On the connection between AGN radiative feedback and massive black hole spin

We present a novel implementation for active galactic nucleus (AGN) feedback through ultra-fast winds in the code gizmo. Our feedback recipe accounts for the angular dependence of radiative feedback upon black hole spin. We self-consistently evolve in time i) the gas accretion process from resolved scales to an unresolved AGN disc, ii) the evolution of the spin of the massive black hole (MBH), iii) the injection of AGN-driven winds into the resolved scales, and iv) the spin-induced anisotropy of the overall feedback process. We test our implementation by following the propagation of the wind-driven outflow into a homogeneous medium, and we compare the results against simple analytical models. Then, we consider an isolated galaxy setup and there we study the impact of the AGN feedback on the evolution of the MBH and the of the host galaxy. We find that: i) AGN feedback limits the gas inflow that powers the MBH, with a consequent weak impact on the host galaxy characterized by a star formation (SF) suppression of about a factor of two in the nuclear region; ii) the impact of AGN feedback on the host galaxy and on MBH growth is primarily determined by the AGN luminosity, rather than by its angular pattern set by the MBH spin; iii) the imprint of the angular pattern of the AGN radiation emission manifest in a more clear way at high accretion rates. At such high rates the more isotropic angular patterns, proper to higher spin values, sweep away gas in the nuclear region more easily, hence causing a slower MBH mass and spin growths and a higher quenching of the SF. We argue that the influence of spin-dependent anisotropy of AGN feedback on MBH and galaxy evolution is likely to be relevant in those scenarios characterized by high and prolonged MBH accretion episodes and by high AGN wind-galaxy coupling. Such conditions are more frequently met in galaxy mergers and/or high redshift galaxies.