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Fixing the BMS Frame of Numerical Relativity Waveforms
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Fixing the BMS Frame of Numerical Relativity Waveforms
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Understanding the Bondi-Metzner-Sachs (BMS) frame of the gravitational waves produced by numerical relativity is crucial for ensuring that analyses on such waveforms are performed properly. It is also important that models are built from waveforms in the same BMS frame. Up until now, however, the BMS frame of numerical waveforms has not been thoroughly examined, largely because the necessary tools have not existed. In this paper, we show how to analyze and map to a suitable BMS frame for numerical waveforms calculated with the Spectral Einstein Code (SpEC). However, the methods and tools that we present are general and can be applied to any numerical waveforms. We present an extensive study of 13 binary black hole systems that broadly span parameter space. From these simulations, we extract the strain and also the Weyl scalars using both SpECTRE's Cauchy-characteristic extraction module and also the standard extrapolation procedure with a displacement memory correction applied during postprocessing. First, we show that the current center-of-mass correction used to map these waveforms to the center-of-mass frame is not as effective as previously thought. Consequently, we also develop an improved correction that utilizes asymptotic Poincar\'e charges instead of a Newtonian center-of-mass trajectory. Next, we map our waveforms to the post-Newtonian (PN) BMS frame using a PN strain waveform. This helps us find the unique BMS transformation that minimizes the $L^{2}$ norm of the difference between the numerical and PN strain waveforms during the early inspiral phase. We find that once the waveforms are mapped to the PN BMS frame, they can be hybridized with a PN strain waveform much more effectively than if one used any of the previous alignment schemes, which only utilize the Poincar\'e transformations.
Forward citations
Cited by 7 Pith papers
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Towards long and accurate numerical relativity waveforms of binary black holes beyond general relativity
Spectral methods plus comoving fixing-the-equations drivers yield 40+ cycle equal-mass sGB binary waveforms with phase error ≲1 rad, distinguishable from GR and merging earlier.
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High-accuracy drivers to simulate black hole binaries beyond general relativity with the fixing-the-equations approach
Comoving tensor-aware driver equations in SpECTRE yield ~40-cycle sGB binary waveforms with O(1) rad phase error and eccentricity ≲10^{-3}, free of spurious spin growth.
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The Bondi--Sachs gauge, BMS frames, and memory in black hole perturbation theory
Introduces a gauge transformation framework for BMS frames in multiscale black hole perturbation theory on Kerr that incorporates memory effects and avoids infrared divergences.
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Fixing the center-of-mass frame of numerical relativity waveforms using the post-Newtonian center-of-mass charge
A post-Newtonian model of the boosted center-of-mass charge makes BMS frame-fixing of nonprecessing, unequal-mass NR waveforms less sensitive to the fitting window, reducing parameter variance by up to ~25x.
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Fixing the center-of-mass frame of numerical relativity waveforms using the post-Newtonian center-of-mass charge
A post-Newtonian boosted center-of-mass charge template makes numerical-relativity frame-fixing up to ~25x more robust to the fitting-window choice.
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A comprehensive look into the accuracy of SpEC binary black hole waveforms
Simulated black-hole merger waveforms accumulate numerical error over time, but the merger stage is not intrinsically less accurate once aligned on its own, and resolution-exchanged differences show no systematic bias...
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Constraining Gravitational Wave Memory with Hierarchical Inference
Hierarchical Bayesian inference on GWTC-5.0 constrains the memory enhancement factor to 0.26 with large uncertainties consistent with the GR value of 1 and forecasts that 2000 detections are needed for a 1σ constraint...
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