Formation of Binary Black Holes Similar to GW190521 with a Total Mass of $\sim 150\,M_{\odot}$ from Population III Binary Star Evolution

Kinugawa, Tomoya; Nakamura, Takashi; Nakano, Hiroyuki

doi:10.48550/arxiv.2009.06922

Cited by 21 publications

(23 citation statements)

References 36 publications

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“…The pair-instability process immediately translates into a promising signature of hierarchical mergers in GW observations: if BHs with 50M m 120M cannot be produced by stars, they might well be the remnants of previous BH mergers. Possible caveats to this statement include envelope retention in low-metallicity population III stars, [52][53][54] stellar mergers prior to BH formation, 37,[55][56][57] evolution in detached binaries, 44 as well as accretion in either molecular clouds, 58 minihalos, 59 dense clusters, 60,61 or isolated binaries. 62…”

Section: Masses: Populating the Pair-instability Mass Gapmentioning

confidence: 99%

“…Several alternative explanations for the occurrence of GW190521 have also been put forward, ranging from critically assessing uncertainties in the lower edge of the mass gap, 47,53,228,229 Population III stars at very low-metallicity, 53,54,230 accretion onto either stellar-origin 58,59,213 or primordial 231,232 BHs, and stellar mergers. 37,55,56 Additional speculations include invoking beyond-standard-model physics 233,234 exotic compact objects, 235,236 and dark-matter annihilation.…”

Section: Gw190521mentioning

confidence: 99%

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Hierarchical mergers of stellar-mass black holes and their gravitational-wave signatures

Gerosa,

Fishbach

2021

Preprint

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We review theoretical findings, astrophysical modeling, and current gravitational-wave evidence of hierarchical stellar-mass black-hole mergers. While most of the compact binary mergers detected by LIGO and Virgo are expected to consist of firstgeneration black holes formed from the collapse of stars, others might instead be of second (or higher) generation, containing the remnants of previous black-hole mergers. Such a subpopulation of hierarchically assembled black holes presents distinctive gravitational-wave signatures, namely higher masses, possibly within the pair-instability mass gap, and dimensionless spins clustered at the characteristic value of ∼ 0.7. In order to produce hierarchical mergers, astrophysical environments need to overcome the relativistic recoils imparted to black-hole merger remnants, a condition which prefers hosts with escape speeds 100 km/s. Promising locations for efficient production of hierarchical mergers include nuclear star clusters and accretion disks surrounding active galactic nuclei, though environments that are less efficient at retaining merger products such as globular clusters may still contribute significantly to the detectable population of repeated mergers. While GW190521 is the single most promising hierarchical-merger candidate to date, constraints coming from large population analyses are becoming increasingly more powerful.

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Section: Masses: Populating the Pair-instability Mass Gapmentioning

confidence: 99%

Section: Gw190521mentioning

confidence: 99%

Hierarchical mergers of stellar-mass black holes and their gravitational-wave signatures

Gerosa,

Fishbach

2021

Preprint

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“…• The initial conditions of zero-age main-sequence stars (e.g., metallicity) evolve over cosmic time, which could affect the resultant masses and spins of black holes (BHs) from stellar evolution (Kudritzki & Puls 2000;Brott et al 2011;Fryer et al 2012;Dominik et al 2015;Safarzadeh & Farr 2019;Neijssel et al 2019;Kinugawa et al 2020;Farrell et al 2020;Vink et al 2020).…”

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confidence: 99%

When are LIGO/Virgo's Big Black-Hole Mergers?

