Analytical meets numerical relativity: status of complete gravitational waveform models for binary black holes

Ohme, F.

doi:10.1088/0264-9381/29/12/124002

Cited by 42 publications

(50 citation statements)

References 92 publications

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“…Clearly the ROM error is much smaller than the uncertainty in the original model. We can then estimate that the mismatch between "true" NR waveforms (against which SEOBNRv1 has been compared) and the surrogate model presented here is better than 1% at high total masses and better than 0.6% below 50M by using the triangle inequality [73] M(h ROM , h true ) ≤ M(h ROM , h SEOBNRv1 ) + M(h SEOBNRv1 , h true ) 2 .…”

Section: Discussionmentioning

confidence: 99%

Frequency-domain reduced order models for gravitational waves from aligned-spin compact binaries

Pürrer

2014

Class. Quantum Grav.

205

288

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Abstract. Black-hole binary coalescences are one of the most promising sources for the first detection of gravitational waves. Fast and accurate theoretical models of the gravitational radiation emitted from these coalescences are highly important for the detection and extraction of physical parameters. Spinning effective-one-body (EOB) models for binaries with aligned spins have been shown to be highly faithful, but are slow to generate and thus have not yet been used for parameter estimation studies. I provide a frequency-domain singular value decomposition (SVD)-based surrogate reduced order model that is thousands of times faster for typical system masses and has a faithfulness mismatch of better than ∼ 0.1% with the original SEOBNRv1 model for advanced LIGO detectors. This model enables parameter estimation studies up to signal-to-noise ratios (SNRs) of 20 and even up to SNR 50 for total masses below 50M . This article discusses various choices for approximations and interpolation over the parameter space that can be made for reduced order models of spinning compact binaries, provides a detailed discussion of errors arising in the construction and assesses the fidelity of such models.

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Section: Discussionmentioning

confidence: 99%

Frequency-domain reduced order models for gravitational waves from aligned-spin compact binaries

Pürrer

2014

Class. Quantum Grav.

205

288

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“…[23] for an overview). In these configurations the black holes orbit in a spatially fixed twodimensional plane, and the dominant mode of the GW signal can be described by simple monotonic functions for the amplitude and phase.…”

Section: Introductionmentioning

confidence: 99%

Towards models of gravitational waveforms from generic binaries: II. Modelling precession effects with a single effective precession parameter

2015

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Gravitational waves (GWs) emitted by generic black-hole binaries show a rich structure that directly reflects the complex dynamics introduced by the precession of the orbital plane, which poses a real challenge to the development of generic waveform models. Recent progress in modelling these signals relies on an approximate decoupling between the nonprecessing secular inspiral and a precession-induced rotation. However, the latter depends in general on all physical parameters of the binary which makes modelling efforts as well as understanding parameter-estimation prospects prohibitively complex. Here we show that the dominant precession effects can be captured by a reduced set of spin parameters. Specifically, we introduce a single effective precession spin parameter, χ p , which is defined from the spin components that lie in the orbital plane at some (arbitrary) instant during the inspiral. We test the efficacy of this parameter by considering binary inspiral configurations specified by the physical parameters of a corresponding nonprecessing-binary configuration (total mass, mass ratio, and spin components (anti) parallel to the orbital angular momentum), plus the effective precession spin applied to the larger black hole. We show that for an overwhelming majority of random precessing configurations, the precession dynamics during the inspiral are well approximated by our equivalent configurations. Our results suggest that in the comparable-mass regime waveform models with only three spin parameters faithfully represent generic waveforms, which has practical implications for the prospects of GW searches, parameter estimation and the numerical exploration of the precessing-binary parameter space.

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“…Such post-Newtonian waveforms play an important role in the waveform modeling for groundbased interferometric gravitational-wave detectors (see, e.g., [8]). …”

Section: Introductionmentioning

confidence: 99%

Comparing post-Newtonian and numerical relativity precession dynamics

et al. 2015

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Binary black-hole systems are expected to be important sources of gravitational waves for upcoming gravitational-wave detectors. If the spins are not colinear with each other or with the orbital angular momentum, these systems exhibit complicated precession dynamics that are imprinted on the gravitational waveform. We develop a new procedure to match the precession dynamics computed by post-Newtonian (PN) theory to those of numerical binary black-hole simulations in full general relativity. For numerical relativity (NR) simulations lasting approximately two precession cycles, we find that the PN and NR predictions for the directions of the orbital angular momentum and the spins agree to better than ∼ 1• with NR during the inspiral, increasing to 5• near merger. Nutation of the orbital plane on the orbital time-scale agrees well between NR and PN, whereas nutation of the spin direction shows qualitatively different behavior in PN and NR. We also examine how the PN equations for precession and orbital-phase evolution converge with PN order, and we quantify the impact of various choices for handling partially known PN terms.

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Analytical meets numerical relativity: status of complete gravitational waveform models for binary black holes

Cited by 42 publications

References 92 publications

Frequency-domain reduced order models for gravitational waves from aligned-spin compact binaries

Frequency-domain reduced order models for gravitational waves from aligned-spin compact binaries

Towards models of gravitational waveforms from generic binaries: II. Modelling precession effects with a single effective precession parameter

Comparing post-Newtonian and numerical relativity precession dynamics

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