not perfect, there is a clear separation between GCs and stars in $UVI$ color space—at a given [$U$–$V$]{}, GCs are redder in [$V$–$I$]{}. $U$-band photometry, though expensive, is valuable for the separation of GCs from stars.

Spectroscopic Yields
--------------------

The results of these three spectroscopic runs are summarized in Table \[table:gcresults\]. The total numbers of clusters listed will be larger than the numbers in the final catalog because some were observed in multiple runs. We took slightly different targeting strategies in each run. For the first 2dF observations, GC candidates were piggybacked onto observations of PNe. PNe had the highest priority while GC candidates were used to fill empty fibers in the uncrowded halo regions. Most of these candidates were in the NE field, and we used only broad color cuts, no morphology cuts, and a magnitude limit of $V<20$. This selection produced very few new GCs (only a 2% yield), because the color cut included a large portion of the stellar locus, and the candidates were restricted being the NE halo field where the density of GCs is low. Our three night Hydra run also combined PNe and GCs, although GCs received the higher priority. This time, we implemented 