  The nearby cluster Abell 1795 is used as a testbed to examine whether hot gas
in cluster galaxies is stripped by the ram pressure of the intracluster medium
(ICM). The expected X-ray emission in and around Abell 1795 galaxies is likely
dominated by the ICM, low-mass X-ray binaries, active galactic nuclei, and hot
gas halos. In order to constrain these components, we use archival Chandra
X-ray Observatory and Sloan Digital Sky Survey (SDSS) observations of Abell
1795 and identify 58 massive (M_star>10^10 M_sun) spectroscopic cluster members
within 5 arcmin of the Chandra optical axis. X-ray images at 0.5-1.5 keV and
4-8 keV were created for each cluster member and then stacked into two
clustercentric radius bins: inner (0.25<R/R_500<1) and outer (1<R/R_500<2.5).
Surface brightness profiles of inner and outer cluster members are fit using
Markov chain Monte Carlo sampling in order to generate model parameters and
measure the 0.5-1.5 keV luminosities of each model component. Leveraging
effective total Chandra exposure times of 3.4 and 1.7 Msec for inner and outer
cluster members, respectively, we report the detection of hot gas halos, in a
statistical sense, around outer cluster members. Outer members have 0.5-1.5 keV
hot halo luminosities (L_X = 8.1(-3.5/+5)x10^39 erg/s) that are six times
larger than the upper limit for inner cluster members (L_X < 1.3x10^39 erg/s).
This result suggests that the ICM is removing hot gas from the halos of Abell
1795 members as they fall into the cluster.
