpose of sla\_CLYD is to support sla\_EARTH,
+        sla\_MOON and sla\_ECOR.
+  \item Between 1900~March~1 and 2100~February~28 it returns answers
+        which are consistent with the ordinary Gregorian calendar.
+        Outside this range there will be a discrepancy which increases
+        by one day for every non-leap century year.
+  \item When an invalid year or month is supplied (status J~=~1 or J~=~2)
+        the results are {\bf not} computed.  When a day is
+        supplied which is outside the conventional range (status J~=~3)
+        the results {\bf are} computed.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_COMBN}{Next Combination}
+{
+ \action{Generate the next combination, a subset of a specified size chosen
+         from a specified number of items.}
+ \call{CALL sla\_COMBN (NSEL, NCAND, LIST, J)}
+}
+\args{GIVEN}
+{
+ \spec{NSEL}{I}{number of items (subset size)} \\
+ \spec{NCAND}{I}{number of candidates (set size)}
+}
+\args{GIVEN and RETURNED}
+{
+ \spec{LIST}{I(NSEL)}{latest combination, LIST(1)=0 to initialize}
+}
+\args{RETURNED}
+{
+ \spec{J}{I}{status:} \\
+ \spec{}{}{\hspace{1.5em} $-$1 = illegal NSEL or NCAND} \\
+ \spec{}{}{\hspace{2.3em}    0 = OK} \\
+ \spec{}{}{\hspace{1.5em} $+$1 = no more combinations available}
+}
+\notes
+{
+ \begin{enumerate}
+  \item NSEL and NCAND must both be at least 1, and NSEL must be less
+        than or equal to NCAND.
+  \item This routine returns, in the LIST array, a subset of NSEL integers
+        chosen from the range 1 to NCAND inclusive, in ascending order.
+        Before calling the routine for the first time, the caller must set
+        the first element of the LIST array to zero (any value less than 1
+        will do) to cause initialization.
+  \item The first combination to be generated is:
+        \begin{verse}
+            LIST(1)=1, LIST(2)=2, \ldots, LIST(NSEL)=NSEL
+        \end{verse}
+        This is also the combination returned for the ``finished'' (J=1) case.
+        The final permutation to be generated is:
+        \begin{verse}
+           LIST(1)=NCAND, LIST(2)=NCAND$-$1, \ldots, \\
+           ~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~LIST(NSEL)=NCAND$-$NSEL+1
+        \end{verse}
+  \item If the ``finished'' (J=1) status is ignored, the routine
+        continues to deliver combinations, the pattern repeating
+        every NCAND!/(NSEL!(NCAND$-$NSEL)!) calls.
+  \item The algorithm is by R.\,F.\,Warren-Smith (private communication).
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_CR2AF}{Radians to Deg,Arcmin,Arcsec}
+{
+ \action{Convert an angle in radians to degrees, arcminutes,
+         arcseconds (single precision).}
+ \call{CALL sla\_CR2AF (NDP, ANGLE, SIGN, IDMSF)}
+}
+\args{GIVEN}
+{
+ \spec{NDP}{I}{number of decimal places of arcseconds} \\
+ \spec{ANGLE}{R}{angle in radians}
+}
+\args{RETURNED}
+{
+ \spec{SIGN}{C}{`+' or `$-$'} \\
+ \spec{IDMSF}{I(4)}{degrees, arcminutes, arcseconds, fraction}
+}
+\notes
+{
+ \begin{enumerate}
+  \item NDP less than zero is interpreted as zero.
+  \item The largest useful value for NDP is determined by the size of
+        ANGLE, the format of REAL floating-point numbers on the target
+        machine, and the risk of overflowing IDMSF(4).  For example,
+        on a VAX computer, for ANGLE up to $2\pi$, the available floating-point
+        precision corresponds roughly to NDP=3.  This is well below
+        the ultimate limit of NDP=9 set by the capacity of the 32-bit
+        integer IHMSF(4).
+  \item The absolute value of ANGLE may exceed $2\pi$.  In cases where it
+        does not, it is up to the caller to test for and handle the
+        case where ANGLE is very nearly $2\pi$ and rounds up to $360^{\circ}$,
+        by testing for IDMSF(1)=360 and setting IDMSF(1-4) to zero.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_CR2TF}{Radians to Hour,Min,Sec}
+{
+ \action{Convert an angle in radians to hours, minutes, seconds
+         (single precision).}
+ \call{CALL sla\_CR2TF (NDP, ANGLE, SIGN, IHMSF)}
+}
+\args{GIVEN}
+{
+ \spec{NDP}{I}{number of decimal places of seconds} \\
+ \spec{ANGLE}{R}{angle in radians}
+}
+\args{RETURNED}
+{
+ \spec{SIGN}{C}{`+' or `$-$'} \\
+ \spec{IHMSF}{I(4)}{hours, minutes, seconds, fraction}
+}
+\notes
+{
+ \begin{enumerate}
+  \item NDP less than zero is interpreted as zero.
+  \item The largest useful value for NDP is determined by the size of
+        ANGLE, the format of REAL floating-point numbers on the target
+        machine, and the risk of overflowing IHMSF(4).  For example,
+        on a VAX computer, for ANGLE up to $2\pi$, the available floating-point
+        precision corresponds roughly to NDP=3.  This is well below
+        the ultimate limit of NDP=9 set by the capacity of the 32-bit
+        integer IHMSF(4).
+  \item The absolute value of ANGLE may exceed $2\pi$.  In cases where it
+        does not, it is up to the caller to test for and handle the
+        case where ANGLE is very nearly $2\pi$ and rounds up to 24~hours,
+        by testing for IHMSF(1)=24 and setting IHMSF(1-4) to zero.
+\end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_CS2C}{Spherical to Cartesian}
+{
+ \action{Spherical coordinates to Cartesian coordinates (single precision).}
+ \call{CALL sla\_CS2C (A, B, V)}
+}
+\args{GIVEN}
+{
+ \spec{A,B}{R}{spherical coordinates in radians: \radec\ {\it etc.}}
+}
+\args{RETURNED}
+{
+ \spec{V}{R(3)}{\xyz\ unit vector}
+}
+\anote{The spherical coordinates are longitude (+ve anticlockwise
+       looking from the +ve latitude pole) and latitude.  The
+       Cartesian coordinates are right handed, with the {\it x}-axis
+       at zero longitude and latitude, and the {\it z}-axis at the
+       +ve latitude pole.}
+%-----------------------------------------------------------------------
+\routine{SLA\_CS2C6}{Spherical Pos/Vel to Cartesian}
+{
+ \action{Conversion of position \& velocity in spherical coordinates
+         to Cartesian coordinates (single precision).}
+ \call{CALL sla\_CS2C6 (A, B, R, AD, BD, RD, V)}
+}
+\args{GIVEN}
+{
+ \spec{A}{R}{longitude (radians) -- for example $\alpha$} \\
+ \spec{B}{R}{latitude (radians) -- for example $\delta$} \\
+ \spec{R}{R}{radial coordinate} \\
+ \spec{AD}{R}{longitude derivative (radians per unit time)} \\
+ \spec{BD}{R}{latitude derivative (radians per unit time)} \\
+ \spec{RD}{R}{radial derivative}
+}
+\args{RETURNED}
+{
+ \spec{V}{R(6)}{\xyzxyzd}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_CTF2D}{Hour,Min,Sec to Days}
+{
+ \action{Convert hours, minutes, seconds to days (single precision).}
+ \call{CALL sla\_CTF2D (IHOUR, IMIN, SEC, DAYS, J)}
+}
+\args{GIVEN}
+{
+ \spec{IHOUR}{I}{hours} \\
+ \spec{IMIN}{I}{minutes} \\
+ \spec{SEC}{R}{seconds}
+}
+\args{RETURNED}
+{
+ \spec{DAYS}{R}{interval in days} \\
+ \spec{J}{I}{status:} \\
+ \spec{}{}{\hspace{1.5em} 0 = OK} \\
+ \spec{}{}{\hspace{1.5em} 1 = IHOUR outside range 0-23} \\
+ \spec{}{}{\hspace{1.5em} 2 = IMIN outside range 0-59} \\
+ \spec{}{}{\hspace{1.5em} 3 = SEC outside range 0-59.999$\cdots$}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The result is computed even if any of the range checks fail.
+  \item The sign must be dealt with outside this routine.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_CTF2R}{Hour,Min,Sec to Radians}
+{
+ \action{Convert hours, minutes, seconds to radians (single precision).}
+ \call{CALL sla\_CTF2R (IHOUR, IMIN, SEC, RAD, J)}
+}
+\args{GIVEN}
+{
+ \spec{IHOUR}{I}{hours} \\
+ \spec{IMIN}{I}{minutes} \\
+ \spec{SEC}{R}{seconds}
+}
+\args{RETURNED}
+{
+ \spec{RAD}{R}{angle in radians} \\
+ \spec{J}{I}{status:} \\
+ \spec{}{}{\hspace{1.5em} 0 = OK} \\
+ \spec{}{}{\hspace{1.5em} 1 = IHOUR outside range 0-23} \\
+ \spec{}{}{\hspace{1.5em} 2 = IMIN outside range 0-59} \\
+ \spec{}{}{\hspace{1.5em} 3 = SEC outside range 0-59.999$\cdots$}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The result is computed even if any of the range checks fail.
+  \item The sign must be dealt with outside this routine.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DAF2R}{Deg,Arcmin,Arcsec to Radians}
+{
+ \action{Convert degrees, arcminutes, arcseconds to radians
+  (double precision).}
+ \call{CALL sla\_DAF2R (IDEG, IAMIN, ASEC, RAD, J)}
+}
+\args{GIVEN}
+{
+ \spec{IDEG}{I}{degrees} \\
+ \spec{IAMIN}{I}{arcminutes} \\
+ \spec{ASEC}{D}{arcseconds}
+}
+\args{RETURNED}
+{
+ \spec{RAD}{D}{angle in radians} \\
+ \spec{J}{I}{status:} \\
+ \spec{}{}{\hspace{1.5em} 1 = IDEG outside range 0$-$359} \\
+ \spec{}{}{\hspace{1.5em} 2 = IAMIN outside range 0$-$59} \\
+ \spec{}{}{\hspace{1.5em} 3 = ASEC outside range 0$-$59.999$\cdots$}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The result is computed even if any of the range checks fail.
+  \item The sign must be dealt with outside this routine.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DAFIN}{Sexagesimal character string to angle}
+{
+ \action{Decode a free-format sexagesimal string (degrees, arcminutes,
+         arcseconds) into a double precision floating point
+         number (radians).}
+ \call{CALL sla\_DAFIN (STRING, NSTRT, DRESLT, JF)}
+}
+\args{GIVEN}
+{
+ \spec{STRING}{C*(*)}{string containing deg, arcmin, arcsec fields} \\
+ \spec{NSTRT}{I}{pointer to start of decode (beginning of STRING = 1)}
+}
+\args{RETURNED}
+{
+ \spec{NSTRT}{I}{advanced past the decoded angle} \\
+ \spec{DRESLT}{D}{angle in radians} \\
+ \spec{JF}{I}{status:} \\
+ \spec{}{}{\hspace{1.5em}   0 = OK} \\
+ \spec{}{}{\hspace{0.7em} $+1$ = default, DRESLT unchanged (note 2)} \\
+ \spec{}{}{\hspace{0.7em} $-1$ = bad degrees (note 3)} \\
+ \spec{}{}{\hspace{0.7em} $-2$ = bad arcminutes (note 3)} \\
+ \spec{}{}{\hspace{0.7em} $-3$ = bad arcseconds (note 3)} \\
+}
+\goodbreak
+\setlength{\oldspacing}{\topsep}
+\setlength{\topsep}{0.3ex}
+\begin{description}
+ \item [EXAMPLE]: \\ [1.5ex]
+  \begin{tabular}{p{7em}p{15em}p{12em}}
+   {\it argument} & {\it before} & {\it after} \\ \\
+   STRING & $'$\verb*}-57 17 44.806  12 34 56.7}$'$ & unchanged \\
+   NSTRT & 1 & 16 ({\it i.e.}\ pointing to 12...) \\
+   RESLT & - & $-1.00000${\tt D0} \\
+   JF & - & 0
+  \end{tabular}
+ \item A further call to sla\_DAFIN, without adjustment of NSTRT, will
+       decode the second angle, \dms{12}{34}{56}{7}.
+\end{description}
+\setlength{\topsep}{\oldspacing}
+\notes
+{
+ \begin{enumerate}
+  \item 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 sla\_DFLTIN routine and is free-format.
+  \item 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 DRESLT is
+   unchanged.  In all other cases DRESLT is changed.
+  \item Range checking:
+   \begin{itemize}
+    \item The degrees field is not range checked.  However, it is
+     expected to be integral unless the other two fields are absent.
+    \item 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...
+    \item The arcseconds field is expected to be 0-59.9999...
+    \item Decoding continues even when a check has failed.  Under these
+     circumstances the field takes the supplied value, defaulting to
+     zero, and the result DRESLT is computed and returned.
+   \end{itemize}
+   \item Further fields after the three expected ones are not treated as
+    an error.  The pointer NSTRT is left in the correct state for
+    further decoding with the present routine or with sla\_DFLTIN
+    {\it etc}.  See the example, above.
+   \item If STRING contains hours, minutes, seconds instead of
+    degrees {\it etc},
+    or if the required units are turns (or days) instead of radians,
+    the result DRESLT should be multiplied as follows: \\ [1.5ex]
+    \begin{tabular}{p{6em}p{5em}p{18em}}
+    {\it for STRING} & {\it to obtain} & {\it multiply DRESLT by} \\ \\
+    ${\circ}$~~\raisebox{-0.7ex}{$'$}~~\raisebox{-0.7ex}{$''$}
+     & radians & $1.0${\tt D0} \\
+    ${\circ}$~~\raisebox{-0.7ex}{$'$}~~\raisebox{-0.7ex}{$''$}
+     & turns & $1/{2 \pi} = 0.1591549430918953358${\tt D0} \\
+    h m s & radians & $15.0${\tt D0} \\
+    h m s & days & $15/{2\pi} = 2.3873241463784300365${\tt D0}
+   \end{tabular}
+ \end{enumerate}
+}
+%------------------------------------------------------------------------------
+\routine{SLA\_DAT}{TAI$-$UTC}
+{
+ \action{Increment to be applied to Coordinated Universal Time UTC to give
+         International Atomic Time TAI.}
+ \call{D~=~sla\_DAT (UTC)}
+}
+\args{GIVEN}
+{
+ \spec{UTC}{D}{UTC date as a modified JD (JD$-$2400000.5)}
+}
+\args{RETURNED}
+{
+ \spec{sla\_DAT}{D}{TAI$-$UTC in seconds}
+}
+\notes
+{
+ \begin{enumerate}
+ \item The UTC is specified to be a date rather than a time to indicate
+       that care needs to be taken not to specify an instant which lies
+       within a leap second.  Though in most cases UTC can include the
+       fractional part, correct behaviour on the day of a leap second
+       can be guaranteed only up to the end of the second
+       $23^{\rm h}\,59^{\rm m}\,59^{\rm s}$.
+ \item UTC began at 1960 January 1.  To specify a UTC prior to this
+       date would be meaningless;  in such cases the parameters
+       for the year 1960 are used by default.
+ \item This routine has to be updated on each occasion that a
+       leap second is announced, and programs using it relinked.
+       Refer to the program source code for information on when the
+       most recent leap second was added.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DAV2M}{Rotation Matrix from Axial Vector}
+{
+ \action{Form the rotation matrix corresponding to a given axial vector
+         (double precision).}
+ \call{CALL sla\_DAV2M (AXVEC, RMAT)}
+}
+\args{GIVEN}
+{
+ \spec{AXVEC}{D(3)}{axial vector (radians)}
+}
+\args{RETURNED}
+{
+ \spec{RMAT}{D(3,3)}{rotation matrix}
+}
+\notes
+{
+ \begin{enumerate}
+  \item A rotation matrix describes a rotation about some arbitrary axis.
+        The axis is called the {\it Euler axis}, and the angle through which the
+        reference frame rotates is called the {\it Euler angle}.  The axial
+        vector supplied to this routine has the same direction as the
+        Euler axis, and its magnitude is the Euler angle in radians.
+  \item If AXVEC is null, the unit matrix is returned.
+  \item The reference frame rotates clockwise as seen looking along
+        the axial vector from the origin.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DBEAR}{Direction Between Points on a Sphere}
+{
+ \action{Returns the bearing (position angle) of one point on a
+         sphere relative to another (double precision).}
+ \call{D~=~sla\_DBEAR (A1, B1, A2, B2)}
+}
+\args{GIVEN}
+{
+ \spec{A1,B1}{D}{spherical coordinates of one point} \\
+ \spec{A2,B2}{D}{spherical coordinates of the other point}
+}
+\args{RETURNED}
+{
+ \spec{sla\_DBEAR}{D}{bearing from first point to second}
+}
+\notes
+{
+ \begin{enumerate}
+ \item The spherical coordinates are \radec,
+       $[\lambda,\phi]$ {\it etc.}, in radians.
+ \item The result is the bearing (position angle), in radians,
+       of point [A2,B2] as seen
+       from point [A1,B1].  It is in the range $\pm \pi$.  The sense
+       is such that if [A2,B2]
+       is a small distance due east of [A1,B1] the result
+       is about $+\pi/2$. Zero is returned
+       if the two points are coincident.
+ \item If either B-coordinate is outside the range $\pm\pi/2$, the
+       result may correspond to ``the long way round''.
+ \item The routine sla\_DPAV performs an equivalent function except
+       that the points are specified in the form of Cartesian unit
+       vectors.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DBJIN}{Decode String to B/J Epoch (DP)}
+{
+ \action{Decode a character string into a DOUBLE PRECISION number,
+         with special provision for Besselian and Julian epochs.
+         The string syntax is as for sla\_DFLTIN, prefixed by
+         an optional `B' or `J'.}
+ \call{CALL sla\_DBJIN (STRING, NSTRT, DRESLT, J1, J2)}
+}
+\args{GIVEN}
+{
+ \spec{STRING}{C}{string containing field to be decoded} \\
+ \spec{NSTRT}{I}{pointer to first character of field in string}
+}
+\args{RETURNED}
+{
+ \spec{NSTRT}{I}{incremented past the decoded field} \\
+ \spec{DRESLT}{D}{result} \\
+ \spec{J1}{I}{DFLTIN status:} \\
+ \spec{}{}{\hspace{0.7em} $-$1 = $-$OK} \\
+ \spec{}{}{\hspace{1.5em}   0 = +OK} \\
+ \spec{}{}{\hspace{1.5em}   1 = null field} \\
+ \spec{}{}{\hspace{1.5em}   2 = error} \\
+ \spec{J2}{I}{syntax flag:} \\
+ \spec{}{}{\hspace{1.5em}   0 = normal DFLTIN syntax} \\
+ \spec{}{}{\hspace{1.5em}   1 = `B' or `b'} \\
+ \spec{}{}{\hspace{1.5em}   2 = `J' or `j'}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The purpose of the syntax extensions is to help cope with mixed
+        FK4 and FK5 data, allowing fields such as `B1950' or `J2000'
+        to be decoded.
+  \item In addition to the syntax accepted by sla\_DFLTIN,
+        the following two extensions are recognized by sla\_DBJIN:
+        \begin{enumerate}
+         \item A valid non-null field preceded by the character `B'
+               (or `b') is accepted.
+         \item A valid non-null field preceded by the character `J'
+               (or `j') is accepted.
+         \end{enumerate}
+  \item The calling program is told of the `B' or `J' through an
+        supplementary status argument.  The rest of
+        the arguments are as for sla\_DFLTIN.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DC62S}{Cartesian 6-Vector to Spherical}
+{
+ \action{Conversion of position \& velocity in Cartesian coordinates
+         to spherical coordinates (double precision).}
+ \call{CALL sla\_DC62S (V, A, B, R, AD, BD, RD)}
+}
+\args{GIVEN}
+{
+ \spec{V}{D(6)}{\xyzxyzd}
+}
+\args{RETURNED}
+{
+ \spec{A}{D}{longitude (radians)} \\
+ \spec{B}{D}{latitude (radians)} \\
+ \spec{R}{D}{radial coordinate} \\
+ \spec{AD}{D}{longitude derivative (radians per unit time)} \\
+ \spec{BD}{D}{latitude derivative (radians per unit time)} \\
+ \spec{RD}{D}{radial derivative}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DCC2S}{Cartesian to Spherical}
+{
+ \action{Cartesian coordinates to spherical coordinates (double precision).}
+ \call{CALL sla\_DCC2S (V, A, B)}
+}
+\args{GIVEN}
+{
+ \spec{V}{D(3)}{\xyz\ vector}
+}
+\args{RETURNED}
+{
+ \spec{A,B}{D}{spherical coordinates in radians}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The spherical coordinates are longitude (+ve anticlockwise
+        looking from the +ve latitude pole) and latitude.  The
+        Cartesian coordinates are right handed, with the {\it x}-axis
+        at zero longitude and latitude, and the {\it z}-axis at the
+        +ve latitude pole.
+  \item If V is null, zero A and B are returned.
+  \item At either pole, zero A is returned.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DCMPF}{Interpret Linear Fit}
+{
+ \action{Decompose an \xy\ linear fit into its constituent parameters:
+         zero points, scales, nonperpendicularity and orientation.}
+ \call{CALL sla\_DCMPF (COEFFS,XZ,YZ,XS,YS,PERP,ORIENT)}
+}
+\args{GIVEN}
+{
+ \spec{COEFFS}{D(6)}{transformation coefficients (see note)}
+}
+\args{RETURNED}
+{
+ \spec{XZ}{D}{{\it x} zero point} \\
+ \spec{YZ}{D}{{\it y} zero point} \\
+ \spec{XS}{D}{{\it x} scale} \\
+ \spec{YS}{D}{{\it y} scale} \\
+ \spec{PERP}{D}{nonperpendicularity (radians)} \\
+ \spec{ORIENT}{D}{orientation (radians)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The model relates two sets of \xy\ coordinates as follows.
+        Naming the six elements of COEFFS $a,b,c,d,e$ \& $f$,
+        the model transforms coordinates $[x_{1},y_{1}\,]$ into coordinates
+        $[x_{2},y_{2}\,]$ as follows:
+        \begin{verse}
+         $x_{2} = a + bx_{1} + cy_{1}$ \\
+         $y_{2} = d + ex_{1} + fy_{1}$
+        \end{verse}
+        The sla\_DCMPF routine decomposes this transformation
+        into four steps:
+        \begin{enumerate}
+        \item Zero points:
+              \begin{verse}
+               $x' = x_{1} + {\rm XZ}$ \\
+               $y' = y_{1} + {\rm YZ}$
+              \end{verse}
+        \item Scales:
+              \begin{verse}
+               $x'' = x' {\rm XS}$ \\
+               $y'' = y' {\rm YS}$
+              \end{verse}
+        \item Nonperpendicularity:
+              \begin{verse}
+               $x''' = + x'' \cos {\rm PERP}/2 + y'' \sin {\rm PERP}/2$ \\
+               $y''' = + x'' \sin {\rm PERP}/2 + y'' \cos {\rm PERP}/2$
+              \end{verse}
+        \item Orientation:
+              \begin{verse}
+               $x_{2} = + x''' \cos {\rm ORIENT} +
+                          y''' \sin {\rm ORIENT}$ \\
+               $y_{2} = - x''' \sin {\rm ORIENT} +
+                          y''' \cos {\rm ORIENT}$
+              \end{verse}
+        \end{enumerate}
+  \item See also sla\_FITXY, sla\_PXY, sla\_INVF, sla\_XY2XY.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DCS2C}{Spherical to Cartesian}
+{
+ \action{Spherical coordinates to Cartesian coordinates (double precision).}
+ \call{CALL sla\_DCS2C (A, B, V)}
+}
+\args{GIVEN}
+{
+ \spec{A,B}{D}{spherical coordinates in radians: \radec\ {\it etc.}}
+}
+\args{RETURNED}
+{
+ \spec{V}{D(3)}{\xyz\ unit vector}
+}
+\anote{The spherical coordinates are longitude (+ve anticlockwise
+       looking from the +ve latitude pole) and latitude.  The
+       Cartesian coordinates are right handed, with the {\it x}-axis
+       at zero longitude and latitude, and the {\it z}-axis at the
+       +ve latitude pole.}
+%-----------------------------------------------------------------------
+\routine{SLA\_DD2TF}{Days to Hour,Min,Sec}
+{
+ \action{Convert an interval in days into hours, minutes, seconds
+         (double precision).}
+ \call{CALL sla\_DD2TF (NDP, DAYS, SIGN, IHMSF)}
+}
+\args{GIVEN}
+{
+ \spec{NDP}{I}{number of decimal places of seconds} \\
+ \spec{DAYS}{D}{interval in days}
+}
+\args{RETURNED}
+{
+ \spec{SIGN}{C}{`+' or `$-$'} \\
+ \spec{IHMSF}{I(4)}{hours, minutes, seconds, fraction}
+}
+\notes
+{
+ \begin{enumerate}
+  \item NDP less than zero is interpreted as zero.
+  \item The largest useful value for NDP is determined by the size
+        of DAYS, the format of DOUBLE PRECISION floating-point numbers
+        on the target machine, and the risk of overflowing IHMSF(4).
+        For example, on a VAX computer, for DAYS up to 1D0, the available
+        floating-point precision corresponds roughly to NDP=12.  However,
+        the practical limit is NDP=9, set by the capacity of the 32-bit
+        integer IHMSF(4).
+  \item The absolute value of DAYS may exceed 1D0.  In cases where it
+        does not, it is up to the caller to test for and handle the
+        case where DAYS is very nearly 1D0 and rounds up to 24~hours,
+        by testing for IHMSF(1)=24 and setting IHMSF(1-4) to zero.
+\end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DE2H}{$h,\delta$ to Az,El}
+{
+ \action{Equatorial to horizon coordinates
+         (double precision).}
+ \call{CALL sla\_DE2H (HA, DEC, PHI, AZ, EL)}
+}
+\args{GIVEN}
+{
+ \spec{HA}{D}{hour angle (radians)} \\
+ \spec{DEC}{D}{declination (radians)} \\
+ \spec{PHI}{D}{latitude (radians)}
+}
+\args{RETURNED}
+{
+ \spec{AZ}{D}{azimuth (radians)} \\
+ \spec{EL}{D}{elevation (radians)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item Azimuth is returned in the range $0\!-\!2\pi$;  north is zero,
+        and east is $+\pi/2$.  Elevation is returned in the range
+        $\pm\pi$.
+  \item The latitude must be geodetic.  In critical applications,
+        corrections for polar motion should be applied.
+  \item 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 {\it observed} \hadec, and the elevation
+        {\it in vacuo}, which would require the {\it topocentric}
+        \hadec.
+        If the effects of diurnal aberration can be neglected, the
+        {\it apparent} \hadec\ may be used instead of the topocentric
+        \hadec.
+  \item No range checking of arguments is carried out.
+  \item 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.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DEULER}{Euler Angles to Rotation Matrix}
+{
+ \action{Form a rotation matrix from the Euler angles -- three
+         successive rotations about specified Cartesian axes
+         (double precision).}
+ \call{CALL sla\_DEULER (ORDER, PHI, THETA, PSI, RMAT)}
+}
+\args{GIVEN}
+{
+ \spec{ORDER}{C}{specifies about which axes the rotations occur} \\
+ \spec{PHI}{D}{1st rotation (radians)} \\
+ \spec{THETA}{D}{2nd rotation (radians)} \\
+ \spec{PSI}{D}{3rd rotation (radians)}
+}
+\args{RETURNED}
+{
+ \spec{RMAT}{D(3,3)}{rotation matrix}
+}
+\notes
+{
+ \begin{enumerate}
+ \item A rotation is positive when the reference frame rotates
+       anticlockwise as seen looking towards the origin from the
+       positive region of the specified axis.
+ \item 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 {\it z}-axis, followed by THETA radians about the resulting
+       {\it x}-axis,
+       then PSI radians about the resulting {\it z}-axis.
+ \item 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 {\it xyz} ($\equiv123$)
+       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.  Zero rotations produces a unit RMAT.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DFLTIN}{Decode a Double Precision Number}
+{
+ \action{Convert free-format input into double precision floating point.}
+ \call{CALL sla\_DFLTIN (STRING, NSTRT, DRESLT, JFLAG)}
+}
+\args{GIVEN}
+{
+ \spec{STRING}{C}{string containing number to be decoded} \\
+ \spec{NSTRT}{I}{pointer to where decoding is to commence} \\
+ \spec{DRESLT}{D}{current value of result}
+}
+\args{RETURNED}
+{
+ \spec{NSTRT}{I}{advanced to next number} \\
+ \spec{DRESLT}{D}{result} \\
+ \spec{JFLAG}{I}{status: $-$1~=~$-$OK, 0~=~+OK, 1~=~null result, 2~=~error}
+}
+\notes
+{
+ \begin{enumerate}
+ \item The reason sla\_DFLTIN has separate `OK' status values
+       for + and $-$ is to enable minus zero to be detected.
+       This is of crucial importance
+       when decoding mixed-radix numbers.  For example, an angle
+       expressed as degrees, arcminutes and arcseconds may have a
+       leading minus sign but a zero degrees field.
+ \item A TAB is interpreted as a space, and lowercase characters are
+       interpreted as uppercase.  {\it n.b.}\ The test for TAB is
+       ASCII-specific.
+ \item The basic format is the sequence of fields $\pm n.n x \pm n$,
+       where $\pm$ is a sign
+       character `+' or `$-$', $n$ means a string of decimal digits,
+       `.' is a decimal point, and $x$, which indicates an exponent,
+       means `D' or `E'.  Various combinations of these fields can be
+       omitted, and embedded blanks are permissible in certain places.
+ \item Spaces:
+       \begin{itemize}
+       \item Leading spaces are ignored.
+       \item Embedded spaces are allowed only after +, $-$, D or E,
+             and after the decimal point if the first sequence of
+             digits is absent.
+       \item Trailing spaces are ignored;  the first signifies
+             end of decoding and subsequent ones are skipped.
+       \end{itemize}
+ \item Delimiters:
+       \begin{itemize}
+       \item Any character other than +,$-$,0-9,.,D,E or space may be
+             used to signal the end of the number and terminate decoding.
+       \item Comma is recognized by sla\_DFLTIN as a special case; it
+             is skipped, leaving the pointer on the next character.  See
+             13, below.
+       \item Decoding will in all cases terminate if end of string
+             is reached.
+       \end{itemize}
+ \item Both signs are optional.  The default is +.
+ \item The mantissa $n.n$ defaults to unity.
+ \item The exponent $x\!\pm\!n$ defaults to `D0'.
+ \item The strings of decimal digits may be of any length.
+ \item The decimal point is optional for whole numbers.
+ \item A {\it null result}\/ occurs when the string of characters
+       being decoded does not begin with +,$-$,0-9,.,D or E, or
+       consists entirely of spaces.  When this condition is
+       detected, JFLAG is set to 1 and DRESLT is left untouched.
+ \item NSTRT = 1 for the first character in the string.
+ \item On return from sla\_DFLTIN, NSTRT is set ready for the next
+       decode -- following trailing blanks and any comma.  If a
+       delimiter other than comma is being used, NSTRT must be
+       incremented before the next call to sla\_DFLTIN, otherwise
+       all subsequent calls will return a null result.
+ \item Errors (JFLAG=2) occur when:
+       \begin{itemize}
+       \item a +, $-$, D or E is left unsatisfied; or
+       \item the decimal point is present without at least
+             one decimal digit before or after it; or
+       \item an exponent more than 100 has been presented.
+       \end{itemize}
+ \item When an error has been detected, NSTRT is left
+       pointing to the character following the last
+       one used before the error came to light.  This
+       may be after the point at which a more sophisticated
+       program could have detected the error.  For example,
+       sla\_DFLTIN does not detect that `1D999' is unacceptable
+       (on a computer where this is so) until the entire number
+       has been decoded.
+ \item Certain highly unlikely combinations of mantissa and
+       exponent can cause arithmetic faults during the
+       decode, in some cases despite the fact that they
+       together could be construed as a valid number.
+ \item Decoding is left to right, one pass.
+ \item See also sla\_FLOTIN and sla\_INTIN.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DH2E}{Az,El to $h,\delta$}
+{
+ \action{Horizon to equatorial coordinates
+         (double precision).}
+ \call{CALL sla\_DH2E (AZ, EL, PHI, HA, DEC)}
+}
+\args{GIVEN}
+{
+ \spec{AZ}{D}{azimuth (radians)} \\
+ \spec{EL}{D}{elevation (radians)} \\
+ \spec{PHI}{D}{latitude (radians)}
+}
+\args{RETURNED}
+{
+ \spec{HA}{D}{hour angle (radians)} \\
+ \spec{DEC}{D}{declination (radians)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The sign convention for azimuth is north zero, east $+\pi/2$.
+  \item HA is returned in the range $\pm\pi$.  Declination is returned
+        in the range $\pm\pi$.
+  \item The latitude is (in principle) geodetic.  In critical
+        applications, corrections for polar motion should be applied
+        (see sla\_POLMO).
+  \item In some applications it will be important to specify the
+        correct type of elevation in order to produce the required
+        type of \hadec.  In particular, it may be important to
+        distinguish between the elevation as affected by refraction,
+        which will yield the {\it observed} \hadec, and the elevation
+        {\it in vacuo}, which will yield the {\it topocentric}
+        \hadec.  If the
+        effects of diurnal aberration can be neglected, the
+        topocentric \hadec\ may be used as an approximation to the
+        {\it apparent} \hadec.
+  \item No range checking of arguments is carried out.
+  \item 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.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DIMXV}{Apply 3D Reverse Rotation}
+{
+ \action{Multiply a 3-vector by the inverse of a rotation
+         matrix (double precision).}
+ \call{CALL sla\_DIMXV (DM, VA, VB)}
+}
+\args{GIVEN}
+{
+ \spec{DM}{D(3,3)}{rotation matrix} \\
+ \spec{VA}{D(3)}{vector to be rotated}
+}
+\args{RETURNED}
+{
+ \spec{VB}{D(3)}{result vector}
+}
+\notes
+{
+ \begin{enumerate}
+  \item This routine performs the operation:
+        \begin{verse}
+         {\bf b} = {\bf M}$^{T}\cdot${\bf a}
+        \end{verse}
+        where {\bf a} and {\bf b} are the 3-vectors VA and VB
+        respectively, and  {\bf M} is the $3\times3$ matrix DM.
+  \item The main function of this routine is apply an inverse
+        rotation;  under these circumstances, ${\bf \rm M}$ is
+        {\it orthogonal}, with its inverse the same as its transpose.
+  \item To comply with the ANSI Fortran 77 standard, VA and VB must
+        {\bf not} be the same array.  The routine is, in fact, coded
+        so as to work properly on the VAX and many other systems even
+        if this rule is violated, something that is {\bf not}, however,
+        recommended.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DJCAL}{MJD to Gregorian for Output}
+{
+ \action{Modified Julian Date to Gregorian Calendar Date, expressed
+         in a form convenient for formatting messages (namely
+         rounded to a specified precision, and with the fields
+         stored in a single array).}
+ \call{CALL sla\_DJCAL (NDP, DJM, IYMDF, J)}
+}
+\args{GIVEN}
+{
+ \spec{NDP}{I}{number of decimal places of days in fraction} \\
+ \spec{DJM}{D}{modified Julian Date (JD$-$2400000.5)}
+}
+\args{RETURNED}
+{
+ \spec{IYMDF}{I(4)}{year, month, day, fraction in Gregorian calendar} \\
+ \spec{J}{I}{status:  nonzero = out of range}
+}
+\notes
+{
+ \begin{enumerate}
+  \item Any date after 4701BC March 1 is accepted.
+  \item NDP should be 4 or less to avoid overflow on machines which
+        use 32-bit integers.
+ \end{enumerate}
+}
+\aref{The algorithm is derived from that of Hatcher,
+      {\it Q.\,Jl.\,R.\,astr.\,Soc.}\ (1984) {\bf 25}, 53-55.}
+%-----------------------------------------------------------------------
+\routine{SLA\_DJCL}{MJD to Year,Month,Day,Frac}
+{
+ \action{Modified Julian Date to Gregorian year, month, day,
+         and fraction of a day.}
+ \call{CALL sla\_DJCL (DJM, IY, IM, ID, FD, J)}
+}
+\args{GIVEN}
+{
+ \spec{DJM}{D}{modified Julian Date (JD$-$2400000.5)}
+}
+\args{RETURNED}
+{
+ \spec{IY}{I}{year} \\
+ \spec{IM}{I}{month} \\
+ \spec{ID}{I}{day} \\
+ \spec{FD}{D}{fraction of day} \\
+ \spec{J}{I}{status:} \\
+ \spec{}{}{\hspace{1.5em} 0 = OK} \\
+ \spec{}{}{\hspace{0.7em} $-$1 = unacceptable date (before 4701BC March 1)}
+}
+\aref{The algorithm is derived from that of Hatcher,
+      {\it Q.\,Jl.\,R.\,astr.\,Soc.}\ (1984) {\bf 25}, 53-55.}
+%-----------------------------------------------------------------------
+\routine{SLA\_DM2AV}{Rotation Matrix to Axial Vector}
+{
+ \action{From a rotation matrix, determine the corresponding axial vector
+        (double precision).}
+ \call{CALL sla\_DM2AV (RMAT, AXVEC)}
+}
+\args{GIVEN}
+{
+ \spec{RMAT}{D(3,3)}{rotation matrix}
+}
+\args{RETURNED}
+{
+ \spec{AXVEC}{D(3)}{axial vector (radians)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item A rotation matrix describes a rotation about some arbitrary axis.
+        The axis is called the {\it Euler axis}, and the angle through
+        which the reference frame rotates is called the {\it Euler angle}.
+        The {\it axial vector}\/ returned by this routine has the same
+        direction as the Euler axis, and its magnitude is the Euler angle
+        in radians.
+  \item The magnitude and direction of the axial vector can be separated
+        by means of the routine sla\_DVN.
+  \item The reference frame rotates clockwise as seen looking along
+        the axial vector from the origin.
+  \item If RMAT is null, so is the result.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DMAT}{Solve Simultaneous Equations}
+{
+ \action{Matrix inversion and solution of simultaneous equations
+         (double precision).}
+ \call{CALL sla\_DMAT (N, A, Y, D, JF, IW)}
+}
+\args{GIVEN}
+{
+ \spec{N}{I}{number of unknowns} \\
+ \spec{A}{D(N,N)}{matrix} \\
+ \spec{Y}{D(N)}{vector}
+}
+\args{RETURNED}
+{
+ \spec{A}{D(N,N)}{matrix inverse} \\
+ \spec{Y}{D(N)}{solution} \\
+ \spec{D}{D}{determinant} \\
+ \spec{JF}{I}{singularity flag: 0=OK} \\
+ \spec{IW}{I(N)}{workspace}
+}
+\notes
+{
+ \begin{enumerate}
+  \item For the set of $n$ simultaneous linear equations in $n$ unknowns:
+        \begin{verse}
+         {\bf A}$\cdot${\bf y} = {\bf x}
+        \end{verse}
+        where:
+        \begin{itemize}
+         \item {\bf A} is a non-singular $n \times n$ matrix,
+         \item {\bf y} is the vector of $n$ unknowns, and
+         \item {\bf x} is the known vector,
+        \end{itemize}
+        sla\_DMAT computes:
+        \begin{itemize}
+         \item the inverse of matrix {\bf A},
+         \item the determinant of matrix {\bf A}, and
+         \item the vector of $n$ unknowns {\bf y}.
+        \end{itemize}
+        Argument N is the order $n$, A (given) is the matrix {\bf A},
+        Y (given) is the vector {\bf x} and Y (returned)
+        is the vector {\bf y}.
+        The argument A (returned) is the inverse matrix {\bf A}$^{-1}$,
+        and D is {\it det}\/({\bf A}).
+  \item JF is the singularity flag.  If the matrix is non-singular,
+        JF=0 is returned.  If the matrix is singular, JF=$-$1
+        and D=0D0 are returned.  In the latter case, the contents
+        of array A on return are undefined.
+  \item The algorithm is Gaussian elimination with partial pivoting.
+        This method is very fast;  some much slower algorithms can give
+        better accuracy, but only by a small factor.
+  \item This routine replaces the obsolete sla\_DMATRX.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DMOON}{Approx Moon Pos/Vel}
+{
+ \action{Approximate geocentric position and velocity of the Moon
+         (double precision).}
+ \call{CALL sla\_DMOON (DATE, PV)}
+}
+\args{GIVEN}
+{
+ \spec{DATE}{D}{TDB (loosely ET) as a Modified Julian Date (JD$-$2400000.5)
+}
+}
+\args{RETURNED}
+{
+ \spec{PV}{D(6)}{Moon \xyzxyzd, mean equator and equinox
+                 of date (AU, AU~s$^{-1}$)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item This routine is a full implementation of the algorithm
+        published by Meeus (see reference).
+  \item Meeus quotes accuracies of \arcseci{10} in longitude,
+        \arcseci{3} in latitude and \arcsec{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
+        \arcsec{3}{7} and 83~mas/hour in longitude,
+        \arcsec{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
+        \arcseci{18} and \arcsec{0}{50}/hour in longitude,
+        \arcseci{11} and \arcsec{0}{24}/hour in latitude,
+        40~km and 0.29~m/s in distance.
+  \item The original algorithm is expressed in terms of the obsolete
+        timescale {\it Ephemeris Time}.  Either TDB or TT can be used,
+        but not UT without incurring significant errors (\arcseci{30} at
+        the present time) due to the Moon's \arcsec{0}{5}/s movement.
+  \item 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.
+  \item Velocity is obtained by a complete analytical differentiation
+        of the Meeus model.
+ \end{enumerate}
+}
+\aref{Meeus, {\it l'Astronomie}, June 1984, p348.}
+%-----------------------------------------------------------------------
+\routine{SLA\_DMXM}{Multiply $3\times3$ Matrices}
+{
+ \action{Product of two $3\times3$ matrices (double precision).}
+ \call{CALL sla\_DMXM (A, B, C)}
+}
+\args{GIVEN}
+{
+ \spec{A}{D(3,3)}{matrix {\bf A}} \\
+ \spec{B}{D(3,3)}{matrix {\bf B}}
+}
+\args{RETURNED}
+{
+ \spec{C}{D(3,3)}{matrix result: {\bf A}$\times${\bf B}}
+}
+\anote{To comply with the ANSI Fortran 77 standard, A, B and C must
+       be different arrays.  The routine is, in fact, coded
+       so as to work properly on the VAX and many other systems even
+       if this rule is violated, something that is {\bf not}, however,
+       recommended.}
+%-----------------------------------------------------------------------
+\routine{SLA\_DMXV}{Apply 3D Rotation}
+{
+ \action{Multiply a 3-vector by a rotation matrix (double precision).}
+ \call{CALL sla\_DMXV (DM, VA, VB)}
+}
+\args{GIVEN}
+{
+ \spec{DM}{D(3,3)}{rotation matrix} \\
+ \spec{VA}{D(3)}{vector to be rotated}
+}
+\args{RETURNED}
+{
+ \spec{VB}{D(3)}{result vector}
+}
+\notes
+{
+ \begin{enumerate}
+  \item This routine performs the operation:
+        \begin{verse}
+           {\bf b} = {\bf M}$\cdot${\bf a}
+        \end{verse}
+        where {\bf a} and {\bf b} are the 3-vectors VA and VB
+        respectively, and {\bf M} is the $3\times3$ matrix DM.
+  \item The main function of this routine is apply a
+        rotation;  under these circumstances, {\bf M} is a
+        {\it proper real orthogonal}\/ matrix.
+  \item To comply with the ANSI Fortran 77 standard, VA and VB must
+        {\bf not} be the same array.  The routine is, in fact, coded
+        so as to work properly on the VAX and many other systems even
+        if this rule is violated, something that is {\bf not}, however,
+        recommended.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DPAV}{Position-Angle Between Two Directions}
+{
+ \action{Returns the bearing (position angle) of one celestial
+         direction with respect to another (double precision).}
+ \call{D~=~sla\_DPAV (V1, V2)}
+}
+\args{GIVEN}
+{
+ \spec{V1}{D(3)}{direction cosines of one point} \\
+ \spec{V2}{D(3)}{directions cosines of the other point}
+}
+\args{RETURNED}
+{
+ \spec{sla\_DPAV}{D}{position-angle of 2nd point with respect to 1st}
+}
+\notes
+{
+ \begin{enumerate}
+ \item The coordinate frames correspond to \radec,
+       $[\lambda,\phi]$ {\it etc.}.
+ \item The result is the bearing (position angle), in radians,
+       of point V2 as seen
+       from point V1.  It is in the range $\pm \pi$.  The sense
+       is such that if V2
+       is a small distance due east of V1 the result
+       is about $+\pi/2$. Zero is returned
+       if the two points are coincident.
+ \item The routine sla\_DBEAR performs an equivalent function except
+       that the points are specified in the form of spherical coordinates.
+ \end{enumerate}
+}
+%------------------------------------------------------------------------------
+\routine{SLA\_DR2AF}{Radians to Deg,Min,Sec,Frac}
+{
+ \action{Convert an angle in radians to degrees, arcminutes, arcseconds,
+         fraction (double precision).}
+ \call{CALL sla\_DR2AF (NDP, ANGLE, SIGN, IDMSF)}
+}
+\args{GIVEN}
+{
+ \spec{NDP}{I}{number of decimal places of arcseconds} \\
+ \spec{ANGLE}{D}{angle in radians}
+}
+\args{RETURNED}
+{
+ \spec{SIGN}{C}{`+' or `$-$'} \\
+ \spec{IDMSF}{I(4)}{degrees, arcminutes, arcseconds, fraction}
+}
+\notes
+{
+ \begin{enumerate}
+  \item NDP less than zero is interpreted as zero.
+  \item The largest useful value for NDP is determined by the size
+        of ANGLE, the format of DOUBLE~PRECISION floating-point numbers
+        on the target machine, and the risk of overflowing IDMSF(4).
+        For example, on a VAX computer, for ANGLE up to $2\pi$, the available
+        floating-point precision corresponds roughly to NDP=12.  However,
+        the practical limit is NDP=9, set by the capacity of the 32-bit
+        integer IDMSF(4).
+  \item The absolute value of ANGLE may exceed $2\pi$.  In cases where it
+        does not, it is up to the caller to test for and handle the
+        case where ANGLE is very nearly $2\pi$ and rounds up to $360^{\circ}$,
+        by testing for IDMSF(1)=360 and setting IDMSF(1-4) to zero.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DR2TF}{Radians to Hour,Min,Sec,Frac}
+{
+ \action{Convert an angle in radians to hours, minutes, seconds,
+         fraction (double precision).}
+ \call{CALL sla\_DR2TF (NDP, ANGLE, SIGN, IHMSF)}
+}
+\args{GIVEN}
+{
+ \spec{NDP}{I}{number of decimal places of seconds} \\
+ \spec{ANGLE}{D}{angle in radians}
+}
+\args{RETURNED}
+{
+ \spec{SIGN}{C}{`+' or `$-$'} \\
+ \spec{IHMSF}{I(4)}{hours, minutes, seconds, fraction}
+}
+\notes
+{
+ \begin{enumerate}
+  \item NDP less than zero is interpreted as zero.
+  \item The largest useful value for NDP is determined by the size
+        of ANGLE, the format of DOUBLE PRECISION floating-point numbers
+        on the target machine, and the risk of overflowing IHMSF(4).
+        For example, on a VAX computer, for ANGLE up to $2\pi$, the available
+        floating-point precision corresponds roughly to NDP=12.  However,
+        the practical limit is NDP=9, set by the capacity of the 32-bit
+        integer IHMSF(4).
+  \item The absolute value of ANGLE may exceed $2\pi$.  In cases where it
+        does not, it is up to the caller to test for and handle the
+        case where ANGLE is very nearly $2\pi$ and rounds up to 24~hours,
+        by testing for IHMSF(1)=24 and setting IHMSF(1-4) to zero.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DRANGE}{Put Angle into Range $\pm\pi$}
+{
+ \action{Normalize an angle into the range $\pm\pi$ (double precision).}
+ \call{D~=~sla\_DRANGE (ANGLE)}
+}
+\args{GIVEN}
+{
+ \spec{ANGLE}{D}{angle in radians}
+}
+\args{RETURNED}
+{
+ \spec{sla\_DRANGE}{D}{ANGLE expressed in the range $\pm\pi$.}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DRANRM}{Put Angle into Range $0\!-\!2\pi$}
+{
+ \action{Normalize an angle into the range $0\!-\!2\pi$
+         (double precision).}
+ \call{D~=~sla\_DRANRM (ANGLE)}
+}
+\args{GIVEN}
+{
+ \spec{ANGLE}{D}{angle in radians}
+}
+\args{RETURNED}
+{
+ \spec{sla\_DRANRM}{D}{ANGLE expressed in the range $0\!-\!2\pi$}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DS2C6}{Spherical Pos/Vel to Cartesian}
+{
+ \action{Conversion of position \& velocity in spherical coordinates
+         to Cartesian coordinates (double precision).}
+ \call{CALL sla\_DS2C6 (A, B, R, AD, BD, RD, V)}
+}
+\args{GIVEN}
+{
+ \spec{A}{D}{longitude (radians) -- for example $\alpha$} \\
+ \spec{B}{D}{latitude (radians) -- for example $\delta$} \\
+ \spec{R}{D}{radial coordinate} \\
+ \spec{AD}{D}{longitude derivative (radians per unit time)} \\
+ \spec{BD}{D}{latitude derivative (radians per unit time)} \\
+ \spec{RD}{D}{radial derivative}
+}
+\args{RETURNED}
+{
+ \spec{V}{D(6)}{\xyzxyzd}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DS2TP}{Spherical to Tangent Plane}
+{
+ \action{Projection of spherical coordinates onto the tangent plane
+         (double precision).}
+ \call{CALL sla\_DS2TP (RA, DEC, RAZ, DECZ, XI, ETA, J)}
+}
+\args{GIVEN}
+{
+ \spec{RA,DEC}{D}{spherical coordinates of star (radians)} \\
+ \spec{RAZ,DECZ}{D}{spherical coordinates of tangent point (radians)}
+}
+\args{RETURNED}
+{
+ \spec{XI,ETA}{D}{tangent plane coordinates (radians)} \\
+ \spec{J}{I}{status:} \\
+ \spec{}{}{\hspace{1.5em} 0 = OK, star on tangent plane} \\
+ \spec{}{}{\hspace{1.5em} 1 = error, star too far from axis} \\
+ \spec{}{}{\hspace{1.5em} 2 = error, antistar on tangent plane} \\
+ \spec{}{}{\hspace{1.5em} 3 = error, antistar too far from axis}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The projection is called the {\it gnomonic}\/ projection;  the
+        Cartesian coordinates \xieta\ are called 
+        {\it standard coordinates.}\/  The latter
+        are in units of the distance from the tangent plane to the projection
+        point, {\it i.e.}\ radians near the origin.
+  \item When working in \xyz\ rather than spherical coordinates, the
+        equivalent Cartesian routine sla\_DV2TP is available.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DSEP}{Angle Between 2 Points on Sphere}
+{
+ \action{Angle between two points on a sphere (double precision).}
+ \call{D~=~sla\_DSEP (A1, B1, A2, B2)}
+}
+\args{GIVEN}
+{
+ \spec{A1,B1}{D}{spherical coordinates of one point (radians)} \\
+ \spec{A2,B2}{D}{spherical coordinates of the other point (radians)}
+}
+\args{RETURNED}
+{
+ \spec{sla\_DSEP}{D}{angle between [A1,B1] and [A2,B2] in radians}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The spherical coordinates are right ascension and declination,
+        longitude and latitude, {\it etc.}, in radians.
+  \item The result is always positive.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DT}{Approximate ET minus UT}
+{
+ \action{Estimate $\Delta$T, the offset between dynamical time
+         and Universal Time, for a given historical epoch.}
+ \call{D~=~sla\_DT (EPOCH)}
+}
+\args{GIVEN}
+{
+ \spec{EPOCH}{D}{(Julian) epoch ({\it e.g.}\ 1850D0)}
+}
+\args{RETURNED}
+{
+ \spec{sla\_DT}{D}{approximate ET$-$UT (after 1984, TT$-$UT1) in seconds}
+}
+\notes
+{
+ \begin{enumerate}
+  \item Depending on the epoch, one of three parabolic approximations
+        is used:
+\begin{tabbing}
+xx \= xxxxxxxxxxxxxxxxxx \= \kill
+\> before AD 979 \> Stephenson \& Morrison's 390 BC to AD 948 model \\
+\> AD 979 to AD 1708 \> Stephenson \& Morrison's AD 948 to AD 1600 model \\
+\> after AD 1708 \> McCarthy \& Babcock's post-1650 model
+\end{tabbing}
+        The breakpoints are chosen to ensure continuity:  they occur
+        at places where the adjacent models give the same answer as
+        each other.
+  \item The accuracy is modest, with errors of up to $20^{\rm s}$ during
+        the interval since 1650, rising to perhaps $30^{\rm m}$
+        by 1000~BC.  Comparatively accurate values from AD~1600
+        are tabulated in
+        the {\it Astronomical Almanac}\/ (see section K8 of the 1995
+        edition).
+  \item The use of {\tt DOUBLE PRECISION} for both argument and result is
+        simply for compatibility with other SLALIB time routines.
+  \item The models used are based on a lunar tidal acceleration value
+        of \arcsec{-26}{00} per century.
+ \end{enumerate}
+}
+\aref{Seidelmann, P.K.\ (ed), 1992.  {\it Explanatory
+      Supplement to the Astronomical Almanac,}\/ ISBN~0-935702-68-7.
+      This contains references to the papers by Stephenson \& Morrison
+      and by McCarthy \& Babcock which describe the models used here.}
+%-----------------------------------------------------------------------
+\routine{SLA\_DTF2D}{Hour,Min,Sec to Days}
+{
+ \action{Convert hours, minutes, seconds to days (double precision).}
+ \call{CALL sla\_DTF2D (IHOUR, IMIN, SEC, DAYS, J)}
+}
+\args{GIVEN}
+{
+ \spec{IHOUR}{I}{hours} \\
+ \spec{IMIN}{I}{minutes} \\
+ \spec{SEC}{D}{seconds}
+}
+\args{RETURNED}
+{
+ \spec{DAYS}{D}{interval in days} \\
+ \spec{J}{I}{status:} \\
+ \spec{}{}{\hspace{1.5em} 0 = OK} \\
+ \spec{}{}{\hspace{1.5em} 1 = IHOUR outside range 0-23} \\
+ \spec{}{}{\hspace{1.5em} 2 = IMIN outside range 0-59} \\
+ \spec{}{}{\hspace{1.5em} 3 = SEC outside range 0-59.999$\cdots$}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The result is computed even if any of the range checks fail.
+  \item The sign must be dealt with outside this routine.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DTF2R}{Hour,Min,Sec to Radians}
+{
+ \action{Convert hours, minutes, seconds to radians (double precision).}
+ \call{CALL sla\_DTF2R (IHOUR, IMIN, SEC, RAD, J)}
+}
+\args{GIVEN}
+{
+ \spec{IHOUR}{I}{hours} \\
+ \spec{IMIN}{I}{minutes} \\
+ \spec{SEC}{D}{seconds}
+}
+\args{RETURNED}
+{
+ \spec{RAD}{D}{angle in radians} \\
+ \spec{J}{I}{status:} \\
+ \spec{}{}{\hspace{1.5em} 0 = OK} \\
+ \spec{}{}{\hspace{1.5em} 1 = IHOUR outside range 0-23} \\
+ \spec{}{}{\hspace{1.5em} 2 = IMIN outside range 0-59} \\
+ \spec{}{}{\hspace{1.5em} 3 = SEC outside range 0-59.999$\cdots$}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The result is computed even if any of the range checks fail.
+  \item The sign must be dealt with outside this routine.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DTP2S}{Tangent Plane to Spherical}
+{
+ \action{Transform tangent plane coordinates into spherical
+         coordinates (double precision)}
+ \call{CALL sla\_DTP2S (XI, ETA, RAZ, DECZ, RA, DEC)}
+}
+\args{GIVEN}
+{
+ \spec{XI,ETA}{D}{tangent plane rectangular coordinates (radians)} \\
+ \spec{RAZ,DECZ}{D}{spherical coordinates of tangent point (radians)}
+}
+\args{RETURNED}
+{
+ \spec{RA,DEC}{D}{spherical coordinates (radians)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The projection is called the {\it gnomonic}\/ projection;  the
+        Cartesian coordinates \xieta\ are called 
+        {\it standard coordinates.}\/  The latter
+        are in units of the distance from the tangent plane to the projection
+        point, {\it i.e.}\ radians near the origin.
+  \item When working in \xyz\ rather than spherical coordinates, the
+        equivalent Cartesian routine sla\_DTP2V is available.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DTP2V}{Tangent Plane to Direction Cosines}
+{
+ \action{Given the tangent-plane coordinates of a star and the direction
+         cosines of the tangent point, determine the direction cosines
+         of the star
+         (double precision).}
+ \call{CALL sla\_DTP2V (XI, ETA, V0, V)}
+}
+\args{GIVEN}
+{
+ \spec{XI,ETA}{D}{tangent plane coordinates of star (radians)} \\
+ \spec{V0}{D(3)}{direction cosines of tangent point}
+}
+\args{RETURNED}
+{
+ \spec{V}{D(3)}{direction cosines of star}
+}
+\notes
+{
+ \begin{enumerate}
+  \item If vector V0 is not of unit length, the returned vector V will
+        be wrong.
+  \item If vector V0 points at a pole, the returned vector V will be
+        based on the arbitrary assumption that $\alpha=0$ at
+        the tangent point.
+  \item The projection is called the {\it gnomonic}\/ projection;  the
+        Cartesian coordinates \xieta\ are called 
+        {\it standard coordinates.}\/  The latter
+        are in units of the distance from the tangent plane to the projection
+        point, {\it i.e.}\ radians near the origin.
+  \item This routine is the Cartesian equivalent of the routine sla\_DTP2S.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DTPS2C}{Plate centre from $\xi,\eta$ and $\alpha,\delta$}
+{
+ \action{From the tangent plane coordinates of a star of known \radec,
+        determine the \radec\ of the tangent point (double precision)}
+ \call{CALL sla\_DTPS2C (XI, ETA, RA, DEC, RAZ1, DECZ1, RAZ2, DECZ2, N)}
+}
+\args{GIVEN}
+{
+ \spec{XI,ETA}{D}{tangent plane rectangular coordinates (radians)} \\
+ \spec{RA,DEC}{D}{spherical coordinates (radians)}
+}
+\args{RETURNED}
+{
+ \spec{RAZ1,DECZ1}{D}{spherical coordinates of tangent point,
+                      solution 1} \\
+ \spec{RAZ2,DECZ2}{D}{spherical coordinates of tangent point,
+                      solution 2} \\
+ \spec{N}{I}{number of solutions:} \\
+ \spec{}{}{\hspace{1em} 0 = no solutions returned  (note 2)} \\
+ \spec{}{}{\hspace{1em} 1 = only the first solution is useful (note 3)} \\
+ \spec{}{}{\hspace{1em} 2 = there are two useful solutions (note 3)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The RAZ1 and RAZ2 values returned are in the range $0\!-\!2\pi$.
+  \item 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 $\delta$.
+  \item 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.
+  \item The DECZ1 and DECZ2 values returned are in the range $\pm\pi$,
+        but in the ordinary, non-pole-crossing, case, the range is
+        $\pm\pi/2$.
+  \item RA, DEC, RAZ1, DECZ1, RAZ2, DECZ2 are all in radians.
+  \item The projection is called the {\it gnomonic}\/ projection;  the
+        Cartesian coordinates \xieta\ are called 
+        {\it standard coordinates.}\/  The latter
+        are in units of the distance from the tangent plane to the projection
+        point, {\it i.e.}\ radians near the origin.
+  \item When working in \xyz\ rather than spherical coordinates, the
+        equivalent Cartesian routine sla\_DTPV2C is available.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DTPV2C}{Plate centre from $\xi,\eta$ and $x,y,z$}
+{
+ \action{From the tangent plane coordinates of a star of known
+         direction cosines, determine the direction cosines
+         of the tangent point (double precision)}
+ \call{CALL sla\_DTPV2C (XI, ETA, V, V01, V02, N)}
+}
+\args{GIVEN}
+{
+ \spec{XI,ETA}{D}{tangent plane coordinates of star (radians)} \\
+ \spec{V}{D(3)}{direction cosines of star}
+}
+\args{RETURNED}
+{
+ \spec{V01}{D(3)}{direction cosines of tangent point, solution 1} \\
+ \spec{V01}{D(3)}{direction cosines of tangent point, solution 2} \\
+ \spec{N}{I}{number of solutions:} \\
+ \spec{}{}{\hspace{1em} 0 = no solutions returned  (note 2)} \\
+ \spec{}{}{\hspace{1em} 1 = only the first solution is useful (note 3)} \\
+ \spec{}{}{\hspace{1em} 2 = there are two useful solutions (note 3)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The vector V must be of unit length or the result will be wrong.
+  \item 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.
+  \item 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 can be regarded as valid if
+        the vector V02 is interpreted as the ``over-the-pole'' case.
+  \item The projection is called the {\it gnomonic}\/ projection;  the
+        Cartesian coordinates \xieta\ are called 
+        {\it standard coordinates.}\/  The latter
+        are in units of the distance from the tangent plane to the projection
+        point, {\it i.e.}\ radians near the origin.
+  \item This routine is the Cartesian equivalent of the routine sla\_DTPS2C.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DTT}{TT minus UTC}
+{
+ \action{Compute $\Delta$TT, the increment to be applied to
+         Coordinated Universal Time UTC to give
+         Terrestrial Time TT.}
+ \call{D~=~sla\_DTT (DJU)}
+}
+\args{GIVEN}
+{
+ \spec{DJU}{D}{UTC date as a modified JD (JD$-$2400000.5)}
+}
+\args{RETURNED}
+{
+ \spec{sla\_DTT}{D}{TT$-$UTC in seconds}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The UTC is specified to be a date rather than a time to indicate
+        that care needs to be taken not to specify an instant which lies
+        within a leap second.  Though in most cases UTC can include the
+        fractional part, correct behaviour on the day of a leap second
+        can be guaranteed only up to the end of the second
+        $23^{\rm h}\,59^{\rm m}\,59^{\rm s}$.
+  \item Pre 1972 January 1 a fixed value of 10 + ET$-$TAI is returned.
+  \item TT is one interpretation of the defunct timescale
+        {\it Ephemeris Time}, ET.
