Massive Star Clusters in Dwarf Galaxies
  Dwarf galaxies can have very high globular cluster specific frequencies, and
the GCs are in general significantly more metal-poor than the bulk of the field
stars. In some dwarfs, such as Fornax, WLM, and IKN, the fraction of metal-poor
stars that belong to GCs can be as high as 20%-25%, an order of magnitude
higher than the 1%-2% typical of GCs in halos of larger galaxies. Given that
chemical abundance anomalies appear to be present also in GCs in dwarf
galaxies, this implies severe difficulties for self-enrichment scenarios that
require GCs to have lost a large fraction of their initial masses. More
generally, the number of metal-poor field stars in these galaxies is today less
than what would originally have been present in the form of low-mass clusters
if the initial cluster mass function was a power-law extending down to low
masses. This may imply that the initial GC mass function in these dwarf
galaxies was significantly more top-heavy than typically observed in
present-day star forming environments.
