Ram Pressure Stripping of Hot Coronal Gas from Group and Cluster
  Galaxies and the Detectability of Surviving X-ray Coronae
  Ram pressure stripping can remove hot and cold gas from galaxies in the
intracluster medium (ICM), as shown by observations of X-ray and HI galaxy
wakes in nearby clusters of galaxies. However, ram pressure stripping,
including pre-processing in group environments, does not remove all the hot
coronal gas from cluster galaxies. Recent high-resolution Chandra observations
have shown that $\sim 1 - 4$ kpc extended, hot galactic coronae are ubiquitous
in group and cluster galaxies. To better understand this result, we simulate
ram pressure stripping of a cosmologically motivated population of galaxies in
isolated group and cluster environments. The galaxies and the host group and
cluster are composed of collisionless dark matter and hot gas initially in
hydrostatic equilibrium with the galaxy and host potentials. We show that the
rate at which gas is lost depends on the galactic and host halo mass. Using
synthetic X-ray observations, we evaluate the detectability of stripped
galactic coronae in real observations by stacking images on the known galaxy
centers. We find that coronal emission should be detected within $\sim 10$
arcsec, or $\sim 5$ kpc up to $\sim 2.3$ Gyr in the lowest (0.1 - 1.2 keV)
energy band. Thus the presence of observed coronae in cluster galaxies
significantly smaller than the hot X-ray halos of field galaxies indicates that
at least some gas removal occurs within cluster environments for recently
accreted galaxies. Finally, we evaluate the possibility that existing and
future X-ray cluster catalogs can be used in combination with optical galaxy
positions to detect galactic coronal emission via stacking analysis. We briefly
discuss the effects of additional physical processes on coronal survival, and
will address them in detail in future papers in this series.
