The Response of Metal Rich Gas to X-Ray Irradiation from a Massive Black
  Hole at High Redshift: Proof of Concept
  Observational studies show that there is a strong link between the formation
and evolution of galaxies and the growth of supermassive black holes (SMBH) at
their centers. However, the underlying physics of this observed relation is
poorly understood. In order to study the effects of X-ray radiation on the
surroundings of the black hole, we implement X-ray Dominated Region (XDR)
physics into Enzo and use the radiation transport module Moray to calculate the
radiative transfer for a polychromatic spectrum. In this work, we investigate
the effects of X-ray irradiation, produced by a central massive black hole
(MBH) with a mass of M = 5x10^4 M_(solar), on ambient gas with solar and zero
metallicity. We find that in the solar metallicity case, due to high opacity of
the metals, the energy deposition rate in the central region (< 20 pc) is high
and hence the temperatures in the center are on the order of 10^(5-7) K.
Moreover, due to the cooling ability and high intrinsic opacity of solar
metallicity gas, column densities of 10^(24) cm^(-2) are reached at a radius of
20 pc from the MBH. These column densities are about 3 orders of magnitudes
higher than in the zero metallicity case. Furthermore, in the zero metallicity
case an X-ray induced H II region is formed already after 5.8 Myr. This causes
a significant outflow of gas (~8x10^6 M_(solar) from the central region, with
the gas reaching outflow velocities up to ~100 km s^(-1). At later times, ~23
Myr after we insert the MBH, we find that the solar metallicity case also
develops an X-ray induced H II region, but delayed by ~17 Myr.