+  \item See also the routine sla\_DT, which roughly estimates ET$-$UT for
+        historical epochs.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DV2TP}{Direction Cosines to Tangent Plane}
+{
+ \action{Given the direction cosines of a star and of the tangent point,
+         determine the star's tangent-plane coordinates
+         (double precision).}
+ \call{CALL sla\_DV2TP (V, V0, XI, ETA, J)}
+}
+\args{GIVEN}
+{
+ \spec{V}{D(3)}{direction cosines of star} \\
+ \spec{V0}{D(3)}{direction cosines of tangent point}
+}
+\args{RETURNED}
+{
+ \spec{XI,ETA}{D}{tangent plane coordinates (radians)} \\
+ \spec{J}{I}{status:} \\
+ \spec{}{}{\hspace{1.5em} 0 = OK, star on tangent plane} \\
+ \spec{}{}{\hspace{1.5em} 1 = error, star too far from axis} \\
+ \spec{}{}{\hspace{1.5em} 2 = error, antistar on tangent plane} \\
+ \spec{}{}{\hspace{1.5em} 3 = error, antistar too far from axis}
+}
+\notes
+{
+ \begin{enumerate}
+  \item If vector V0 is not of unit length, or if vector V is of zero
+        length, the results will be wrong.
+  \item If V0 points at a pole, the returned $\xi,\eta$
+        will be based on the
+        arbitrary assumption that $\alpha=0$ at the tangent point.
+  \item The projection is called the {\it gnomonic}\/ projection;  the
+        Cartesian coordinates \xieta\ are called 
+        {\it standard coordinates.}\/  The latter
+        are in units of the distance from the tangent plane to the projection
+        point, {\it i.e.}\ radians near the origin.
+  \item This routine is the Cartesian equivalent of the routine sla\_DS2TP.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DVDV}{Scalar Product}
+{
+ \action{Scalar product of two 3-vectors (double precision).}
+ \call{D~=~sla\_DVDV (VA, VB)}
+}
+\args{GIVEN}
+{
+ \spec{VA}{D(3)}{first vector} \\
+ \spec{VB}{D(3)}{second vector}
+}
+\args{RETURNED}
+{
+ \spec{sla\_DVDV}{D}{scalar product VA.VB}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_DVN}{Normalize Vector}
+{
+ \action{Normalize a 3-vector, also giving the modulus (double precision).}
+ \call{CALL sla\_DVN (V, UV, VM)}
+}
+\args{GIVEN}
+{
+ \spec{V}{D(3)}{vector}
+}
+\args{RETURNED}
+{
+ \spec{UV}{D(3)}{unit vector in direction of V} \\
+ \spec{VM}{D}{modulus of V}
+}
+\anote{If the modulus of V is zero, UV is set to zero as well.}
+%-----------------------------------------------------------------------
+\routine{SLA\_DVXV}{Vector Product}
+{
+ \action{Vector product of two 3-vectors (double precision).}
+ \call{CALL sla\_DVXV (VA, VB, VC)}
+}
+\args{GIVEN}
+{
+ \spec{VA}{D(3)}{first vector} \\
+ \spec{VB}{D(3)}{second vector}
+}
+\args{RETURNED}
+{
+ \spec{VC}{D(3)}{vector product VA$\times$VB}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_E2H}{$h,\delta$ to Az,El}
+{
+ \action{Equatorial to horizon coordinates
+         (single precision).}
+ \call{CALL sla\_DE2H (HA, DEC, PHI, AZ, EL)}
+}
+\args{GIVEN}
+{
+ \spec{HA}{R}{hour angle (radians)} \\
+ \spec{DEC}{R}{declination (radians)} \\
+ \spec{PHI}{R}{latitude (radians)}
+}
+\args{RETURNED}
+{
+ \spec{AZ}{R}{azimuth (radians)} \\
+ \spec{EL}{R}{elevation (radians)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item Azimuth is returned in the range $0\!-\!2\pi$;  north is zero,
+        and east is $+\pi/2$.  Elevation is returned in the range
+        $\pm\pi$.
+  \item The latitude must be geodetic.  In critical applications,
+        corrections for polar motion should be applied.
+  \item 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 {\it observed} \hadec, and the elevation
+        {\it in vacuo}, which would require the {\it topocentric}
+        \hadec.
+        If the effects of diurnal aberration can be neglected, the
+        {\it apparent} \hadec\ may be used instead of the topocentric
+        \hadec.
+  \item No range checking of arguments is carried out.
+  \item 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.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_EARTH}{Approx Earth Pos/Vel}
+{
+ \action{Approximate heliocentric position and velocity of the Earth
+         (single precision).}
+ \call{CALL sla\_EARTH (IY, ID, FD, PV)}
+}
+\args{GIVEN}
+{
+ \spec{IY}{I}{year} \\
+ \spec{ID}{I}{day in year (1 = Jan 1st)} \\
+ \spec{FD}{R}{fraction of day}
+}
+\args{RETURNED}
+{
+ \spec{PV}{R(6)}{Earth \xyzxyzd\ (AU, AU~s$^{-1}$)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The date and time is TDB (loosely ET) in a Julian calendar
+        which has been aligned to the ordinary Gregorian
+        calendar for the interval 1900~March~1 to 2100~February~28.
+        The year and day can be obtained by calling sla\_CALYD or
+        sla\_CLYD.
+  \item The Earth heliocentric 6-vector is referred to the
+        FK4 mean equator and equinox of date.
+  \item Maximum/RMS errors 1950-2050:
+        \begin{itemize}
+         \item 13/5~$\times10^{-5}$~AU = 19200/7600~km in position
+         \item 47/26~$\times10^{-10}$~AU~s$^{-1}$ =
+               0.0070/0.0039~km~s$^{-1}$ in speed
+        \end{itemize}
+  \item More accurate results are obtainable with the routine sla\_EVP.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_ECLEQ}{Ecliptic to Equatorial}
+{
+ \action{Transformation from ecliptic longitude and latitude to
+         J2000.0 \radec.}
+ \call{CALL sla\_ECLEQ (DL, DB, DATE, DR, DD)}
+}
+\args{GIVEN}
+{
+ \spec{DL,DB}{D}{ecliptic longitude and latitude
+                          (mean of date, IAU 1980 theory, radians)} \\
+ \spec{DATE}{D}{TDB (formerly ET) as Modified Julian Date
+                                             (JD$-$2400000.5)}
+}
+\args{RETURNED}
+{
+ \spec{DR,DD}{D}{J2000.0 mean \radec\ (radians)}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_ECMAT}{Form $\alpha,\delta\rightarrow\lambda,\beta$ Matrix}
+{
+ \action{Form the equatorial to ecliptic rotation matrix (IAU 1980 theory).}
+ \call{CALL sla\_ECMAT (DATE, RMAT)}
+}
+\args{GIVEN}
+{
+ \spec{DATE}{D}{TDB (formerly ET) as Modified Julian Date
+                                           (JD$-$2400000.5)}
+}
+\args{RETURNED}
+{
+ \spec{RMAT}{D(3,3)}{rotation matrix}
+}
+\notes
+{
+ \begin{enumerate}
+  \item RMAT is matrix {\bf M} in the expression
+        {\bf v}$_{ecl}$~=~{\bf M}$\cdot${\bf v}$_{equ}$.
+  \item The equator, equinox and ecliptic are mean of date.
+ \end{enumerate}
+}
+\aref{Murray, C.A., {\it Vectorial Astrometry}, section 4.3.}
+%-----------------------------------------------------------------------
+\routine{SLA\_ECOR}{RV \& Time Corrns to Sun}
+{
+ \action{Component of Earth orbit velocity and heliocentric
+         light time in a given direction.}
+ \call{CALL sla\_ECOR (RM, DM, IY, ID, FD, RV, TL)}
+}
+\args{GIVEN}
+{
+ \spec{RM,DM}{R}{mean \radec\ of date (radians)} \\
+ \spec{IY}{I}{year} \\
+ \spec{ID}{I}{day in year (1 = Jan 1st)} \\
+ \spec{FD}{R}{fraction of day}
+}
+\args{RETURNED}
+{
+ \spec{RV}{R}{component of Earth orbital velocity (km~s$^{-1}$)} \\
+ \spec{TL}{R}{component of heliocentric light time (s)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The date and time is TDB (loosely ET) in a Julian calendar
+        which has been aligned to the ordinary Gregorian
+        calendar for the interval 1900 March 1 to 2100 February 28.
+        The year and day can be obtained by calling sla\_CALYD or
+        sla\_CLYD.
+  \item Sign convention:
+        \begin{itemize}
+         \item The velocity component is +ve when the
+               Earth is receding from
+               the given point on the sky.
+         \item The light time component is +ve
+               when the Earth lies between the Sun and
+               the given point on the sky.
+        \end{itemize}
+ \item Accuracy:
+       \begin{itemize}
+        \item The velocity component is usually within 0.004~km~s$^{-1}$
+              of the correct value and is never in error by more than
+              0.007~km~s$^{-1}$.
+        \item The error in light time correction is about
+              \tsec{0}{03} at worst,
+              but is usually better than \tsec{0}{01}.
+       \end{itemize}
+       For applications requiring higher accuracy, see the sla\_EVP routine.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_EG50}{B1950 $\alpha,\delta$ to Galactic}
+{
+ \action{Transformation from B1950.0 FK4 equatorial coordinates to
+         IAU 1958 galactic coordinates.}
+ \call{CALL sla\_EG50 (DR, DD, DL, DB)}
+}
+\args{GIVEN}
+{
+ \spec{DR,DD}{D}{B1950.0 \radec\ (radians)}
+}
+\args{RETURNED}
+{
+ \spec{DL,DB}{D}{galactic longitude and latitude \gal\ (radians)}
+}
+\anote{The equatorial coordinates are B1950.0 FK4.  Use the
+       routine sla\_EQGAL if conversion from J2000.0 FK5 coordinates
+       is required.}
+\aref{Blaauw {\it et al.}, 1960, {\it Mon.Not.R.astr.Soc.},
+      {\bf 121}, 123.}
+%-----------------------------------------------------------------------
+\routine{SLA\_EL2UE}{Conventional to Universal Elements}
+{
+ \action{Transform conventional osculating orbital elements
+         into ``universal'' form.}
+ \call{CALL sla\_EL2UE (\vtop{
+         \hbox{DATE, JFORM, EPOCH, ORBINC, ANODE,}
+         \hbox{PERIH, AORQ, E, AORL, DM,}
+         \hbox{U, JSTAT)}}}
+}
+\args{GIVEN}
+{
+ \spec{DATE}{D}{epoch (TT MJD) of osculation (Note~3)} \\
+ \spec{JFORM}{I}{choice of element set (1-3; Note~6)} \\
+ \spec{EPOCH}{D}{epoch of elements ($t_0$ or $T$, TT MJD)} \\
+ \spec{ORBINC}{D}{inclination ($i$, radians)} \\
+ \spec{ANODE}{D}{longitude of the ascending node ($\Omega$, radians)} \\
+ \spec{PERIH}{D}{longitude or argument of perihelion
+                            ($\varpi$ or $\omega$,} \\
+ \spec{}{}{\hspace{1.5em} radians)} \\
+ \spec{AORQ}{D}{mean distance or perihelion distance ($a$ or $q$, AU)} \\
+ \spec{E}{D}{eccentricity ($e$)} \\
+ \spec{AORL}{D}{mean anomaly or longitude
+                               ($M$ or $L$, radians,} \\
+ \spec{}{}{\hspace{1.5em} JFORM=1,2 only)} \\
+ \spec{DM}{D}{daily motion ($n$, radians, JFORM=1 only)}
+}
+\args{RETURNED}
+{
+ \spec{U}{D(13)}{universal orbital elements (Note~1)} \\
+ \specel {(1)}     {combined mass ($M+m$)} \\
+ \specel {(2)}     {total energy of the orbit ($\alpha$)} \\
+ \specel {(3)}     {reference (osculating) epoch ($t_0$)} \\
+ \specel {(4-6)}   {position at reference epoch (${\rm \bf r}_0$)} \\
+ \specel {(7-9)}   {velocity at reference epoch (${\rm \bf v}_0$)} \\
+ \specel {(10)}    {heliocentric distance at reference epoch} \\
+ \specel {(11)}    {${\rm \bf r}_0.{\rm \bf v}_0$} \\
+ \specel {(12)}    {date ($t$)} \\
+ \specel {(13)}    {universal eccentric anomaly ($\psi$) of date,
+                    approx} \\ \\
+ \spec{JSTAT}{I}{status:} \\
+ \spec{}{}{\hspace{1.95em}       0 = OK} \\
+ \spec{}{}{\hspace{1.2em}  $-$1 = illegal JFORM} \\
+ \spec{}{}{\hspace{1.2em}   $-$2 = illegal E} \\
+ \spec{}{}{\hspace{1.2em}   $-$3 = illegal AORQ} \\
+ \spec{}{}{\hspace{1.2em}   $-$4 = illegal DM} \\
+ \spec{}{}{\hspace{1.2em}   $-$5 = numerical error}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The ``universal'' elements are those which define the orbit for
+        the purposes of the method of universal variables (see reference).
+        They consist of the combined mass of the two bodies, an epoch,
+        and the position and velocity vectors (arbitrary reference frame)
+        at that epoch.  The parameter set used here includes also various
+        quantities that can, in fact, be derived from the other
+        information.  This approach is taken to avoiding unnecessary
+        computation and loss of accuracy.  The supplementary quantities
+        are (i)~$\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.
+  \item The companion routine is sla\_UE2PV.  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 sla\_UE2PV;
+        for convenience, the two calls are packaged as the routine
+        sla\_PLANEL.  Multiple predictions may be made by again calling the
+        present routine once, but then calling sla\_UE2PV multiple times,
+        which is faster than multiple calls to sla\_PLANEL.
+  \item 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).
+  \item 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.
+  \item The universal elements returned in the array U are in canonical
+        units (solar masses, AU and canonical days).
+  \item Three different element-format options are supported, as
+        follows. \\
+
+        JFORM=1, suitable for the major planets:
+
+        \begin{tabbing}
+        xxx \= xxxxxxxx \= xx \= \kill
+        \> EPOCH  \> = \> epoch of elements $t_0$ (TT MJD) \\
+        \> ORBINC \> = \> inclination $i$ (radians) \\
+        \> ANODE  \> = \> longitude of the ascending node $\Omega$ (radians) \\
+        \> PERIH  \> = \> longitude of perihelion $\varpi$ (radians) \\
+        \> AORQ   \> = \> mean distance $a$ (AU) \\
+        \> E      \> = \> eccentricity $e$ $( 0 \leq e < 1 )$ \\
+        \> AORL   \> = \> mean longitude $L$ (radians) \\
+        \> DM     \> = \> daily motion $n$ (radians)
+        \end{tabbing}
+
+        JFORM=2, suitable for minor planets:
+
+        \begin{tabbing}
+        xxx \= xxxxxxxx \= xx \= \kill
+        \> EPOCH  \> = \> epoch of elements $t_0$ (TT MJD) \\
+        \> ORBINC \> = \> inclination $i$ (radians) \\
+        \> ANODE  \> = \> longitude of the ascending node $\Omega$ (radians) \\
+        \> PERIH  \> = \> argument of perihelion $\omega$ (radians) \\
+        \> AORQ   \> = \> mean distance $a$ (AU) \\
+        \> E      \> = \> eccentricity $e$ $( 0 \leq e < 1 )$ \\
+        \> AORL   \> = \> mean anomaly $M$ (radians)
+        \end{tabbing}
+
+        JFORM=3, suitable for comets:
+
+        \begin{tabbing}
+        xxx \= xxxxxxxx \= xx \= \kill
+        \> EPOCH  \> = \> epoch of perihelion $T$ (TT MJD) \\
+        \> ORBINC \> = \> inclination $i$ (radians) \\
+        \> ANODE  \> = \> longitude of the ascending node $\Omega$ (radians) \\
+        \> PERIH  \> = \> argument of perihelion $\omega$ (radians) \\
+        \> AORQ   \> = \> perihelion distance $q$ (AU) \\
+        \> E      \> = \> eccentricity $e$ $( 0 \leq e \leq 10 )$
+        \end{tabbing}
+  \item Unused elements (DM for JFORM=2, AORL and DM for JFORM=3) are
+        not accessed.
+  \item 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.
+ \end{enumerate}
+}
+\aref{Everhart, E. \& Pitkin, E.T., Am.~J.~Phys.~51, 712, 1983.}
+%------------------------------------------------------------------------------
+\routine{SLA\_EPB}{MJD to Besselian Epoch}
+{
+ \action{Conversion of Modified Julian Date to Besselian Epoch.}
+ \call{D~=~sla\_EPB (DATE)}
+}
+\args{GIVEN}
+{
+ \spec{DATE}{D}{Modified Julian Date (JD$-$2400000.5)}
+}
+\args{RETURNED}
+{
+ \spec{sla\_EPB}{D}{Besselian Epoch}
+}
+\aref{Lieske, J.H., 1979, {\it Astr.Astrophys.}\ {\bf 73}, 282.}
+%-----------------------------------------------------------------------
+\routine{SLA\_EPB2D}{Besselian Epoch to MJD}
+{
+ \action{Conversion of Besselian Epoch to Modified Julian Date.}
+ \call{D~=~sla\_EPB2D (EPB)}
+}
+\args{GIVEN}
+{
+ \spec{EPB}{D}{Besselian Epoch}
+}
+\args{RETURNED}
+{
+ \spec{sla\_EPB2D}{D}{Modified Julian Date (JD$-$2400000.5)}
+}
+\aref{Lieske, J.H., 1979. {\it Astr.Astrophys.}\ {\bf 73}, 282.}
+%-----------------------------------------------------------------------
+\routine{SLA\_EPCO}{Convert Epoch to B or J}
+{
+ \action{Convert an epoch to Besselian or Julian to match another one.}
+ \call{D~=~sla\_EPCO (K0, K, E)}
+
+}
+\args{GIVEN}
+{
+ \spec{K0}{C}{form of result:  `B'=Besselian, `J'=Julian} \\
+ \spec{K}{C}{form of given epoch:  `B' or `J'} \\
+ \spec{E}{D}{epoch}
+}
+\args{RETURNED}
+{
+ \spec{sla\_EPCO}{D}{the given epoch converted as necessary}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The result is always either equal to or very close to
+        the given epoch E.  The routine is required only in
+        applications where punctilious treatment of heterogeneous
+        mixtures of star positions is necessary.
+  \item K0 and K are not validated.  They are interpreted as follows:
+        \begin{itemize}
+         \item If K0 and K are the same, the result is E.
+         \item If K0 is `B' and K isn't, the conversion is J to B.
+         \item In all other cases, the conversion is B to J.
+        \end{itemize}
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_EPJ}{MJD to Julian Epoch}
+{
+ \action{Convert Modified Julian Date to Julian Epoch.}
+ \call{D~=~sla\_EPJ (DATE)}
+}
+\args{GIVEN}
+{
+ \spec{DATE}{D}{Modified Julian Date (JD$-$2400000.5)}
+}
+\args{RETURNED}
+{
+ \spec{sla\_EPJ}{D}{Julian Epoch}
+}
+\aref{Lieske, J.H., 1979.\ {\it Astr.Astrophys.}, {\bf 73}, 282.}
+%-----------------------------------------------------------------------
+\routine{SLA\_EPJ2D}{Julian Epoch to MJD}
+{
+ \action{Convert Julian Epoch to Modified Julian Date.}
+ \call{D~=~sla\_EPJ2D (EPJ)}
+}
+\args{GIVEN}
+{
+ \spec{EPJ}{D}{Julian Epoch}
+}
+\args{RETURNED}
+{
+ \spec{sla\_EPJ2D}{D}{Modified Julian Date (JD$-$2400000.5)}
+}
+\aref{Lieske, J.H., 1979.\ {\it Astr.Astrophys.}, {\bf 73}, 282.}
+%-----------------------------------------------------------------------
+\routine{SLA\_EQECL}{J2000 $\alpha,\delta$ to Ecliptic}
+{
+ \action{Transformation from J2000.0 equatorial coordinates to
+         ecliptic longitude and latitude.}
+ \call{CALL sla\_EQECL (DR, DD, DATE, DL, DB)}
+}
+\args{GIVEN}
+{
+ \spec{DR,DD}{D}{J2000.0 mean \radec\ (radians)} \\
+ \spec{DATE}{D}{TDB (formerly ET) as Modified Julian Date (JD$-$2400000.5)}
+}
+\args{RETURNED}
+{
+ \spec{DL,DB}{D}{ecliptic longitude and latitude
+                        (mean of date, IAU 1980 theory, radians)}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_EQEQX}{Equation of the Equinoxes}
+{
+ \action{Equation of the equinoxes (IAU 1994).}
+ \call{D~=~sla\_EQEQX (DATE)}
+}
+\args{GIVEN}
+{
+ \spec{DATE}{D}{TDB (formerly ET) as Modified Julian Date (JD$-$2400000.5)}
+}
+\args{RETURNED}
+{
+ \spec{sla\_EQEQX}{D}{The equation of the equinoxes (radians)}
+}
+\notes{
+ \begin{enumerate}
+  \item The equation of the equinoxes is defined here as GAST~$-$~GMST:
+        it is added to a {\it mean}\/ sidereal time to give the
+        {\it apparent}\/ sidereal time.
+  \item The change from the classic ``textbook'' expression
+        $\Delta\psi\,cos\,\epsilon$ occurred with IAU Resolution C7,
+        Recommendation~3 (1994).  The new formulation takes into
+        account cross-terms between the various precession and
+        nutation quantities, amounting to about 3~milliarcsec.
+        The transition from the old to the new model officially
+        takes place on 1997 February~27.
+ \end{enumerate}
+}
+\aref{Capitaine, N.\ \& Gontier, A.-M.\ (1993),
+      {\it Astron. Astrophys.},
+      {\bf 275}, 645-650.}
+%-----------------------------------------------------------------------
+\routine{SLA\_EQGAL}{J2000 $\alpha,\delta$ to Galactic}
+{
+ \action{Transformation from J2000.0 FK5 equatorial coordinates to
+ IAU 1958 galactic coordinates.}
+ \call{CALL sla\_EQGAL (DR, DD, DL, DB)}
+}
+\args{GIVEN}
+{
+ \spec{DR,DD}{D}{J2000.0 \radec\ (radians)}
+}
+\args{RETURNED}
+{
+ \spec{DL,DB}{D}{galactic longitude and latitude \gal\ (radians)}
+}
+\anote{The equatorial coordinates are J2000.0 FK5.  Use the routine
+       sla\_EG50 if conversion from B1950.0 FK4 coordinates is required.}
+\aref{Blaauw {\it et al.}, 1960, {\it Mon.Not.R.astr.Soc.},
+      {\bf 121}, 123.}
+%-----------------------------------------------------------------------
+\routine{SLA\_ETRMS}{E-terms of Aberration}
+{
+ \action{Compute the E-terms vector -- the part of the annual
+         aberration which arises from the eccentricity of the
+         Earth's orbit.}
+ \call{CALL sla\_ETRMS (EP, EV)}
+}
+\args{GIVEN}
+{
+ \spec{EP}{D}{Besselian epoch}
+}
+\args{RETURNED}
+{
+ \spec{EV}{D(3)}{E-terms as $[\Delta x, \Delta y, \Delta z\,]$}
+}
+\anote{Note the use of the J2000 aberration constant (\arcsec{20}{49552}).
+       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.}
+\refs
+{
+ \begin{enumerate}
+  \item Smith, C.A.\ {\it et al.}, 1989.  {\it Astr.J.}\ {\bf 97}, 265.
+  \item Yallop, B.D.\ {\it et al.}, 1989.  {\it Astr.J.}\ {\bf 97}, 274.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_EULER}{Rotation Matrix from Euler Angles}
+{
+ \action{Form a rotation matrix from the Euler angles -- three
+         successive rotations about specified Cartesian axes
+         (single precision).}
+ \call{CALL sla\_EULER (ORDER, PHI, THETA, PSI, RMAT)}
+}
+\args{GIVEN}
+{
+ \spec{ORDER}{C*(*)}{specifies about which axes the rotations occur} \\
+ \spec{PHI}{R}{1st rotation (radians)} \\
+ \spec{THETA}{R}{2nd rotation (radians)} \\
+ \spec{PSI}{R}{3rd rotation (radians)}
+}
+\args{RETURNED}
+{
+ \spec{RMAT}{R(3,3)}{rotation matrix}
+}
+\notes
+{
+ \begin{enumerate}
+  \item A rotation is positive when the reference frame rotates
+        anticlockwise as seen looking towards the origin from the
+        positive region of the specified axis.
+  \item 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 {\it z}-axis, followed by THETA radians about the resulting
+        {\it x}-axis,
+        then PSI radians about the resulting {\it z}-axis.  In detail:
+        \begin{itemize}
+         \item 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 {\it xyz} ($\equiv123$)
+               triad is right-handed.  Thus, the `ZXZ' example given above
+               could be written `zxz' or `313' (or even `ZxZ' or `3xZ').
+         \item ORDER is terminated by length or by the first unrecognized
+               character.
+         \item Fewer than three rotations are acceptable, in which case
+               the later angle arguments are ignored.
+        \end{itemize}
+  \item Zero rotations produces a unit RMAT.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_EVP}{Earth Position \& Velocity}
+{
+ \action{Barycentric and heliocentric velocity and position of the Earth.}
+ \call{CALL sla\_EVP (DATE, DEQX, DVB, DPB, DVH, DPH)}
+}
+\args{GIVEN}
+{
+ \spec{DATE}{D}{TDB (formerly ET) as a Modified Julian Date
+                                        (JD$-$2400000.5)} \\
+ \spec{DEQX}{D}{Julian Epoch ({\it e.g.}\ 2000D0) of mean equator and
+                equinox of the vectors returned.  If DEQX~$<0$,
+                  all vectors are referred to the mean equator and
+                  equinox (FK5) of date DATE.}
+}
+\args{RETURNED}
+{
+ \spec{DVB}{D(3)}{barycentric \xyzd, AU~s$^{-1}$} \\
+ \spec{DPB}{D(3)}{barycentric \xyz, AU} \\
+ \spec{DVH}{D(3)}{heliocentric \xyzd, AU~s$^{-1}$} \\
+ \spec{DPH}{D(3)}{heliocentric \xyz, AU}
+}
+\notes
+{
+ \begin{enumerate}
+  \item This routine is used when accuracy is more important
+        than CPU time, yet the extra complication of reading a
+        pre-computed ephemeris is not justified.  The maximum
+        deviations from the JPL~DE96 ephemeris are as follows:
+        \begin{itemize}
+         \item velocity (barycentric or heliocentric): 420~mm~s$^{-1}$
+         \item position (barycentric): 6900~km
+         \item position (heliocentric): 1600~km
+        \end{itemize}
+  \item The routine is an adaption of the BARVEL and BARCOR
+        subroutines of P.Stumpff, which are described in
+        {\it Astr.Astrophys.Suppl.Ser.}\ {\bf 41}, 1-8 (1980).
+        Most of the changes are merely cosmetic and do not affect
+        the results at all.  However, some adjustments have been
+        made so as to give results that refer to the new (IAU 1976
+        `FK5') equinox and precession, although the differences these
+        changes make relative to the results from Stumpff's original
+        `FK4' version are smaller than the inherent accuracy of the
+        algorithm.  One minor shortcoming in the original routines
+        that has {\bf not} been corrected is that slightly better
+        numerical accuracy could be achieved if the various polynomial
+        evaluations were to be so arranged that the smallest terms were
+        computed first.  Note also that one of Stumpff's precession
+        constants differs by \arcsec{0}{001} from the value given in the
+        {\it Explanatory Supplement}.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_FITXY}{Fit Linear Model to Two \xy\ Sets}
+{
+ \action{Fit a linear model to relate two sets of \xy\ coordinates.}
+ \call{CALL sla\_FITXY (ITYPE,NP,XYE,XYM,COEFFS,J)}
+}
+\args{GIVEN}
+{
+ \spec{ITYPE}{I}{type of model: 4 or 6 (note 1)} \\
+ \spec{NP}{I}{number of samples (note 2)} \\
+ \spec{XYE}{D(2,NP)}{expected \xy\ for each sample} \\
+ \spec{XYM}{D(2,NP)}{measured \xy\ for each sample}
+}
+\args{RETURNED}
+{
+ \spec{COEFFS}{D(6)}{coefficients of model (note 3)} \\
+ \spec{J}{I}{status:} \\
+ \spec{}{}{\hspace{1.5em} 0 = OK} \\
+ \spec{}{}{\hspace{0.7em} $-$1 = illegal ITYPE} \\
+ \spec{}{}{\hspace{0.7em} $-$2 = insufficient data} \\
+ \spec{}{}{\hspace{0.7em} $-$3 = singular solution}
+}
+\notes
+{
+ \begin{enumerate}
+  \item ITYPE, which must be either 4 or 6, selects the type of model
+        fitted.  Both allowed ITYPE values produce a model COEFFS which
+        consists of six coefficients, namely the zero points and, for
+        each of XE and YE, the coefficient of XM and YM.  For ITYPE=6,
+        all six coefficients are independent, modelling squash and shear
+        as well as origin, scale, and orientation.  However, ITYPE=4
+        selects the {\it solid body rotation}\/ option;  the model COEFFS
+        still consists of the same six coefficients, but now two of
+        them are used twice (appropriately signed).  Origin, scale
+        and orientation are still modelled, but not squash or shear --
+        the units of X and Y have to be the same.
+  \item For NC=4, NP must be at least 2.  For NC=6, NP must be at
+        least 3.
+  \item The model is returned in the array COEFFS.  Naming the
+        six elements of COEFFS $a,b,c,d,e$ \& $f$,
+        the model transforms {\it measured}\/ coordinates
+        $[x_{m},y_{m}\,]$ into {\it expected}\/ coordinates
+        $[x_{e},y_{e}\,]$ as follows:
+        \begin{verse}
+         $x_{e} = a + bx_{m} + cy_{m}$ \\
+         $y_{e} = d + ex_{m} + fy_{m}$
+        \end{verse}
+        For the {\it solid body rotation}\/ option (ITYPE=4), the
+        magnitudes of $b$ and $f$, and of $c$ and $e$, are equal.  The
+        signs of these coefficients depend on whether there is a
+        sign reversal between $[x_{e},y_{e}]$ and $[x_{m},y_{m}]$;
+        fits are performed
+        with and without a sign reversal and the best one chosen.
+  \item Error status values J=$-$1 and $-$2 leave COEFFS unchanged;
+        if J=$-$3 COEFFS may have been changed.
+  \item See also sla\_PXY, sla\_INVF, sla\_XY2XY, sla\_DCMPF.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_FK425}{FK4 to FK5}
+{
+ \action{Convert B1950.0 FK4 star data to J2000.0 FK5.
+         This routine converts stars from the old, Bessel-Newcomb, FK4
+         system to the new, IAU~1976, FK5, Fricke system.  The precepts
+         of Smith~{\it et~al.}\ (see reference~1) are followed,
+         using the implementation
+         by Yallop~{\it et~al.}\ (reference~2) of a matrix method
+         due to Standish.
+         Kinoshita's development of Andoyer's post-Newcomb precession is
+         used.  The numerical constants from 
+         Seidelmann~{\it et~al.}\  (reference~3) are used canonically.}
+ \call{CALL sla\_FK425 (\vtop{
+         \hbox{R1950,D1950,DR1950,DD1950,P1950,V1950,}
+         \hbox{R2000,D2000,DR2000,DD2000,P2000,V2000)}}}
+}
+\args{GIVEN}
+{
+ \spec{R1950}{D}{B1950.0 $\alpha$ (radians)} \\
+ \spec{D1950}{D}{B1950.0 $\delta$ (radians)} \\
+ \spec{DR1950}{D}{B1950.0 proper motion in $\alpha$
+                              (radians per tropical year)} \\
+ \spec{DD1950}{D}{B1950.0 proper motion in $\delta$
+                              (radians per tropical year)} \\
+ \spec{P1950}{D}{B1950.0 parallax (arcsec)} \\
+ \spec{V1950}{D}{B1950.0 radial velocity (km~s$^{-1}$, +ve = moving away)}
+}
+\args{RETURNED}
+{
+ \spec{R2000}{D}{J2000.0 $\alpha$ (radians)} \\
+ \spec{D2000}{D}{J2000.0 $\delta$ (radians)} \\
+ \spec{DR2000}{D}{J2000.0 proper motion in $\alpha$
+                              (radians per Julian year)} \\
+ \spec{DD2000}{D}{J2000.0 proper motion in $\delta$
+                              (radians per Julian year)} \\
+ \spec{P2000}{D}{J2000.0 parallax (arcsec)} \\
+ \spec{V2000}{D}{J2000.0 radial velocity (km~s$^{-1}$, +ve = moving away)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The $\alpha$ proper motions are $\dot{\alpha}$ rather than
+        $\dot{\alpha}\cos\delta$, and are per year rather than per century.
+  \item 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 FK425
+        is called.
+  \item In the FK4 catalogue the proper motions of stars within
+        $10^{\circ}$ of the poles do not include the {\it differential
+        E-terms}\/ 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 J2000,
+        and measuring on the sky rather than in terms of $\Delta\alpha$,
+        the errors resulting from this simplification are less than
+        1~milliarcsecond in position and 1~milliarcsecond per
+        century in proper motion.
+  \item See also sla\_FK45Z, sla\_FK524, sla\_FK54Z.
+ \end{enumerate}
+}
+\refs
+{
+ \begin{enumerate}
+  \item Smith, C.A.\ {\it et al.}, 1989.\  {\it Astr.J.}\ {\bf 97}, 265.
+  \item Yallop, B.D.\ {\it et al.}, 1989.\ {\it Astr.J.}\ {\bf 97}, 274.
+  \item Seidelmann, P.K.\ (ed), 1992.  {\it Explanatory
+        Supplement to the Astronomical Almanac,}\/ ISBN~0-935702-68-7.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_FK45Z}{FK4 to FK5, no P.M. or Parallax}
+{
+ \action{Convert B1950.0 FK4 star data to J2000.0 FK5 assuming zero
+         proper motion in the FK5 frame.
+         This routine converts stars from the old, Bessel-Newcomb, FK4
+         system to the new, 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
+         reference~1, but using the constants of reference~4.}
+ \call{CALL sla\_FK45Z (R1950,D1950,BEPOCH,R2000,D2000)}
+}
+\args{GIVEN}
+{
+ \spec{R1950}{D}{B1950.0 FK4 $\alpha$ at epoch BEPOCH (radians)} \\
+ \spec{D1950}{D}{B1950.0 FK4 $\delta$ at epoch BEPOCH (radians)} \\
+ \spec{BEPOCH}{D}{Besselian epoch ({\it e.g.}\ 1979.3D0)}
+}
+\args{RETURNED}
+{
+ \spec{R2000}{D}{J2000.0 FK5 $\alpha$ (radians)} \\
+ \spec{D2000}{D}{J2000.0 FK5 $\delta$ (radians)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The epoch BEPOCH is strictly speaking Besselian, but
+        if a Julian epoch is supplied the result will be
+        affected only to a negligible extent.
+  \item 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 FK45Z is called.
+  \item In the FK4 catalogue the proper motions of stars within
+        $10^{\circ}$ of the poles do not include the {\it differential
+        E-terms}\/ 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 $\Delta\alpha$,
+        the errors resulting from this simplification are less than
+        1~milliarcsecond in position and 1~milliarcsecond per
+        century in proper motion.
+  \item See also sla\_FK425, sla\_FK524, sla\_FK54Z.
+ \end{enumerate}
+}
+\refs
+{
+ \begin{enumerate}
+  \item Aoki, S., {\it et al.}, 1983.\ {\it Astr.Astrophys.}, {\bf 128}, 263.
+  \item Smith, C.A.\ {\it et al.}, 1989.\  {\it Astr.J.}\ {\bf 97}, 265.
+  \item Yallop, B.D.\ {\it et al.}, 1989.\ {\it Astr.J.}\ {\bf 97}, 274.
+  \item Seidelmann, P.K.\ (ed), 1992.  {\it Explanatory
+        Supplement to the Astronomical Almanac,}\/ ISBN~0-935702-68-7.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_FK524}{FK5 to FK4}
+{
+ \action{Convert J2000.0 FK5 star data to B1950.0 FK4.
+         This routine converts stars from the new, IAU~1976, FK5, Fricke
+         system, to the old, Bessel-Newcomb, FK4 system.
+         The precepts of Smith~{\it et~al.}\ (reference~1) are followed,
+         using the implementation by Yallop~{\it et~al.}\ (reference~2)
+         of a matrix method due to Standish.  Kinoshita's development of
+         Andoyer's post-Newcomb precession is used.  The numerical
+         constants from Seidelmann~{\it et~al.}\ (reference~3) are
+         used canonically.}
+ \call{CALL sla\_FK524 (\vtop{
+         \hbox{R2000,D2000,DR2000,DD2000,P2000,V2000,}
+         \hbox{R1950,D1950,DR1950,DD1950,P1950,V1950)}}}
+}
+\args{GIVEN}
+{
+ \spec{R2000}{D}{J2000.0 $\alpha$ (radians)} \\
+ \spec{D2000}{D}{J2000.0 $\delta$ (radians)} \\
+ \spec{DR2000}{D}{J2000.0 proper motion in $\alpha$
+                              (radians per Julian year)} \\
+ \spec{DD2000}{D}{J2000.0 proper motion in $\delta$
+                              (radians per Julian year)} \\
+ \spec{P2000}{D}{J2000.0 parallax (arcsec)} \\
+ \spec{V2000}{D}{J2000 radial velocity (km~s$^{-1}$, +ve = moving away)}
+}
+\args{RETURNED}
+{
+ \spec{R1950}{D}{B1950.0 $\alpha$ (radians)} \\
+ \spec{D1950}{D}{B1950.0 $\delta$ (radians)} \\
+ \spec{DR1950}{D}{B1950.0 proper motion in $\alpha$
+                              (radians per tropical year)} \\
+ \spec{DD1950}{D}{B1950.0 proper motion in $\delta$
+                              (radians per tropical year)} \\
+ \spec{P1950}{D}{B1950.0 parallax (arcsec)} \\
+ \spec{V1950}{D}{radial velocity (km~s$^{-1}$, +ve = moving away)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The $\alpha$ proper motions are $\dot{\alpha}$ rather than
+        $\dot{\alpha}\cos\delta$, and are per year rather than per century.
+  \item 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.
+  \item In the FK4 catalogue the proper motions of stars within
+        $10^{\circ}$ of the poles do not include the {\it differential
+        E-terms}\/ 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 $\Delta\alpha$,
+        the errors resulting from this simplification are less than
+        1~milliarcsecond in position and 1~milliarcsecond per
+        century in proper motion.
+  \item See also sla\_FK425, sla\_FK45Z, sla\_FK54Z.
+ \end{enumerate}
+}
+\refs
+{
+ \begin{enumerate}
+  \item Smith, C.A.\ {\it et al.}, 1989.\  {\it Astr.J.}\ {\bf 97}, 265.
+  \item Yallop, B.D.\ {\it et al.}, 1989.\ {\it Astr.J.}\ {\bf 97}, 274.
+  \item Seidelmann, P.K.\ (ed), 1992.  {\it Explanatory
+        Supplement to the Astronomical Almanac,}\/ ISBN~0-935702-68-7.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_FK52H}{FK5 to Hipparcos}
+{
+ \action{Transform an FK5 (J2000) position and proper motion
+         into the frame of the Hipparcos catalogue.}
+ \call{CALL sla\_FK52H (R5,D5,DR5,DD5,RH,DH,DRH,DDH)}
+}
+\args{GIVEN}
+{
+ \spec{R5}{D}{J2000.0 FK5 $\alpha$ (radians)} \\
+ \spec{D5}{D}{J2000.0 FK5 $\delta$ (radians)} \\
+ \spec{DR5}{D}{J2000.0 FK5 proper motion in $\alpha$
+                              (radians per Julian year)} \\
+ \spec{DD5}{D}{J2000.0 FK5 proper motion in $\delta$
+                              (radians per Julian year)}
+}
+\args{RETURNED}
+{
+ \spec{RH}{D}{Hipparcos $\alpha$ (radians)} \\
+ \spec{DH}{D}{Hipparcos $\delta$ (radians)} \\
+ \spec{DRH}{D}{Hipparcos proper motion in $\alpha$
+                              (radians per Julian year)} \\
+ \spec{DDH}{D}{Hipparcos proper motion in $\delta$
+                              (radians per Julian year)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The $\alpha$ proper motions are $\dot{\alpha}$ rather than
+        $\dot{\alpha}\cos\delta$, and are per year rather than per century.
+  \item The FK5 to Hipparcos
+        transformation consists of a pure rotation and spin;
+        zonal errors in the FK5 catalogue are not taken into account.
+  \item The adopted epoch J2000.0 FK5 to Hipparcos orientation and spin
+        values are as follows (see reference):
+
+        \vspace{2ex}
+
+        ~~~~~~~~~~~~
+        \begin{tabular}{|r|r|r|} \hline
+        &
+        \multicolumn{1}{|c}{\it orientation} &
+        \multicolumn{1}{|c|}{\it ~~~spin~~~} \\ \hline
+        $x$ & $-19.9$~~~~ & ~$-0.30$~~ \\
+        $y$ &  $-9.1$~~~~ & ~$+0.60$~~ \\
+        $z$ & $+22.9$~~~~ & ~$+0.70$~~ \\ \hline
+        & {\it mas}~~~~~ & ~{\it mas/y}~ \\ \hline
+        \end{tabular}
+
+        \vspace{3ex}
+
+        These orientation and spin components are interpreted as
+        {\it axial vectors.}  An axial vector points at the pole of
+        the rotation and its length is the amount of rotation in radians.
+  \item See also sla\_FK5HZ, sla\_H2FK5, sla\_HFK5Z.
+ \end{enumerate}
+}
+\aref {Feissel, M.\ \& Mignard, F., 1998.,  {\it Astron.Astrophys.}\
+       {\bf 331}, L33-L36.}
+%-----------------------------------------------------------------------
+\routine{SLA\_FK54Z}{FK5 to FK4, no P.M. or Parallax}
+{
+ \action{Convert a J2000.0 FK5 star position to B1950.0 FK4 assuming
+         FK5 zero proper motion and parallax.
+         This routine converts star positions from the new, IAU~1976,
+         FK5, Fricke system to the old, Bessel-Newcomb, FK4 system.}
+ \call{CALL sla\_FK54Z (R2000,D2000,BEPOCH,R1950,D1950,DR1950,DD1950)}
+}
+\args{GIVEN}
+{
+ \spec{R2000}{D}{J2000.0 FK5 $\alpha$ (radians)} \\
+ \spec{D2000}{D}{J2000.0 FK5 $\delta$ (radians)} \\
+ \spec{BEPOCH}{D}{Besselian epoch ({\it e.g.}\ 1950D0)}
+}
+\args{RETURNED}
+{
+ \spec{R1950}{D}{B1950.0 FK4 $\alpha$ at epoch BEPOCH (radians)} \\
+ \spec{D1950}{D}{B1950.0 FK4 $\delta$ at epoch BEPOCH (radians)} \\
+ \spec{DR1950}{D}{B1950.0 FK4 proper motion in $\alpha$
+                              (radians per tropical year)} \\
+ \spec{DD1950}{D}{B1950.0 FK4 proper motion in $\delta$
+                              (radians per tropical year)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The $\alpha$ proper motions are $\dot{\alpha}$ rather than
+        $\dot{\alpha}\cos\delta$, and are per year rather than per century.
+  \item 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 routines before and
+        after this routine is called.
+  \item Unlike in the sla\_FK524 routine, the FK5 proper motions, the
+        parallax and the radial velocity are presumed zero.
+  \item It was 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 routine returns those {\it fictitious proper
+        motions}.
+  \item The position returned by this routine is in the B1950
+        reference frame but at Besselian epoch BEPOCH.  For
+        comparison with catalogues the BEPOCH argument will
+        frequently be 1950D0.
+  \item See also sla\_FK425, sla\_FK45Z, sla\_FK524.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_FK5HZ}{FK5 to Hipparcos, no P.M.}
+{
+ \action{Transform an FK5 (J2000) star position into the frame of the
+         Hipparcos catalogue, assuming zero Hipparcos proper motion.}
+ \call{CALL sla\_FK52H (R5,D5,EPOCH,RH,DH)}
+}
+\args{GIVEN}
+{
+ \spec{R5}{D}{J2000.0 FK5 $\alpha$ (radians)} \\
+ \spec{D5}{D}{J2000.0 FK5 $\delta$ (radians)} \\
+ \spec{EPOCH}{D}{Julian epoch (TDB)}
+}
+\args{RETURNED}
+{
+ \spec{RH}{D}{Hipparcos $\alpha$ (radians)} \\
+ \spec{DH}{D}{Hipparcos $\delta$ (radians)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The $\alpha$ proper motions are $\dot{\alpha}$ rather than
+        $\dot{\alpha}\cos\delta$, and are per year rather than per century.
+  \item The FK5 to Hipparcos
+        transformation consists of a pure rotation and spin;
+        zonal errors in the FK5 catalogue are not taken into account.
+  \item The adopted epoch J2000.0 FK5 to Hipparcos orientation and spin
+        values are as follows (see reference):
+
+        \vspace{2ex}
+
+        ~~~~~~~~~~~~
+        \begin{tabular}{|r|r|r|} \hline
+        &
+        \multicolumn{1}{|c}{\it orientation} &
+        \multicolumn{1}{|c|}{\it ~~~spin~~~} \\ \hline
+        $x$ & $-19.9$~~~~ & ~$-0.30$~~ \\
+        $y$ &  $-9.1$~~~~ & ~$+0.60$~~ \\
+        $z$ & $+22.9$~~~~ & ~$+0.70$~~ \\ \hline
+        & {\it mas}~~~~~ & ~{\it mas/y}~ \\ \hline
+        \end{tabular}
+
+        \vspace{3ex}
+
+        These orientation and spin components are interpreted as
+        {\it axial vectors.}  An axial vector points at the pole of
+        the rotation and its length is the amount of rotation in radians.
+  \item See also sla\_FK52H, sla\_H2FK5, sla\_HFK5Z.
+ \end{enumerate}
+}
+\aref {Feissel, M.\ \& Mignard, F., 1998.,  {\it Astron.Astrophys.}\
+       {\bf 331}, L33-L36.}
+%-----------------------------------------------------------------------
+\routine{SLA\_FLOTIN}{Decode a Real Number}
+{
+ \action{Convert free-format input into single precision floating point.}
+ \call{CALL sla\_FLOTIN (STRING, NSTRT, RESLT, JFLAG)}
+}
+\args{GIVEN}
+{
+ \spec{STRING}{C}{string containing number to be decoded} \\
+ \spec{NSTRT}{I}{pointer to where decoding is to commence} \\
+ \spec{RESLT}{R}{current value of result}
+}
+\args{RETURNED}
+{
+ \spec{NSTRT}{I}{advanced to next number} \\
+ \spec{RESLT}{R}{result} \\
+ \spec{JFLAG}{I}{status: $-$1~=~$-$OK, 0~=~+OK, 1~=~null result, 2~=~error}
+}
+\notes
+{
+ \begin{enumerate}
+ \item The reason sla\_FLOTIN has separate `OK' status values
+       for + and $-$ is to enable minus zero to be detected.
+       This is of crucial importance
+       when decoding mixed-radix numbers.  For example, an angle
+       expressed as degrees, arcminutes and arcseconds may have a
+       leading minus sign but a zero degrees field.
+ \item A TAB is interpreted as a space, and lowercase characters are
+       interpreted as uppercase.  {\it n.b.}\ The test for TAB is
+       ASCII-specific.
+ \item The basic format is the sequence of fields $\pm n.n x \pm n$,
+       where $\pm$ is a sign
+       character `+' or `$-$', $n$ means a string of decimal digits,
+       `.' is a decimal point, and $x$, which indicates an exponent,
+       means `D' or `E'.  Various combinations of these fields can be
+       omitted, and embedded blanks are permissible in certain places.
+ \item Spaces:
+       \begin{itemize}
+       \item Leading spaces are ignored.
+       \item Embedded spaces are allowed only after +, $-$, D or E,
+             and after the decimal point if the first sequence of
+             digits is absent.
+       \item Trailing spaces are ignored;  the first signifies
+             end of decoding and subsequent ones are skipped.
+       \end{itemize}
+ \item Delimiters:
+       \begin{itemize}
+       \item Any character other than +,$-$,0-9,.,D,E or space may be
+             used to signal the end of the number and terminate decoding.
+       \item Comma is recognized by sla\_FLOTIN as a special case; it
+             is skipped, leaving the pointer on the next character.  See
+             13, below.
+       \item Decoding will in all cases terminate if end of string
+             is reached.
+       \end{itemize}
+ \item Both signs are optional.  The default is +.
+ \item The mantissa $n.n$ defaults to unity.
+ \item The exponent $x\!\pm\!n$ defaults to `E0'.
+ \item The strings of decimal digits may be of any length.
+ \item The decimal point is optional for whole numbers.
+ \item A {\it null result}\/ occurs when the string of characters
+       being decoded does not begin with +,$-$,0-9,.,D or E, or
+       consists entirely of spaces.  When this condition is
+       detected, JFLAG is set to 1 and RESLT is left untouched.
+ \item NSTRT = 1 for the first character in the string.
+ \item On return from sla\_FLOTIN, NSTRT is set ready for the next
+       decode -- following trailing blanks and any comma.  If a
+       delimiter other than comma is being used, NSTRT must be
+       incremented before the next call to sla\_FLOTIN, otherwise
+       all subsequent calls will return a null result.
+ \item Errors (JFLAG=2) occur when:
+       \begin{itemize}
+       \item a +, $-$, D or E is left unsatisfied; or
+       \item the decimal point is present without at least
+             one decimal digit before or after it; or
+       \item an exponent more than 100 has been presented.
+       \end{itemize}
+ \item When an error has been detected, NSTRT is left
+       pointing to the character following the last
+       one used before the error came to light.  This
+       may be after the point at which a more sophisticated
+       program could have detected the error.  For example,
+       sla\_FLOTIN does not detect that `1E999' is unacceptable
+       (on a computer where this is so)
+       until the entire number has been decoded.
+ \item Certain highly unlikely combinations of mantissa and
+       exponent can cause arithmetic faults during the
+       decode, in some cases despite the fact that they
+       together could be construed as a valid number.
+ \item Decoding is left to right, one pass.
+ \item See also sla\_DFLTIN and sla\_INTIN.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_GALEQ}{Galactic to J2000 $\alpha,\delta$}
+{
+ \action{Transformation from IAU 1958 galactic coordinates
+         to J2000.0 FK5 equatorial coordinates.}
+ \call{CALL sla\_GALEQ (DL, DB, DR, DD)}
+}
+\args{GIVEN}
+{
+ \spec{DL,DB}{D}{galactic longitude and latitude \gal}
+}
+\args{RETURNED}
+{
+ \spec{DR,DD}{D}{J2000.0 \radec}
+}
+\notes
+{
+ \begin{enumerate}
+  \item All arguments are in radians.
+  \item The equatorial coordinates are J2000.0 FK5.  Use the routine
+        sla\_GE50 if conversion to B1950.0 FK4 coordinates is
+                           required.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_GALSUP}{Galactic to Supergalactic}
+{
+ \action{Transformation from IAU 1958 galactic coordinates to
+         de Vaucouleurs supergalactic coordinates.}
+ \call{CALL sla\_GALSUP (DL, DB, DSL, DSB)}
+}
+\args{GIVEN}
+{
+ \spec{DL,DB}{D}{galactic longitude and latitude \gal\ (radians)}
+}
+\args{RETURNED}
+{
+ \spec{DSL,DSB}{D}{supergalactic longitude and latitude (radians)}
+}
+\refs
+{
+ \begin{enumerate}
+  \item de Vaucouleurs, de Vaucouleurs, \& Corwin, {\it Second Reference
+    Catalogue of Bright Galaxies}, U.Texas, p8.
+  \item Systems \& Applied Sciences Corp., documentation for the
+        machine-readable version of the above catalogue,
+        Contract NAS 5-26490.
+ \end{enumerate}
+ (These two references give different values for the galactic
+ longitude of the supergalactic origin.  Both are wrong;  the
+ correct value is $l^{I\!I}=137.37$.)
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_GE50}{Galactic to B1950 $\alpha,\delta$}
+{
+ \action{Transformation from IAU 1958 galactic coordinates to
+         B1950.0 FK4 equatorial coordinates.}
+ \call{CALL sla\_GE50 (DL, DB, DR, DD)}
+}
+\args{GIVEN}
+{
+ \spec{DL,DB}{D}{galactic longitude and latitude \gal}
+}
+\args{RETURNED}
+{
+ \spec{DR,DD}{D}{B1950.0 \radec}
+}
+\notes
+{
+ \begin{enumerate}
+  \item All arguments are in radians.
+  \item The equatorial coordinates are B1950.0 FK4.  Use the
+        routine sla\_GALEQ if conversion to J2000.0 FK5 coordinates
+        is required.
+ \end{enumerate}
+}
+\aref{Blaauw {\it et al.}, 1960, {\it Mon.Not.R.astr.Soc.},
+      {\bf 121}, 123.}
+%-----------------------------------------------------------------------
+\routine{SLA\_GEOC}{Geodetic to Geocentric}
+{
+ \action{Convert geodetic position to geocentric.}
+ \call{CALL sla\_GEOC (P, H, R, Z)}
+}
+\args{GIVEN}
+{
+ \spec{P}{D}{latitude (geodetic, radians)} \\
+ \spec{H}{D}{height above reference spheroid (geodetic, metres)}
+}
+\args{RETURNED}
+{
+ \spec{R}{D}{distance from Earth axis (AU)} \\
+ \spec{Z}{D}{distance from plane of Earth equator (AU)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item Geocentric latitude can be obtained by evaluating {\tt ATAN2(Z,R)}.
+  \item IAU 1976 constants are used.
+ \end{enumerate}
+}
+\aref{Green, R.M., 1985.\ {\it Spherical Astronomy}, Cambridge U.P., p98.}
+%-----------------------------------------------------------------------
+\routine{SLA\_GMST}{UT to GMST}
+{
+ \action{Conversion from universal time UT1 to Greenwich mean
+         sidereal time.}
+ \call{D~=~sla\_GMST (UT1)}
+}
+\args{GIVEN}
+{
+ \spec{UT1}{D}{universal time (strictly UT1) expressed as
+                 modified Julian Date (JD$-$2400000.5)}
+}
+\args{RETURNED}
+{
+ \spec{sla\_GMST}{D}{Greenwich mean sidereal time (radians)}
+}
+\notes
+{
+  \begin{enumerate}
+       \item The IAU~1982 expression
+       (see page~S15 of the 1984 {\it Astronomical
+       Almanac})\/ is used, but rearranged to reduce rounding errors.  This
+       expression is always described as giving the GMST at $0^{\rm h}$UT;
+       in fact, it gives the difference between the
+       GMST and the UT, which happens to equal the GMST (modulo
+       24~hours) at $0^{\rm h}$UT each day.  In sla\_GMST, the
+       entire UT is used directly as the argument for the
+       canonical formula, and the fractional part of the UT is
+       added separately;  note that the factor $1.0027379\cdots$ does
+       not appear.
+       \item See also the routine sla\_GMSTA, which
+       delivers better numerical
+       precision by accepting the UT date and time as separate arguments.
+  \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_GMSTA}{UT to GMST (extra precision)}
+{
+ \action{Conversion from universal time UT1 to Greenwich Mean
+         sidereal time, with rounding errors minimized.}
+ \call{D~=~sla\_GMSTA (DATE, UT1)}
+}
+\args{GIVEN}
+{
+ \spec{DATE}{D}{UT1 date as Modified Julian Date (integer part
+                of JD$-$2400000.5)} \\
+ \spec{UT1}{D}{UT1 time (fraction of a day)}
+}
+\args{RETURNED}
+{
+ \spec{sla\_GMST}{D}{Greenwich mean sidereal time (radians)}
+}
+\notes
+{
+  \begin{enumerate}
+       \item The algorithm is derived from the IAU 1982 expression
+       (see page~S15 of the 1984 Astronomical Almanac).
+       \item There is no restriction on how the UT is apportioned between the
+       DATE and UT1 arguments.  Either of the two arguments could, for
+       example, be zero and the entire date\,+\,time supplied in the other.
+       However, the routine is designed to deliver maximum accuracy when
+       the DATE argument is a whole number and the UT1 argument
+       lies in the range $[\,0,\,1\,]$, or {\it vice versa}.
+       \item See also the routine sla\_GMST, which accepts the UT1 as a single
+       argument.  Compared with sla\_GMST, the extra numerical precision
+       delivered by the present routine is unlikely to be important in
+       an absolute sense, but may be useful when critically comparing
+       algorithms and in applications where two sidereal times close
+       together are differenced.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_GRESID}{Gaussian Residual}
+{
+ \action{Generate pseudo-random normal deviate or {\it Gaussian residual}.}
+ \call{R~=~sla\_GRESID (S)}
+}
+\args{GIVEN}
+{
+ \spec{S}{R}{standard deviation}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The results of many calls to this routine will be
+        normally distributed with mean zero and standard deviation S.
+  \item The Box-Muller algorithm is used.
+  \item The implementation is machine-dependent.
+ \end{enumerate}
+}
+\aref{Ahrens \& Dieter, 1972.\ {\it Comm.A.C.M.}\ {\bf 15}, 873.}
+%-----------------------------------------------------------------------
+\routine{SLA\_H2E}{Az,El to $h,\delta$}
+{
+ \action{Horizon to equatorial coordinates
+         (single precision).}
+ \call{CALL sla\_H2E (AZ, EL, PHI, HA, DEC)}
+}
+\args{GIVEN}
+{
+ \spec{AZ}{R}{azimuth (radians)} \\
+ \spec{EL}{R}{elevation (radians)} \\
+ \spec{PHI}{R}{latitude (radians)}
+}
+\args{RETURNED}
+{
+ \spec{HA}{R}{hour angle (radians)} \\
+ \spec{DEC}{R}{declination (radians)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The sign convention for azimuth is north zero, east $+\pi/2$.
+  \item HA is returned in the range $\pm\pi$.  Declination is returned
+        in the range $\pm\pi$.
+  \item The latitude is (in principle) geodetic.  In critical
+        applications, corrections for polar motion should be applied
+        (see sla\_POLMO).
+  \item In some applications it will be important to specify the
+        correct type of elevation in order to produce the required
+        type of \hadec.  In particular, it may be important to
+        distinguish between the elevation as affected by refraction,
+        which will yield the {\it observed} \hadec, and the elevation
+        {\it in vacuo}, which will yield the {\it topocentric}
+        \hadec.  If the
+        effects of diurnal aberration can be neglected, the
+        topocentric \hadec\ may be used as an approximation to the
+        {\it apparent} \hadec.
+  \item No range checking of arguments is carried out.
+  \item 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.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_H2FK5}{Hipparcos to FK5}
+{
+ \action{Transform a Hipparcos star position and proper motion
+         into the FK5 (J2000) frame.}
+ \call{CALL sla\_H2FK5 (RH,DH,DRH,DDH,R5,D5,DR5,DD5)}
+}
+\args{GIVEN}
+{
+ \spec{RH}{D}{Hipparcos $\alpha$ (radians)} \\
+ \spec{DH}{D}{Hipparcos $\delta$ (radians)} \\
+ \spec{DRH}{D}{Hipparcos proper motion in $\alpha$
+                              (radians per Julian year)} \\
+ \spec{DDH}{D}{Hipparcos proper motion in $\delta$
+                              (radians per Julian year)}
+}
+\args{RETURNED}
+{
+ \spec{R5}{D}{J2000.0 FK5 $\alpha$ (radians)} \\
+ \spec{D5}{D}{J2000.0 FK5 $\delta$ (radians)} \\
+ \spec{DR5}{D}{J2000.0 FK5 proper motion in $\alpha$
+                              (radians per Julian year)} \\
+ \spec{DD5}{D}{FK5 J2000.0 proper motion in $\delta$
+                              (radians per Julian year)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The $\alpha$ proper motions are $\dot{\alpha}$ rather than
+        $\dot{\alpha}\cos\delta$, and are per year rather than per century.
+  \item The FK5 to Hipparcos
+        transformation consists of a pure rotation and spin;
+        zonal errors in the FK5 catalogue are not taken into account.
+  \item The adopted epoch J2000.0 FK5 to Hipparcos orientation and spin
+        values are as follows (see reference):
+
+        \vspace{2ex}
+
+        ~~~~~~~~~~~~
+        \begin{tabular}{|r|r|r|} \hline
+        &
+        \multicolumn{1}{|c}{\it orientation} &
+        \multicolumn{1}{|c|}{\it ~~~spin~~~} \\ \hline
+        $x$ & $-19.9$~~~~ & ~$-0.30$~~ \\
+        $y$ &  $-9.1$~~~~ & ~$+0.60$~~ \\
+        $z$ & $+22.9$~~~~ & ~$+0.70$~~ \\ \hline
+        & {\it mas}~~~~~ & ~{\it mas/y}~ \\ \hline
+        \end{tabular}
+
+        \vspace{3ex}
+
+        These orientation and spin components are interpreted as
+        {\it axial vectors.}  An axial vector points at the pole of
+        the rotation and its length is the amount of rotation in radians.
+  \item See also sla\_FK52H, sla\_FK5HZ, sla\_HFK5Z.
+ \end{enumerate}
+}
+\aref {Feissel, M.\ \& Mignard, F., 1998.,  {\it Astron.Astrophys.}\
+       {\bf 331}, L33-L36.}
+%-----------------------------------------------------------------------
+\routine{SLA\_HFK5Z}{Hipparcos to FK5, no P.M.}
+{
+ \action{Transform a Hipparcos star position
+         into the FK5 (J2000) frame assuming zero Hipparcos proper motion.}
+ \call{CALL sla\_HFK5Z (RH,DH,EPOCH,R5,D5,DR5,DD5)}
+}
+\args{GIVEN}
+{
+ \spec{RH}{D}{Hipparcos $\alpha$ (radians)} \\
+ \spec{DH}{D}{Hipparcos $\delta$ (radians)} \\
+ \spec{EPOCH}{D}{Julian epoch (TDB)}
+}
+\args{RETURNED}
+{
+ \spec{R5}{D}{J2000.0 FK5 $\alpha$ (radians)} \\
+ \spec{D5}{D}{J2000.0 FK5 $\delta$ (radians)} \\
+ \spec{DR5}{D}{J2000.0 FK5 proper motion in $\alpha$
+                              (radians per Julian year)} \\
+ \spec{DD5}{D}{FK5 J2000.0 proper motion in $\delta$
+                              (radians per Julian year)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The $\alpha$ proper motions are $\dot{\alpha}$ rather than
+        $\dot{\alpha}\cos\delta$, and are per year rather than per century.
+  \item The FK5 to Hipparcos
+        transformation consists of a pure rotation and spin;
+        zonal errors in the FK5 catalogue are not taken into account.
