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We present a 70ks Chandra observation of the radio galaxy 3C293. This galaxybelongs to the class of molecular hydrogen emission galaxies (MOHEGs) that havevery luminous emission from warm molecular hydrogen. In radio galaxies, themolecular gas appears to be heated by jet-driven shocks, but exactly how thismechanism works is still poorly understood. With Chandra, we observe X-rayemission from the jets within the host galaxy and along the 100 kpc radio jets.We model the X-ray spectra of the nucleus, the inner jets, and the X-rayfeatures along the extended radio jets. Both the nucleus and the inner jetsshow evidence of 10^7 K shock-heated gas. The kinetic power of the jets is morethan sufficient to heat the X-ray emitting gas within the host galaxy. Thethermal X-ray and warm H2 luminosities of 3C293 are similar, indicating similarmasses of X-ray hot gas and warm molecular gas. This is consistent with apicture where both derive from a multiphase, shocked interstellar medium (ISM).We find that radio-loud MOHEGs that are not brightest cluster galaxies (BCGs),like 3C293, typically have LH2/LX~1 and MH2/MX~1, whereas MOHEGs that are BCGshave LH2/LX~0.01 and MH2/MX~0.01. The more massive, virialized, hot atmospherein BCGs overwhelms any direct X-ray emission from current jet-ISM interaction.On the other hand, LH2/LX~1 in the Spiderweb BCG at z=2, which resides in anunvirialized protocluster and hosts a powerful radio source. Over time, jet-ISMinteraction may contribute to the establishment of a hot atmosphere in BCGs andother massive elliptical galaxies.

Jet-ISM Interaction in the Radio Galaxy 3C293: Jet-driven Shocks Heat ISM to Power X-ray and Molecular H2 emission