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 3 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_{2text{-}10 keV} = (1.1 ± 0.4)× 10^{39} erg s- 1 and properties typical of a low-luminosity AGN. Finally, we report evidence for a recent merger from the surface brightness, temperature and metallicity structure of the IGM.
