though the total population ${\cal N}_
{\rm tot}$ of any GCS is bound to decrease over time*]{}, as individual globulars are disrupted by the cumulative effects of external gravitational shocks and internal two-body relaxation (see, e.g., Aguilar, Hut, & Ostriker 1988; Ostriker, Binney, & Saha 1989; Capuzzo-Dolcetta 1993; Murali & Weinberg 1997a, 1997b, 1997c; Gnedin & Ostriker 1997; Vesperini & Heggie 1997; but cf. Portegies Zwart et al. 1998). These dynamical processes discriminate preferentially against low-mass and low-density globular clusters, and it turns out that even if large [*numbers*]{} of such objects are lost, no great change is effected in the total [*mass*]{} of the remaining GCS. This conclusion rests on the fact that the mass functions of GCSs—particularly those in early-type galaxies—are shallow enough that most of the total $M_{\rm gcs}$ is contained in the most massive members of the system; but these are the least susceptible to dynamical destruction. The implication is that the total mass of a GCS may not change much over its lifetime; thus, [*if*]{} the current stellar mass of a galaxy were a reliable indication of the total amount of gas that was initially available to form stars, then the presently observed ratio $M_{\rm 