+  \item The adopted epoch J2000.0 FK5 to Hipparcos orientation and spin
+        values are as follows (see reference):
+
+        \vspace{2ex}
+
+        ~~~~~~~~~~~~
+        \begin{tabular}{|r|r|r|} \hline
+        &
+        \multicolumn{1}{|c}{\it orientation} &
+        \multicolumn{1}{|c|}{\it ~~~spin~~~} \\ \hline
+        $x$ & $-19.9$~~~~ & ~$-0.30$~~ \\
+        $y$ &  $-9.1$~~~~ & ~$+0.60$~~ \\
+        $z$ & $+22.9$~~~~ & ~$+0.70$~~ \\ \hline
+        & {\it mas}~~~~~ & ~{\it mas/y}~ \\ \hline
+        \end{tabular}
+
+        \vspace{3ex}
+
+        These orientation and spin components are interpreted as
+        {\it axial vectors.}  An axial vector points at the pole of
+        the rotation and its length is the amount of rotation in radians.
+        The order of the rotations, which are very small,
+  \item It was the intention that Hipparcos 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 FK5, and this routine returns those
+        {\it fictitious proper motions.}
+  \item The position returned by this routine is in the FK5 J2000
+        reference frame but at Julian epoch EPOCH.
+  \item See also sla\_FK52H, sla\_FK5HZ, sla\_H2FK5.
+ \end{enumerate}
+}
+\aref {Feissel, M.\ \& Mignard, F., 1998.,  {\it Astron.Astrophys.}\
+       {\bf 331}, L33-L36.}
+%-----------------------------------------------------------------------
+\routine{SLA\_IMXV}{Apply 3D Reverse Rotation}
+{
+ \action{Multiply a 3-vector by the inverse of a rotation
+         matrix (single precision).}
+ \call{CALL sla\_IMXV (RM, VA, VB)}
+}
+\args{GIVEN}
+{
+ \spec{RM}{R(3,3)}{rotation matrix} \\
+ \spec{VA}{R(3)}{vector to be rotated}
+}
+\args{RETURNED}
+{
+ \spec{VB}{R(3)}{result vector}
+}
+\notes
+{
+ \begin{enumerate}
+  \item This routine performs the operation:
+        \begin{verse}
+         {\bf b} = {\bf M}$^{T}\cdot${\bf a}
+        \end{verse}
+        where {\bf a} and {\bf b} are the 3-vectors VA and VB
+        respectively, and {\bf M} is the $3\times3$ matrix RM.
+  \item The main function of this routine is apply an inverse
+        rotation;  under these circumstances, ${\bf M}$ is
+        {\it orthogonal}, with its inverse the same as its transpose.
+  \item To comply with the ANSI Fortran 77 standard, VA and VB must
+        {\bf not} be the same array.  The routine is, in fact, coded
+        so as to work properly on the VAX and many other systems even
+        if this rule is violated, something that is {\bf not}, however,
+        recommended.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_INTIN}{Decode an Integer Number}
+{
+ \action{Convert free-format input into an integer.}
+ \call{CALL sla\_INTIN (STRING, NSTRT, IRESLT, JFLAG)}
+}
+\args{GIVEN}
+{
+ \spec{STRING}{C}{string containing number to be decoded} \\
+ \spec{NSTRT}{I}{pointer to where decoding is to commence} \\
+ \spec{IRESLT}{I}{current value of result}
+}
+\args{RETURNED}
+{
+ \spec{NSTRT}{I}{advanced to next number} \\
+ \spec{IRESLT}{I}{result} \\
+ \spec{JFLAG}{I}{status: $-$1 = $-$OK, 0~=~+OK, 1~=~null result, 2~=~error}
+}
+\notes
+{
+ \begin{enumerate}
+ \item The reason sla\_INTIN has separate `OK' status values
+       for + and $-$ is to enable minus zero to be detected.
+       This is of crucial importance
+       when decoding mixed-radix numbers.  For example, an angle
+       expressed as degrees, arcminutes and arcseconds may have a
+       leading minus sign but a zero degrees field.
+ \item A TAB is interpreted as a space. {\it n.b.}\ The test for TAB is
+       ASCII-specific.
+ \item The basic format is the sequence of fields $\pm n$,
+       where $\pm$ is a sign
+       character `+' or `$-$', and $n$ means a string of decimal digits.
+ \item Spaces:
+       \begin{itemize}
+       \item Leading spaces are ignored.
+       \item Spaces between the sign and the number are allowed.
+       \item Trailing spaces are ignored;  the first signifies
+             end of decoding and subsequent ones are skipped.
+       \end{itemize}
+ \item Delimiters:
+       \begin{itemize}
+       \item Any character other than +,$-$,0-9 or space may be
+             used to signal the end of the number and terminate decoding.
+       \item Comma is recognized by sla\_INTIN as a special case; it
+             is skipped, leaving the pointer on the next character.  See
+             9, below.
+       \item Decoding will in all cases terminate if end of string
+             is reached.
+       \end{itemize}
+ \item The sign is optional.  The default is +.
+ \item A {\it null result}\/ occurs when the string of characters
+       being decoded does not begin with +,$-$ or 0-9, or
+       consists entirely of spaces.  When this condition is
+       detected, JFLAG is set to 1 and IRESLT is left untouched.
+ \item NSTRT = 1 for the first character in the string.
+ \item On return from sla\_INTIN, NSTRT is set ready for the next
+       decode -- following trailing blanks and any comma.  If a
+       delimiter other than comma is being used, NSTRT must be
+       incremented before the next call to sla\_INTIN, otherwise
+       all subsequent calls will return a null result.
+ \item Errors (JFLAG=2) occur when:
+       \begin{itemize}
+       \item there is a + or $-$ but no number; or
+       \item the number is greater than $2^{31}-1$.
+       \end{itemize}
+ \item When an error has been detected, NSTRT is left
+       pointing to the character following the last
+       one used before the error came to light.
+ \item See also sla\_FLOTIN and sla\_DFLTIN.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_INVF}{Invert Linear Model}
+{
+ \action{Invert a linear model of the type produced by the
+         sla\_FITXY routine.}
+ \call{CALL sla\_INVF (FWDS,BKWDS,J)}
+}
+\args{GIVEN}
+{
+ \spec{FWDS}{D(6)}{model coefficients}
+}
+\args{RETURNED}
+{
+ \spec{BKWDS}{D(6)}{inverse model} \\
+ \spec{J}{I}{status:  0 = OK, $-$1 = no inverse}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The models relate two sets of \xy\ coordinates as follows.
+        Naming the six elements of FWDS $a,b,c,d,e$ \& $f$,
+        where two sets of coordinates $[x_{1},y_{1}]$ and
+        $[x_{2},y_{2}\,]$ are related thus:
+        \begin{verse}
+         $x_{2} = a + bx_{1} + cy_{1}$ \\
+         $y_{2} = d + ex_{1} + fy_{1}$
+        \end{verse}
+        The present routine generates a new set of coefficients
+        $p,q,r,s,t$ \& $u$ (the array BKWDS) such that:
+        \begin{verse}
+         $x_{1} = p + qx_{2} + ry_{2}$ \\
+         $y_{1} = s + tx_{2} + uy_{2}$
+        \end{verse}
+  \item Two successive calls to this routine will deliver a set
+        of coefficients equal to the starting values.
+  \item To comply with the ANSI Fortran 77 standard, FWDS and BKWDS must
+        {\bf not} be the same array.  The routine is, in fact, coded
+        so as to work properly on the VAX and many other systems even
+        if this rule is violated, something that is {\bf not}, however,
+        recommended.
+  \item See also sla\_FITXY, sla\_PXY, sla\_XY2XY, sla\_DCMPF.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_KBJ}{Select Epoch Prefix}
+{
+ \action{Select epoch prefix `B' or `J'.}
+ \call{CALL sla\_KBJ (JB, E, K, J)}
+}
+\args{GIVEN}
+{
+ \spec{JB}{I}{sla\_DBJIN prefix status:  0=none, 1=`B', 2=`J'} \\
+ \spec{E}{D}{epoch -- Besselian or Julian}
+}
+\args{RETURNED}
+{
+ \spec{K}{C}{`B' or `J'} \\
+ \spec{J}{I}{status:  0=OK}
+}
+\anote{The routine is mainly intended for use in conjunction with the
+       sla\_DBJIN routine.  If the value of JB indicates that an explicit
+       B or J prefix was detected by sla\_DBJIN, a `B' or `J'
+       is returned to match.  If JB indicates that no explicit B or J
+       was supplied, the choice is made on the basis of the epoch
+       itself;  B is assumed for E $<1984$, otherwise J.}
+%-----------------------------------------------------------------------
+\routine{SLA\_M2AV}{Rotation Matrix to Axial Vector}
+{
+ \action{From a rotation matrix, determine the corresponding axial vector
+        (single precision).}
+ \call{CALL sla\_M2AV (RMAT, AXVEC)}
+}
+\args{GIVEN}
+{
+ \spec{RMAT}{R(3,3)}{rotation matrix}
+}
+\args{RETURNED}
+{
+ \spec{AXVEC}{R(3)}{axial vector (radians)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item A rotation matrix describes a rotation about some arbitrary axis.
+        The axis is called the {\it Euler axis}, and the angle through
+        which the reference frame rotates is called the {\it Euler angle}.
+        The {\it axial vector}\/ returned by this routine has the same
+        direction as the Euler axis, and its magnitude is the Euler angle
+        in radians.
+  \item The magnitude and direction of the axial vector can be separated
+        by means of the routine sla\_VN.
+  \item The reference frame rotates clockwise as seen looking along
+        the axial vector from the origin.
+  \item If RMAT is null, so is the result.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_MAP}{Mean to Apparent}
+{
+ \action{Transform star \radec\ from mean place to geocentric apparent.
+         The reference frames and timescales used are post IAU~1976.}
+ \call{CALL sla\_MAP (RM, DM, PR, PD, PX, RV, EQ, DATE, RA, DA)}
+}
+\args{GIVEN}
+{
+ \spec{RM,DM}{D}{mean \radec\ (radians)} \\
+ \spec{PR,PD}{D}{proper motions:  \radec\ changes per Julian year} \\
+ \spec{PX}{D}{parallax (arcsec)} \\
+ \spec{RV}{D}{radial velocity (km~s$^{-1}$, +ve if receding)} \\
+ \spec{EQ}{D}{epoch and equinox of star data (Julian)} \\
+ \spec{DATE}{D}{TDB for apparent place (JD$-$2400000.5)}
+}
+\args{RETURNED}
+{
+ \spec{RA,DA}{D}{apparent \radec\ (radians)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item 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 sla\_PM to apply proper
+        motion corrections before using this routine.
+  \item The distinction between the required TDB and TT is
+        always negligible.  Moreover, for all but the most
+        critical applications UTC is adequate.
+  \item The $\alpha$ proper motions are $\dot{\alpha}$ rather than
+        $\dot{\alpha}\cos\delta$, and are per year rather than per century.
+  \item 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 sla\_MAPPA routine
+        once and then either the sla\_MAPQK routine (which includes
+        parallax and proper motion) or sla\_MAPQKZ (which assumes
+        zero parallax and FK5 proper motion).
+ \end{enumerate}
+}
+\refs
+{
+ \begin{enumerate}
+  \item 1984 {\it Astronomical Almanac}, pp B39-B41.
+  \item Lederle \& Schwan, 1984.\ {\it Astr.Astrophys.}\ {\bf 134}, 1-6.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_MAPPA}{Mean to Apparent Parameters}
+{
+ \action{Compute star-independent parameters in preparation for
+         conversions between mean place and geocentric apparent place.
+         The parameters produced by this routine are required in the
+         parallax, light deflection, aberration, and precession/nutation
+         parts of the mean/apparent transformations.
+         The reference frames and timescales used are post IAU~1976.}
+ \call{CALL sla\_MAPPA (EQ, DATE, AMPRMS)}
+}
+\args{GIVEN}
+{
+ \spec{EQ}{D}{epoch of mean equinox to be used (Julian)} \\
+ \spec{DATE}{D}{TDB (JD$-$2400000.5)}
+}
+\args{RETURNED}
+{
+ \spec{AMPRMS}{D(21)}{star-independent mean-to-apparent parameters:} \\
+ \specel   {(1)}     {time interval for proper motion (Julian years)} \\
+ \specel   {(2-4)}   {barycentric position of the Earth (AU)} \\
+ \specel   {(5-7)}   {heliocentric direction of the Earth (unit vector)} \\
+ \specel   {(8)}     {(gravitational radius of
+                      Sun)$\times 2 / $(Sun-Earth distance)} \\
+ \specel   {(9-11)}  {{\bf v}: barycentric Earth velocity in units of c} \\
+ \specel   {(12)}    {$\sqrt{1-\left|\mbox{\bf v}\right|^2}$} \\
+ \specel   {(13-21)} {precession/nutation $3\times3$ matrix}
+}
+\notes
+{
+ \begin{enumerate}
+  \item For DATE, the distinction between the required TDB and TT
+        is always negligible.  Moreover, for all but the most
+        critical applications UTC is adequate.
+  \item The accuracy of the routines using the parameters AMPRMS is
+        limited by the routine sla\_EVP, used here to compute the
+        Earth position and velocity by the methods of Stumpff.
+        The maximum error in the resulting aberration corrections is
+        about 0.3 milliarcsecond.
+  \item The vectors AMPRMS(2-4) and AMPRMS(5-7) are referred to
+        the mean equinox and equator of epoch EQ.
+  \item The parameters produced by this routine are used by
+        sla\_MAPQK and sla\_MAPQKZ.
+ \end{enumerate}
+}
+\refs
+{
+ \begin{enumerate}
+  \item 1984 {\it Astronomical Almanac}, pp B39-B41.
+  \item Lederle \& Schwan, 1984.\ {\it Astr.Astrophys.}\ {\bf 134}, 1-6.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_MAPQK}{Quick Mean to Apparent}
+{
+ \action{Quick mean to apparent place:  transform a star \radec\ from
+         mean place to geocentric apparent place, given the
+         star-independent parameters.  The reference frames and
+         timescales used are post IAU 1976.}
+ \call{CALL sla\_MAPQK (RM, DM, PR, PD, PX, RV, AMPRMS, RA, DA)}
+}
+\args{GIVEN}
+{
+ \spec{RM,DM}{D}{mean \radec\ (radians)} \\
+ \spec{PR,PD}{D}{proper motions:  \radec\ changes per Julian year} \\
+ \spec{PX}{D}{parallax (arcsec)} \\
+ \spec{RV}{D}{radial velocity (km~s$^{-1}$, +ve if receding)} \\
+ \spec{AMPRMS}{D(21)}{star-independent mean-to-apparent parameters:} \\
+ \specel   {(1)}     {time interval for proper motion (Julian years)} \\
+ \specel   {(2-4)}   {barycentric position of the Earth (AU)} \\
+ \specel   {(5-7)}   {heliocentric direction of the Earth (unit vector)} \\
+ \specel   {(8)}     {(gravitational radius of
+                      Sun)$\times 2 / $(Sun-Earth distance)} \\
+ \specel   {(9-11)}  {{\bf v}: barycentric Earth velocity in units of c} \\
+ \specel   {(12)}    {$\sqrt{1-\left|\mbox{\bf v}\right|^2}$} \\
+ \specel   {(13-21)} {precession/nutation $3\times3$ matrix}
+}
+\args{RETURNED}
+{
+ \spec{RA,DA}{D }{apparent \radec\ (radians)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item 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
+        sla\_MAPPA routine.
+  \item If the parallax and proper motions are zero the sla\_MAPQKZ
+        routine can be used instead.
+  \item The vectors AMPRMS(2-4) and AMPRMS(5-7) are referred to
+        the mean equinox and equator of epoch EQ.
+  \item Strictly speaking, the routine is not valid for solar-system
+        sources, though the error will usually be extremely small.
+        However, to prevent gross errors in the case where the
+        position of the Sun is specified, the gravitational
+        deflection term is restrained within about \arcseci{920} of the
+        centre of the Sun's disc.  The term has a maximum value of
+        about \arcsec{1}{85} at this radius, and decreases to zero as
+        the centre of the disc is approached.
+ \end{enumerate}
+}
+\refs
+{
+ \begin{enumerate}
+  \item 1984 {\it Astronomical Almanac}, pp B39-B41.
+  \item Lederle \& Schwan, 1984.\ {\it Astr.Astrophys.}\ {\bf 134}, 1-6.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_MAPQKZ}{Quick Mean-Appt, no PM {\it etc.}}
+{
+ \action{Quick mean to apparent place:  transform a star \radec\ from
+         mean place to geocentric apparent place, given the
+         star-independent parameters, and assuming zero parallax
+         and FK5 proper motion.
+         The reference frames and timescales used are post IAU~1976.}
+ \call{CALL sla\_MAPQKZ (RM, DM, AMPRMS, RA, DA)}
+}
+\args{GIVEN}
+{
+ \spec{RM,DM}{D}{mean \radec\ (radians)} \\
+ \spec{AMPRMS}{D(21)}{star-independent mean-to-apparent parameters:} \\
+ \specel   {(1)}     {time interval for proper motion (Julian years)} \\
+ \specel   {(2-4)}   {barycentric position of the Earth (AU)} \\
+ \specel   {(5-7)}   {heliocentric direction of the Earth (unit vector)} \\
+ \specel   {(8)}     {(gravitational radius of
+                      Sun)$\times 2 / $(Sun-Earth distance)} \\
+ \specel   {(9-11)}  {{\bf v}: barycentric Earth velocity in units of c} \\
+ \specel   {(12)}    {$\sqrt{1-\left|\mbox{\bf v}\right|^2}$} \\
+ \specel   {(13-21)} {precession/nutation $3\times3$ matrix}
+}
+\args{RETURNED}
+{
+ \spec{RA,DA}{D}{apparent \radec\ (radians)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item Use of this routine 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 sla\_MAPPA routine.
+  \item The corresponding routine for the case of non-zero parallax
+        and FK5 proper motion is sla\_MAPQK.
+  \item The vectors AMPRMS(2-4) and AMPRMS(5-7) are referred to the
+        mean equinox and equator of epoch EQ.
+  \item Strictly speaking, the routine is not valid for solar-system
+        sources, though the error will usually be extremely small.
+        However, to prevent gross errors in the case where the
+        position of the Sun is specified, the gravitational
+        deflection term is restrained within about \arcseci{920} of the
+        centre of the Sun's disc.  The term has a maximum value of
+        about \arcsec{1}{85} at this radius, and decreases to zero as
+        the centre of the disc is approached.
+ \end{enumerate}
+}
+\refs
+{
+ \begin{enumerate}
+  \item 1984 {\it Astronomical Almanac}, pp B39-B41.
+  \item Lederle \& Schwan, 1984.\ {\it Astr.Astrophys.}\ {\bf 134}, 1-6.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_MOON}{Approx Moon Pos/Vel}
+{
+ \action{Approximate geocentric position and velocity of the Moon
+         (single precision).}
+ \call{CALL sla\_MOON (IY, ID, FD, PV)}
+}
+\args{GIVEN}
+{
+ \spec{IY}{I}{year} \\
+ \spec{ID}{I}{day in year (1 = Jan 1st)} \\
+ \spec{FD}{R }{fraction of day}
+}
+\args{RETURNED}
+{
+ \spec{PV}{R(6)}{Moon \xyzxyzd, mean equator and equinox of
+                 date (AU, AU~s$^{-1}$)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The date and time is TDB (loosely ET) in a Julian calendar
+        which has been aligned to the ordinary Gregorian
+        calendar for the interval 1900 March 1 to 2100 February 28.
+        The year and day can be obtained by calling sla\_CALYD or
+        sla\_CLYD.
+  \item The position is accurate to better than 0.5~arcminute
+        in direction and 1000~km in distance.  The velocity
+        is accurate to better than \arcsec{0}{5} per hour in direction
+        and 4~metres per socond in distance.  (RMS figures with respect
+        to JPL DE200 for the interval 1960-2025 are \arcseci{14} and
+        \arcsec{0}{2} per hour in longitude, \arcseci{9} and \arcsec{0}{2}
+        per hour in latitude, 350~km and 2~metres per second in distance.)
+        Note that the distance accuracy is comparatively poor because this
+        routine is principally intended for computing topocentric direction.
+  \item This routine is only a partial implementation of the original
+        Meeus algorithm (reference below), which offers 4 times the
+        accuracy in direction and 20 times the accuracy in distance
+        when fully implemented (as it is in sla\_DMOON).
+ \end{enumerate}
+}
+\aref{Meeus, {\it l'Astronomie}, June 1984, p348.}
+%-----------------------------------------------------------------------
+\routine{SLA\_MXM}{Multiply $3\times3$ Matrices}
+{
+ \action{Product of two $3\times3$ matrices (single precision).}
+ \call{CALL sla\_MXM (A, B, C)}
+}
+\args{GIVEN}
+{
+ \spec{A}{R(3,3)}{matrix {\bf A}} \\
+ \spec{B}{R(3,3)}{matrix {\bf B}}
+}
+\args{RETURNED}
+{
+ \spec{C}{R(3,3)}{matrix result: {\bf A}$\times${\bf B}}
+}
+\anote{To comply with the ANSI Fortran 77 standard, A, B and C must
+       be different arrays.  The routine is, in fact, coded
+       so as to work properly on the VAX and many other systems even
+       if this rule is violated, something that is {\bf not}, however,
+       recommended.}
+%-----------------------------------------------------------------------
+\routine{SLA\_MXV}{Apply 3D Rotation}
+{
+ \action{Multiply a 3-vector by a rotation matrix (single precision).}
+ \call{CALL sla\_MXV (RM, VA, VB)}
+}
+\args{GIVEN}
+{
+ \spec{RM}{R(3,3)}{rotation matrix} \\
+ \spec{VA}{R(3)}{vector to be rotated}
+}
+\args{RETURNED}
+{
+ \spec{VB}{R(3)}{result vector}
+}
+\notes
+{
+ \begin{enumerate}
+  \item This routine performs the operation:
+        \begin{verse}
+         {\bf b} = {\bf M}$\cdot${\bf a}
+        \end{verse}
+        where {\bf a} and {\bf b} are the 3-vectors VA and VB
+        respectively, and {\bf M} is the $3\times3$ matrix RM.
+  \item The main function of this routine is apply a
+        rotation;  under these circumstances, ${\bf M}$ is a
+        {\it proper real orthogonal}\/ matrix.
+  \item To comply with the ANSI Fortran 77 standard, VA and VB must
+        {\bf not} be the same array.  The routine is, in fact, coded
+        so as to work properly on the VAX and many other systems even
+        if this rule is violated, something that is {\bf not}, however,
+        recommended.
+ \end{enumerate}
+}
+%------------------------------------------------------------------------------
+\routine{SLA\_NUT}{Nutation Matrix}
+{
+ \action{Form the matrix of nutation (IAU 1980 theory) for a given date.}
+ \call{CALL sla\_NUT (DATE, RMATN)}
+}
+\args{GIVEN}
+{
+ \spec{DATE}{D}{TDB (formerly ET) as Modified Julian Date
+                                          (JD$-$2400000.5)}
+}
+\args{RETURNED}
+{
+ \spec{RMATN}{D(3,3)}{nutation matrix}
+}
+\anote{The matrix is in the sense:
+       \begin{verse}
+        {\bf v}$_{true}$ =  {\bf M}$\cdot${\bf v}$_{mean}$
+       \end{verse}
+       where {\bf v}$_{true}$ is the star vector relative to the
+       true equator and equinox of date, {\bf M} is the
+       $3\times3$ matrix RMATN and
+       {\bf v}$_{mean}$ is the star vector relative to the
+       mean equator and equinox of date.}
+\refs
+{
+ \begin{enumerate}
+  \item Final report of the IAU Working Group on Nutation,
+        chairman P.K.Seidelmann, 1980.
+  \item Kaplan, G.H., 1981.\ {\it USNO circular No.\ 163}, pA3-6.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_NUTC}{Nutation Components}
+{
+ \action{Nutation (IAU 1980 theory):  longitude \& obliquity
+         components, and mean obliquity.}
+ \call{CALL sla\_NUTC (DATE, DPSI, DEPS, EPS0)}
+}
+\args{GIVEN}
+{
+ \spec{DATE}{D}{TDB (formerly ET) as Modified Julian Date
+                                           (JD$-$2400000.5)}
+}
+\args{RETURNED}
+{
+ \spec{DPSI,DEPS}{D}{nutation in longitude and obliquity (radians)} \\
+ \spec{EPS0}{D}{mean obliquity (radians)}
+}
+\refs
+{
+ \begin{enumerate}
+  \item Final report of the IAU Working Group on Nutation,
+        chairman P.K.Seidelmann, 1980.
+  \item Kaplan, G.H., 1981.\ {\it USNO circular no.\ 163}, pA3-6.
+ \end{enumerate}
+}
+%------------------------------------------------------------------------------
+\routine{SLA\_OAP}{Observed to Apparent}
+{
+ \action{Observed to apparent place.}
+ \call{CALL sla\_OAP (\vtop{
+         \hbox{TYPE, OB1, OB2, DATE, DUT, ELONGM, PHIM,}
+         \hbox{HM, XP, YP, TDK, PMB, RH, WL, TLR, RAP, DAP)}}}
+}
+\args{GIVEN}
+{
+ \spec{TYPE}{C*(*)}{type of coordinates -- `R', `H' or `A' (see below)} \\
+ \spec{OB1}{D}{observed Az, HA or RA (radians; Az is N=0, E=$90^{\circ}$)} \\
+ \spec{OB2}{D}{observed zenith distance or $\delta$ (radians)} \\
+ \spec{DATE}{D }{UTC date/time (Modified Julian Date, JD$-$2400000.5)} \\
+ \spec{DUT}{D}{$\Delta$UT:  UT1$-$UTC (UTC seconds)} \\
+ \spec{ELONGM}{D}{observer's mean longitude (radians, east +ve)} \\
+ \spec{PHIM}{D}{observer's mean geodetic latitude (radians)} \\
+ \spec{HM}{D}{observer's height above sea level (metres)} \\
+ \spec{XP,YP}{D}{polar motion \xy\ coordinates (radians)} \\
+ \spec{TDK}{D}{local ambient temperature (degrees K; std=273.155D0)} \\
+ \spec{PMB}{D}{local atmospheric pressure (mB; std=1013.25D0)} \\
+ \spec{RH}{D}{local relative humidity (in the range 0D0\,--\,1D0)} \\
+ \spec{WL}{D}{effective wavelength ($\mu{\rm m}$, {\it e.g.}\ 0.55D0)} \\
+ \spec{TLR}{D}{tropospheric lapse rate (degrees K per metre,
+                                                {\it e.g.}\ 0.0065D0)}
+}
+\args{RETURNED}
+{
+ \spec{RAP,DAP}{D}{geocentric apparent \radec}
+}
+\notes
+{
+ \begin{enumerate}
+  \item 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 is $90^{\circ}$) 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.)
+  \item 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 azimuth and elevation should be within about
+        \arcsec{0}{1} for $\zeta<70^{\circ}$.  Even
+        at a topocentric zenith distance of
+        $90^{\circ}$, the accuracy in elevation should be better than
+        1~arcminute;  useful results are available for a further
+        $3^{\circ}$, beyond which the sla\_REFRO routine returns a
+        fixed value of the refraction.  The complementary
+        routines sla\_AOP (or sla\_AOPQK) and sla\_OAP (or sla\_OAPQK)
+        are self-consistent to better than 1~microarcsecond all over
+        the celestial sphere.
+  \item 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.
+  \item {\it Observed}\/ \azel\ means the position that would be seen by a
+        perfect theodolite located at the observer.  This is
+        related to the observed \hadec\ 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.  {\it Observed}\/ \radec\ or \hadec\ 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 ({\it n.b.}\ not to the refracted pole).
+        By removing from the observed place the effects of
+        atmospheric refraction and diurnal aberration, the
+        geocentric apparent \radec\ is obtained.
+  \item Frequently, {\it mean}\/ rather than {\it apparent}\,
+        \radec\ will be required,
+        in which case further transformations will be necessary.  The
+        sla\_AMP {\it etc.}\ routines will convert
+        the apparent \radec\ 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 B1950
+        coordinates be needed, the routines sla\_FK524 {\it etc.}\ will also
+        need to be applied.
+  \item To convert to apparent \radec\ 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.
+  \item The star-independent apparent-to-observed-place parameters
+        in AOPRMS may be computed by means of the sla\_AOPPA routine.
+        If nothing has changed significantly except the time, the
+        sla\_AOPPAT routine may be used to perform the requisite
+        partial recomputation of AOPRMS.
+  \item 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 $\Delta$UT changes by one second to its post-leap new value.
+  \item 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 $\pm$\tsec{0}{9}.
+  \item IMPORTANT -- TAKE CARE WITH THE LONGITUDE SIGN CONVENTION.  The
+        longitude required by the present routine is {\bf 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 (as in the {\it Astronomical
+        Almanac}\/ before 1984) and must be reversed in sign before use
+        in the present routine.
+  \item The polar coordinates XP,YP can be obtained from IERS
+        circulars and equivalent publications.  The
+        maximum amplitude is about \arcsec{0}{3}.  If XP,YP values
+        are unavailable, use XP=YP=0D0.  See page B60 of the 1988
+        {\it Astronomical Almanac}\/ for a definition of the two angles.
+  \item The height above sea level of the observing station, HM,
+        can be obtained from the {\it Astronomical Almanac}\/ (Section J
+        in the 1988 edition), or via the routine sla\_OBS.  If P,
+        the pressure in mB, is available, an adequate
+        estimate of HM can be obtained from the following expression:
+        \begin{quote}
+         {\tt HM=-29.3D0*TSL*LOG(P/1013.25D0)}
+        \end{quote}
+        where TSL is the approximate sea-level air temperature in degrees K
+        (see {\it Astrophysical Quantities}, C.W.Allen, 3rd~edition,
+        \S 52).  Similarly, if the pressure P is not known,
+        it can be estimated from the height of the observing
+        station, HM as follows:
+        \begin{quote}
+         {\tt P=1013.25D0*EXP(-HM/(29.3D0*TSL))}
+        \end{quote}
+        Note, however, that the refraction is proportional to the
+        pressure and that an accurate P value is important for
+        precise work.
+  \item The azimuths {\it etc.}\ used by the present routine are with
+        respect to the celestial pole.  Corrections from the terrestrial pole
+        can be computed using sla\_POLMO.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_OAPQK}{Quick Observed to Apparent}
+{
+ \action{Quick observed to apparent place.}
+ \call{CALL sla\_OAPQK (TYPE, OB1, OB2, AOPRMS, RAP, DAP)}
+}
+\args{GIVEN}
+{
+ \spec{TYPE}{C*(*)}{type of coordinates -- `R', `H' or `A' (see below)} \\
+ \spec{OB1}{D}{observed Az, HA or RA (radians; Az is N=0, E=$90^{\circ}$)} \\
+ \spec{OB2}{D}{observed zenith distance or $\delta$ (radians)} \\
+ \spec{AOPRMS}{D(14)}{star-independent apparent-to-observed parameters:} \\
+ \specel   {(1)}     {geodetic latitude (radians)} \\
+ \specel   {(2,3)}   {sine and cosine of geodetic latitude} \\
+ \specel   {(4)}     {magnitude of diurnal aberration vector} \\
+ \specel   {(5)}     {height (HM)} \\
+ \specel   {(6)}     {ambient temperature (TDK)} \\
+ \specel   {(7)}     {pressure (PMB)} \\
+ \specel   {(8)}     {relative humidity (RH)} \\
+ \specel   {(9)}     {wavelength (WL)} \\
+ \specel   {(10)}    {lapse rate (TLR)} \\
+ \specel   {(11,12)} {refraction constants A and B (radians)} \\
+ \specel   {(13)}    {longitude + eqn of equinoxes +
+                       ``sidereal $\Delta$UT'' (radians)} \\
+ \specel   {(14)}    {local apparent sidereal time (radians)}
+}
+\args{RETURNED}
+{
+ \spec{RAP,DAP}{D}{geocentric apparent \radec}
+}
+\notes
+{
+ \begin{enumerate}
+  \item 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 is $90^{\circ}$) 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.)
+  \item 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 azimuth and elevation should be within about
+        \arcsec{0}{1} for $\zeta<70^{\circ}$.  Even
+        at a topocentric zenith distance of
+        $90^{\circ}$, the accuracy in elevation should be better than
+        1~arcminute;  useful results are available for a further
+        $3^{\circ}$, beyond which the sla\_REFRO routine returns a
+        fixed value of the refraction.  The complementary
+        routines sla\_AOP (or sla\_AOPQK) and sla\_OAP (or sla\_OAPQK)
+        are self-consistent to better than 1~microarcsecond all over
+        the celestial sphere.
+  \item 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.
+  \item {\it Observed}\/ \azel\ means the position that would be seen by a
+        perfect theodolite located at the observer.  This is
+        related to the observed \hadec\ 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.  {\it Observed}\/ \radec\ or \hadec\ 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 ({\it n.b.}\ not to the refracted pole).
+        By removing from the observed place the effects of
+        atmospheric refraction and diurnal aberration, the
+        geocentric apparent \radec\ is obtained.
+  \item Frequently, {\it mean}\/ rather than {\it apparent}\,
+        \radec\ will be required,
+        in which case further transformations will be necessary.  The
+        sla\_AMP {\it etc.}\ routines will convert
+        the apparent \radec\ 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 B1950
+        coordinates be needed, the routines sla\_FK524 {\it etc.}\ will also
+        need to be applied.
+  \item To convert to apparent \radec\ 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.
+  \item The star-independent apparent-to-observed-place parameters
+        in AOPRMS may be computed by means of the sla\_AOPPA routine.
+        If nothing has changed significantly except the time, the
+        sla\_AOPPAT routine may be used to perform the requisite
+        partial recomputation of AOPRMS.
+  \item The azimuths {\it etc.}\ used by the present routine are with
+        respect to the celestial pole.  Corrections from the terrestrial pole
+        can be computed using sla\_POLMO.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_OBS}{Observatory Parameters}
+{
+ \action{Look up an entry in a standard list of
+         groundbased observing stations parameters.}
+ \call{CALL sla\_OBS (N, C, NAME, W, P, H)}
+}
+\args{GIVEN}
+{
+ \spec{N}{I}{number specifying observing station}
+}
+\args{GIVEN or RETURNED}
+{
+ \spec{C}{C*(*)}{identifier specifying observing station}
+}
+\args{RETURNED}
+{
+ \spec{NAME}{C*(*)}{name of specified observing station} \\
+ \spec{W}{D}{longitude (radians, west +ve)} \\
+ \spec{P}{D}{geodetic latitude (radians, north +ve)} \\
+ \spec{H}{D}{height above sea level (metres)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item Station identifiers C may be up to 10 characters long,
+        and station names NAME may be up to 40 characters long.
+  \item C and N are {\it alternative}\/ ways of specifying the observing
+        station.  The C option, which is the most generally useful,
+        may be selected by specifying an N value of zero or less.
+        If N is 1 or more, the parameters of the Nth station
+        in the currently supported list are interrogated, and
+        the station identifier C is returned as well as NAME, W,
+        P and H.
+  \item If the station parameters are not available, either because
+        the station identifier C is not recognized, or because an
+        N value greater than the number of stations supported is
+        given, a name of `?' is returned and W, P and H are left in
+        their current states.
+  \item Programs can obtain a list of all currently supported
+        stations by calling the routine repeatedly, with N=1,2,3...
+        When NAME=`?' is seen, the list of stations has been
+        exhausted.  The stations at the time of writing are listed
+        below.
+  \item Station numbers, identifiers, names and other details are
+        subject to change and should not be hardwired into
+        application programs.
+  \item All station identifiers C are uppercase only;  lower case
+        characters must be converted to uppercase by the calling
+        program.  The station names returned may contain both upper-
+        and lowercase.  All characters 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.
+  \item IMPORTANT -- BEWARE OF THE LONGITUDE SIGN CONVENTION.  The
+        longitude returned by sla\_OBS is
+        {\bf west-positive}, following the pre-1984 {\it Astronomical
+        Almanac}.  However, this sign convention is left-handed and is
+        the opposite of the one now used; elsewhere in
+        SLALIB the preferable east-positive convention is used.  In
+        particular, note that for use in sla\_AOP, sla\_AOPPA and
+        sla\_OAP the sign of the longitude must be reversed.
+  \item Users are urged to inform the author of any improvements
+        they would like to see made.  For example:
+        \begin{itemize}
+         \item typographical corrections
+         \item more accurate parameters
+         \item better station identifiers or names
+         \item additional stations
+        \end{itemize}
+ \end{enumerate}
+Stations supported by sla\_OBS at the time of writing:
+\begin{tabbing}
+xxxxxxxxxxxxxxxxx \= \kill
+{\it ID} \> {\it NAME} \\ \\
+AAT \> Anglo-Australian 3.9m Telescope \\
+ANU2.3 \> Siding Spring 2.3 metre \\
+APO3.5 \> Apache Point 3.5m \\
+ARECIBO \> Arecibo 1000 foot \\
+ATCA \> Australia Telescope Compact Array \\
+BLOEMF \> Bloemfontein 1.52 metre \\
+BOSQALEGRE \> Bosque Alegre 1.54 metre \\
+CAMB1MILE \> Cambridge 1 mile \\
+CAMB5KM \> Cambridge 5km \\
+CATALINA61 \> Catalina 61 inch \\
+CFHT \> Canada-France-Hawaii 3.6m Telescope \\
+CSO \> Caltech Sub-mm Observatory, Mauna Kea \\
+DAO72 \> DAO Victoria BC 1.85 metre \\
+DUNLAP74 \> David Dunlap 74 inch \\
+DUPONT \> Du Pont 2.5m Telescope, Las Campanas \\
+EFFELSBERG \> Effelsberg 100 metre \\
+ESO3.6 \> ESO 3.6 metre \\
+ESONTT \> ESO 3.5 metre NTT \\
+ESOSCHM \> ESO 1 metre Schmidt, La Silla \\
+FCRAO \> Five College Radio Astronomy Obs \\
+FLAGSTF61 \> USNO 61 inch astrograph, Flagstaff \\
+GBVA140 \> Greenbank 140 foot \\
+GBVA300 \> Greenbank 300 foot \\
+GEMININ \> Gemini North 8-m telescope \\
+HARVARD \> Harvard College Observatory 1.55m \\
+HPROV1.52 \> Haute Provence 1.52 metre \\
+HPROV1.93 \> Haute Provence 1.93 metre \\
+IRTF \> NASA IR Telescope Facility, Mauna Kea \\
+JCMT \> JCMT 15 metre \\
+JODRELL1 \> Jodrell Bank 250 foot \\
+KECK1 \> Keck 10m Telescope 1 \\
+KECK2 \> Keck 10m Telescope 2 \\
+KISO \> Kiso 1.05 metre Schmidt, Japan \\
+KOTTAMIA \> Kottamia 74 inch \\
+KPNO158 \> Kitt Peak 158 inch \\
+KPNO36FT \> Kitt Peak 36 foot \\
+KPNO84 \> Kitt Peak 84 inch \\
+KPNO90 \> Kitt Peak 90 inch \\
+LICK120 \> Lick 120 inch \\
+LOWELL72 \> Perkins 72 inch, Lowell \\
+LPO1 \> Jacobus Kapteyn 1m Telescope \\
+LPO2.5 \> Isaac Newton 2.5m Telescope \\
+LPO4.2 \> William Herschel 4.2m Telescope \\
+MAUNAK88 \> Mauna Kea 88 inch \\
+MCDONLD2.1 \> McDonald 2.1 metre \\
+MCDONLD2.7 \> McDonald 2.7 metre \\
+MMT \> MMT, Mt Hopkins \\
+MOPRA \> ATNF Mopra Observatory \\
+MTEKAR \> Mt Ekar 1.82 metre \\
+MTHOP1.5 \> Mt Hopkins 1.5 metre \\
+MTLEMMON60 \> Mt Lemmon 60 inch \\
+NOBEYAMA \> Nobeyama 45 metre \\
+OKAYAMA \> Okayama 1.88 metre \\
+PALOMAR200 \> Palomar 200 inch \\
+PALOMAR48 \> Palomar 48-inch Schmidt \\
+PALOMAR60 \> Palomar 60 inch \\
+PARKES \> Parkes 64 metre \\
+QUEBEC1.6 \> Quebec 1.6 metre \\
+SAAO74 \> Sutherland 74 inch \\
+SANPM83 \> San Pedro Martir 83 inch \\
+ST.ANDREWS \> St Andrews University Observatory \\
+STEWARD90 \> Steward 90 inch \\
+STROMLO74 \> Mount Stromlo 74 inch \\
+SUBARU \> Subaru 8 metre \\
+SUGARGROVE \> Sugar Grove 150 foot \\
+TAUTNBG \> Tautenburg 2 metre \\
+TAUTSCHM \> Tautenberg 1.34 metre Schmidt \\
+TIDBINBLA \> Tidbinbilla 64 metre \\
+TOLOLO1.5M \> Cerro Tololo 1.5 metre \\
+TOLOLO4M \> Cerro Tololo 4 metre \\
+UKIRT \> UK Infra Red Telescope \\
+UKST \> UK 1.2 metre Schmidt, Siding Spring \\
+USSR6 \> USSR 6 metre \\
+USSR600 \> USSR 600 foot \\
+VLA \> Very Large Array
+\end{tabbing}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_PA}{$h,\delta$ to Parallactic Angle}
+{
+ \action{Hour angle and declination to parallactic angle
+         (double precision).}
+ \call{D~=~sla\_PA (HA, DEC, PHI)}
+}
+\args{GIVEN}
+{
+ \spec{HA}{D}{hour angle in radians (geocentric apparent)} \\
+ \spec{DEC}{D}{declination in radians (geocentric apparent)} \\
+ \spec{PHI}{D}{latitude in radians (geodetic)}
+}
+\args{RETURNED}
+{
+ \spec{sla\_PA}{D}{parallactic angle (radians, in the range $\pm \pi$)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The parallactic angle at a point in the sky is the position
+        angle of the vertical, {\it 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 \hadec\ and to consider
+        separately the effects of atmospheric refraction and telescope
+        mount errors.
+  \item At the pole a zero result is returned.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_PAV}{Position-Angle Between Two Directions}
+{
+ \action{Returns the bearing (position angle) of one celestial
+         direction with respect to another (single precision).}
+ \call{R~=~sla\_PAV (V1, V2)}
+}
+\args{GIVEN}
+{
+ \spec{V1}{R(3)}{direction cosines of one point} \\
+ \spec{V2}{R(3)}{directions cosines of the other point}
+}
+\args{RETURNED}
+{
+ \spec{sla\_PAV}{R}{position-angle of 2nd point with respect to 1st}
+}
+\notes
+{
+ \begin{enumerate}
+ \item The coordinate frames correspond to \radec,
+       $[\lambda,\phi]$ {\it etc.}.
+ \item The result is the bearing (position angle), in radians,
+       of point V2 as seen
+       from point V1.  It is in the range $\pm \pi$.  The sense
+       is such that if V2
+       is a small distance due east of V1 the result
+       is about $+\pi/2$. Zero is returned
+       if the two points are coincident.
+ \item The routine sla\_BEAR performs an equivalent function except
+       that the points are specified in the form of spherical coordinates.
+ \end{enumerate}
+}
+%------------------------------------------------------------------------------
+\routine{SLA\_PCD}{Apply Radial Distortion}
+{
+ \action{Apply pincushion/barrel distortion to a tangent-plane \xy.}
+ \call{CALL sla\_PCD (DISCO,X,Y)}
+}
+\args{GIVEN}
+{
+ \spec{DISCO}{D}{pincushion/barrel distortion coefficient} \\
+ \spec{X,Y}{D}{tangent-plane \xy}
+}
+\args{RETURNED}
+{
+ \spec{X,Y}{D}{distorted \xy}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The distortion is of the form $\rho = r (1 + c r^{2})$, where $r$ is
+        the radial distance from the tangent point, $c$ is the DISCO
+        argument, and $\rho$ is the radial distance in the presence of
+        the distortion.
+  \item For {\it pincushion}\/ distortion, C is +ve;  for
+        {\it barrel}\/ distortion, C is $-$ve.
+  \item For X,Y in units of one projection radius (in the case of
+        a photographic plate, the focal length), the following
+        DISCO values apply:
+
+        \vspace{2ex}
+
+        \hspace{5em}
+        \begin{tabular}{|l|c|} \hline
+         Geometry & DISCO \\ \hline \hline
+         astrograph & 0.0 \\ \hline
+         Schmidt & $-$0.3333 \\ \hline
+         AAT PF doublet & +147.069 \\ \hline
+         AAT PF triplet & +178.585 \\ \hline
+         AAT f/8 & +21.20 \\ \hline
+         JKT f/8 & +14.6 \\ \hline
+        \end{tabular}
+
+        \vspace{2ex}
+
+  \item There is a companion routine, sla\_UNPCD, which performs
+        an approximately inverse operation.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_PDA2H}{H.A.\ for a Given Azimuth}
+{
+ \action{Hour Angle corresponding to a given azimuth (double precision).}
+ \call{CALL sla\_PDA2H (P, D, A, H1, J1, H2, J2)}
+}
+\args{GIVEN}
+{
+ \spec{P}{D}{latitude} \\
+ \spec{D}{D}{declination} \\
+ \spec{A}{D}{azimuth}
+}
+\args{RETURNED}
+{
+ \spec{H1}{D}{hour angle:  first solution if any} \\
+ \spec{J1}{I}{flag: 0 = solution 1 is valid} \\
+ \spec{H2}{D}{hour angle:  second solution if any} \\
+ \spec{J2}{I}{flag: 0 = solution 2 is valid}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_PDQ2H}{H.A.\ for a Given P.A.}
+{
+ \action{Hour Angle corresponding to a given parallactic angle
+         (double precision).}
+ \call{CALL sla\_PDQ2H (P, D, Q, H1, J1, H2, J2)}
+}
+\args{GIVEN}
+{
+ \spec{P}{D}{latitude} \\
+ \spec{D}{D}{declination} \\
+ \spec{Q}{D}{azimuth}
+}
+\args{RETURNED}
+{
+ \spec{H1}{D}{hour angle:  first solution if any} \\
+ \spec{J1}{I}{flag: 0 = solution 1 is valid} \\
+ \spec{H2}{D}{hour angle:  second solution if any} \\
+ \spec{J2}{I}{flag: 0 = solution 2 is valid}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_PERMUT}{Next Permutation}
+{
+ \action{Generate the next permutation of a specified number of items.}
+ \call{CALL sla\_PERMUT (N, ISTATE, IORDER, J)}
+}
+\args{GIVEN}
+{
+ \spec{N}{I}{number of items:  there will be N! permutations} \\
+ \spec{ISTATE}{I(N)}{state, ISTATE(1)$=-1$ to initialize}
+}
+\args{RETURNED}
+{
+ \spec{ISTATE}{I(N)}{state, updated ready for next time} \\
+ \spec{IORDER}{I(N)}{next permutation of numbers 1,2,\ldots,N} \\
+ \spec{J}{I}{status:} \\
+ \spec{}{}{\hspace{1.5em} $-$1 = illegal N (zero or less is illegal)} \\
+ \spec{}{}{\hspace{2.3em}    0 = OK} \\
+ \spec{}{}{\hspace{1.5em} $+$1 = no more permutations available}
+}
+\notes
+{
+ \begin{enumerate}
+  \item This routine returns, in the IORDER array, the integers 1 to N
+        inclusive, in an order that depends on the current contents of
+        the ISTATE array.  Before calling the routine for the first
+        time, the caller must set the first element of the ISTATE array
+        to $-1$ (any negative number will do) to cause the ISTATE array
+        to be fully initialized.
+  \item The first permutation to be generated is:
+        \begin{verse}
+           IORDER(1)=N, IORDER(2)=N-1, ..., IORDER(N)=1
+        \end{verse}
+        This is also the permutation returned for the ``finished'' (J=1) case.
+        The final permutation to be generated is:
+        \begin{verse}
+           IORDER(1)=1, IORDER(2)=2, ..., IORDER(N)=N
+        \end{verse}
+  \item If the ``finished'' (J=1) status is ignored, the routine continues
+        to deliver permutations, the pattern repeating every~N!\,~calls.
+ \end{enumerate}
+}
+%------------------------------------------------------------------------------
+\routine{SLA\_PERTEL}{Perturbed Orbital Elements}
+{
+ \action{Update the osculating elements of an asteroid or comet by
+         applying planetary perturbations.}
+ \call{CALL sla\_PERTEL (\vtop{
+         \hbox{JFORM, DATE0, DATE1,}
+         \hbox{EPOCH0, ORBI0, ANODE0, PERIH0, AORQ0, E0, AM0,}
+         \hbox{EPOCH1, ORBI1, ANODE1, PERIH1, AORQ1, E1, AM1,}
+         \hbox{JSTAT)}}}
+}
+\args{GIVEN (format and dates)}
+{
+ \spec{JFORM}{I}{choice of element set (2 or 3; Note~1)} \\
+ \spec{DATE0}{D}{date of osculation (TT MJD) for the given} \\
+ \spec{}{}{\hspace{1.5em} elements} \\
+ \spec{DATE1}{D}{date of osculation (TT MJD) for the updated} \\
+ \spec{}{}{\hspace{1.5em} elements}
+}
+\args{GIVEN (the unperturbed elements)}
+{
+ \spec{EPOCH0}{D}{epoch of the given element set
+                            ($t_0$ or $T$, TT MJD;} \\
+ \spec{}{}{\hspace{1.5em} Note~2)} \\
+ \spec{ORBI0}{D}{inclination ($i$, radians)} \\
+ \spec{ANODE0}{D}{longitude of the ascending node ($\Omega$, radians)} \\
+ \spec{PERIH0}{D}{argument of perihelion
+                            ($\omega$, radians)} \\
+ \spec{AORQ0}{D}{mean distance or perihelion distance ($a$ or $q$, AU)} \\
+ \spec{E0}{D}{eccentricity ($e$)} \\
+ \spec{AM0}{D}{mean anomaly ($M$, radians, JFORM=2 only)}
+}
+\args{RETURNED (the updated elements)}
+{
+ \spec{EPOCH1}{D}{epoch of the updated element set
+                            ($t_0$ or $T$,} \\
+ \spec{}{}{\hspace{1.5em} TT MJD; Note~2)} \\
+ \spec{ORBI1}{D}{inclination ($i$, radians)} \\
+ \spec{ANODE1}{D}{longitude of the ascending node ($\Omega$, radians)} \\
+ \spec{PERIH1}{D}{argument of perihelion
+                            ($\omega$, radians)} \\
+ \spec{AORQ1}{D}{mean distance or perihelion distance ($a$ or $q$, AU)} \\
+ \spec{E1}{D}{eccentricity ($e$)} \\
+ \spec{AM1}{D}{mean anomaly ($M$, radians, JFORM=2 only)}
+}
+\args{RETURNED (status flag)}
+{
+ \spec{JSTAT}{I}{status:} \\
+ \spec{}{}{\hspace{0.5em}+102 = warning, distant epoch} \\
+ \spec{}{}{\hspace{0.5em}+101 = warning, large timespan
+                                            ($>100$ years)} \\
+ \spec{}{}{\hspace{-1.3em}+1 to +8 = coincident with major planet
+                                                  (Note~6)} \\
+ \spec{}{}{\hspace{1.95em}       0 = OK} \\
+ \spec{}{}{\hspace{1.2em}    $-$1 = illegal JFORM} \\
+ \spec{}{}{\hspace{1.2em}    $-$2 = illegal E0} \\
+ \spec{}{}{\hspace{1.2em}    $-$3 = illegal AORQ0} \\
+ \spec{}{}{\hspace{1.2em}    $-$4 = internal error} \\
+ \spec{}{}{\hspace{1.2em}    $-$5 = numerical error}
+}
+\notes
+{
+ \begin{enumerate}
+  \item Two different element-format options are supported, as follows. \\
+
+        JFORM=2, suitable for minor planets:
+
+        \begin{tabbing}
+        xxx \= xxxxxxxx \= xx \= \kill
+        \> EPOCH  \> = \> epoch of elements $t_0$ (TT MJD) \\
+        \> ORBINC \> = \> inclination $i$ (radians) \\
+        \> ANODE  \> = \> longitude of the ascending node $\Omega$ (radians) \\
+        \> PERIH  \> = \> argument of perihelion $\omega$ (radians) \\
+        \> AORQ   \> = \> mean distance $a$ (AU) \\
+        \> E      \> = \> eccentricity $e$ $( 0 \leq e < 1 )$ \\
+        \> AORL   \> = \> mean anomaly $M$ (radians)
+        \end{tabbing}
+
+        JFORM=3, suitable for comets:
+
+        \begin{tabbing}
+        xxx \= xxxxxxxx \= xx \= \kill
+        \> EPOCH  \> = \> epoch of perihelion $T$ (TT MJD) \\
+        \> ORBINC \> = \> inclination $i$ (radians) \\
+        \> ANODE  \> = \> longitude of the ascending node $\Omega$ (radians) \\
+        \> PERIH  \> = \> argument of perihelion $\omega$ (radians) \\
+        \> AORQ   \> = \> perihelion distance $q$ (AU) \\
+        \> E      \> = \> eccentricity $e$ $( 0 \leq e \leq 10 )$
+        \end{tabbing}
+ \item 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).
+       \begin{itemize}
+       \item DATE0 is the instant at which the given
+             ({\it i.e.}\ unperturbed) osculating elements are correct.
+       \item DATE1 is the specified instant at which the updated osculating
+             elements are correct.
+       \item 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.
+       \end{itemize}
+ \item The elements are with respect to the J2000 ecliptic and mean equinox.
+ \item Unused elements (AM0 and AM1 for JFORM=3) are not accessed.
+ \item See the sla\_PERTUE routine for details of the algorithm used.
+ \item 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 (Mercury=1,\ldots,Neptune=8) as a warning.
+ \end{enumerate}
+}
+\aref{Sterne, Theodore E., {\it An Introduction to Celestial Mechanics,}\/
+      Interscience Publishers, 1960.  Section 6.7, p199.}
+%------------------------------------------------------------------------------
+\routine{SLA\_PERTUE}{Perturbed Universal Elements}
+{
+ \action{Update the universal elements of an asteroid or comet by
+         applying planetary perturbations.}
+ \call{CALL sla\_PERTUE (DATE, U, JSTAT)}
+}
+\args{GIVEN}
+{
+ \spec{DATE1}{D}{final epoch (TT MJD) for the updated elements}
+}
+\args{GIVEN and RETURNED}
+{
+ \spec{U}{D(13)}{universal elements (updated in place)} \\
+ \specel {(1)}     {combined mass ($M+m$)} \\
+ \specel {(2)}     {total energy of the orbit ($\alpha$)} \\
+ \specel {(3)}     {reference (osculating) epoch ($t_0$)} \\
+ \specel {(4-6)}   {position at reference epoch (${\rm \bf r}_0$)} \\
+ \specel {(7-9)}   {velocity at reference epoch (${\rm \bf v}_0$)} \\
+ \specel {(10)}    {heliocentric distance at reference epoch} \\
+ \specel {(11)}    {${\rm \bf r}_0.{\rm \bf v_0}$} \\
+ \specel {(12)}    {date ($t$)} \\
+ \specel {(13)}    {universal eccentric anomaly ($\psi$) of date, approx}
+}
+\args{RETURNED}
+{
+ \spec{JSTAT}{I}{status:} \\
+ \spec{}{}{\hspace{0.5em}+102 = warning, distant epoch} \\
+ \spec{}{}{\hspace{0.5em}+101 = warning, large timespan
+                                            ($>100$ years)} \\
+ \spec{}{}{\hspace{-1.3em}+1 to +8 = coincident with major planet
+                                                  (Note~5)} \\
+ \spec{}{}{\hspace{1.95em}       0 = OK} \\
+ \spec{}{}{\hspace{1.2em}    $-$1 = numerical error}
+}
+\notes
+{
+ \begin{enumerate}
+  \setlength{\parskip}{\medskipamount}
+  \item The ``universal'' elements are those which define the orbit for the
+        purposes of the method of universal variables (see reference 2).
+        They consist of the combined mass of the two bodies, an epoch,
+        and the position and velocity vectors (arbitrary reference frame)
+        at that epoch.  The parameter set used here includes also various
+        quantities that can, in fact, be derived from the other
+        information.  This approach is taken to avoiding unnecessary
+        computation and loss of accuracy.  The supplementary quantities
+        are (i)~$\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.
+  \item The universal elements are with respect to the J2000 equator and
+        equinox.
+  \item The epochs DATE, U(3) and U(12) are all Modified Julian Dates
+        (JD$-$2400000.5).
+  \item 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 sla\_PLANET.  Two
+        levels of interpolation are used, to enhance speed without
+        significantly degrading accuracy.  At a low frequency, the routine
+        sla\_PLANET is called to generate updated position+velocity ``state
+        vectors''.  The only task remaining to be carried out at the full
+        frequency ({\it 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, relativistic effects
+        are not taken into account and the Earth-Moon system is treated as
+        a single body.
+
+        In the interests of simplicity, the background calculations for
+        the major planets are carried out {\it 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.
+
+  \item 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 (Mercury=1,\ldots,Neptune=8) as a warning.
+ \end{enumerate}
+}
+\refs{
+   \begin{enumerate}
+   \item Sterne, Theodore E., {\it An Introduction to Celestial Mechanics,}\/
+         Interscience Publishers, 1960.  Section 6.7, p199.
+   \item Everhart, E. \& Pitkin, E.T., Am.~J.~Phys.~51, 712, 1983.
+   \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_PLANEL}{Planet Position from Elements}
+{
+ \action{Heliocentric position and velocity of a planet,
+         asteroid or comet, starting from orbital elements.}
+ \call{CALL sla\_PLANEL (\vtop{
+         \hbox{DATE, JFORM, EPOCH, ORBINC, ANODE, PERIH,}
+         \hbox{AORQ, E, AORL, DM, PV, JSTAT)}}}
+}
+\args{GIVEN}
+{
+ \spec{DATE}{D}{Modified Julian Date (JD$-$2400000.5)} \\
+ \spec{JFORM}{I}{choice of element set (1-3, see Note~3, below)} \\
+ \spec{EPOCH}{D}{epoch of elements ($t_0$ or $T$, TT MJD)} \\
+ \spec{ORBINC}{D}{inclination ($i$, radians)} \\
+ \spec{ANODE}{D}{longitude of the ascending node ($\Omega$, radians)} \\
+ \spec{PERIH}{D}{longitude or argument of perihelion
+                            ($\varpi$ or $\omega$,} \\
+ \spec{}{}{\hspace{1.5em} radians)} \\
+ \spec{AORQ}{D}{mean distance or perihelion distance ($a$ or $q$, AU)} \\
+ \spec{E}{D}{eccentricity ($e$)} \\
+ \spec{AORL}{D}{mean anomaly or longitude
+                               ($M$ or $L$, radians,} \\
+ \spec{}{}{\hspace{1.5em} JFORM=1,2 only)} \\
+ \spec{DM}{D}{daily motion ($n$, radians, JFORM=1 only)}
+}
+\args{RETURNED}
+{
+ \spec{PV}{D(6)}{heliocentric \xyzxyzd, equatorial, J2000} \\
+ \spec{}{}{\hspace{1.5em} (AU, AU/s)} \\
+ \spec{JSTAT}{I}{status:} \\
+ \spec{}{}{\hspace{2.3em}    0 = OK} \\
+ \spec{}{}{\hspace{1.5em} $-$1 = illegal JFORM} \\
+ \spec{}{}{\hspace{1.5em} $-$2 = illegal E} \\
+ \spec{}{}{\hspace{1.5em} $-$3 = illegal AORQ} \\
+ \spec{}{}{\hspace{1.5em} $-$4 = illegal DM} \\
+ \spec{}{}{\hspace{1.5em} $-$5 = numerical error}
+}
+\notes
+{
+ \begin{enumerate}
+  \item DATE is the instant for which the prediction is
+        required.  It is in the TT timescale (formerly
+        Ephemeris Time, ET) and is a
+        Modified Julian Date (JD$-$2400000.5).
+  \item The elements are with respect to
+        the J2000 ecliptic and equinox.
+  \item Three different element-format options are available, as
+        follows. \\
+
+        JFORM=1, suitable for the major planets:
+
+        \begin{tabbing}
+        xxx \= xxxxxxxx \= xx \= \kill
+        \> EPOCH  \> = \> epoch of elements $t_0$ (TT MJD) \\
+        \> ORBINC \> = \> inclination $i$ (radians) \\
+        \> ANODE  \> = \> longitude of the ascending node $\Omega$ (radians) \\
+        \> PERIH  \> = \> longitude of perihelion $\varpi$ (radians) \\
+        \> AORQ   \> = \> mean distance $a$ (AU) \\
+        \> E      \> = \> eccentricity $e$ $( 0 \leq e < 1 )$ \\
+        \> AORL   \> = \> mean longitude $L$ (radians) \\
+        \> DM     \> = \> daily motion $n$ (radians)
+        \end{tabbing}
+
+        JFORM=2, suitable for minor planets:
+
+        \begin{tabbing}
+        xxx \= xxxxxxxx \= xx \= \kill
+        \> EPOCH  \> = \> epoch of elements $t_0$ (TT MJD) \\
+        \> ORBINC \> = \> inclination $i$ (radians) \\
+        \> ANODE  \> = \> longitude of the ascending node $\Omega$ (radians) \\
+        \> PERIH  \> = \> argument of perihelion $\omega$ (radians) \\
+        \> AORQ   \> = \> mean distance $a$ (AU) \\
+        \> E      \> = \> eccentricity $e$ $( 0 \leq e < 1 )$ \\
+        \> AORL   \> = \> mean anomaly $M$ (radians)
+        \end{tabbing}
+
+        JFORM=3, suitable for comets:
+
+        \begin{tabbing}
+        xxx \= xxxxxxxx \= xx \= \kill
+        \> EPOCH  \> = \> epoch of perihelion $T$ (TT MJD) \\
+        \> ORBINC \> = \> inclination $i$ (radians) \\
+        \> ANODE  \> = \> longitude of the ascending node $\Omega$ (radians) \\
+        \> PERIH  \> = \> argument of perihelion $\omega$ (radians) \\
+        \> AORQ   \> = \> perihelion distance $q$ (AU) \\
+        \> E      \> = \> eccentricity $e$ $( 0 \leq e \leq 10 )$
+        \end{tabbing}
+  \item Unused elements (DM for JFORM=2, AORL and DM for JFORM=3) are
+        not accessed.
+  \item The reference frame for the result is equatorial and is with
+        respect to the mean equinox and ecliptic of epoch J2000.
+  \item 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.
