Growth of Supermassive Black Hole Seeds in ETG Star-forming Progenitors: Multiple Merging of Stellar Compact Remnants via Gaseous Dynamical Friction and Gravitational-wave Emission

Boco, Lumen; Lapi, A.; Danese, L.

doi:10.3847/1538-4357/ab7446

Cited by 33 publications

(62 citation statements)

References 187 publications

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“…the ratio of the perturber velocity to the sound speed c s of the background medium, and of the Coulomb logarithm ln Λ. In the collisional case several formulas for the computation of f (M, ln Λ) have been proposed (see [60][61][62][63]) and tested numerically [64], while the value of the Coulomb logarithm is still somewhat debated, this is extensively discussed in [1] and in the references therein.…”

Section: Gaseous Dynamical Friction Migration Timescales and Merging ...mentioning

confidence: 99%

Growth of Massive Black Hole Seeds by Migration of Stellar and Primordial Black Holes: Gravitational Waves and Stochastic Background

Boco,

Lapi,

Sicilia

et al. 2021

Preprint

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We investigate the formation and growth of massive black hole (BH) seeds in dusty star-forming galaxies, relying and extending the framework proposed by [1]. Specifically, the latter envisages the migration of stellar compact remnants (neutron stars and stellar-mass black holes) via gaseous dynamical friction towards the galaxy nuclear region, and their subsequent merging to grow a massive central BH seed. In this paper we add two relevant ingredients: (i) we include primordial BHs, that could constitute a fraction f pBH of the dark matter, as an additional component participating in the seed growth; (ii) we predict the stochastic gravitational wave background originated during the seed growth, both from stellar compact remnant and from primordial BH mergers. We find that the latter events contribute most to the initial growth of the central seed during a timescale of 10 6 − 10 7 yr, before stellar compact remnant mergers and gas accretion take over. In addition, if the fraction of primordial BHs f pBH is large enough, gravitational waves emitted by their mergers in the nuclear galactic regions could be detected by future interferometers like Einsten Telescope, DECIGO and LISA. As for the associated stochastic gravitational wave background, we predict that it extends over the wide frequency band 10 −6 f [Hz] 10, which is very different from the typical range originated by mergers of isolated binary compact objects. On the one hand, the detection of such a background could be a smoking gun to test the proposed seed growth mechanism; on the other hand, it constitutes a relevant contaminant from astrophysical sources to be characterized and subtracted, in the challenging search for a primordial background of cosmological origin.

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Section: Gaseous Dynamical Friction Migration Timescales and Merging ...mentioning

confidence: 99%

Growth of Massive Black Hole Seeds by Migration of Stellar and Primordial Black Holes: Gravitational Waves and Stochastic Background

Boco,

Lapi,

Sicilia

et al. 2021

Preprint

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“…Light seeds, with a BH mass ∼ 100 M , are supposed to be the remnants of the first generation of metal-free (Population III/Pop III) stars and are expected to form with masses ranging between a few 10s to a few 100s M , inside dark matter (DM) minihalos (𝑀 halo ∼ 10 5 − 10 6 M ) at very high redshifts (𝑧 ≥ 20, see Bromm 2013 for a review, and Hirano et al 2014;Hirano et al 2015;Hosokawa et al 2016;Sugimura et al 2020 for more recent works). 2018; Reinoso et al 2019;Sassano et al 2021), although even more massive BH seeds could originate from merger episodes between stellar mass BHs (aided by strong gas inflows) inside similarly dense environments (Lupi et al 2014;Boco et al 2020).…”

Section: Introductionmentioning

confidence: 99%

The low-end of the black hole mass function at cosmic dawn

Trinca,

Schneider,

Valiante

et al. 2022

Preprint

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Understanding the formation and growth of supermassive black holes (SMBHs) at high redshift represents a major challenge for theoretical models. In this work we investigate the early evolution of the first SMBHs by constraining their distribution in mass and luminosity at 𝑧 > 4. In particular, we focus on the poorly explored low-mass end of the nuclear black hole (BH) distribution down to 𝑧 4, and explore its connection with the nature of the first BH seeds and the processes governing their mass growth. To this aim, we have developed CAT (Cosmic Archaeology Tool), a new semi-analytic model that describes the formation of the first stars and black holes in a self-consistent way and follows the co-evolution of nuclear BHs and their host galaxies for a representative population at 𝑧 > 4. We find that current observational constraints favour models where the growth of BH seeds is Eddington limited and occurs at the Bondi-Hoyle-Lyttleton rate or where super-Eddington accretion occurs via a slim disk during gas rich galaxy mergers. The main difference between these two model variants lies at the low-end of the predicted mass and luminosity functions at 4 ≤ 𝑧 ≤ 6, where a clear gap appears in the first model, reflecting the stunted growth of light BH seeds formed as remnants of the first stars. Detecting this signature will be extremely challenging even for the future generation of space observatories, such as JWST, Athena and Lynx.

