Feedback from active galactic nuclei: energy- versus momentum-driving

We employ hydrodynamical simulations using the moving-mesh code AREPO to investigate the role of energy and momentum input from active galactic nuclei (AGN) in driving large-scale galactic outflows. We start by reproducing analytic solutions for both energy-and momentum-driven outflowing shells in simulations of a spherical isolated dark matter potential with gas in hydrostatic equilibrium and with no radiative cooling. We confirm that for this simplified setup, galactic outflows driven by a momentum input rate of order L-Edd/c can establish an M-BH-sigma relation with slope and normalization similar to that observed. We show that momentum input at a rate of L-Edd/c is however insufficient to drive efficient outflows once cooling and gas inflows as predicted by cosmological simulations at resolved scales are taken into account. We argue that observed large-scaleAGN-driven outflows are instead likely to be energy-driven and show that such outflows can reach momentum fluxes exceeding 10L(Edd)/c within the innermost 10 kpc of the galaxy. The outflows are highly anisotropic, with outflow rates and a velocity structure found to be inadequately described by spherical outflow models. We verify that the hot energy-driven outflowing gas is expected to be strongly affected by metal-line cooling, leading to significant amounts (greater than or similar to 10(9)M(circle dot)) of entrained cold gas.