+ \end{enumerate}
+}
+\aref{Everhart, E. \& Pitkin, E.T., Am.~J.~Phys.~51, 712, 1983.}
+%------------------------------------------------------------------------------
+\routine{SLA\_PLANET}{Planetary Ephemerides}
+{
+ \action{Approximate heliocentric position and velocity of a planet.}
+ \call{CALL sla\_PLANET (DATE, NP, PV, JSTAT)}
+}
+\args{GIVEN}
+{
+ \spec{DATE}{D}{Modified Julian Date (JD$-$2400000.5)} \\
+ \spec{NP}{I}{planet:} \\
+ \spec{}{}{\hspace{1.5em} 1\,=\,Mercury} \\
+ \spec{}{}{\hspace{1.5em} 2\,=\,Venus} \\
+ \spec{}{}{\hspace{1.5em} 3\,=\,Earth-Moon Barycentre} \\
+ \spec{}{}{\hspace{1.5em} 4\,=\,Mars} \\
+ \spec{}{}{\hspace{1.5em} 5\,=\,Jupiter} \\
+ \spec{}{}{\hspace{1.5em} 6\,=\,Saturn} \\
+ \spec{}{}{\hspace{1.5em} 7\,=\,Uranus} \\
+ \spec{}{}{\hspace{1.5em} 8\,=\,Neptune} \\
+ \spec{}{}{\hspace{1.5em} 9\,=\,Pluto}
+}
+\args{RETURNED}
+{
+ \spec{PV}{D(6)}{heliocentric \xyzxyzd, equatorial, J2000} \\
+ \spec{}{}{\hspace{1.5em} (AU, AU/s)} \\
+ \spec{JSTAT}{I}{status:} \\
+ \spec{}{}{\hspace{1.5em} $+$1 = warning: date outside of range} \\
+ \spec{}{}{\hspace{2.3em}    0 = OK} \\
+ \spec{}{}{\hspace{1.5em} $-$1 = illegal NP (outside 1-9)} \\
+ \spec{}{}{\hspace{1.5em} $-$2 = solution didn't converge}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The epoch, DATE, is in the TDB timescale and is in the form
+        of a Modified Julian Date (JD$-$2400000.5).
+  \item The reference frame is equatorial and is with respect to
+        the mean equinox and ecliptic of epoch J2000.
+  \item If a planet number, NP, outside the range 1-9 is supplied, an error
+        status is returned (JSTAT~=~$-1$) and the PV vector
+        is set to zeroes.
+  \item The algorithm for obtaining the mean elements of the
+        planets from Mercury to Neptune is due to
+        J.\,L.\,Simon, P.\,Bretagnon, J.\,Chapront,
+        M.\,Chapront-Touze, G.\,Francou and J.\,Laskar (Bureau des
+        Longitudes, Paris, France).  The (completely different)
+        algorithm for calculating the ecliptic coordinates of
+        Pluto is by Meeus.
+  \item Comparisons of the present routine with the JPL DE200 ephemeris
+        give the following RMS errors over the interval 1960-2025:
+        \begin{tabbing}
+         xxxxx \= xxxxxxxxxxxxxxxxx \= xxxxxxxxxxxxxx \= \kill
+         \> \> {\it position (km)} \> {\it speed (metre/sec)} \\ \\
+         \> Mercury \> \hspace{2em}334 \> \hspace{2.5em}0.437 \\
+         \> Venus   \> \hspace{1.5em}1060 \> \hspace{2.5em}0.855 \\
+         \> EMB     \> \hspace{1.5em}2010 \> \hspace{2.5em}0.815 \\
+         \> Mars    \> \hspace{1.5em}7690 \> \hspace{2.5em}1.98 \\
+         \> Jupiter \> \hspace{1em}71700 \> \hspace{2.5em}7.70 \\
+         \> Saturn  \> \hspace{0.5em}199000 \> \hspace{2em}19.4 \\
+         \> Uranus  \> \hspace{0.5em}564000 \> \hspace{2em}16.4 \\
+         \> Neptune \> \hspace{0.5em}158000 \> \hspace{2em}14.4 \\
+         \> Pluto \> \hspace{1em}36400 \> \hspace{2.5em}0.137
+        \end{tabbing}
+        From comparisons with DE102, Simon {\it et al.}\/ quote the following
+        longitude accuracies over the interval 1800-2200:
+        \begin{tabbing}
+         xxxxx \= xxxxxxxxxxxxxxxxxxxx \= \kill
+         \> Mercury \> \hspace{0.5em}\arcseci{4} \\
+         \> Venus   \> \hspace{0.5em}\arcseci{5} \\
+         \> EMB     \> \hspace{0.5em}\arcseci{6} \\
+         \> Mars    \> \arcseci{17} \\
+         \> Jupiter \> \arcseci{71} \\
+         \> Saturn  \> \arcseci{81} \\
+         \> Uranus  \> \arcseci{86} \\
+         \> Neptune \> \arcseci{11}
+        \end{tabbing}
+        In the case of Pluto, Meeus quotes an accuracy of \arcsec{0}{6}
+        in longitude and \arcsec{0}{2} in latitude for the period
+        1885-2099.
+
+        For all except Pluto, over the period 1000-3000,
+        the accuracy is better than 1.5
+        times that over 1800-2200.  Outside the interval 1000-3000 the
+        accuracy declines.  For Pluto the accuracy declines rapidly
+        outside the period 1885-2099.  Outside these ranges
+        (1885-2099 for Pluto, 1000-3000 for the rest) a ``date out
+        of range'' warning status ({\tt JSTAT=+1}) is returned.
+  \item The algorithms for (i)~Mercury through Neptune and
+        (ii)~Pluto are completely independent.  In the Mercury
+        through Neptune case, the present SLALIB
+        implementation differs from the original
+        Simon {\it et al.}\/ Fortran code in the following respects:
+        \begin{itemize}
+         \item The date is supplied as a Modified Julian Date rather
+               a Julian Date (${\rm MJD} = ({\rm JD} - 2400000.5$).
+         \item The result is returned only in equatorial
+               Cartesian form;  the ecliptic
+               longitude, latitude and radius vector are not returned.
+         \item The velocity is in AU per second, not AU per day.
+         \item Different error/warning status values are used.
+         \item Kepler's Equation is not solved inline.
+         \item Polynomials in T are nested to minimize rounding errors.
+         \item Explicit double-precision constants are used to avoid
+               mixed-mode expressions.
+         \item There are other, cosmetic, changes to comply with
+               Starlink/SLALIB style guidelines.
+        \end{itemize}
+        None of the above changes affects the result significantly.
+  \item NP\,=\,3 the result is for the Earth-Moon Barycentre.  To
+        obtain the heliocentric position and velocity of the Earth,
+        either use the SLALIB routine sla\_EVP or call sla\_DMOON and
+        subtract 0.012150581 times the geocentric Moon vector from
+        the EMB vector produced by the present routine.  (The Moon
+        vector should be precessed to J2000 first, but this can
+        be omitted for modern epochs without introducing significant
+        inaccuracy.)
+ \end{enumerate}
+\refs
+{
+ \begin{enumerate}
+  \item Simon {\it et al.,}\/
+        Astron.\ Astrophys.\ {\bf 282}, 663 (1994).
+  \item Meeus, J.,
+        {\it Astronomical Algorithms,}\/ Willmann-Bell (1991).
+ \end{enumerate}
+}
+}
+%------------------------------------------------------------------------------
+\routine{SLA\_PLANTE}{\radec\ of Planet from Elements}
+{
+ \action{Topocentric apparent \radec\ of a Solar-System object whose
+         heliocentric orbital elements are known.}
+ \call{CALL sla\_PLANTE (\vtop{
+         \hbox{DATE, ELONG, PHI, JFORM, EPOCH, ORBINC, ANODE, PERIH,}
+         \hbox{AORQ, E, AORL, DM, RA, DEC, R, JSTAT)}}}
+}
+\args{GIVEN}
+{
+ \spec{DATE}{D}{MJD of observation (JD$-$2400000.5)} \\
+ \spec{ELONG,PHI}{D}{observer's longitude (east +ve) and latitude} \\
+ \spec{}{}{\hspace{1.5em} radians)} \\
+ \spec{JFORM}{I}{choice of element set (1-3, see Note~4, below)} \\
+ \spec{EPOCH}{D}{epoch of elements ($t_0$ or $T$, TT MJD)} \\
+ \spec{ORBINC}{D}{inclination ($i$, radians)} \\
+ \spec{ANODE}{D}{longitude of the ascending node ($\Omega$, radians)} \\
+ \spec{PERIH}{D}{longitude or argument of perihelion
+                            ($\varpi$ or $\omega$,} \\
+ \spec{}{}{\hspace{1.5em} radians)} \\
+ \spec{AORQ}{D}{mean distance or perihelion distance ($a$ or $q$, AU)} \\
+ \spec{E}{D}{eccentricity ($e$)} \\
+ \spec{AORL}{D}{mean anomaly or longitude ($M$ or $L$,} \\
+  \spec{}{}{\hspace{1.5em} radians, JFORM=1,2 only)} \\
+ \spec{DM}{D}{daily motion ($n$, radians, JFORM=1 only)}
+}
+\args{RETURNED}
+{
+ \spec{RA,DEC}{D}{topocentric apparent \radec\ (radians)} \\
+ \spec{R}{D}{distance from observer (AU)} \\
+ \spec{JSTAT}{I}{status:} \\
+ \spec{}{}{\hspace{2.3em}    0 = OK} \\
+ \spec{}{}{\hspace{1.5em} $-$1 = illegal JFORM} \\
+ \spec{}{}{\hspace{1.5em} $-$2 = illegal E} \\
+ \spec{}{}{\hspace{1.5em} $-$3 = illegal AORQ} \\
+ \spec{}{}{\hspace{1.5em} $-$4 = illegal DM} \\
+ \spec{}{}{\hspace{1.5em} $-$5 = numerical error}
+}
+\notes
+{
+ \begin{enumerate}
+  \item DATE is the instant for which the prediction is
+        required.  It is in the TT timescale (formerly
+        Ephemeris Time, ET) and is a
+        Modified Julian Date (JD$-$2400000.5).
+  \item The longitude and latitude allow correction for geocentric
+        parallax.  This is usually a small effect, but can become
+        important for Earth-crossing asteroids.  Geocentric positions
+        can be generated by appropriate use of the routines
+        sla\_EVP and sla\_PLANEL.
+  \item The elements are with respect to the J2000 ecliptic and equinox.
+  \item Three different element-format options are available, as
+        follows. \\
+
+        JFORM=1, suitable for the major planets:
+
+        \begin{tabbing}
+        xxx \= xxxxxxx \= xx \= \kill
+        \> EPOCH  \> = \> epoch of elements $t_0$ (TT MJD) \\
+        \> ORBINC \> = \> inclination $i$ (radians) \\
+        \> ANODE  \> = \> longitude of the ascending node $\Omega$ (radians) \\
+        \> PERIH  \> = \> longitude of perihelion $\varpi$ (radians) \\
+        \> AORQ   \> = \> mean distance $a$ (AU) \\
+        \> E      \> = \> eccentricity $e$ \\
+        \> AORL   \> = \> mean longitude $L$ (radians) \\
+        \> DM     \> = \> daily motion $n$ (radians)
+        \end{tabbing}
+
+        JFORM=2, suitable for minor planets:
+
+        \begin{tabbing}
+        xxx \= xxxxxxx \= xx \= \kill
+        \> EPOCH  \> = \> epoch of elements $t_0$ (TT MJD) \\
+        \> ORBINC \> = \> inclination $i$ (radians) \\
+        \> ANODE  \> = \> longitude of the ascending node $\Omega$ (radians) \\
+        \> PERIH  \> = \> argument of perihelion $\omega$ (radians) \\
+        \> AORQ   \> = \> mean distance $a$ (AU) \\
+        \> E      \> = \> eccentricity $e$ \\
+        \> AORL   \> = \> mean anomaly $M$ (radians)
+        \end{tabbing}
+
+        JFORM=3, suitable for comets:
+
+        \begin{tabbing}
+        xxx \= xxxxxxx \= xx \= \kill
+        \> EPOCH  \> = \> epoch of perihelion $T$ (TT MJD) \\
+        \> ORBINC \> = \> inclination $i$ (radians) \\
+        \> ANODE  \> = \> longitude of the ascending node $\Omega$ (radians) \\
+        \> PERIH  \> = \> argument of perihelion $\omega$ (radians) \\
+        \> AORQ   \> = \> perihelion distance $q$ (AU) \\
+        \> E      \> = \> eccentricity $e$
+        \end{tabbing}
+  \item Unused elements (DM for JFORM=2, AORL and DM for JFORM=3) are
+        not accessed.
+ \end{enumerate}
+}
+%------------------------------------------------------------------------------
+\routine{SLA\_PM}{Proper Motion}
+{
+ \action{Apply corrections for proper motion to a star \radec.}
+ \call{CALL sla\_PM (R0, D0, PR, PD, PX, RV, EP0, EP1, R1, D1)}
+}
+\args{GIVEN}
+{
+ \spec{R0,D0}{D}{\radec\ at epoch EP0 (radians)} \\
+ \spec{PR,PD}{D}{proper motions:  rate of change of 
+                 \radec\  (radians per year)} \\
+ \spec{PX}{D}{parallax (arcsec)} \\
+ \spec{RV}{D}{radial velocity (km~s$^{-1}$, +ve if receding)} \\
+ \spec{EP0}{D}{start epoch in years ({\it e.g.}\ Julian epoch)} \\
+ \spec{EP1}{D}{end epoch in years (same system as EP0)}
+}
+\args{RETURNED}
+{
+ \spec{R1,D1}{D}{\radec\ at epoch EP1 (radians)}
+}
+\anote{The $\alpha$ proper motions are $\dot{\alpha}$ rather than
+       $\dot{\alpha}\cos\delta$, and are in the same coordinate
+       system as R0,D0.}
+\refs
+{
+ \begin{enumerate}
+  \item 1984 {\it Astronomical Almanac}, pp B39-B41.
+  \item Lederle \& Schwan, 1984.\ {\it Astr. Astrophys.}\ {\bf 134}, 1-6.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_POLMO}{Polar Motion}
+{
+ \action{Polar motion:  correct site longitude and latitude for polar
+         motion and calculate azimuth difference between celestial and
+         terrestrial poles.}
+ \call{CALL sla\_POLMO (ELONGM, PHIM, XP, YP, ELONG, PHI, DAZ)}
+}
+\args{GIVEN}
+{
+ \spec{ELONGM}{D}{mean longitude of the site (radians, east +ve)} \\
+ \spec{PHIM}{D}{mean geodetic latitude of the site (radians)} \\
+ \spec{XP}{D}{polar motion $x$-coordinate (radians)} \\
+ \spec{YP}{D}{polar motion $y$-coordinate (radians)}
+}
+\args{RETURNED}
+{
+ \spec{ELONG}{D}{true longitude of the site (radians, east +ve)} \\
+ \spec{PHI}{D}{true geodetic latitude of the site (radians)} \\
+ \spec{DAZ}{D}{azimuth correction (terrestrial$-$celestial, radians)}
+}
+\notes
+{
+\begin{enumerate}
+\item ``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.
+\item 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 $0^\circ$,
+      and YP is positive along the meridian at longitude
+      $270^\circ$ ({\it i.e.}\ $90^\circ$ west).  Values for XP,YP can
+      be obtained from IERS circulars and equivalent publications;
+      the maximum amplitude observed so far is about \arcsec{0}{3}.
+\item ``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 {\it etc}).
+\item 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.
+\item The present routine is rigorous.  For most practical
+      purposes, the following simplified formulae provide an
+      adequate approximation: \\[2ex]
+      \hspace*{1em}\begin{tabular}{lll}
+        {\tt ELONG} & {\tt =} &
+             {\tt ELONGM+XP*COS(ELONGM)-YP*SIN(ELONGM)} \\
+        {\tt PHI  } & {\tt =} &
+             {\tt PHIM+(XP*SIN(ELONGM)+YP*COS(ELONGM))*TAN(PHIM)} \\
+        {\tt DAZ  } & {\tt =} &
+             {\tt -SQRT(XP*XP+YP*YP)*COS(ELONGM-ATAN2(XP,YP))/COS(PHIM)} \\
+      \end{tabular} \\[2ex]
+      An alternative formulation for DAZ is:\\[2ex]
+      \hspace*{1em}\begin{tabular}{lll}
+        {\tt X  } & {\tt =} & {\tt COS(ELONGM)*COS(PHIM)} \\
+        {\tt Y  } & {\tt =} & {\tt SIN(ELONGM)*COS(PHIM)} \\
+        {\tt DAZ} & {\tt =} & {\tt ATAN2(-X*YP-Y*XP,X*X+Y*Y)} \\
+      \end{tabular}
+\end{enumerate}
+}
+\aref{Seidelmann, P.K.\ (ed), 1992.  {\it Explanatory
+      Supplement to the Astronomical Almanac,}\/ ISBN~0-935702-68-7,
+      sections 3.27, 4.25, 4.52.}
+%-----------------------------------------------------------------------
+\routine{SLA\_PREBN}{Precession Matrix (FK4)}
+{
+ \action{Generate the matrix of precession between two epochs,
+         using the old, pre IAU~1976, Bessel-Newcomb model, in
+         Andoyer's formulation.}
+ \call{CALL sla\_PREBN (BEP0, BEP1, RMATP)}
+}
+\args{GIVEN}
+{
+ \spec{BEP0}{D}{beginning Besselian epoch} \\
+ \spec{BEP1}{D}{ending Besselian epoch}
+}
+\args{RETURNED}
+{
+ \spec{RMATP}{D(3,3)}{precession matrix}
+}
+\anote{The matrix is in the sense:
+       \begin{verse}
+        {\bf v}$_{1}$ =  {\bf M}$\cdot${\bf v}$_{0}$
+       \end{verse}
+       where {\bf v}$_{1}$ is the star vector relative to the
+       mean equator and equinox of epoch BEP1, {\bf M} is the
+       $3\times3$ matrix RMATP and
+       {\bf v}$_{0}$ is the star vector relative to the
+       mean equator and equinox of epoch BEP0.}
+\aref{Smith {\it et al.}, 1989.\ {\it Astr.J.}\ {\bf 97}, 269.}
+%-----------------------------------------------------------------------
+\routine{SLA\_PREC}{Precession Matrix (FK5)}
+{
+ \action{Form the matrix of precession between two epochs (IAU 1976, FK5).}
+ \call{CALL sla\_PREC (EP0, EP1, RMATP)}
+}
+\args{GIVEN}
+{
+ \spec{EP0}{D}{beginning epoch} \\
+ \spec{EP1}{D}{ending epoch}
+}
+\args{RETURNED}
+{
+ \spec{RMATP}{D(3,3)}{precession matrix}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The epochs are TDB Julian epochs.
+  \item The matrix is in the sense:
+        \begin{verse}
+         {\bf v}$_{1}$ =  {\bf M}$\cdot${\bf v}$_{0}$
+        \end{verse}
+        where {\bf v}$_{1}$ is the star vector relative to the
+        mean equator and equinox of epoch EP1, {\bf M} is the
+        $3\times3$ matrix RMATP and
+        {\bf v}$_{0}$ is the star vector relative to the
+        mean equator and equinox of epoch EP0.
+  \item Though the matrix method itself is rigorous, the precession
+        angles are expressed through canonical polynomials which are
+        valid only for a limited time span.  There are also known
+        errors in the IAU precession rate.  The absolute accuracy
+        of the present formulation is better than \arcsec{0}{1} from
+        1960\,AD to 2040\,AD, better than \arcseci{1} from 1640\,AD to 2360\,AD,
+        and remains below \arcseci{3} for the whole of the period
+        500\,BC to 3000\,AD.  The errors exceed \arcseci{10} outside the
+        range 1200\,BC to 3900\,AD, exceed \arcseci{100} outside 4200\,BC to
+        5600\,AD and exceed \arcseci{1000} outside 6800\,BC to 8200\,AD.
+        The SLALIB routine sla\_PRECL implements a more elaborate
+        model which is suitable for problems spanning several
+        thousand years.
+ \end{enumerate}
+}
+\refs
+{
+ \begin{enumerate}
+  \item Lieske, J.H., 1979.\ {\it Astr.Astrophys.}\ {\bf 73}, 282;
+        equations 6 \& 7, p283.
+  \item Kaplan, G.H., 1981.\ {\it USNO circular no.\ 163}, pA2.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_PRECES}{Precession}
+{
+ \action{Precession -- either the old ``FK4'' (Bessel-Newcomb, pre~IAU~1976)
+         or new ``FK5'' (Fricke, post~IAU~1976) as required.}
+ \call{CALL sla\_PRECES (SYSTEM, EP0, EP1, RA, DC)}
+}
+\args{GIVEN}
+{
+ \spec{SYSTEM}{C}{precession to be applied: `FK4' or `FK5'} \\
+ \spec{EP0,EP1}{D}{starting and ending epoch} \\
+ \spec{RA,DC}{D}{\radec, mean equator \& equinox of epoch EP0}
+}
+\args{RETURNED}
+{
+ \spec{RA,DC}{D}{\radec, mean equator \& equinox of epoch EP1}
+}
+\notes
+{
+ \begin{enumerate}
+  \item Lowercase characters in SYSTEM are acceptable.
+  \item 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:
+        \begin{quote}
+         {\tt CALL sla\_PRECES ('FK4', 1900D0, 1950D0, RA, DC)}
+        \end{quote}
+  \item This routine will {\bf NOT} correctly convert between the old and
+        the new systems -- for example conversion from B1950 to J2000.
+        For these purposes see sla\_FK425, sla\_FK524, sla\_FK45Z and
+        sla\_FK54Z.
+  \item If an invalid SYSTEM is supplied, values of $-$99D0,$-$99D0 are
+        returned for both RA and DC.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_PRECL}{Precession Matrix (latest)}
+{
+ \action{Form the matrix of precession between two epochs, using the
+         model of Simon {\it et al}.\ (1994), which is suitable for long
+         periods of time.}
+ \call{CALL sla\_PRECL (EP0, EP1, RMATP)}
+}
+\args{GIVEN}
+{
+ \spec{EP0}{D}{beginning epoch} \\
+ \spec{EP1}{D}{ending epoch}
+}
+\args{RETURNED}
+{
+ \spec{RMATP}{D(3,3)}{precession matrix}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The epochs are TDB Julian epochs.
+  \item The matrix is in the sense:
+        \begin{verse}
+         {\bf v}$_{1}$ =  {\bf M}$\cdot${\bf v}$_{0}$
+        \end{verse}
+        where {\bf v}$_{1}$ is the star vector relative to the
+        mean equator and equinox of epoch EP1, {\bf M} is the
+        $3\times3$ matrix RMATP and
+        {\bf v}$_{0}$ is the star vector relative to the
+        mean equator and equinox of epoch EP0.
+  \item The absolute accuracy of the model is limited by the
+        uncertainty in the general precession, about \arcsec{0}{3} per
+        1000~years.  The remainder of the formulation provides a
+        precision of 1~milliarcsecond over the interval from 1000\,AD
+        to 3000\,AD, \arcsec{0}{1} from 1000\,BC to 5000\,AD and
+        \arcseci{1} from 4000\,BC to 8000\,AD.
+ \end{enumerate}
+}
+\aref{Simon, J.L.\ {\it et al}., 1994.\ {\it Astr.Astrophys.}\ {\bf 282},
+      663.}
+%-----------------------------------------------------------------------
+\routine{SLA\_PRENUT}{Precession/Nutation Matrix}
+{
+ \action{Form the matrix of precession and nutation (IAU~1976, FK5).}
+ \call{CALL sla\_PRENUT (EPOCH, DATE, RMATPN)}
+}
+\args{GIVEN}
+{
+ \spec{EPOCH}{D}{Julian Epoch for mean coordinates} \\
+ \spec{DATE}{D}{Modified Julian Date (JD$-$2400000.5)
+                       for true coordinates}
+}
+\args{RETURNED}
+{
+ \spec{RMATPN}{D(3,3)}{combined precession/nutation matrix}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The epoch and date are TDB.
+  \item The matrix is in the sense:
+        \begin{verse}
+         {\bf v}$_{true}$ =  {\bf M}$\cdot${\bf v}$_{mean}$
+        \end{verse}
+        where {\bf v}$_{true}$ is the star vector relative to the
+        true equator and equinox of epoch DATE, {\bf M} is the
+        $3\times3$ matrix RMATPN and
+        {\bf v}$_{mean}$ is the star vector relative to the
+        mean equator and equinox of epoch EPOCH.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_PV2EL}{Orbital Elements from Position/Velocity}
+{
+ \action{Heliocentric osculating elements obtained from instantaneous
+         position and velocity.}
+ \call{CALL sla\_PV2EL (\vtop{
+         \hbox{PV, DATE, PMASS, JFORMR, JFORM, EPOCH, ORBINC,}
+         \hbox{ANODE, PERIH, AORQ, E, AORL, DM, JSTAT)}}}
+}
+\args{GIVEN}
+{
+ \spec{PV}{D(6)}{heliocentric \xyzxyzd, equatorial, J2000} \\
+ \spec{}{}{\hspace{1.5em} (AU, AU/s; Note~1)} \\
+ \spec{DATE}{D}{date (TT Modified Julian Date = JD$-$2400000.5)} \\
+ \spec{PMASS}{D}{mass of the planet (Sun = 1; Note~2)} \\
+ \spec{JFORMR}{I}{requested element set (1-3; Note~3)}
+}
+\args{RETURNED}
+{
+ \spec{JFORM}{I}{element set actually returned (1-3; Note~4)} \\
+ \spec{EPOCH}{D}{epoch of elements ($t_0$ or $T$, TT MJD)} \\
+ \spec{ORBINC}{D}{inclination ($i$, radians)} \\
+ \spec{ANODE}{D}{longitude of the ascending node ($\Omega$, radians)} \\
+ \spec{PERIH}{D}{longitude or argument of perihelion
+                            ($\varpi$ or $\omega$,} \\
+ \spec{}{}{\hspace{1.5em} radians)} \\
+ \spec{AORQ}{D}{mean distance or perihelion distance ($a$ or $q$, AU)} \\
+ \spec{E}{D}{eccentricity ($e$)} \\
+ \spec{AORL}{D}{mean anomaly or longitude
+                               ($M$ or $L$, radians,} \\
+ \spec{}{}{\hspace{1.5em} JFORM=1,2 only)} \\
+ \spec{DM}{D}{daily motion ($n$, radians, JFORM=1 only)} \\
+ \spec{JSTAT}{I}{status:} \\
+ \spec{}{}{\hspace{2.3em}    0 = OK} \\
+ \spec{}{}{\hspace{1.5em} $-$1 = illegal PMASS} \\
+ \spec{}{}{\hspace{1.5em} $-$2 = illegal JFORMR} \\
+ \spec{}{}{\hspace{1.5em} $-$3 = position/velocity out of allowed range}
+}
+\notes
+{
+ \begin{enumerate}
+  \item 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.
+  \item The mass, PMASS, is important only for the larger planets.  For
+        most purposes ({\it e.g.}~asteroids) use 0D0.  Values less than zero
+        are illegal.
+  \item Three different element-format options are supported, as
+        follows. \\
+
+        JFORM=1, suitable for the major planets:
+
+        \begin{tabbing}
+        xxx \= xxxxxxxx \= xx \= \kill
+        \> EPOCH  \> = \> epoch of elements $t_0$ (TT MJD) \\
+        \> ORBINC \> = \> inclination $i$ (radians) \\
+        \> ANODE  \> = \> longitude of the ascending node $\Omega$ (radians) \\
+        \> PERIH  \> = \> longitude of perihelion $\varpi$ (radians) \\
+        \> AORQ   \> = \> mean distance $a$ (AU) \\
+        \> E      \> = \> eccentricity $e$ $( 0 \leq e < 1 )$ \\
+        \> AORL   \> = \> mean longitude $L$ (radians) \\
+        \> DM     \> = \> daily motion $n$ (radians)
+        \end{tabbing}
+
+        JFORM=2, suitable for minor planets:
+
+        \begin{tabbing}
+        xxx \= xxxxxxxx \= xx \= \kill
+        \> EPOCH  \> = \> epoch of elements $t_0$ (TT MJD) \\
+        \> ORBINC \> = \> inclination $i$ (radians) \\
+        \> ANODE  \> = \> longitude of the ascending node $\Omega$ (radians) \\
+        \> PERIH  \> = \> argument of perihelion $\omega$ (radians) \\
+        \> AORQ   \> = \> mean distance $a$ (AU) \\
+        \> E      \> = \> eccentricity $e$ $( 0 \leq e < 1 )$ \\
+        \> AORL   \> = \> mean anomaly $M$ (radians)
+        \end{tabbing}
+
+        JFORM=3, suitable for comets:
+
+        \begin{tabbing}
+        xxx \= xxxxxxxx \= xx \= \kill
+        \> EPOCH  \> = \> epoch of perihelion $T$ (TT MJD) \\
+        \> ORBINC \> = \> inclination $i$ (radians) \\
+        \> ANODE  \> = \> longitude of the ascending node $\Omega$ (radians) \\
+        \> PERIH  \> = \> argument of perihelion $\omega$ (radians) \\
+        \> AORQ   \> = \> perihelion distance $q$ (AU) \\
+        \> E      \> = \> eccentricity $e$ $( 0 \leq e \leq 10 )$
+        \end{tabbing}
+  \item 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:
+
+        \begin{tabbing}
+        xx \= xxxxxxxxxx \= xxxxxxxxxxx \= \kill
+        \> 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
+        \end{tabbing}
+  \item The arguments returned for each value of JFORM ({\it cf}\/ Note~5:
+        JFORM may not be the same as JFORMR) are as follows:
+
+        \begin{tabbing}
+        xxx \= xxxxxxxxxxxx \= xxxxxx \= xxxxxx \= \kill
+        \> JFORM  \> 1        \> 2        \> 3 \\ \\
+        \> EPOCH  \> $t_0$    \> $t_0$    \> $T$ \\
+        \> ORBINC \> $i$      \> $i$      \> $i$ \\
+        \> ANODE  \> $\Omega$ \> $\Omega$ \> $\Omega$ \\
+        \> PERIH  \> $\varpi$ \> $\omega$ \> $\omega$ \\
+        \> AORQ   \> $a$      \> $a$      \> $q$ \\
+        \> E      \> $e$      \> $e$      \> $e$ \\
+        \> AORL   \> $L$      \> $M$      \> - \\
+        \> DM     \> $n$      \> -        \> -
+        \end{tabbing}
+
+        where:
+        \begin{tabbing}
+        xxx \= xxxxxxxx \= xxx \= \kill
+        \> $t_0$    \> is the epoch of the elements (MJD, TT) \\
+        \> $T$      \> is the epoch of perihelion (MJD, TT) \\
+        \> $i$      \> is the inclination (radians) \\
+        \> $\Omega$ \> is the longitude of the ascending node (radians) \\
+        \> $\varpi$ \> is the longitude of perihelion (radians) \\
+        \> $\omega$ \> is the argument of perihelion (radians) \\
+        \> $a$      \> is the mean distance (AU) \\
+        \> $q$      \> is the perihelion distance (AU) \\
+        \> $e$      \> is the eccentricity \\
+        \> $L$      \> is the longitude (radians, $0-2\pi$) \\
+        \> $M$      \> is the mean anomaly (radians, $0-2\pi$) \\
+        \> $n$      \> is the daily motion (radians) \\
+        \> - \> means no value is set
+        \end{tabbing}
+  \item 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.
+ \end{enumerate}
+}
+\aref{Sterne, Theodore E., {\it An Introduction to Celestial Mechanics,}\/
+      Interscience Publishers, 1960.}
+%-----------------------------------------------------------------------
+\routine{SLA\_PV2UE}{Position/Velocity to Universal Elements}
+{
+ \action{Construct a universal element set based on an instantaneous
+         position and velocity.}
+ \call{CALL sla\_PV2UE (PV, DATE, PMASS, U, JSTAT)}
+}
+\args{GIVEN}
+{
+ \spec{PV}{D(6)}{heliocentric \xyzxyzd, equatorial, J2000} \\
+ \spec{}{}{\hspace{1.5em} (AU, AU/s; Note~1)} \\
+ \spec{DATE}{D}{date (TT Modified Julian Date = JD$-$2400000.5)} \\
+ \spec{PMASS}{D}{mass of the planet (Sun = 1; Note~2)}
+}
+\args{RETURNED}
+{
+ \spec{U}{D(13)}{universal orbital elements (Note~3)} \\
+ \specel {(1)}     {combined mass ($M+m$)} \\
+ \specel {(2)}     {total energy of the orbit ($\alpha$)} \\
+ \specel {(3)}     {reference (osculating) epoch ($t_0$)} \\
+ \specel {(4-6)}   {position at reference epoch (${\rm \bf r}_0$)} \\
+ \specel {(7-9)}   {velocity at reference epoch (${\rm \bf v}_0$)} \\
+ \specel {(10)}    {heliocentric distance at reference epoch} \\
+ \specel {(11)}    {${\rm \bf r}_0.{\rm \bf v}_0$} \\
+ \specel {(12)}    {date ($t$)} \\
+ \specel {(13)}    {universal eccentric anomaly ($\psi$) of date, approx} \\
+ \spec{JSTAT}{I}{status:} \\
+ \spec{}{}{\hspace{1.95em}      0 = OK} \\
+ \spec{}{}{\hspace{1.2em}    $-$1 = illegal PMASS} \\
+ \spec{}{}{\hspace{1.2em}    $-$2 = too close to Sun} \\
+ \spec{}{}{\hspace{1.2em}    $-$3 = too slow}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The PV 6-vector can be with respect to any chosen inertial frame,
+        and the resulting universal-element set will be with respect to
+        the same frame.  A common choice will be mean equator and ecliptic
+        of epoch J2000.
+  \item The mass, PMASS, is important only for the larger planets.  For
+        most purposes ({\it e.g.}~asteroids) use 0D0.  Values less than zero
+        are illegal.
+  \item The ``universal'' elements are those which define the orbit for the
+        purposes of the method of universal variables (see reference).
+        They consist of the combined mass of the two bodies, an epoch,
+        and the position and velocity vectors (arbitrary reference frame)
+        at that epoch.  The parameter set used here includes also various
+        quantities that can, in fact, be derived from the other
+        information.  This approach is taken to avoiding unnecessary
+        computation and loss of accuracy.  The supplementary quantities
+        are (i)~$\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.
+ \end{enumerate}
+}
+\aref{Everhart, E. \& Pitkin, E.T., Am.~J.~Phys.~51, 712, 1983.}
+%-----------------------------------------------------------------------
+\routine{SLA\_PVOBS}{Observatory Position \& Velocity}
+{
+ \action{Position and velocity of an observing station.}
+ \call{CALL sla\_PVOBS (P, H, STL, PV)}
+}
+\args{GIVEN}
+{
+ \spec{P}{D}{latitude (geodetic, radians)} \\
+ \spec{H}{D}{height above reference spheroid (geodetic, metres)} \\
+ \spec{STL}{D}{local apparent sidereal time (radians)}
+}
+\args{RETURNED}
+{
+ \spec{PV}{D(6)}{\xyzxyzd\ (AU, AU~s$^{-1}$, true equator and equinox
+                                                            of date)}
+}
+\anote{IAU 1976 constants are used.}
+%-----------------------------------------------------------------------
+\routine{SLA\_PXY}{Apply Linear Model}
+{
+ \action{Given arrays of {\it expected}\/ and {\it measured}\,
+         \xy\ coordinates, and a
+         linear model relating them (as produced by sla\_FITXY), compute
+         the array of {\it predicted}\/ coordinates and the RMS residuals.}
+ \call{CALL sla\_PXY (NP,XYE,XYM,COEFFS,XYP,XRMS,YRMS,RRMS)}
+}
+\args{GIVEN}
+{
+ \spec{NP}{I}{number of samples} \\
+ \spec{XYE}{D(2,NP)}{expected \xy\ for each sample} \\
+ \spec{XYM}{D(2,NP)}{measured \xy\ for each sample} \\
+ \spec{COEFFS}{D(6)}{coefficients of model (see below)}
+}
+\args{RETURNED}
+{
+ \spec{XYP}{D(2,NP)}{predicted \xy\ for each sample} \\
+ \spec{XRMS}{D}{RMS in X} \\
+ \spec{YRMS}{D}{RMS in Y} \\
+ \spec{RRMS}{D }{total RMS (vector sum of XRMS and YRMS)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The model is supplied in the array COEFFS.  Naming the
+        six elements of COEFFS $a,b,c,d,e$ \& $f$,
+        the model transforms {\it measured}\/ coordinates
+        $[x_{m},y_{m}\,]$ into {\it predicted}\/ coordinates
+        $[x_{p},y_{p}\,]$ as follows:
+        \begin{verse}
+         $x_{p} = a + bx_{m} + cy_{m}$ \\
+         $y_{p} = d + ex_{m} + fy_{m}$
+        \end{verse}
+  \item The residuals are $(x_{p}-x_{e})$ and $(y_{p}-y_{e})$.
+  \item If NP is less than or equal to zero, no coordinates are
+        transformed, and the RMS residuals are all zero.
+  \item See also sla\_FITXY, sla\_INVF, sla\_XY2XY, sla\_DCMPF
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_RANDOM}{Random Number}
+{
+ \action{Generate pseudo-random real number in the range $0 \leq x < 1$.}
+ \call{R~=~sla\_RANDOM (SEED)}
+}
+\args{GIVEN}
+{
+ \spec{SEED}{R}{an arbitrary real number}
+}
+\args{RETURNED}
+{
+ \spec{SEED}{R}{a new arbitrary value} \\
+ \spec{sla\_RANDOM}{R}{Pseudo-random real number $0 \leq x < 1$.}
+}
+\anote{The implementation is machine-dependent.}
+%-----------------------------------------------------------------------
+\routine{SLA\_RANGE}{Put Angle into Range $\pm\pi$}
+{
+ \action{Normalize an angle into the range $\pm\pi$ (single precision).}
+ \call{R~=~sla\_RANGE (ANGLE)}
+}
+\args{GIVEN}
+{
+ \spec{ANGLE}{R}{angle in radians}
+}
+\args{RETURNED}
+{
+ \spec{sla\_RANGE}{R}{ANGLE expressed in the range $\pm\pi$.}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_RANORM}{Put Angle into Range $0\!-\!2\pi$}
+{
+ \action{Normalize an angle into the range $0\!-\!2\pi$ (single precision).}
+ \call{R~=~sla\_RANORM (ANGLE)}
+}
+\args{GIVEN}
+{
+ \spec{ANGLE}{R}{angle in radians}
+}
+\args{RETURNED}
+{
+ \spec{sla\_RANORM}{R}{ANGLE expressed in the range $0\!-\!2\pi$}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_RCC}{Barycentric Coordinate Time}
+{
+ \call{D~=~sla\_RCC (TDB, UT1, WL, U, V)}
+ \action{The relativistic clock correction TDB$-$TT, the
+         difference between {\it proper time}\,
+         on Earth and {\it coordinate time}\/ in the solar system barycentric
+         space-time frame of reference.  The proper time is TT;  the
+         coordinate time is {\it an implementation}\/ of TDB.}
+}
+\args{GIVEN}
+{
+ \spec{TDB}{D}{coordinate time (MJD: JD$-$2400000.5)} \\
+ \spec{UT1}{D}{universal time (fraction of one day)} \\
+ \spec{WL}{D}{clock longitude (radians west)} \\
+ \spec{U}{D}{clock distance from Earth spin axis (km)} \\
+ \spec{V}{D}{clock distance north of Earth equatorial plane (km)}
+}
+\args{RETURNED}
+{
+ \spec{sla\_RCC}{D}{TDB$-$TT (sec)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item TDB may be considered to
+        be the coordinate time in the solar system barycentre frame of
+        reference, and TT is the proper time given by clocks at mean sea
+        level on the Earth.
+  \item The result has a main (annual) sinusoidal term of amplitude
+        approximately 1.66ms, plus planetary terms up to about
+        20$\mu$s, and lunar and diurnal terms up to 2$\mu$s.  The
+        variation arises from the transverse Doppler effect and the
+        gravitational red-shift as the observer varies in speed and
+        moves through different gravitational potentials.
+  \item The argument TDB is, strictly, the barycentric coordinate time;
+        however, the terrestrial proper time (TT) can in practice be used.
+  \item The geocentric model is that of Fairhead \& Bretagnon (1990),
+        in its full
+        form.  It was supplied by Fairhead (private communication)
+        as a Fortran subroutine.  A number of coding changes were made to
+        this subroutine in order
+        match the calling sequence of previous versions of the present
+        routine, to comply with Starlink programming standards and to
+        avoid compilation problems on certain machines.  On the supported
+        computer types,
+        the numerical results are essentially unaffected by the
+        changes.  The topocentric model is from Moyer (1981) and Murray (1983).
+        During the interval 1950-2050, the absolute accuracy of the
+        geocentric model is better than $\pm3$~nanoseconds
+        relative to direct numerical integrations using the JPL DE200/LE200
+        solar system ephemeris.
+  \item The IAU definition of TDB is that it must differ from TT only by
+        periodic terms.  Though practical, this is an imprecise definition
+        which ignores the existence of very long-period and secular effects
+        in the dynamics of the solar system.  As a consequence, different
+        implementations of TDB will, in general, differ in zero-point and
+        will drift linearly relative to one other.
+ \end{enumerate}
+}
+\refs
+{
+ \begin{enumerate}
+  \item Fairhead, L.\ \& 
+        Bretagnon, P., 1990.\ {\it Astr.Astrophys.}\ {\bf 229}, 240-247.
+  \item Moyer, T.D., 1981.\ {\it Cel.Mech.}\ {\bf 23}, 33.
+  \item Murray, C.A., 1983,\ {\it Vectorial Astrometry}, Adam Hilger.
+ \end{enumerate}
+}
+%------------------------------------------------------------------------------
+\routine{SLA\_RDPLAN}{Apparent \radec\ of Planet}
+{
+ \action{Approximate topocentric apparent \radec\ and angular
+         size of a planet.}
+ \call{CALL sla\_RDPLAN (DATE, NP, ELONG, PHI, RA, DEC, DIAM)}
+}
+\args{GIVEN}
+{
+ \spec{DATE}{D}{MJD of observation (JD$-$2400000.5)} \\
+ \spec{NP}{I}{planet:} \\
+ \spec{}{}{\hspace{1.5em} 1\,=\,Mercury} \\
+ \spec{}{}{\hspace{1.5em} 2\,=\,Venus} \\
+ \spec{}{}{\hspace{1.5em} 3\,=\,Moon} \\
+ \spec{}{}{\hspace{1.5em} 4\,=\,Mars} \\
+ \spec{}{}{\hspace{1.5em} 5\,=\,Jupiter} \\
+ \spec{}{}{\hspace{1.5em} 6\,=\,Saturn} \\
+ \spec{}{}{\hspace{1.5em} 7\,=\,Uranus} \\
+ \spec{}{}{\hspace{1.5em} 8\,=\,Neptune} \\
+ \spec{}{}{\hspace{1.5em} 9\,=\,Pluto} \\
+ \spec{}{}{\hspace{0.44em} else\,=\,Sun} \\
+ \spec{ELONG,PHI}{D}{observer's longitude (east +ve) and latitude
+                     (radians)}
+}
+\args{RETURNED}
+{
+ \spec{RA,DEC}{D}{topocentric apparent \radec\ (radians)} \\
+ \spec{DIAM}{D}{angular diameter (equatorial, radians)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The date is in a dynamical timescale (TDB, formerly ET)
+        and is in the form of a Modified
+        Julian Date (JD$-$2400000.5).  For all practical purposes, TT can
+        be used instead of TDB, and for many applications UT will do
+        (except for the Moon).
+  \item 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 sla\_DMOON and sla\_PLANET.
+  \item The direction accuracy (arcsec, 1000-3000\,AD) is of order:
+        \begin{tabbing}
+         xxxxxxx \= xxxxxxxxxxxxxxxxxx \= \kill
+         \> Sun     \>  \hspace{0.5em}5 \\
+         \> Mercury \>  \hspace{0.5em}2 \\
+         \> Venus   \> 10 \\
+         \> Moon    \> 30 \\
+         \> Mars    \> 50 \\
+         \> Jupiter \> 90 \\
+         \> Saturn  \> 90 \\
+         \> Uranus  \> 90 \\
+         \> Neptune \> 10 \\
+         \> Pluto \> \hspace{0.5em}1~~~(1885-2099\,AD only)
+        \end{tabbing}
+        The angular diameter accuracy is about 0.4\% for the Moon,
+        and 0.01\% or better for the Sun and planets.
+        For more information on accuracy,
+        refer to the routines sla\_PLANET and sla\_DMOON,
+        which the present routine uses.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_REFCO}{Refraction Constants}
+{
+ \action{Determine the constants $a$ and $b$ in the
+         atmospheric refraction model
+         $\Delta \zeta = a \tan \zeta + b \tan^{3} \zeta$,
+         where $\zeta$ is the {\it observed}\/ zenith distance
+         ({\it i.e.}\ affected by refraction) and $\Delta \zeta$ is
+         what to add to $\zeta$ to give the {\it topocentric}\,
+         ({\it i.e.\ in vacuo}) zenith distance.}
+ \call{CALL sla\_REFCO (HM, TDK, PMB, RH, WL, PHI, TLR, EPS, REFA, REFB)}
+}
+\args{GIVEN}
+{
+ \spec{HM}{D}{height of the observer above sea level (metre)} \\
+ \spec{TDK}{D}{ambient temperature at the observer (degrees K)} \\
+ \spec{PMB}{D}{pressure at the observer (mB)} \\
+ \spec{RH}{D}{relative humidity at the observer (range 0\,--\,1)} \\
+ \spec{WL}{D}{effective wavelength of the source ($\mu{\rm m}$)} \\
+ \spec{PHI}{D}{latitude of the observer (radian, astronomical)} \\
+ \spec{TLR}{D}{temperature lapse rate in the troposphere
+                                     (degrees K per metre)} \\
+ \spec{EPS}{D}{precision required to terminate iteration (radian)}
+}
+\args{RETURNED}
+{
+ \spec{REFA}{D}{$\tan \zeta$ coefficient (radians)} \\
+ \spec{REFB}{D}{$\tan^{3} \zeta$ coefficient (radians)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item Suggested values for the TLR and EPS arguments are 0.0065D0 and
+        1D$-$8 respectively.
+  \item The radio refraction is chosen by specifying WL $>100$~$\mu{\rm m}$.
+  \item The routine is a slower but more accurate alternative to the
+        sla\_REFCOQ routine.  The constants it produces give perfect
+        agreement with sla\_REFRO at zenith distances
+        $\tan^{-1} 1$ ($45^\circ$) and $\tan^{-1} 4$ ($\sim 76^\circ$).
+        At other zenith distances, the model achieves:
+        \arcsec{0}{5} accuracy for $\zeta<80^{\circ}$,
+        \arcsec{0}{01} accuracy for $\zeta<60^{\circ}$, and
+        \arcsec{0}{001} accuracy for $\zeta<45^{\circ}$.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_REFCOQ}{Refraction Constants (fast)}
+{
+ \action{Determine the constants $a$ and $b$ in the
+         atmospheric refraction model
+         $\Delta \zeta = a \tan \zeta + b \tan^{3} \zeta$,
+         where $\zeta$ is the {\it observed}\/ zenith distance
+         ({\it i.e.}\ affected by refraction) and $\Delta \zeta$ is
+         what to add to $\zeta$ to give the {\it topocentric}\,
+         ({\it i.e.\ in vacuo}) zenith distance. (This is a fast
+         alternative to the sla\_REFCO routine -- see notes.)}
+ \call{CALL sla\_REFCOQ (TDK, PMB, RH, WL, REFA, REFB)}
+}
+\args{GIVEN}
+{
+ \spec{TDK}{D}{ambient temperature at the observer (degrees K)} \\
+ \spec{PMB}{D}{pressure at the observer (mB)} \\
+ \spec{RH}{D}{relative humidity at the observer (range 0\,--\,1)} \\
+ \spec{WL}{D}{effective wavelength of the source ($\mu{\rm m}$)}
+}
+\args{RETURNED}
+{
+ \spec{REFA}{D}{$\tan \zeta$ coefficient (radians)} \\
+ \spec{REFB}{D}{$\tan^{3} \zeta$ coefficient (radians)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The radio refraction is chosen by specifying WL $>100$~$\mu{\rm m}$.
+  \item The model is an approximation, for moderate zenith distances,
+        to the predictions of the sla\_REFRO routine.  The approximation
+        is maintained across a range of conditions, and applies to
+        both optical/IR and radio.
+  \item The algorithm is a fast alternative to the sla\_REFCO routine.
+        The latter calls the sla\_REFRO routine itself:  this involves
+        integrations through a model atmosphere, and is costly in
+        processor time.  However, the model which is produced is precisely
+        correct for two zenith distances ($45^\circ$ and $\sim\!76^\circ$)
+        and at other zenith distances is limited in accuracy only by the
+        $\Delta \zeta = a \tan \zeta + b \tan^{3} \zeta$ formulation
+        itself.  The present routine is not as accurate, though it
+        satisfies most practical requirements.
+  \item The model omits the effects of (i)~height above sea level (apart
+        from the reduced pressure itself), (ii)~latitude ({\it i.e.}\ the
+        flattening of the Earth) and (iii)~variations in tropospheric
+        lapse rate.
+  \item The model has been tested using the following range of conditions:
+        \begin{itemize}
+        \item [$\cdot$] lapse rates 0.0055, 0.0065, 0.0075~degrees K per metre
+        \item [$\cdot$] latitudes $0^\circ$, $25^\circ$, $50^\circ$, $75^\circ$
+        \item [$\cdot$] heights 0, 2500, 5000 metres above sea level
+        \item [$\cdot$] pressures mean for height $-10$\% to $+5$\% in steps of $5$\%
+        \item [$\cdot$] temperatures $-10^\circ$ to $+20^\circ$ with respect to
+              $280^\circ$K at sea level
+        \item [$\cdot$] relative humidity 0, 0.5, 1
+        \item [$\cdot$] wavelength 0.4, 0.6, \ldots\ $2\mu{\rm m}$, + radio
+        \item [$\cdot$] zenith distances $15^\circ$, $45^\circ$, $75^\circ$
+        \end{itemize}
+        For the above conditions, the comparison with sla\_REFRO
+        was as follows:
+
+        \vspace{2ex}
+
+        ~~~~~~~~~~
+        \begin{tabular}{|r|r|r|} \hline
+              & {\it worst} & {\it RMS} \\ \hline
+              optical/IR & 62 & 8 \\
+              radio & 319 & 49 \\ \hline
+              & mas & mas \\ \hline
+        \end{tabular}
+
+        \vspace{3ex}
+
+        For this particular set of conditions:
+        \begin{itemize}
+        \item [$\cdot$] lapse rate $6.5^\circ K km^{-1}$
+        \item [$\cdot$] latitude $50^\circ$
+        \item [$\cdot$] sea level
+        \item [$\cdot$] pressure 1005\,mB
+        \item [$\cdot$] temperature $7^\circ$C
+        \item [$\cdot$] humidity 80\%
+        \item [$\cdot$] wavelength 5740\,\.{A}
+        \end{itemize}
+        the results were as follows:
+
+        \vspace{2ex}
+
+        ~~~~~~~~~~
+        \begin{tabular}{|r|r|r|r|} \hline
+        \multicolumn{1}{|c}{$\zeta$} &
+        \multicolumn{1}{|c}{sla\_REFRO} &
+        \multicolumn{1}{|c}{sla\_REFCOQ} &
+        \multicolumn{1}{|c|}{Saastamoinen} \\ \hline
+        10 &  10.27 &  10.27 &  10.27 \\
+        20 &  21.19 &  21.20 &  21.19 \\
+        30 &  33.61 &  33.61 &  33.60 \\
+        40 &  48.82 &  48.83 &  48.81 \\
+        45 &  58.16 &  58.18 &  58.16 \\
+        50 &  69.28 &  69.30 &  69.27 \\
+        55 &  82.97 &  82.99 &  82.95 \\
+        60 & 100.51 & 100.54 & 100.50 \\
+        65 & 124.23 & 124.26 & 124.20 \\
+        70 & 158.63 & 158.68 & 158.61 \\
+        72 & 177.32 & 177.37 & 177.31 \\
+        74 & 200.35 & 200.38 & 200.32 \\
+        76 & 229.45 & 229.43 & 229.42 \\
+        78 & 267.44 & 267.29 & 267.41 \\
+        80 & 319.13 & 318.55 & 319.10 \\ \hline
+        deg & arcsec & arcsec & arcsec \\ \hline
+        \end{tabular}
+
+        \vspace{3ex}
+
+        The values for Saastamoinen's formula (which includes terms
+        up to $\tan^5$) are taken from Hohenkerk and Sinclair (1985).
+
+        The results from the much slower but more accurate sla\_REFCO
+        routine have not been included in the tabulation as they are
+        identical to those in the sla\_REFRO column to the \arcsec{0}{01}
+        resolution used.
+  \item Outlandish input parameters are silently limited
+        to mathematically safe values.  Zero pressure is permissible,
+        and causes zeroes to be returned.
+  \item The algorithm draws on several sources, as follows:
+        \begin{itemize}
+        \item The formula for the saturation vapour pressure of water as
+              a function of temperature and temperature is taken from
+              expressions A4.5-A4.7 of Gill (1982).
+        \item The formula for the water vapour pressure, given the
+              saturation pressure and the relative humidity is from
+              Crane (1976), expression 2.5.5.
+        \item The refractivity of air is a function of temperature,
+              total pressure, water-vapour pressure and, in the case
+              of optical/IR but not radio, wavelength.  The formulae
+              for the two cases are developed from the Essen and Froome
+              expressions adopted in Resolution 1 of the 12th International
+              Geodesy Association General Assembly (1963).
+        \end{itemize}
+        The above three items are as used in the sla\_REFRO routine.
+        \begin{itemize}
+        \item The formula for $\beta~(=H_0/r_0)$ is
+              an adaption of expression 9 from Stone (1996).  The
+              adaptations, arrived at empirically, consist of (i)~a
+              small adjustment to the coefficient and (ii)~a humidity
+              term for the radio case only.
+        \item The formulae for the refraction constants as a function of
+              $n-1$ and $\beta$ are from Green (1987), expression 4.31.
+        \end{itemize}
+  \end{enumerate}
+}
+\refs
+{
+ \begin{enumerate}
+  \item Crane, R.K., Meeks, M.L.\ (ed), ``Refraction Effects in
+        the Neutral Atmosphere'',
+        {\it Methods of Experimental Physics: Astrophysics 12B,}\/
+        Academic Press, 1976.
+  \item Gill, Adrian E., {\it Atmosphere-Ocean Dynamics,}\/
+        Academic Press, 1982.
+  \item Hohenkerk, C.Y., \& Sinclair, A.T., NAO Technical Note
+        No.~63, 1985.
+  \item International Geodesy Association General Assembly, Bulletin
+        G\'{e}od\'{e}sique {\bf 70} p390, 1963.
+  \item Stone, Ronald C., P.A.S.P.~{\bf 108} 1051-1058, 1996.
+  \item Green, R.M., {\it Spherical Astronomy,}\/ Cambridge
+        University Press, 1987.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_REFRO}{Refraction}
+{
+ \action{Atmospheric refraction, for radio or optical/IR wavelengths.}
+ \call{CALL sla\_REFRO (ZOBS, HM, TDK, PMB, RH, WL, PHI, TLR, EPS, REF)}
+}
+\args{GIVEN}
+{
+ \spec{ZOBS}{D}{observed zenith distance of the source (radians)} \\
+ \spec{HM}{D}{height of the observer above sea level (metre)} \\
+ \spec{TDK}{D}{ambient temperature at the observer (degrees K)} \\
+ \spec{PMB}{D}{pressure at the observer (mB)} \\
+ \spec{RH}{D}{relative humidity at the observer (range 0\,--\,1)} \\
+    \spec{WL}{D}{effective wavelength of the source ($\mu{\rm m}$)} \\
+ \spec{PHI}{D}{latitude of the observer (radian, astronomical)} \\
+ \spec{TLR}{D}{temperature lapse rate in the troposphere
+                                     (degrees K per metre)} \\
+ \spec{EPS}{D}{precision required to terminate iteration (radian)}
+}
+\args{RETURNED}
+{
+ \spec{REF}{D}{refraction: {\it in vacuo}\/ ZD minus observed ZD (radians)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item A suggested value for the TLR argument is 0.0065D0.  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.
+  \item A suggested value for the EPS argument is 1D$-$8.  The result is
+        usually at least two orders of magnitude more computationally
+        precise than the supplied EPS value.
+  \item The routine computes the refraction for zenith distances up
+        to and a little beyond $90^\circ$ using the method of Hohenkerk
+        \& Sinclair (NAO Technical Notes 59 and 63, subsequently adopted
+        in the {\it Explanatory Supplement to the Astronomical Almanac,}\/
+        1992 -- see section 3.281).
+  \item The code is based on the AREF optical/IR refraction subroutine
+        of C.\,Hohenkerk (HMNAO, September 1984), with extensions to
+        support the radio case.  The modifications to the original HMNAO
+        optical/IR refraction code which affect the results are:
+        \begin{itemize}
+         \item Murray's values for the gas constants have been used
+               ({\it Vectorial Astrometry,}\/ Adam Hilger, 1983).
+         \item A better model for $P_s(T)$ has been adopted (taken from
+               Gill, {\it Atmosphere-Ocean Dynamics,}\/ Academic Press, 1982).
+         \item More accurate expressions for $Pw_o$ have been adopted
+               (again from Gill 1982).
+         \item Provision for radio wavelengths has been added using
+               expressions devised by A.\,T.\,Sinclair, RGO (private
+               communication 1989), based on the Essen \& Froome
+               refractivity formula adopted in Resolution~1 of the
+               12th International Geodesy Association General Assembly
+               (Bulletin G\'{e}od\'{e}sique {\bf 70} p390, 1963).
+        \end{itemize}
+        None of the changes significantly affects the optical/IR results
+        with respect to the algorithm given in the 1992 {\it Explanatory
+        Supplement.}\/  For example, at $70^\circ$ zenith distance the present
+        routine agrees with the ES algorithm to better than \arcsec{0}{05}
+        for any reasonable combination of parameters.  However, the
+        improved water-vapour expressions do make a significant difference
+        in the radio band, at $70^\circ$ zenith distance reaching almost
+        \arcseci{4} for a hot, humid, low-altitude site during a period of
+        low pressure.
+  \item The radio refraction is chosen by specifying WL $>100$~$\mu{\rm m}$.
+        Because the algorithm takes no account of the ionosphere, the
+        accuracy deteriorates at low frequencies, below about 30\,MHz.
+  \item Before use, the value of ZOBS is expressed in the range $\pm\pi$.
+        If this ranged ZOBS is negative, the result REF is computed from its
+        absolute value before being made negative to match.  In addition, if
+        it has an absolute value greater than $93^\circ$, a fixed REF value
+        equal to the result for ZOBS~$=93^\circ$ is returned, appropriately
+        signed.
+  \item 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.
+  \item 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 \arcsec{0}{1} level is achieved for moderate ZD,
+        worsening to perhaps \arcsec{0}{5}\,--\,\arcsec{1}{0} at ZD $80^\circ$.
+        At hot and humid sea-level sites the accuracy will not be as good.
+  \item 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 familiar
+        $\nu=p_w/p_s$ or $\nu=\rho_w/\rho_s$ expressions can differ from
+        the formal definition by several percent, significant in the
+        radio case.
+  \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_REFV}{Apply Refraction to Vector}
+{
+ \action{Adjust an unrefracted Cartesian vector to include the effect of
+         atmospheric refraction, using the simple
+         $\Delta \zeta = a \tan \zeta + b \tan^{3} \zeta$ model.}
+ \call{CALL sla\_REFV (VU, REFA, REFB, VR)}
+}
+\args{GIVEN}
+{
+ \spec{VU}{D}{unrefracted position of the source (\azel\ 3-vector)} \\
+ \spec{REFA}{D}{$\tan \zeta$ coefficient (radians)} \\
+ \spec{REFB}{D}{$\tan^{3} \zeta$ coefficient (radians)}
+}
+\args{RETURNED}
+{
+ \spec{VR}{D}{refracted position of the source (\azel\ 3-vector)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item This routine applies the adjustment for refraction in the
+        opposite sense to the usual one -- it takes an unrefracted
+        ({\it in vacuo}\/) position and produces an observed (refracted)
+        position, whereas the
+        $\Delta \zeta = a \tan \zeta + b \tan^{3} \zeta$
+        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.
+  \item Though optimized for speed rather than precision, the present
+        routine achieves consistency with the refracted-to-unrefracted
+        $\Delta \zeta = a \tan \zeta + b \tan^{3} \zeta$
+        model at better than 1~microarcsecond within
+        $30^\circ$ of the zenith and remains within 1~milliarcsecond to
+        $\zeta=70^\circ$.  The inherent accuracy of the model is, of
+        course, far worse than this -- see the documentation for sla\_REFCO
+        for more information.
+  \item At low elevations (below about $3^\circ$) the refraction
+        correction is held back to prevent arithmetic problems and
+        wildly wrong results.  Over a wide range of observer heights
+        and corresponding temperatures and pressures, the following
+        levels of accuracy are achieved, relative to numerical
+        integration through a model atmosphere:
+
+        \begin{center}
+        \begin{tabular}{ccl}
+              $\zeta_{obs}$ & {\it error} \\ \\
+              $80^\circ$ & \arcsec{0}{4}  \\
+              $81^\circ$ & \arcsec{0}{8}  \\
+              $82^\circ$ & \arcsec{1}{6}  \\
+              $83^\circ$ & \arcseci{3}    \\
+              $84^\circ$ & \arcseci{7}    \\
+              $85^\circ$ & \arcseci{17}   \\
+              $86^\circ$ & \arcseci{45}   \\
+              $87^\circ$ & \arcseci{150}  \\
+              $88^\circ$ & \arcseci{340}  \\
+              $89^\circ$ & \arcseci{620}  \\
+              $90^\circ$ & \arcseci{1100} \\
+              $91^\circ$ & \arcseci{1900} & $<$ high-altitude \\
+              $92^\circ$ & \arcseci{3200} & $<$ sites only \\
+        \end{tabular}
+        \end{center}
+  \item See also the routine sla\_REFZ, which performs the adjustment to
+        the zenith distance rather than in \xyz .
+        The present routine is faster than sla\_REFZ and,
+        except very low down,
+        is equally accurate for all practical purposes.  However, beyond
+        about $\zeta=84^\circ$ sla\_REFZ should be used, and for the utmost
+        accuracy iterative use of sla\_REFRO should be considered.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_REFZ}{Apply Refraction to ZD}
+{
+ \action{Adjust an unrefracted zenith distance to include the effect of
+         atmospheric refraction, using the simple
+         $\Delta \zeta = a \tan \zeta + b \tan^{3} \zeta$ model.}
+ \call{CALL sla\_REFZ (ZU, REFA, REFB, ZR)}
+}
+\args{GIVEN}
+{
+ \spec{ZU}{D}{unrefracted zenith distance of the source (radians)} \\
+ \spec{REFA}{D}{$\tan \zeta$ coefficient (radians)} \\
+ \spec{REFB}{D}{$\tan^{3} \zeta$ coefficient (radians)}
+}
+\args{RETURNED}
+{
+ \spec{ZR}{D}{refracted zenith distance (radians)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item This routine applies the adjustment for refraction in the
+        opposite sense to the usual one -- it takes an unrefracted
+        ({\it in vacuo}\/) position and produces an observed (refracted)
+        position, whereas the
+        $\Delta \zeta = a \tan \zeta + b \tan^{3} \zeta$
+        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 $10^{-11}$~arcsecond level
+        for $\zeta=80^\circ$.  The inherent accuracy of the model
+        is, of course, far worse than this -- see the documentation for
+        sla\_REFCO for more information.
