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