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We present high angular resolution multi-wavelength data of the 3C 298radio-loud quasar host galaxy (z=1.439) taken using the W.M. Keck ObservatoryOSIRIS integral field spectrograph with adaptive optics, Atacama LargeMillimeter/submillimeter Array (ALMA), Hubble Space Telescope (HST) WFC3, andthe Very Large Array (VLA). Extended emission is detected in the rest-frameoptical nebular emission lines H$\beta$, [OIII], H$\alpha$, [NII], and [SII],as well as molecular lines CO (J=3-2) and (J=5-4). Along the path of 3C 298'srelativistic jets we detect conical outflows of ionized gas with velocities upto 1700 km s$^{-1}$ and outflow rate of 450-1500 M$_\odot$yr$^{-1}$. Near thespatial center of the conical outflow, CO (J=3-2) emission shows a moleculargas disc with a total molecular mass ($\rm M_{H_{2}}$) of6.6$\pm0.36\times10^{9}$M$_{\odot}$. On the molecular disc's blueshifted sidewe observe a molecular outflow with a rate of 2300 M$_\odot$yr$^{-1}$ anddepletion time scale of 3 Myr. We detect no narrow H$\alpha$ emission in theoutflow regions, suggesting a limit on star formation of 0.3M$_\odot$yr$^{-1}$kpc$^{-2}$. Quasar driven winds are evacuating the moleculargas reservoir thereby directly impacting star formation in the host galaxy. Theobserved mass of the supermassive black hole is $10^{9.37-9.56}$M$_{\odot}$ andwe determine a dynamical bulge mass of 1-1.7$\rm\times10^{10}\frac{R}{1.6 kpc}$M$_{\odot}$. The bulge mass of 3C 298 resides 2-2.5 orders of magnitude belowthe expected value from the local M$\rm_{bulge}-M_{BH}$ relationship. A secondgalactic disc observed in nebular emission is offset from the quasar by 9 kpcsuggesting the system is an intermediate stage merger. These results show thatgalactic scale negative feedback is occurring early in the merger phase of 3C298, well before the coalescence of the galactic nuclei and assembly on thelocal relationship.

Galactic Scale Feedback Observed in the 3C 298 Quasar Host Galaxy