Galactic Scale Feedback Observed in the 3C 298 Quasar Host Galaxy
  We present high angular resolution multi-wavelength data of the 3C 298
radio-loud quasar host galaxy (z=1.439) taken using the W.M. Keck Observatory
OSIRIS integral field spectrograph with adaptive optics, Atacama Large
Millimeter/submillimeter Array (ALMA), Hubble Space Telescope (HST) WFC3, and
the Very Large Array (VLA). Extended emission is detected in the rest-frame
optical 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's
relativistic jets we detect conical outflows of ionized gas with velocities up
to 1700 km s$^{-1}$ and outflow rate of 450-1500 M$_\odot$yr$^{-1}$. Near the
spatial center of the conical outflow, CO (J=3-2) emission shows a molecular
gas disc with a total molecular mass ($\rm M_{H_{2}}$) of
6.6$\pm0.36\times10^{9}$M$_{\odot}$. On the molecular disc's blueshifted side
we observe a molecular outflow with a rate of 2300 M$_\odot$yr$^{-1}$ and
depletion time scale of 3 Myr. We detect no narrow H$\alpha$ emission in the
outflow regions, suggesting a limit on star formation of 0.3
M$_\odot$yr$^{-1}$kpc$^{-2}$. 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 $10^{9.37-9.56}$M$_{\odot}$ and
we 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 below
the expected value from the local M$\rm_{bulge}-M_{BH}$ relationship. A second
galactic disc observed in nebular emission is offset from the quasar by 9 kpc
suggesting 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.
