The transformation and quenching of simulated gas-rich dwarf satellites
  within a group environment
  The underlying mechanisms driving the quenching of dwarf-mass satellite
galaxies remain poorly constrained, but recent studies suggest they are
particularly inefficient for those satellites with stellar mass 10$^{\rm 9}$
M$_{\odot}$. We investigate the characteristic evolution of these systems with
chemodynamical simulations and idealised models of their tidal/hydrodynamic
interactions within the 10$^{\rm 13-13.5}$ M$_{\odot}$ group-mass hosts in
which they are preferentially quenched. Our fiducial simulations highlight the
role played by secular star formation and stellar bars, and demonstrate a
transition from a gas-rich to passive, HI-deficient state (i.e.
$\Delta$SFR$\le$-1, def$_{\rm HI}$$\ge$0.5) within 6 Gyr of first infall.
Furthermore, in the 8-10 Gyr in which these systems have typically been
resident within group hosts, the bulge-to-total ratio of an initially bulgeless
disc can increase to 0.3$<$B/T$<$0.4, its specific angular momentum
$\lambda_{\rm R}$ reduce to $\sim$0.5, and strong bisymmetries formed.
Ultimately, this scenario yields satellites resembling dwarf S0s, a result that
holds for a variety of infall inclinations/harassments albeit with broad
scatter. The key assumptions here lie in the rapid removal of the satellite's
gaseous halo upon virial infall, and the satellite's local intra-group medium
density being defined by the host's spherically-averaged profile. We
demonstrate how quenching can be greatly enhanced if the satellite lies in an
overdensity, consistent with recent cosmological-scale simulations but
contrasting with observationally-inferred quenching mechanisms/timescales; an
appraisal of these results with respect to the apparent preferential formation
of dS0s/S0s in groups is also given.
