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Intermediate-mass black holes (IMBHs: masses between $100 - 10^{6}M_{\odot}$) historically comprise of an elusive population compared tostellar-mass and supermassive BHs. Recently IMBHs have started to be observedat the centers of low-mass galaxies. We perform cosmological hydrodynamicalsimulations of $(2 h^{-1} ~ {\rm Mpc})^3$ comoving boxes and investigate thegrowth and feedback of central IMBHs in dwarf galaxies (DGs). The earliest BHsappear at $z \sim 18 - 25$, and grow thereafter by accreting gas and by mergerwith other BHs. We find that, starting from $10^{2} M_{\odot}$, it is possibleto build up IMBHs of a few$\times 10^{5} - 10^{6} M_{\odot}$ by $z = 5$, whenthe BHs are seeded in halos less massive than $4 \times 10^{7} M_{\odot}$. TheBH accretion rates increase with time, and reaches $\dot{M}_{\rm BH} = (0.2 -0.8) \dot{M}_{\rm Edd}$ for the massive IMBHs by $z = 4$. The star formationrate density (SFRD) evolution of the DGs (stellar mass $10^{5} - 10^{8}M_{\odot}$) has a peak plateau between $z = 4 - 6$. Star formation is quenchedbetween $z = 9 - 4$. The SFRD is reduced by factors up to $3$, when the BHshave grown to a few times $10^5 M_{\odot}$. Even in the presence of strongerSN-driven mass ejection, the BHs continue to grow up to $z \sim 6$, sustainedby gas inflows driven by galaxy mergers and interactions in a cosmologicalenvironment. Our conclusions, based on numerical simulation results, supportthe scenario that early feedback from IMBHs in gas-rich DGs at $z = 5 - 8$ canpotentially solve several anomalies in the DG mass range within the concordance$\Lambda$CDM cosmological scenario (Silk 2017). Our results suggest that IMBHsat DG centers grow faster than their host galaxies in the early Universe, andthe resulting BH feedback turns the DGs and the BHs dormant.

Intermediate-Mass Black Hole Growth and Feedback in Dwarf Galaxies at High Redshifts