literature. The central cores of the clusters were not targeted because the PHOTO pipeline does not resolve the very crowded fields into single star detections, and also due to limitations on the separations of the fibers during the spectroscopic follow-up stage. The primary method for selecting member candidates was performed by plotting a photometric CMD for a given cluster, and choosing stars from regions of this diagram that correspond to location on the MS turnoff or RGB of the cluster. An additional list of bright stars for M 15 and M 2 with previously available proper motions consistent with membership in the clusters was provided by Cudworth (1976 and private communication) and Cudworth $\&$ Rauscher (1987). Other stars in the fields of these clusters were used to fill spectroscopic fibers using the default SEGUE target selection algorithm (Adelman-McCarthy et al. 2007b). While many of these additional targets turned out to be stars from the general field populations, a significant fraction turned out serendipitously to be members of the clusters.

For M 13, three specially designed plates were obtained. Two of the three plates followed the standard SEGUE target selection procedure (Adelman-McCarthy et al. 2007b) of sampling stars with a variety 