On the Assembly of Dwarf Galaxies in Clusters and their Efficient
  Formation of Globular Clusters
  Galaxy clusters contain a large population of low mass dwarf elliptical
galaxies whose exact origin is unclear: their colors, structural properties and
kinematics differ substantially from those of dwarf irregulars in the field. We
use the Illustris cosmological simulation to study differences in the assembly
paths of dwarf galaxies (3e8 < M_*/M_sun < 1e10) according to their
environment. We find that cluster dwarfs achieve their maximum total and
stellar mass on average ~ 8 and ~ 4.5 Gyr ago (or redshifts z = 1.0 and z =
0.4, respectively), around the time of infall into the clusters. In contrast,
field dwarfs not subjected to environmental stripping, reach their maximum mass
at redshift z = 0. This different assembly history naturally produces a color
bimodality, with blue isolated dwarfs and redder cluster dwarfs exhibiting
negligible star-formation today. The cessation of star formation happens over
median times 3.5-5 Gyr depending on stellar mass, and shows a large scatter (~
1-8 Gyr), with the lower values associated with starburst events that occur at
infall through the virial radius or pericentric passages. We argue that such
starbursts together with the early assembly of cluster dwarfs can provide a
natural explanation for the higher specific frequency of globular clusters
(GCs) in cluster dwarfs, as found observationally. We present a simple model
for the formation and stripping of GCs that supports this interpretation. The
origin of dwarf ellipticals in clusters is, therefore, consistent with an
environmentally-driven evolution of field dwarf irregulars. However the z = 0
field analogs of cluster dwarf progenitors have today stellar masses a factor ~
3 larger --a difference arising from the early truncation of star formation in
cluster dwarfs.
