the distance of [NGC 5128]{}, $1\arcsec\approx17~$pc); W.Harris [et al. ]{}(2002) used HST imaging to determine that GCs in [NGC 5128]{} have characteristic half-light radii of $0\farcs3-1\farcs0$. While size and morphology can be used as leverage in selecting high-probability GCs, radial velocities are the best way to distinguish between GCs and foreground stars. The systemic velocity of [NGC 5128]{} is 541 [km s$^{-1}$]{}  (Hui [et al. ]{}1995), which means that most GCs will have radial velocities larger than those of Galactic stars. The central stellar velocity dispersion of [NGC 5128]{} is $\sim140$ [km s$^{-1}$]{} (Wilkinson [et al. ]{}1986). Assuming that the GC system has a gaussian line-of-sight velocity distribution with a similar dispersion, introducing a velocity cutoff at $v_r>250$ [km s$^{-1}$]{} excludes only the lowest $1.9\%$ of the GC velocity distribution. The PN radial velocity distribution is consistent with this, as only eight of 780 PNe in [NGC 5128]{} ($1.0\%$) have $v_r < 250$ (Peng, Ford, & Freeman 2004). Even at this velocity cutoff, however, there is a chance that a few high-velocity Galactic halo stars will contaminate our sample. The sun’s direction of motion in the disk is generally away from [NGC 5128]{}, so the velocity conversion from the the 