be stellar (i.e., a *point source*), or not (an *extended* source) are obtained. Afterwards, the photometric data are further calibrated by matching to brighter known standards observed with a smaller calibration telescope on Apache Point (Hogg et al. 2001; Smith et al. 2002; Tucker et al. 2006). The processed photometric data have been shown to exhibit 2% relative and absolute errors (0.02 magnitudes) in $g$, $r$, and $i$, and $3 \%-5 \%$ errors in $u$ and $z$ for all stellar objects brighter than $g = 20$ (Stoughton et al. 2002; Abazajian et al. 2004, 2005; Ivezic et al. 2004). The first-pass photometric data for each of the clusters used in the present study were secured by querying the DR-3 (Abazanjian et al. 2005), DR-5 (Adelman-McCarthy et al. 2007a), and DR-6 (Adelman-McCarthy et al. 2007b) releases from the SDSS Catalog Archive Server (CAS).

Figure 1 illustrates one of the primary challenges in working with data for clusters obtained with SDSS – the automated PHOTO pipeline (Lupton et al. 2001) was not designed to adequately deal with crowded fields such as the central regions of globular clusters. As a result, essentially all of the stars in this region (which are by definition 