of Zickgraf [et al. ]{}(1990) show that our photometry is consistent with their published values. We also checked against the list of confirmed GCs in HGHH92 and other previous work. This sample is considerably brighter than that of Rejkuba (2001) and we detect all known GCs that are in our field of view.

Building a Catalog of Globular Clusters
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A Spectroscopic Survey
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Determining which of our detected objects are actually GCs in [NGC 5128]{} is a non-trivial task. While the total number of GCs in [NGC 5128]{} is estimated to be 1200–1900 (G.Harris [et al. ]{}1984), there are 17,407 unique objects in our catalog that fall in the magnitude range that corresponds to the bright half of the globular cluster luminosity function (GCLF) $14.0<V<20.5$. Our faint end cut off for spectroscopy is approximately the magnitude of the GCLF peak, yet we estimate that only 3–$6\%$ of objects in this magnitude range are GCs. With such a high level of contamination from foreground stars (background galaxies are not so important at these relatively bright magnitudes), it is difficult to know which objects are really GCs.

Some of the more extended GCs will be resolved in our ground-based imaging (at 