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