+  \item At $\zeta=83^\circ$, the rapidly-worsening
+        $\Delta \zeta = a \tan \zeta + b \tan^{3} \zeta$
+        model is abandoned and an empirical formula takes over:
+
+          \[\Delta \zeta = F \left(
+  \frac{0^\circ\hspace{-0.37em}.\hspace{0.02em}55445
+                - 0^\circ\hspace{-0.37em}.\hspace{0.02em}01133 E
+                          + 0^\circ\hspace{-0.37em}.\hspace{0.02em}00202 E^2}
+             {1 + 0.28385 E +0.02390 E^2} \right) \]
+        where $E=90^\circ-\zeta_{true}$
+        and $F$ is a factor chosen to meet the
+        $\Delta \zeta = a \tan \zeta + b \tan^{3} \zeta$
+        formula at $\zeta=83^\circ$.  Over a
+        wide range of observer heights and corresponding temperatures and
+        pressures, the following levels of accuracy are achieved,
+        relative to numerical integration through a model atmosphere:
+
+        \begin{center}
+        \begin{tabular}{ccl}
+              $\zeta_{obs}$ & {\it error} \\ \\
+              $80^\circ$ & \arcsec{0}{4}  \\
+              $81^\circ$ & \arcsec{0}{8}  \\
+              $82^\circ$ & \arcsec{1}{5}  \\
+              $83^\circ$ & \arcsec{3}{2}  \\
+              $84^\circ$ & \arcsec{4}{9}  \\
+              $85^\circ$ & \arcsec{5}{8}  \\
+              $86^\circ$ & \arcsec{6}{1}  \\
+              $87^\circ$ & \arcsec{7}{1}  \\
+              $88^\circ$ & \arcseci{11}   \\
+              $89^\circ$ & \arcseci{21}   \\
+              $90^\circ$ & \arcseci{43}   \\
+              $91^\circ$ & \arcseci{92}  & $<$ high-altitude \\
+              $92^\circ$ & \arcseci{220} & $<$ sites only \\
+        \end{tabular}
+        \end{center}
+  \item See also the routine sla\_REFV, which performs the adjustment in
+        \xyz , and with the emphasis on speed rather than numerical accuracy.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_RVEROT}{RV Corrn to Earth Centre}
+{
+ \action{Velocity component in a given direction due to Earth rotation.}
+ \call{R~=~sla\_RVEROT (PHI, RA, DA, ST)}
+}
+\args{GIVEN}
+{
+ \spec{PHI}{R}{geodetic latitude of observing station (radians)} \\
+ \spec{RA,DA}{R}{apparent \radec\ (radians)} \\
+ \spec{ST}{R}{local apparent sidereal time (radians)}
+}
+\args{RETURNED}
+{
+ \spec{sla\_RVEROT}{R}{Component of Earth rotation in
+                       direction RA,DA (km~s$^{-1}$)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item Sign convention: the result is positive when the observatory
+        is receding from the given point on the sky.
+  \item Accuracy: the simple algorithm used assumes a spherical Earth and
+        an observing station at sea level;  for actual observing
+        sites, the error is unlikely to be greater than 0.0005~km~s$^{-1}$.
+        For applications requiring greater precision, use the routine
+        sla\_PVOBS.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_RVGALC}{RV Corrn to Galactic Centre}
+{
+ \action{Velocity component in a given direction due to the rotation
+         of the Galaxy.}
+ \call{R~=~sla\_RVGALC (R2000, D2000)}
+}
+\args{GIVEN}
+{
+ \spec{R2000,D2000}{R}{J2000.0 mean \radec\ (radians)}
+}
+\args{RETURNED}
+{
+ \spec{sla\_RVGALC}{R}{Component of dynamical LSR motion in direction
+                       R2000,D2000 (km~s$^{-1}$)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item Sign convention: the result is positive when the LSR
+        is receding from the given point on the sky.
+  \item 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 {\it dynamical}\/ LSR,
+        it is not to be confused with a {\it kinematical}\/ LSR, which
+        is the mean standard of rest of star catalogues or stellar
+        populations.
+  \item The dynamical LSR velocity due to Galactic rotation is assumed to
+        be 220~km~s$^{-1}$ towards $l^{I\!I}=90^{\circ}$,
+                                   $b^{I\!I}=0$.
+ \end{enumerate}
+}
+\aref{Kerr \& Lynden-Bell (1986), MNRAS, 221, p1023.}
+%-----------------------------------------------------------------------
+\routine{SLA\_RVLG}{RV Corrn to Local Group}
+{
+ \action{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.}
+ \call{R~=~sla\_RVLG (R2000, D2000)}
+}
+\args{GIVEN}
+{
+ \spec{R2000,D2000}{R}{J2000.0 mean \radec\ (radians)}
+}
+\args{RETURNED}
+{
+ \spec{sla\_RVLG}{R}{Component of {\bf solar} ({\it n.b.})
+                     motion in direction R2000,D2000 (km~s$^{-1}$)}
+}
+\anote{Sign convention: the result is positive when
+       the Sun is receding from the given point on the sky.}
+\aref{{\it IAU Trans.}\ 1976.\ {\bf 16B}, p201.}
+%-----------------------------------------------------------------------
+\routine{SLA\_RVLSRD}{RV Corrn to Dynamical LSR}
+{
+ \action{Velocity component in a given direction due to the Sun's
+         motion with respect to the ``dynamical'' Local Standard of Rest.}
+ \call{R~=~sla\_RVLSRD (R2000, D2000)}
+}
+\args{GIVEN}
+{
+ \spec{R2000,D2000}{R}{J2000.0 mean \radec\ (radians)}
+}
+\args{RETURNED}
+{
+ \spec{sla\_RVLSRD}{R}{Component of {\it peculiar}\/ solar motion
+                      in direction R2000,D2000 (km~s$^{-1}$)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item Sign convention: the result is positive when
+        the Sun is receding from the given point on the sky.
+  \item The Local Standard of Rest used here is the {\it 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 {\it peculiar}\/ solar
+        motion.
+  \item There is another type of LSR, called a {\it 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
+        {\it standard}\/ solar motion.
+        The dynamical LSR is seldom used by observational astronomers,
+        who conventionally use a kinematical LSR such as the one implemented
+        in the routine sla\_RVLSRK.
+  \item The peculiar solar motion is from Delhaye (1965), in {\it Stars
+        and Stellar Systems}, vol~5, p73:  in Galactic Cartesian
+        coordinates (+9,+12,+7)~km~s$^{-1}$.
+        This corresponds to about 16.6~km~s$^{-1}$
+        towards Galactic coordinates $l^{I\!I}=53^{\circ},b^{I\!I}=+25^{\circ}$.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_RVLSRK}{RV Corrn to Kinematical LSR}
+{
+ \action{Velocity component in a given direction due to the Sun's
+         motion with respect to a kinematical Local Standard of Rest.}
+ \call{R~=~sla\_RVLSRK (R2000, D2000)}
+}
+\args{GIVEN}
+{
+ \spec{R2000,D2000}{R}{J2000.0 mean \radec\ (radians)}
+}
+\args{RETURNED}
+{
+ \spec{sla\_RVLSRK}{R}{Component of {\it standard}\/ solar motion
+                      in direction R2000,D2000 (km~s$^{-1}$)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item Sign convention: the result is positive when
+        the Sun is receding from the given point on the sky.
+  \item The Local Standard of Rest used here is one of several
+        {\it 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 {\it standard}\/ solar motion.
+  \item There is another sort of LSR, seldom used by observational
+        astronomers, called the {\it dynamical}\/ LSR.  This 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 {\it peculiar}\/ solar motion.  To
+        obtain a radial velocity correction with respect to the
+        dynamical LSR use the routine sla\_RVLSRD.
+  \item The adopted standard solar motion is 20~km~s$^{-1}$
+        towards $\alpha=18^{\rm h},\delta=+30^{\circ}$ (1900).
+ \end{enumerate}
+}
+\refs
+{
+ \begin{enumerate}
+  \item Delhaye (1965), in {\it Stars and Stellar Systems}, vol~5, p73.
+  \item {\it Methods of Experimental Physics}\/ (ed Meeks), vol~12,
+        part~C, sec~6.1.5.2, p281.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_S2TP}{Spherical to Tangent Plane}
+{
+ \action{Projection of spherical coordinates onto the tangent plane
+         (single precision).}
+ \call{CALL sla\_S2TP (RA, DEC, RAZ, DECZ, XI, ETA, J)}
+}
+\args{GIVEN}
+{
+ \spec{RA,DEC}{R}{spherical coordinates of star (radians)} \\
+ \spec{RAZ,DECZ}{R}{spherical coordinates of tangent point (radians)}
+}
+\args{RETURNED}
+{
+ \spec{XI,ETA}{R}{tangent plane coordinates (radians)} \\
+ \spec{J}{I}{status:} \\
+ \spec{}{}{\hspace{1.5em} 0 = OK, star on tangent plane} \\
+ \spec{}{}{\hspace{1.5em} 1 = error, star too far from axis} \\
+ \spec{}{}{\hspace{1.5em} 2 = error, antistar on tangent plane} \\
+ \spec{}{}{\hspace{1.5em} 3 = error, antistar too far from axis}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The projection is called the {\it gnomonic}\/ projection;  the
+        Cartesian coordinates \xieta\ are called 
+        {\it standard coordinates.}\/  The latter
+        are in units of the distance from the tangent plane to the projection
+        point, {\it i.e.}\ radians near the origin.
+  \item When working in \xyz\ rather than spherical coordinates, the
+        equivalent Cartesian routine sla\_V2TP is available.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_SEP}{Angle Between 2 Points on Sphere}
+{
+ \action{Angle between two points on a sphere (single precision).}
+ \call{R~=~sla\_SEP (A1, B1, A2, B2)}
+}
+\args{GIVEN}
+{
+ \spec{A1,B1}{R}{spherical coordinates of one point (radians)} \\
+ \spec{A2,B2}{R}{spherical coordinates of the other point (radians)}
+}
+\args{RETURNED}
+{
+ \spec{sla\_SEP}{R}{angle between [A1,B1] and [A2,B2] in radians}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The spherical coordinates are right ascension and declination,
+  longitude and latitude, {\it etc.}\ in radians.
+  \item The result is always positive.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_SMAT}{Solve Simultaneous Equations}
+{
+ \action{Matrix inversion and solution of simultaneous equations
+         (single precision).}
+ \call{CALL sla\_SMAT (N, A, Y, D, JF, IW)}
+}
+\args{GIVEN}
+{
+ \spec{N}{I}{number of unknowns} \\
+ \spec{A}{R(N,N)}{matrix} \\
+ \spec{Y}{R(N)}{vector}
+}
+\args{RETURNED}
+{
+ \spec{A}{R(N,N)}{matrix inverse} \\
+ \spec{Y}{R(N)}{solution} \\
+ \spec{D}{R}{determinant} \\
+ \spec{JF}{I}{singularity flag: 0=OK} \\
+ \spec{IW}{I(N)}{workspace}
+}
+\notes
+{
+ \begin{enumerate}
+  \item For the set of $n$ simultaneous linear equations in $n$ unknowns:
+        \begin{verse}
+         {\bf A}$\cdot${\bf y} = {\bf x}
+        \end{verse}
+        where:
+        \begin{itemize}
+         \item {\bf A} is a non-singular $n \times n$ matrix,
+         \item {\bf y} is the vector of $n$ unknowns, and
+         \item {\bf x} is the known vector,
+        \end{itemize}
+        sla\_SMAT computes:
+        \begin{itemize}
+         \item the inverse of matrix {\bf A},
+         \item the determinant of matrix {\bf A}, and
+         \item the vector of $n$ unknowns {\bf y}.
+        \end{itemize}
+        Argument N is the order $n$, A (given) is the matrix {\bf A},
+        Y (given) is the vector {\bf x} and Y (returned)
+        is the vector {\bf y}.
+        The argument A (returned) is the inverse matrix {\bf A}$^{-1}$,
+        and D is {\it det}\/({\bf A}).
+  \item JF is the singularity flag.  If the matrix is non-singular,
+        JF=0 is returned.  If the matrix is singular, JF=$-$1
+        and D=0.0 are returned.  In the latter case, the contents
+        of array A on return are undefined.
+  \item The algorithm is Gaussian elimination with partial pivoting.
+        This method is very fast;  some much slower algorithms can give
+        better accuracy, but only by a small factor.
+  \item This routine replaces the obsolete sla\_SMATRX.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_SUBET}{Remove E-terms}
+{
+ \action{Remove the E-terms (elliptic component of annual aberration)
+         from a pre IAU~1976 catalogue \radec\ to give a mean place.}
+ \call{CALL sla\_SUBET (RC, DC, EQ, RM, DM)}
+}
+\args{GIVEN}
+{
+ \spec{RC,DC}{D}{\radec\ with E-terms included (radians)} \\
+ \spec{EQ}{D}{Besselian epoch of mean equator and equinox}
+}
+\args{RETURNED}
+{
+ \spec{RM,DM}{D}{\radec\ without E-terms (radians)}
+}
+\anote{Most star positions from pre-1984 optical catalogues (or
+       obtained by astrometry with respect to such stars) have the
+       E-terms built-in.  This routine converts such a position to a
+       formal mean place (allowing, for example, comparison with a
+       pulsar timing position).}
+\aref{{\it Explanatory Supplement to the Astronomical Ephemeris},
+      section 2D, page 48.}
+%-----------------------------------------------------------------------
+\routine{SLA\_SUPGAL}{Supergalactic to Galactic}
+{
+ \action{Transformation from de Vaucouleurs supergalactic coordinates
+         to IAU 1958 galactic coordinates.}
+ \call{CALL sla\_GALSUP (DL, DB, DSL, DSB)}
+}
+\args{GIVEN}
+{
+ \spec{DSL,DSB}{D}{supergalactic longitude and latitude (radians)}
+}
+\args{RETURNED}
+{
+ \spec{DL,DB}{D}{galactic longitude and latitude \gal\ (radians)}
+}
+\refs
+{
+ \begin{enumerate}
+  \item de Vaucouleurs, de Vaucouleurs, \& Corwin, {\it Second Reference
+    Catalogue of Bright Galaxies}, U.Texas, p8.
+  \item Systems \& Applied Sciences Corp., documentation for the
+        machine-readable version of the above catalogue,
+        Contract NAS 5-26490.
+ \end{enumerate}
+ (These two references give different values for the galactic
+ longitude of the supergalactic origin.  Both are wrong;  the
+ correct value is $l^{I\!I}=137.37$.)
+}
+%------------------------------------------------------------------------------
+\routine{SLA\_SVD}{Singular Value Decomposition}
+{
+ \action{Singular value decomposition.
+         This routine expresses a given matrix {\bf A} as the product of
+         three matrices {\bf U}, {\bf W}, {\bf V}$^{T}$:
+         \begin{tabbing}
+         XXXXXX \= \kill
+         \> {\bf A} = {\bf U} $\cdot$ {\bf W} $\cdot$ {\bf V}$^{T}$
+         \end{tabbing}
+         where:
+         \begin{tabbing}
+         XXXXXX \= XXXX \= \kill
+         \> {\bf A} \> is any $m$ (rows) $\times n$ (columns) matrix,
+                       where $m \geq n$ \\
+         \> {\bf U} \> is an $m \times n$ column-orthogonal matrix \\
+         \> {\bf W} \> is an $n \times n$ diagonal matrix with
+                       $w_{ii} \geq 0$ \\
+         \> {\bf V}$^{T}$ \> is the transpose of an $n \times n$
+                             orthogonal matrix
+\end{tabbing}
+}
+ \call{CALL sla\_SVD (M, N, MP, NP, A, W, V, WORK, JSTAT)}
+}
+\args{GIVEN}
+{
+ \spec{M,N}{I}{$m$, $n$, the numbers of rows and columns in matrix {\bf A}} \\
+ \spec{MP,NP}{I}{physical dimensions of array containing matrix {\bf A}} \\
+ \spec{A}{D(MP,NP)}{array containing $m \times n$ matrix {\bf A}}
+}
+\args{RETURNED}
+{
+ \spec{A}{D(MP,NP)}{array containing $m \times n$ column-orthogonal
+                    matrix {\bf U}} \\
+ \spec{W}{D(N)}{$n \times n$ diagonal matrix {\bf W}
+               (diagonal elements only)} \\
+ \spec{V}{D(NP,NP)}{array containing $n \times n$ orthogonal
+                    matrix {\bf V} ({\it n.b.}\ not {\bf V}$^{T}$)} \\
+ \spec{WORK}{D(N)}{workspace} \\
+ \spec{JSTAT}{I}{0~=~OK, $-$1~=~array A wrong shape, $>$0~=~index of W
+                 for which convergence failed (see note~3, below)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item M and N are the {\it logical}\/ dimensions of the
+        matrices and vectors concerned, which can be located in
+        arrays of larger {\it physical}\/ dimensions, given by MP and NP.
+  \item V contains matrix V, not the transpose of matrix V.
+  \item If the status JSTAT is greater than zero, this need not
+        necessarily be treated as a failure.  It means that, due to
+        chance properties of the matrix A, the QR transformation
+        phase of the routine did not fully converge in a predefined
+        number of iterations, something that very seldom occurs.
+        When this condition does arise, it is possible that the
+        elements of the diagonal matrix W have not been correctly
+        found.  However, in practice the results are likely to
+        be trustworthy.  Applications should report the condition
+        as a warning, but then proceed normally.
+ \end{enumerate}
+}
+\refs{The algorithm is an adaptation of the routine SVD in the {\it EISPACK}\,
+      library (Garbow~{\it et~al.}\ 1977, {\it EISPACK Guide Extension},
+      Springer Verlag), which is a FORTRAN~66 implementation of the Algol
+      routine SVD of Wilkinson \& Reinsch 1971 ({\it Handbook for Automatic
+      Computation}, vol~2, ed Bauer~{\it et~al.}, Springer Verlag).  These
+      references give full details of the algorithm used here.
+      A good account of the use of SVD in least squares problems is given
+      in {\it Numerical Recipes}\/ (Press~{\it et~al.}\ 1987, Cambridge
+      University Press), which includes another variant of the EISPACK code.}
+%-----------------------------------------------------------------------
+\routine{SLA\_SVDCOV}{Covariance Matrix from SVD}
+{
+ \action{From the {\bf W} and {\bf V} matrices from the SVD
+         factorization of a matrix
+         (as obtained from the sla\_SVD routine), obtain
+         the covariance matrix.}
+ \call{CALL sla\_SVDCOV (N, NP, NC, W, V, WORK, CVM)}
+}
+\args{GIVEN}
+{
+ \spec{N}{I}{$n$, the number of rows and columns in
+             matrices {\bf W} and {\bf V}} \\
+ \spec{NP}{I}{first dimension of array containing $n \times n$
+              matrix {\bf V}} \\
+ \spec{NC}{I}{first dimension of array CVM} \\
+ \spec{W}{D(N)}{$n \times n$ diagonal matrix {\bf W}
+                (diagonal elements only)} \\
+ \spec{V}{D(NP,NP)}{array containing $n \times n$ orthogonal matrix {\bf V}}
+}
+\args{RETURNED}
+{
+ \spec{WORK}{D(N)}{workspace} \\
+ \spec{CVM}{D(NC,NC)}{array to receive covariance matrix}
+}
+\aref{{\it Numerical Recipes}, section 14.3.}
+%-----------------------------------------------------------------------
+\routine{SLA\_SVDSOL}{Solution Vector from SVD}
+{
+ \action{From a given vector and the SVD of a matrix (as obtained from
+         the sla\_SVD routine), obtain the solution vector.
+         This routine solves the equation:
+         \begin{tabbing}
+         XXXXXX \= \kill
+         \> {\bf A} $\cdot$ {\bf x} = {\bf b}
+         \end{tabbing}
+         where:
+         \begin{tabbing}
+         XXXXXX \= XXXX \= \kill
+         \> {\bf A} \> is a given $m$ (rows) $\times n$ (columns)
+                       matrix, where $m \geq n$ \\
+         \> {\bf x} \> is the $n$-vector we wish to find, and \\
+         \> {\bf b} \> is a given $m$-vector
+         \end{tabbing}
+         by means of the {\it Singular Value Decomposition}\/ method (SVD).}
+ \call{CALL sla\_SVDSOL (M, N, MP, NP, B, U, W, V, WORK, X)}
+}
+\args{GIVEN}
+{
+ \spec{M,N}{I}{$m$, $n$, the numbers of rows and columns in matrix {\bf A}} \\
+ \spec{MP,NP}{I}{physical dimensions of array containing matrix {\bf A}} \\
+ \spec{B}{D(M)}{known vector {\bf b}} \\
+ \spec{U}{D(MP,NP)}{array containing $m \times n$ matrix {\bf U}} \\
+ \spec{W}{D(N)}{$n \times n$ diagonal matrix {\bf W}
+                (diagonal elements only)} \\
+ \spec{V}{D(NP,NP)}{array containing $n \times n$ orthogonal matrix {\bf V}}
+}
+\args{RETURNED}
+{
+ \spec{WORK}{D(N)}{workspace} \\
+ \spec{X}{D(N)}{unknown vector {\bf x}}
+}
+\notes
+{
+ \begin{enumerate}
+  \item In the Singular Value Decomposition method (SVD),
+        the matrix {\bf A} is first factorized (for example by
+        the routine sla\_SVD) into the following components:
+        \begin{tabbing}
+        XXXXXX \= \kill
+        \> {\bf A} = {\bf U} $\cdot$ {\bf W} $\cdot$ {\bf V}$^{T}$
+        \end{tabbing}
+        where:
+        \begin{tabbing}
+        XXXXXX \= XXXX \= \kill
+        \> {\bf A} \> is any $m$ (rows) $\times n$ (columns) matrix,
+                      where $m > n$ \\
+        \> {\bf U} \> is an $m \times n$ column-orthogonal matrix \\
+        \> {\bf W} \> is an $n \times n$ diagonal matrix with
+                      $w_{ii} \geq 0$ \\
+        \> {\bf V}$^{T}$ \> is the transpose of an $n \times n$
+                            orthogonal matrix
+        \end{tabbing}
+        Note that $m$ and $n$ are the {\it logical}\/ dimensions of the
+        matrices and vectors concerned, which can be located in
+        arrays of larger {\it physical}\/ dimensions MP and NP.
+        The solution is then found from the expression:
+        \begin{tabbing}
+        XXXXXX \= \kill
+        \> {\bf x} = {\bf V} $\cdot~[diag(1/${\bf W}$_{j})]
+           \cdot (${\bf U}$^{T} \cdot${\bf b})
+        \end{tabbing}
+  \item If matrix {\bf A} is square, and if the diagonal matrix {\bf W} is not
+        altered, the method is equivalent to conventional solution
+        of simultaneous equations.
+  \item If $m > n$, the result is a least-squares fit.
+  \item If the solution is poorly determined, this shows up in the
+        SVD factorization as very small or zero {\bf W}$_{j}$ values.  Where
+        a {\bf W}$_{j}$ value is small but non-zero it can be set to zero to
+        avoid ill effects.  The present routine detects such zero
+        {\bf W}$_{j}$ values and produces a sensible solution, with highly
+        correlated terms kept under control rather than being allowed
+        to elope to infinity, and with meaningful values for the
+       other terms.
+ \end{enumerate}
+}
+\aref{{\it Numerical Recipes}, section 2.9.}
+%-----------------------------------------------------------------------
+\routine{SLA\_TP2S}{Tangent Plane to Spherical}
+{
+ \action{Transform tangent plane coordinates into spherical
+         coordinates (single precision)}
+ \call{CALL sla\_TP2S (XI, ETA, RAZ, DECZ, RA, DEC)}
+}
+\args{GIVEN}
+{
+ \spec{XI,ETA}{R}{tangent plane rectangular coordinates (radians)} \\
+ \spec{RAZ,DECZ}{R}{spherical coordinates of tangent point (radians)}
+}
+\args{RETURNED}
+{
+ \spec{RA,DEC}{R}{spherical coordinates (radians)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The projection is called the {\it gnomonic}\/ projection;  the
+        Cartesian coordinates \xieta\ are called 
+        {\it standard coordinates.}\/  The latter
+        are in units of the distance from the tangent plane to the projection
+        point, {\it i.e.}\ radians near the origin.
+  \item When working in \xyz\ rather than spherical coordinates, the
+        equivalent Cartesian routine sla\_TP2V is available.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_TP2V}{Tangent Plane to Direction Cosines}
+{
+ \action{Given the tangent-plane coordinates of a star and the direction
+         cosines of the tangent point, determine the direction cosines
+         of the star
+         (single precision).}
+ \call{CALL sla\_TP2V (XI, ETA, V0, V)}
+}
+\args{GIVEN}
+{
+ \spec{XI,ETA}{R}{tangent plane coordinates of star (radians)} \\
+ \spec{V0}{R(3)}{direction cosines of tangent point}
+}
+\args{RETURNED}
+{
+ \spec{V}{R(3)}{direction cosines of star}
+}
+\notes
+{
+ \begin{enumerate}
+  \item If vector V0 is not of unit length, the returned vector V will
+        be wrong.
+  \item If vector V0 points at a pole, the returned vector V will be
+        based on the arbitrary assumption that $\alpha=0$ at
+        the tangent point.
+  \item The projection is called the {\it gnomonic}\/ projection;  the
+        Cartesian coordinates \xieta\ are called 
+        {\it standard coordinates.}\/  The latter
+        are in units of the distance from the tangent plane to the projection
+        point, {\it i.e.}\ radians near the origin.
+  \item This routine is the Cartesian equivalent of the routine sla\_TP2S.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_TPS2C}{Plate centre from $\xi,\eta$ and $\alpha,\delta$}
+{
+ \action{From the tangent plane coordinates of a star of known \radec,
+        determine the \radec\ of the tangent point (single precision)}
+ \call{CALL sla\_TPS2C (XI, ETA, RA, DEC, RAZ1, DECZ1, RAZ2, DECZ2, N)}
+}
+\args{GIVEN}
+{
+ \spec{XI,ETA}{R}{tangent plane rectangular coordinates (radians)} \\
+ \spec{RA,DEC}{R}{spherical coordinates (radians)}
+}
+\args{RETURNED}
+{
+ \spec{RAZ1,DECZ1}{R}{spherical coordinates of tangent point,
+                      solution 1} \\
+ \spec{RAZ2,DECZ2}{R}{spherical coordinates of tangent point,
+                      solution 2} \\
+ \spec{N}{I}{number of solutions:} \\
+ \spec{}{}{\hspace{1em} 0 = no solutions returned  (note 2)} \\
+ \spec{}{}{\hspace{1em} 1 = only the first solution is useful (note 3)} \\
+ \spec{}{}{\hspace{1em} 2 = there are two useful solutions (note 3)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The RAZ1 and RAZ2 values returned are in the range $0\!-\!2\pi$.
+  \item 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 $\delta$.
+  \item 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.
+  \item The DECZ1 and DECZ2 values returned are in the range $\pm\pi$,
+        but in the ordinary, non-pole-crossing, case, the range is
+        $\pm\pi/2$.
+  \item RA, DEC, RAZ1, DECZ1, RAZ2, DECZ2 are all in radians.
+  \item The projection is called the {\it gnomonic}\/ projection;  the
+        Cartesian coordinates \xieta\ are called 
+        {\it standard coordinates.}\/  The latter
+        are in units of the distance from the tangent plane to the projection
+        point, {\it i.e.}\ radians near the origin.
+  \item When working in \xyz\ rather than spherical coordinates, the
+        equivalent Cartesian routine sla\_TPV2C is available.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_TPV2C}{Plate centre from $\xi,\eta$ and $x,y,z$}
+{
+ \action{From the tangent plane coordinates of a star of known
+         direction cosines, determine the direction cosines
+         of the tangent point (single precision)}
+ \call{CALL sla\_TPV2C (XI, ETA, V, V01, V02, N)}
+}
+\args{GIVEN}
+{
+ \spec{XI,ETA}{R}{tangent plane coordinates of star (radians)} \\
+ \spec{V}{R(3)}{direction cosines of star}
+}
+\args{RETURNED}
+{
+ \spec{V01}{R(3)}{direction cosines of tangent point, solution 1} \\
+ \spec{V01}{R(3)}{direction cosines of tangent point, solution 2} \\
+ \spec{N}{I}{number of solutions:} \\
+ \spec{}{}{\hspace{1em} 0 = no solutions returned  (note 2)} \\
+ \spec{}{}{\hspace{1em} 1 = only the first solution is useful (note 3)} \\
+ \spec{}{}{\hspace{1em} 2 = there are two useful solutions (note 3)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The vector V must be of unit length or the result will be wrong.
+  \item 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.
+  \item 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 can be regarded as valid if
+        the vector V02 is interpreted as the ``over-the-pole'' case.
+  \item The projection is called the {\it gnomonic}\/ projection;  the
+        Cartesian coordinates \xieta\ are called 
+        {\it standard coordinates.}\/  The latter
+        are in units of the distance from the tangent plane to the projection
+        point, {\it i.e.}\ radians near the origin.
+  \item This routine is the Cartesian equivalent of the routine sla\_TPS2C.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_UE2EL}{Universal to Conventional Elements}
+{
+ \action{Transform universal elements into conventional heliocentric
+         osculating elements.}
+ \call{CALL sla\_UE2EL (\vtop{
+         \hbox{U, JFORMR,}
+         \hbox{JFORM, EPOCH, ORBINC, ANODE, PERIH,}
+         \hbox{AORQ, E, AORL, DM, JSTAT)}}}
+}
+\args{GIVEN}
+{
+ \spec{U}{D(13)}{universal orbital elements (updated; Note~1)} \\
+ \specel {(1)}     {combined mass ($M+m$)} \\
+ \specel {(2)}     {total energy of the orbit ($\alpha$)} \\
+ \specel {(3)}     {reference (osculating) epoch ($t_0$)} \\
+ \specel {(4-6)}   {position at reference epoch (${\rm \bf r}_0$)} \\
+ \specel {(7-9)}   {velocity at reference epoch (${\rm \bf v}_0$)} \\
+ \specel {(10)}    {heliocentric distance at reference epoch} \\
+ \specel {(11)}    {${\rm \bf r}_0.{\rm \bf v}_0$} \\
+ \specel {(12)}    {date ($t$)} \\
+ \specel {(13)}    {universal eccentric anomaly ($\psi$) of date, approx} \\ \\
+ \spec{JFORMR}{I}{requested element set (1-3; Note~3)}
+}
+\args{RETURNED}
+{
+ \spec{JFORM}{I}{element set actually returned (1-3; Note~4)} \\
+ \spec{EPOCH}{D}{epoch of elements ($t_0$ or $T$, TT MJD)} \\
+ \spec{ORBINC}{D}{inclination ($i$, radians)} \\
+ \spec{ANODE}{D}{longitude of the ascending node ($\Omega$, radians)} \\
+ \spec{PERIH}{D}{longitude or argument of perihelion
+                            ($\varpi$ or $\omega$,} \\
+ \spec{}{}{\hspace{1.5em} radians)} \\
+ \spec{AORQ}{D}{mean distance or perihelion distance ($a$ or $q$, AU)} \\
+ \spec{E}{D}{eccentricity ($e$)} \\
+ \spec{AORL}{D}{mean anomaly or longitude
+                               ($M$ or $L$, radians,} \\
+ \spec{}{}{\hspace{1.5em} JFORM=1,2 only)} \\
+ \spec{DM}{D}{daily motion ($n$, radians, JFORM=1 only)} \\
+ \spec{JSTAT}{I}{status:} \\
+ \spec{}{}{\hspace{2.3em}    0 = OK} \\
+ \spec{}{}{\hspace{1.5em} $-$1 = illegal PMASS} \\
+ \spec{}{}{\hspace{1.5em} $-$2 = illegal JFORMR} \\
+ \spec{}{}{\hspace{1.5em} $-$3 = position/velocity out of allowed range}
+}
+\notes
+{
+ \begin{enumerate}
+  \setlength{\parskip}{\medskipamount}
+  \item The ``universal'' elements are those which define the orbit for the
+        purposes of the method of universal variables (see reference 2).
+        They consist of the combined mass of the two bodies, an epoch,
+        and the position and velocity vectors (arbitrary reference frame)
+        at that epoch.  The parameter set used here includes also various
+        quantities that can, in fact, be derived from the other
+        information.  This approach is taken to avoiding unnecessary
+        computation and loss of accuracy.  The supplementary quantities
+        are (i)~$\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.
+  \item 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.
+  \item Three different element-format options are supported, as
+        follows. \\
+
+        JFORM=1, suitable for the major planets:
+
+        \begin{tabbing}
+        xxx \= xxxxxxxx \= xx \= \kill
+        \> EPOCH  \> = \> epoch of elements $t_0$ (TT MJD) \\
+        \> ORBINC \> = \> inclination $i$ (radians) \\
+        \> ANODE  \> = \> longitude of the ascending node $\Omega$ (radians) \\
+        \> PERIH  \> = \> longitude of perihelion $\varpi$ (radians) \\
+        \> AORQ   \> = \> mean distance $a$ (AU) \\
+        \> E      \> = \> eccentricity $e$ $( 0 \leq e < 1 )$ \\
+        \> AORL   \> = \> mean longitude $L$ (radians) \\
+        \> DM     \> = \> daily motion $n$ (radians)
+        \end{tabbing}
+
+        JFORM=2, suitable for minor planets:
+
+        \begin{tabbing}
+        xxx \= xxxxxxxx \= xx \= \kill
+        \> EPOCH  \> = \> epoch of elements $t_0$ (TT MJD) \\
+        \> ORBINC \> = \> inclination $i$ (radians) \\
+        \> ANODE  \> = \> longitude of the ascending node $\Omega$ (radians) \\
+        \> PERIH  \> = \> argument of perihelion $\omega$ (radians) \\
+        \> AORQ   \> = \> mean distance $a$ (AU) \\
+        \> E      \> = \> eccentricity $e$ $( 0 \leq e < 1 )$ \\
+        \> AORL   \> = \> mean anomaly $M$ (radians)
+        \end{tabbing}
+
+        JFORM=3, suitable for comets:
+
+        \begin{tabbing}
+        xxx \= xxxxxxxx \= xx \= \kill
+        \> EPOCH  \> = \> epoch of perihelion $T$ (TT MJD) \\
+        \> ORBINC \> = \> inclination $i$ (radians) \\
+        \> ANODE  \> = \> longitude of the ascending node $\Omega$ (radians) \\
+        \> PERIH  \> = \> argument of perihelion $\omega$ (radians) \\
+        \> AORQ   \> = \> perihelion distance $q$ (AU) \\
+        \> E      \> = \> eccentricity $e$ $( 0 \leq e \leq 10 )$
+        \end{tabbing}
+  \item 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:
+
+        \begin{tabbing}
+        xx \= xxxxxxxxxx \= xxxxxxxxxxx \= \kill
+        \> 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
+        \end{tabbing}
+  \item The arguments returned for each value of JFORM ({\it cf}\/ Note~5:
+        JFORM may not be the same as JFORMR) are as follows:
+
+        \begin{tabbing}
+        xxx \= xxxxxxxxxxxx \= xxxxxx \= xxxxxx \= \kill
+        \> JFORM  \> 1        \> 2        \> 3 \\ \\
+        \> EPOCH  \> $t_0$    \> $t_0$    \> $T$ \\
+        \> ORBINC \> $i$      \> $i$      \> $i$ \\
+        \> ANODE  \> $\Omega$ \> $\Omega$ \> $\Omega$ \\
+        \> PERIH  \> $\varpi$ \> $\omega$ \> $\omega$ \\
+        \> AORQ   \> $a$      \> $a$      \> $q$ \\
+        \> E      \> $e$      \> $e$      \> $e$ \\
+        \> AORL   \> $L$      \> $M$      \> - \\
+        \> DM     \> $n$      \> -        \> -
+        \end{tabbing}
+
+        where:
+        \begin{tabbing}
+        xxx \= xxxxxxxx \= xxx \= \kill
+        \> $t_0$    \> is the epoch of the elements (MJD, TT) \\
+        \> $T$      \> is the epoch of perihelion (MJD, TT) \\
+        \> $i$      \> is the inclination (radians) \\
+        \> $\Omega$ \> is the longitude of the ascending node (radians) \\
+        \> $\varpi$ \> is the longitude of perihelion (radians) \\
+        \> $\omega$ \> is the argument of perihelion (radians) \\
+        \> $a$      \> is the mean distance (AU) \\
+        \> $q$      \> is the perihelion distance (AU) \\
+        \> $e$      \> is the eccentricity \\
+        \> $L$      \> is the longitude (radians, $0-2\pi$) \\
+        \> $M$      \> is the mean anomaly (radians, $0-2\pi$) \\
+        \> $n$      \> is the daily motion (radians) \\
+        \> - \> means no value is set
+        \end{tabbing}
+  \item 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.
+ \end{enumerate}
+}
+\refs{
+   \begin{enumerate}
+   \item Sterne, Theodore E., {\it An Introduction to Celestial Mechanics,}\/
+         Interscience Publishers, 1960.  Section 6.7, p199.
+   \item Everhart, E. \& Pitkin, E.T., Am.~J.~Phys.~51, 712, 1983.
+   \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_UE2PV}{Pos/Vel from Universal Elements}
+{
+ \action{Heliocentric position and velocity of a planet, asteroid or comet,
+         starting from orbital elements in the ``universal variables'' form.}
+ \call{CALL sla\_UE2PV (DATE, U, PV, JSTAT)}
+}
+\args{GIVEN}
+{
+ \spec{DATE}{D}{date (TT Modified Julian Date = JD$-$2400000.5)}
+}
+\args{GIVEN and RETURNED}
+{
+ \spec{U}{D(13)}{universal orbital elements (updated; Note~1)} \\
+ \specel {(1)}     {combined mass ($M+m$)} \\
+ \specel {(2)}     {total energy of the orbit ($\alpha$)} \\
+ \specel {(3)}     {reference (osculating) epoch ($t_0$)} \\
+ \specel {(4-6)}   {position at reference epoch (${\rm \bf r}_0$)} \\
+ \specel {(7-9)}   {velocity at reference epoch (${\rm \bf v}_0$)} \\
+ \specel {(10)}    {heliocentric distance at reference epoch} \\
+ \specel {(11)}    {${\rm \bf r}_0.{\rm \bf v}_0$} \\
+ \specel {(12)}    {date ($t$)} \\
+ \specel {(13)}    {universal eccentric anomaly ($\psi$) of date, approx}
+}
+\args{RETURNED}
+{
+ \spec{PV}{D(6)}{heliocentric \xyzxyzd, equatorial, J2000} \\
+ \spec{}{}{\hspace{1.5em} (AU, AU/s; Note~1)} \\
+ \spec{JSTAT}{I}{status:} \\
+ \spec{}{}{\hspace{1.95em}      0 = OK} \\
+ \spec{}{}{\hspace{1.2em}    $-$1 = radius vector zero} \\
+ \spec{}{}{\hspace{1.2em}    $-2$ = failed to converge}
+}
+\notes
+{
+ \begin{enumerate}
+  \setlength{\parskip}{\medskipamount}
+  \item 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.
+  \item The companion routine is sla\_EL2UE.  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 sla\_EL2UE 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 sla\_EL2UE once, but then calling the present routine
+        multiple times, which is faster than multiple calls to sla\_PLANEL.
+
+        It is not obligatory to use sla\_EL2UE to obtain the parameters.
+        However, it should be noted that because sla\_EL2UE performs its
+        own validation, no checks on the contents of the array U are made
+        by the present routine.
+  \item 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).
+  \item 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
+        sla\_EL2UE routine in fact produces coordinates with respect to the
+        J2000 equator and equinox.
+  \item 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.
+ \end{enumerate}
+}
+\aref{Everhart, E. \& Pitkin, E.T., Am.~J.~Phys.~51, 712, 1983.}
+%-----------------------------------------------------------------------
+\routine{SLA\_UNPCD}{Remove Radial Distortion}
+{
+ \action{Remove pincushion/barrel distortion from a distorted 
+         \xy\  to give tangent-plane \xy.}
+ \call{CALL sla\_UNPCD (DISCO,X,Y)}
+}
+\args{GIVEN}
+{
+ \spec{DISCO}{D}{pincushion/barrel distortion coefficient} \\
+ \spec{X,Y}{D}{distorted \xy}
+}
+\args{RETURNED}
+{
+ \spec{X,Y}{D}{tangent-plane \xy}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The distortion is of the form $\rho = r (1 + c r^{2})$, where $r$ is
+        the radial distance from the tangent point, $c$ is the DISCO
+        argument, and $\rho$ is the radial distance in the presence of
+        the distortion.
+  \item For {\it pincushion}\/ distortion, C is +ve;  for
+        {\it barrel}\/ distortion, C is $-$ve.
+  \item For X,Y in units of one projection radius (in the case of
+        a photographic plate, the focal length), the following
+        DISCO values apply:
+
+        \vspace{2ex}
+
+        \hspace{5em}
+        \begin{tabular}{|l|c|} \hline
+         Geometry & DISCO \\ \hline \hline
+         astrograph & 0.0 \\ \hline
+         Schmidt & $-$0.3333 \\ \hline
+         AAT PF doublet & +147.069 \\ \hline
+         AAT PF triplet & +178.585 \\ \hline
+         AAT f/8 & +21.20 \\ \hline
+         JKT f/8 & +14.6 \\ \hline
+        \end{tabular}
+
+        \vspace{2ex}
+
+  \item The present routine is an approximate inverse to the
+        companion routine sla\_PCD, obtained from two iterations
+        of Newton's method.  The mismatch between the sla\_PCD
+        and sla\_UNPCD is negligible for astrometric applications;
+        to reach 1~milliarcsec at the edge of the AAT triplet or
+        Schmidt field would require field diameters of \degree{2}{4}
+        and $42^{\circ}$ respectively.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_V2TP}{Direction Cosines to Tangent Plane}
+{
+ \action{Given the direction cosines of a star and of the tangent point,
+         determine the star's tangent-plane coordinates
+         (single precision).}
+ \call{CALL sla\_V2TP (V, V0, XI, ETA, J)}
+}
+\args{GIVEN}
+{
+ \spec{V}{R(3)}{direction cosines of star} \\
+ \spec{V0}{R(3)}{direction cosines of tangent point}
+}
+\args{RETURNED}
+{
+ \spec{XI,ETA}{R}{tangent plane coordinates (radians)} \\
+ \spec{J}{I}{status:} \\
+ \spec{}{}{\hspace{1.5em} 0 = OK, star on tangent plane} \\
+ \spec{}{}{\hspace{1.5em} 1 = error, star too far from axis} \\
+ \spec{}{}{\hspace{1.5em} 2 = error, antistar on tangent plane} \\
+ \spec{}{}{\hspace{1.5em} 3 = error, antistar too far from axis}
+}
+\notes
+{
+ \begin{enumerate}
+  \item If vector V0 is not of unit length, or if vector V is of zero
+        length, the results will be wrong.
+  \item If V0 points at a pole, the returned $\xi,\eta$
+        will be based on the
+        arbitrary assumption that $\alpha=0$ at the tangent point.
+  \item The projection is called the {\it gnomonic}\/ projection;  the
+        Cartesian coordinates \xieta\ are called 
+        {\it standard coordinates.}\/  The latter
+        are in units of the distance from the tangent plane to the projection
+        point, {\it i.e.}\ radians near the origin.
+  \item This routine is the Cartesian equivalent of the routine sla\_S2TP.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_VDV}{Scalar Product}
+{
+ \action{Scalar product of two 3-vectors (single precision).}
+ \call{R~=~sla\_VDV (VA, VB)}
+}
+\args{GIVEN}
+{
+ \spec{VA}{R(3)}{first vector} \\
+ \spec{VB}{R(3)}{second vector}
+}
+\args{RETURNED}
+{
+ \spec{sla\_VDV}{R}{scalar product VA.VB}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_VN}{Normalize Vector}
+{
+ \action{Normalize a 3-vector, also giving the modulus (single precision).}
+ \call{CALL sla\_VN (V, UV, VM)}
+}
+\args{GIVEN}
+{
+ \spec{V}{R(3)}{vector}
+}
+\args{RETURNED}
+{
+ \spec{UV}{R(3)}{unit vector in direction of V} \\
+ \spec{VM}{R}{modulus of V}
+}
+\anote{If the modulus of V is zero, UV is set to zero as well.}
+%-----------------------------------------------------------------------
+\routine{SLA\_VXV}{Vector Product}
+{
+ \action{Vector product of two 3-vectors (single precision).}
+ \call{CALL sla\_VXV (VA, VB, VC)}
+}
+\args{GIVEN}
+{
+ \spec{VA}{R(3)}{first vector} \\
+ \spec{VB}{R(3)}{second vector}
+}
+\args{RETURNED}
+{
+ \spec{VC}{R(3)}{vector product VA$\times$VB}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_WAIT}{Time Delay}
+{
+ \action{Wait for a specified interval.}
+ \call{CALL sla\_WAIT (DELAY)}
+}
+\args{GIVEN}
+{
+ \spec{DELAY}{R}{delay in seconds}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The implementation is machine-specific.
+  \item The delay actually requested is restricted to the range
+        100ns-200s in the present implementation.
+  \item There is no guarantee of accuracy, though on almost all
+        types of computer the program will certainly not
+        resume execution {\it before}\/ the stated interval has
+        elapsed.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_XY2XY}{Apply Linear Model to an \xy}
+{
+ \action{Transform one \xy\ into another using a linear model of the type
+         produced by the sla\_FITXY routine.}
+ \call{CALL sla\_XY2XY (X1,Y1,COEFFS,X2,Y2)}
+}
+\args{GIVEN}
+{
+ \spec{X1,Y1}{D}{\xy\ before transformation} \\
+ \spec{COEFFS}{D(6)}{transformation coefficients (see note)}
+}
+\args{RETURNED}
+{
+ \spec{X2,Y2}{D}{\xy\ after transformation}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The model relates two sets of \xy\ coordinates as follows.
+        Naming the six elements of COEFFS $a,b,c,d,e$ \& $f$,
+        the present routine performs the transformation:
+        \begin{verse}
+          $x_{2} = a + bx_{1} + cy_{1}$ \\
+          $y_{2} = d + ex_{1} + fy_{1}$
+        \end{verse}
+  \item See also sla\_FITXY, sla\_PXY, sla\_INVF, sla\_DCMPF.
+ \end{enumerate}
+}
+%-----------------------------------------------------------------------
+\routine{SLA\_ZD}{$h,\delta$ to Zenith Distance}
+{
+ \action{Hour angle and declination to zenith distance
+         (double precision).}
+ \call{D~=~sla\_ZD (HA, DEC, PHI)}
+}
+\args{GIVEN}
+{
+ \spec{HA}{D}{hour angle in radians} \\
+ \spec{DEC}{D}{declination in radians} \\
+ \spec{PHI}{D}{latitude in radians}
+}
+\args{RETURNED}
+{
+ \spec{sla\_ZD}{D}{zenith distance (radians, $0\!-\!\pi$)}
+}
+\notes
+{
+ \begin{enumerate}
+  \item The latitude must be geodetic.  In critical applications,
+        corrections for polar motion should be applied (see sla\_POLMO).
+  \item 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 zenith distance.  In particular, it may be
+        important to distinguish between the zenith distance
+        as affected by refraction, which would require the
+        {\it observed}\/ \hadec, and the zenith distance {\it in vacuo},
+        which would require the {\it topocentric}\/ \hadec.  If
+        the effects of diurnal aberration can be neglected, the
+        {\it apparent}\/ \hadec\ may be used instead of the
+        {\it topocentric}\/ \hadec.
+  \item No range checking of arguments is done.
+  \item In applications which involve many zenith distance 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 perhaps sine and
+        cosine of declination.
+ \end{enumerate}
+}
+
+\pagebreak
+
+\section{EXPLANATION AND EXAMPLES}
+To guide the writer of positional-astronomy applications software,
+this final chapter puts the SLALIB routines into the context of
+astronomical phenomena and techniques, and presents a few
+``cookbook'' examples
+of the SLALIB calls in action.  The astronomical content of the chapter
+is not, of course, intended to be a substitute for specialist text-books on
+positional astronomy, but may help bridge the gap between
+such books and the SLALIB routines.  For further reading, the following
+cover a wide range of material and styles:
+\begin{itemize}
+\item {\it Explanatory Supplement to the Astronomical Almanac},
+      ed.\ P.\,Kenneth~Seidelmann (1992), University Science Books.
+\item {\it Vectorial Astrometry}, C.\,A.\,Murray (1983), Adam Hilger.
+\item {\it Spherical Astronomy}, Robin~M.\,Green (1985), Cambridge
+      University Press.
+\item {\it Spacecraft Attitude Determination and Control},
+      ed.\ James~R.\,Wertz (1986), Reidel.
+\item {\it Practical Astronomy with your Calculator},
+      Peter~Duffett-Smith (1981), Cambridge University Press.
+\end{itemize}
+Also of considerable value, though out of date in places, are:
+\begin{itemize}
+\item {\it Explanatory Supplement to the Astronomical Ephemeris
+      and the American Ephemeris and Nautical Almanac}, RGO/USNO (1974),
+      HMSO.
+\item {\it Textbook on Spherical Astronomy}, W.\,M.\,Smart (1977),
+      Cambridge University Press.
+\end{itemize}
+Only brief details of individual SLALIB routines are given here, and
+readers will find it useful to refer to the subprogram specifications
+elsewhere in this document.  The source code for the SLALIB routines
+(available in both Fortran and C) is also intended to be used as
+documentation.
+
+\subsection {Spherical Trigonometry}
+Celestial phenomena occur at such vast distances from the
+observer that for most practical purposes there is no need to
+work in 3D;  only the direction
+of a source matters, not how far away it is.  Things can
+therefore be viewed as if they were happening
+on the inside of sphere with the observer at the centre --
+the {\it celestial sphere}.  Problems involving
+positions and orientations in the sky can then be solved by
+using the formulae of {\it spherical trigonometry}, which
+apply to {\it spherical triangles}, the sides of which are
+{\it great circles}.
+
+Positions on the celestial sphere may be specified by using
+a spherical polar coordinate system, defined in terms of
+some fundamental plane and a line in that plane chosen to
+represent zero longitude.  Mathematicians usually work with the
+co-latitude, with zero at the principal pole, whereas most
+astronomical coordinate systems use latitude, reckoned plus and
+minus from the equator.
+Astronomical coordinate systems may be either right-handed
+({\it e.g.}\ right ascension and declination \radec,
+Galactic longitude and latitude \gal)
+or left-handed ({\it e.g.}\ hour angle and
+declination \hadec).  In some cases
+different conventions have been used in the past, a fruitful source of
+mistakes.  Azimuth and geographical longitude are examples;  azimuth
+is now generally reckoned north through east
+(making a left-handed system);  geographical longitude is now usually
+taken to increase eastwards (a right-handed system) but astronomers
+used to employ a west-positive convention.  In reports
+and program comments it is wise to spell out what convention
+is being used, if there is any possibility of confusion.
+
+When applying spherical trigonometry formulae, attention must be
+paid to
+rounding errors (for example it is a bad idea to find a
+small angle through its cosine) and to the possibility of
+problems close to poles.
+Also, if a formulation relies on inspection to establish
+the quadrant of the result, it is an indication that a vector-related
+method might be preferable.
+
+As well as providing many routines which work in terms of specific
+spherical coordinates such as \radec, SLALIB provides
+two routines which operate directly on generic spherical
+coordinates:
+sla\_SEP
+computes the separation between
+two points (the distance along a great circle) and
+sla\_BEAR
+computes the bearing (or {\it position angle})
+of one point seen from the other.  The routines
+sla\_DSEP
+and
+sla\_DBEAR
+are double precision equivalents.  As a simple demonstration
+of SLALIB, we will use these facilities to estimate the distance from
+London to Sydney and the initial compass heading:
+\goodbreak
+\begin{verbatim}
+            IMPLICIT NONE
+
+      *  Degrees to radians
+            REAL D2R
+            PARAMETER (D2R=0.01745329252)
+
+      *  Longitudes and latitudes (radians) for London and Sydney
+            REAL AL,BL,AS,BS
+            PARAMETER (AL=-0.2*D2R,BL=51.5*D2R,AS=151.2*D2R,BS=-33.9*D2R)
+
+      *  Earth radius in km (spherical approximation)
+            REAL RKM
+            PARAMETER (RKM=6375.0)
+
+            REAL sla_SEP,sla_BEAR
+
+
+      *  Distance and initial heading (N=0, E=90)
+            WRITE (*,'(1X,I5,'' km,'',I4,'' deg'')')
+           :    NINT(sla_SEP(AL,BL,AS,BS)*RKM),NINT(sla_BEAR(AL,BL,AS,BS)/D2R)
+
+            END
+\end{verbatim}
+\goodbreak
+(The result is 17011~km, $61^\circ$.)
+
+The routines
+sla\_PAV and
+sla\_DPAV
+are equivalents of sla\_BEAR and sla\_DBEAR but starting from
+direction-cosines instead of spherical coordinates.
+
+\subsubsection{Formatting angles}
+SLALIB has routines for decoding decimal numbers
+from character form and for converting angles to and from
+sexagesimal form (hours, minutes, seconds or degrees,
+arcminutes, arcseconds).  These apparently straightforward
+operations contain hidden traps which the SLALIB routines
+avoid.
+
+There are five routines for decoding numbers from a character
+string, such as might be entered using a keyboard.
+They all work in the same style, and successive calls
+can work their way along a single string decoding
+a sequence of numbers of assorted types.  Number
+fields can be separated by spaces or commas, and can be defaulted
+to previous values or to preset defaults.
+
+Three of the routines decode single numbers:
+sla\_INTIN
+(integer),
+sla\_FLOTIN
+(single precision floating point) and
+sla\_DFLTIN
+(double precision).  A minus sign can be
+detected even when the number is zero;  this avoids
+the frequently-encountered ``minus zero'' bug, where
+declinations {\it etc.}\ in
+the range $0^{\circ}$ to $-1^{\circ}$ mysteriously migrate to
+the range $0^{\circ}$ to $+1^{\circ}$.
+Here is an example (in Fortran) where we wish to
+read two numbers, and integer {\tt IX} and a real, {\tt Y},
+with {\tt X} defaulting to zero and {\tt Y} defaulting to
+{\tt X}:
+\goodbreak
+\begin{verbatim}
+            DOUBLE PRECISION Y
+            CHARACTER*80 A
+            INTEGER IX,I,J
+
+      *  Input the string to be decoded
+            READ (*,'(A)') A
+
+      *  Preset IX to its default value
+            IX = 0
+
+      *  Point to the start of the string
+            I = 1
+
+      *  Decode an integer
+            CALL sla_INTIN(A,I,IX,J)
+            IF (J.GT.1) GO TO ... (bad IX)
+
+      *  Preset Y to its default value
+            Y = DBLE(IX)
+
+      *  Decode a double precision number
+            CALL sla_DFLTIN(A,I,Y,J)
+            IF (J.GT.1) GO TO ... (bad Y)
+\end{verbatim}
+\goodbreak
+Two additional routines decode a 3-field sexagesimal number:
+sla\_AFIN
+(degrees, arcminutes, arcseconds to single
+precision radians) and
+sla\_DAFIN
+(the same but double precision).  They also
+work using other units such as hours {\it etc}.\ if
+you multiply the result by the appropriate factor.  An example
+Fortran program which uses
+sla\_DAFIN
+was given earlier, in section 1.2.
+
+SLALIB provides four routines for expressing an angle in radians
+in a preferred range.  The function
+sla\_RANGE
+expresses an angle
+in the range $\pm\pi$;
+sla\_RANORM
+expresses an angle in the range
+$0-2\pi$.  The functions
+sla\_DRANGE
+and
+sla\_DRANRM
+are double precision versions.
+
+Several routines
+(sla\_CTF2D,
+sla\_CR2AF
+{\it etc.}) are provided to convert
+angles to and from
+sexagesimal form (hours, minute, seconds or degrees,
+arcminutes and arcseconds).
+They avoid the common
+``converting from integer to real at the wrong time''
+bug, which produces angles like \hms{24}{59}{59}{999}.
+Here is a program which displays an hour angle
+stored in radians:
+\goodbreak
+\begin{verbatim}
+            DOUBLE PRECISION HA
+            CHARACTER SIGN
+            INTEGER IHMSF(4)
+            :
+            CALL sla_DR2TF(3,HA,SIGN,IHMSF)
+            WRITE (*,'(1X,A,3I3.2,''.'',I3.3)') SIGN,IHMSF
+\end{verbatim}
+\goodbreak
+
+\subsection {Vectors and Matrices}
+As an alternative to employing a spherical polar coordinate system,
+the direction of an object can be defined in terms of the sum of any
+three vectors as long as they are different and
+not coplanar.  In practice, three vectors at right angles are
+usually chosen, forming a system
+of {\it Cartesian coordinates}.  The {\it x}- and {\it y}-axes
+lie in the fundamental plane ({\it e.g.}\ the equator in the
+case of \radec), with the {\it x}-axis pointing to zero longitude.
+The {\it z}-axis is normal to the fundamental plane and points
+towards positive latitudes.  The {\it y}-axis can lie in either
+of the two possible directions, depending on whether the
+coordinate system is right-handed or left-handed.
+The three axes are sometimes called
+a {\it triad}.  For most applications involving arbitrarily
+distant objects such as stars, the vector which defines
+the direction concerned is constrained to have unit length.
+The {\it x}-, {\it y-} and {\it z-}components
+can be regarded as the scalar (dot) product of this vector
+onto the three axes of the triad in turn.  Because the vector
+is a unit vector,
+each of the three dot-products is simply the cosine of the angle
+between the unit vector and the axis concerned, and the
+{\it x}-, {\it y-} and {\it z-}components are sometimes
+called {\it direction cosines}.
+
+For some applications involving objects
+with the Solar System, unit vectors are inappropriate, and
+it is necessary to use vectors scaled in length-units such as
+AU, km {\it etc.}
+In these cases the origin of the coordinate system may not be
+the observer, but instead might be the Sun, the Solar-System
+barycentre, the centre of the Earth {\it etc.}  But whatever the application,
+the final direction in which the observer sees the object can be
+expressed as direction cosines.
+
+But where has this got us?  Instead of two numbers -- a longitude and
+a latitude -- we now have three numbers to look after
+-- the {\it x}-, {\it y-} and
+{\it z-}components -- whose quadratic sum we have somehow to contrive to
+be unity.  And, in addition to this apparent redundancy,
+most people find it harder to visualize
+problems in terms of \xyz\ than in $[\,\theta,\phi~]$.
+Despite these objections, the vector approach turns out to have
+significant advantages over the spherical trigonometry approach:
+\begin{itemize}
+\item Vector formulae tend to be much more succinct;  one vector
+      operation is the equivalent of strings of sines and cosines.
+\item The formulae are as a rule rigorous, even at the poles.
+\item Accuracy is maintained all over the celestial sphere.
+      When one Cartesian component is nearly unity and
+      therefore insensitive to direction, the others become small
+      and therefore more precise.
+\item Formulations usually deliver the quadrant of the result
+      without the need for any inspection (except within the
+      library function ATAN2).
+\end{itemize}
+A number of important transformations in positional
+astronomy turn out to be nothing more than changes of coordinate
+system, something which is especially convenient if
+the vector approach is used.  A direction with respect
+to one triad can be expressed relative to another triad simply
+by multiplying the \xyz\ column vector by the appropriate
+$3\times3$ orthogonal matrix
+(a tensor of Rank~2, or {\it dyadic}).  The three rows of this
+{\it rotation matrix}\/
+are the vectors in the old coordinate system of the three
+new axes, and the transformation amounts to obtaining the
+dot-product of the direction-vector with each of the three
+new axes.  Precession, nutation, \hadec\ to \azel,
+\radec\ to \gal\ and so on are typical examples of the
+technique.  A useful property of the rotation matrices
+is that they can be inverted simply by taking the transpose.
+
+The elements of these vectors and matrices are assorted combinations of
+the sines and cosines of the various angles involved (hour angle,
+declination and so on, depending on which transformation is
+being applied).  If you write out the matrix multiplications
+in full you get expressions which are essentially the same as the
+equivalent spherical trigonometry formulae.  Indeed, many of the
+standard formulae of spherical trigonometry are most easily
+derived by expressing the problem initially in
+terms of vectors.
+
+\subsubsection{Using vectors}
+SLALIB provides conversions between spherical and vector
+form
+(sla\_CS2C,
+sla\_CC2S
+{\it etc.}), plus an assortment
+of standard vector and matrix operations
+(sla\_VDV,
+sla\_MXV
+{\it etc.}).
+There are also routines
+(sla\_EULER
+{\it etc.}) for creating a rotation matrix
+from three {\it Euler angles}\/ (successive rotations about
+specified Cartesian axes).  Instead of Euler angles, a rotation
+matrix can be expressed as an {\it axial vector}\/ (the pole of the rotation,
+and the amount of rotation), and routines are provided for this
+(sla\_AV2M,
+sla\_M2AV
+{\it etc.}).
+
+Here is an example where spherical coordinates {\tt P1} and {\tt Q1}
+undergo a coordinate transformation and become {\tt P2} and {\tt Q2};
+the transformation consists of a rotation of the coordinate system
+through angles {\tt A}, {\tt B} and {\tt C} about the
+{\it z}, new {\it y}\/ and new {\it z}\/ axes respectively:
+\goodbreak
+\begin{verbatim}
+            REAL A,B,C,R(3,3),P1,Q1,V1(3),V2(3),P2,Q2
+             :
+      *  Create rotation matrix
+            CALL sla_EULER('ZYZ',A,B,C,R)
+
+      *  Transform position (P,Q) from spherical to Cartesian
+            CALL sla_CS2C(P1,Q1,V1)
+
+      *  Multiply by rotation matrix
+            CALL sla_MXV(R,V1,V2)
+
+      *  Back to spherical
+            CALL sla_CC2S(V2,P2,Q2)
+\end{verbatim}
+\goodbreak
+Small adjustments to the direction of a position
+vector are often most conveniently described in terms of
+$[\,\Delta x,\Delta y, \Delta z\,]$.  Adding the correction
+vector needs careful handling if the position
+vector is to remain of length unity, an advisable precaution which
+ensures that
+the \xyz\ components are always available to mean the cosines of
+the angles between the vector and the axis concerned.  Two types
+of shifts are commonly used,
+the first where a small vector of arbitrary direction is
+added to the unit vector, and the second where there is a displacement
+in the latitude coordinate (declination, elevation {\it etc.}) alone.
+
+For a shift produced by adding a small \xyz\ vector ${\bf D}$ to a
+unit vector ${\bf V1}$, the resulting vector ${\bf V2}$ has direction
+$<{\bf V1}+{\bf D}>$ but is no longer of unit length.  A better approximation
+is available if the result is multiplied by a scaling factor of
+$(1-{\bf D}\cdot{\bf V1})$, where the dot
+means scalar product.  In Fortran:
+\goodbreak
+\begin{verbatim}
+            F = (1D0-(DX*V1X+DY*V1Y+DZ*V1Z))
+            V2X = F*(V1X+DX)
+            V2Y = F*(V1Y+DY)
+            V2Z = F*(V1Z+DZ)
+\end{verbatim}
+\goodbreak
+\noindent
+The correction for diurnal aberration (discussed later) is
+an example of this form of shift.
