Probing the z ≳ 6 quasars in a universe with IllustrisTNG physics: impact of gas-based black hole seeding models

Author:

Bhowmick Aklant K1ORCID,Blecha Laura1,Ni Yueying23,Matteo Tiziana Di23,Torrey Paul1ORCID,Kelley Luke Zoltan4ORCID,Vogelsberger Mark5ORCID,Weinberger Rainer6ORCID,Hernquist Lars7

Affiliation:

1. Department of Physics, University of Florida , Gainesville, FL 32611, USA

2. McWilliams Center for Cosmology , 5000 Forbes Avenue, Pittsburgh, PA 15213, USA

3. NSF AI Planning Institute for Physics of the Future, Carnegie Mellon University , Pittsburgh, PA 15213, USA

4. Center for Interdisciplinary Exploration and Research in Astrophysics, Northwestern University , Evanston, IL 60208, USA

5. Department of Physics, Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology , Cambridge, MA 02139, USA

6. Canadian Institute for Theoretical Astrophysics , 60 St George Street, Toronto, ON M5S 3H8, Canada

7. Harvard-Smithsonian Center for Astrophysics , 60 Garden Street, Cambridge, MA 02138, USA

Abstract

ABSTRACT We explore implications of a range of black hole (BH) seeding prescriptions on the formation of the brightest $z$ ≳ 6 quasars in cosmological hydrodynamic simulations. The underlying galaxy formation model is the same as in the IllustrisTNG simulations. Using constrained initial conditions, we study the growth of BHs in rare overdense regions (forming $\gtrsim 10^{12}\, {\rm M}_{\odot }\,h^{-1}$ haloes by $z$ = 7) using a  (9 Mpc h−1)3 simulated volume. BH growth is maximal within haloes that are compact and have a low tidal field. For these haloes, we consider an array of gas-based seeding prescriptions wherein $M_{\mathrm{seed}}=10^4\!-\!10^6\, {\rm M}_{\odot }\,h^{-1}$ seeds are inserted in haloes above critical thresholds for halo mass and dense, metal-poor gas mass (defined as $\tilde{M}_{\mathrm{h}}$ and $\tilde{M}_{\mathrm{sf,mp}}$, respectively, in units of Mseed). We find that a seed model with $\tilde{M}_{\mathrm{sf,mp}}=5$ and $\tilde{M}_{\mathrm{h}}=3000$ successfully produces a $z$ ∼ 6 quasar with $\sim 10^9\, {\rm M}_{\odot }$ mass and ∼1047 erg s−1 luminosity. BH mergers play a crucial role at $z$ ≳ 9, causing an early boost in BH mass at a time when accretion-driven BH growth is negligible. With more stringent seeding conditions (e.g. $\tilde{M}_{\mathrm{sf,mp}}=1000$), the relative paucity of BH seeds results in a much lower merger rate. In this case, $z$ ≳ 6 quasars can only be formed if we enhance the maximum allowed BH accretion rates (by factors ≳10) compared to the accretion model used in IllustrisTNG. This can be achieved either by allowing for super-Eddington accretion, or by reducing the radiative efficiency. Our results demonstrate that progenitors of $z$ ∼ 6 quasars have distinct BH merger histories for different seeding models, which will be distinguishable with Laser Interferometer Space Antenna observations.

Funder

NSF

Natural Sciences and Engineering Research Council of Canada

NASA

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

Cited by 12 articles. 订阅此论文施引文献 订阅此论文施引文献,注册后可以免费订阅5篇论文的施引文献,订阅后可以查看论文全部施引文献

1. Growth of high-redshift supermassive black holes from heavy seeds in the BRAHMA cosmological simulations: implications of overmassive black holes;Monthly Notices of the Royal Astronomical Society;2024-07-27

2. Introducing the BRAHMA simulation suite: signatures of low-mass black hole seeding models in cosmological simulations;Monthly Notices of the Royal Astronomical Society;2024-06-06

3. Sustained super-Eddington accretion in high-redshift quasars;Astronomy & Astrophysics;2024-06

4. Supermassive black holes are growing slowly by z∼5;Monthly Notices of the Royal Astronomical Society;2024-05-20

5. The host dark matter haloes of the first quasars;Monthly Notices of the Royal Astronomical Society;2024-04-30

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