2000PASP..112..932V

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. Currently 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 R_Gc≃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.