et al. 1994 and Harris et al. 1998; though see also Kavelaars & Hanes 1997 and Murali & Weinberg 1997b). Nevertheless, it should be noted that dynamical friction, gravitational shocks, and even evaporation couple to galactic tidal fields in such a way that if a GCS’s present-day mass function [*were*]{} sculpted to any great extent by these processes, then the [*local*]{} ratios ${\cal N}_{\rm tot}^{\rm obs}/{\cal N}_{\rm tot}^{\rm init}$ and $M_{\rm gcs}^{\rm obs}/M_{\rm gcs}^{\rm init}$ would be expected to increase outwards from the center of the system, from values less than equation (\[eq:28\]) at small galactocentric radii to near unity at large distances (e.g., beyond a stellar effective radius; see especially Murali & Weinberg 1997b).

Returning now to the main issue, the global efficiency of globular cluster formation in a galaxy may be defined as $$\epsilon_{\rm cl}\,\equiv\,
M_{\rm gcs}^{\rm init}/M_{\rm gas}^{\rm init}\ ,
\label{eq:29}$$ where $M_{\rm gas}^{\rm init}$ refers to the total gas supply that was available to the protogalaxy, whether in a rapid monolithic collapse or, more likely, in a slower assembly (at high redshift) of many distinct, subgalactic clouds. From the preceding discussion, it is clear that if a newly formed GCS were able to evolve “passively”—that is, 