  Large-scale, broad outflows are common in active galaxies. In systems where
star formation coexists with an AGN, it is unclear yet the role that both play
on driving the outflows. In this work we present three-dimensional
radiative-cooling MHD simulations of the formation of these outflows,
considering the feedback from both the AGN and supernovae-driven winds. We find
that a large-opening-angle AGN wind develops fountain structures that make the
expanding gas to fall back. Furthermore, it exhausts the gas near the nuclear
region, extinguishing star formation and accretion within a few 100.000 yr,
which establishes the duty cycle of these outflows. The AGN wind accounts for
the highest speed features in the outflow with velocities around 10.000 km
s$^{-1}$ (as observed in UFOs), but these are not as cold and dense as required
by observations of molecular outflows. The SNe-driven wind is the main
responsible for the observed mass-loading of the outflows.
