High-redshift Galaxy Formation with Self-consistently Modeled Stars and
  Massive Black Holes: Stellar Feedback and Quasar Growth
  As computational resolution of modern cosmological simulations reach ever so
close to resolving individual star-forming clumps in a galaxy, a need for
"resolution-appropriate" physics for a galaxy-scale simulation has never been
greater. To this end, we introduce a self-consistent numerical framework that
includes explicit treatments of feedback from star-forming molecular clouds
(SFMCs) and massive black holes (MBHs). In addition to the thermal supernovae
feedback from SFMC particles, photoionizing radiation from both SFMCs and MBHs
is tracked through full 3-dimensional ray tracing. A mechanical feedback
channel from MBHs is also considered. Using our framework, we perform a
state-of-the-art cosmological simulation of a quasar-host galaxy at z~7.5 for
~25 Myrs with all relevant galactic components such as dark matter, gas, SFMCs,
and an embedded MBH seed of ~> 1e6 Ms. We find that feedback from SFMCs and an
accreting MBH suppresses runaway star formation locally in the galactic core
region. Newly included radiation feedback from SFMCs, combined with feedback
from the MBH, helps the MBH grow faster by retaining gas that eventually
accretes on to the MBH. Our experiment demonstrates that previously undiscussed
types of interplay between gas, SFMCs, and a MBH may hold important clues about
the growth and feedback of quasars and their host galaxies in the high-redshift
Universe.
