models for high-quality spatially resolved photometric and kinematic data. With these goals in mind we obtained spectroscopic data in vDvdM06 that was deep enough to extract spatially resolved rotation curves and velocity dispersion profiles for the sample galaxies in CL3C295, CL0016+16 and CL1601+42. In van der Marel & van Dokkum (2006, hereafter Paper I) we presented the kinematical profiles and constructed detailed dynamical models to interpret them. The models are axisymmetric and are based on solving the Jeans equations of hydrostatic equilibrium under the assumption of a two-integral distribution function $f=f(E,L_z)$, where $E$ is the energy and $L_z$ the angular momentum around the symmetry axis. Fitting of the models to the available HST imaging and observed kinematical profiles yields two quantities: a normalized measure $k$ of the galaxy’s rotation rate and the $M/L$ of the stellar population (in rest-frame $B$ band solar units). The inferred values for these quantities and their formal uncertainties were presented in Paper I. The implications of the inferred rotation rates were also discussed in that paper. In the present paper we interpret the inferred $M/L$ values. To do this, we first compile and homogenize a comparison sample of galaxies in the local Universe with reliable 