Galactic-scale Feedback Observed in the 3C 298 Quasar Host Galaxy

We present high angular resolution multiwavelength data of the 3C 298 radio-loud quasar host galaxy (z = 1.439) taken using the W.M. Keck Observatory OSIRIS integral field spectrograph (IFS) with adaptive optics, the Atacama Large Millimeter/submillimeter Array (ALMA), the Hubble Space Telescope (HST) WFC3, and the Very Large Array (VLA). Extended emission is detected in the rest-frame optical nebular emission lines Hβ, [O iii], H , [N ii], and [S ii], as well as in the molecular lines CO (J = 3−2) and (J = 5−4). Along the path of the relativistic jets of 3C 298, we detect conical outflows in ionized gas emission with velocities of up to 1700 and an outflow rate of 450-1500 extended over 12 kpc. Near the spatial center of the conical outflow, CO (J = 3−2) emission shows a molecular gas disk with a rotational velocity of 150 and total molecular mass ( ) of . On the blueshifted side of the molecular disk, we observe broad extended emission that is due to a molecular outflow with a rate of 2300 and depletion timescale of 3 Myr. We detect no narrow H emission in the outflow regions, suggesting a limit on star formation of 0.3 . Quasar-driven winds are evacuating the molecular gas reservoir, thereby directly impacting star formation in the host galaxy. The observed mass of the supermassive black hole is , and we determine a dynamical bulge mass of . The bulge mass of 3C 298 lies 2-2.5 orders of magnitude below the expected value from the local galactic bulge-supermassive black hole mass ( ) relationship. A second galactic disk observed in nebular emission is offset from the quasar by 9 kpc, suggesting that the system is an intermediate-stage merger. These results show that galactic-scale negative feedback is occurring early in the merger phase of 3C 298, well before the coalescence of the galactic nuclei and assembly on the local relationship.