  We extend our initial study of the connection between the UV colour of
galaxies and both the inferred stellar mass-to-light ratio, $\Upsilon_*$, and a
mass-to-light ratio referenced to Salpeter initial mass function (IMF) models
of the same age and metallicity, $\Upsilon_*/\Upsilon_{Sal}$, using new UV
magnitude measurements for a much larger sample of early-type galaxies, ETGs,
with dynamically determined mass-to-light ratios. We confirm the principal
empirical finding of our first study, a strong correlation between the GALEX
FUV-NUV colour and $\Upsilon_*$. We show that this finding is not the result of
spectral distortions limited to a single passband (eg. metallicity-dependent
line-blanketing in the NUV band), or of the analysis methodology used to
measure $\Upsilon_*$, or of the inclusion or exclusion of the correction for
stellar population effects as accounted for using $\Upsilon_*/\Upsilon_{Sal}$.
The sense of the correlation is that galaxies with larger $\Upsilon_*$, or
larger $\Upsilon_*/\Upsilon_{Sal}$, are bluer in the UV. We conjecture that
differences in the low mass end of the stellar initial mass function, IMF, are
related to the nature of the extreme horizontal branch stars generally
responsible for the UV flux in ETGs. If so, then UV color can be used to
identify ETGs with particular IMF properties and to estimate $\Upsilon_*$. We
also demonstrate that UV colour can be used to decrease the scatter about the
Fundamental Plane and Manifold, and to select peculiar galaxies for follow-up
with which to further explore the cause of variations in $\Upsilon_*$ and UV
colour.
