Quenching of Satellite Galaxies at the Outskirts of Galaxy Clusters
  We find, using cosmological simulations of galaxy clusters, that the hot
X-ray emitting intra-cluster medium (ICM) enclosed within the outer accretion
shock extends out to $R_{\rm shock}\sim(2 - 3) R_{\rm vir}$, where $R_{\rm
vir}$ is the standard virial radius of the halo. Using a simple analytic model
for satellite galaxies in the cluster, we evaluate the effect of ram pressure
stripping on the gas in the inner discs and in the haloes at different
distances from the cluster centre. We find that significant removal of
star-forming disc gas occurs only at $r \lesssim 0.5 R_{\rm vir}$, while gas
removal from the satellite halo is more effective and can occur when the
satellite is found between $ R_{\rm vir}$ and $R_{\rm shock}$. Removal of halo
gas sets the stage for quenching of the star formation by starvation over
$2\textrm{--}3\,\mathrm{Gyr}$, prior to the satellite entry to the inner
cluster halo. This scenario explains the presence of quenched galaxies,
preferentially discs, at the outskirts of galaxy clusters, and the delayed
quenching of satellites compared to central galaxies.
