Impact of dust cooling on direct collapse black hole formation

Abstract

Observations of quasars at $z>6$ suggest the presence of black holes with a few times $10^9{\mathrm{M}}_{\odot }$. Numerous models have been proposed to explain their existence including the direct collapse which provides massive seeds of $10^5{\mathrm{M}}_{\odot }$. The isothermal direct collapse requires a strong Lyman-Werner flux to quench ${\mathrm{H}}_2$ formation in massive primordial halos. In this study, we explore the impact of trace amounts of metals and dust enrichment. We perform three dimensional cosmological simulations for two halos of $>10^7{\mathrm{M}}_{\odot }$ with $Z/{\mathrm{Z}}_{\odot }=10^{-4}-10^{-6}$ illuminated by an intense Lyman Werner flux of ${\mathrm{J}}_{21}=10^5$. Our results show that initially the collapse proceeds isothermally with $\mathrm{T}\sim 8000$ K but dust cooling becomes effective at densities of $10^8-10^{12}\mathrm{c}{\mathrm{m}}^{-3}$ and brings the gas temperature down to a few 100-1000 K for $Z/{\mathrm{Z}}_{\odot }\ge 10^{-6}$. No gravitationally bound clumps are found in $Z/{\mathrm{Z}}_{\odot }\le 10^{-5}$ cases by the end of our simulations in contrast to the case with $Z/{\mathrm{Z}}_{\odot }=10^{-4}$. Large inflow rates of $\ge 0.1{\mathrm{M}}_{\odot }/yr$ are observed for $Z/{\mathrm{Z}}_{\odot }\le 10^{-5}$ similar to a zero-metallicity case while for $Z/{\mathrm{Z}}_{\odot }=10^{-4}$ the inflow rate starts to decline earlier due to the dust cooling and fragmentation. For given large inflow rates a central star of $\sim 10^4{\mathrm{M}}_{\odot }$ may form for $Z/{\mathrm{Z}}_{\odot }\le 10^{-5}$.

Accepted for publication in ApJ, comments are still welcome

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