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SMBH seeds from dissipative dark matter

Xiao, Huangyu and Shen, Xuejian and Hopkins, Philip F. and Zurek, Kathryn M. (2021) SMBH seeds from dissipative dark matter. Journal of Cosmology and Astroparticle Physics, 2021 (7). Art. No. 039. ISSN 1475-7516. doi:10.1088/1475-7516/2021/07/039.

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The existence of supermassive black holes (SMBHs) with masses greater than ~ 10⁹M☉ at high redshift (z ≳ 7) is difficult to accommodate in standard astrophysical scenarios. We study the possibility that (nearly) totally dissipative self-interacting dark matter (tdSIDM)–in rare, high density dark matter fluctuations in the early Universe — produces SMBH seeds through catastrophic collapse. We use a semi-analytic model, tested and calibrated by a series of N-body simulations of isolated dark matter halos, to compute the collapse criteria and timescale of tdSIDM halos, where dark matter loses nearly all of its kinetic energy in a single collision in the center-of-momentum frame. Applying this model to halo merger trees, we empirically assign SMBH seeds to halos and trace the formation and evolution history of SMBHs. We make predictions for the quasar luminosity function, the M_(BH)-σ_v* relation, and cosmic SMBH mass density at high redshift and compare them to observations. We find that a dissipative dark matter interaction cross-section of σ/m ~ 0.05 cm²/g is sufficient to produce the SMBHs observed in the early Universe while remaining consistent with ordinary SMBHs in the late Universe.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Xiao, Huangyu0000-0003-2485-5700
Shen, Xuejian0000-0002-6196-823X
Hopkins, Philip F.0000-0003-3729-1684
Zurek, Kathryn M.0000-0002-2629-337X
Additional Information:© 2021 IOP Publishing Ltd and Sissa Medialab. Received 6 May 2021; Accepted 30 June 2021; Published 20 July 2021. We thank Fangzhou Jiang for useful discussion regarding halo merger trees with the SatGen code. Numerical calculations were run on the Caltech compute cluster "Wheeler," allocations FTA-Hopkins/AST20016 supported by the NSF and TACC, and NASA HEC SMD-16-7592. Support for PFH and XS was provided by NSF Research Grants 1911233 & 20009234, NSF CAREER grant 1455342, NASA grants 80NSSC18K0562, HST-AR-15800.001-A. HX is supported in part by the U.S. Department of Energy under grant number DE-SC0011637 and the Kenneth K. Young Chair in Physics. KZ is supported by the U.S. Department of Energy, Office of Science, Office of High Energy Physics, under Award Number DE-SC0021431 and a Simons Investigator award.
Group:Astronomy Department, TAPIR, Walter Burke Institute for Theoretical Physics
Funding AgencyGrant Number
Department of Energy (DOE)DE-SC0011637
Kenneth K. Young ChairUNSPECIFIED
Department of Energy (DOE)DE-SC0021431
Simons FoundationUNSPECIFIED
Issue or Number:7
Record Number:CaltechAUTHORS:20210408-124720174
Persistent URL:
Official Citation:Huangyu Xiao et al JCAP07(2021)039
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:108661
Deposited By: Tony Diaz
Deposited On:09 Apr 2021 18:32
Last Modified:12 Jul 2022 17:28

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