Supermassive and Intermediate-Mass Black Hole Growth at Galaxy Centers
  and Resulting Feedback using Cosmological Simulations
  Accretion of matter onto central Black Holes (BHs) in galaxies liberates
enormous amounts of feedback energy, which influence the formation and
evolution of structures, affecting the environment from pc to Mpc scales. These
BHs are usually Supermassive BHs (SMBHs: mass $\geq 10^6 M_{\odot}$) existing
at the centers of active galactic nuclei (AGN), which are widely observed
through their multi-wavelength emission at all cosmic epochs. The SMBH energy
output is often observed as powerful AGN outflows in a wide variety of forms.
Relatively recently, Intermediate-Mass BHs (IMBHs: mass = $100 - 10^6
M_{\odot}$) have started to be observed hosted in Dwarf Galaxy (DG) centers.
Some of the central IMBHs in DGs show signatures of activity in the form of
low-luminosity AGN. We have performed Cosmological Hydrodynamical Simulations
to probe SMBHs in high-z quasars (Barai et al. 2018), and IMBHs in DGs (Barai &
de Gouveia Dal Pino 2019). Our simulations employ the 3D TreePM SPH code
GADGET-3, and include metal cooling, star formation, chemical enrichment,
stellar evolution, supernova feedback, AGN accretion and feedback. Analyzing
the simulation output in post-processing, we investigate the growth of the
first IMBHs, and the growth of the first SMBHs, their impact on star-formation,
as well as their co-evolution with the respective host galaxies. We quantify
the impact of SMBHs and IMBHs on their host galaxies, especially the effects on
quenching star-formation. We also study the corresponding BH outflow
properties.
