with templates that were obtained from SDSS commissioning spectra (Stoughton et al. 2002). Another comes from matching the spectra with ELODIE template spectra (Prugniel $\&$ Soubiran 2001). In most cases the velocity based on the ELODIE template matches appears to be the best available estimate, as spectra of “quality assurance” stars with multiple measurements show the most repeatable values for this estimator. However, this is not always the case. We proceed to select the best available velocity in the following manner. If the velocity determined by comparison with the ELODIE templates has a reported error of 20 km s$^{-1}$ or less then this velocity is adopted. If the error from the ELODIE template comparison is larger than 20 km s$^{-1}$, and the relative offset between the two radial velocities is less than 40 km s$^{-1}$, we take an average of the two. If none of the criteria above are satisfied, which happens only rarely, and mainly for quite low $S/N$ spectra, or for hot/cool stars without adequate templates, we obtain the calculated radial velocity from a custom routine that examines the wavelengths of a number of prominent absorption features. If none of these methods yield a reasonable estimate of radial 