Parameterizing the Outflow from a Central Black Hole in Dwarf Spheroidal
  Galaxies: A 3D Hydrodynamic Simulation
  Large galaxies harbor massive central black holes and their feedback causes a
substantial impact in their evolution. Recently, observations suggested that
dwarf galaxies might host black holes in their centers, but with lower masses
(intermediate-mass black holes - IMBH). The impact of such IMBHs on the
evolution of the dwarf spheroidal galaxies (dSphs), however, has not been so
far properly analysed. In this work, we investigate the effects of an outflow
from an IMBH on the gas dynamics in dSph galaxies by means of non-cosmological,
three-dimensional hydrodynamic simulations, letting the galactic gas
distribution evolve over 3 Gyr under the influence of the IMBH's outflow and
supernova feedback. All simulations have a numerical resolution of 20.0 pc
cell$^{-1}$. Two scenarios are considered to infer the differences in the
propagation of the outflow, one with a homogeneous ISM and another one with
inhomogeneities caused by supernovae feedback. A minimal initial speed and a
minimal initial density are required for the outflow to propagate, with the
values depending on the conditions of the medium. In an unperturbed medium, the
outflow propagates freely in both directions with the same velocity (lower than
the initial one), removing a small fraction of the gas from the galaxy (the
exact fraction depends on the initial physical conditions of the outflow).
However, in an inhomogeneous ISM, the impact of the outflow is substantially
reduced, and its contribution to the removal of gas from the galaxy is almost
negligible.
