  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.
