  There is growing evidence for physical influence between supermassive black
holes and their host galaxies. We present a case study of nearby galaxy NGC
7582, for which we find evidence that galactic substructure plays an important
role in affecting the collimation of ionized outflows as well as contributing
to the heavy active galactic nucleus (AGN) obscuration. This result contrasts
with a simple, small-scale AGN torus model, according to which AGN wind
collimation may take place inside the torus itself, at subparsec scale. Using
3D spectroscopy with the MUSE instrument, we probe the kinematics of the
stellar and ionized gas components as well as the ionization state of the gas
from a combination of emission line ratios. We report for the first time a
kinematically distinct core (KDC) in NGC 7582, on a scale of ~600pc. This KDC
coincides spatially with dust lanes and starbursting complexes previously
observed. We interpret it as a circumnuclear ring of stars and dusty, gas-rich
material. We obtain a clear view of the outflowing cones over kpc scales, and
demonstrate that they are predominantly photoionized by the central engine. We
detect the back cone (behind the galaxy), and confirm previous results of a
large nuclear obscuration of both the stellar continuum and HII regions. While
we tentatively associate the presence of the KDC to a large-scale bar and/or a
minor galaxy merger, we stress the importance of gaining a better understanding
of the role of galaxy substructure in controlling the fueling, feedback and
obscuration of AGN.