Fishbach,

Doctor,

Callister

et al. 2021

Preprint

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We study the evolution of the binary black hole (BBH) mass distribution across cosmic time. The second gravitational-wave transient catalog (GWTC-2) from LIGO/Virgo contains BBH events out to redshifts z ∼ 1, with component masses in the range ∼ 5-80 M . In this catalog, the biggest black holes, with m 1 45 M , are only found at the highest redshifts, z 0.4. We ask whether the absence of high-mass BBH observations at low redshift indicates that the astrophysical BBH mass distribution evolves: the biggest BBHs only merge at high redshift, and cease merging at low redshift. Alternatively, this feature might be explained by gravitational-wave selection effects. Modeling the BBH primary mass spectrum as a power law with a sharp maximum mass cutoff (Truncated model), we find that the cutoff increases with redshift (> 99.9% credibility). An abrupt cutoff in the mass spectrum is expected from (pulsational) pair instability supernova simulations; however, GWTC-2 is only consistent with a Truncated mass model if the location of the cutoff increases from 45 +13 −5 M at z < 0.4 to 80 +16−13 M at z > 0.4. Alternatively, if the primary mass spectrum has a break in the power law (Broken Power Law ) at 38 +15 −8 M , rather than a sharp cutoff, the data are consistent with a non-evolving mass distribution. In this case the overall rate of mergers, at all masses, increases with increasing redshift. Future observations will confidently distinguish between a sharp maximum mass cutoff that evolves with redshift and a non-evolving mass distribution with a gradual taper, such as a Broken Power Law. After ∼ 100 BBH merger observations, a continued absence of high-mass, low-redshift events would provide a clear signature that the mass distribution evolves with redshift.

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“…This event is associated with the most massive binary system detected by LIGO/Virgo so far, with a total mass of ∼ 150 M . This makes GW190521 particularly interesting, since the origin of black holes in the mass gap challenges the standard theories of stellar evolution (Abbott et al 2020e), although the origin of this event as isolated binary cannot be excluded (Farrell et al 2020;Kinugawa et al 2020), and the components mass may fall outside of the mass gap (Fishbach & Holz 2020). This detection therefore resulted in a large number of proposed alternative Corresponding author: Antonella Palmese palmese@fnal.gov * NASA Hubble Fellowship Program Einstein Postdoctoral Fellow formation scenarios including primordial black holes (Luca et al 2020), exotic Proca stars (Bustillo et al 2021), lowmass dwarf galaxy mergers (Conselice et al 2020;, dynamical interactions in dense stellar environments (Romero-Shaw et al 2020;Gayathri et al 2020a;Fragione et al 2020) and black holes grown by accretion (Safarzadeh & Haiman 2020).…”

Section: Introductionmentioning

confidence: 99%

Do LIGO/Virgo black hole mergers produce AGN flares? The case of GW190521 and prospects for reaching a confident association

Palmese,

Fishbach,

Burke

et al. 2021

Preprint

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The recent report of an association of the gravitational-wave (GW) binary black hole (BBH) merger GW190521 with a flare in the Active Galactic Nuclei (AGN) J124942.3+344929 has generated tremendous excitement. However, GW190521 has one of the largest localization volumes amongst all of the GW events detected so far. The 90% localization volume likely contains 7, 400 unobscured AGN brighter than g ≤ 20.5 AB mag, and it results in a 70% probability of chance coincidence for an AGN flare consistent with the GW event. We present a Bayesian formalism to estimate the confidence of an AGN association by analyzing a population of BBH events with dedicated follow-up observations. Depending on the fraction of BBH arising from AGNs, counterpart searches of O(1) − O(100) GW events are needed to establish a confident association, and more than an order of magnitude more for searches without followup (i.e, using only the locations of AGNs and GW events). Follow-up campaigns of the top ∼ 5% (based on volume localization and binary mass) of BBH events with total rest frame mass ≥ 50 M are expected to establish a confident association during the next LIGO/Virgo/KAGRA observing run (O4), as long as the true value of the fraction of BBH giving rise to AGN flares is > 0.1. Our formalism allows us to jointly infer cosmological parameters from a sample of BBH events that include chance coincidence flares. Until the confidence of AGN associations is established, the probability of chance coincidence must be taken into account to avoid biasing astrophysical and cosmological constraints.

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Formation of Binary Black Holes Similar to GW190521 with a Total Mass of $\sim 150\,M_{\odot}$ from Population III Binary Star Evolution

Cited by 21 publications

References 36 publications

Hierarchical mergers of stellar-mass black holes and their gravitational-wave signatures

Hierarchical mergers of stellar-mass black holes and their gravitational-wave signatures

When are LIGO/Virgo's Big Black-Hole Mergers?

Do LIGO/Virgo black hole mergers produce AGN flares? The case of GW190521 and prospects for reaching a confident association

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