Command Line Arguments

filename	Name of FITS or IRAF image file. This must be present.
-a rotation angle	WCS rotation angle in degrees. This angle is used in the nominal plane tangent WCS used to match references stars with image stars. (default 0)
-b RA Dec	Center right ascension and declination in degrees or sexigesimal in B1950 (FK4). Sexigesimal coordinates are hours:minutes:seconds degrees:minutes:seconds. This center is used in the nominal plane tangent WCS used to match references stars with image stars. (default `RA`, `DEC`, and `EPOCH` keywords in the image header).
-c name	Reference catalog (`GSC`, `UJC`, `UAC`, or Starbase table filename)
-d name	Use this DAOFIND-format output catalog of X, Y, and magnitude instead of searching for stars in the image. The format is simply white-space-separated numbers on a line, with # at the beginning of comment lines. The fourth and later columns are ignored.
-g class	Guide Star Catalog object class (-1=all,0,3 (default -1)
-h number	Maximum number of reference stars to use (10-200, default 25).
-i value	Set the minimum peak value for a star in image. If value is less than zero, the minimum peak is -value image pixel standard deviations. Setting this number rejects faint stars early in the selection process for a significant saving in computing time.
-j RA Dec	Center right ascension and declination in degrees or sexigesimal in J2000 (FK5). Sexigesimal coordinates are hours:minutes:seconds degrees:minutes:seconds. This center is used in the nominal plane tangent WCS used to match references stars with image stars. (default `RA`, `DEC`, and `EPOCH` keywords in the image header).
-l	Reflect image left <-> right before rotating and fitting WCS
-m faint [bright]	Initial reference star faint limiting magnitude, if only one number is given, or magnitude range, if two numbers are given. Order does not matter.
-p plate scale	Initial plate scale in arcseconds per pixel. This is used when matching image and reference stars and as an initial value for the fit. (default `SECPIX` or `SECPIX1` and `SECPIX2` keywords in the image header). (default 0)
-q	Fit polynomial image magnitude to catalog magnitude conversion, writing the coefficients at the bottom of the residual plot where they may be retrieved by xy2sky using its -c command. (added in WCSTools 3.0.1)
-r rotation angle	Rotate by this angle in degrees before fitting WCS. It must be a multiple of 90 degrees. (default 0)
-s fraction	If there are more image stars (`ni`) than reference stars found in the image area (`nr`), match the `nr` reference stars against fraction * `ni` image stars. If there are more reference stars found in the image area than stars found in the images, match fraction * `nr` reference stars against `ni` image stars.
-t offset tolerance	Offset tolerance in pixels (default 20)
-u plate number	When using a USNO Catalog, accept reference star positions from this plate only
-v	print more information about process
-x Xref Yref	Pixel coordinates of the reference pixel used in the WCS projection
-y frac	Multiply image dimensions by this for search (default 1.0)

Last updated 25 July 2001 by Doug Mink dmink@cfa.harvard.edu