|The same techniques for determining completeness on the deep field
have been applied to the wide field. The results (tenative until the final
images are available) are quite similar.
|The completeness of the deep field has tested already. The technique
and the results are described here. This page
examines the wide field.
A 1024x1024 subsection was chopped out of the wide field. It was selected
to have uniform weighting and to not have too many saturated stars.
Currently, only the I band image is available. Therefore, the chi-squared technique of galaxy detection cannot be used.
|The following graphs are plots of surface brightness in the I band vs. total I magnitude. The black dots show detected galaxies. The red numbers give the completeness levels (in percent) at different values of magnitude and surface brightness as determined from the simulations. The blue lines are contours at the 90%, 70% and 50% completeness limits. These contours bound the detected galaxies on both the the total magnitude and peak surface brightness edges. The join between these two bounds takes a variety of shapes, but is generally not a right angle. The green dots show the false-positive detections. The magenta line shows the locus of point-sources in the I - µI plane. The line was made by identify a few stars in the image and plotting their magnitudes and surface brightnesses. The I - µI values for these stars are simply connected (join-the-dots). This locus seems fairly well defined|
|The detection criteria for the graphs to the right are: 3 contiguous pixels in the I band image must be greater than 0.7 times the RMS of the background.|
|The detection criteria for the graph to the right are: 3 contiguous pixels in the I band image must be greater than 1.0 times the RMS of the background.|
|The detection criteria for the graph to the right are: 3 contiguous pixels in the I band image must be greater than 2.0 times the RMS of the background.|