velocity, or it appears spurious (i.e., falls outside of the range $\pm 1000$ km s$^{-1}$), we simply ignore the star in subsequent analyses. A more detailed description of the procedures used for determination of the best available radial velocity, and of zero-point offsets of the radial velocities, can be found in Paper I.

Membership Selection from the Spectroscopic Samples
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Owing to an insufficient number of stars with available spectroscopy for each cluster, it is not possible to obtain a well-defined Color Magnitude Diagram (CMD) based solely on spectroscopically confirmed member stars. Thus, we make use of photometric data in the field of each cluster, and describe below how we obtain a relatively clean CMD for individual clusters, and select likely member stars from the spectroscopic data.

Likely Member Star Selection for Globular Clusters
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One of the primary issues that one needs to address when creating a CMD, or selecting likely member stars, for a star cluster is removal of contamination from field stars. In order to approximately isolate the likely cluster members from the field stars we have made use of the CMD mask algorithm described by Grillmair et al. (1995). We illustrate the basic idea by application 