Witnessing the birth of a supermassive protostar

Abstract

The detection of $\mathrm{z}>6$ quasars reveals the existence of supermassive black holes of a few $10^9{\mathrm{M}}_{\odot }$. One of the potential pathways to explain their formation in the infant universe is the so-called direct collapse model which provides massive seeds of $10^5-10^6{\mathrm{M}}_{\odot }$. An isothermal direct collapse mandates that halos should be of a primordial composition and the formation of molecular hydrogen remains suppressed in the presence of a strong Lyman Werner flux. In this study, we perform high resolution cosmological simulations for two massive primordial halos employing a detailed chemical model which includes ${\mathrm{H}}^{-}$ cooling as well as realistic opacities for both the bound-free ${\mathrm{H}}^{-}$ emission and the Rayleigh scattering of hydrogen atoms. We are able to resolve the collapse up to unprecedentedly high densities of $\sim 10^{-3}g/c{\mathrm{m}}^3$ and to scales of about $10^{-4}$ AU. Our results show that the gas cools down to $\sim$ 5000 K in the presence of ${\mathrm{H}}^{-}$ cooling, and induces fragmentation at scales of about 8000 AU in one of the two simulated halos, which may lead to the formation of a binary. In addition, fragmentation also occurs on the AU scale in one of the halos but the clumps are expected to merge on short time scales. Our results confirm that ${\mathrm{H}}^{-}$ cooling does not prevent the formation of a supermassive star and the trapping of cooling radiation stabilises the collapse on small scales.

Accpeted version, to appear in MNRAS, comments are still welcome and high resolution version is available at http://www2.iap.fr/users/latif/DCBH.pdf

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