+
+As an example of the second kind of displacement
+we will apply a small change in elevation $\delta E$ to an
+\azel\ direction vector.  The direction of the
+result can be obtained by making the allowable approximation
+${\tan \delta E\approx\delta E}$ and adding a adjustment
+vector of length $\delta E$ normal
+to the direction vector in the vertical plane containing the direction
+vector.  The $z$-component of the adjustment vector is
+$\delta E \cos E$,
+and the horizontal component is
+$\delta E \sin E$ which has then to be
+resolved into $x$ and $y$ in proportion to their current sizes. To
+approximate a unit vector more closely, a correction factor of
+$\cos \delta E$ can then be applied, which is nearly
+$(1-\delta E^2 /2)$ for
+small $\delta E$.  Expressed in Fortran, for initial vector
+{\tt V1X,V1Y,V1Z}, change in elevation {\tt DEL}
+(+ve $\equiv$ upwards), and result
+vector {\tt V2X,V2Y,V2Z}:
+\goodbreak
+\begin{verbatim}
+            COSDEL = 1D0-DEL*DEL/2D0
+            R1 = SQRT(V1X*V1X+V1Y*V1Y)
+            F = COSDEL*(R1-DEL*V1Z)/R1
+            V2X = F*V1X
+            V2Y = F*V1Y
+            V2Z = COSDEL*(V1Z+DEL*R1)
+\end{verbatim}
+\goodbreak
+An example of this type of shift is the correction for atmospheric
+refraction (see later).
+Depending on the relationship between $\delta E$ and $E$, special
+handling at the pole (the zenith for our example) may be required.
+
+SLALIB includes routines for the case where both a position
+and a velocity are involved.  The routines
+sla\_CS2C6
+and
+sla\_CC62S
+convert from $[\theta,\phi,\dot{\theta},\dot{\phi}]$
+to \xyzxyzd\ and back;
+sla\_DCS26
+and
+sla\_DC62S
+are double precision equivalents.
+
+\subsection {Celestial Coordinate Systems}
+SLALIB has routines to perform transformations
+of celestial positions between different spherical
+coordinate systems, including those shown in the following table:
+
+\begin{center}
+\begin{tabular}{|l|c|c|c|c|c|c|} \hline
+{\it system} & {\it symbols} & {\it longitude} & {\it latitude} &
+          {\it x-y plane} & {\it long.\ zero} & {\it RH/LH}
+\\ \hline \hline
+horizon & -- & azimuth & elevation & horizontal & north & L
+\\ \hline
+equatorial & $\alpha,\delta$ & R.A.\ & Dec.\ & equator & equinox & R
+\\ \hline
+local equ.\ & $h,\delta$ & H.A.\ & Dec.\ & equator & meridian & L
+\\ \hline
+ecliptic & $\lambda,\beta$ & ecl.\ long.\ & ecl.\ lat.\ &
+                                       ecliptic & equinox & R
+\\ \hline
+galactic & $l^{I\!I},b^{I\!I}$ & gal.\ long.\ & gal.\ lat.\ &
+                                       gal.\ equator & gal.\ centre & R
+\\ \hline
+supergalactic & SGL,SGB & SG long.\ & SG lat.\ &
+                                       SG equator & node w.\ gal.\ equ.\ & R
+\\ \hline
+\end{tabular}
+\end{center}
+Transformations between \hadec\ and \azel\ can be performed by
+calling
+sla\_E2H
+and
+sla\_H2E,
+or, in double precision,
+sla\_DE2H
+and
+sla\_DH2E.
+There is also a routine for obtaining
+zenith distance alone for a given \hadec,
+sla\_ZD,
+and one for determining the parallactic angle,
+sla\_PA.
+Three routines are included which relate to altazimuth telescope
+mountings.  For a given \hadec\ and latitude,
+sla\_ALTAZ
+returns the azimuth, elevation and parallactic angle, plus
+velocities and accelerations for sidereal tracking.
+The routines
+sla\_PDA2H
+and
+sla\_PDQ2H
+predict at what hour angle a given azimuth or
+parallactic angle will be reached.
+
+The routines
+sla\_EQECL
+and
+sla\_ECLEQ
+transform between ecliptic
+coordinates and \radec\/; there is also a routine for generating the
+equatorial to ecliptic rotation matrix for a given date:
+sla\_ECMAT.
+
+For conversion between Galactic coordinates and \radec\ there are
+two sets of routines, depending on whether the \radec\ is
+old-style, B1950, or new-style, J2000;
+sla\_EG50
+and
+sla\_GE50
+are \radec\ to \gal\ and {\it vice versa}\/ for the B1950 case, while
+sla\_EQGAL
+and
+sla\_GALEQ
+are the J2000 equivalents.
+
+Finally, the routines
+sla\_GALSUP
+and
+sla\_SUPGAL
+transform \gal\ to de~Vaucouleurs supergalactic longitude and latitude
+and {\it vice versa.}
+
+It should be appreciated that the table, above, constitutes
+a gross oversimplification.   Apparently
+simple concepts such as equator, equinox {\it etc.}\ are apt to be very hard to
+pin down precisely (polar motion, orbital perturbations \ldots) and
+some have several interpretations, all subtly different.  The various
+frames move in complicated ways with respect to one another or to
+the stars (themselves in motion).  And in some instances the
+coordinate system is slightly distorted, so that the
+ordinary rules of spherical trigonometry no longer strictly apply.
+
+These {\it caveats}\/
+apply particularly to the bewildering variety of different
+\radec\ systems that are in use.  Figure~1 shows how
+some of these systems are related, to one another and
+to the direction in which a celestial source actually
+appears in the sky.  At the top of the diagram are
+the various sorts of {\it mean place}\/
+found in star catalogues and papers;\footnote{One frame not included in
+Figure~1 is that of the Hipparcos catalogue.  This is currently the
+best available implementation in the optical of the {\it International
+Celestial Reference System}\/ (ICRS), which is based on extragalactic
+radio sources observed by VLBI.  The distinction between FK5 J2000
+and Hipparcos coordinates only becomes important when accuracies of
+50~mas or better are required.  More details are given in
+Section~4.14.} at the bottom is the
+{\it observed}\/ \azel, where a perfect theodolite would
+be pointed to see the source;  and in the body of
+the diagram are
+the intermediate processing steps and coordinate
+systems.  To help
+understand this diagram, and the SLALIB routines that can
+be used to carry out the various calculations, we will look at the coordinate
+systems involved, and the astronomical phenomena that
+affect them.
+
+\begin{figure}
+\begin{center}
+\begin{tabular}{|cccccc|}   \hline
+& & & & & \\
+\hspace{5em} & \hspace{5em} & \hspace{5em} &
+   \hspace{5em} & \hspace{5em} & \hspace{5em}  \\
+\multicolumn{2}{|c}{\hspace{0em}\fbox{\parbox{8.5em}{\center \vspace{-2ex}
+                                                   mean \radec, FK4, \\
+                                                   any equinox
+                                                   \vspace{0.5ex}}}} &
+ \multicolumn{2}{c}{\hspace{0em}\fbox{\parbox{8.5em}{\center \vspace{-2ex}
+                                                   mean \radec, FK4,
+                                                   no $\mu$, any equinox
+                                                   \vspace{0.5ex}}}} &
+\multicolumn{2}{c|}{\hspace{0em}\fbox{\parbox{8.5em}{\center \vspace{-2ex}
+                                                   mean \radec, FK5, \\
+                                                   any equinox
+                                                   \vspace{0.5ex}}}} \\
+& \multicolumn{2}{|c|}{} & \multicolumn{2}{c|}{} & \\
+\multicolumn{2}{|c}{space motion} & \multicolumn{1}{c|}{} & &
+   \multicolumn{2}{c|}{space motion} \\
+\multicolumn{2}{|c}{-- E-terms} &
+   \multicolumn{2}{c}{-- E-terms} & \multicolumn{1}{c|}{} & \\
+\multicolumn{2}{|c}{precess to B1950} & \multicolumn{2}{c}{precess to B1950} &
+   \multicolumn{2}{c|}{precess to J2000} \\
+\multicolumn{2}{|c}{+ E-terms} &
+   \multicolumn{2}{c}{+ E-terms} & \multicolumn{1}{c|}{} & \\
+\multicolumn{2}{|c}{FK4 to FK5, no $\mu$} &
+   \multicolumn{2}{c}{FK4 to FK5, no $\mu$} & \multicolumn{1}{c|}{} & \\
+\multicolumn{2}{|c}{parallax} & \multicolumn{1}{c|}{} & &
+   \multicolumn{2}{c|}{parallax} \\
+& \multicolumn{2}{|c|}{} & \multicolumn{2}{c|}{} & \\ \cline{2-5}
+\multicolumn{3}{|c|}{} & & & \\
+& \multicolumn{4}{c}{\fbox{\parbox{18em}{\center \vspace{-2ex}
+                                   FK5, J2000, current epoch, geocentric
+                                          \vspace{0.5ex}}}} & \\
+\multicolumn{3}{|c|}{} & & & \\
+& \multicolumn{4}{c}{light deflection} & \\
+& \multicolumn{4}{c}{annual aberration} & \\
+& \multicolumn{4}{c}{precession/nutation} & \\
+\multicolumn{3}{|c|}{} & & & \\
+& \multicolumn{4}{c}{\fbox{Apparent \radec}} & \\
+\multicolumn{3}{|c|}{} & & & \\
+& \multicolumn{4}{c}{Earth rotation} & \\
+\multicolumn{3}{|c|}{} & & & \\
+& \multicolumn{4}{c}{\fbox{Apparent \hadec}} & \\
+\multicolumn{3}{|c|}{} & & & \\
+& \multicolumn{4}{c}{diurnal aberration} & \\
+\multicolumn{3}{|c|}{} & & & \\
+& \multicolumn{4}{c}{\fbox{Topocentric \hadec}} & \\
+\multicolumn{3}{|c|}{} & & & \\
+& \multicolumn{4}{c}{\hadec\ to \azel} & \\
+\multicolumn{3}{|c|}{} & & & \\
+& \multicolumn{4}{c}{\fbox{Topocentric \azel}} & \\
+\multicolumn{3}{|c|}{} & & & \\
+& \multicolumn{4}{c}{refraction} & \\
+\multicolumn{3}{|c|}{} & & & \\
+& \multicolumn{4}{c}{\fbox{Observed \azel}} & \\
+& & & & & \\
+& & & & & \\ \hline
+\end{tabular}
+\end{center}
+\vspace{-0.5ex}
+\caption{Relationship Between Celestial Coordinates}
+
+Star positions are published or catalogued using
+one of the mean \radec\ systems shown at
+the top.  The ``FK4'' systems
+were used before about 1980 and are usually
+equinox B1950.  The ``FK5'' system, equinox J2000, is now preferred,
+or rather its modern equivalent, the International Celestial Reference
+Frame (in the optical, the Hipparcos catalogue).
+The figure relates a star's mean \radec\ to the actual
+line-of-sight to the star.
+Note that for the conventional choices of equinox, namely
+B1950 or J2000, all of the precession and E-terms corrections
+are superfluous.
+\end{figure}
+
+\subsection{Precession and Nutation}
+{\it Right ascension and declination}, (\radec), are the names
+of the longitude and latitude in a spherical
+polar coordinate system based on the Earth's axis of rotation.
+The zero point of $\alpha$ is the point of intersection of
+the {\it celestial
+equator}\/ and the {\it ecliptic}\/ (the apparent path of the Sun
+through the year) where the Sun moves into the northern
+hemisphere.  This point is called the
+{\it first point of Aries},
+the {\it vernal equinox}\/ (with apologies to
+southern-hemisphere readers) or simply the {\it equinox}.\footnote{With
+the introduction of the International Celestial Reference System (ICRS), the
+connection between (i)~star coordinates and (ii)~the Earth's orientation
+and orbit has been broken.  However, the orientation of the
+International Celestial Reference Frame (ICRF) axes was, for convenience,
+chosen to match J2000 FK5, and for most practical purposes ICRF coordinates
+(for example entries in the Hipparcos catalogue) can be regarded as
+synonymous with J2000 FK5.  See Section 4.14 for further details.}
+
+This simple picture is unfortunately
+complicated by the difficulty of defining
+a suitable equator and equinox.  One problem is that the
+Sun's apparent motion is not completely regular, due to the
+ellipticity of the Earth's orbit and its continuous disturbance
+by the Moon and planets.  This is dealt with by
+separating the motion into (i)~a smooth and steady {\it mean Sun}\/
+and (ii)~a set of periodic corrections and perturbations; only the former
+is involved in establishing reference frames and timescales.
+A second, far larger problem, is that
+the celestial equator and the ecliptic
+are both moving with respect to the stars.
+These motions arise because of the gravitational
+interactions between the Earth and the other solar-system bodies.
+
+By far the largest effect is the
+so-called ``precession of the equinoxes'', where the Earth's
+rotation axis sweeps out a cone centred on the ecliptic
+pole, completing one revolution in about 26,000 years.  The
+cause of the motion is the torque exerted on the distorted and
+spinning Earth by the Sun and the Moon.  Consider the effect of the
+Sun alone, at or near the northern summer solstice.  The Sun
+`sees' the top (north pole) of the Earth tilted towards it
+(by about \degree{23}{5}, the {\it obliquity of the
+ecliptic}\/),
+and sees the nearer part of the Earth's equatorial bulge
+below centre and the further part above centre.
+Although the Earth is in free fall,
+the gravitational force on the nearer part of the
+equatorial bulge is greater than that on the further part, and
+so there is a net torque acting
+as if to eliminate the tilt.  Six months later the same thing
+is happening in reverse, except that the torque is still
+trying to eliminate the tilt.  In between (at the equinoxes) the
+torque shrinks to zero.  A torque acting on a spinning body
+is gyroscopically translated
+into a precessional motion of the spin axis at right-angles to the torque,
+and this happens to the Earth.
+The motion varies during the
+year, going through two maxima, but always acts in the
+same direction.  The Moon produces the same effect,
+adding a contribution to the precession which peaks twice
+per month.  The Moon's proximity to the Earth more than compensates
+for its smaller mass and gravitational attraction, so that it
+in fact contributes most of the precessional effect.
+
+The complex interactions between the three bodies produce a
+precessional motion that is wobbly rather than completely smooth.
+However, the main 26,000-year component is on such a grand scale that
+it dwarfs the remaining terms, the biggest of
+which has an amplitude of only \arcseci{17} and a period of
+about 18.6~years.  This difference of scale makes it convenient to treat
+these two components of the motion separately.  The main 26,000-year
+effect is called {\it luni-solar precession};  the smaller,
+faster, periodic terms are called the {\it nutation}.
+
+Note that precession and nutation are simply
+different frequency components of the same physical effect.  It is
+a common misconception that precession is caused
+by the Sun and nutation is caused by the Moon.  In fact
+the Moon is responsible for two-thirds of the precession, and,
+while it is true that much of the complex detail of the nutation is
+a reflection of the intricacies of the lunar orbit, there are
+nonetheless important solar terms in the nutation.
+
+In addition to and quite separate
+from the precession/nutation effect, the orbit of the Earth-Moon system
+is not fixed in orientation, a result of the attractions of the
+planets.  This slow (about \arcsec{0}{5}~per~year)
+secular rotation of the ecliptic about a slowly-moving diameter is called,
+confusingly, {\it planetary
+precession}\/ and, along with the luni-solar precession is
+included in the {\it general precession}.  The equator and
+ecliptic as affected by general precession
+are what define the various ``mean'' \radec\ reference frames.
+
+The models for precession and nutation come from a combination
+of observation and theory, and are subject to continuous
+refinement.  Nutation models in particular have reached a high
+degree of sophistication, taking into account such things as
+the non-rigidity of the Earth and the effects of
+the planets; SLALIB's nutation
+model (IAU~1980) involves 106 terms in each of $\psi$ (longitude)
+and $\epsilon$ (obliquity), some as small as \arcsec{0}{0001}.
+
+\subsubsection{SLALIB support for precession and nutation}
+SLALIB offers a choice of three precession models:
+\begin{itemize}
+\item The old Bessel-Newcomb, pre IAU~1976, ``FK4'' model, used for B1950
+      star positions and other pre-1984.0 purposes
+(sla\_PREBN).
+\item The new Fricke, IAU~1976, ``FK5'' model, used for J2000 star
+      positions and other post-1984.0 purposes
+(sla\_PREC).
+\item A model published by Simon {\it et al.}\ which is more accurate than
+      the IAU~1976 model and which is suitable for long
+      periods of time
+(sla\_PRECL).
+\end{itemize}
+In each case, the named SLALIB routine generates the $(3\times3)$
+{\it precession
+matrix}\/ for a given start and finish time.  For example,
+here is the Fortran code for generating the rotation
+matrix which describes the precession between the epochs
+J2000 and J1985.372 (IAU 1976 model):
+\goodbreak
+\begin{verbatim}
+            DOUBLE PRECISION PMAT(3,3)
+             :
+            CALL sla_PREC(2000D0,1985.372D0,PMAT)
+\end{verbatim}
+\goodbreak
+It is instructive to examine the resulting matrix:
+\goodbreak
+\begin{verbatim}
+            +0.9999936402  +0.0032709208  +0.0014214694
+            -0.0032709208  +0.9999946505  -0.0000023247
+            -0.0014214694  -0.0000023248  +0.9999989897
+\end{verbatim}
+\goodbreak
+Note that the diagonal elements are close to unity, and the
+other elements are small.  This shows that over an interval as
+short as 15~years the precession isn't going to move a
+position vector very far (in this case about \degree{0}{2}).
+
+For convenience, a direct \radec\ to \radec\ precession routine is
+also provided
+(sla\_PRECES),
+suitable for either the old or the new system (but not a
+mixture of the two).
+
+SLALIB provides only one nutation model, the new, IAU~1980 model,
+implemented in the routine
+sla\_NUTC.
+This returns the components of nutation
+in longitude and latitude (and also provides the obliquity) from
+which a nutation matrix can be generated by calling
+sla\_DEULER
+(and from which the {\it equation of the equinoxes}, described
+later, can be found).  Alternatively,
+the nutation matrix can be generated in a single call by using
+sla\_NUT.
+
+A rotation matrix for applying the entire precession/nutation
+transformation in one go can be generated by calling
+sla\_PRENUT.
+
+\subsection{Mean Places}
+The main effect of the precession/nutation is a steady increase of about
+\arcseci{50}/year in the ecliptic longitudes of the stars.  It is therefore
+essential, when reporting the position of an astronomical target, to
+qualify the coordinates with a date, or {\it epoch}.
+Specifying the epoch ties down the equator and
+equinox which define the \radec\ coordinate system that is
+being used.
+\footnote{An equinox is, however, not required for coordinates
+in the International Celestial Reference System.  Such coordinates must
+be labelled simply ``ICRS'', or the specific catalogue can be mentioned,
+such as ``Hipparcos'';  constructions such as ``Hipparcos, J2000'' are
+redundant and misleading.}  For simplicity, only
+the smooth and steady ``general
+precession'' part of the complete precession/nutation effect is
+included, thereby defining what is called the {\it mean}\/
+equator and equinox for the epoch concerned.  We say a star
+has a mean place of (for example)
+\hms{12}{07}{58}{09}~\dms{-19}{44}{37}{1} ``with respect to the mean equator
+and equinox of epoch J2000''.  The short way of saying
+this is ``\radec\ equinox J2000'' ({\bf not} ``\radec\ epoch J2000'', 
+which means something different to do with
+proper motion).
+
+\subsection{Epoch}
+The word ``epoch'' just means a moment in time, and can be supplied
+in a variety of forms, using different calendar systems and timescales.
+
+For the purpose of specifying the epochs associated with the
+mean place of a star, two conventions exist.  Both sorts of epoch
+superficially resemble years AD but are not tied to the civil
+(Gregorian) calendar;  to distinguish them from ordinary calendar-years
+there is often
+a ``.0'' suffix (as in ``1950.0''), although any other fractional
+part is perfectly legal ({\it e.g.}\ 1987.5).
+
+The older system,
+{\it Besselian epoch}, is defined in such a way that its units are
+tropical years of about 365.2422~days and its timescale is the
+obsolete {\it Ephemeris Time}.
+The start of the Besselian year is the moment
+when the ecliptic longitude of the mean Sun is
+$280^{\circ}$;  this happens near the start of the
+calendar year (which is why $280^{\circ}$ was chosen).
+
+The new system, {\it Julian epoch}, was adopted as
+part of the IAU~1976 revisions (about which more will be said
+in due course) and came formally into use at the
+beginning of 1984.  It uses the Julian year of exactly
+365.25~days; Julian epoch 2000 is defined to be 2000~January~1.5 in the
+TT timescale.
+
+For specifying mean places, various standard epochs are in use, the
+most common ones being Besselian epoch 1950.0 and Julian epoch 2000.0.
+To distinguish the two systems, Besselian epochs
+are now prefixed ``B'' and Julian epochs are prefixed ``J''.
+Epochs without an initial letter can be assumed to be Besselian
+if before 1984.0, otherwise Julian.  These details are supported by
+the SLALIB routines
+sla\_DBJIN
+(decodes numbers from a
+character string, accepting an optional leading B or J),
+sla\_KBJ
+(decides whether B or J depending on prefix or range) and
+sla\_EPCO
+(converts one epoch to match another).
+
+SLALIB has four routines for converting
+Besselian and Julian epochs into other forms.
+The functions
+sla\_EPB2D
+and
+sla\_EPJ2D
+convert Besselian and Julian epochs into MJD; the functions
+sla\_EPB
+and
+sla\_EPJ
+do the reverse.  For example, to express B1950 as a Julian epoch:
+\goodbreak
+\begin{verbatim}
+            DOUBLE PRECISION sla_EPJ,sla_EPB2D
+             :
+            WRITE (*,'(1X,''J'',F10.5)') sla_EPJ(sla_EPB2D(1950D0))
+\end{verbatim}
+\goodbreak
+(The answer is J1949.99979.)
+
+\subsection{Proper Motion}
+Stars in catalogues usually have, in addition to the 
+\radec\  coordinates, a {\it proper motion} $[\mu_\alpha,\mu_\delta]$.
+This is an intrinsic motion
+of the star across the background.  Very few stars have a
+proper motion which exceeds \arcseci{1}/year, and most are
+far below this level.  A star observed as part of normal
+astronomy research will, as a rule, have a proper motion
+which is unknown.
+
+Mean \radec\ and rate of change are not sufficient to pin
+down a star;  the epoch at which the \radec\ was or will
+be correct is also needed.  Note the distinction
+between the epoch which specifies the
+coordinate system and the epoch at which the star passed
+through the given \radec.  The full specification for a star
+is \radec, proper motions, equinox and epoch (plus something to
+identify which set of models for the precession {\it etc.}\ is 
+being used -- see the next section).
+For convenience, coordinates given in star catalogues are almost
+always adjusted to make the equinox and epoch the same -- for
+example B1950 in the case of the SAO~catalogue.
+
+SLALIB provides one routine to handle proper motion on its own,
+sla\_PM.
+Proper motion is also allowed for in various other
+routines as appropriate, for example
+sla\_MAP
+and
+sla\_FK425.
+Note that in all SLALIB routines which involve proper motion
+the units are radians per year and the
+$\alpha$ component is in the form $\dot{\alpha}$ ({\it i.e.}\ big
+numbers near the poles).
+Some star catalogues have proper motion per century, and
+in some catalogues the $\alpha$ component is in the form
+$\dot{\alpha}\cos\delta$ ({\it i.e.}\ angle on the sky).
+
+\subsection{Parallax and Radial Velocity}
+For the utmost accuracy and the nearest stars, allowance can
+be made for {\it annual parallax}\/ and for the effects of perspective
+on the proper motion.
+
+Parallax is appreciable only for nearby stars;  even
+the nearest, Proxima Centauri, is displaced from its average
+position by less than
+an arcsecond as the Earth revolves in its orbit.
+
+For stars with a known parallax, knowledge of the radial velocity
+allows the proper motion to be expressed as an actual space
+motion in 3~dimensions.  The proper motion is,
+in fact, a snapshot of the transverse component of the
+space motion, and in the case of nearby stars will
+change with time due to perspective.
+
+SLALIB does not provide facilities for handling parallax
+and radial-velocity on their own, but their contribution is
+allowed for in such routines as
+sla\_PM,
+sla\_MAP
+and
+sla\_FK425.
+Catalogue mean
+places do not include the effects of parallax and are therefore
+{\it barycentric};  when pointing telescopes {\it etc.}\ it is 
+usually most efficient to apply the slowly-changing
+parallax correction to the mean place of the target early on
+and to work with the {\it geocentric}\/ mean place.  This latter
+approach is implied in Figure~1.
+
+\subsection{Aberration}
+The finite speed of light combined with the motion of the observer
+around the Sun during the year causes apparent displacements of
+the positions of the stars.  The effect is called
+the {\it annual aberration} (or ``stellar''
+aberration).  Its maximum size, about \arcsec{20}{5},
+occurs for stars $90^{\circ}$ from the point towards which
+the Earth is headed as it orbits the Sun;  a star exactly in line with
+the Earth's motion is not displaced.  To receive the light of
+a star, the telescope has to be offset slightly in the direction of
+the Earth's motion.  A familiar analogy is the need to tilt your
+umbrella forward when on the move, to avoid getting wet.  This
+Newtonian model is,
+in fact, highly misleading in the context of light as opposed
+to rain, but happens to give the same answer as a relativistic
+treatment to first order (better than 1~milliarcsecond).
+
+Before the IAU 1976 resolutions, different
+values for the approximately
+\arcsec{20}{5} {\it aberration constant}\/ were employed
+at different times, and this can complicate comparisons
+between different catalogues.  Another complication comes from
+the so-called {\it E-terms of aberration},
+that small part of the annual aberration correction that is a
+function of the eccentricity of the Earth's orbit.  The E-terms,
+maximum amplitude about \arcsec{0}{3},
+happen to be approximately constant for a given star, and so they
+used to be incorporated in the catalogue \radec\/
+to reduce the labour of converting to and from apparent place.
+The E-terms can be removed from a catalogue \radec\/ by
+calling
+sla\_SUBET
+or applied (for example to allow a pulsar
+timing-position to be plotted on a B1950 finding chart)
+by calling
+sla\_ADDET;
+the E-terms vector itself can be obtained by calling
+sla\_ETRMS.
+Star positions post IAU 1976 are free of these distortions, and to
+apply corrections for annual aberration involves the actual
+barycentric velocity of the Earth rather than the use of
+canonical circular-orbit models.
+
+The annual aberration is the aberration correction for
+an imaginary observer at the Earth's centre.
+The motion of a real observer around the Earth's rotation axis in
+the course of the day makes a small extra contribution to the total
+aberration effect called the {\it diurnal aberration}.  Its
+maximum amplitude is about \arcsec{0}{2}.
+
+No SLALIB routine is provided for calculating the aberration on
+its own, though the required velocity vectors can be
+generated using
+sla\_EVP
+and
+sla\_GEOC.
+Annual and diurnal aberration are allowed for where required, for example in
+sla\_MAP
+{\it etc}.\ and
+sla\_AOP
+{\it etc}.  Note that this sort
+of aberration is different from the {\it planetary
+aberration}, which is the apparent displacement of a solar-system
+body, with respect to the ephemeris position, as a consequence
+of the motion of {\it both}\/ the Earth and the source.  The
+planetary aberration can be computed either by correcting the
+position of the solar-system body for light-time, followed by
+the ordinary stellar aberration correction, or more
+directly by expressing the position and velocity of the source
+in the observer's frame and correcting for light-time alone.
+
+\subsection{Different Sorts of Mean Place}
+A particularly confusing aspect of published mean places is that they
+are sensitive to the precise way they were determined.  A mean
+place is not directly observable, even with fundamental
+instruments such as transit circles, and to produce a mean
+place will involve relying on some existing star catalogue,
+for example the fundamental catalogues FK4 and FK5,
+and applying given mathematical models of precession, nutation,
+aberration and so on.
+Note in particular that no star catalogue,
+even a fundamental catalogue such as FK4 or
+FK5, defines a coordinate system, strictly speaking;
+it is merely a list of star positions and proper motions.
+However, once the stars from a given catalogue
+are used as position calibrators, {\it e.g.}\ for
+transit-circle observations or for plate reductions, then a
+broader sense of there being a coordinate grid naturally
+arises, and such phrases as ``in the system of
+the FK4'' can legitimately be employed.  However,
+there is no formal link between the
+two concepts -- no ``standard least squares fit'' between
+reality and the inevitably flawed catalogues.\footnote{This was
+true until the inception of the International Celestial Reference
+System, which is based on the idea of axes locked into the
+distant background.  The coordinates
+of the extragalactic sources which realize these
+axes have no individual significance; there is a ``no net rotation''
+condition which has to be satisfied each time any revisions take
+place.}  All such
+catalogues suffer at some level from systematic, zonal distortions
+of both the star positions and of the proper motions,
+and include measurement errors peculiar to individual
+stars.
+
+Many of these complications are of little significance except to
+specialists.  However, observational astronomers cannot
+escape exposure to at least the two main varieties of
+mean place, loosely called
+FK4 and FK5, and should be aware of
+certain pitfalls.  For most practical purposes the more recent
+system, FK5, is free of surprises and tolerates naive
+use well.  FK4, in contrast, contains two important traps:
+\begin{itemize}
+\item The FK4 system rotates at about
+      \arcsec{0}{5} per century relative to distant galaxies.
+      This is manifested as a systematic distortion in the
+      proper motions of all FK4-derived catalogues, which will
+      in turn pollute any astrometry done using those catalogues.
+      For example, FK4-based astrometry of a QSO using plates
+      taken decades apart will reveal a non-zero {\it fictitious proper
+      motion}, and any FK4 star which happens to have zero proper
+      motion is, in fact, slowly moving against the distant
+      background.  The FK4 frame rotates because it was
+      established before the nature of the Milky Way, and hence the
+      existence of systematic motions of nearby stars, had been
+      recognized.
+\item Star positions in the FK4 system are part-corrected for
+      annual aberration (see above) and embody the so-called
+      E-terms of aberration.
+\end{itemize}
+The change from the old FK4-based system to FK5
+occurred at the beginning
+of 1984 as part of a package of resolutions made by the IAU in 1976,
+along with the adoption of J2000 as the reference epoch.  Star
+positions in the newer, FK5, system are free from the E-terms, and
+the system is a much better approximation to an
+inertial frame (about five times better).
+
+It may occasionally be convenient to specify the FK4 fictitious proper
+motion directly.  In FK4, the centennial proper motion of (for example)
+a QSO is:
+
+$\mu_\alpha=-$\tsec{0}{015869}$
+          +(($\tsec{0}{029032}$~\sin \alpha
+            +$\tsec{0}{000340}$~\cos \alpha ) \sin \delta
+            -$\tsec{0}{000105}$~\cos \alpha
+            -$\tsec{0}{000083}$~\sin \alpha ) \sec \delta $ \\
+$\mu_\delta\,=+$\arcsec{0}{43549}$~\cos \alpha
+              -$\arcsec{0}{00510}$~\sin \alpha +
+              ($\arcsec{0}{00158}$~\sin \alpha
+              -$\arcsec{0}{00125}$~\cos \alpha ) \sin \delta
+              -$\arcsec{0}{00066}$~\cos \delta $
+
+\subsection{Mean Place Transformations}
+Figure~1 is based upon three varieties of mean \radec\ all of which are
+of practical significance to observing astronomers in the present era:
+\begin{itemize}
+   \item Old style (FK4) with known proper motion in the FK4
+         system, and with parallax and radial velocity either
+         known or assumed zero.
+   \item Old style (FK4) with zero proper motion in FK5,
+         and with parallax and radial velocity assumed zero.
+   \item New style (FK5) with proper motion, parallax and
+         radial velocity either known or assumed zero.
+\end{itemize}
+The figure outlines the steps required to convert positions in
+any of these systems to a J2000 \radec\ for the current
+epoch, as might be required in a telescope-control
+program for example.
+Most of the steps can be carried out by calling a single
+SLALIB routines;  there are other SLALIB routines which
+offer set-piece end-to-end transformation routines for common cases.
+Note, however, that SLALIB does not set out to provide the capability
+for arbitrary transformations of star-catalogue data
+between all possible systems of mean \radec.
+Only in the (common) cases of FK4, equinox and epoch B1950,
+to FK5, equinox and epoch J2000, and {\it vice versa}\/ are
+proper motion, parallax and radial velocity transformed
+along with the star position itself, the
+focus of SLALIB support.
+
+As an example of using SLALIB to transform mean places, here is
+a program which implements the top-left path of Figure~1.
+An FK4 \radec\ of arbitrary equinox and epoch and with
+known proper motion and
+parallax is transformed into an FK5 J2000 \radec\ for the current
+epoch.  As a test star we will use $\alpha=$\hms{16}{09}{55}{13},
+$\delta=$\dms{-75}{59}{27}{2}, equinox 1900, epoch 1963.087,
+$\mu_\alpha=$\tsec{-0}{0312}$/y$, $\mu_\delta=$\arcsec{+0}{103}$/y$,
+parallax = \arcsec{0}{062}, radial velocity = $-34.22$~km/s.  The
+epoch of observation is 1994.35.
+\goodbreak
+\begin{verbatim}
+            IMPLICIT NONE
+            DOUBLE PRECISION AS2R,S2R
+            PARAMETER (AS2R=4.8481368110953599D-6,S2R=7.2722052166430399D-5)
+            INTEGER J,I
+            DOUBLE PRECISION R0,D0,EQ0,EP0,PR,PD,PX,RV,EP1,R1,D1,R2,D2,R3,D3,
+           :                 R4,D4,R5,D5,R6,D6,EP1D,EP1B,W(3),EB(3),PXR,V(3)
+            DOUBLE PRECISION sla_EPB,sla_EPJ2D
+
+      *  RA, Dec etc of example star
+            CALL sla_DTF2R(16,09,55.13D0,R0,J)
+            CALL sla_DAF2R(75,59,27.2D0,D0,J)
+            D0=-D0
+            EQ0=1900D0
+            EP0=1963.087D0
+            PR=-0.0312D0*S2R
+            PD=+0.103D0*AS2R
+            PX=0.062D0
+            RV=-34.22D0
+            EP1=1994.35D0
+
+      *  Epoch of observation as MJD and Besselian epoch
+            EP1D=sla_EPJ2D(EP1)
+            EP1B=sla_EPB(EP1D)
+
+      *  Space motion to the current epoch
+            CALL sla_PM(R0,D0,PR,PD,PX,RV,EP0,EP1B,R1,D1)
+
+      *  Remove E-terms of aberration for the original equinox
+            CALL sla_SUBET(R1,D1,EQ0,R2,D2)
+
+      *  Precess to B1950
+            R3=R2
+            D3=D2
+            CALL sla_PRECES('FK4',EQ0,1950D0,R3,D3)
+
+      *  Add E-terms for the standard equinox B1950
+            CALL sla_ADDET(R3,D3,1950D0,R4,D4)
+
+      *  Transform to J2000, no proper motion
+            CALL sla_FK45Z(R4,D4,EP1B,R5,D5)
+
+      *  Parallax
+            CALL sla_EVP(sla_EPJ2D(EP1),2000D0,W,EB,W,W)
+            PXR=PX*AS2R
+            CALL sla_DCS2C(R5,D5,V)
+            DO I=1,3
+               V(I)=V(I)-PXR*EB(I)
+            END DO
+            CALL sla_DCC2S(V,R6,D6)
+             :
+\end{verbatim}
+\goodbreak
+It is interesting to look at how the \radec\ changes during the
+course of the calculation:
+\begin{tabbing}
+xxxxxxxxxxxxxx \= xxxxxxxxxxxxxxxxxxxxxxxxx \= x \= \kill
+\> {\tt 16 09 55.130 -75 59 27.20} \> \> {\it original equinox and epoch} \\
+\> {\tt 16 09 54.155 -75 59 23.98} \> \> {\it with space motion} \\
+\> {\tt 16 09 54.229 -75 59 24.18} \> \> {\it with old E-terms removed} \\
+\> {\tt 16 16 28.213 -76 06 54.57} \> \> {\it precessed to 1950.0} \\
+\> {\tt 16 16 28.138 -76 06 54.37} \> \> {\it with new E-terms} \\
+\> {\tt 16 23 07.901 -76 13 58.87} \> \> {\it J2000, current epoch} \\
+\> {\tt 16 23 07.907 -76 13 58.92} \> \> {\it including parallax}
+\end{tabbing}
+
+Other remarks about the above (unusually complicated) example:
+\begin{itemize}
+\item If the original equinox and epoch were B1950, as is quite
+      likely, then it would be unnecessary to treat space motions
+      and E-terms explicitly.  Transformation to FK5 J2000 could
+      be accomplished simply by calling
+sla\_FK425, after which
+      a call to
+sla\_PM and the parallax code would complete the
+      work.
+\item The rigorous treatment of the E-terms
+      has only a small effect on the result.  Such refinements
+      are, nevertheless, worthwhile in order to facilitate comparisons and
+      to increase the chances that star positions from different
+      suppliers are compatible.
+\item The FK4 to FK5 transformations,
+sla\_FK425
+      and
+sla\_FK45Z,
+      are not as is sometimes assumed simply 50 years of precession,
+      though this indeed accounts for most of the change.  The
+      transformations also include adjustments
+      to the equinox, a revised precession model, elimination of the
+      E-terms, a change to the proper-motion time unit and so on.
+      The reason there are two routines rather than just one
+      is that the FK4 frame rotates relative to the background, whereas
+      the FK5 frame is a much better approximation to an
+      inertial frame, and zero proper
+      motion in FK4 does not, therefore, mean zero proper motion in FK5.
+      SLALIB also provides two routines,
+sla\_FK524
+      and
+sla\_FK54Z,
+      to perform the inverse transformations.
+\item Some star catalogues (FK4 itself is one) were constructed using slightly
+      different procedures for the polar regions compared with
+      elsewhere.  SLALIB ignores this inhomogeneity and always
+      applies the standard
+      transformations irrespective of location on the celestial sphere.
+\end{itemize}
+
+\subsection {Mean Place to Apparent Place}
+The {\it geocentric apparent place}\/ of a source, or {\it apparent place}\/
+for short,
+is the \radec\ if viewed from the centre of the Earth,
+with respect to the true equator and equinox of date.
+Transformation of an FK5 mean \radec, equinox J2000,
+current epoch, to apparent place involves the following effects:
+\goodbreak
+\begin{itemize}
+   \item Light deflection -- the gravitational lens effect of
+         the sun.
+   \item Annual aberration.
+   \item Precession/nutation.
+\end{itemize}
+The {\it light deflection}\/ is seldom significant.  Its value
+at the limb of the Sun is about
+\arcsec{1}{74};  it falls off rapidly with distance from the
+Sun and has shrunk to about
+\arcsec{0}{02} at an elongation of $20^\circ$.
+
+As already described, the {\it annual aberration}\/
+is a function of the Earth's velocity
+relative to the solar system barycentre (available through the
+SLALIB routine
+sla\_EVP)
+and produces shifts of up to about \arcsec{20}{5}.
+
+The {\it precession/nutation}, from J2000 to the current epoch, is
+expressed by a rotation matrix which is available through the
+SLALIB routine
+sla\_PRENUT.
+
+The whole mean-to-apparent transformation can be done using the SLALIB
+routine
+sla\_MAP.  As a demonstration, here is a program which lists the
+{\it North Polar Distance}\/ ($90^\circ-\delta$) of Polaris for
+the decade of closest approach to the Pole:
+\goodbreak
+\begin{verbatim}
+            IMPLICIT NONE
+            DOUBLE PRECISION PI,PIBY2,D2R,S2R,AS2R
+            PARAMETER (PI=3.141592653589793238462643D0)
+            PARAMETER (D2R=PI/180D0,
+           :           PIBY2=PI/2D0,
+           :           S2R=PI/(12D0*3600D0),
+           :           AS2R=PI/(180D0*3600D0))
+            DOUBLE PRECISION RM,DM,PR,PD,DATE,RA,DA
+            INTEGER J,IDS,IDE,ID,IYMDF(4),I
+            DOUBLE PRECISION sla_EPJ2D
+
+            CALL sla_DTF2R(02,31,49.8131D0,RM,J)
+            CALL sla_DAF2R(89,15,50.661D0,DM,J)
+            PR=+21.7272D0*S2R/100D0
+            PD=-1.571D0*AS2R/100D0
+            WRITE (*,'(1X,'//
+           :            '''Polaris north polar distance (deg) 2096-2105''/)')
+            WRITE (*,'(4X,''Date'',7X''NPD''/)')
+            CALL sla_CLDJ(2096,1,1,DATE,J)
+            IDS=NINT(DATE)
+            CALL sla_CLDJ(2105,12,31,DATE,J)
+            IDE=NINT(DATE)
+            DO ID=IDS,IDE,10
+               DATE=DBLE(ID)
+               CALL sla_DJCAL(0,DATE,IYMDF,J)
+               CALL sla_MAP(RM,DM,PR,PD,0D0,0D0,2000D0,DATE,RA,DA)
+               WRITE (*,'(1X,I4,2I3.2,F9.5)') (IYMDF(I),I=1,3),(PIBY2-DA)/D2R
+            END DO
+
+            END
+\end{verbatim}
+\goodbreak
+For cases where the transformation has to be repeated for different
+times or for more than one star, the straightforward
+sla\_MAP
+approach is apt to be
+wasteful as both the Earth velocity and the
+precession/nutation matrix can be re-calculated relatively
+infrequently without ill effect.  A more efficient method is to
+perform the target-independent calculations only when necessary,
+by calling
+sla\_MAPPA,
+and then to use either
+sla\_MAPQKZ,
+when only the \radec\/ is known, or
+sla\_MAPQK,
+when full catalogue positions, including proper motion, parallax and
+radial velocity, are available.  How frequently to call
+sla\_MAPPA
+depends on the accuracy objectives;  once per
+night will deliver sub-arcsecond accuracy for example.
+
+The routines
+sla\_AMP
+and
+sla\_AMPQK
+allow the reverse transformation, from apparent to mean place.
+
+\subsection{Apparent Place to Observed Place}
+The {\it observed place}\/ of a source is its position as
+seen by a perfect theodolite at the location of the
+observer.  Transformation of an apparent \radec\ to observed 
+place involves the following effects:
+\goodbreak
+\begin{itemize}
+   \item \radec\ to \hadec.
+   \item Diurnal aberration.
+   \item \hadec\ to \azel.
+   \item Refraction.
+\end{itemize}
+The transformation from apparent \radec\ to
+apparent \hadec\ is made by allowing for
+{\it Earth rotation}\/ through the {\it sidereal time}, $\theta$:
+\[ h = \theta - \alpha \]
+For this equation to work, $\alpha$ must be the apparent right
+ascension for the time of observation, and $\theta$ must be
+the {\it local apparent sidereal time}.  The latter is obtained
+as follows:
+\begin{enumerate}
+\item from civil time obtain the coordinated universal time, UTC
+      (more later on this);
+\item add the UT1$-$UTC (typically a few tenths of a second) to
+      give the UT;
+\item from the UT compute the Greenwich mean sidereal time (using
+sla\_GMST);
+\item add the observer's (east) longitude, giving the local mean
+      sidereal time;
+\item add the equation of the equinoxes (using
+sla\_EQEQX).
+\end{enumerate}
+The {\it equation of the equinoxes}\/~($=\Delta\psi\cos\epsilon$ plus
+small terms)
+is the effect of nutation on the sidereal time.
+Its value is typically a second or less.  It is
+interesting to note that if the object of the exercise is to
+transform a mean place all the way into an observed place (very
+often the case),
+then the equation of the
+equinoxes and the longitude component of nutation can both be
+omitted, removing a great deal of computation.  However, SLALIB
+follows the normal convention and  works {\it via}\/ the apparent place.
+
+Note that for very precise work the observer's longitude should
+be corrected for {\it polar motion}.  This can be done with
+sla\_POLMO.
+The corrections are always less than about \arcsec{0}{3}, and
+are futile unless the position of the observer's telescope is known
+to better than a few metres.
+
+Tables of observed and
+predicted UT1$-$UTC corrections and polar motion data
+are published every few weeks by the International Earth Rotation Service.
+
+The transformation from apparent \hadec\ to {\it topocentric}\/
+\hadec\ consists of allowing for
+{\it diurnal aberration}.  This effect, maximum amplitude \arcsec{0}{2},
+was described earlier.  There is no specific SLALIB routine
+for computing the diurnal aberration,
+though the routines
+sla\_AOP {\it etc.}\
+include it, and the required velocity vector can be
+determined by calling
+sla\_GEOC.
+
+The next stage is the major coordinate rotation from local equatorial
+coordinates \hadec\ into horizon coordinates.  The SLALIB routines
+sla\_E2H
+{\it etc.}\ can be used for this.  For high-precision
+applications the mean geodetic latitude should be corrected for polar
+motion.
+
+\subsubsection{Refraction}
+The final correction is for atmospheric refraction.
+This effect, which depends on local meteorological conditions and
+the effective colour of the source/detector combination,
+increases the observed elevation of the source by a
+significant effect even at moderate zenith distances, and near the
+horizon by over \degree{0}{5}.  The amount of refraction can by
+computed by calling the SLALIB routine
+sla\_REFRO;
+however,
+this requires as input the observed zenith distance, which is what
+we are trying to predict.  For high precision it is
+therefore necessary to iterate, using the topocentric
+zenith distance as the initial estimate of the
+observed zenith distance.
+
+The full
+sla\_REFRO refraction calculation is onerous, and for
+zenith distances of less than, say, $75^{\circ}$ the following
+model can be used instead:
+
+\[ \zeta _{vac} \approx \zeta _{obs}
+                     + A \tan \zeta _{obs}
+                     + B \tan ^{3}\zeta _{obs} \]
+where $\zeta _{vac}$ is the topocentric
+zenith distance (i.e.\ {\it in vacuo}),
+$\zeta _{obs}$ is the observed
+zenith distance (i.e.\ affected by refraction), and $A$ and $B$ are
+constants, about \arcseci{60}
+and \arcsec{-0}{06} respectively for a sea-level site.
+The two constants can be calculated for a given set of conditions
+by calling either
+sla\_REFCO or
+sla\_REFCOQ.
+
+sla\_REFCO works by calling
+sla\_REFRO for two zenith distances and fitting $A$ and $B$
+to match.  The calculation is onerous, but delivers accurate
+results whatever the conditions.
+sla\_REFCOQ uses a direct formulation of $A$ and $B$ and
+is much faster;  it is slightly less accurate than
+sla\_REFCO but more than adequate for most practical purposes.
+
+Like the full refraction model, the two-term formulation works in the wrong
+direction for our purposes, predicting
+the {\it in vacuo}\/ (topocentric) zenith distance
+given the refracted (observed) zenith distance,
+rather than {\it vice versa}.  The obvious approach of
+interchanging $\zeta _{vac}$ and $\zeta _{obs}$ and
+reversing the signs, though approximately
+correct, gives avoidable errors which are just significant in
+some applications;  for
+example about \arcsec{0}{2} at $70^\circ$ zenith distance.  A
+much better result can easily be obtained, by using one Newton-Raphson
+iteration as follows:
+
+\[ \zeta _{obs} \approx \zeta _{vac}
+    - \frac{A \tan \zeta _{vac} + B \tan ^{3}\zeta _{vac}}
+    {1 + ( A + 3 B \tan ^{2}\zeta _{vac} ) \sec ^{2}\zeta _{vac}}\]
+
+The effect of refraction can be applied to an unrefracted
+zenith distance by calling
+sla\_REFZ or to an unrefracted
+\xyz\ by calling
+sla\_REFV.
+Over most of the sky these two routines deliver almost identical
+results, but beyond $\zeta=83^\circ$
+sla\_REFV
+becomes unacceptably inaccurate while
+sla\_REFZ
+remains usable.  (However
+sla\_REFV
+is significantly faster, which may be important in some applications.)
+SLALIB also provides a routine for computing the airmass, the function
+sla\_AIRMAS.
+
+The refraction ``constants'' returned by
+sla\_REFCO and
+sla\_REFCOQ
+are slightly affected by colour, especially at the blue end
+of the spectrum.  Where values for more than one
+wavelength are needed, rather than calling
+sla\_REFCO
+several times it is more efficient to call
+sla\_REFCO
+just once, for a selected ``base'' wavelength, and then to call
+sla\_ATMDSP
+once for each wavelength of interest.
+
+All the SLALIB refraction routines work for radio wavelengths as well
+as the optical/IR band.  The radio refraction is very dependent on
+humidity, and an accurate value must be supplied.  There is no
+wavelength dependence, however.  The choice of optical/IR or
+radio is made by specifying a wavelength greater than $100\mu m$
+for the radio case.
+
+\subsubsection{Efficiency considerations}
+The complete apparent place to observed place transformation
+can be carried out by calling
+sla\_AOP.
+For improved efficiency
+in cases of more than one star or a sequence of times, the
+target-independent calculations can be done once by
+calling
+sla\_AOPPA,
+the time can be updated by calling
+sla\_AOPPAT,
+and
+sla\_AOPQK
+can then be used to perform the
+apparent-to-observed transformation.  The reverse transformation
+is available through
+sla\_OAP
+and
+sla\_OAPQK.
+({\it n.b.}\ These routines use accurate but computationally-expensive
+refraction algorithms for zenith distances beyond about $76^\circ$.
+For many purposes, in-line code tailored to the accuracy requirements
+of the application will be preferable, for example ignoring UT1$-$UTC,
+omitting diurnal aberration and using
+sla\_REFZ
+to apply the refraction.)
+
+\subsection{The Hipparcos Catalogue and the ICRS}
+With effect from the beginning of 1998, the IAU adopted a new
+reference system to replace FK5 J2000.  The new system, called the
+International Celestial Reference System (ICRS), differs profoundly
+from all predecessors in that the link with solar-system dynamics
+was broken;  the ICRS axes are defined in terms of the directions
+of a set of extragalactic sources, not in terms of the mean equator and
+equinox at a given reference epoch.  Although the ICRS and FK5 coordinates
+of any given object are almost the same, the orientation of the new frame
+was essentially arbitrary, and the close match to FK5 J2000 was contrived
+purely for reasons of continuity and convenience.
+
+A distinction is made between the reference {\it system}\/ (the ICRS)
+and {\it frame}\/ (ICRF).  The ICRS is the set of prescriptions and
+conventions together with the modelling required to define, at any
+time, a triad of axes.  The ICRF is a practical realization, and
+currently consists of a catalogue of equatorial coordinates for 608
+extragalactic radio sources observed by VLBI.
+
+The best optical realization of the ICRF currently available is the
+Hipparcos catalogue.  The extragalactic sources were not directly
+observable by the Hipparcos satellite and so the link from Hipparcos
+to ICRF was established through a variety of indirect techniques: VLBI and
+conventional interferometry of radio stars, photographic astrometry
+and so on.  The Hipparcos frame is aligned to the ICRF to within about
+0.5~mas and 0.5~mas/year (at epoch 1991.25).
+
+The Hipparcos catalogue includes all of the FK5 stars, which has enabled
+the orientation and spin of the latter to be studied.  At epoch J2000,
+the misalignment of the FK5 frame with respect to Hipparcos
+(and hence ICRS) are about 32~mas and 1~mas/year respectively.
+Consequently, for many practical purposes, including pointing
+telescopes, the IAU 1976-1982 conventions on reference frames and
+Earth orientation remain adequate and there is no need to change to
+Hipparcos coordinates, new precession/nutation models and so on.
+However, for the most exacting astrometric applications, SLALIB
+provides some support for Hipparcos coordinates in the form of
+four new routines:
+sla\_FK52H and
+sla\_H2FK5,
+which transform FK5 positions and proper motions to the Hipparcos frame
+and {\it vice versa,}\/ and
+sla\_FK5HZ and
+sla\_HFK5Z,
+where the transformations are for stars whose Hipparcos proper motion is
+zero. 
+
+Further information on the ICRS can be found in the paper by M.\,Feissel
+and F.\,Mignard, Astron.\,Astrophys. 331, L33-L36 (1988).
+
+\subsection{Timescales}
+SLALIB provides for conversion between several timescales, and involves
+use of one or two others.  The full list is as follows:
+\begin{itemize}
+\item TAI: International Atomic Time
+\item UTC: Coordinated Universal Time
+\item UT: Universal Time
+\item GMST: Greenwich Mean Sidereal Time
+\item LAST: Local Apparent Sidereal Time
+\item TT: Terrestrial Time
+\item TDB: Barycentric Dynamical Time.
+\end{itemize}
+Three obsolete timescales should be mentioned here to avoid confusion.
+\begin{itemize}
+\item GMT: Greenwich Mean Time -- can mean either UTC or UT.
+\item ET: Ephemeris Time -- more or less the same as either TT or TDB.
+\item TDT: Terrestrial Dynamical Time -- former name of TT.
+\end{itemize}
+
+\subsubsection{Atomic Time: TAI}
+{\it International Atomic Time}\/ TAI is a laboratory timescale.  Its
+unit is the SI second, which is defined in terms of a
+defined number
+of wavelengths of the radiation produced by a certain electronic
+transition in the caesium 133 atom.  It
+is realized through a changing
+population of high-precision atomic clocks held
+at standards institutes in various countries.  There is an
+elaborate process of continuous intercomparison, leading to
+a weighted average of all the clocks involved.
+
+Though TAI shares the same second as the more familiar UTC, the
+two timescales are noticeably separated in epoch because of the
+build-up of leap seconds.  At the time of writing, UTC
+lags about half a minute behind TAI.
+
+For any given date, the difference TAI$-$UTC
+can be obtained by calling the SLALIB routine
+sla\_DAT.
+Note, however, that an up-to-date copy of the routine must be used if
+the most recent leap seconds are required.  For applications
+where this is critical, mechanisms independent of SLALIB
+and under local control must
+be set up;  in such cases
+sla\_DAT
+can be useful as an
+independent check, for test dates within the range of the
+available version.  Up-to-date information on TAI$-$UTC is available
+from {\tt ftp://maia.usno.navy.mil/ser7/tai-utc.dat}.
+
+\subsubsection{Universal Time: UTC, UT1}
+{\it Coordinated Universal Time}\/ UTC is the basis of civil timekeeping.
+Most time zones differ from UTC by an integer number
+of hours, though a few ({\it e.g.}\ parts of Canada and Australia) differ
+by $n+0.5$~hours.  The UTC second is the same as the SI second,
+as for TAI.  In the long term, UTC keeps in step with the
+Sun.  It does so even though the Earth's rotation is slightly
+variable (due to large scale movements of water and atmosphere
+among other things) by occasionally introducing a {\it leap
+second}.
+
+{\it Universal Time}\/ UT, or more specifically UT1,
+is in effect the mean solar time.  It is continuous
+({\it i.e.}\ there are no leap seconds) but has a variable
+rate because of the Earth's non-uniform rotation period.  It is
+needed for computing the sidereal time, an essential part of
+pointing a telescope at a celestial source.  To obtain UT1, you
+have to look up the value of UT1$-$UTC for the date concerned
+in tables published by the International Earth Rotation
+Service;  this quantity, kept in the range
+$\pm$\tsec{0}{9} by means of UTC leap
+seconds, is then added to the UTC.  The quantity UT1$-$UTC,
+which typically changes by 1 or 2~ms per day,
+can only be obtained by observation, though seasonal trends
+are known and the IERS listings are able to predict some way into
+the future with adequate accuracy for pointing telescopes.
+
+UTC leap seconds are introduced as necessary,
+usually at the end of December or June.
+On the average the solar day is slightly longer
+than the nominal 86,400~SI~seconds and so leap seconds are always positive;
+however, provision exists for negative leap seconds if needed.
+The form of a leap second can be seen from the
+following description of the end of June~1994:
+
+\hspace{3em}
+\begin{tabular}{clrccc} \\
+     &      &    &   UTC    & UT1$-$UTC  &    UT1       \\ \\
+1994 & June & 30 & 23 59 58 & $-0.218$ & 23 59 57.782 \\
+     &      &    & 23 59 59 & $-0.218$ & 23 59 58.782 \\
+     &      &    & 23 59 60 & $-0.218$ & 23 59 59.782 \\
+     & July &  1 & 00 00 00 & $+0.782$ & 00 00 00.782 \\
+     &      &    & 00 00 01 & $+0.782$ & 00 00 01.782 \\
+\end{tabular}
+
+Note that UTC has to be expressed as hours, minutes and
+seconds (or at least in seconds for a given date) if leap seconds
+are to be taken into account.  It is improper to express a UTC as a
+Julian Date, for example, because there will be an ambiguity
+during a leap second (in the above example,
+1994~June~30 \hms{23}{59}{60}{0} and
+1994~July~1 \hms{00}{00}{00}{0} would {\it both}\/ come out as
+MJD~49534.00000).  Although in the vast majority of
+cases this won't matter, there are potential problems in
+on-line data acquisition systems and in applications involving
+taking the difference between two times.  Note that although the routines
+sla\_DAT
+and
+sla\_DTT
+expect UTC in the form of an MJD, the meaning here is really a
+whole-number {\it date}\/ rather than a time.  Though the routines will accept
+a fractional part and will almost always function correctly, on a day
+which ends with a leap
+second incorrect results would be obtained during the leap second
+itself because by then the MJD would have moved into the next day.
+
+\subsubsection{Sidereal Time: GMST, LAST}
+Sidereal Time is the ``time of day'' relative to the
+stars rather than to the Sun.  After
+one sidereal day the stars come back to the same place in the
+sky, apart from sub-arcsecond precession effects.  Because the Earth
+rotates faster relative to the stars than to the Sun by one day
+per year, the sidereal second is shorter than the solar
+second; the ratio is about 0.9973.
+
+The {\it Greenwich Mean Sidereal Time}\/ GMST is
+linked to UT1 by a numerical formula which
+is implemented in the SLALIB routines
+sla\_GMST
+and
+sla\_GMSTA.
+There are, of course, no leap seconds in GMST, but the second
+changes in length along with the UT1 second, and also varies
+over long periods of time because of slow changes in the Earth's
+orbit.  This makes the timescale unsuitable for everything except
+predicting the apparent directions of celestial sources.
+
+The {\it Local Apparent Sidereal Time}\/ LAST is the apparent right
+ascension of the local meridian, from which the hour angle of any
+star can be determined knowing its $\alpha$.  It can be obtained from the
+GMST by adding the east longitude (corrected for polar motion
+in precise work) and the {\it equation of the equinoxes}.  The
+latter, already described, is an aspect of the nutation effect
+and can be predicted by calling the SLALIB routine
+sla\_EQEQX
+or, neglecting certain very small terms, by calling
+sla\_NUTC
+and using the expression $\Delta\psi\cos\epsilon$.
+
+\subsubsection{Dynamical Time: TT, TDB}
+Dynamical time is the independent variable in the theories
+which describe the motions of bodies in the solar system.  When
+you use published formulae which model the position of the
+Earth in its orbit, for example, or look up
+the Moon's position in a precomputed ephemeris, the date and time
+you use must be in terms of one of the dynamical timescales.  It
+is a common but understandable mistake to use UT directly, in which
+case the results will be about 1~minute out (in the present
+era).
+
+It is not hard to see why such timescales are necessary.
+UTC would clearly be unsuitable as the argument of an
+ephemeris because of leap seconds.
+A solar-system ephemeris based on UT1 or sidereal time would somehow
+have to include the unpredictable variations of the Earth's rotation.
+TAI would work, but eventually
+the ephemeris and the ensemble of atomic clocks would drift apart.
+In effect, the ephemeris {\it is}\/ a clock, with the bodies of
+the solar system the hands.
+
+Only two of the dynamical timescales are of any great importance to
+observational astronomers, TT and TDB.  (The obsolete
+timescale ET, ephemeris time, was more or less the same as TT.)
+
+{\it Terrestrial Time}\/ TT is
+the theoretical timescale of apparent geocentric ephemerides of solar
+system bodies.  It applies, in principle,
+to an Earthbound clock, at sea-level, and for practical purposes
+it is tied to
+Atomic Time TAI through the formula TT~$=$~TAI~$+$~\tsec{32}{184}.
+In practice, therefore, the units of TT are ordinary SI seconds, and
+the offset of \tsec{32}{184} with respect to TAI is fixed.
+The SLALIB routine
+sla\_DTT
+returns TT$-$UTC for a given UTC 
+({\it n.b.}\  sla\_DTT
+calls
+sla\_DAT,
+and the latter must be an up-to-date version if recent leap seconds are
+to be taken into account).
+
+{\it Barycentric Dynamical Time}\/ TDB differs from TT by an amount which
+cycles back and forth by a millisecond or two due to
+relativistic effects.  The variation is
+negligible for most purposes, but unless taken into
+account would swamp
+long-term analysis of pulse arrival times from the
+millisecond pulsars.  It is a consequence of
+the TT clock being on the Earth rather than in empty
+space:  the ellipticity of
+the Earth's orbit means that the TT clock's speed and
+gravitational potential vary slightly
+during the course of the year, and as a consequence
+its rate as seen from an outside observer
+varies due to transverse Doppler effect and gravitational
+redshift.  By definition, TDB and TT differ only
+by periodic terms, and the main effect
+is a sinusoidal variation of amplitude \tsec{0}{0016};  the
+largest planetary terms are nearly two orders of magnitude
+smaller.  The SLALIB routine
+sla\_RCC
+provides a model of
+TDB-TT accurate to a few nanoseconds.
+There are other dynamical timescales, not supported by
+SLALIB routines, which include allowance also for the secular terms.
+These timescales gain on TT and TDB by about \tsec{0}{0013}/day.
+
+For most purposes the more accessible TT is the timescale to use,
+for example when calling
+sla\_PRENUT
+to generate a precession/nutation matrix or when calling
+sla\_EVP
+to predict the
+Earth's position and velocity.  For some purposes TDB is the
+correct timescale, for example when interrogating the JPL planetary
+ephemeris (see {\it Starlink User Note~87}\/), though in most cases
+TT will be near enough and will involve less computation.
+
+Investigations of topocentric solar-system phenomena such as
+occultations and eclipses require solar time as well as dynamical
+time.  TT/TDB/ET is all that is required in order to compute the geocentric
+circumstances, but if horizon coordinates or geocentric parallax
+are to be tackled UT is also needed.  A rough estimate
+of $\Delta {\rm T} = {\rm ET} - {\rm UT}$ is
+available via the routine
+sla\_DT.
+For a given epoch ({\it e.g.}\ 1650) this returns an approximation
+to $\Delta {\rm T}$ in seconds.
+
+\subsection{Calendars}
+The ordinary {\it Gregorian Calendar Date},
+together with a time of day, can be
+used to express an epoch in any desired timescale.  For many purposes,
+however, a continuous count of days is more convenient, and for
+this purpose the system of {\it Julian Day Number}\/ can be used.
