Feedback by AGN Jets and Wide-Angle Winds on a Galactic Scale

TL;DR

This study uses 3D hydrodynamic simulations to compare the effects of AGN jets and winds on galaxy evolution, revealing distinct feedback mechanisms and their influence on star formation and gas dynamics.

Contribution

It provides a comparative analysis of jet and wind feedback in galaxies, highlighting the impact of wind inclination on star formation and gas distribution, which is a novel aspect.

Findings

Jet feedback is energy-driven, wind feedback is momentum-driven.

Winds at 90° inclination induce higher star formation rates.

All simulations show cavity formation and positive feedback at larger radii.

Abstract

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.