A super-massive black hole (BH) sits at the center of most, if not
all, bulge galaxies. While the black hole gravitational potential
dominates the gas dynamics on a tiny (~pc^3) spatial scale only, the
tight relation between black hole mass and stellar velocity
dispersion in the bulge suggests that black holes can affect the
interstellar gas and the star formation across the whole host galaxy.
This happens through a still poorly understood process called
"AGN feedback". In this talk I review the observational evidence for
"nuclear" (i.e. accretion disk, torus) winds playing a fundamental
role in AGN feedback. While the exact geometry of the outflows is
still subject to large uncertainties, kinetic outflow rates are
consistent with the feedback requirements set by cosmological
simulations of galaxy evolution in powerful quasars, as well as
(and more surprisingly) in some lower-luminosity Seyfert galaxies.