  In this paper we report on the analysis of a deep ROSAT HRI image of the
moderately-rich cluster, Abell 2634, by which we have been able to detect the
X-ray emission from the galaxies in the cluster. The ICM of Abell 2634 is an
order of magnitude denser than that of the Virgo cluster, and so this analysis
allows us to explore the X-ray properties of individual galaxies in the richest
environment yet explored. By stacking the X-ray images of the galaxies
together, we have shown that their emission appears to be marginally resolved
by the HRI. This extent is smaller than for galaxies in poorer environments,
and is comparable to the size of the galaxies in optical light. These facts
suggest that the detected X-ray emission originates from the stellar
populations of the galaxies, rather than from extended hot interstellar media.
Support for this hypothesis comes from placing the optical and X-ray
luminosities of these galaxies in the L_B - L_X plane: the galaxies of Abell
2634 lie in the region of this plane where models indicate that all the X-ray
emission can be explained by the usual population of X-ray binaries. It is
therefore probable that ram pressure stripping has removed the hot gas
component from these galaxies.
