  Active galactic nuclei (AGN) are massive black holes (BHs) caught in the act
of accreting gas at the centre of their host galaxies. Part of the accreting
mass is converted to energy and released into the surrounding medium, in a
process loosely referred to as AGN feedback. Most numerical simulations include
AGN feedback as a sub-grid model, wherein energy or momentum (or both) is
coupled to the nearby gas. In this work, we implement a new momentum-driven
model in the hydrodynamics code GIZMO, in which accretion from large scales is
mediated by a sub-grid accretion disc model, and gas particles are
stochastically kicked over a bi-conical region, to mimic observed kinetic
winds. The feedback cone's axis can be set either parallel to the angular
momentum of the gas surrounding the BH or to the BH spin direction, which is
self-consistently evolved within the accretion-disc model. Using a
circumnuclear disc (CND) as a test bed, we find that (i) the conical shape of
the outflow is always visible and is weakly dependent on the launching
orientation and aperture, resulting in comparable mass inflows and outflows;
(ii) the cone's orientation is also similar amongst our tests, and it is not
always the same as the initial value, due to the interaction with the CND
playing a crucial role in shaping the outflow; and (iii) the velocity of the
outflow, instead, differs and strongly depends on the interplay with the CND.

Astrophysics of Galaxies;Cosmology and Nongalactic Astrophysics;High Energy Astrophysical Phenomena