Zirm, Dickinson, & Dey 2003).

Some of the early work on extragalactic GCs was done in [NGC 5128]{}. Noting a slightly diffuse 17th magnitude object on photographic plates, Graham & Phillips (1980; GP80) obtained follow-up spectroscopy and identified the first GC in this galaxy. Five more GCs were confirmed by van den Bergh, Hesser, & G.Harris (1981; VHH81). Using [*UVR*]{} star counts, G.Harris, Hesser, H.Harris, & Curry (1984) estimated that the total cluster population in [NGC 5128]{} is 1200–1900. Subsequent spectroscopic work (Hesser, H.Harris, & G.Harris 1986 \[HHH86\]; Sharples 1988) increased the number of GCs with radial velocities. Finally, G.Harris [et al. ]{}(1992; HGHH92) obtained CCD photometry on the Washington system for 62 confirmed GCs. This study produced one of the best GC system metallicity distributions at the time, and was later cited by Zepf & Ashman (1993) as evidence for bimodality.

Since then, the relatively small fields of view of modern detectors have forced studies to concentrated on the inner regions of the [NGC 5128]{} GC system. Minniti [et al. ]{}(1996; MAGJM96) used infrared imaging to identify possible intermediate-age, metal-rich GCs. Holland, Côté, & Hesser (1999; HCH99) used HST WFPC2 imaging to identify spatially resolved GC candidates in the 