  Data are presently available on the luminosities and half-light radii of 101
globular clusters associated with low-luminosity parent galaxies. The
luminosity distribution of globulars embedded in dwarf galaxies having $M_{v} >
-16$ is found to differ dramatically from that for globular clusters
surrounding giant host galaxies with $M_{v} < -16$. The luminosity distribution
of globular clusters in giant galaxies peaks at $M_{v} \sim -7.5$, whereas that
for dwarfs is found to increases monotonically down to the completeness limit
of the cluster data at $M_{v} \sim -5.0$. Unexpectedly, the power law
distribution of the luminosities of globular clusters hosted by dwarf galaxies
is seen to be much flatter than the that of bright unevolved part of the
luminosity distribution of globular clusters associated with giant galaxies.
The specific frequency of globular clusters that are fainter than $M_{v} =
-7.5$ is found to be particularly high in dwarf galaxies. The luminosity
distribution of the LMC globular clusters is similar to that in giant galaxies,
and differs from those of the globulars in dwarf galaxies. The present data
appear to show no strong dependence of globular cluster luminosity on the
morphological types of their parent galaxies. No attempt is made to explain the
unexpected discovery that the luminosity distribution of globular clusters is
critically dependent on parent galaxy luminosity (mass?), but insensitive to
the morphological type of their host galaxy.
