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Accretion of matter onto central Black Holes (BHs) in galaxies liberatesenormous amounts of feedback energy, which influence the formation andevolution of structures, affecting the environment from pc to Mpc scales. TheseBHs are usually Supermassive BHs (SMBHs: mass $\geq 10^6 M_{\odot}$) existingat the centers of active galactic nuclei (AGN), which are widely observedthrough their multi-wavelength emission at all cosmic epochs. The SMBH energyoutput is often observed as powerful AGN outflows in a wide variety of forms.Relatively recently, Intermediate-Mass BHs (IMBHs: mass = $100 - 10^6M_{\odot}$) 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 oflow-luminosity AGN. We have performed Cosmological Hydrodynamical Simulationsto 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 codeGADGET-3, and include metal cooling, star formation, chemical enrichment,stellar evolution, supernova feedback, AGN accretion and feedback. Analyzingthe simulation output in post-processing, we investigate the growth of thefirst 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 quantifythe impact of SMBHs and IMBHs on their host galaxies, especially the effects onquenching star-formation. We also study the corresponding BH outflowproperties.

Supermassive and Intermediate-Mass Black Hole Growth at Galaxy Centers and Resulting Feedback using Cosmological Simulations