JET-POWERED MOLECULAR HYDROGEN EMISSION FROM RADIO GALAXIES

Abstract

H[subscript 2] pure-rotational emission lines are detected from warm (100-1500 K) molecular gas in [17 over 55] (31% of) radio galaxies at redshift z < 0.22 observed with the Spitzer IR Spectrograph. The summed H[subscript 2] 0-0 S(0)-S(3) line luminosities are L(H[subscript 2]) = 7 × 10[superscript 38]-2 × 10[superscript 42] erg s[superscript –1], yielding warm H[subscript 2] masses up to 2 × 10[superscript 10] M [subscript ☉]. These radio galaxies, of both FR radio morphological types, help to firmly establish the new class of radio-selected molecular hydrogen emission galaxies (radio MOHEGs). MOHEGs have extremely large H[subscript 2] to 7.7 μm polycyclic aromatic hydrocarbon (PAH) emission ratios: L(H[subscript 2]) [over L(PAH7.7)] = 0.04-4, up to a factor 300 greater than the median value for normal star-forming galaxies. In spite of large H[subscript 2] masses, MOHEGs appear to be inefficient at forming stars, perhaps because the molecular gas is kinematically unsettled and turbulent. Low-luminosity mid-IR continuum emission together with low-ionization emission line spectra indicates low-luminosity active galactic nuclei (AGNs) in all but three radio MOHEGs. The AGN X-ray emission measured with Chandra is not luminous enough to power the H[subscript 2] emission from MOHEGs. Nearly all radio MOHEGs belong to clusters or close pairs, including four cool-core clusters (Perseus, Hydra, A2052, and A2199). We suggest that the H[subscript 2] in radio MOHEGs is delivered in galaxy collisions or cooling flows, then heated by radio-jet feedback in the form of kinetic energy dissipation by shocks or cosmic rays.