METAL-RICH GLOBULAR-CLUSTERS WITH R-LESS-THAN-OR-EQUAL-TO-3 KPC - DISK OR BULGE CLUSTERS

We compare the metal-rich globular clusters within 3 kpc of the galactic center with the underlying stellar population. On the basis of kinematics, spatial distribution, and metallicity, we argue that these clusters may be associated with the galactic bulge (as concluded by Frenk & White 1982) rather than with the thick disk. On the basis of the available ages for some of these clusters, it is argued that the galactic bulge formed after the halo. Different formation scenarios of the galaxy are examined, and it is concluded that dissipation played a major role in the inner 3 kpc.