Simulations of AGN-driven Galactic Outflow Morphology and Content

Abstract Using a series of 3D relativistic hydrodynamical simulations active galactic nuclei (AGN) we investigate how AGN power, clumpy interstellar medium (ISM) structure, and jet angle with respect to the disk affect morphology content resulting outflow. For low-power across three orders magnitude luminosities (10 41 –10 43 erg s −1 ) our did not show significant changes either or total mass Changing galaxy small in outflow factor 2–3. Jets perpendicular created hot single-phase outflows, while jets close parallel multiphase outflows equal parts warm hot, cold gas. Overall final depends primarily on impacts interacts large, dense clouds ISM. These can disrupt, deflect, split, suppress jet, preventing it from leaving as coherent structure. But for > 10 44 ISM played minor role determining an undisrupted disk. The is different AGNs versus high-power dependent structure within first kiloparsec surrounding AGN.