Improved Cauchy-characteristic evolution system for high-precision numerical relativity waveforms

Moxon, Jordan; Scheel, Mark A.; Teukolsky, Saul A.

doi:10.1103/physrevd.102.044052

Cited by 44 publications

(75 citation statements)

References 41 publications

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“…(ii) The small amplitude of some of these modes [particularly (4,1) and (4,0)] can behave poorly when extrapolated [26]. We expect that this will be resolved in the future with Cauchy characteristic extraction [32,33].…”

Section: Modeling Methodsmentioning

confidence: 99%

Gravitational wave peak luminosity model for precessing binary black holes

Taylor

Varma

2020

Phys. Rev. D

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When two black holes merge, a tremendous amount of energy is released in the form of gravitational radiation in a short span of time, making such events among the most luminous phenomenon in the Universe. Models that predict the peak luminosity of black hole mergers are of interest to the gravitational wave community, with potential applications in tests of general relativity. We present a surrogate model for the peak luminosity that is directly trained on numerical relativity simulations of precessing binary black holes. Using Gaussian process regression, we interpolate the peak luminosity in the seven-dimensional parameter space of precessing binaries with mass ratios q ≤ 4 and spin magnitudes χ 1 , χ 2 ≤ 0.8. We demonstrate that our errors in estimating the peak luminosity are lower than those of existing fitting formulas by about an order of magnitude. In addition, we construct a model for the peak luminosity of aligned-spin binaries with mass ratios q ≤ 8 and spin magnitudes jχ 1z j; jχ 2z j ≤ 0.8. We apply our precessing model to infer the peak luminosity of the GW event GW190521 and find the results to be consistent with previous predictions.

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Section: Modeling Methodsmentioning

confidence: 99%

Gravitational wave peak luminosity model for precessing binary black holes

Taylor

Varma

2020

Phys. Rev. D

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“…In Appendix Sec. C 1, we derive the alteration between the SpEC tetrad and the tetrad used in SXS CCE [63]. In…”

Section: Appendix C: Subleading Tetrad Hazardsmentioning

confidence: 99%

“…where the Bondi-Sachs scalars J, K, β, V, U and coordinates are as defined in [63], which each represent components of the metric in Bondi-Sachs coordinates.…”

Section: Appendix A: Complex Weyl Characteristic Fieldsmentioning

confidence: 99%

Extending gravitational wave extraction using Weyl characteristic fields

et al. 2021

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We present a detailed methodology for extracting the full set of Newman-Penrose Weyl scalars from numerically generated spacetimes without requiring a tetrad that is completely orthonormal or perfectly aligned to the principal null directions. We also describe how to implement an extrapolation technique for computing the Weyl scalars' contribution at asymptotic null infinity in postprocessing. These methods have been used to produce Ψ 4 and h waveforms for the Simulating eXtreme Spacetimes (SXS) waveform catalog and now have been expanded to produce the entire set of Weyl scalars. These new waveform quantities are critical for the future of gravitational wave astronomy in order to understand the finiteamplitude gauge differences that can occur in numerical waveforms. We also present a new analysis of the accuracy of waveforms produced by the Spectral Einstein Code. While ultimately we expect Cauchy characteristic extraction to yield more accurate waveforms, the extraction techniques described here are far easier to implement and have already proven to be a viable way to produce production-level waveforms that can meet the demands of current gravitational-wave detectors.

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“…Therefore, we model all nonzero l ≤ 3 and ð4; AE4Þ modes, except the m ¼ 0 modes. We exclude m ¼ 0 memory modes because (nonoscillatory) Christodoulou memory is not accumulated sufficiently in our NR simulations [82]; this defect was recently addressed in both Cauchy characteristic extraction (CCE) [83][84][85] and extrapolation [86] approaches. The (4,2) mode, on the other hand, was found to have significant numerical error in the extrapolation procedure [77,79].…”

Section: Numerical Relativity Datamentioning

confidence: 99%

Eccentric binary black hole surrogate models for the gravitational waveform and remnant properties: Comparable mass, nonspinning case

et al. 2021

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We develop new strategies to build numerical relativity surrogate models for eccentric binary black hole systems, which are expected to play an increasingly important role in current and future gravitational-wave detectors. We introduce a new surrogate waveform model, NRSur2dq1Ecc, using 47 nonspinning, equalmass waveforms with eccentricities up to 0.2 when measured at a reference time of 5500M before merger. This is the first waveform model that is directly trained on eccentric numerical relativity simulations and does not require that the binary circularizes before merger. The model includes the (2,2), (3,2), and (4,4) spin-weighted spherical harmonic modes. We also build a final black hole model, NRSur2dq1Ec-cRemnant, which models the mass, and spin of the remnant black hole. We show that our waveform model can accurately predict numerical relativity waveforms with mismatches ≈10 −3 , while the remnant model can recover the final mass and dimensionless spin with absolute errors smaller than ≈5 × 10 −4 M and ≈2 × 10 −3 respectively. We demonstrate that the waveform model can also recover subtle effects like mode mixing in the ringdown signal without any special ad hoc modeling steps. Finally, we show that despite being trained only on equal-mass binaries, NRSur2dq1Ecc can be reasonably extended up to mass ratio q ≈ 3 with mismatches ≃10 −2 for eccentricities smaller than ∼0.05 as measured at a reference time of 2000M before merger. The methods developed here should prove useful in the building of future eccentric surrogate models over larger regions of the parameter space.

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Improved Cauchy-characteristic evolution system for high-precision numerical relativity waveforms

Cited by 44 publications

References 41 publications

Gravitational wave peak luminosity model for precessing binary black holes

Gravitational wave peak luminosity model for precessing binary black holes

Extending gravitational wave extraction using Weyl characteristic fields

Eccentric binary black hole surrogate models for the gravitational waveform and remnant properties: Comparable mass, nonspinning case

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