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We investigate the effects of massive black hole growth on the structuralevolution of dwarf galaxies within the Romulus25 cosmological hydrodynamicalsimulation. We study a sample of 228 central, isolated dwarf galaxies withstellar masses $M_{star} < 10^{10} M_\odot$ and a central BH. We find that thelocal $M_{BH} - M_{star}$ relation exhibits a high degree of scatter below$M_{star} < 10^{10} M_\odot$, which we use to classify BHs as overmassive orundermassive relative to their host $M_{star}$. Overmassive BHs grow through amixture of BH mergers and relatively high average accretion rates, whileundermassive BHs grow slowly through accretion. We find that isolated dwarfgalaxies that host overmassive BHs also follow different evolutionary tracksrelative to their undermassive BH counterparts, building up their stars anddark matter earlier and experiencing star formation suppression starting around$z=2$. By $z=0.05$, overmassive BH hosts above $M_{star} > 10^{9} M_\odot$ aremore likely to exhibit lower central stellar mass density, lower HI gascontent, and lower star formation rates than their undermassive BHcounterparts. Our results suggest that overmassive BHs in isolated galaxiesabove $M_{star} > 10^{9} M_\odot$ are capable of driving feedback, in manycases suppressing and even quenching star formation by late times.

Black Hole Growth and Feedback in Isolated Romulus25 Dwarf Galaxies