Radiation Hydrodynamical Simulations of the Birth of Intermediate-Mass Black Holes in the First Galaxies

Abstract

The leading contenders for the seeds of $z>6$ quasars are direct-collapse black holes (DCBHs) forming in atomically-cooled halos at $z\sim$ 20. However, the Lyman-Werner (LW) UV background required to form DCBHs of 10${}^5$ \Ms\ are extreme, about 10${}^4$ J${}_{21}$, and may have been rare in the early universe. Here we investigate the formation of intermediate-mass black holes (IMBHs) under moderate LW backgrounds of 100 and 500 J${}_{21}$ that were much more common at early times. These backgrounds allow halos to grow to a few 10${}^6$ - 10${}^7$ \Ms\ and virial temperatures of nearly 10${}^4$ K before collapsing but do not completely sterilize them of H${}_2$. Gas collapse then proceeds via Ly$\alpha$ and rapid H${}_2$ cooling at rates that are 10 - 50 times those in normal Pop III star-forming haloes but less than those in purely atomically-cooled haloes. Pop III stars accreting at such rates become blue and hot, and we find that their ionizing UV radiation limits their final masses to 1800 - 2800 \Ms\, at which they later collapse to IMBHs. Moderate LW backgrounds thus produced IMBHs in far greater numbers than DCBHs in the early universe.

arXiv commentPublished in MNRAS, comments welcome

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