  Globular cluster systems exhibit a bewildering variety of characteristics. No
single scenario appears to be able to account for the wide range of specific
globular cluster frequencies that are observed in galaxies of various types.
The fraction of all star formation that produces massive bound clusters differs
from galaxy to galaxy, and (in some cases) appears to vary with time. Presently
available data strongly suggest that the specific cluster forming frequency is
highest during violent bursts of star formation. Globular cluster systems show
a wide variety of color (metallicity) distributions, with many luminous
galaxies having double (or even multiple) metallicity peaks that were probably
produced during distinct episodes of cluster formation. The bulk of the
globulars in the main body of the Galactic halo appear to have formed during a
single short-lived burst that took place ~ 13 Gyr ago. This was followed by a
second, perhaps more extended, burst associated with the formation of the
Galactic bulge. A few metal-rich clusters may also be associated with the
formation of the Galactic Thick Disk. Finally many of the clusters beyond RGc ?
15 kpc might have been formed in dwarf spheroidal galaxies that, after a few
Gyr, were accreted by the main body of the Galactic halo. Some of these outer
clusters are younger, and less luminous, than the majority of globular clusters
formed at smaller Galactocentric distances.
