for PNe, was performed on the GC spectra.

Also unlike in the case of PNe, we performed radial velocity measurements on GCs using the Fourier cross-correlation method implemented in the [fxcor]{} task of the IRAF radial velocity package. During our CTIO-Hydra run, we observed the radial velocity standard HR 5196, which has a published velocity of $-39.598$ [km s$^{-1}$]{} (Skuljan, Hearnshaw, & Cottrell 2000), but stars are not always optimal templates for cross-correlating with globular clusters. We used HR 5196 to check the velocity of a high S/N Keck spectrum of an M31 GC, and we subsequently used this GC as our velocity template.

Target Selection: Morphology
----------------------------

Even with the 400 fibers on 2dF and the 130 fibers on Hydra, we cannot take a spectrum of every object in the expected magnitude range. Thus, it is important that we develop an efficient algorithm to select likely GCs. We developed our target selection algorithm using structural parameters and colors. With the best seeing in each field being nearly $1\arcsec$, it is possible to resolve some of the more extended GCs in our imaging. We use two structural parameters, sharpness and full-width at half maximum (FWHM), in conjunction with ellipticity to 