region near the dust lane. Rejkuba (2001) showed what is possible with excellent (06) seeing and 8-meter telescopes when she used imaging taken at the Very Large Telescope to define a sample of fainter GC candidates based on their resolved appearance in two $7\arcmin\times7\arcmin$ fields. Only with the availability of mosaic cameras are CCD studies now able to cover an area comparable to the photographic studies of the 1980s. Recent programs include this one and an imaging study using the Big Throughput Camera on the CTIO 4-meter (G.Harris & W.Harris 2003) with the Washington photometric system (Canterna 1976).

Unfortunately, [NGC 5128]{}’s nearness and relative proximity to the Galactic bulge and disk ($l=309\fdg5$, $b=+19.4$) conspire to make GC studies difficult. At the distance of [NGC 5128]{}, $1\arcmin = 1.02$ kpc, which means that [NGC 5128]{}’s halo subtends over two degrees of sky. The density of foreground stars is also high, such that even in the central regions, all but a few percent of objects within the magnitude range expected for [NGC 5128]{} GCs are actually stars in our own Milky Way. Spectroscopic follow-up to obtain radial velocities is the only way to confidently identify true GCs. It is only with the 