gcs}/M_{\rm stars}\sim2\times10^{-3}$ would serve as a rough, [*global*]{} estimate of the efficiency of globular cluster formation. Note that this reasoning also shows that galactic halos cannot be built up from disrupted globulars; see, e.g., Ashman & Zepf (1992) and Harris & Pudritz (1994). (One of the main conclusions of this paper will be that, in fact, $M_{\rm stars}$ is [*not*]{} always an adequate measure of an initial gas supply, and that $M_{\rm gcs}/M_{\rm stars}$ therefore cannot always be equated directly to a cluster formation efficiency. However, since most previous discussions of GCS specific frequencies do draw on this simple assumption at some level, it is of interest to develop some of its implications.)

A simple numerical example should emphasize the robustness of $M_{\rm gcs}$. Thus, consider a newly formed system of globulars whose masses are distributed according to a power-law mass function between some lower and upper limits: $$\left({{d{\cal N}}\over{dm}}\right)_{\rm init}\,=\,K\,m^{-\gamma_2}\,,
\ \ \ \ \ \ \ \ m_\ell \leq m\leq m_u\ ,
\label{eq:24}$$ where $\gamma_2>0$ and reasonable choices for $m_\ell$ and $m_u$ may be $500\,M_\odot$ and $5\times10^6\,M_\odot$. (The precise values are not critical here.) Now let this GCS be eroded over $10^{10}$ yr, keeping in mind that each 