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We explore the effect of momentum-driven winds representing radiationpressure driven outflows from accretion onto supermassive black holes in a setof numerical hydrodynamical simulations. We explore two matched sets ofcosmological zoom-in runs of 24 halos with masses ~$10^{12.0}-10^{13.4}$ M_sunrun with two different feedback models. Our `NoAGN' model includes stellarfeedback via UV heating, stellar winds and supernovae, photoelectric heatingand cosmic X-ray background heating from a meta-galactic background. Ourfiducial `MrAGN' model is identical except that it also includes a model forblack hole seeding and accretion, as well as heating and momentum injectionassociated with the radiation from black hole accretion. Our MrAGN modellaunches galactic outflows which result in both `ejective' feedback - theoutflows themselves which drive gas out of galaxies - and `preventative'feedback, which suppresses the inflow of new and recycling gas. As much as 80 %of outflowing galactic gas can be expelled, and accretion can be suppressed byas much as a factor of 30 in the MrAGN runs when compared with the NoAGN runs.The histories of NoAGN galaxies are recycling-dominated, with ~70% of materialthat leaves the galaxy eventually returning, and the majority of outflowing gasre-accretes on 1 Gyr timescales without AGN feedback. Outflowing gas in theMrAGN runs has higher characteristic velocity (500 - 1,000 km/s versus 100-300km/s for outflowing NoAGN gas) and travels as far as a few Mpcs. Only ~10% ofejected material is re-accreted in the MrAGN galaxies.

Momentum-driven Winds from Radiatively Efficient Black Hole Accretion and Their Impact on Galaxies