  Here we examine the relationship between the virial and stellar mass for a
range of old stellar systems, from GCs to giant ellipticals, and including such
Intermediate Mass Objects (IMOs). Improvements on previous work in this area
include the use of (i) near-infrared magnitudes from the 2MASS survey, (ii)
aperture corrections to velocity dispersions, (iii) homogeneous half light
radii and (iv) accounting for the effects of non-homology in galaxies. We find
a virial-to-stellar mass relation that ranges from ~10$^4$ M_o systems (GCs) to
~10$^11$ M_o systems (elliptical galaxies). The lack of measured velocity
dispersions for dwarf ellipticals with -16 > M_K > -18 (~10$^8$ M_o) currently
inhibits our ability to determine how, or indeed if, these galaxies connect
continuously with GCs in terms of their virial-to-stellar mass ratios. We find
elliptical galaxies to have roughly equal fractions of dark and stellar matter
within a virial radius; only in the most massive (greater than 10$^11$ M_o)
ellipticals does dark matter dominate the virial mass. Although the IMOs reveal
slightly higher virial-to-stellar mass ratios than lower mass GCs, this may
simply reflect our limited understanding of their IMF (and hence their stellar
mass-to-light ratios) or structural properties. We argue that most of these
intermediate mass objects are a natural extension of the GC sequence to higher
masses, i.e. IMOs are essentially massive star clusters. [Abridged].
