This project is ongoing, for more, see the preprint paper (still working on it, or the Google Drive file)
Globular culsters (GC) are the tracers of galaxy evolution, richness and other properties of GC
systems can help make clear formation history and constrain models.
Thanks to the deep image from Next Generation Virgo Cluster Survey (NGVS), we have calculated specific frequency (SN, scale of richness normalized to luminosity) for 20 nucleated dwarf ellipticals (dE,Ns) in Virgo cluster, all of which are fainter than MV = -16.5, and found that their SN is significantly larger and scattered than massive galaxies and the trend shows SN increases monotonically with MV at MV > -16.5 (see fig.1). We also studied GC color distribution and the influence of environment on GC richness of galaxies.
We confirmed the U-shape in SN MV relationship at low luminosity end. Our result favors the stripping model (or intrinsically quenching model?).
for more, see the undergoing paper