galaxies, by concentrating on two of the primary attributes of GCSs: their specific frequencies (or total populations) and radial distributions. The next Section discusses the significance of these GCS properties as they relate to general questions on the formation of stellar clusters. In §3 below, data are compiled from the literature, and a geometrical deprojection algorithm applied, to construct [*volume*]{} density profiles for the stars, the X-ray gas, and the globular clusters in three galaxies with well studied GCSs: M87 (the cD at the center of the Virgo Cluster), M49 (giant elliptical in Virgo), and NGC 1399 (cD galaxy in the Fornax Cluster). An intercomparison of the density profiles of the three halo components yields a point-by-point measure of the GCS contribution to the total luminous mass in each system, as a function of [*three-dimensional*]{} galactocentric radius, $r_{\rm gc}$. These GCS mass ratios, which are constant throughout each galaxy (at large $r_{\rm gc}$) and the same in all three, are interpreted as an indication of the formation efficiency of globular clusters. In §4, these results are supplemented with broader considerations of the GCSs in other early-type galaxies and in the Milky Way halo, and with a direct estimate for the 