IOP : Probing Supermassive Black Hole Seed Scenarios with Gravitational-wave Measurements

Ellis, John; Fairbairn, Malcolm; Vaskonen, Ville; Urrutia, Juan

doi:10.3847/1538-4357/ad27d5

Article
Report number	arXiv:2312.02983 ; KCL-PH-TH/2023-69 ; CERN-TH-2023-227
Title	Probing Supermassive Black Hole Seed Scenarios with Gravitational-wave Measurements
Author(s)	Ellis, John (King's Coll. London ; CERN) ; Fairbairn, Malcolm (King's Coll. London) ; Urrutia, Juan ; Vaskonen, Ville
Publication	2024-03-11
Imprint	2023-12-05
Number of pages	7
Note	7 pages, 5 figs, updated to match the published version
In:	Astrophys. J. 964 (2024) 11
DOI	10.3847/1538-4357/ad27d5
Subject category	astro-ph.HE ; Astrophysics and Astronomy ; astro-ph.CO ; Astrophysics and Astronomy ; General Relativity and Cosmology
Abstract	The process whereby the supermassive black holes populating the centers of galaxies have been assembled remains to be established, with the relative importance of seeds provided by collapsed Population-III stars, black holes formed in nuclear star clusters via repeated mergers, or direct collapses of protogalactic disks yet to be determined. In this paper we study the prospects for casting light on this issue by future measurements of gravitational waves emitted during the inspirals and mergers of pairs of intermediate-mass black holes, discussing in particular the roles of prospective measurements by LISA and the proposed atom interferometers AION and AEDGE. We find that, the expected number of detectable IMBH binaries is $O(100)$ for LISA and AEDGE and $O(10)$ for AION in low-mass seeds scenarios and goes down to $O(10)$ for LISA and below one for AEDGE and AION in high-mass seed scenarios. This allows all of these observatories to probe the parameters of the seed model, in particular if at least a fraction of the SMBHs arise from a low-mass seed population. We also show that the measurement accuracy of the binary parameters is, in general, best for AEDGE that sees very precisely the merger of the binary.
Copyright/License	publication: © 2024-2025 The Author(s) (License: CC-BY-4.0) preprint: (License: CC BY 4.0)

$\emph{Upper panel:} The low-mass cut on the massive BH population for different values of $m_{\rm cut}$, for $w=1$ (solid) and $w=2$ (dashed). \emph{Lower panel:} The halo mass-BH mass relation: The color coding shows the BH occupation fraction $p_{\rm occ}$ as a function of the halo mass $M_v$ and the BH mass $m_{\rm BH}$ for a scenario with $f_1 = f_2 = 0.5$, $w_1 = w_2 = 1$, $m_{{\rm cut},1} = 100\Msun$ and $m_{{\rm cut},2} = 10^5\Msun$.$ $\emph{Left panel:} The low-mass cut on the massive BH population for different values of $m_{\rm cut}$, for $w=1$ (solid) and $w=2$ (dashed). \emph{Right panel:} The halo mass-BH mass relation: The color coding shows the BH occupation fraction $p_{\rm occ}$ as a function of the halo mass $M_v$ and the BH mass $m_{\rm BH}$ for a scenario with $f_1 = f_2 = 0.5$, $w_1 = w_2 = 1$, $m_{{\rm cut},1} = 100\Msun$ and $m_{{\rm cut},2} = 10^5\Msun$.$ $\emph{Upper panel:} The low-mass cut on the massive BH population for different values of $m_{\rm cut}$, for $w=1$ (solid) and $w=2$ (dashed). \emph{Lower panel:} The halo mass-BH mass relation: The color coding shows the BH occupation fraction $p_{\rm occ}$ as a function of the halo mass $M_v$ and the BH mass $m_{\rm BH}$ for a scenario with $f_1 = f_2 = 0.5$, $w_1 = w_2 = 1$, $m_{{\rm cut},1} = 100\Msun$ and $m_{{\rm cut},2} = 10^5\Msun$.$ Show more plots

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