Probing Satellite Quenching With Galaxy Clustering
  Satellites within simulated massive clusters are significantly spatially
correlated with each other, even when those satellites are not gravitationally
bound to each other. This correlation is produced by satellites that entered
their hosts relatively recently, and is undetectable for satellites that have
resided in their hosts for multiple dynamical timescales. Therefore, a
measurement of clustering statistics of cluster satellites may be used to
determine the typical accretion redshifts of those satellites into their
observed hosts. We argue that such measurements may be used to determine the
fraction of satellite galaxies that were quenched by their current hosts,
thereby discriminating among models for quenching of star formation in
satellite galaxies.
