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We present a novel implementation for active galactic nucleus (AGN) feedbackthrough ultra-fast winds in the code gizmo. Our feedback recipe accounts forthe angular dependence of radiative feedback upon black hole spin. Weself-consistently evolve in time i) the gas accretion process from resolvedscales to an unresolved AGN disc, ii) the evolution of the spin of the massiveblack hole (MBH), iii) the injection of AGN-driven winds into the resolvedscales, and iv) the spin-induced anisotropy of the overall feedback process. Wetest our implementation by following the propagation of the wind-driven outflowinto a homogeneous medium, and we compare the results against simple analyticalmodels. Then, we consider an isolated galaxy setup and there we study theimpact of the AGN feedback on the evolution of the MBH and the of the hostgalaxy. We find that: i) AGN feedback limits the gas inflow that powers theMBH, with a consequent weak impact on the host galaxy characterized by a starformation (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 primarilydetermined by the AGN luminosity, rather than by its angular pattern set by theMBH spin; iii) the imprint of the angular pattern of the AGN radiation emissionmanifest in a more clear way at high accretion rates. At such high rates themore isotropic angular patterns, proper to higher spin values, sweep away gasin the nuclear region more easily, hence causing a slower MBH mass and spingrowths and a higher quenching of the SF. We argue that the influence ofspin-dependent anisotropy of AGN feedback on MBH and galaxy evolution is likelyto be relevant in those scenarios characterized by high and prolonged MBHaccretion episodes and by high AGN wind-galaxy coupling. Such conditions aremore frequently met in galaxy mergers and/or high redshift galaxies.

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