de Gouveia Dal Pino, Elisabete M.
Total Authors: 2
 Univ Sao Paulo, IAG, Inst Astron Geofis & Ciencias Atmosfer, Rua Matao 1226, BR-05508090 Sao Paulo - Brazil
Total Affiliations: 1
Monthly Notices of the Royal Astronomical Society;
Web of Science Citations:
Intermediate-mass black holes (IMBHs; masses between ) historically comprise of an elusive population compared to stellar-mass and supermassive black holes (BHs). Recently, IMBHs have started to be observed at the centres of low-mass galaxies. We perform cosmological hydrodynamical simulations of comoving boxes and investigate the growth and feedback of central IMBHs in dwarf galaxies (DGs). The earliest BHs appear at z similar to 18-25 and grow thereafter by accreting gas and by merger with other BHs. We find that, starting from , it is possible to build up IMBHs of a few by z = 5, when the BHs are seeded in haloes less massive than . The BH accretion rates increase with time and reach for the massive IMBHs by z = 4. The star formation rate density (SFRD) evolution of the DGs (stellar mass ) has a peak plateau between z = 4 and 6. Star formation is quenched between z = 9 and 4. The SFRD is reduced by factors up to 3 when the BHs have grown to a few times . Even in the presence of stronger supernova (SN)-driven mass ejection, the BHs continue to grow up to z similar to 6, sustained by gas inflows driven by galaxy mergers and interactions in a cosmological environment. Our conclusions, based on numerical simulation results, support the scenario that early feedback from IMBHs in gas-rich DGs at z = 5-8 can potentially solve several anomalies in the DG mass range within the concordance Lambda cold dark matter (Lambda CDM) cosmological scenario (Silk 2017). Our results suggest that IMBHs at DG centres grow faster than their host galaxies in the early Universe, and the resulting BH feedback turns the DGs and the BHs dormant. (AU)