The Globular Cluster Luminosity Function and Specific Frequency in Dwarf Elliptical Galaxies

The globular cluster luminosity function, specific globular cluster frequency, S sub(N), specific globular cluster mass, T sub(MP), and globular cluster mass fraction in dwarf elliptical galaxies are explored using the full 69 galaxy sample of the HST WFPC2 Dwarf Elliptical Galaxy Snapshot Survey. The GCLFs of the dEs are well represented with a t sub(5) function with a peak at M super(0) sub(V.Z) (dE .HST) = -7.3 plus or minus 0.1. This is similar to 0.3 mag fainter than the GCLF peaks in giant spiral and elliptical galaxies, but the results are consistent within the uncertainties. The bright-end slope of the luminosity distribution has a power-law form with slope alpha = -1.9 plus or minus 0.1. The trend of increasing S sub(N) or T sub(MP) with decreasing host galaxy luminosity is confirmed. The mean value for T sub(MP) in dE, N galaxies is about a factor of 2 higher than the mean value for nonnucleated galaxies and the distributions of T sub(MP) in dE, N and dE, noN galaxies are statistically different. These data are combined with results from the literature for a wide range of galaxy types and environments. At low host galaxy masses the distribution of T sub(MP) for dE, noN and dI galaxies are similar. This supports the idea that one pathway for forming dE, noN galaxies is by the stripping of dIs. The formation of nuclei and the larger values of T sub(MP) in dE, N galaxies may be due to higher star formation rates and star cluster formation efficiencies due to interactions in galaxy cluster environments.