These subroutines extract parameters from FITS headers and use the
resulting data structure to convert image pixel coordinates to sky
coordinates and vice versa. They are used in several image viewing
programs and so are distributed separately in wcssubs as well as in libwcs.a
Subroutines to implant values into FITS headers by keyword (and to
delete headers).
dsspos.c
dsspos( ) uses the WCS structure to compute sky coordinates given
image pixel X and Y for images with Digitized Sky Survey plate solutions
in their headers. dsspix( ) uses the WCS structure to compute image
pixel X and Y given sky coordinates for DSS images. (Algorithms from
StSCI CASB)
platepos.c
platepos( ) uses the WCS structure to compute sky coordinates given
image pixel X and Y for images with polynomial plate solutions
in their headers. dsspix( ) uses the WCS structure to compute image
pixel X and Y given sky coordinates for those images.
tnxpos.c
tnxpos( ) uses the WCS structure to compute sky coordinates given
image pixel X and Y for images with IRAF polynomial plate solutions
in their headers. tnxpix( ) uses the WCS structure to compute image
pixel X and Y given sky coordinates for those images. (Algorithms
from Lindsey Davis, NOAO)
Subroutines for extracting WCS information from a FITS image header.
wcslib.c lin.c cel.c proj.c wcstrig.c sph.c
WCSLIB subroutines for 26 proposed FITS standard projections by
Mark Calabretta of CSIRO.
worldpos.c
worldpos( ) uses the WCS structure to compute sky coordinates given
image pixel X and Y for images with header information for any of 8
standard world coordinate systems. worldpix( ) uses the WCS structure
to compute image pixel X and Y given sky coordinates for the same images.
(Mostly from NRAO)
fitshead.h
Declarations of FITS header and image access subroutines and FITS
table data structure.
