The globular cluster luminosity function , specific globular cluster frequency , S _ { N } , specific globular cluster mass , T _ { 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 _ { 5 } function with a peak at M _ { V,Z } ^ { 0 } ( dE,HST ) = -7.3 \pm 0.1 .
This is \sim 0.3 magnitudes 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 \pm 0.1 .
The trend of increasing S _ { N } or T _ { MP } with decreasing host galaxy luminosity is confirmed .
The mean value for T _ { MP } in dE , N galaxies is about a factor of two higher than the mean value for non-nucleated galaxies and the distributions of T _ { 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 _ { 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 _ { 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 .