  We present recent multi-object spectroscopy of globular clusters in the Virgo
gEs M49 and M87. In M49, we have a total of 144 confirmed clusters out to 8
arcmin radius (~6 R_eff or 35 kpc). We find that the blue (metal-poor) clusters
have both a higher velocity dispersion and rotation than the red (metal-poor)
clusters. For the metal-rich population we place an upper limit of
(v/sigma)_proj < 0.34 at 99% confidence. We calculate the velocity dispersion
as a function of radius, and show that this is consistent with isotropic
cluster orbits and the M49 mass distribution determined from X-ray data. For
M87, we combine new CFHT data with previous data to obtain a total sample of
278 clusters out to 10 arcmin radius (~45 kpc). We find a similar global
rotation for the metal-poor and metal-rich clusters of 160-170 km/sec. Beyond ~
2 R_eff (15 kpc), both the metal-poor and metal-rich clusters appear to rotate
about the photometric minor axis. The combined cluster sample is consistent
with isotropic orbits, but when considered separately, the metal-poor clusters
show significant tangential bias of beta_cl ~ -0.4, while the metal-rich
clusters show a radial bias with beta_cl ~ +0.4. In both galaxies, the
metal-rich and metal-poor clusters share different kinematics, but there is no
clear preference for any one formation scenario.
