purpose of demonstration. It is also important to remember that when we first decided on our cuts, we based our selection on the 63 HGHH92 GCs and some of the brighter high-probability GCs from Rejkuba (2001). We did not have a sample of confirmed foreground stars until after our first spectroscopic run. Results from each observing run were used to improve the selection for subsequent runs.

[ll|c|ccccc|c]{} AAO/2dF & 2001 Jan 20 & 120 & 2 & 0 & 0 & 0 & 0 & 28\
CTIO/Hydra & 2001 Feb 18–20 & 254 & 88 & 2 & 28 & 4 & 6 & 7\
AAO/2dF & 2002 Apr 4–6, 9–10 & 59 & 19 & 0 & 0 & 0 & 0 & 8\

The GCs are clearly in a locus offset from the stars. This morphological selection bias has been built into the sample—most known GCs in earlier work and our study were selected at least in part because of their spatial extent—yet it shows that at least some GCs can be separated from stars given the seeing in our images. Not all stars are concentrated at (1,1), as there is a tail of stars to higher FWHM. 