  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.
