Light, medium-weight or heavy? The nature of the first supermassive black hole seeds
Federica Sassano,Raffaella Schneider,Raffaella Schneider,Rosa Valiante,Kohei Inayoshi,Sunmyon Chon,Kazuyuki Omukai,Lucio Mayer,Pedro R. Capelo +8 more
TLDR
In this article, the relative role of three seed populations in the formation of supermassive black holes (SMBHs) within an Eddington-limited gas accretion scenario was investigated.Abstract:
Observations of hyper-luminous quasars at $z>6$ reveal the rapid growth of supermassive black holes (SMBHs $>10^9 \rm M_{\odot}$) whose origin is still difficult to explain. Their progenitors may have formed as remnants of massive, metal free stars (light seeds), via stellar collisions (medium-weight seeds) and/or massive gas clouds direct collapse (heavy seeds). In this work we investigate for the first time the relative role of these three seed populations in the formation of $z>6$ SMBHs within an Eddington-limited gas accretion scenario. To this aim, we implement in our semi-analytical data-constrained model a statistical description of the spatial fluctuations of Lyman-Werner (LW) photo-dissociating radiation and of metal/dust enrichment. This allows us to set the physical conditions for BH seeds formation, exploring their relative birth rate in a highly biased region of the Universe at $z>6$. We find that the inclusion of medium-weight seeds does not qualitatively change the growth history of the first SMBHs: although less massive seeds ($ 15$.read more
Citations
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The low-end of the black hole mass function at cosmic dawn
Alessandro Trinca,Raffaella Schneider,Rosa Valiante,L. Graziani,Luca Zappacosta,Francesco Shankar +5 more
TL;DR: In this paper , the authors investigated the early evolution of the first supermassive black holes (SMBHs) by constraining their distribution in mass and luminosity at z > 4, focusing on the poorly explored low-mass end of the nuclear black hole (BH) distribution down to z ' 4.
Journal ArticleDOI
The X–shooter/ALMA Sample of Quasars in the Epoch of Reionization. II. Black Hole Masses, Eddington Ratios, and the Formation of the First Quasars
Emanuele Paolo Farina,Jan-Torge Schindler,Fabian Walter,Eduardo Bañados,Frederick B. Davies,Roberto Decarli,Anna-Christina Eilers,Xiaohui Fan,Joseph F. Hennawi,Chiara Mazzucchelli,Romain A. Meyer,Benny Trakhtenbrot,Marta Volonteri,Feige Wang,Gabor Worseck,Jinyi Yang,Thales A. Gutcke,Bram Venemans,Sarah E. I. Bosman,Tiago Costa,G. De Rosa,Alyssa B. Drake,Masafusa Onoue +22 more
TL;DR: In this paper , the first supermassive black holes reside in massive halos at z ≳ 6 and lead the first stages of galaxy formation by rapidly growing in mass with a duty cycle of order unity.
Journal ArticleDOI
Public Release of A-SLOTH: Ancient Stars and Local Observables by Tracing Halos
Tilman Hartwig,Mattis Magg,Li-Hsin Chen,Yuta Tarumi,Volker Bromm,Simon C. O. Glover,Alexander P. Ji,Ralf S. Klessen,Muhammad Latif,Marta Volonteri,Naoki Yoshida +10 more
TL;DR: The a-sloth model as mentioned in this paper is based on dark matter merger trees that can either be generated based on Extended Press-Schechter theory or be imported from dark matter simulations, and applies analytical recipes for baryonic physics to model the formation of both metal-free and metal-poor stars and the transition between them.
Journal ArticleDOI
Rapid Growth of Seed Black Holes during Early Bulge Formation
TL;DR: In this article , the early growth of massive seed black holes via accretion in protogalactic nuclei where the stellar bulge component is assembled, performing axisymmetric two-dimensional radiation hydrodynamical simulations.
Journal ArticleDOI
Origin of supermassive black holes in massive metal-poor protoclusters
Dominik R. G. Schleicher,B. Reinoso,Muhammad Latif,Ralf S. Klessen,Muñoz Vergara,Anish Das,P. Alister,V. B. D'iaz,P. Solar +8 more
TL;DR: In this paper , the mass of the central massive object, formed via collisions and gas accretion, considering the extreme cases of a logarithmically flat and a Salpeter-type initial mass function, was estimated.
References
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