A Deep Chandra Observation of the AGN Outburst and Merger in Hickson
  Compact Group 62
  We report on an analysis of new Chandra data of the galaxy group HCG 62, well
known for possessing cavities in its intragroup medium (IGM) that were inflated
by the radio lobes of its central active galactic nucleus (AGN). With the new
data, a factor of three deeper than previous Chandra data, we re-examine the
energetics of the cavities and determine new constraints on their contents. We
confirm that the ratio of radiative to mechanical power of the AGN outburst
that created the cavities is less than 10^-4, among the lowest of any known
cavity system, implying that the relativistic electrons in the lobes can supply
only a tiny fraction of the pressure required to support the cavities. This
finding implies additional pressure support in the lobes from heavy particles
(e.g., protons) or thermal gas. Using spectral fits to emission in the
cavities, we constrain any such volume-filling thermal gas to have a
temperature kT > 4.3 keV. For the first time, we detect X-ray emission from the
central AGN, with a luminosity of L(2-10 keV) = (1.1 +/- 0.4) x 10^39 erg s^-1
and properties typical of a low-luminosity AGN. Lastly, we report evidence for
a recent merger from the surface brightness, temperature, and metallicity
structure of the IGM.
