Exploring the origin of a large cavity in Abell 1795 using deep Chandra
  observations
  We examine deep stacked Chandra observations of the galaxy cluster Abell 1795
(over 700ks) to study in depth a large (34 kpc radius) cavity in the X-ray
emission. Curiously, despite the large energy required to form this cavity
(4PV=4x10^60 erg), there is no obvious counterpart to the cavity on the
opposite side of the cluster, which would be expected if it has formed due to
jets from the central AGN inflating bubbles. There is also no radio emission
associated with the cavity, and no metal enhancement or filaments between it
and the BCG, which are normally found for bubbles inflated by AGN which have
risen from the core. One possibility is that this is an old ghost cavity, and
that gas sloshing has dominated the distribution of metals around the core.
Projection effects, particularly the long X-ray bright filament to the south
east, may prevent us from seeing the companion bubble on the opposite side of
the cluster core. We calculate that such a companion bubble would easily have
been able to uplift the gas in the southern filament from the core.
Interestingly, it has recently been found that inside the cavity is a highly
variable X-ray point source coincident with a small dwarf galaxy. Given the
remarkable spatial correlation of this point source and the X-ray cavity, we
explore the possibility that an outburst from this dwarf galaxy in the past
could have led to the formation of the cavity, but find this to be an unlikely
scenario.
