observations do not go as deep as the VLT data. There is a $\sim0.14$ mag offset between the two systems (our magnitudes are fainter), with $\sim0.3$ mag RMS scatter. If significant, this difference could be a result of slightly different calibrations or aperture corrections. Globular clusters at the distance of [NGC 5128]{} may also be slightly extended in appearance. Because our aperture corrections are derived from stellar profiles, we may underestimate the total flux of the more extended GCs by as much as $\sim0.1$ mag, although a more typical value would be $\sim0.06$ mag. However, this effect is much smaller on GC colors since the seeing did not vary much across most of our observations. Because the science goals of this study focused mostly on the relative colors of the GCs, we chose to defer a more precise treatment of GC light profiles to a later study.

[llcclcl]{} PN/GC & AAO/2dF & 120 & 400 & 1200B & 2.2 & 2001 Jan 20\
PN/GC & CTIO/Hydra & 40 & 130 & KPGL3 & 4.9 & 2001 Feb 18–20\
PN/GC & AAO/2dF & 120 & 400 & 1200V & 2.2 & 2002 Apr 4–6, 9–10\

Comparisons with the [*UBVR*]{} photoelectric photometry 