When Are LIGO/Virgo’s Big Black Hole Mergers?

Fishbach, M.; Doctor, Z.; Callister, T. A.; Edelman, B.; Ye, Jiani; Essick, R. C.; Farr, W. M.; Farr, B.; Holz, D. E.

doi:10.3847/1538-4357/abee11

Cited by 82 publications

(59 citation statements)

References 51 publications

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“…Firstgeneration black holes may predominantly arise in scenarios with a common-envelope history, which would lead to aligned spins (Kalogera 2000;Mandel & O'Shaughnessy 2010;Dominik et al 2013;Giacobbo et al 2018;Eldridge et al 2017;Olejak et al 2020), whereas second-generation black holes would be formed hierarchically and thereby have a more uniform spin distribution (Rodriguez et al 2016;Vitale et al 2017). One might also plausibly expect characteristic differences in the redshift (Fishbach et al 2021) and eccentricity (Samsing et al 2014;Samsing 2018;Rodriguez et al 2018;Zevin et al 2019) distributions between first-generation and second-generation black holes. These will be easy to incorporate in our model, and we look forward to future work that incorporates models for these physical effects alongside the ones that we have modeled, which we have argued are revealed by the mass function.…”

Section: Discussionmentioning

confidence: 99%

“…Though the higher-generation black hole merger rate will not be completely negligible, nevertheless we emphasize that such objects are rare by assumption: not every first-generation black hole merger product will be involved in a higher-generation merger within a Hubble time. In addition, properly accounting for the contributions of these higher-generation black holes to the merger rate will entail accounting for mass-and environment-dependence related to the efficiency of formation of higher-generation binary systems (Chatziioannou et al 2019;Arca Sedda et al 2020;Fishbach et al 2021). For the parameters of interest in this work, we find that Equation (5) has a discernible two-sided peak at…”

Section: Bhmentioning

confidence: 95%

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Find the Gap: Black Hole Population Analysis with an Astrophysically Motivated Mass Function

Baxter

Croon

McDermott

et al. 2021

ApJL

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We introduce a novel black hole mass function that realistically models the physics of pair-instability supernovae with a minimal number of parameters. Applying this to all events in the LIGO-Virgo Gravitational-Wave Transient Catalog 2 (GWTC-2), we detect a peak at. Repeating the analysis without the black holes from the event GW190521, we find this feature at M BHMG = 54 ± 6 M e . These results establish the edge of the anticipated "black hole mass gap" at a value compatible with the expectation from standard stellar structure theory. The mass gap manifests itself as a discontinuity in the mass function and is populated by a distinct, less-abundant population of higher-mass black holes. We find that the primary black hole population scales with power-law index −1.95 ± 0.51 (−1.97 ± 0.44) with (without) GW190521, consistent with models of star formation. Using Bayesian techniques, we establish that our mass function fits a new catalog of black hole masses approximately as well as pre-existing phenomenological mass functions. We also remark on the implications of these results for constraining or discovering new phenomena in nuclear and particle physics. Unified Astronomy Thesaurus concepts: Astrophysical black holes (98); Black holes (162); Gravitational waves (678); Particle astrophysics (96); Gravitational wave astronomy (675); Nuclear astrophysics (1129); Stellar evolution (1599); Stellar populations (1622); Population III stars (1285); Helium burning (716)

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Section: Discussionmentioning

confidence: 99%

Section: Bhmentioning

confidence: 95%

Find the Gap: Black Hole Population Analysis with an Astrophysically Motivated Mass Function

Baxter

Croon

McDermott

et al. 2021

ApJL

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“…peak multi-source (separate BH mass models in BH-BH and NS-BH binaries) and Binned Gaussian process (unmodelled with regularisation). Secondly, another uncertainty arises from the possibility that the merger rate varies with redshift, for which there is already significant support in the data (Fishbach et al 2021;Abbott et al 2021e). Allowing for the variation of the merger rate with redshift (but not yet of the mass distribution with redshift, although some theoretical models predict this) further shifts the binary black hole merger rate at redshift z ¼ 0.…”

Section: Gravitational Wavesmentioning

confidence: 99%

Rates of compact object coalescences

2022

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Gravitational-wave detections are enabling measurements of the rate of coalescences of binaries composed of two compact objects—neutron stars and/or black holes. The coalescence rate of binaries containing neutron stars is further constrained by electromagnetic observations, including Galactic radio binary pulsars and short gamma-ray bursts. Meanwhile, increasingly sophisticated models of compact objects merging through a variety of evolutionary channels produce a range of theoretically predicted rates. Rapid improvements in instrument sensitivity, along with plans for new and improved surveys, make this an opportune time to summarise the existing observational and theoretical knowledge of compact-binary coalescence rates.

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“…Still, we do not know much about the origin of these black holes. There is a possibility that those are ordinary astrophysical black holes from stellar collapses (possibly from different channels) [7,8]. The other interesting conjecture is that the LIGO detectors have detected primordial black holes (PBHs).…”

Section: Introductionmentioning

confidence: 99%

Primordial Black Hole Merger Rate in Self-Interacting Dark Matter Halo Models

Fakhry,

Naseri,

Firouzjaee

et al. 2021

Preprint

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We study the merger rate of primordial black holes (PBHs) in the self-interacting dark matter (SIDM) halo models. To explore a numerical description for the density profile of the SIDM halo models, we use the result of a previously performed simulation for the SIDM halo models with σ/m = 10 cm 2 g −1 . We also propose a concentration-mass-time relation that can explain the evolution of the halo density profile related to the SIDM models. Furthermore, we investigate the encounter condition of PBHs that may have been distributed in the medium of dark matter halos randomly. Under these assumptions, we calculate the merger rate of PBHs within each halo considering the SIDM halo models and compare the results with the one obtained for the cold dark matter (CDM) halo models. We indicate that the merger rate of PBHs for the SIDM halo models during the first epoch (i.e., ∆t ≤ 1 Gyr after the halo virialization) should be lower than the corresponding result for the CDM halo models, while by the time entering the second epoch (i.e., ∆t > 1 Gyr after the halo virialization) sufficient PBH mergers in the SIDM halo models can be generated and even exceed the one resulted from the CDM halo models. By considering the spherical-collapse halo mass function, we obtain similar results for the cumulative merger rate of PBHs. Moreover, we calculate the redshift evolution of the PBH total merger rate. To determine a constraint on the PBH abundance, we study the merger rate of PBHs in terms of their fraction and masses and compare those with the black hole merger rate estimated by the Advanced LIGO (aLIGO) detectors during the third observing run. The results demonstrate that within the context of the SIDM halo models during the second epoch, the merger rate of 10 M⊙ − 10 M⊙ events falls within the aLIGO window. We also estimate a relation between the fraction of PBHs and their masses, which is well consistent with our findings.

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When Are LIGO/Virgo’s Big Black Hole Mergers?

Cited by 82 publications

References 51 publications

Find the Gap: Black Hole Population Analysis with an Astrophysically Motivated Mass Function

Find the Gap: Black Hole Population Analysis with an Astrophysically Motivated Mass Function

Rates of compact object coalescences

Primordial Black Hole Merger Rate in Self-Interacting Dark Matter Halo Models

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