of GCSs, as a function of parent galaxy luminosity, Hubble type, and local environment, to make arguments relating to issues such as biasing in a cold dark matter cosmology (West 1993); the merger history of ellipticals (Harris 1981; van den Bergh 1984; Ashman & Zepf 1992; Forbes et al. 1997); the formation of cD galaxies and their envelopes (McLaughlin, Harris, & Hanes 1993, 1994); star formation in galaxies at the centers of cluster cooling flows (Harris, Pritchet, & McClure 1995); the influence of early galactic winds on the evolution of giant ellipticals (Harris, Harris, & McLaughlin 1998); and even larger-scale aspects of galaxy clusters such as populations of intergalactic stars (e.g., West et al. 1995; Harris et al. 1998). Yet a third characteristic of GCSs—their radial distributions (the projected number density of globulars around a galaxy as a function of galactocentric radius)—has also served as the basis for discussions of elliptical galaxy formation (e.g., Harris 1986; Ashman & Zepf 1992; Kissler-Patig 1997; van den Bergh 1998).

Rather less developed, however, is a clear sense of the relevance of GCSs to [*local*]{} star formation on smaller scales: What relation, if any, do the fundamental properties of globular cluster systems bear to 