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We study the interaction of feedback from active galactic nuclei (AGN) and amulti-phase interstellar medium (ISM), in simulations including explicitstellar feedback, multi-phase cooling, accretion-disk winds, and Comptonheating. We examine radii ~0.1-100 pc around a black hole (BH), where theaccretion rate onto the BH is determined and where AGN-powered winds andradiation couple to the ISM. We conclude: (1) The BH accretion rate isdetermined by exchange of angular momentum between gas and stars ingravitational instabilities. This produces accretion rates ~0.03-1 Msun/yr,sufficient to power luminous AGN. (2) The gas disk in the galactic nucleusundergoes an initial burst of star formation followed by several Myrs wherestellar feedback suppresses the star formation rate (SFR). (3) AGN windsinjected at small radii with momentum fluxes ~L/c couple efficiently to the ISMand have dramatic effects on ISM properties within ~100 pc. AGN winds suppressthe nuclear SFR by factors ~10-30 and BH accretion rate by factors ~3-30. Theyincrease the outflow rate from the nucleus by factors ~10, consistent withobservational evidence for galaxy-scale AGN-driven outflows. (4) With AGNfeedback, the predicted column density distribution to the BH is consistentwith observations. Absent AGN feedback, the BH is isotropically obscured andthere are not enough optically-thin sightlines to explain Type-I AGN. A'torus-like' geometry arises self-consistently as AGN feedback evacuates gas inpolar regions.

Stellar and Quasar Feedback in Concert: Effects on AGN Accretion, Obscuration, and Outflows