component are known. As is discussed further in §3.1 below, the basic distribution of globular cluster masses is quite similar from galaxy to galaxy, so that the mean cluster mass in the Milky Way GCS—$\langle m\rangle_
{\rm cl}=2.4\times10^5\,M_\odot$—serves as a reliable estimate for other systems as well. Meanwhile, the stellar mass-to-light ratios of large galaxies are essentially equal to the dynamical $M/L$ in their [*cores*]{}, which are baryon-dominated. As is also discussed below (§4.1), observations show that the core $M/L$ of hot galaxies increases with luminosity; but, even though this turns out to be rather an important consideration in detail, it will suffice for now to use a single value of $\Upsilon_V\equiv M/L_V=7\,M_\odot\,
L_\odot^{-1}$ as a rough characterization of large ellipticals (van der Marel 1991; cf. Faber & Gallagher 1979; Binney & Tremaine 1987). The definition of $S_N$ in equation (\[eq:21\]) may then be rewritten as (cf. Zepf & Ashman 1993; Harris & Pudritz 1994; Harris et al. 1998) $$S_N\simeq2500\,\left({{\langle m\rangle_{\rm cl}}\over{2.4\times10^5\,M_\odot}}
\right)^{-1}\,\left({{\Upsilon_V}\over{7\,M_\odot\,L_\odot^{-1}}}\right)\,
{{M_{\rm gcs}}\over{M_{\rm stars}}}\ .
\label{eq:22}$$ To be clear, it is stressed again that the mass-to-light ratio applied here refers to measurements in the cores of ellipticals, and is not meant to include any dark matter other than 