the most likely ones to be cluster members) do not have reported apparent magnitudes in the SDSS CAS. To circumvent this limitation as much as possible, we have instead performed crowded field photometry for the center of the clusters, using the DAOPHOT/ALLFRAME suite of programs (Stetson 1987; Stetson 1994) in IRAF[^1]. A full description of the methods used and the photometric measures obtained is provided by Johnson et al. (2007). Briefly, DAOPHOT was run on each image, and the five images of each field (one for each filter) were then simultaneously run through ALLFRAME. DAOGROW (Stetson 1990) was used to derive aperture corrections to the point-spread-function photometry for the SDSS aperture radius of 7.4 arcsecs. Finally, the zeropoint term from the [*tsField*]{} files was applied to calibrate the data. This procedure also permits a check on the techniques used by the SDSS PHOTO pipeline in regions outside the cluster where the areal density of sources on the sky is sufficiently low that it may be used.

After completing the above procedures, we finally combine the results from the PHOTO pipeline with those from the crowded-field photometry to obtain an almost complete catalog of $ugriz$ photometry for stars in the region 