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We study the interactions of a relativistic jet with a dense turbulentgaseous disk of radius $\sim 2$ kpc. We have performed a suite of simulationswith 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 inflatedby the jet and its back-flow compresses the disk at the outer edges, drivinginflows within the disk. C) Jets inclined towards the disk couple more stronglywith the disk and launch sub-relativistic, wide-angle outflows along the minoraxis. D) Shocks driven directly by the jet and the jet-driven energy bubbleraise the velocity dispersion throughout the disk by several times its initialvalue. E) Compression by the jet-driven shocks can enhance the star formationrate in the disk, especially in a ring-like geometry close to the axis.However, enhanced turbulent dispersion in the disk also leads to quenching ofstar formation. Whether positive or negative feedback dominates depends on jetpower, ISM density, jet orientation with respect to the disc, and thetime-scale under consideration. Qualitatively, our simulations comparefavourably with kinematic and morphological signatures of several observedgalaxies such as NGC 1052, NGC 3079, 3C 326 and 3C 293.

Relativistic jet feedback III: feedback on gas disks