+JD zero is located about 7000~years ago, well before the
+historical era, and is formally defined in terms of Greenwich noon;
+Julian Day Number 2449444 began at noon on 1994 April~1.  {\it Julian Date}\/
+is the same system but with a fractional part appended;
+Julian Date 2449443.5 was the midnight on which 1994 April~1
+commenced.  Because of the unwieldy size of Julian Dates
+and the awkwardness of the half-day offset, it is
+accepted practice to remove the leading `24' and the trailing `.5',
+producing what is called the {\it Modified Julian Date}:
+MJD~=~JD$-2400000.5$.  SLALIB routines use MJD, as opposed to
+JD, throughout, largely to avoid loss of precision.
+1994 April~1 commenced at MJD~49443.0.
+
+Despite JD (and hence MJD) being defined in terms of (in effect)
+UT, the system can be used in conjunction with other timescales
+such as TAI, TT and TDB (and even sidereal time through the
+concept of {\it Greenwich Sidereal Date}).  However, it is improper
+to express a UTC as a JD or MJD because of leap seconds.
+
+SLALIB has six routines for converting to and from dates in
+the Gregorian calendar.  The routines
+sla\_CLDJ
+and
+sla\_CALDJ
+both convert a calendar date into an MJD, the former interpreting
+years between 0 and 99 as 1st century and the latter as late 20th or
+early 21st century.  The routines sla\_DJCL
+and
+sla\_DJCAL
+both convert an MJD into calendar year, month, day and fraction of a day;
+the latter performs rounding to a specified precision, important
+to avoid dates like `{\tt 94 04 01.***}' appearing in messages.
+Some of SLALIB's low-precision ephemeris routines
+(sla\_EARTH,
+sla\_MOON
+and
+sla\_ECOR)
+work in terms of year plus day-in-year (where
+day~1~=~January~1st, at least for the modern era).
+This form of date can be generated by
+calling
+sla\_CALYD
+(which defaults years 0-99 into 1950-2049)
+or
+sla\_CLYD
+(which covers the full range from prehistoric times).
+
+\subsection{Geocentric Coordinates}
+The location of the observer on the Earth is significant in a
+number of ways.  The most obvious, of course, is the effect of latitude
+on the observed \azel\ of a star.  Less obvious is the need to
+allow for geocentric parallax when finding the Moon with a
+telescope (and when doing high-precision work involving the
+Sun or planets), and the need to correct observed radial
+velocities and apparent pulsar periods for the effects
+of the Earth's rotation.
+
+The SLALIB routine
+sla\_OBS
+supplies details of groundbased observatories from an internal
+list.  This is useful when writing applications that apply to
+more than one observatory;  the user can enter a brief name,
+or browse through a list, and be spared the trouble of typing
+in the full latitude, longitude {\it etc}.  The following
+Fortran code returns the full name, longitude and latitude
+of a specified observatory:
+\goodbreak
+\begin{verbatim}
+            CHARACTER IDENT*10,NAME*40
+            DOUBLE PRECISION W,P,H
+             :
+            CALL sla_OBS(0,IDENT,NAME,W,P,H)
+            IF (NAME.EQ.'?') ...             (not recognized)
+\end{verbatim}
+\goodbreak
+(Beware of the longitude sign convention, which is west +ve
+for historical reasons.)  The following lists all
+the supported observatories:
+\goodbreak
+\begin{verbatim}
+             :
+            INTEGER N
+             :
+            N=1
+            NAME=' '
+            DO WHILE (NAME.NE.'?')
+               CALL sla_OBS(N,IDENT,NAME,W,P,H)
+               IF (NAME.NE.'?') THEN
+                  WRITE (*,'(1X,I3,4X,A,4X,A)') N,IDENT,NAME
+                  N=N+1
+               END IF
+            END DO
+\end{verbatim}
+\goodbreak
+The routine
+sla\_GEOC
+converts a {\it geodetic latitude}\/
+(one referred to the local horizon) to a geocentric position,
+taking into account the Earth's oblateness and also the height
+above sea level of the observer.  The results are expressed in
+vector form, namely as the distance of the observer from
+the spin axis and equator respectively.  The {\it geocentric
+latitude}\/ can be found be evaluating ATAN2 of the
+two numbers.  A full 3-D vector description of the position
+and velocity of the observer is available through the routine
+sla\_PVOBS.
+For a specified geodetic latitude, height above
+sea level, and local sidereal time,
+sla\_PVOBS
+generates a 6-element vector containing the position and
+velocity with respect to the true equator and equinox of
+date ({\it i.e.}\ compatible with apparent \radec).  For
+some applications it will be necessary to convert to a
+mean \radec\ frame (notably FK5, J2000) by multiplying
+elements 1-3 and 4-6 respectively with the appropriate
+precession matrix.  (In theory an additional correction to the
+velocity vector is needed to allow for differential precession,
+but this correction is always negligible.)
+
+See also the discussion of the routine
+sla\_RVEROT,
+later.
+
+\subsection{Ephemerides}
+SLALIB includes routines for generating positions and
+velocities of Solar-System bodies.  The accuracy objectives are
+modest, and the SLALIB facilities do not attempt
+to compete with precomputed ephemerides such as
+those provided by JPL, or with models containing
+thousands of terms.  It is also worth noting
+that SLALIB's very accurate star coordinate conversion
+routines are not strictly applicable to solar-system cases,
+though they are adequate for most practical purposes.
+
+Earth/Sun ephemerides can be generated using the routine
+sla\_EVP,
+which predicts Earth position and velocity with respect to both the
+solar-system barycentre and the
+Sun.  Maximum velocity error is 0.42~metres per second;  maximum
+heliocentric position error is 1600~km (about \arcseci{2}), with
+barycentric position errors about 4 times worse.
+(The Sun's position as
+seen from the Earth can, of course, be obtained simply by
+reversing the signs of the Cartesian components of the
+Earth\,:\,Sun vector.)
+
+Geocentric Moon ephemerides are available from
+sla\_DMOON,
+which predicts the Moon's position and velocity with respect to
+the Earth's centre.  Direction accuracy is usually better than
+10~km (\arcseci{5}) and distance accuracy a little worse.
+
+Lower-precision but faster predictions for the Sun and Moon
+can be made by calling
+sla\_EARTH
+and
+sla\_MOON.
+Both are single precision and accept dates in the form of
+year, day-in-year and fraction of day
+(starting from a calendar date you need to call
+sla\_CLYD
+or
+sla\_CALYD
+to get the required year and day).
+The
+sla\_EARTH
+routine returns the heliocentric position and velocity
+of the Earth's centre for the mean equator and
+equinox of date.  The accuracy is better than 20,000~km in position
+and 10~metres per second in speed.
+The
+position and velocity of the Moon with respect to the
+Earth's centre for the mean equator and ecliptic of date
+can be obtained by calling
+sla\_MOON.
+The positional accuracy is better than \arcseci{30} in direction
+and 1000~km in distance.
+
+Approximate ephemerides for all the major planets
+can be generated by calling
+sla\_PLANET
+or
+sla\_RDPLAN.  These routines offer arcminute accuracy (much
+better for the inner planets and for Pluto) over a span of several
+millennia (but only $\pm100$ years for Pluto).
+The routine
+sla\_PLANET produces heliocentric position and
+velocity in the form of equatorial \xyzxyzd\ for the
+mean equator and equinox of J2000.  The vectors
+produced by
+sla\_PLANET
+can be used in a variety of ways according to the
+requirements of the application concerned.  The routine
+sla\_RDPLAN
+uses
+sla\_PLANET
+and
+sla\_DMOON
+to deal with the common case of predicting
+a planet's apparent \radec\ and angular size as seen by a
+terrestrial observer.
+
+Note that in predicting the position in the sky of a solar-system body
+it is necessary to allow for geocentric parallax.  This correction
+is {\it essential}\/ in the case of the Moon, where the observer's
+position on the Earth can affect the Moon's \radec\ by up to
+$1^\circ$.  The calculation can most conveniently be done by calling
+sla\_PVOBS and subtracting the resulting 6-vector from the
+one produced by
+sla\_DMOON, as is demonstrated by the following example:
+\goodbreak
+\begin{verbatim}
+      *  Demonstrate the size of the geocentric parallax correction
+      *  in the case of the Moon.  The test example is for the AAT,
+      *  before midnight, in summer, near first quarter.
+
+            IMPLICIT NONE
+            CHARACTER NAME*40,SH,SD
+            INTEGER J,I,IHMSF(4),IDMSF(4)
+            DOUBLE PRECISION SLONGW,SLAT,H,DJUTC,FDUTC,DJUT1,DJTT,STL,
+           :                 RMATN(3,3),PMM(6),PMT(6),RM,DM,PVO(6),TL
+            DOUBLE PRECISION sla_DTT,sla_GMST,sla_EQEQX,sla_DRANRM
+
+      *  Get AAT longitude and latitude in radians and height in metres
+            CALL sla_OBS(0,'AAT',NAME,SLONGW,SLAT,H)
+
+      *  UTC (1992 January 13, 11 13 59) to MJD
+            CALL sla_CLDJ(1992,1,13,DJUTC,J)
+            CALL sla_DTF2D(11,13,59.0D0,FDUTC,J)
+            DJUTC=DJUTC+FDUTC
+
+      *  UT1 (UT1-UTC value of -0.152 sec is from IERS Bulletin B)
+            DJUT1=DJUTC+(-0.152D0)/86400D0
+
+      *  TT
+            DJTT=DJUTC+sla_DTT(DJUTC)/86400D0
+
+      *  Local apparent sidereal time
+            STL=sla_GMST(DJUT1)-SLONGW+sla_EQEQX(DJTT)
+
+      *  Geocentric position/velocity of Moon (mean of date)
+            CALL sla_DMOON(DJTT,PMM)
+
+      *  Nutation to true equinox of date
+            CALL sla_NUT(DJTT,RMATN)
+            CALL sla_DMXV(RMATN,PMM,PMT)
+            CALL sla_DMXV(RMATN,PMM(4),PMT(4))
+
+      *  Report geocentric HA,Dec
+            CALL sla_DCC2S(PMT,RM,DM)
+            CALL sla_DR2TF(2,sla_DRANRM(STL-RM),SH,IHMSF)
+            CALL sla_DR2AF(1,DM,SD,IDMSF)
+            WRITE (*,'(1X,'' geocentric:'',2X,A,I2.2,2I3.2,''.'',I2.2,'//
+           :                              '1X,A,I2.2,2I3.2,''.'',I1)')
+           :                                                SH,IHMSF,SD,IDMSF
+
+      *  Geocentric position of observer (true equator and equinox of date)
+            CALL sla_PVOBS(SLAT,H,STL,PVO)
+
+      *  Place origin at observer
+            DO I=1,6
+               PMT(I)=PMT(I)-PVO(I)
+            END DO
+
+      *  Allow for planetary aberration
+            TL=499.004782D0*SQRT(PMT(1)**2+PMT(2)**2+PMT(3)**2)
+            DO I=1,3
+               PMT(I)=PMT(I)-TL*PMT(I+3)
+            END DO
+
+      *  Report topocentric HA,Dec
+            CALL sla_DCC2S(PMT,RM,DM)
+            CALL sla_DR2TF(2,sla_DRANRM(STL-RM),SH,IHMSF)
+            CALL sla_DR2AF(1,DM,SD,IDMSF)
+            WRITE (*,'(1X,''topocentric:'',2X,A,I2.2,2I3.2,''.'',I2.2,'//
+           :                              '1X,A,I2.2,2I3.2,''.'',I1)')
+           :                                                SH,IHMSF,SD,IDMSF
+            END
+\end{verbatim}
+\goodbreak
+The output produced is as follows:
+\goodbreak
+\begin{verbatim}
+       geocentric:  +03 06 55.59 +15 03 39.0
+      topocentric:  +03 09 23.79 +15 40 51.5
+\end{verbatim}
+\goodbreak
+(An easier but
+less instructive method of estimating the topocentric apparent place of the
+Moon is to call the routine
+sla\_RDPLAN.)
+
+As an example of using
+sla\_PLANET,
+the following program estimates the geocentric separation
+between Venus and Jupiter during a close conjunction
+in 2\,BC, which is a star-of-Bethlehem candidate:
+\goodbreak
+\begin{verbatim}
+      *  Compute time and minimum geocentric apparent separation
+      *  between Venus and Jupiter during the close conjunction of 2 BC.
+
+            IMPLICIT NONE
+
+            DOUBLE PRECISION SEPMIN,DJD0,FD,DJD,DJDM,DF,PV(6),RMATP(3,3),
+           :                 PVM(6),PVE(6),TL,RV,DV,RJ,DJ,SEP
+            INTEGER IHOUR,IMIN,J,I,IHMIN,IMMIN
+            DOUBLE PRECISION sla_EPJ,sla_DSEP
+
+
+      *  Search for closest approach on the given day
+            DJD0=1720859.5D0
+            SEPMIN=1D10
+            DO IHOUR=20,22
+               DO IMIN=0,59
+                  CALL sla_DTF2D(IHOUR,IMIN,0D0,FD,J)
+
+      *        Julian date and MJD
+                  DJD=DJD0+FD
+                  DJDM=DJD-2400000.5D0
+
+      *        Earth to Moon (mean of date)
+                  CALL sla_DMOON(DJDM,PV)
+
+      *        Precess Moon position to J2000
+                  CALL sla_PRECL(sla_EPJ(DJDM),2000D0,RMATP)
+                  CALL sla_DMXV(RMATP,PV,PVM)
+
+      *        Sun to Earth-Moon Barycentre (mean J2000)
+                  CALL sla_PLANET(DJDM,3,PVE,J)
+
+      *        Correct from EMB to Earth
+                  DO I=1,3
+                     PV(I)=PVE(I)-0.012150581D0*PVM(I)
+                  END DO
+
+      *        Sun to Venus
+                  CALL sla_PLANET(DJDM,2,PV,J)
+
+      *        Earth to Venus
+                  DO I=1,6
+                     PV(I)=PV(I)-PVE(I)
+                  END DO
+
+      *        Light time to Venus (sec)
+                  TL=499.004782D0*SQRT((PV(1)-PVE(1))**2+
+           :                           (PV(2)-PVE(2))**2+
+           :                           (PV(3)-PVE(3))**2)
+
+      *        Extrapolate backwards in time by that much
+                  DO I=1,3
+                     PV(I)=PV(I)-TL*PV(I+3)
+                  END DO
+
+      *       To RA,Dec
+                  CALL sla_DCC2S(PV,RV,DV)
+
+      *        Same for Jupiter
+                  CALL sla_PLANET(DJDM,5,PV,J)
+                  DO I=1,6
+                     PV(I)=PV(I)-PVE(I)
+                  END DO
+                  TL=499.004782D0*SQRT((PV(1)-PVE(1))**2+
+           :                           (PV(2)-PVE(2))**2+
+           :                           (PV(3)-PVE(3))**2)
+                  DO I=1,3
+                     PV(I)=PV(I)-TL*PV(I+3)
+                  END DO
+                  CALL sla_DCC2S(PV,RJ,DJ)
+
+      *        Separation (arcsec)
+                  SEP=sla_DSEP(RV,DV,RJ,DJ)
+
+      *        Keep if smallest so far
+                  IF (SEP.LT.SEPMIN) THEN
+                     IHMIN=IHOUR
+                     IMMIN=IMIN
+                     SEPMIN=SEP
+                  END IF
+               END DO
+            END DO
+
+      *  Report
+            WRITE (*,'(1X,I2.2,'':'',I2.2,F6.1)') IHMIN,IMMIN,
+           :                                      206264.8062D0*SEPMIN
+
+            END
+\end{verbatim}
+\goodbreak
+The output produced (the Ephemeris Time on the day in question, and
+the closest approach in arcseconds) is as follows:
+\goodbreak
+\begin{verbatim}
+      21:19  33.7
+\end{verbatim}
+\goodbreak
+For comparison, accurate predictions based on the JPL DE\,102 ephemeris
+give a separation about \arcseci{8} less than
+the above estimate, occurring about half an hour earlier
+(see {\it Sky and Telescope,}\/ April~1987, p\,357).
+
+The following program demonstrates
+sla\_RDPLAN.
+\begin{verbatim}
+      *  For a given date, time and geographical location, output
+      *  a table of planetary positions and diameters.
+
+            IMPLICIT NONE
+            CHARACTER PNAMES(0:9)*7,B*80,S
+            INTEGER I,NP,IY,J,IM,ID,IHMSF(4),IDMSF(4)
+            DOUBLE PRECISION R2AS,FD,DJM,ELONG,PHI,RA,DEC,DIAM
+            PARAMETER (R2AS=206264.80625D0)
+            DATA PNAMES / 'Sun','Mercury','Venus','Moon','Mars','Jupiter',
+           :              'Saturn','Uranus','Neptune', 'Pluto' /
+
+
+      *  Loop until 'end' typed
+            B=' '
+            DO WHILE (B.NE.'END'.AND.B.NE.'end')
+
+      *     Get date, time and observer's location
+               PRINT *,'Date? (Y,M,D, Gregorian)'
+               READ (*,'(A)') B
+               IF (B.NE.'END'.AND.B.NE.'end') THEN
+                  I=1
+                  CALL sla_INTIN(B,I,IY,J)
+                  CALL sla_INTIN(B,I,IM,J)
+                  CALL sla_INTIN(B,I,ID,J)
+                  PRINT *,'Time? (H,M,S, dynamical)'
+                  READ (*,'(A)') B
+                  I=1
+                  CALL sla_DAFIN(B,I,FD,J)
+                  FD=FD*2.3873241463784300365D0
+                  CALL sla_CLDJ(IY,IM,ID,DJM,J)
+                  DJM=DJM+FD
+                  PRINT *,'Longitude? (D,M,S, east +ve)'
+                  READ (*,'(A)') B
+                  I=1
+                  CALL sla_DAFIN(B,I,ELONG,J)
+                  PRINT *,'Latitude? (D,M,S, (geodetic)'
+                  READ (*,'(A)') B
+                  I=1
+                  CALL sla_DAFIN(B,I,PHI,J)
+
+      *        Loop planet by planet
+                  DO NP=0,8
+
+      *           Get RA,Dec and diameter
+                     CALL sla_RDPLAN(DJM,NP,ELONG,PHI,RA,DEC,DIAM)
+
+      *           One line of report
+                     CALL sla_DR2TF(2,RA,S,IHMSF)
+                     CALL sla_DR2AF(1,DEC,S,IDMSF)
+                     WRITE (*,
+           : '(1X,A,2X,3I3.2,''.'',I2.2,2X,A,I2.2,2I3.2,''.'',I1,F8.1)')
+           :                          PNAMES(NP),IHMSF,S,IDMSF,R2AS*DIAM
+
+      *           Next planet
+                  END DO
+                  PRINT *,' '
+               END IF
+
+      *     Next case
+            END DO
+
+            END
+\end{verbatim}
+Entering the following data (for 1927~June~29 at $5^{\rm h}\,25^{\rm m}$~ET
+and the position of Preston, UK.):
+\begin{verbatim}
+      1927 6 29
+      5 25
+      -2 42
+      53 46
+\end{verbatim}
+produces the following report:
+\begin{verbatim}
+      Sun       06 28 14.03  +23 17 17.5  1887.8
+      Mercury   08 08 58.62  +19 20 57.3     9.3
+      Venus     09 38 53.64  +15 35 32.9    22.8
+      Moon      06 28 18.30  +23 18 37.3  1903.9
+      Mars      09 06 49.34  +17 52 26.7     4.0
+      Jupiter   00 11 12.06  -00 10 57.5    41.1
+      Saturn    16 01 43.34  -18 36 55.9    18.2
+      Uranus    00 13 33.53  +00 39 36.0     3.5
+      Neptune   09 49 35.75  +13 38 40.8     2.2
+      Pluto     07 05 29.50  +21 25 04.2      .1
+\end{verbatim}
+Inspection of the Sun and Moon data reveals that
+a total solar eclipse is in progress.
+
+SLALIB also provides for the case where orbital elements (with respect
+to the J2000 equinox and ecliptic)
+are available.  This allows predictions to be made for minor-planets and
+(if you ignore non-gravitational effects)
+comets.  Furthermore, if major-planet elements for an epoch close to the date
+in question are available, more accurate predictions can be made than
+are offered by
+sla\_RDPLAN and
+sla\_PLANET.
+
+The SLALIB planetary-prediction
+routines that work with orbital elements are
+sla\_PLANTE (the orbital-elements equivalent of
+sla\_RDPLAN), which predicts the topocentric \radec, and
+sla\_PLANEL (the orbital-elements equivalent of
+sla\_PLANET), which predicts the heliocentric \xyzxyzd\ with respect to the
+J2000 equinox and equator.  In addition, the routine
+sla\_PV2EL does the inverse of
+sla\_PLANEL, transforming \xyzxyzd\ into {\it osculating elements.}
+
+Osculating elements describe the unperturbed 2-body orbit.  This is
+a good approximation to the actual orbit for a few weeks either
+side of the specified epoch, outside which perturbations due to
+the other bodies of the Solar System lead to
+increasing errors.  Given a minor planet's osculating elements for
+a particular date, predictions for a date even just
+100 days earlier or later
+are likely to be in error by several arcseconds.
+These errors can
+be reduced if new elements are generated which take account of
+the perturbations of the major planets, and this is what the routine
+sla\_PERTEL does.  Once
+sla\_PERTEL has been called, to provide osculating elements
+close to the required date, the elements can be passed to
+sla\_PLANEL or
+sla\_PLANTE in the normal way.  Predictions of arcsecond accuracy
+over a span of a decade or more are available using this
+technique.
+
+Three different combinations of orbital elements are
+provided for, matching the usual conventions
+for major planets, minor planets and
+comets respectively.  The choice is made through the
+argument {\tt JFORM}:\\
+
+\hspace{4em}
+\begin{tabular}{|c|c|c|} \hline
+{\tt JFORM=1} & {\tt JFORM=2} & {\tt JFORM=3} \\
+\hline \hline
+$t_0$ & $t_0$ & $T$ \\
+\hline
+$i$ & $i$ & $i$ \\
+\hline
+$\Omega$ & $\Omega$ & $\Omega$ \\
+\hline
+$\varpi$ & $\omega$ & $\omega$ \\
+\hline
+$a$ & $a$ & $q$ \\
+\hline
+$e$ & $e$ & $e$ \\
+\hline
+$L$ & $M$ & \\
+\hline
+$n$ & & \\
+\hline
+\end{tabular}\\[5ex]
+The symbols have the following meanings:
+\begin{tabbing}
+xxxxxxx \= xxxx \= \kill
+\> $t_0$ \> epoch at which the elements were correct \\
+\> $T$ \> epoch of perihelion passage \\
+\> $i$ \> inclination of the orbit \\
+\> $\Omega$ \> longitude of the ascending node \\
+\> $\varpi$ \> longitude of perihelion ($\varpi = \Omega + \omega$) \\
+\> $\omega$ \> argument of perihelion \\
+\> $a$ \> semi-major axis of the orbital ellipse \\
+\> $q$ \> perihelion distance \\
+\> $e$ \> orbital eccentricity \\
+\> $L$ \> mean longitude ($L = \varpi + M$) \\
+\> $M$ \> mean anomaly \\
+\> $n$ \> mean motion \\
+\end{tabbing}
+
+The mean motion, $n$, tells sla\_PLANEL the mass of the planet.
+If it is not available, it should be claculated
+from $n^2 a^3 = k^2 (1+m)$, where $k = 0.01720209895$ and
+m is the mass of the planet ($M_\odot = 1$); $a$ is in AU.
+
+Conventional elements are not the only way of specifying an orbit.
+The \xyzxyzd\ state vector is an equally valid specification,
+and the so-called {\it method of universal variables}\/ allows
+orbital calculations to be made directly, bypassing angular
+quantities and avoiding Kepler's Equation.  The universal-variables
+approach has various advantages, including better handling of
+near-parabolic cases and greater efficiency.
+SLALIB uses universal variables for its internal
+calculations and also offers a number of routines which
+applications can call.
+
+The universal elements are the \xyzxyzd\ and its epoch, plus the mass
+of the body.  The SLALIB routines supplement these elements with
+certain redundant values in order to
+avoid unnecessary recomputation when the elements are next used.
+
+The routines
+sla\_EL2UE and
+sla\_UE2EL transform conventional elements into the
+universal form and {\it vice versa.}
+The routine
+sla\_PV2UE takes an \xyzxyzd\ and forms the set of universal
+elements;
+sla\_UE2PV takes a set of universal elements and predicts the \xyzxyzd\
+for a specified epoch.
+The routine
+sla\_PERTUE provides updated universal elements,
+taking into account perturbations from the major planets.
+
+\subsection{Radial Velocity and Light-Time Corrections}
+When publishing high-resolution spectral observations
+it is necessary to refer them to a specified standard of rest.
+This involves knowing the component in the direction of the
+source of the velocity of the observer.  SLALIB provides a number
+of routines for this purpose, allowing observations to be
+referred to the Earth's centre, the Sun, a Local Standard of Rest
+(either dynamical or kinematical), the centre of the Galaxy, and
+the mean motion of the Local Group.
+
+The routine
+sla\_RVEROT
+corrects for the diurnal rotation of
+the observer around the Earth's axis.  This is always less than 0.5~km/s.
+
+No specific routine is provided to correct a radial velocity
+from geocentric to heliocentric, but this can easily be done by calling
+sla\_EVP
+as follows (array declarations {\it etc}.\ omitted):
+\goodbreak
+\begin{verbatim}
+             :
+      *  Star vector, J2000
+            CALL sla_DCS2C(RM,DM,V)
+
+      *  Earth/Sun velocity and position, J2000
+            CALL sla_EVP(TDB,2000D0,DVB,DPB,DVH,DPH)
+
+      *  Radial velocity correction due to Earth orbit (km/s)
+            VCORB = -sla_DVDV(V,DVH)*149.597870D6
+             :
+\end{verbatim}
+\goodbreak
+The maximum value of this correction is the Earth's orbital speed
+of about 30~km/s.  A related routine,
+sla\_ECOR,
+computes the light-time correction with respect to the Sun.  It
+would be used when reducing observations of a rapid variable-star
+for instance.
+Note, however, that the accuracy objectives for pulsar work are
+beyond the scope of these SLALIB routines, and even the superior
+sla\_EVP
+routine is unsuitable for arrival-time calculations of better
+than 25~millisecond accuracy.
+
+To remove the intrinsic $\sim20$~km/s motion of the Sun relative
+to other stars in the solar neighbourhood,
+a velocity correction to a
+{\it local standard of rest}\/ (LSR) is required.  There are
+opportunities for mistakes here.  There are two sorts of LSR,
+{\it dynamical}\/ and {\it kinematical}, and
+multiple definitions exist for the latter.  The
+dynamical LSR is a point near the Sun which is in a circular
+orbit around the Galactic centre;  the Sun has a ``peculiar''
+motion relative to the dynamical LSR.  A kinematical LSR is
+the mean standard of rest of specified star catalogues or stellar
+populations, and its precise definition depends on which
+catalogues or populations were used and how the analysis was
+carried out.  The Sun's motion with respect to a kinematical
+LSR is called the ``standard'' solar motion.  Radial
+velocity corrections to the dynamical LSR are produced by the routine
+sla\_RVLSRD
+and to the adopted kinematical LSR by
+sla\_RVLSRK.
+See the individual specifications for these routines for the
+precise definition of the LSR in each case.
+
+For extragalactic sources, the centre of the Galaxy can be used as
+a standard of rest.  The radial velocity correction from the
+dynamical LSR to the Galactic centre can be obtained by calling
+sla\_RVGALC.
+Its maximum value is 220~km/s.
+
+For very distant sources it is appropriate to work relative
+to the mean motion of the Local Group.  The routine for
+computing the radial velocity correction in this case is
+sla\_RVLG.
+Note that in this case the correction is with respect to the
+dynamical LSR, not the Galactic centre as might be expected.
+This conforms to the IAU definition, and confers immunity from
+revisions of the Galactic rotation speed.
+
+\subsection{Focal-Plane Astrometry}
+The relationship between the position of a star image in
+the focal plane of a telescope and the star's celestial
+coordinates is usually described in terms of the {\it tangent plane}\/
+or {\it gnomonic}\/ projection.  This is the projection produced
+by a pin-hole camera and is a good approximation to the projection
+geometry of a traditional large {\it f}\/-ratio astrographic refractor.
+SLALIB includes a group of routines which transform
+star positions between their observed places on the celestial
+sphere and their \xy\ coordinates in the tangent plane.  The
+spherical coordinate system does not have to be \radec\ but
+usually is.  The so-called {\it standard coordinates}\/ of a star
+are the tangent plane \xy, in radians, with respect to an origin
+at the tangent point, with the $y$-axis pointing north and
+the $x$-axis pointing east (in the direction of increasing $\alpha$).
+The factor relating the standard coordinates to
+the actual \xy\ coordinates in, say, millimetres is simply
+the focal length of the telescope.
+
+Given the \radec\ of the {\it plate centre}\/ (the tangent point)
+and the \radec\ of a star within the field, the standard
+coordinates can be determined by calling
+sla\_S2TP
+(single precision) or
+sla\_DS2TP
+(double precision).  The reverse transformation, where the
+\xy\ is known and we wish to find the \radec, is carried out by calling
+sla\_TP2S
+or
+sla\_DTP2S.
+Occasionally we know the both the \xy\ and the \radec\ of a 
+star and need to deduce the \radec\ of the tangent point;  
+this can be done by calling
+sla\_TPS2C
+or
+sla\_DTPS2C.
+(All of these transformations apply not just to \radec\ but to
+other spherical coordinate systems, of course.)
+Equivalent (and faster)
+routines are provided which work directly in \xyz\ instead of
+spherical coordinates:
+sla\_V2TP and
+sla\_DV2TP,
+sla\_TP2V and
+sla\_DTP2V,
+sla\_TPV2C and
+sla\_DTPV2C.
+
+Even at the best of times, the tangent plane projection is merely an
+approximation.  Some telescopes and cameras exhibit considerable pincushion
+or barrel distortion and some have a curved focal surface.
+For example, neither Schmidt cameras nor (especially)
+large reflecting telescopes with wide-field corrector lenses
+are adequately modelled by tangent-plane geometry.  In such
+cases, however, it is still possible to do most of the work
+using the (mathematically convenient) tangent-plane
+projection by inserting an extra step which applies or
+removes the distortion peculiar to the system concerned.
+A simple $r_1=r_0(1+Kr_0^2)$ law works well in the
+majority of cases; $r_0$ is the radial distance in the
+tangent plane, $r_1$ is the radial distance after adding
+the distortion, and $K$ is a constant which depends on the
+telescope ($\theta$ is unaffected).  The routine
+sla\_PCD
+applies the distortion to an \xy\ and
+sla\_UNPCD
+removes it.  For \xy\ in radians, $K$ values range from $-1/3$ for the
+tiny amount of barrel distortion in Schmidt geometry to several
+hundred for the serious pincushion distortion
+produced by wide-field correctors in big reflecting telescopes
+(the AAT prime focus triplet corrector is about $K=+178.6$).
+
+SLALIB includes a group of routines which can be put together
+to build a simple plate-reduction program.  The heart of the group is
+sla\_FITXY,
+which fits a linear model to relate two sets of \xy\ coordinates,
+in the case of a plate reduction the measured positions of the
+images of a set of
+reference stars and the standard
+coordinates derived from their catalogue positions.  The
+model is of the form:
+\[x_{p} = a + bx_{m} + cy_{m}\]
+\[y_{p} = d + ex_{m} + fy_{m}\]
+
+where the {\it p}\/ subscript indicates ``predicted'' coordinates
+(the model's approximation to the ideal ``expected'' coordinates) and the
+{\it m}\/ subscript indicates ``measured coordinates''.  The
+six coefficients {\it a--f}\/ can optionally be
+constrained to represent a ``solid body rotation'' free of
+any squash or shear distortions.  Without this constraint
+the model can, to some extent, accommodate effects like refraction,
+allowing mean places to be used directly and
+avoiding the extra complications of a
+full mean-apparent-observed transformation for each star.
+Having obtained the linear model,
+sla\_PXY
+can be used to process the set of measured and expected
+coordinates, giving the predicted coordinates and determining
+the RMS residuals in {\it x}\/ and {\it y}.
+The routine
+sla\_XY2XY
+transforms one \xy\ into another using the linear model.  A model
+can be inverted by calling
+sla\_INVF,
+and decomposed into zero points, scales, $x/y$ nonperpendicularity
+and orientation by calling
+sla\_DCMPF.
+
+\subsection{Numerical Methods}
+SLALIB contains a small number of simple, general-purpose
+numerical-methods routines.  They have no specific
+connection with positional astronomy but have proved useful in
+applications to do with simulation and fitting.
+
+At the heart of many simulation programs is the generation of
+pseudo-random numbers, evenly distributed in a given range:
+sla\_RANDOM
+does this.  Pseudo-random normal deviates, or ``Gaussian
+residuals'', are often required to simulate noise and
+can be generated by means of the function
+sla\_GRESID.
+Neither routine will pass super-sophisticated
+statistical tests, but they work adequately for most
+practical purposes and avoid the need to call non-standard
+library routines peculiar to one sort of computer.
+
+Applications which perform a least-squares fit using a traditional
+normal-equations methods can accomplish the required matrix-inversion
+by calling either
+sla\_SMAT
+(single precision) or
+sla\_DMAT
+(double).  A generally better way to perform such fits is
+to use singular value decomposition.  SLALIB provides a routine
+to do the decomposition itself,
+sla\_SVD,
+and two routines to use the results:
+sla\_SVDSOL
+generates the solution, and
+sla\_SVDCOV
+produces the covariance matrix.
+A simple demonstration of the use of the SLALIB SVD
+routines is given below.  It generates 500 simulated data
+points and fits them to a model which has 4 unknown coefficients.
+(The arrays in the example are sized to accept up to 1000
+points and 20 unknowns.)  The model is:
+\[ y = C_{1} +C_{2}x +C_{3}sin{x} +C_{4}cos{x} \]
+The test values for the four coefficients are
+$C_1\!=\!+50.0$,
+$C_2\!=\!-2.0$,
+$C_3\!=\!-10.0$ and
+$C_4\!=\!+25.0$.
+Gaussian noise, $\sigma=5.0$, is added to each ``observation''.
+\goodbreak
+\begin{verbatim}
+            IMPLICIT NONE
+
+      *  Sizes of arrays, physical and logical
+            INTEGER MP,NP,NC,M,N
+            PARAMETER (MP=1000,NP=10,NC=20,M=500,N=4)
+
+      *  The unknowns we are going to solve for
+            DOUBLE PRECISION C1,C2,C3,C4
+            PARAMETER (C1=50D0,C2=-2D0,C3=-10D0,C4=25D0)
+
+      *  Arrays
+            DOUBLE PRECISION A(MP,NP),W(NP),V(NP,NP),
+           :                 WORK(NP),B(MP),X(NP),CVM(NC,NC)
+
+            DOUBLE PRECISION VAL,BF1,BF2,BF3,BF4,SD2,D,VAR
+            REAL sla_GRESID
+            INTEGER I,J
+
+      *  Fill the design matrix
+            DO I=1,M
+
+      *     Dummy independent variable
+               VAL=DBLE(I)/10D0
+
+      *     The basis functions
+               BF1=1D0
+               BF2=VAL
+               BF3=SIN(VAL)
+               BF4=COS(VAL)
+
+      *     The observed value, including deliberate Gaussian noise
+               B(I)=C1*BF1+C2*BF2+C3*BF3+C4*BF4+DBLE(sla_GRESID(5.0))
+
+      *     Fill one row of the design matrix
+               A(I,1)=BF1
+               A(I,2)=BF2
+               A(I,3)=BF3
+               A(I,4)=BF4
+            END DO
+
+      *  Factorize the design matrix, solve and generate covariance matrix
+            CALL sla_SVD(M,N,MP,NP,A,W,V,WORK,J)
+            CALL sla_SVDSOL(M,N,MP,NP,B,A,W,V,WORK,X)
+            CALL sla_SVDCOV(N,NP,NC,W,V,WORK,CVM)
+
+      *  Compute the variance
+            SD2=0D0
+            DO I=1,M
+               VAL=DBLE(I)/10D0
+               BF1=1D0
+               BF2=VAL
+               BF3=SIN(VAL)
+               BF4=COS(VAL)
+               D=B(I)-(X(1)*BF1+X(2)*BF2+X(3)*BF3+X(4)*BF4)
+               SD2=SD2+D*D
+            END DO
+            VAR=SD2/DBLE(M)
+
+      *  Report the RMS and the solution
+            WRITE (*,'(1X,''RMS ='',F5.2/)') SQRT(VAR)
+            DO I=1,N
+               WRITE (*,'(1X,''C'',I1,'' ='',F7.3,'' +/-'',F6.3)')
+           :                                         I,X(I),SQRT(VAR*CVM(I,I))
+            END DO
+            END
+\end{verbatim}
+\goodbreak
+The program produces the following output:
+\goodbreak
+\begin{verbatim}
+            RMS = 4.88
+
+            C1 = 50.192 +/- 0.439
+            C2 = -2.002 +/- 0.015
+            C3 = -9.771 +/- 0.310
+            C4 = 25.275 +/- 0.310
+\end{verbatim}
+\goodbreak
+In this above example, essentially
+identical results would be obtained if the more
+commonplace normal-equations method had been used, and the large
+$1000\times20$ array would have been avoided.  However, the SVD method
+comes into its own when the opportunity is taken to edit the W-matrix
+(the so-called ``singular values'') in order to control
+possible ill-conditioning.  The procedure involves replacing with
+zeroes any W-elements smaller than a nominated value, for example
+0.001 times the largest W-element.  Small W-elements indicate
+ill-conditioning, which in the case of the normal-equations
+method would produce spurious large coefficient values and
+possible arithmetic overflows.  Using SVD, the effect on the solution
+of setting suspiciously small W-elements to zero is to restrain
+the offending coefficients from moving very far.  The
+fact that action was taken can be reported to show the program user that
+something is amiss.  Furthermore, if element W(J) was set to zero,
+the row numbers of the two biggest elements in the Jth column of the
+V-matrix identify the pair of solution coefficients that are
+dependent.
+
+A more detailed description of SVD and its use in least-squares
+problems would be out of place here, and the reader is urged
+to refer to the relevant sections of the book {\it Numerical Recipes}
+(Press {\it et al.}, Cambridge University Press, 1987).
+
+The routines
+sla\_COMBN
+and
+sla\_PERMUT
+are useful for problems which involve combinations (different subsets)
+and permutations (different orders).
+Both return the next in a sequence of results, cycling through all the
+possible results as the routine is called repeatedly.
+
+\pagebreak
+
+\section{SUMMARY OF CALLS}
+The basic trigonometrical and numerical facilities are supplied in both single
+and double precision versions.
+Most of the more esoteric position and time routines use double precision
+arguments only, even in cases where single precision would normally be adequate
+in practice.
+Certain routines with modest accuracy objectives are supplied in
+single precision versions only.
+In the calling sequences which follow, no attempt has been made
+to distinguish between single and double precision argument names,
+and frequently the same name is used on different occasions to
+mean different things.
+However, none of the routines uses a mixture of single and
+double precision arguments;  each routine is either wholly
+single precision or wholly double precision.
+
+In the classified list, below,
+{\it subroutine}\/ subprograms are those whose names and argument lists
+are preceded by `CALL', whereas {\it function}\/ subprograms are
+those beginning `R=' (when the result is REAL) or `D=' (when
+the result is DOUBLE~PRECISION).
+
+The list is, of course, merely for quick reference;  inexperienced
+users {\bf must} refer to the detailed specifications given later.
+In particular, {\bf don't guess} whether arguments are single or
+double precision; the result could be a program that happens to
+works on one sort of machine but not on another.
+
+\callhead{String Decoding}
+\begin{callset}
+\subp{CALL sla\_INTIN (STRING, NSTRT, IRESLT, JFLAG)}
+   Convert free-format string into integer
+\subq{CALL sla\_FLOTIN (STRING, NSTRT, RESLT, JFLAG)}
+     {CALL sla\_DFLTIN (STRING, NSTRT, DRESLT, JFLAG)}
+   Convert free-format string into floating-point number
+\subq{CALL sla\_AFIN (STRING, NSTRT, RESLT, JFLAG)}
+     {CALL sla\_DAFIN (STRING, NSTRT, DRESLT, JFLAG)}
+   Convert free-format string from deg,arcmin,arcsec to radians
+\end{callset}
+
+\callhead{Sexagesimal Conversions}
+\begin{callset}
+\subq{CALL sla\_CTF2D (IHOUR, IMIN, SEC, DAYS, J)}
+     {CALL sla\_DTF2D (IHOUR, IMIN, SEC, DAYS, J)}
+   Hours, minutes, seconds to days
+\subq{CALL sla\_CD2TF (NDP, DAYS, SIGN, IHMSF)}
+     {CALL sla\_DD2TF (NDP, DAYS, SIGN, IHMSF)}
+   Days to hours, minutes, seconds
+\subq{CALL sla\_CTF2R (IHOUR, IMIN, SEC, RAD, J)}
+     {CALL sla\_DTF2R (IHOUR, IMIN, SEC, RAD, J)}
+   Hours, minutes, seconds to radians
+\subq{CALL sla\_CR2TF (NDP, ANGLE, SIGN, IHMSF)}
+     {CALL sla\_DR2TF (NDP, ANGLE, SIGN, IHMSF)}
+   Radians to hours, minutes, seconds
+\subq{CALL sla\_CAF2R (IDEG, IAMIN, ASEC, RAD, J)}
+     {CALL sla\_DAF2R (IDEG, IAMIN, ASEC, RAD, J)}
+   Degrees, arcminutes, arcseconds to radians
+\subq{CALL sla\_CR2AF (NDP, ANGLE, SIGN, IDMSF)}
+     {CALL sla\_DR2AF (NDP, ANGLE, SIGN, IDMSF)}
+   Radians to degrees, arcminutes, arcseconds
+\end{callset}
+
+\callhead{Angles, Vectors and Rotation Matrices}
+\begin{callset}
+\subq{R~=~sla\_RANGE (ANGLE)}
+     {D~=~sla\_DRANGE (ANGLE)}
+   Normalize angle into range $\pm\pi$
+\subq{R~=~sla\_RANORM (ANGLE)}
+     {D~=~sla\_DRANRM (ANGLE)}
+   Normalize angle into range $0\!-\!2\pi$
+\subq{CALL sla\_CS2C (A, B, V)}
+     {CALL sla\_DCS2C (A, B, V)}
+   Spherical coordinates to \xyz
+\subq{CALL sla\_CC2S (V, A, B)}
+     {CALL sla\_DCC2S (V, A, B)}
+   \xyz\ to spherical coordinates
+\subq{R~=~sla\_VDV (VA, VB)}
+     {D~=~sla\_DVDV (VA, VB)}
+   Scalar product of two 3-vectors
+\subq{CALL sla\_VXV (VA, VB, VC)}
+     {CALL sla\_DVXV (VA, VB, VC)}
+   Vector product of two 3-vectors
+\subq{CALL sla\_VN (V, UV, VM)}
+     {CALL sla\_DVN (V, UV, VM)}
+   Normalize a 3-vector also giving the modulus
+\subq{R~=~sla\_SEP (A1, B1, A2, B2)}
+     {D~=~sla\_DSEP (A1, B1, A2, B2)}
+   Angle between two points on a sphere
+\subq{R~=~sla\_BEAR (A1, B1, A2, B2)}
+     {D~=~sla\_DBEAR (A1, B1, A2, B2)}
+   Direction of one point on a sphere seen from another
+\subq{R~=~sla\_PAV (V1, V2)}
+     {D~=~sla\_DPAV (V1, V2)}
+   Position-angle of one \xyz\ with respect to another
+\subq{CALL sla\_EULER (ORDER, PHI, THETA, PSI, RMAT)}
+     {CALL sla\_DEULER (ORDER, PHI, THETA, PSI, RMAT)}
+   Form rotation matrix from three Euler angles
+\subq{CALL sla\_AV2M (AXVEC, RMAT)}
+     {CALL sla\_DAV2M (AXVEC, RMAT)}
+   Form rotation matrix from axial vector
+\subq{CALL sla\_M2AV (RMAT, AXVEC)}
+     {CALL sla\_DM2AV (RMAT, AXVEC)}
+   Determine axial vector from rotation matrix
+\subq{CALL sla\_MXV (RM, VA, VB)}
+     {CALL sla\_DMXV (DM, VA, VB)}
+   Rotate vector forwards
+\subq{CALL sla\_IMXV (RM, VA, VB)}
+     {CALL sla\_DIMXV (DM, VA, VB)}
+   Rotate vector backwards
+\subq{CALL sla\_MXM (A, B, C)}
+     {CALL sla\_DMXM (A, B, C)}
+   Product of two 3x3 matrices
+\subq{CALL sla\_CS2C6 (A, B, R, AD, BD, RD, V)}
+     {CALL sla\_DS2C6 (A, B, R, AD, BD, RD, V)}
+   Conversion of position and velocity in spherical
+     coordinates to Cartesian coordinates
+\subq{CALL sla\_CC62S (V, A, B, R, AD, BD, RD)}
+     {CALL sla\_DC62S (V, A, B, R, AD, BD, RD)}
+   Conversion of position and velocity in Cartesian
+     coordinates to spherical coordinates
+\end{callset}
+
+\callhead{Calendars}
+\begin{callset}
+\subp{CALL sla\_CLDJ (IY, IM, ID, DJM, J)}
+   Gregorian Calendar to Modified Julian Date
+\subp{CALL sla\_CALDJ (IY, IM, ID, DJM, J)}
+   Gregorian Calendar to Modified Julian Date,
+     permitting century default
+\subp{CALL sla\_DJCAL (NDP, DJM, IYMDF, J)}
+   Modified Julian Date to Gregorian Calendar,
+     in a form convenient for formatted output
+\subp{CALL sla\_DJCL (DJM, IY, IM, ID, FD, J)}
+   Modified Julian Date to Gregorian Year, Month, Day, Fraction
+\subp{CALL sla\_CALYD (IY, IM, ID, NY, ND, J)}
+   Calendar to year and day in year, permitting century default
+\subp{CALL sla\_CLYD (IY, IM, ID, NY, ND, J)}
+   Calendar to year and day in year
+\subp{D~=~sla\_EPB (DATE)}
+   Modified Julian Date to Besselian Epoch
+\subp{D~=~sla\_EPB2D (EPB)}
+   Besselian Epoch to Modified Julian Date
+\subp{D~=~sla\_EPJ (DATE)}
+   Modified Julian Date to Julian Epoch
+\subp{D~=~sla\_EPJ2D (EPJ)}
+   Julian Epoch to Modified Julian Date
+\end{callset}
+
+\callhead{Timescales}
+\begin{callset}
+\subp{D~=~sla\_GMST (UT1)}
+   Conversion from Universal Time to sidereal time
+\subp{D~=~sla\_GMSTA (DATE, UT1)}
+   Conversion from Universal Time to sidereal time, rounding errors minimized
+\subp{D~=~sla\_EQEQX (DATE)}
+   Equation of the equinoxes
+\subp{D~=~sla\_DAT (DJU)}
+   Offset of Atomic Time from Coordinated Universal Time: TAI$-$UTC
+\subp{D~=~sla\_DT (EPOCH)}
+   Approximate offset between dynamical time and universal time
+\subp{D~=~sla\_DTT (DJU)}
+   Offset of Terrestrial Time from Coordinated Universal Time: TT$-$UTC
+\subp{D~=~sla\_RCC (TDB, UT1, WL, U, V)}
+   Relativistic clock correction: TDB$-$TT
+\end{callset}
+
+\callhead{Precession and Nutation}
+\begin{callset}
+\subp{CALL sla\_NUT (DATE, RMATN)}
+   Nutation matrix
+\subp{CALL sla\_NUTC (DATE, DPSI, DEPS, EPS0)}
+   Longitude and obliquity components of nutation, and
+     mean obliquity
+\subp{CALL sla\_PREC (EP0, EP1, RMATP)}
+   Precession matrix (IAU)
+\subp{CALL sla\_PRECL (EP0, EP1, RMATP)}
+   Precession matrix (suitable for long periods)
+\subp{CALL sla\_PRENUT (EPOCH, DATE, RMATPN)}
+   Combined precession/nutation matrix
+\subp{CALL sla\_PREBN (BEP0, BEP1, RMATP)}
+   Precession matrix, old system
+\subp{CALL sla\_PRECES (SYSTEM, EP0, EP1, RA, DC)}
+   Precession, in either the old or the new system
+\end{callset}
+
+\callhead{Proper Motion}
+\begin{callset}
+\subp{CALL sla\_PM (R0, D0, PR, PD, PX, RV, EP0, EP1, R1, D1)}
+   Adjust for proper motion
+\end{callset}
+
+\callhead{FK4/FK5/Hipparcos Conversions}
+\begin{callset}
+\subp{CALL sla\_FK425 (\vtop
+                       {\hbox{R1950, D1950, DR1950, DD1950, P1950, V1950,}
+                        \hbox{R2000, D2000, DR2000, DD2000, P2000, V2000)}}}
+   Convert B1950.0 FK4 star data to J2000.0 FK5
+\subp{CALL sla\_FK45Z (R1950, D1950, EPOCH, R2000, D2000)}
+   Convert B1950.0 FK4 position to J2000.0 FK5 assuming zero
+   FK5 proper motion and no parallax
+\subp{CALL sla\_FK524 (\vtop
+                       {\hbox{R2000, D2000, DR2000, DD2000, P2000, V2000,}
+                        \hbox{R1950, D1950, DR1950, DD1950, P1950, V1950)}}}
+   Convert J2000.0 FK5 star data to B1950.0 FK4
+\subp{CALL sla\_FK54Z (R2000, D2000, BEPOCH,
+               R1950, D1950, DR1950, DD1950)}
+   Convert J2000.0 FK5 position to B1950.0 FK4 assuming zero
+   FK5 proper motion and no parallax
+\subp{CALL sla\_FK52H (R5, D5, DR5, DD5, RH, DH, DRH, DDH)}
+   Convert J2000.0 FK5 star data to Hipparcos
+\subp{CALL sla\_FK5HZ (R5, D5, EPOCH, RH, DH )}
+   Convert J2000.0 FK5 position to Hipparcos assuming zero Hipparcos
+   proper motion
+\subp{CALL sla\_H2FK5 (RH, DH, DRH, DDH, R5, D5, DR5, DD5)}
+   Convert Hipparcos star data to J2000.0 FK5
+\subp{CALL sla\_HFK5Z (RH, DH, EPOCH, R5, D5, DR5, DD5)}
+   Convert Hipparcos position to J2000.0 FK5 assuming zero Hipparcos
+   proper motion
+\subp{CALL sla\_DBJIN (STRING, NSTRT, DRESLT, J1, J2)}
+   Like sla\_DFLTIN but with extensions to accept leading `B' and `J'
+\subp{CALL sla\_KBJ (JB, E, K, J)}
+   Select epoch prefix `B' or `J'
+\subp{D~=~sla\_EPCO (K0, K, E)}
+   Convert an epoch into the appropriate form -- `B' or `J'
+\end{callset}
+
+\callhead{Elliptic Aberration}
+\begin{callset}
+\subp{CALL sla\_ETRMS (EP, EV)}
+   E-terms
+\subp{CALL sla\_SUBET (RC, DC, EQ, RM, DM)}
+   Remove the E-terms
+\subp{CALL sla\_ADDET (RM, DM, EQ, RC, DC)}
+   Add the E-terms
+\end{callset}
+
+\callhead{Geographical and Geocentric Coordinates}
+\begin{callset}
+\subp{CALL sla\_OBS (NUMBER, ID, NAME, WLONG, PHI, HEIGHT)}
+   Interrogate list of observatory parameters
+\subp{CALL sla\_GEOC (P, H, R, Z)}
+   Convert geodetic position to geocentric
+\subp{CALL sla\_POLMO (ELONGM, PHIM, XP, YP, ELONG, PHI, DAZ)}
+   Polar motion
+\subp{CALL sla\_PVOBS (P, H, STL, PV)}
+   Position and velocity of observatory
+\end{callset}
+
+\callhead{Apparent and Observed Place}
+\begin{callset}
+\subp{CALL sla\_MAP (RM, DM, PR, PD, PX, RV, EQ, DATE, RA, DA)}
+   Mean place to geocentric apparent place
+\subp{CALL sla\_MAPPA (EQ, DATE, AMPRMS)}
+   Precompute mean to apparent parameters
+\subp{CALL sla\_MAPQK (RM, DM, PR, PD, PX, RV, AMPRMS, RA, DA)}
+   Mean to apparent using precomputed parameters
+\subp{CALL sla\_MAPQKZ (RM, DM, AMPRMS, RA, DA)}
+   Mean to apparent using precomputed parameters, for zero proper
+     motion, parallax and radial velocity
+\subp{CALL sla\_AMP (RA, DA, DATE, EQ, RM, DM)}
+   Geocentric apparent place to mean place
+\subp{CALL sla\_AMPQK (RA, DA, AOPRMS, RM, DM)}
+   Apparent to mean using precomputed parameters
+\subp{CALL sla\_AOP (\vtop
+                      {\hbox{RAP, DAP, UTC, DUT, ELONGM, PHIM, HM, XP, YP,}
+                       \hbox{TDK, PMB, RH, WL, TLR, AOB, ZOB, HOB, DOB, ROB)}}}
+   Apparent place to observed place
+\subp{CALL sla\_AOPPA (\vtop
+                        {\hbox{UTC, DUT, ELONGM, PHIM, HM, XP, YP,}
+                         \hbox{TDK, PMB, RH, WL, TLR, AOPRMS)}}}
+   Precompute apparent to observed parameters
+\subp{CALL sla\_AOPPAT (UTC, AOPRMS)}
+   Update sidereal time in apparent to observed parameters
+\subp{CALL sla\_AOPQK (RAP, DAP, AOPRMS, AOB, ZOB, HOB, DOB, ROB)}
+   Apparent to observed using precomputed parameters
+\subp{CALL sla\_OAP (\vtop
+                     {\hbox{TYPE, OB1, OB2, UTC, DUT, ELONGM, PHIM, HM, XP, YP,}
+                      \hbox{TDK, PMB, RH, WL, TLR, RAP, DAP)}}}
+   Observed to apparent
+\subp{CALL sla\_OAPQK (TYPE, OB1, OB2, AOPRMS, RA, DA)}
+   Observed to apparent using precomputed parameters
+\end{callset}
+
+\callhead{Azimuth and Elevation}
+\begin{callset}
+\subp{CALL sla\_ALTAZ (\vtop
+               {\hbox{HA, DEC, PHI,}
+                \hbox{AZ, AZD, AZDD, EL, ELD, ELDD, PA, PAD, PADD)}}}
+   Positions, velocities {\it etc.}\ for an altazimuth mount
+\subq{CALL sla\_E2H (HA, DEC, PHI, AZ, EL)}
+     {CALL sla\_DE2H (HA, DEC, PHI, AZ, EL)}
+   \hadec\ to \azel
+\subq{CALL sla\_H2E (AZ, EL, PHI, HA, DEC)}
+     {CALL sla\_DH2E (AZ, EL, PHI, HA, DEC)}
+   \azel\ to \hadec
+\subp{CALL sla\_PDA2H (P, D, A, H1, J1, H2, J2)}
+   Hour Angle corresponding to a given azimuth
+\subp{CALL sla\_PDQ2H (P, D, Q, H1, J1, H2, J2)}
+   Hour Angle corresponding to a given parallactic angle
+\subp{D~=~sla\_PA (HA, DEC, PHI)}
+   \hadec\ to parallactic angle
+\subp{D~=~sla\_ZD (HA, DEC, PHI)}
+   \hadec\ to zenith distance
+\end{callset}
+
+\callhead{Refraction and Air Mass}
+\begin{callset}
+\subp{CALL sla\_REFRO (ZOBS, HM, TDK, PMB, RH, WL, PHI, TLR, EPS, REF)}
+   Change in zenith distance due to refraction
+\subp{CALL sla\_REFCO (HM, TDK, PMB, RH, WL, PHI, TLR, EPS, REFA, REFB)}
+   Constants for simple refraction model (accurate)
+\subp{CALL sla\_REFCOQ (TDK, PMB, RH, WL, REFA, REFB)}
+   Constants for simple refraction model (fast)
+\subp{CALL sla\_ATMDSP ( TDK, PMB, RH, WL1, REFA1, REFB1, WL2, REFA2, REFB2 )}
+   Adjust refraction constants for colour
+\subp{CALL sla\_REFZ (ZU, REFA, REFB, ZR)}
+   Unrefracted to refracted ZD, simple model
+\subp{CALL sla\_REFV (VU, REFA, REFB, VR)}
+   Unrefracted to refracted \azel\ vector, simple model
+\subp{D~=~sla\_AIRMAS (ZD)}
+   Air mass
+\end{callset}
+
+\callhead{Ecliptic Coordinates}
+\begin{callset}
+\subp{CALL sla\_ECMAT (DATE, RMAT)}
+   Equatorial to ecliptic rotation matrix
+\subp{CALL sla\_EQECL (DR, DD, DATE, DL, DB)}
+   J2000.0 `FK5' to ecliptic coordinates
+\subp{CALL sla\_ECLEQ (DL, DB, DATE, DR, DD)}
+   Ecliptic coordinates to J2000.0 `FK5'
+\end{callset}
+
+\callhead{Galactic Coordinates}
+\begin{callset}
+\subp{CALL sla\_EG50 (DR, DD, DL, DB)}
+   B1950.0 `FK4' to galactic
+\subp{CALL sla\_GE50 (DL, DB, DR, DD)}
+   Galactic to B1950.0 `FK4'
+\subp{CALL sla\_EQGAL (DR, DD, DL, DB)}
+   J2000.0 `FK5' to galactic
+\subp{CALL sla\_GALEQ (DL, DB, DR, DD)}
+   Galactic to J2000.0 `FK5'
+\end{callset}
+
+\callhead{Supergalactic Coordinates}
+\begin{callset}
+\subp{CALL sla\_GALSUP (DL, DB, DSL, DSB)}
+   Galactic to supergalactic
+\subp{CALL sla\_SUPGAL (DSL, DSB, DL, DB)}
+   Supergalactic to galactic
+\end{callset}
+
+\callhead{Ephemerides}
+\begin{callset}
+\subp{CALL sla\_DMOON (DATE, PV)}
+   Approximate geocentric position and velocity of the Moon
+\subp{CALL sla\_EARTH (IY, ID, FD, PV)}
+   Approximate heliocentric position and velocity of the Earth
+\subp{CALL sla\_EVP (DATE, DEQX, DVB, DPB, DVH, DPH)}
+   Barycentric and heliocentric velocity and position of the Earth
+\subp{CALL sla\_MOON (IY, ID, FD, PV)}
+   Approximate geocentric position and velocity of the Moon
+\subp{CALL sla\_PLANET (DATE, NP, PV, JSTAT)}
+   Approximate heliocentric position and velocity of a planet
+\subp{CALL sla\_RDPLAN (DATE, NP, ELONG, PHI, RA, DEC, DIAM)}
+   Approximate topocentric apparent place of a planet
+\subp{CALL sla\_PLANEL (\vtop
+                       {\hbox{DATE, JFORM, EPOCH, ORBINC, ANODE, PERIH,}
+                      \hbox{AORQ, E, AORL, DM, PV, JSTAT)}}}
+   Heliocentric position and velocity of a planet, asteroid or
+   comet, starting from orbital elements
+\subp{CALL sla\_PLANTE (\vtop
+                       {\hbox{DATE, ELONG, PHI, JFORM, EPOCH, ORBINC, ANODE,}
+                      \hbox{PERIH, AORQ, E, AORL, DM, RA, DEC, R, JSTAT)}}}
+   Topocentric apparent place of a Solar-System object whose
+   heliocentric orbital elements are known
+\subp{CALL sla\_PV2EL (\vtop
+                      {\hbox{PV, DATE, PMASS, JFORMR, JFORM, EPOCH, ORBINC,}
+                     \hbox{ANODE, PERIH, AORQ, E, AORL, DM, JSTAT)}}}
+   Orbital elements of a planet from instantaneous position and velocity
+\subp{CALL sla\_PERTEL (\vtop
+                       {\hbox{JFORM, DATE0, DATE1,}
+                     \hbox{EPOCH0, ORBI0, ANODE0, PERIH0, AORQ0, E0, AM0,}
+                     \hbox{EPOCH1, ORBI1, ANODE1, PERIH1, AORQ1, E1, AM1,}
+                     \hbox{JSTAT)}}}
+   Update elements by applying perturbations
+\subp{CALL sla\_EL2UE (\vtop
+                      {\hbox{DATE, JFORM, EPOCH, ORBINC, ANODE,}
+                     \hbox{PERIH, AORQ, E, AORL, DM,}
+                     \hbox{U, JSTAT)}}}
+   Transform conventional elements to universal elements
+\subp{CALL sla\_UE2EL (\vtop
+                      {\hbox{U, JFORMR,}
+                     \hbox{JFORM, EPOCH, ORBINC, ANODE, PERIH,}
+                     \hbox{AORQ, E, AORL, DM, JSTAT)}}}
+   Transform universal elements to conventional elements
+\subp{CALL sla\_PV2UE (PV, DATE, PMASS, U, JSTAT)}
+   Package a position and velocity for use as universal elements
+\subp{CALL sla\_UE2PV (DATE, U, PV, JSTAT)}
+   Extract the position and velocity from universal elements
+\subp{CALL sla\_PERTUE (DATE, U, JSTAT)}
+   Update universal elements by applying perturbations
+\subp{R~=~sla\_RVEROT (PHI, RA, DA, ST)}
+   Velocity component due to rotation of the Earth
+\subp{CALL sla\_ECOR (RM, DM, IY, ID, FD, RV, TL)}
+   Components of velocity and light time due to Earth orbital motion
+\subp{R~=~sla\_RVLSRD (R2000, D2000)}
+   Velocity component due to solar motion wrt dynamical LSR
+\subp{R~=~sla\_RVLSRK (R2000, D2000)}
+   Velocity component due to solar motion wrt kinematical LSR
+\subp{R~=~sla\_RVGALC (R2000, D2000)}
+   Velocity component due to rotation of the Galaxy
+\subp{R~=~sla\_RVLG (R2000, D2000)}
+   Velocity component due to rotation and translation of the
+   Galaxy, relative to the mean motion of the local group
+\end{callset}
+
+\callhead{Astrometry}
+\begin{callset}
+\subq{CALL sla\_S2TP (RA, DEC, RAZ, DECZ, XI, ETA, J)}
+     {CALL sla\_DS2TP (RA, DEC, RAZ, DECZ, XI, ETA, J)}
+   Transform spherical coordinates into tangent plane
+\subq{CALL sla\_V2TP (V, V0, XI, ETA, J)}
+     {CALL sla\_DV2TP (V, V0, XI, ETA, J)}
+   Transform \xyz\ into tangent plane coordinates
+\subq{CALL sla\_DTP2S (XI, ETA, RAZ, DECZ, RA, DEC)}
+     {CALL sla\_TP2S (XI, ETA, RAZ, DECZ, RA, DEC)}
+   Transform tangent plane coordinates into spherical coordinates
+\subq{CALL sla\_DTP2V (XI, ETA, V0, V)}
+     {CALL sla\_TP2V (XI, ETA, V0, V)}
+   Transform tangent plane coordinates into \xyz
+\subq{CALL sla\_DTPS2C (XI, ETA, RA, DEC, RAZ1, DECZ1, RAZ2, DECZ2, N)}
+     {CALL sla\_TPS2C (XI, ETA, RA, DEC, RAZ1, DECZ1, RAZ2, DECZ2, N)}
+   Get plate centre from star \radec\ and tangent plane coordinates
+\subq{CALL sla\_DTPV2C (XI, ETA, V, V01, V02, N)}
+     {CALL sla\_TPV2C (XI, ETA, V, V01, V02, N)}
+   Get plate centre from star \xyz\ and tangent plane coordinates
+\subp{CALL sla\_PCD (DISCO, X, Y)}
+   Apply pincushion/barrel distortion
+\subp{CALL sla\_UNPCD (DISCO, X, Y)}
+   Remove pincushion/barrel distortion
+\subp{CALL sla\_FITXY (ITYPE, NP, XYE, XYM, COEFFS, J)}
+   Fit a linear model to relate two sets of \xy\ coordinates
+\subp{CALL sla\_PXY (NP, XYE, XYM, COEFFS, XYP, XRMS, YRMS, RRMS)}
+   Compute predicted coordinates and residuals
+\subp{CALL sla\_INVF (FWDS, BKWDS, J)}
+   Invert a linear model
+\subp{CALL sla\_XY2XY (X1, Y1, COEFFS, X2, Y2)}
+   Transform one \xy
+\subp{CALL sla\_DCMPF (COEFFS, XZ, YZ, XS, YS, PERP, ORIENT)}
+   Decompose a linear fit into scales {\it etc.}
+\end{callset}
+
+\callhead{Numerical Methods}
+\begin{callset}
+\subp{CALL sla\_COMBN (NSEL, NCAND, LIST, J)}
+   Next combination (subset from a specified number of items)
+\subp{CALL sla\_PERMUT (N, ISTATE, IORDER, J)}
+   Next permutation of a specified number of items
+\subq{CALL sla\_SMAT (N, A, Y, D, JF, IW)}
+     {CALL sla\_DMAT (N, A, Y, D, JF, IW)}
+   Matrix inversion and solution of simultaneous equations
+\subp{CALL sla\_SVD (M, N, MP, NP, A, W, V, WORK, JSTAT)}
+   Singular value decomposition of a matrix
+\subp{CALL sla\_SVDSOL (M, N, MP, NP, B, U, W, V, WORK, X)}
+   Solution from given vector plus SVD
+\subp{CALL sla\_SVDCOV (N, NP, NC, W, V, WORK, CVM)}
+   Covariance matrix from SVD
+\subp{R~=~sla\_RANDOM (SEED)}
+   Generate pseudo-random real number in the range {$0 \leq x < 1$}
+\subp{R~=~sla\_GRESID (S)}
+   Generate pseudo-random normal deviate ($\equiv$ `Gaussian residual')
+\end{callset}
+
+\callhead{Real-time}
+\begin{callset}
+\subp{CALL sla\_WAIT (DELAY)}
+    Interval wait
+\end{callset}
+
+\end{document}
diff --git a/src/slalib/supgal.f b/src/slalib/supgal.f
new file mode 100644
index 0000000..4658c8a
--- /dev/null
+++ b/src/slalib/supgal.f
@@ -0,0 +1,79 @@
+      SUBROUTINE sla_SUPGAL (DSL, DSB, DL, DB)
+*+
+*     - - - - - - -
+*      S U P G A L
+*     - - - - - - -
+*
+*  Transformation from de Vaucouleurs supergalactic coordinates
+*  to IAU 1958 galactic coordinates (double precision)
+*
+*  Given:
+*     DSL,DSB     dp       supergalactic longitude and latitude
+*
+*  Returned:
+*     DL,DB       dp       galactic longitude and latitude L2,B2
+*
+*  (all arguments are radians)
+*
+*  Called:
+*     sla_DCS2C, sla_DIMXV, sla_DCC2S, sla_DRANRM, sla_DRANGE
+*
+*  References:
+*
+*     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.)
