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New radial velocity measurements for previously known and newly confirmedglobular clusters (GCs) in the nearby massive galaxy NGC 5128 are presented. Wehave obtained spectroscopy from LDSS-2/Magellan, VIMOS/VLT, and Hydra/CTIO fromwhich we have measured the radial velocities of 218 known, and identified 155new, GCs. The current sample of confirmed GCs in NGC 5128 is now 605 with 564of these having radial velocity measurements. We have performed a new kinematicanalysis of the GC system that extends out to 45 arcmin in galactocentricradius. We have examined the systemic velocity, projected rotation amplitudeand axis, and the projected velocity dispersion of the GCs as functions ofgalactocentric distance and metallicity. Our results indicate that themetal-poor GCs have a very mild rotation signature of (26 pm 15) km/s. Themetal-rich GCs are rotating with a higher, though still small signature of (43pm 15) km/s around the isophotal major axis of NGC 5128 within 15 arcmin. Theirvelocity dispersions are consistent within the uncertainties and the profilesappear flat or declining within 20 arcmin. We note the small sample ofmetal-rich GCs with ages less than 5 Gyr in the literature appear to havedifferent kinematic properties than the old, metal-rich GC subpopulation. Themass and mass-to-light ratios have also been estimated using the GCs as tracerparticles for NGC 5128. Out to a distance of 20 arcmin, we have obtained a massof (5.9 pm 2.0) x 10^(11) M_(sun) and a mass-to-light ratio in the B-band of 16M_(sun)/L_(B,sun). Combined with previous work on the ages and metallicities ofits GCs, as well as properties of its stellar halo, our findings suggest NGC5128 formed via hierarchical merging over other methods of formation, such asmajor merging at late times.

The Kinematics of the Globular Cluster System of NGC 5128 with a New, Large Sample of Radial Velocity Measurements