Feedback by AGN Jets and Wide-Angle Winds on a Galactic Scale
  To investigate the differences in mechanical feedback from radio-loud and
radio-quiet Active Galactic Nuclei (AGN) on the host galaxy, we perform 3D AMR
hydrodynamic simulations of wide angle, radio-quiet winds with different
inclinations on a single, massive, gas-rich disk galaxy at a redshift of 2-3.
We compare our results to hydrodynamic simulations of the same galaxy but with
a jet. The jet has an inclination of 0 degrees (perpendicular to the galactic
plane), and the winds have inclinations of 0, 45, and 90 degrees. We analyze
the impact on the host's gas, star formation, and circum-galactic medium. We
find that jet feedback is energy-driven and wind feedback is momentum-driven.
In all the simulations, the jet or wind creates a cavity mostly devoid of dense
gas in the nuclear region where star formation is then quenched, but we find
strong positive feedback in all the simulations at radii greater than 3 kpc.
All four simulations have similar SFRs and stellar velocities with large radial
and vertical components. However, the wind at an inclination of 90 degrees
creates the highest density regions through ram pressure and generates the
highest rates of star formation due to its ongoing strong interaction with the
dense gas of the galactic plane. With increased wind inclination, we find
greater asymmetry in gas distribution and resulting star formation. Our model
generates an expanding ring of triggered star formation with typical velocity
of order 1/3 of the circular velocity, superimposed on the older stellar
population. This should result in a potentially detectable blue asymmetry in
stellar absorption features at kpc scales.
