%0 Generic %1 regan2017rapid %A Regan, John %A Visbal, Eli %A Wise, John H. %A Haiman, Zoltan %A Johansson, Peter H. %A Bryan, Greg L. %D 2017 %K black collapse direct hole simulation %T Rapid Formation of Massive Black Holes in close proximity to Embryonic Proto-Galaxies %U http://arxiv.org/abs/1703.03805 %X The Direct Collapse Black Hole (DCBH) scenario provides a solution for forming the massive black holes powering bright quasars observed in the early Universe. A prerequisite for forming a DCBH is that the formation of (much less massive) Population III stars be avoided - this can be achieved by destroying H$_2$ via Lyman-Werner (LW) radiation (E$_LW$ = 12.6 eV). We find that two conditions must be met in the proto-galaxy that will host the DCBH. First, prior star formation must be delayed; this can be achieved with a background LW flux of J$_BG 100\ J_21$. Second, an intense burst of LW radiation from a neighbouring star-bursting proto-galaxy is required, just before the gas cloud undergoes gravitational collapse, to finally suppress star formation completely. We show here for the first time using high-resolution hydrodynamical simulations, including full radiative transfer, that this low-level background, combined with tight synchronisation and irradiation of a secondary proto-galaxy by a primary proto-galaxy, inevitably moves the secondary proto-galaxy onto the isothermal atomic cooling track, without the deleterious effects of either photo-evaporating the gas or polluting it by heavy elements. These, atomically cooled, massive proto-galaxies are expected to ultimately form a DCBH of mass $10^4 - 10^5 M_ødot$.

@misc{regan2017rapid, abstract = {The Direct Collapse Black Hole (DCBH) scenario provides a solution for forming the massive black holes powering bright quasars observed in the early Universe. A prerequisite for forming a DCBH is that the formation of (much less massive) Population III stars be avoided - this can be achieved by destroying H$_2$ via Lyman-Werner (LW) radiation (E$_{\rm{LW}}$ = 12.6 eV). We find that two conditions must be met in the proto-galaxy that will host the DCBH. First, prior star formation must be delayed; this can be achieved with a background LW flux of J$_{\rm BG} \gtrsim 100\ J_{21}$. Second, an intense burst of LW radiation from a neighbouring star-bursting proto-galaxy is required, just before the gas cloud undergoes gravitational collapse, to finally suppress star formation completely. We show here for the first time using high-resolution hydrodynamical simulations, including full radiative transfer, that this low-level background, combined with tight synchronisation and irradiation of a secondary proto-galaxy by a primary proto-galaxy, inevitably moves the secondary proto-galaxy onto the isothermal atomic cooling track, without the deleterious effects of either photo-evaporating the gas or polluting it by heavy elements. These, atomically cooled, massive proto-galaxies are expected to ultimately form a DCBH of mass $10^4 - 10^5 M_{\odot}$.}, added-at = {2017-03-14T09:54:35.000+0100}, author = {Regan, John and Visbal, Eli and Wise, John H. and Haiman, Zoltan and Johansson, Peter H. and Bryan, Greg L.}, biburl = {https://www.bibsonomy.org/bibtex/2faa7877c38b963f217c3a16b5a67bad2/miki}, description = {[1703.03805] Rapid Formation of Massive Black Holes in close proximity to Embryonic Proto-Galaxies}, interhash = {717bf5be1b523600f4852b7686c6d83e}, intrahash = {faa7877c38b963f217c3a16b5a67bad2}, keywords = {black collapse direct hole simulation}, note = {cite arxiv:1703.03805Comment: Published in Nature Astronomy, March 13th 2017}, timestamp = {2017-03-14T09:54:35.000+0100}, title = {Rapid Formation of Massive Black Holes in close proximity to Embryonic Proto-Galaxies}, url = {http://arxiv.org/abs/1703.03805}, year = 2017 }