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We present a comparison of the molecular gas properties in the outflow vs. inthe ambient medium of the local prototype radio-loud and ultraluminous-infraredgalaxy 4C12.50 (IRAS13451+1232), using new data from the IRAM Plateau de Bureinterferometer and 30m telescope, and the Herschel space telescope. PreviousH_2 (0-0) S(1) and S(2) observations with the Spitzer space telescope hadindicated that the warm (~400K) molecular gas in 4C12.50 is made up of a1.4(+-0.2)x10^8 M_sun ambient reservoir and a 5.2(+-1.7)x10^7 M_sun outflow.The new CO(1-0) data cube indicates that the corresponding cold (25K) H_2 gasmass is 1.0(+-0.1)x10^10 M_sun for the ambient medium and <1.3x10^8 M_sun forthe outflow, when using a CO-intensity-to-H_2-mass conversion factor alpha of0.8 M_sun /(K km/s pc^2). The combined mass outflow rate is high, 230-800M_sun/yr, but the amount of gas that could escape the galaxy is low. Apotential inflow of gas from a 3.3(+-0.3)x10^8 M_sun tidal tail could moderateany mass loss. The mass ratio of warm-to-cold molecular gas is >= 30 timeshigher in the outflow than in the ambient medium, indicating that anon-negligible fraction of the accelerated gas is heated to temperatures atwhich star formation is inefficient. This conclusion is robust against the useof different alpha factor values, and/or different warm gas tracers (H_2 vs.H_2 plus CO): with the CO-probed gas mass being at least 40 times lower at 400Kthan at 25K, the total warm-to-cold mass ratio is always lower in the ambientgas than in the entrained gas. Heating of the molecular gas could facilitatethe detection of new outflows in distant galaxies by enhancing their emissionin intermediate rotational number CO lines.

Heating of the molecular gas in the massive outflow of the local ultraluminous-infrared and radio-loud galaxy 4C12.50