However, for this cluster, many candidate members with positions, magnitudes, and colors from the WEBDA (http: //www.univie.ac.at/webda/) catalogs were added to the target lists. The bright targets (with $r < 14$) saturate the SDSS imaging camera, so these were added from the literature (Sanders 1989; Fan et al. 1996). Such bright stars normally saturate a regular SDSS spectroscopic exposure, so there were exposed for shorter than normal. About 200 very bright stars between about 12 $<$ $g$ $<$ 14 were targeted.

In total, we obtained SDSS spectroscopy for 1920, 1280, 640, 1280, and 640 targets, including sky spectra and calibration object spectra, in the fields of M 13, M 15, M 2, NGC 2420, and M 67 respectively. The reduced spectra were then processed through the SSPP in order to estimate $T_{\rm eff}$, log $g$, and \[Fe/H\], among other quantities. Table 1 summarizes the global properties of the clusters under consideration in this paper, taken from the compilation of Harris (1996) for the globular clusters and from WEDBA or Gratton (2000) for the open clusters.

Radial Velocities
-----------------

There are two estimated radial velocities provided from the SDSS spectroscopic pipeline. One is an absorption redshift obtained by cross-correlating the spectra 