Halo Mergers Enhance the Growth of Massive Black Hole Seeds

Abstract

High redshift observations of 10${}^9$ M${}_{\odot }$ supermassive black holes (SMBHs) at $z\sim 7$ and `Little Red Dots' that may host overmassive black holes at $z>4$ suggests the existence of so-called heavy seeds (>1000 M${}_{\odot }$) in the early Universe. Recent work has suggested that the rapid assembly of halos may be the key to forming heavy seeds early enough in the Universe to match such observations without the need for extreme radiation fields or dark matter streaming velocities. We perform simulations of BH seed formation in 4 distinct idealised halo collapse scenarios; an isolated 10${}^6$ M${}_{\odot }$ minihalo, an isolated 10${}^7$ M${}_{\odot }$ atomic halo, the direct collision of two 10${}^7$ M${}_{\odot }$ halos and a fly-by collision of two 10${}^7$ M${}_{\odot }$ halos. We have shown that halo collisions create a central environment of enhanced density, inside which BH seeds can accrete at enhanced rates. For direct collisions, the gas density peaks are disrupted by the interaction, as the collisionless DM peaks pass through each other while the colliding gas is left in the center, removing the sink particle from its accretion source. When the central density peaks instead experience a fly-by interaction, the sink particle remains embedded in the dense gas and maintains enhanced accretion rates throughout the simulated period when compared to the isolated halo cases. Here the final mass of the sink particle achieved a factor of 2 greater in mass than in the isolated atomic halo case, and a factor of 3 greater than the minihalo case, reaching 10${}^4$ M${}_{\odot }$ via its 0.03 pc accretion radius. As the maximum halo mass before collapse is determined by the atomic cooling limit of a few times 10${}^7$ M${}_{\odot }$, the ability of halo-halo mergers to further boost accretion rates onto the central object may play a crucial role in growing SMBH seeds.

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