Satellite dwarf galaxies: Stripped but not quenched
  In the Local Group, quenched gas-poor dwarfs galaxies are most often found
close to the Milky Way and Andromeda, while star forming gas-rich ones are
located at greater distances. This so-called morphology-density relation is
often interpreted as the consequence of the ram pressure stripping of the
satellites during their interaction with the Milky Way hot halo gas. While this
process has been often investigated, self-consistent high resolution
simulations were still missing. In this study, we have analysed the impact of
both the ram pressure and tidal forces induced by a host galaxy on dwarf models
as realistic as possible emerging from cosmological simulations. These models
were re-simulated using both a wind tunnel and a moving box technique. The
secular mass growth of the central host galaxy, as well as the gas density and
temperature profiles of its hot halo have been taken into account. We show that
while ram pressure is very efficient at stripping the hot and diffuse gas of
the dwarf galaxies, it can remove their cold gas ($T < 10^3$~[K]) only in very
specific conditions. Depending on the infall time of the satellites relatively
to the build-up stage of the massive host, star formation can thus be prolonged
instead of being quenched. This is the direct consequence of the clumpy nature
of the cold gas and the thermal pressure the hot gas exerts onto it. We discuss
the possibility that the variety in satellite populations among Milky Way-like
galaxies reflects their accretion histories.