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“…In the mass range m • ∼ 5 − 150 M , BHs are originated from the final, often dramatic stages in the evolution of massive stars (possibly hosted in binary systems). These compact remnants can produce luminous X-ray binaries (e.g., Mapelli et al 2010;Farr et al 2011;Inoue et al 2016), can constitute powerful sources of gravitational waves for ground-based detectors like the current LIGO/Virgo facility (e.g., Belczynski et al 2010;Dominik et al 2015;Spera et al 2017Spera et al , 2019Boco et al 2019;Abbott et al 2021a,b), can possibly energize short gamma-ray bursts and associated kilonovas (e.g., Abbott et al 2020Abbott et al , 2021cAckley et al 2020;Gompertz et al 2020), can inject strong energy inputs in the primeval Universe (e.g., Mirabel et al 2011;Justham & Schawinski 2012;Artale et al 2015;Madau & Fragos 2017;Lehmer et al 2021), and can provide light seeds for the subsequent growth of more massive BHs (e.g., Volonteri et al 2015;Lupi et al 2016;Pacucci et al 2017;Boco et al 2020;Das et al 2021). At the other end, in the range M • ∼ 10 6 − 10 10 M , supermassive BHs grow mainly by gaseous accretion, that energize the spectacular broadband emission of AGNs.…”

Section: Introductionmentioning

confidence: 99%

“…However, the chase is open in view of their astrophysical relevance. Most noticeably, they can provide heavy seeds for quick (super)massive BHs growth (e.g., Mayer & Bonoli 2019;Boco et al 2020), as it seems required by the puzzling observations of an increasing numbers of giant monsters M • 10 9 M when the age of the Universe was shorter than 0.8 Gyr (e.g., Mortlock et al 2011;Venemans et al 2017;Banados et al 2018). Moreover, such intermediate-mass BHs will constitute important targets for space-based gravitational wave detectors like LISA and DECIGO (see eLISA Consortium 2013; Kawamura et al 2021; also Boco et al 2021a;Barausse & Lapi 2021).…”

Section: Introductionmentioning

confidence: 99%

The Black Hole Mass Function Across Cosmic Times I. Stellar Black Holes and Light Seed Distribution

Sicilia,

Lapi,

Boco

et al. 2021

Preprint

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This is the first paper in a series aimed at modeling the black hole (BH) mass function, from the stellar to the intermediate to the (super)massive regime. In the present work we focus on stellar BHs and provide an ab-initio computation of their mass function across cosmic times; we mainly consider the standard, and likely dominant production channel of stellar-mass BHs constituted by isolated single/binary star evolution. Specifically, we exploit the state-of-the-art stellar and binary evolutionary code SEVN, and couple its outputs with redshift-dependent galaxy statistics and empirical scaling relations involving galaxy metallicity, star-formation rate and stellar mass. The resulting relic mass function dN/dV d log m • as a function of the BH mass m • features a rather flat shape up to m • ≈ 50 M and then a log-normal decline for larger masses, while its overall normalization at a given mass increases with decreasing redshift. We highlight the contribution to the local mass function from isolated stars evolving into BHs and from binary stellar systems ending up in single or binary BHs. We also include the distortion on the mass function induced by binary BH mergers, finding that it has a minor effect at the high-mass end. We estimate a local stellar BH relic mass density of ρ • ≈ 5 × 10 7 M Mpc −3 , which exceeds by more than two orders of magnitude that in supermassive BHs; this translates into an energy density parameter Ω • ≈ 4 × 10 −4 , implying that the total mass in stellar BHs amounts to 1% of the local baryonic matter. We show how our mass function for merging BH binaries compares with the recent estimates from gravitational wave observations by LIGO/Virgo, and discuss the possible implications for dynamical formation of BH binaries in dense environments like star clusters. We address the impact of adopting different binary stellar evolution codes (SEVN and COSMIC) on the mass function, and find the main differences to occur at the high mass end, in connection with the numerical treatment of stellar binary evolution effects. We highlight that our results can provide a firm theoretical basis for a physically-motivated light seed distribution at high redshift, to be implemented in semi-analytic and numerical models of BH formation and evolution. Finally, we stress that the present work can constitute a starting point to investigate the origin of heavy seeds and the growth of (super)massive BHs in high-redshift star-forming galaxies, that we will pursue in forthcoming papers.

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Growth of Supermassive Black Hole Seeds in ETG Star-forming Progenitors: Multiple Merging of Stellar Compact Remnants via Gaseous Dynamical Friction and Gravitational-wave Emission

Cited by 33 publications

References 187 publications

Growth of Massive Black Hole Seeds by Migration of Stellar and Primordial Black Holes: Gravitational Waves and Stochastic Background

Growth of Massive Black Hole Seeds by Migration of Stellar and Primordial Black Holes: Gravitational Waves and Stochastic Background

The low-end of the black hole mass function at cosmic dawn

The Black Hole Mass Function Across Cosmic Times I. Stellar Black Holes and Light Seed Distribution

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