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 ( IFS ) 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 , [ O III ] , H \alpha , [ N II ] , and [ S II ] , 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 in ionized gas emission with velocities up to 1700 km s ^ { -1 } and outflow rate of 450-1500 M _ { \odot } yr ^ { -1 } extended over 12 kpc .
Near the spatial center of the conical outflow , CO ( J=3-2 ) emission shows a molecular gas disc with a rotational velocity of \pm 150km s ^ { -1 } and total molecular mass ( M _ { H _ { 2 } } ) of 6.6 \pm 0.36 \times 10 ^ { 9 } ~ { } M _ { \odot } .
On the molecular disc ’ s blueshifted side we observe broad extended emission due to 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 M _ { bulge } = 1-1.7 \times 10 ^ { 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 galactic bulge - supermassive black hole mass ( M _ { 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 M _ { bulge } - M _ { BH } relationship .