+*
+*  P.T.Wallace   Starlink   March 1986
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DSL,DSB,DL,DB
+
+      DOUBLE PRECISION sla_DRANRM,sla_DRANGE
+
+      DOUBLE PRECISION V1(3),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 PRECISION RMAT(3,3)
+      DATA RMAT(1,1),RMAT(1,2),RMAT(1,3),
+     :     RMAT(2,1),RMAT(2,2),RMAT(2,3),
+     :     RMAT(3,1),RMAT(3,2),RMAT(3,3)/
+     : -0.735742574804D0,+0.677261296414D0,+0.000000000000D0,
+     : -0.074553778365D0,-0.080991471307D0,+0.993922590400D0,
+     : +0.673145302109D0,+0.731271165817D0,+0.110081262225D0/
+
+
+
+*  Spherical to Cartesian
+      CALL sla_DCS2C(DSL,DSB,V1)
+
+*  Supergalactic to galactic
+      CALL sla_DIMXV(RMAT,V1,V2)
+
+*  Cartesian to spherical
+      CALL sla_DCC2S(V2,DL,DB)
+
+*  Express in conventional ranges
+      DL=sla_DRANRM(DL)
+      DB=sla_DRANGE(DB)
+
+      END
diff --git a/src/slalib/svd.f b/src/slalib/svd.f
new file mode 100644
index 0000000..8498333
--- /dev/null
+++ b/src/slalib/svd.f
@@ -0,0 +1,379 @@
+      SUBROUTINE sla_SVD (M, N, MP, NP, A, W, V, WORK, JSTAT)
+*+
+*     - - - -
+*      S V D
+*     - - - -
+*
+*  Singular value decomposition  (double precision)
+*
+*  This routine expresses a given matrix A as the product of
+*  three matrices U, W, V:
+*
+*     A = U x W x VT
+*
+*  Where:
+*
+*     A   is any M (rows) x N (columns) matrix, where M.GE.N
+*     U   is an M x N column-orthogonal matrix
+*     W   is an N x N diagonal matrix with W(I,I).GE.0
+*     VT  is the transpose of an N x N orthogonal matrix
+*
+*     Note that M and N, above, are the LOGICAL dimensions of the
+*     matrices and vectors concerned, which can be located in
+*     arrays of larger PHYSICAL dimensions, given by MP and NP.
+*
+*  Given:
+*     M,N    i         numbers of rows and columns in matrix A
+*     MP,NP  i         physical dimensions of array containing matrix A
+*     A      d(MP,NP)  array containing MxN matrix A
+*
+*  Returned:
+*     A      d(MP,NP)  array containing MxN column-orthogonal matrix U
+*     W      d(N)      NxN diagonal matrix W (diagonal elements only)
+*     V      d(NP,NP)  array containing NxN orthogonal matrix V
+*     WORK   d(N)      workspace
+*     JSTAT  i         0 = OK, -1 = A wrong shape, >0 = index of W
+*                      for which convergence failed.  See note 2, below.
+*
+*   Notes:
+*
+*   1)  V contains matrix V, not the transpose of matrix V.
+*
+*   2)  If the status JSTAT is greater than zero, this need not
+*       necessarily be treated as a failure.  It means that, due to
+*       chance properties of the matrix A, the QR transformation
+*       phase of the routine did not fully converge in a predefined
+*       number of iterations, something that very seldom occurs.
+*       When this condition does arise, it is possible that the
+*       elements of the diagonal matrix W have not been correctly
+*       found.  However, in practice the results are likely to
+*       be trustworthy.  Applications should report the condition
+*       as a warning, but then proceed normally.
+*
+*  References:
+*     The algorithm is an adaptation of the routine SVD in the EISPACK
+*     library (Garbow et al 1977, EISPACK Guide Extension, Springer
+*     Verlag), which is a FORTRAN 66 implementation of the Algol
+*     routine SVD of Wilkinson & Reinsch 1971 (Handbook for Automatic
+*     Computation, vol 2, ed Bauer et al, Springer Verlag).  These
+*     references give full details of the algorithm used here.  A good
+*     account of the use of SVD in least squares problems is given in
+*     Numerical Recipes (Press et al 1986, Cambridge University Press),
+*     which includes another variant of the EISPACK code.
+*
+*  P.T.Wallace   Starlink   22 December 1993
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER M,N,MP,NP
+      DOUBLE PRECISION A(MP,NP),W(N),V(NP,NP),WORK(N)
+      INTEGER JSTAT
+
+*  Maximum number of iterations in QR phase
+      INTEGER ITMAX
+      PARAMETER (ITMAX=30)
+
+      INTEGER I,K,L,J,K1,ITS,L1,I1
+      LOGICAL CANCEL
+      DOUBLE PRECISION G,SCALE,AN,S,X,F,H,C,Y,Z
+
+
+
+*  Check that the matrix is the right shape
+      IF (M.LT.N) THEN
+
+*     No:  error status
+         JSTAT = -1
+
+      ELSE
+
+*     Yes:  preset the status to OK
+         JSTAT = 0
+
+*
+*     Householder reduction to bidiagonal form
+*     ----------------------------------------
+
+         G = 0D0
+         SCALE = 0D0
+         AN = 0D0
+         DO I=1,N
+            L = I+1
+            WORK(I) = SCALE*G
+            G = 0D0
+            S = 0D0
+            SCALE = 0D0
+            IF (I.LE.M) THEN
+               DO K=I,M
+                  SCALE = SCALE+ABS(A(K,I))
+               END DO
+               IF (SCALE.NE.0D0) THEN
+                  DO K=I,M
+                     X = A(K,I)/SCALE
+                     A(K,I) = X
+                     S = S+X*X
+                  END DO
+                  F = A(I,I)
+                  G = -SIGN(SQRT(S),F)
+                  H = F*G-S
+                  A(I,I) = F-G
+                  IF (I.NE.N) THEN
+                     DO J=L,N
+                        S = 0D0
+                        DO K=I,M
+                           S = S+A(K,I)*A(K,J)
+                        END DO
+                        F = S/H
+                        DO K=I,M
+                           A(K,J) = A(K,J)+F*A(K,I)
+                        END DO
+                     END DO
+                  END IF
+                  DO K=I,M
+                     A(K,I) = SCALE*A(K,I)
+                  END DO
+               END IF
+            END IF
+            W(I) = SCALE*G
+            G = 0D0
+            S = 0D0
+            SCALE = 0D0
+            IF (I.LE.M .AND. I.NE.N) THEN
+               DO K=L,N
+                  SCALE = SCALE+ABS(A(I,K))
+               END DO
+               IF (SCALE.NE.0D0) THEN
+                  DO K=L,N
+                     X = A(I,K)/SCALE
+                     A(I,K) = X
+                     S = S+X*X
+                  END DO
+                  F = A(I,L)
+                  G = -SIGN(SQRT(S),F)
+                  H = F*G-S
+                  A(I,L) = F-G
+                  DO K=L,N
+                     WORK(K) = A(I,K)/H
+                  END DO
+                  IF (I.NE.M) THEN
+                     DO J=L,M
+                        S = 0D0
+                        DO K=L,N
+                           S = S+A(J,K)*A(I,K)
+                        END DO
+                        DO K=L,N
+                           A(J,K) = A(J,K)+S*WORK(K)
+                        END DO
+                     END DO
+                  END IF
+                  DO K=L,N
+                     A(I,K) = SCALE*A(I,K)
+                  END DO
+               END IF
+            END IF
+
+*        Overestimate of largest column norm for convergence test
+            AN = MAX(AN,ABS(W(I))+ABS(WORK(I)))
+
+         END DO
+
+*
+*     Accumulation of right-hand transformations
+*     ------------------------------------------
+
+         DO I=N,1,-1
+            IF (I.NE.N) THEN
+               IF (G.NE.0D0) THEN
+                  DO J=L,N
+                     V(J,I) = (A(I,J)/A(I,L))/G
+                  END DO
+                  DO J=L,N
+                     S = 0D0
+                     DO K=L,N
+                        S = S+A(I,K)*V(K,J)
+                     END DO
+                     DO K=L,N
+                        V(K,J) = V(K,J)+S*V(K,I)
+                     END DO
+                  END DO
+               END IF
+               DO J=L,N
+                  V(I,J) = 0D0
+                  V(J,I) = 0D0
+               END DO
+            END IF
+            V(I,I) = 1D0
+            G = WORK(I)
+            L = I
+         END DO
+
+*
+*     Accumulation of left-hand transformations
+*     -----------------------------------------
+
+         DO I=N,1,-1
+            L = I+1
+            G = W(I)
+            IF (I.NE.N) THEN
+               DO J=L,N
+                  A(I,J) = 0D0
+               END DO
+            END IF
+            IF (G.NE.0D0) THEN
+               IF (I.NE.N) THEN
+                  DO J=L,N
+                     S = 0D0
+                     DO K=L,M
+                        S = S+A(K,I)*A(K,J)
+                     END DO
+                     F = (S/A(I,I))/G
+                     DO K=I,M
+                        A(K,J) = A(K,J)+F*A(K,I)
+                     END DO
+                  END DO
+               END IF
+               DO J=I,M
+                  A(J,I) = A(J,I)/G
+               END DO
+            ELSE
+               DO J=I,M
+                  A(J,I) = 0D0
+               END DO
+            END IF
+            A(I,I) = A(I,I)+1D0
+         END DO
+
+*
+*     Diagonalisation of the bidiagonal form
+*     --------------------------------------
+
+         DO K=N,1,-1
+            K1 = K-1
+
+*        Iterate until converged
+            ITS = 0
+            DO WHILE (ITS.LT.ITMAX)
+               ITS = ITS+1
+
+*           Test for splitting into submatrices
+               CANCEL = .TRUE.
+               DO L=K,1,-1
+                  L1 = L-1
+                  IF (AN+ABS(WORK(L)).EQ.AN) THEN
+                     CANCEL = .FALSE.
+                     GO TO 10
+                  END IF
+*              (Following never attempted for L=1 because WORK(1) is zero)
+                  IF (AN+ABS(W(L1)).EQ.AN) GO TO 10
+               END DO
+ 10            CONTINUE
+
+*           Cancellation of WORK(L) if L>1
+               IF (CANCEL) THEN
+                  C = 0D0
+                  S = 1D0
+                  DO I=L,K
+                     F = S*WORK(I)
+                     IF (AN+ABS(F).EQ.AN) GO TO 20
+                     G = W(I)
+                     H = SQRT(F*F+G*G)
+                     W(I) = H
+                     C = G/H
+                     S = -F/H
+                     DO J=1,M
+                        Y = A(J,L1)
+                        Z = A(J,I)
+                        A(J,L1) = Y*C+Z*S
+                        A(J,I) = -Y*S+Z*C
+                     END DO
+                  END DO
+ 20               CONTINUE
+               END IF
+
+*           Converged?
+               Z = W(K)
+               IF (L.EQ.K) THEN
+
+*              Yes:  stop iterating
+                  ITS = ITMAX
+
+*              Ensure singular values non-negative
+                  IF (Z.LT.0D0) THEN
+                     W(K) = -Z
+                     DO J=1,N
+                        V(J,K) = -V(J,K)
+                     END DO
+                  END IF
+               ELSE
+
+*              Not converged yet:  set status if iteration limit reached
+                  IF (ITS.EQ.ITMAX) JSTAT = K
+
+*              Shift from bottom 2x2 minor
+                  X = W(L)
+                  Y = W(K1)
+                  G = WORK(K1)
+                  H = WORK(K)
+                  F = ((Y-Z)*(Y+Z)+(G-H)*(G+H))/(2D0*H*Y)
+                  IF (ABS(F).LE.1D15) THEN
+                     G = SQRT(F*F+1D0)
+                  ELSE
+                     G = ABS(F)
+                  END IF
+                  F = ((X-Z)*(X+Z)+H*(Y/(F+SIGN(G,F))-H))/X
+
+*              Next QR transformation
+                  C = 1D0
+                  S = 1D0
+                  DO I1=L,K1
+                     I = I1+1
+                     G = WORK(I)
+                     Y = W(I)
+                     H = S*G
+                     G = C*G
+                     Z = SQRT(F*F+H*H)
+                     WORK(I1) = Z
+                     IF (Z.NE.0D0) THEN
+                        C = F/Z
+                        S = H/Z
+                     ELSE
+                        C = 1D0
+                        S = 0D0
+                     END IF
+                     F = X*C+G*S
+                     G = -X*S+G*C
+                     H = Y*S
+                     Y = Y*C
+                     DO J=1,N
+                        X = V(J,I1)
+                        Z = V(J,I)
+                        V(J,I1) = X*C+Z*S
+                        V(J,I) = -X*S+Z*C
+                     END DO
+                     Z = SQRT(F*F+H*H)
+                     W(I1) = Z
+                     IF (Z.NE.0D0) THEN
+                        C = F/Z
+                        S = H/Z
+                     END IF
+                     F = C*G+S*Y
+                     X = -S*G+C*Y
+                     DO J=1,M
+                        Y = A(J,I1)
+                        Z = A(J,I)
+                        A(J,I1) = Y*C+Z*S
+                        A(J,I) = -Y*S+Z*C
+                     END DO
+                  END DO
+                  WORK(L) = 0D0
+                  WORK(K) = F
+                  W(K) = X
+               END IF
+            END DO
+         END DO
+      END IF
+
+      END
diff --git a/src/slalib/svdcov.f b/src/slalib/svdcov.f
new file mode 100644
index 0000000..86d882c
--- /dev/null
+++ b/src/slalib/svdcov.f
@@ -0,0 +1,60 @@
+      SUBROUTINE sla_SVDCOV (N, NP, NC, W, V, WORK, CVM)
+*+
+*     - - - - - - -
+*      S V D C O V
+*     - - - - - - -
+*
+*  From the W and V matrices from the SVD factorisation of a matrix
+*  (as obtained from the sla_SVD routine), obtain the covariance matrix.
+*
+*  (double precision)
+*
+*  Given:
+*     N      i         number of rows and columns in matrices W and V
+*     NP     i         first dimension of array containing matrix V
+*     NC     i         first dimension of array to receive CVM
+*     W      d(N)      NxN diagonal matrix W (diagonal elements only)
+*     V      d(NP,NP)  array containing NxN orthogonal matrix V
+*
+*  Returned:
+*     WORK   d(N)      workspace
+*     CVM    d(NC,NC)  array to receive covariance matrix
+*
+*  Reference:
+*     Numerical Recipes, section 14.3.
+*
+*  P.T.Wallace   Starlink   December 1988
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER N,NP,NC
+      DOUBLE PRECISION W(N),V(NP,NP),WORK(N),CVM(NC,NC)
+
+      INTEGER I,J,K
+      DOUBLE PRECISION S
+
+
+
+      DO I=1,N
+         S=W(I)
+         IF (S.NE.0D0) THEN
+            WORK(I)=1D0/(S*S)
+         ELSE
+            WORK(I)=0D0
+         END IF
+      END DO
+      DO I=1,N
+         DO J=1,I
+            S=0D0
+            DO K=1,N
+               S=S+V(I,K)*V(J,K)*WORK(K)
+            END DO
+            CVM(I,J)=S
+            CVM(J,I)=S
+         END DO
+      END DO
+
+      END
diff --git a/src/slalib/svdsol.f b/src/slalib/svdsol.f
new file mode 100644
index 0000000..46ef6bb
--- /dev/null
+++ b/src/slalib/svdsol.f
@@ -0,0 +1,109 @@
+      SUBROUTINE sla_SVDSOL (M, N, MP, NP, B, U, W, V, WORK, X)
+*+
+*     - - - - - - -
+*      S V D S O L
+*     - - - - - - -
+*
+*  From a given vector and the SVD of a matrix (as obtained from
+*  the SVD routine), obtain the solution vector (double precision)
+*
+*  This routine solves the equation:
+*
+*     A . x = b
+*
+*  where:
+*
+*     A   is a given M (rows) x N (columns) matrix, where M.GE.N
+*     x   is the N-vector we wish to find
+*     b   is a given M-vector
+*
+*  by means of the Singular Value Decomposition method (SVD).  In
+*  this method, the matrix A is first factorised (for example by
+*  the routine sla_SVD) into the following components:
+*
+*     A = U x W x VT
+*
+*  where:
+*
+*     A   is the M (rows) x N (columns) matrix
+*     U   is an M x N column-orthogonal matrix
+*     W   is an N x N diagonal matrix with W(I,I).GE.0
+*     VT  is the transpose of an NxN orthogonal matrix
+*
+*     Note that M and N, above, are the LOGICAL dimensions of the
+*     matrices and vectors concerned, which can be located in
+*     arrays of larger PHYSICAL dimensions MP and NP.
+*
+*  The solution is found from the expression:
+*
+*     x = V . [diag(1/Wj)] . (transpose(U) . b)
+*
+*  Notes:
+*
+*  1)  If matrix A is square, and if the diagonal matrix W is not
+*      adjusted, the method is equivalent to conventional solution
+*      of simultaneous equations.
+*
+*  2)  If M>N, the result is a least-squares fit.
+*
+*  3)  If the solution is poorly determined, this shows up in the
+*      SVD factorisation as very small or zero Wj values.  Where
+*      a Wj value is small but non-zero it can be set to zero to
+*      avoid ill effects.  The present routine detects such zero
+*      Wj values and produces a sensible solution, with highly
+*      correlated terms kept under control rather than being allowed
+*      to elope to infinity, and with meaningful values for the
+*      other terms.
+*
+*  Given:
+*     M,N    i         numbers of rows and columns in matrix A
+*     MP,NP  i         physical dimensions of array containing matrix A
+*     B      d(M)      known vector b
+*     U      d(MP,NP)  array containing MxN matrix U
+*     W      d(N)      NxN diagonal matrix W (diagonal elements only)
+*     V      d(NP,NP)  array containing NxN orthogonal matrix V
+*
+*  Returned:
+*     WORK   d(N)      workspace
+*     X      d(N)      unknown vector x
+*
+*  Reference:
+*     Numerical Recipes, section 2.9.
+*
+*  P.T.Wallace   Starlink   29 October 1993
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      INTEGER M,N,MP,NP
+      DOUBLE PRECISION B(M),U(MP,NP),W(N),V(NP,NP),WORK(N),X(N)
+
+      INTEGER J,I,JJ
+      DOUBLE PRECISION S
+
+
+
+*  Calculate [diag(1/Wj)] . transpose(U) . b (or zero for zero Wj)
+      DO J=1,N
+         S=0D0
+         IF (W(J).NE.0D0) THEN
+            DO I=1,M
+               S=S+U(I,J)*B(I)
+            END DO
+            S=S/W(J)
+         END IF
+         WORK(J)=S
+      END DO
+
+*  Multiply by matrix V to get result
+      DO J=1,N
+         S=0D0
+         DO JJ=1,N
+            S=S+V(J,JJ)*WORK(JJ)
+         END DO
+         X(J)=S
+      END DO
+
+      END
diff --git a/src/slalib/tp2s.f b/src/slalib/tp2s.f
new file mode 100644
index 0000000..11be54a
--- /dev/null
+++ b/src/slalib/tp2s.f
@@ -0,0 +1,42 @@
+      SUBROUTINE sla_TP2S (XI, ETA, RAZ, DECZ, RA, DEC)
+*+
+*     - - - - -
+*      T P 2 S
+*     - - - - -
+*
+*  Transform tangent plane coordinates into spherical
+*  (single precision)
+*
+*  Given:
+*     XI,ETA      real  tangent plane rectangular coordinates
+*     RAZ,DECZ    real  spherical coordinates of tangent point
+*
+*  Returned:
+*     RA,DEC      real  spherical coordinates (0-2pi,+/-pi/2)
+*
+*  Called:        sla_RANORM
+*
+*  P.T.Wallace   Starlink   24 July 1995
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL XI,ETA,RAZ,DECZ,RA,DEC
+
+      REAL sla_RANORM
+
+      REAL SDECZ,CDECZ,DENOM
+
+
+
+      SDECZ=SIN(DECZ)
+      CDECZ=COS(DECZ)
+
+      DENOM=CDECZ-ETA*SDECZ
+
+      RA=sla_RANORM(ATAN2(XI,DENOM)+RAZ)
+      DEC=ATAN2(SDECZ+ETA*CDECZ,SQRT(XI*XI+DENOM*DENOM))
+
+      END
diff --git a/src/slalib/tp2v.f b/src/slalib/tp2v.f
new file mode 100644
index 0000000..cd8db96
--- /dev/null
+++ b/src/slalib/tp2v.f
@@ -0,0 +1,56 @@
+      SUBROUTINE sla_TP2V (XI, ETA, V0, V)
+*+
+*     - - - - -
+*      T P 2 V
+*     - - - - -
+*
+*  Given the tangent-plane coordinates of a star and the direction
+*  cosines of the tangent point, determine the direction cosines
+*  of the star.
+*
+*  (single precision)
+*
+*  Given:
+*     XI,ETA    r       tangent plane coordinates of star
+*     V0        r(3)    direction cosines of tangent point
+*
+*  Returned:
+*     V         r(3)    direction cosines of star
+*
+*  Notes:
+*
+*  1  If vector V0 is not of unit length, the returned vector V will
+*     be wrong.
+*
+*  2  If vector V0 points at a pole, the returned vector V will be
+*     based on the arbitrary assumption that the RA of the tangent
+*     point is zero.
+*
+*  3  This routine is the Cartesian equivalent of the routine sla_TP2S.
+*
+*  P.T.Wallace   Starlink   11 February 1995
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL XI,ETA,V0(3),V(3)
+
+      REAL X,Y,Z,F,R
+
+
+      X=V0(1)
+      Y=V0(2)
+      Z=V0(3)
+      F=SQRT(1.0+XI*XI+ETA*ETA)
+      R=SQRT(X*X+Y*Y)
+      IF (R.EQ.0.0) THEN
+         R=1E-20
+         X=R
+      END IF
+      V(1)=(X-(XI*Y+ETA*X*Z)/R)/F
+      V(2)=(Y+(XI*X-ETA*Y*Z)/R)/F
+      V(3)=(Z+ETA*R)/F
+
+      END
diff --git a/src/slalib/tps2c.f b/src/slalib/tps2c.f
new file mode 100644
index 0000000..d7a7a52
--- /dev/null
+++ b/src/slalib/tps2c.f
@@ -0,0 +1,91 @@
+      SUBROUTINE sla_TPS2C (XI, ETA, RA, DEC, RAZ1, DECZ1,
+     :                                        RAZ2, DECZ2, N)
+*+
+*     - - - - - -
+*      T P S 2 C
+*     - - - - - -
+*
+*  From the tangent plane coordinates of a star of known RA,Dec,
+*  determine the RA,Dec of the tangent point.
+*
+*  (single precision)
+*
+*  Given:
+*     XI,ETA      r    tangent plane rectangular coordinates
+*     RA,DEC      r    spherical coordinates
+*
+*  Returned:
+*     RAZ1,DECZ1  r    spherical coordinates of tangent point, solution 1
+*     RAZ2,DECZ2  r    spherical coordinates of tangent point, solution 2
+*     N           i    number of solutions:
+*                        0 = no solutions returned (note 2)
+*                        1 = only the first solution is useful (note 3)
+*                        2 = both solutions are useful (note 3)
+*
+*  Notes:
+*
+*  1  The RAZ1 and RAZ2 values are returned in the range 0-2pi.
+*
+*  2  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.
+*
+*  3  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.
+*
+*  4  The DECZ1 and DECZ2 values are returned in the range +/-pi, but
+*     in the usual, non-pole-crossing, case, the range is +/-pi/2.
+*
+*  5  This routine is the spherical equivalent of the routine sla_DTPV2C.
+*
+*  Called:  sla_RANORM
+*
+*  P.T.Wallace   Starlink   5 June 1995
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL XI,ETA,RA,DEC,RAZ1,DECZ1,RAZ2,DECZ2
+      INTEGER N
+
+      REAL X2,Y2,SD,CD,SDF,R2,R,S,C
+
+      REAL sla_RANORM
+
+
+      X2=XI*XI
+      Y2=ETA*ETA
+      SD=SIN(DEC)
+      CD=COS(DEC)
+      SDF=SD*SQRT(1.0+X2+Y2)
+      R2=CD*CD*(1.0+Y2)-SD*SD*X2
+      IF (R2.GE.0.0) THEN
+         R=SQRT(R2)
+         S=SDF-ETA*R
+         C=SDF*ETA+R
+         IF (XI.EQ.0.0.AND.R.EQ.0.0) R=1.0
+         RAZ1=sla_RANORM(RA-ATAN2(XI,R))
+         DECZ1=ATAN2(S,C)
+         R=-R
+         S=SDF-ETA*R
+         C=SDF*ETA+R
+         RAZ2=sla_RANORM(RA-ATAN2(XI,R))
+         DECZ2=ATAN2(S,C)
+         IF (ABS(SDF).LT.1.0) THEN
+            N=1
+         ELSE
+            N=2
+         END IF
+      ELSE
+         N=0
+      END IF
+
+      END
diff --git a/src/slalib/tpv2c.f b/src/slalib/tpv2c.f
new file mode 100644
index 0000000..7afe25d
--- /dev/null
+++ b/src/slalib/tpv2c.f
@@ -0,0 +1,83 @@
+      SUBROUTINE sla_TPV2C (XI, ETA, V, V01, V02, N)
+*+
+*     - - - - - -
+*      T P V 2 C
+*     - - - - - -
+*
+*  Given the tangent-plane coordinates of a star and its direction
+*  cosines, determine the direction cosines of the tangent-point.
+*
+*  (single precision)
+*
+*  Given:
+*     XI,ETA    r       tangent plane coordinates of star
+*     V         r(3)    direction cosines of star
+*
+*  Returned:
+*     V01       r(3)    direction cosines of tangent point, solution 1
+*     V02       r(3)    direction cosines of tangent point, solution 2
+*     N         i       number of solutions:
+*                         0 = no solutions returned (note 2)
+*                         1 = only the first solution is useful (note 3)
+*                         2 = both solutions are useful (note 3)
+*
+*  Notes:
+*
+*  1  The vector V must be of unit length or the result will be wrong.
+*
+*  2  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.
+*
+*  3  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 can be regarded as valid if the vector V02 is interpreted
+*     as the "over-the-pole" case.
+*
+*  4  This routine is the Cartesian equivalent of the routine sla_TPS2C.
+*
+*  P.T.Wallace   Starlink   5 June 1995
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL XI,ETA,V(3),V01(3),V02(3)
+      INTEGER N
+
+      REAL X,Y,Z,RXY2,XI2,ETA2P1,SDF,R2,R,C
+
+
+      X=V(1)
+      Y=V(2)
+      Z=V(3)
+      RXY2=X*X+Y*Y
+      XI2=XI*XI
+      ETA2P1=ETA*ETA+1.0
+      SDF=Z*SQRT(XI2+ETA2P1)
+      R2=RXY2*ETA2P1-Z*Z*XI2
+      IF (R2.GT.0.0) THEN
+         R=SQRT(R2)
+         C=(SDF*ETA+R)/(ETA2P1*SQRT(RXY2*(R2+XI2)))
+         V01(1)=C*(X*R+Y*XI)
+         V01(2)=C*(Y*R-X*XI)
+         V01(3)=(SDF-ETA*R)/ETA2P1
+         R=-R
+         C=(SDF*ETA+R)/(ETA2P1*SQRT(RXY2*(R2+XI2)))
+         V02(1)=C*(X*R+Y*XI)
+         V02(2)=C*(Y*R-X*XI)
+         V02(3)=(SDF-ETA*R)/ETA2P1
+         IF (ABS(SDF).LT.1.0) THEN
+            N=1
+         ELSE
+            N=2
+         END IF
+      ELSE
+         N=0
+      END IF
+
+      END
diff --git a/src/slalib/ue2el.f b/src/slalib/ue2el.f
new file mode 100644
index 0000000..d7187d9
--- /dev/null
+++ b/src/slalib/ue2el.f
@@ -0,0 +1,194 @@
+      SUBROUTINE sla_UE2EL (U, JFORMR,
+     :                      JFORM, EPOCH, ORBINC, ANODE, PERIH,
+     :                      AORQ, E, AORL, DM, JSTAT)
+*+
+*     - - - - - -
+*      U E 2 E L
+*     - - - - - -
+*
+*  Transform universal elements into conventional heliocentric
+*  osculating elements.
+*
+*  Given:
+*     U         d(13)  universal orbital elements (Note 1)
+*
+*                 (1)  combined mass (M+m)
+*                 (2)  total energy of the orbit (alpha)
+*                 (3)  reference (osculating) epoch (t0)
+*               (4-6)  position at reference epoch (r0)
+*               (7-9)  velocity at reference epoch (v0)
+*                (10)  heliocentric distance at reference epoch
+*                (11)  r0.v0
+*                (12)  date (t)
+*                (13)  universal eccentric anomaly (psi) of date, approx
+*
+*     JFORMR    i      requested element set (1-3; Note 3)
+*
+*  Returned:
+*     JFORM     d      element set actually returned (1-3; Note 4)
+*     EPOCH     d      epoch of elements (TT MJD)
+*     ORBINC    d      inclination (radians)
+*     ANODE     d      longitude of the ascending node (radians)
+*     PERIH     d      longitude or argument of perihelion (radians)
+*     AORQ      d      mean distance or perihelion distance (AU)
+*     E         d      eccentricity
+*     AORL      d      mean anomaly or longitude (radians, JFORM=1,2 only)
+*     DM        d      daily motion (radians, JFORM=1 only)
+*     JSTAT     i      status:  0 = OK
+*                              -1 = illegal combined mass
+*                              -2 = illegal JFORMR
+*                              -3 = position/velocity out of range
+*
+*  Notes
+*
+*  1  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.
+*
+*  2  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.
+*
+*  3  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
+*
+*  4  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
+*
+*  5  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
+*
+*  6  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.
+*
+*  References:
+*
+*     1  Sterne, Theodore E., "An Introduction to Celestial Mechanics",
+*        Interscience Publishers Inc., 1960.  Section 6.7, p199.
+*
+*     2  Everhart, E. & Pitkin, E.T., Am.J.Phys. 51, 712, 1983.
+*
+*  Called:  sla_PV2EL
+*
+*  P.T.Wallace   Starlink   18 March 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION U(13)
+      INTEGER JFORMR,JFORM
+      DOUBLE PRECISION EPOCH,ORBINC,ANODE,PERIH,AORQ,E,AORL,DM
+      INTEGER JSTAT
+
+*  Gaussian gravitational constant (exact)
+      DOUBLE PRECISION GCON
+      PARAMETER (GCON=0.01720209895D0)
+
+*  Canonical days to seconds
+      DOUBLE PRECISION CD2S
+      PARAMETER (CD2S=GCON/86400D0)
+
+      INTEGER I
+      DOUBLE PRECISION PMASS,DATE,PV(6)
+
+
+*  Unpack the universal elements.
+      PMASS = U(1)-1D0
+      DATE = U(3)
+      DO I=1,3
+         PV(I) = U(I+3)
+         PV(I+3) = U(I+6)*CD2S
+      END DO
+
+*  Convert the position and velocity etc into conventional elements.
+      CALL sla_PV2EL(PV,DATE,PMASS,JFORMR,JFORM,EPOCH,ORBINC,ANODE,
+     :               PERIH,AORQ,E,AORL,DM,JSTAT)
+
+      END
diff --git a/src/slalib/ue2pv.f b/src/slalib/ue2pv.f
new file mode 100644
index 0000000..be7b59f
--- /dev/null
+++ b/src/slalib/ue2pv.f
@@ -0,0 +1,215 @@
+      SUBROUTINE sla_UE2PV (DATE, U, PV, JSTAT)
+*+
+*     - - - - - -
+*      U E 2 P V
+*     - - - - - -
+*
+*  Heliocentric position and velocity of a planet, asteroid or comet,
+*  starting from orbital elements in the "universal variables" form.
+*
+*  Given:
+*     DATE     d       date, Modified Julian Date (JD-2400000.5)
+*
+*  Given and returned:
+*     U        d(13)   universal orbital elements (updated; Note 1)
+*
+*       given    (1)   combined mass (M+m)
+*         "      (2)   total energy of the orbit (alpha)
+*         "      (3)   reference (osculating) epoch (t0)
+*         "    (4-6)   position at reference epoch (r0)
+*         "    (7-9)   velocity at reference epoch (v0)
+*         "     (10)   heliocentric distance at reference epoch
+*         "     (11)   r0.v0
+*     returned  (12)   date (t)
+*         "     (13)   universal eccentric anomaly (psi) of date
+*
+*  Returned:
+*     PV       d(6)    position (AU) and velocity (AU/s)
+*     JSTAT    i       status:  0 = OK
+*                              -1 = radius vector zero
+*                              -2 = failed to converge
+*
+*  Notes
+*
+*  1  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.
+*
+*  2  The companion routine is sla_EL2UE.  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 sla_EL2UE 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 sla_EL2UE once, but then calling the present routine
+*     multiple times, which is faster than multiple calls to sla_PLANEL.
+*
+*     It is not obligatory to use sla_EL2UE to obtain the parameters.
+*     However, it should be noted that because sla_EL2UE performs its
+*     own validation, no checks on the contents of the array U are made
+*     by the present routine.
+*
+*  3  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).
+*
+*  4  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
+*     sla_EL2UE routine in fact produces coordinates with respect to the
+*     J2000 equator and equinox.
+*
+*  5  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.
+*
+*  P.T.Wallace   Starlink   19 March 1999
+*
+*  Copyright (C) 1999 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DATE,U(13),PV(6)
+      INTEGER JSTAT
+
+*  Gaussian gravitational constant (exact)
+      DOUBLE PRECISION GCON
+      PARAMETER (GCON=0.01720209895D0)
+
+*  Canonical days to seconds
+      DOUBLE PRECISION CD2S
+      PARAMETER (CD2S=GCON/86400D0)
+
+*  Test value for solution and maximum number of iterations
+      DOUBLE PRECISION TEST
+      INTEGER NITMAX
+      PARAMETER (TEST=1D-13,NITMAX=20)
+
+      INTEGER I,NIT,N
+
+      DOUBLE PRECISION 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
+
+
+
+*  Unpack the parameters.
+      CM = U(1)
+      ALPHA = U(2)
+      T0 = U(3)
+      DO I=1,3
+         P0(I) = U(I+3)
+         V0(I) = U(I+6)
+      END DO
+      R0 = U(10)
+      SIGMA0 = U(11)
+      T = U(12)
+      PSI = U(13)
+
+*  Approximately update the universal eccentric anomaly.
+      PSI = PSI+(DATE-T)*GCON/R0
+
+*  Time from reference epoch to date (in Canonical Days: a canonical
+*  day is 58.1324409... days, defined as 1/GCON).
+      DT = (DATE-T0)*GCON
+
+*  Refine the universal eccentric anomaly.
+      NIT = 1
+      W = 1D0
+      TOL = 0D0
+      DO WHILE (ABS(W).GE.TOL)
+
+*     Form half angles until BETA small enough.
+         N = 0
+         PSJ = PSI
+         PSJ2 = PSJ*PSJ
+         BETA = ALPHA*PSJ2
+         DO WHILE (ABS(BETA).GT.0.7D0)
+            N = N+1
+            BETA = BETA/4D0
+            PSJ = PSJ/2D0
+            PSJ2 = PSJ2/4D0
+         END DO
+
+*     Calculate Universal Variables S0,S1,S2,S3 by nested series.
+         S3 = PSJ*PSJ2*((((((BETA/210D0+1D0)
+     :                      *BETA/156D0+1D0)
+     :                      *BETA/110D0+1D0)
+     :                      *BETA/72D0+1D0)
+     :                      *BETA/42D0+1D0)
+     :                      *BETA/20D0+1D0)/6D0
+         S2 = PSJ2*((((((BETA/182D0+1D0)
+     :                  *BETA/132D0+1D0)
+     :                  *BETA/90D0+1D0)
+     :                  *BETA/56D0+1D0)
+     :                  *BETA/30D0+1D0)
+     :                  *BETA/12D0+1D0)/2D0
+         S1 = PSJ+ALPHA*S3
+         S0 = 1D0+ALPHA*S2
+
+*     Undo the angle-halving.
+         TOL = TEST
+         DO WHILE (N.GT.0)
+            S3 = 2D0*(S0*S3+PSJ*S2)
+            S2 = 2D0*S1*S1
+            S1 = 2D0*S0*S1
+            S0 = 2D0*S0*S0-1D0
+            PSJ = PSJ+PSJ
+            TOL = TOL+TOL
+            N = N-1
+         END DO
+
+*     Improve the approximation to PSI.
+         FF = R0*S1+SIGMA0*S2+CM*S3-DT
+         R = R0*S0+SIGMA0*S1+CM*S2
+         IF (R.EQ.0D0) GO TO 9010
+         W = FF/R
+         PSI = PSI-W
+
+*     Next iteration, unless too many already.
+         IF (NIT.GE.NITMAX) GO TO 9020
+         NIT = NIT+1
+      END DO
+
+*  Project the position and velocity vectors (scaling velocity to AU/s).
+      W = CM*S2
+      F = 1D0-W/R0
+      G = DT-CM*S3
+      FD = -CM*S1/(R0*R)
+      GD = 1D0-W/R
+      DO I=1,3
+         PV(I) = P0(I)*F+V0(I)*G
+         PV(I+3) = CD2S*(P0(I)*FD+V0(I)*GD)
+      END DO
+
+*  Update the parameters to allow speedy prediction of PSI next time.
+      U(12) = DATE
+      U(13) = PSI
+
+*  OK exit.
+      JSTAT = 0
+      GO TO 9999
+
+*  Null radius vector.
+ 9010 CONTINUE
+      JSTAT = -1
+      GO TO 9999
+
+*  Failed to converge.
+ 9020 CONTINUE
+      JSTAT = -2
+
+ 9999 CONTINUE
+      END
diff --git a/src/slalib/unpcd.f b/src/slalib/unpcd.f
new file mode 100644
index 0000000..9502671
--- /dev/null
+++ b/src/slalib/unpcd.f
@@ -0,0 +1,68 @@
+      SUBROUTINE sla_UNPCD (DISCO,X,Y)
+*+
+*     - - - - - -
+*      U N P C D
+*     - - - - - -
+*
+*  Remove pincushion/barrel distortion from a distorted [x,y]
+*  to give tangent-plane [x,y].
+*
+*  Given:
+*     DISCO    d      pincushion/barrel distortion coefficient
+*     X,Y      d      distorted coordinates
+*
+*  Returned:
+*     X,Y      d      tangent-plane coordinates
+*
+*  Notes:
+*
+*  1)  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.
+*
+*  2)  For pincushion distortion, C is +ve;  for barrel distortion,
+*      C is -ve.
+*
+*  3)  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
+*
+*  4)  The present routine is an approximate inverse to the
+*      companion routine sla_PCD, obtained from two iterations
+*      of Newton's method.  The mismatch between the sla_PCD and
+*      sla_UNPCD routines is negligible for astrometric applications;
+*      to reach 1 milliarcsec at the edge of the AAT triplet or
+*      Schmidt field would require field diameters of 2.4 degrees
+*      and 42 degrees respectively.
+*
+*  P.T.Wallace   Starlink   1 August 1994
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION DISCO,X,Y
+
+      DOUBLE PRECISION CR2,A,CR2A2,F
+
+
+
+      CR2=DISCO*(X*X+Y*Y)
+      A=(2D0*CR2+1D0)/(3D0*CR2+1D0)
+      CR2A2=CR2*A*A
+      F=(2D0*CR2A2*A+1D0)/(3D0*CR2A2+1D0)
+      X=X*F
+      Y=Y*F
+
+      END
diff --git a/src/slalib/v2tp.f b/src/slalib/v2tp.f
new file mode 100644
index 0000000..c072bc8
--- /dev/null
+++ b/src/slalib/v2tp.f
@@ -0,0 +1,78 @@
+      SUBROUTINE sla_V2TP (V, V0, XI, ETA, J)
+*+
+*     - - - - -
+*      V 2 T P
+*     - - - - -
+*
+*  Given the direction cosines of a star and of the tangent point,
+*  determine the star's tangent-plane coordinates.
+*
+*  (single precision)
+*
+*  Given:
+*     V         r(3)    direction cosines of star
+*     V0        r(3)    direction cosines of tangent point
+*
+*  Returned:
+*     XI,ETA    r       tangent plane coordinates of star
+*     J         i       status:   0 = OK
+*                                 1 = error, star too far from axis
+*                                 2 = error, antistar on tangent plane
+*                                 3 = error, antistar too far from axis
+*
+*  Notes:
+*
+*  1  If vector V0 is not of unit length, or if vector V is of zero
+*     length, the results will be wrong.
+*
+*  2  If V0 points at a pole, the returned XI,ETA will be based on the
+*     arbitrary assumption that the RA of the tangent point is zero.
+*
+*  3  This routine is the Cartesian equivalent of the routine sla_S2TP.
+*
+*  P.T.Wallace   Starlink   27 November 1996
+*
+*  Copyright (C) 1996 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL V(3),V0(3),XI,ETA
+      INTEGER J
+
+      REAL X,Y,Z,X0,Y0,Z0,R2,R,W,D
+
+      REAL TINY
+      PARAMETER (TINY=1E-6)
+
+
+      X=V(1)
+      Y=V(2)
+      Z=V(3)
+      X0=V0(1)
+      Y0=V0(2)
+      Z0=V0(3)
+      R2=X0*X0+Y0*Y0
+      R=SQRT(R2)
+      IF (R.EQ.0.0) THEN
+         R=1E-20
+         X0=R
+      END IF
+      W=X*X0+Y*Y0
+      D=W+Z*Z0
+      IF (D.GT.TINY) THEN
+         J=0
+      ELSE IF (D.GE.0.0) THEN
+         J=1
+         D=TINY
+      ELSE IF (D.GT.-TINY) THEN
+         J=2
+         D=-TINY
+      ELSE
+         J=3
+      END IF
+      D=D*R
+      XI=(Y*X0-X*Y0)/D
+      ETA=(Z*R2-Z0*W)/D
+
+      END
diff --git a/src/slalib/vdv.f b/src/slalib/vdv.f
new file mode 100644
index 0000000..eddeac2
--- /dev/null
+++ b/src/slalib/vdv.f
@@ -0,0 +1,27 @@
+      REAL FUNCTION sla_VDV (VA, VB)
+*+
+*     - - - -
+*      V D V
+*     - - - -
+*
+*  Scalar product of two 3-vectors  (single precision)
+*
+*  Given:
+*      VA      real(3)     first vector
+*      VB      real(3)     second vector
+*
+*  The result is the scalar product VA.VB (single precision)
+*
+*  P.T.Wallace   Starlink   November 1984
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL VA(3),VB(3)
+
+
+      sla_VDV=VA(1)*VB(1)+VA(2)*VB(2)+VA(3)*VB(3)
+
+      END
diff --git a/src/slalib/vn.f b/src/slalib/vn.f
new file mode 100644
index 0000000..e252867
--- /dev/null
+++ b/src/slalib/vn.f
@@ -0,0 +1,46 @@
+      SUBROUTINE sla_VN (V, UV, VM)
+*+
+*     - - -
+*      V N
+*     - - -
+*
+*  Normalizes a 3-vector also giving the modulus (single precision)
+*
+*  Given:
+*     V       real(3)      vector
+*
+*  Returned:
+*     UV      real(3)      unit vector in direction of V
+*     VM      real         modulus of V
+*
+*  If the modulus of V is zero, UV is set to zero as well
+*
+*  P.T.Wallace   Starlink   23 November 1995
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL V(3),UV(3),VM
+
+      INTEGER I
+      REAL W1,W2
+
+
+*  Modulus
+      W1=0.0
+      DO I=1,3
+         W2=V(I)
+         W1=W1+W2*W2
+      END DO
+      W1=SQRT(W1)
+      VM=W1
+
+*  Normalize the vector
+      IF (W1.LE.0.0) W1=1.0
+      DO I=1,3
+         UV(I)=V(I)/W1
+      END DO
+
+      END
diff --git a/src/slalib/vxv.f b/src/slalib/vxv.f
new file mode 100644
index 0000000..e0b9d93
--- /dev/null
+++ b/src/slalib/vxv.f
@@ -0,0 +1,39 @@
+      SUBROUTINE sla_VXV (VA, VB, VC)
+*+
+*     - - - -
+*      V X V
+*     - - - -
+*
+*  Vector product of two 3-vectors (single precision)
+*
+*  Given:
+*      VA      real(3)     first vector
+*      VB      real(3)     second vector
+*
+*  Returned:
+*      VC      real(3)     vector result
+*
+*  P.T.Wallace   Starlink   March 1986
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL VA(3),VB(3),VC(3)
+
+      REAL VW(3)
+      INTEGER I
+
+
+*  Form the vector product VA cross VB
+      VW(1)=VA(2)*VB(3)-VA(3)*VB(2)
+      VW(2)=VA(3)*VB(1)-VA(1)*VB(3)
+      VW(3)=VA(1)*VB(2)-VA(2)*VB(1)
+
+*  Return the result
+      DO I=1,3
+         VC(I)=VW(I)
+      END DO
+
+      END
diff --git a/src/slalib/wait.f_alpha_OSF1 b/src/slalib/wait.f_alpha_OSF1
new file mode 100644
index 0000000..8eb80e1
--- /dev/null
+++ b/src/slalib/wait.f_alpha_OSF1
@@ -0,0 +1,32 @@
+      SUBROUTINE sla_WAIT (DELAY)
+*+
+*     - - - - -
+*      W A I T
+*     - - - - -
+*
+*  Interval wait
+*
+*  !!! Version for: SPARC/SunOS4, 
+*                   SPARC/Solaris2, 
+*                   DEC Mips/Ultrix
+*                   DEC AXP/Digital Unix
+*                   Intel/Linux
+*                   Convex
+*
+*  Given:
+*     DELAY     real      delay in seconds
+*
+*  Called:  SLEEP (a Fortran Intrinsic on all obove platforms)
+*
+*  P.T.Wallace   Starlink   22 January 1998
+*
+*  Copyright (C) 1998 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL DELAY
+
+      CALL SLEEP(NINT(DELAY))
+
+      END
diff --git a/src/slalib/wait.f_convex b/src/slalib/wait.f_convex
new file mode 100644
index 0000000..8eb80e1
--- /dev/null
+++ b/src/slalib/wait.f_convex
@@ -0,0 +1,32 @@
+      SUBROUTINE sla_WAIT (DELAY)
+*+
+*     - - - - -
+*      W A I T
+*     - - - - -
+*
+*  Interval wait
+*
+*  !!! Version for: SPARC/SunOS4, 
+*                   SPARC/Solaris2, 
+*                   DEC Mips/Ultrix
+*                   DEC AXP/Digital Unix
+*                   Intel/Linux
+*                   Convex
+*
+*  Given:
+*     DELAY     real      delay in seconds
+*
+*  Called:  SLEEP (a Fortran Intrinsic on all obove platforms)
+*
+*  P.T.Wallace   Starlink   22 January 1998
+*
+*  Copyright (C) 1998 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL DELAY
+
+      CALL SLEEP(NINT(DELAY))
+
+      END
diff --git a/src/slalib/wait.f_ix86_Linux b/src/slalib/wait.f_ix86_Linux
new file mode 100644
index 0000000..8eb80e1
--- /dev/null
+++ b/src/slalib/wait.f_ix86_Linux
@@ -0,0 +1,32 @@
+      SUBROUTINE sla_WAIT (DELAY)
+*+
+*     - - - - -
+*      W A I T
+*     - - - - -
+*
+*  Interval wait
+*
+*  !!! Version for: SPARC/SunOS4, 
+*                   SPARC/Solaris2, 
+*                   DEC Mips/Ultrix
+*                   DEC AXP/Digital Unix
+*                   Intel/Linux
+*                   Convex
+*
+*  Given:
+*     DELAY     real      delay in seconds
+*
+*  Called:  SLEEP (a Fortran Intrinsic on all obove platforms)
+*
+*  P.T.Wallace   Starlink   22 January 1998
+*
+*  Copyright (C) 1998 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL DELAY
+
+      CALL SLEEP(NINT(DELAY))
+
+      END
diff --git a/src/slalib/wait.f_mips b/src/slalib/wait.f_mips
new file mode 100644
index 0000000..8eb80e1
--- /dev/null
+++ b/src/slalib/wait.f_mips
@@ -0,0 +1,32 @@
+      SUBROUTINE sla_WAIT (DELAY)
+*+
+*     - - - - -
+*      W A I T
+*     - - - - -
+*
+*  Interval wait
+*
+*  !!! Version for: SPARC/SunOS4, 
+*                   SPARC/Solaris2, 
+*                   DEC Mips/Ultrix
+*                   DEC AXP/Digital Unix
+*                   Intel/Linux
+*                   Convex
+*
+*  Given:
+*     DELAY     real      delay in seconds
+*
+*  Called:  SLEEP (a Fortran Intrinsic on all obove platforms)
+*
+*  P.T.Wallace   Starlink   22 January 1998
+*
+*  Copyright (C) 1998 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL DELAY
+
+      CALL SLEEP(NINT(DELAY))
+
+      END
diff --git a/src/slalib/wait.f_pcm b/src/slalib/wait.f_pcm
new file mode 100644
index 0000000..d79e78a
--- /dev/null
+++ b/src/slalib/wait.f_pcm
@@ -0,0 +1,66 @@
+      SUBROUTINE sla_WAIT (DELAY)
+*+
+*     - - - - -
+*      W A I T
+*     - - - - -
+*
+*  Interval wait
+*
+*  !!! PC only - Microsoft Fortran specific !!!
+*
+*  Given:
+*     DELAY     real      delay in seconds
+*
+*  A delay of up to 10000 seconds occurs.
+*
+*  Called:  GETTIM (Microsoft Fortran run-time library)
+*
+*  P.T.Wallace   Starlink   14 October 1991
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL DELAY
+
+      INTEGER IDELAY,IH,IM,IS,I,IT,IT0,IDT
+      LOGICAL FIRST,LOOP
+
+
+
+
+*  Convert requested delay to 0.01 second ticks
+      IDELAY=NINT(MAX(MIN(DELAY,1E4),0.0)*1E2)
+
+*  Set "note start time" flag
+      FIRST=.TRUE.
+
+*  Set "wait in progress" flag
+      LOOP=.TRUE.
+
+*  Main loop
+      DO WHILE (LOOP)
+
+*     Get the current time and convert to 0.01 second ticks
+         CALL GETTIM(IH,IM,IS,I)
+         IT=((IH*60+IM)*60+IS)*100+I
+
+*     First time through the loop?
+         IF (FIRST) THEN
+
+*        Yes: note the time and reset the flag
+            IT0=IT
+            FIRST=.FALSE.
+         ELSE
+
+*        No: subtract the start time, handling 0 hours wrap
+            IDT=IT-IT0
+            IF (IDT.LT.0) IDT=IDT+8640000
+
+*        If the requested delay has elapsed, stop looping
+            LOOP=IDT.LT.IDELAY
+         END IF
+      END DO
+
+      END
diff --git a/src/slalib/wait.f_sun4 b/src/slalib/wait.f_sun4
new file mode 100644
index 0000000..8eb80e1
--- /dev/null
+++ b/src/slalib/wait.f_sun4
@@ -0,0 +1,32 @@
+      SUBROUTINE sla_WAIT (DELAY)
+*+
+*     - - - - -
+*      W A I T
+*     - - - - -
+*
+*  Interval wait
+*
+*  !!! Version for: SPARC/SunOS4, 
+*                   SPARC/Solaris2, 
+*                   DEC Mips/Ultrix
+*                   DEC AXP/Digital Unix
+*                   Intel/Linux
+*                   Convex
+*
+*  Given:
+*     DELAY     real      delay in seconds
+*
+*  Called:  SLEEP (a Fortran Intrinsic on all obove platforms)
+*
+*  P.T.Wallace   Starlink   22 January 1998
+*
+*  Copyright (C) 1998 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL DELAY
+
+      CALL SLEEP(NINT(DELAY))
+
+      END
diff --git a/src/slalib/wait.f_sun4_Solaris b/src/slalib/wait.f_sun4_Solaris
new file mode 100644
index 0000000..8eb80e1
--- /dev/null
+++ b/src/slalib/wait.f_sun4_Solaris
@@ -0,0 +1,32 @@
+      SUBROUTINE sla_WAIT (DELAY)
+*+
+*     - - - - -
+*      W A I T
+*     - - - - -
+*
+*  Interval wait
+*
+*  !!! Version for: SPARC/SunOS4, 
+*                   SPARC/Solaris2, 
+*                   DEC Mips/Ultrix
+*                   DEC AXP/Digital Unix
+*                   Intel/Linux
+*                   Convex
+*
+*  Given:
+*     DELAY     real      delay in seconds
+*
+*  Called:  SLEEP (a Fortran Intrinsic on all obove platforms)
+*
+*  P.T.Wallace   Starlink   22 January 1998
+*
+*  Copyright (C) 1998 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL DELAY
+
+      CALL SLEEP(NINT(DELAY))
+
+      END
diff --git a/src/slalib/wait.f_vax b/src/slalib/wait.f_vax
new file mode 100644
index 0000000..1fd2e94
--- /dev/null
+++ b/src/slalib/wait.f_vax
@@ -0,0 +1,43 @@
+      SUBROUTINE sla_WAIT (DELAY)
+*+
+*     - - - - -
+*      W A I T
+*     - - - - -
+*
+*  Interval wait
+*
+*  !!! VAX/VMS specific !!!
+*
+*  Given:
+*     DELAY     real      delay in seconds
+*
+*  A delay 100ns < DELAY < 200s is requested.
+*
+*  P.T.Wallace   Starlink   14 October 1991
+*-
+
+      IMPLICIT NONE
+
+      REAL DELAY
+
+      INTEGER JSTAT
+      INTEGER SYS$SCHDWK,SYS$HIBER
+
+      INTEGER IDT(2)
+      DATA IDT(2)/-1/
+
+
+
+*  Encode delta time
+      IDT(1)=-NINT(MAX(1.0,1E7*MIN(200.0,DELAY)))
+
+
+*  Schedule a wakeup
+      JSTAT=SYS$SCHDWK(,,IDT,)
+      IF (.NOT.JSTAT) CALL LIB$STOP(%VAL(JSTAT))
+
+*  Hibernate
+      JSTAT=SYS$HIBER()
+      IF (.NOT.JSTAT) CALL LIB$STOP(%VAL(JSTAT))
+
+      END
diff --git a/src/slalib/wait.f_x86_64 b/src/slalib/wait.f_x86_64
new file mode 100644
index 0000000..8eb80e1
--- /dev/null
+++ b/src/slalib/wait.f_x86_64
@@ -0,0 +1,32 @@
+      SUBROUTINE sla_WAIT (DELAY)
+*+
+*     - - - - -
+*      W A I T
+*     - - - - -
+*
+*  Interval wait
+*
+*  !!! Version for: SPARC/SunOS4, 
+*                   SPARC/Solaris2, 
+*                   DEC Mips/Ultrix
+*                   DEC AXP/Digital Unix
+*                   Intel/Linux
+*                   Convex
+*
+*  Given:
+*     DELAY     real      delay in seconds
+*
+*  Called:  SLEEP (a Fortran Intrinsic on all obove platforms)
+*
+*  P.T.Wallace   Starlink   22 January 1998
+*
+*  Copyright (C) 1998 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      REAL DELAY
+
+      CALL SLEEP(NINT(DELAY))
+
+      END
diff --git a/src/slalib/xy2xy.f b/src/slalib/xy2xy.f
new file mode 100644
index 0000000..d830f44
--- /dev/null
+++ b/src/slalib/xy2xy.f
@@ -0,0 +1,49 @@
+      SUBROUTINE sla_XY2XY (X1,Y1,COEFFS,X2,Y2)
+*+
+*     - - - - - -
+*      X Y 2 X Y
+*     - - - - - -
+*
+*  Transform one [X,Y] into another using a linear model of the type
+*  produced by the sla_FITXY routine.
+*
+*  Given:
+*     X1       d        x-coordinate
+*     Y1       d        y-coordinate
+*     COEFFS  d(6)      transformation coefficients (see note)
+*
+*  Returned:
+*     X2       d        x-coordinate
+*     Y2       d        y-coordinate
+*
+*  The model relates two sets of [X,Y] coordinates as follows.
+*  Naming the elements of COEFFS:
+*
+*     COEFFS(1) = A
+*     COEFFS(2) = B
+*     COEFFS(3) = C
+*     COEFFS(4) = D
+*     COEFFS(5) = E
+*     COEFFS(6) = F
+*
+*  the present routine performs the transformation:
+*
+*     X2 = A + B*X1 + C*Y1
+*     Y2 = D + E*X1 + F*Y1
+*
+*  See also sla_FITXY, sla_PXY, sla_INVF, sla_DCMPF
+*
+*  P.T.Wallace   Starlink   5 December 1994
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION X1,Y1,COEFFS(6),X2,Y2
+
+
+      X2=COEFFS(1)+COEFFS(2)*X1+COEFFS(3)*Y1
+      Y2=COEFFS(4)+COEFFS(5)*X1+COEFFS(6)*Y1
+
+      END
diff --git a/src/slalib/zd.f b/src/slalib/zd.f
new file mode 100644
index 0000000..f3dd34f
--- /dev/null
+++ b/src/slalib/zd.f
@@ -0,0 +1,62 @@
+      DOUBLE PRECISION FUNCTION sla_ZD (HA, DEC, PHI)
+*+
+*     - - -
+*      Z D
+*     - - -
+*
+*  HA, Dec to Zenith Distance (double precision)
+*
+*  Given:
+*     HA     d     Hour Angle in radians
+*     DEC    d     declination in radians
+*     PHI    d     observatory latitude in radians
+*
+*  The result is in the range 0 to pi.
+*
+*  Notes:
+*
+*  1)  The latitude must be geodetic.  In critical applications,
+*      corrections for polar motion should be applied.
+*
+*  2)  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 zenith distance.  In particular,
+*      it may be important to distinguish between the zenith distance
+*      as affected by refraction, which would require the "observed"
+*      HA,Dec, and the zenith distance 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.
+*
+*  3)  No range checking of arguments is done.
+*
+*  4)  In applications which involve many zenith distance 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 perhaps sine and cosine of
+*      declination.
+*
+*  P.T.Wallace   Starlink   3 April 1994
+*
+*  Copyright (C) 1995 Rutherford Appleton Laboratory
+*-
+
+      IMPLICIT NONE
+
+      DOUBLE PRECISION HA,DEC,PHI
+
+      DOUBLE PRECISION SH,CH,SD,CD,SP,CP,X,Y,Z
+
+
+      SH=SIN(HA)
+      CH=COS(HA)
+      SD=SIN(DEC)
+      CD=COS(DEC)
+      SP=SIN(PHI)
+      CP=COS(PHI)
+      X=CH*CD*SP-SD*CP
+      Y=SH*CD
+      Z=CH*CD*CP+SD*SP
+      sla_ZD=ATAN2(SQRT(X*X+Y*Y),Z)
+
+      END