The most powerful astrophysical events: Gravitational-wave peak luminosity of binary black holes as predicted by numerical relativity

Keitel, D.; Forteza, Xisco Jiménez; Husa, S.; London, L. T.; Bernuzzi, Sebastiano; Harms, Enno; Nagar, Alessandro; Hannam, M. D.; Khan, S.; Pürrer, M.; Pratten, G.; Chaurasia, Vivek

doi:10.1103/physrevd.96.024006

Cited by 41 publications

(55 citation statements)

References 99 publications

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“…The approach used in this paper can be used to estimate the GW peak luminosity, thus complementing the result derived for BBHs and binary NS systems in [67,68] (see [8] for an application of those results). The GW peak luminosity is computed from the (2, 2) mode of the GW strain,…”

Section: Gw Peak Luminositymentioning

confidence: 89%

Black-Hole Remnants from Black-Hole–Neutron-Star Mergers

et al. 2019

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Observations of gravitational waves and their electromagnetic counterparts may soon uncover the existence of coalescing compact binary systems formed by a stellar-mass black hole and a neutron star. These mergers result in a remnant black hole, possibly surrounded by an accretion disk. The mass and spin of the remnant black hole depend on the properties of the coalescing binary. We construct a map from the binary components to the remnant black hole using a sample of numericalrelativity simulations of different mass ratios q, (anti-)aligned dimensionless spins of the black hole aBH, and several neutron star equations of state. Given the binary total mass, the mass and spin of the remnant black hole can therefore be determined from the three parameters (q, aBH, Λ), where Λ is the tidal deformability of the neutron star. Our models also incorporate the binary black hole and test-mass limit cases and we discuss a simple extension for generic black hole spins. We combine the remnant characterization with recent population synthesis simulations for various metallicities of the progenitor stars that generated the binary system. We predict that black-hole-neutron-star mergers produce a population of remnant black holes with masses distributed around 7M and 9M . For isotropic spin distributions, nonmassive accretion disks are favoured: no bright electromagnetic counterparts are expected in such mergers.Introduction.-Mergers of a stellar-mass black hole (BH) and a neutron star (NS), hereafter BHNS, are expected sources of gravitational waves (GWs) detectable by ground-based laser-interferometers and possibly accompanied by electromagnetic counterparts [1][2][3][4][5][6][7]. No GW observations of BHNS binaries have been made to date. The 90% confidence upper limit on their merger rate is 610 Gpc −3 yr −1 [8]. To prepare these observations quantitative general-relativistic theoretical models of the GW and merger outcome are required.

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Section: Gw Peak Luminositymentioning

confidence: 89%

Black-Hole Remnants from Black-Hole–Neutron-Star Mergers

et al. 2019

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“…The final mass, radiated energy, final spin, and peak luminosity of the BH remnant from a BBH coalescence are computed using averages of fits to numerical relativity (NR) results [15,[148][149][150][151][152][153]. Posteriors for the mass and spin of the BH remnant for BBH coalescences are shown in the right in Fig.…”

Section: B Massesmentioning

confidence: 99%

GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs

Abbott¹,

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Abbott³

et al. 2019

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We present the results from three gravitational-wave searches for coalescing compact binaries with component masses above 1 M ⊙ during the first and second observing runs of the advanced gravitationalwave detector network. During the first observing run (O1), from September 12, 2015 to January 19, 2016, gravitational waves from three binary black hole mergers were detected. The second observing run (O2), which ran from November 30, 2016 to August 25, 2017, saw the first detection of gravitational waves from a binary neutron star inspiral, in addition to the observation of gravitational waves from a total of seven binary black hole mergers, four of which we report here for the first time: GW170729, GW170809, GW170818, and GW170823. For all significant gravitational-wave events, we provide estimates of the source properties. The detected binary black holes have total masses between 18.6 þ3.2 −0.7 M ⊙ and 84.4 þ15.8 −11.1 M ⊙ and range in distance between 320 þ120 −110 and 2840 þ1400 −1360 Mpc. No neutron star-black hole mergers were detected. In addition to highly significant gravitational-wave events, we also provide a list of marginal event candidates with an estimated false-alarm rate less than 1 per 30 days. From these results over the first two observing runs, which include approximately one gravitational-wave detection per 15 days of data searched, we infer merger rates at the 90% confidence intervals of 110 − 3840 Gpc −3 y −1 for binary neutron stars and 9.7 − 101 Gpc −3 y −1 for binary black holes assuming fixed population distributions and determine a neutron star-black hole merger rate 90% upper limit of 610 Gpc −3 y −1 .

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“…Unfaithfulness comparison between TEOBResumS and the set of BAM waveforms mostly presented in Refs [73][74][75]. and listed in…”

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Time-domain effective-one-body gravitational waveforms for coalescing compact binaries with nonprecessing spins, tides, and self-spin effects

et al. 2018

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We present TEOBResumS, a new effective-one-body (EOB) waveform model for nonprecessing (spinaligned) and tidally interacting compact binaries. Spin-orbit and spin-spin effects are blended together by making use of the concept of centrifugal EOB radius. The point-mass sector through merger and ringdown is informed by numerical relativity (NR) simulations of binary black holes (BBH) computed with the SpEC and BAM codes. An improved, NR-based phenomenological description of the postmerger waveform is developed. The tidal sector of TEOBResumS describes the dynamics of neutron star binaries up to merger and incorporates a resummed attractive potential motivated by recent advances in the post-Newtonian and gravitational self-force description of relativistic tidal interactions. Equation-of-state dependent self-spin interactions (monopole-quadrupole effects) are incorporated in the model using leading-order post-Newtonian results in a new expression of the centrifugal radius. TEOBResumS is compared to 135 SpEC and 19 BAM BBH waveforms. The maximum unfaithfulness to SpEC dataF -at design Advanced-LIGO sensitivity and evaluated with total mass M varying between 10M ≤ M ≤ 200M -is always below 2.5 × 10 −3 except for a single outlier that grazes the 7.1 × 10 −3 level. When compared to BAM data,F is smaller than 0.01 except for a single outlier in one of the corners of the NR-covered parameter space, that reaches the 0.052 level. TEOBResumS is also compatible, up to merger, to high end NR waveforms from binary neutron stars with spin effects and reduced initial eccentricity computed with the BAM and THC codes. The data quality of binary neutron star waveforms is assessed via rigorous convergence tests from multiple resolution runs and takes into account systematic effects estimated by using the two independent high-order NR codes. The model is designed to generate accurate templates for the analysis of LIGO-Virgo data through merger and ringdown. We demonstrate its use by analyzing the publicly available data for GW150914.PACS numbers: 04.25.D-, 04.30. Db, 95.30.Sf, 97.60.Jd

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The most powerful astrophysical events: Gravitational-wave peak luminosity of binary black holes as predicted by numerical relativity

Cited by 41 publications

References 99 publications

Black-Hole Remnants from Black-Hole–Neutron-Star Mergers

Black-Hole Remnants from Black-Hole–Neutron-Star Mergers

GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs

Time-domain effective-one-body gravitational waveforms for coalescing compact binaries with nonprecessing spins, tides, and self-spin effects

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