First, I congratulate you and all Skycat designers and programmers because
it has been -at least for me- a very useful tool.

My question is the following:

Now I'm working on astrometric and limiting magnitude improvements that
bayesian reconstruction algorithms incorporate. In order to locate
automatically the stars of the image, I use IRAF package called DAOPHOT.
This one has a routine called 'daofind', that generates an output like this:

#K IRAF = NOAO/IRAFV2.10EXPORT version %-23s
#K USER = octavi name %-23s
#K HOST = fajnm1 computer %-23s
#K DATE = 09-19-97 mm-dd-yr %-23s
#K TIME = 12:02:03 hh:mm:ss %-23s
#K PACKAGE = apphot name %-23s
#K TASK = daofind name %-23s
#
#K SCALE = 1.19 units %-23.7g
#K FWHMPSF = 4.16 scaleunit %-23.7g
#K EMISSION = yes switch %-23b
#K DATAMIN = INDEF counts %-23.7g
#K DATAMAX = INDEF counts %-23.7g
#K EXPOSURE = "" keyword %-23s
#K AIRMASS = "" keyword %-23s
#K FILTER = "" keyword %-23s
#K OBSTIME = "" keyword %-23s
#
#K NOISE = poisson model %-23s
#K SIGMA = 2.817 counts %-23.7g
#K GAIN = GAIN keyword %-23s
#K EPADU = 4.07 e-/adu %-23.7g
#K CCDREAD = RDNOISE keyword %-23s
#K READNOISE = 4.9 e- %-23.7g
#
#K IMAGE = ../../f96d312.108_t_ori imagename %-23s
#K FWHMPSF = 4.16 scaleunit %-23.7g
#K THRESHOLD = 4. sigma %-23.7g
#K NSIGMA = 1.5 sigma %-23.7g
#K RATIO = 1. number %-23.7g
#K THETA = 0. degrees %-23.7g
#
#K SHARPLO = 0.2 number %-23.7g
#K SHARPHI = 1. number %-23.7g
#K ROUNDLO = -1. number %-23.7g
#K ROUNDHI = 1. number %-23.7g
#
#N XCENTER YCENTER MAG SHARPNESS SROUND GROUND ID \
#U pixels pixels # # # # # \
#F %-13.3f %-10.3f %-9.3f %-12.3f %-12.3f %-12.3f %-6d \
#
367.152 5.504 -2.616 0.453 0.294 0.176 1
319.928 8.802 -0.076 0.352 -0.506 -0.537 2
65.968 16.768 -0.631 0.509 0.134 0.100 3
187.129 23.329 -0.183 0.265 0.114 0.109 4
944.462 27.992 -0.590 0.306 -0.315 -0.019 5
645.943 32.781 -0.108 0.396 0.310 0.290 6
172.217 37.837 -3.943 0.513 0.007 0.010 7
69.953 45.869 -3.555 0.492 0.059 -0.026 8
993.736 49.312 -3.161 0.492 -0.060 -0.033 9
276.782 73.810 -3.160 0.496 0.168 0.027 10
27.206 75.972 -0.492 0.316 0.613 0.230 11
722.087 91.526 -1.894 0.506 -0.213 0.153 12
820.559 116.932 -6.815 0.464 0.039 -0.123 13

The interesting columns are XCENTER and YCENTER.

What I want to do is to represent these (X,Y) image coordinates over a FITS
image with WCS support, which have an on-line catalog query plotted over,
too. How can I do this?

Thanks in advance,

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Octavi Fors Aldrich

Astronomy Department
Physics Faculty
Diagonal Av., 647
08028 Barcelona
SPAIN

octavi@fajnm1.am.ub.es

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