  The outskirts of galaxy clusters host complex interactions between the
intra-cluster and circumcluster media. During cluster evolution, ram-pressure
stripped gas clumps from infalling substructures break the uniformity of the
gas distribution, which may lead to observational biases at large radii.
Assessing the contribution of gas clumping, however, poses observational
challenges, and requires robust X-ray measurements in the background-dominated
regime of cluster outskirts. The aims of this work are isolating faint gas
clumps from field sources and from the diffuse emission in the Abell 1795
galaxy cluster, then probing their impact on the observed surface brightness
and thermodynamic profiles. We performed imaging analysis on deep Chandra
ACIS-I observations of the outskirts of Abell 1795, extending to
$\sim1.5r_{200}$ with full azimuthal coverage. We built the $0.7-2.0$ keV
surface brightness distribution from the adaptively binned image of the diffuse
emission and looked for clumps as $>2\sigma$ outliers. Classification of the
clump candidates was based on Chandra and SDSS data. Benefiting from the
Chandra point source list, we extracted the thermodynamic profiles of the
intra-cluster medium from the associated Suzaku XIS data out to $r_{200}$ using
multiple point source and clump candidate removal approaches. We identified 24
clump candidates in the Abell 1795 field, most of which are likely associated
with background objects, including AGN, galaxies, and clusters or groups of
galaxies, as opposed to intrinsic gas clumps. These sources had minimal impact
on the surface brightness and thermodynamic profiles of the cluster emission.
After correcting for clump candidates, the measured entropy profile still
deviates from a pure gravitational collapse, suggesting complex physics at play
in the outskirts, including potential electron-ion non-equilibrium and
non-thermal pressure support.
