ASTXY2RD

Name

astxy2rd

Purpose

Astrometry conversion from image (x,y) to ($\alpha$,$\delta$)

Description

This transformation can either be based on a simple linear transformation
with rotation from the celestial sphere to linear CCD chip coordinates.
Or, it can use a full astrometric solution (including linear). The
simple linear transformation is only an approximate treatment and
will not work for very large fields. The best results will come from
the full-up treatment.

Calling Sequence

astxy2rd,x,y,info,ra,dec

Inputs

x - X coordinate in image
y - Y coordinate in image
info - Transformation information held in an anonymous structure. There
are two different groups of tags that can appear. The original
simple linear transformation needs the following tags:
pscale - Plate scale (arcsec/pixel).
rang - Rotation angle of image (radians).
xflip - -1 if image flipped in X, 1 if not.
yflip - -1 if image flipped in Y, 1 if not.
The full-up transformation requires a different set of tags:
renormfac - normalization factor
cxi - xi transformations coefficients (x,y -> xi)
ceta - eta transformations coefficients (x,y -> eta)
terms - list of terms to fit
prot - Rotation to get to standard coordinates (radians)
Both types need the following.
xcref - X center of image.
ycref - Y center of image.
raref - Right ascension of center of image (tangent plane).
decref - Declination of center of image (tangent plane).

Optional Input Parameters

Keyword Input Parameters

FULL - Flag, if set indicates the full transformation should be used.
Only the tags needed must be provided.

Outputs

ra - Right ascension (radians)
dec - Declination (radians)

Keyword Output Parameters

DX - Internal transformed x value (normalized for /full)
DY - Internal transformed y value (normalized for /full)
XI - tangent plane coordinate (arcsec)
ETA - tangent plane coordinate (arcsec)

Common Blocks

Side Effects

Restrictions

Procedure

The following applies to the /FULL conversion.
The solution is a two-step conversion. You start with raw coordinates
that typically relate to the original position in the native coordinate
system for the device. The first transformation step is to convert
to another system related to the first by a translation and rotation.
e.g. xp = ( (x-xc)*cos(prot) + (y-yc)*sin(prot) ) / renormfac
yp = ( -(x-xc)*sin(prot) + (y-yc)*cos(prot) ) / renormfac
The astrometric transformation then maps xp,yp to ra,dec.

Modification History

1997/04/05 - Written by Marc W. Buie, Lowell Observatory
2009/06/22, MWB added full-up transformation and changed the simple
linear transformation to use xi/eta tangent plane
2009/08/05, MWB, modified full transformation to include a coordinate
rotation, this requires an extra tag in info structure.
2009/11/02, MWB, split off most of code into astxy2sn