Globular Clusters as Probes of the Virgo gE NGC 4472

We present radial velocities for 144 globular clusters around the Virgo gE NGC 4472 (M49), and ages and metallicities from co-added spectra of 131 clusters. We confirm our earlier finding that the metal-poor clusters have a significantly higher velocity dispersion than the metal-rich clusters, and we find little or no rotation in the metal-rich clusters. The velocity dispersion profile is consistent with isotropic orbits for the clusters and the NGC 4472 mass distribution inferred from X-ray data. Our sample of clusters spans a metallicity range of -1.6 < [Fe/H] < 0 dex. The metal-poor and metal-rich cluster populations are coeval within the errors, and all clusters are older than 6 Gyr at 95% confidence. Our findings are consistent with a merger origin for NGC 4472, but other elliptical formation models cannot be ruled out.