Relativistic jet feedback III: feedback on gas disks
  We study the interactions of a relativistic jet with a dense turbulent
gaseous disk of radius $\sim 2$ kpc. We have performed a suite of simulations
with different mean density, jet power and orientation. Our results show that:
A) the relativistic jet couples strongly with the gas in the inner kpc,
creating a cavity and launching outflows. B) The high pressure bubble inflated
by the jet and its back-flow compresses the disk at the outer edges, driving
inflows within the disk. C) Jets inclined towards the disk couple more strongly
with the disk and launch sub-relativistic, wide-angle outflows along the minor
axis. D) Shocks driven directly by the jet and the jet-driven energy bubble
raise the velocity dispersion throughout the disk by several times its initial
value. E) Compression by the jet-driven shocks can enhance the star formation
rate in the disk, especially in a ring-like geometry close to the axis.
However, enhanced turbulent dispersion in the disk also leads to quenching of
star formation. Whether positive or negative feedback dominates depends on jet
power, ISM density, jet orientation with respect to the disc, and the
time-scale under consideration. Qualitatively, our simulations compare
favourably with kinematic and morphological signatures of several observed
galaxies such as NGC 1052, NGC 3079, 3C 326 and 3C 293.
