Accurate inspiral-merger-ringdown gravitational waveforms for nonspinning black-hole binaries including the effect of subdominant modes

Mehta, A. K.; Mishra, C.; Varma, V.; Ajith, P.

doi:10.1103/physrevd.96.124010

Cited by 43 publications

(53 citation statements)

References 64 publications

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“…In this work, we model the following spin-weighted spherical harmonic modes: ≤ 4 and (5,5), but not the (4,1) or (4,0) modes 2 . Several inspiral-mergerringdown waveform models [14,15,20,21] that include nonquadrupole modes have been developed in recent years; however, compared to those models we show an improved accuracy and we include more modes. The rest of the paper is organized as follows.…”

Section: Introductionmentioning

confidence: 83%

“…However, because NR simulations are computationally expensive, it is impractical to use them directly for applications such as parameter estimation, which can require upwards of 10 7 waveform evaluations. Therefore, the GW community has developed several approximate waveform models [12][13][14][15][16][17][18][19][20][21], some of which are fast to evaluate. These models make certain physically-motivated assumptions about the underlying phenomenology of the waveforms, and they fit for any remaining free parameters using NR simulations.…”

Section: Introductionmentioning

confidence: 99%

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Surrogate model of hybridized numerical relativity binary black hole waveforms

et al. 2019

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Numerical relativity (NR) simulations provide the most accurate binary black hole gravitational waveforms, but are prohibitively expensive for applications such as parameter estimation. Surrogate models of NR waveforms have been shown to be both fast and accurate. However, NR-based surrogate models are limited by the training waveforms' length, which is typically about 20 orbits before merger. We remedy this by hybridizing the NR waveforms using both post-Newtonian and effective one body waveforms for the early inspiral. We present NRHybSur3dq8, a surrogate model for hybridized nonprecessing numerical relativity waveforms, that is valid for the entire LIGO band (starting at 20 Hz) for stellar mass binaries with total masses as low as 2.25 M . We include the ≤ 4 and (5, 5) spin-weighted spherical harmonic modes but not the (4, 1) or (4, 0) modes. This model has been trained against hybridized waveforms based on 104 NR waveforms with mass ratios q ≤ 8, and |χ1z|, |χ2z| ≤ 0.8, where χ1z (χ2z) is the spin of the heavier (lighter) BH in the direction of orbital angular momentum. The surrogate reproduces the hybrid waveforms accurately, with mismatches 3 × 10 −4 over the mass range 2.25M ≤ M ≤ 300M . At high masses (M 40M ), where the merger and ringdown are more prominent, we show roughly two orders of magnitude improvement over existing waveform models. We also show that the surrogate works well even when extrapolated outside its training parameter space range, including at spins as large as 0.998. Finally, we show that this model accurately reproduces the spheroidal-spherical mode mixing present in the NR ringdown signal. arXiv:1812.07865v3 [gr-qc]

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Section: Introductionmentioning

confidence: 83%

Section: Introductionmentioning

confidence: 99%

Surrogate model of hybridized numerical relativity binary black hole waveforms

et al. 2019

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“…To be able to characterize the full range of potential systems, models of the gravitational radiation emitted by BBHs are continuously being improved. In particular, physical effects associated with unequal masses and misaligned spins have recently been extended in models covering the inspiral, merger and ringdown of BBHs [21][22][23][24][25][26][27][28][29][30][31][32][33]. For GW signals with sufficient signal-to-noise ratio (SNR), the inclusion of these effects is important to accurately infer the source parameters.…”

Section: Introductionmentioning

confidence: 99%

GW190412: Observation of a binary-black-hole coalescence with asymmetric masses

Abbott¹,

Abbott²,

Abraham³

et al. 2020

Phys. Rev. D

578

408

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We report the observation of gravitational waves from a binary-black-hole coalescence during the first two weeks of LIGO's and Virgo's third observing run. The signal was recorded on April 12, 2019 at 05∶30∶44 UTC with a network signal-to-noise ratio of 19. The binary is different from observations during the first two observing runs most notably due to its asymmetric masses: a ∼30 M ⊙ black hole merged with a ∼8 M ⊙ black hole companion. The more massive black hole rotated with a dimensionless spin magnitude between 0.22 and 0.60 (90% probability). Asymmetric systems are predicted to emit gravitational waves with stronger contributions from higher multipoles, and indeed we find strong evidence for gravitational radiation beyond the leading quadrupolar order in the observed signal. A suite of tests performed on GW190412 indicates consistency with Einstein's general theory of relativity. While the mass ratio of this system differs from all previous detections, we show that it is consistent with the population model of stellar binary black holes inferred from the first two observing runs.

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“…Unfortunately, NR simulations are too expensive to be directly used in data analysis applications and incorporated into astrophysical models. As a result, several approximate models that are much faster to evaluate have been developed for both waveforms [21][22][23][24][25][26][27][28][29][30][31] and remnant properties [18,19,[32][33][34][35][36][37][38][39][40][41][42][43][44][45][46][47][48][49][50]. These models typically assume an underlying phenomenology based on physical motivations, and calibrate any remaining free parameters to NR simulations.…”

Section: Introductionmentioning

confidence: 99%

Surrogate models for precessing binary black hole simulations with unequal masses

Varma

Field

Scheel

et al. 2019

Phys. Rev. Research

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352

358

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Only numerical relativity simulations can capture the full complexities of binary black hole mergers. These simulations, however, are prohibitively expensive for direct data analysis applications such as parameter estimation. We present two new fast and accurate surrogate models for the outputs of these simulations: the first model, NRSur7dq4, predicts the gravitational waveform and the second model, NRSur7dq4Remnant, predicts the properties of the remnant black hole. These models extend previous 7-dimensional, non-eccentric precessing models to higher mass ratios, and have been trained against 1528 simulations with mass ratios q ≤ 4 and spin magnitudes χ1, χ2 ≤ 0.8, with generic spin directions. The waveform model, NRSur7dq4, which begins about 20 orbits before merger, includes all ≤ 4 spin-weighted spherical harmonic modes, as well as the precession frame dynamics and spin evolution of the black holes. The final black hole model, NRSur7dq4Remnant, models the mass, spin, and recoil kick velocity of the remnant black hole. In their training parameter range, both models are shown to be more accurate than existing models by at least an order of magnitude, with errors comparable to the estimated errors in the numerical relativity simulations. We also show that the surrogate models work well even when extrapolated outside their training parameter space range, up to mass ratios q = 6.

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Accurate inspiral-merger-ringdown gravitational waveforms for nonspinning black-hole binaries including the effect of subdominant modes

Cited by 43 publications

References 64 publications

Surrogate model of hybridized numerical relativity binary black hole waveforms

Surrogate model of hybridized numerical relativity binary black hole waveforms

GW190412: Observation of a binary-black-hole coalescence with asymmetric masses

Surrogate models for precessing binary black hole simulations with unequal masses

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