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Fixing the BMS frame of numerical relativity waveforms

Mitman, Keefe and Khera, Neev and Iozzo, Dante A. B. and Stein, Leo C. and Boyle, Michael and Deppe, Nils and Kidder, Lawrence E. and Moxon, Jordan and Pfeiffer, Harald P. and Scheel, Mark A. and Teukolsky, Saul A. and Throwe, William (2021) Fixing the BMS frame of numerical relativity waveforms. Physical Review D, 104 (2). Art. No. 024051. ISSN 2470-0010. doi:10.1103/physrevd.104.024051.

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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 Poincaré 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 L² 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 Poincaré transformations.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Mitman, Keefe0000-0003-0276-3856
Khera, Neev0000-0003-3515-2859
Iozzo, Dante A. B.0000-0002-7244-1900
Stein, Leo C.0000-0001-7559-9597
Boyle, Michael0000-0002-5075-5116
Deppe, Nils0000-0003-4557-4115
Kidder, Lawrence E.0000-0001-5392-7342
Moxon, Jordan0000-0001-9891-8677
Pfeiffer, Harald P.0000-0001-9288-519X
Scheel, Mark A.0000-0001-6656-9134
Teukolsky, Saul A.0000-0001-9765-4526
Throwe, William0000-0001-5059-4378
Additional Information:© 2021 American Physical Society. Received 11 May 2021; accepted 17 June 2021; published 20 July 2021. Computations were performed with the High Performance Computing Center and the Wheeler cluster at Caltech. This work was supported in part by the Sherman Fairchild Foundation and by NSF Grants No. PHY-2011961, No. PHY-2011968, and No. OAC-1931266 at Caltech, NSF Grants No. PHY-1912081 and No. OAC-1931280 at Cornell, and NSF Grant No. PHY-1806356, Grant No. UN2017-92945 from the Urania Stott Fund of the Pittsburgh Foundation, and the Eberly research funds of Penn State at Penn State.
Funding AgencyGrant Number
Sherman Fairchild FoundationUNSPECIFIED
Pittsburgh FoundationUN2017-92945
Pennsylvania State UniversityUNSPECIFIED
Issue or Number:2
Record Number:CaltechAUTHORS:20210821-163947559
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:110367
Deposited By: Tony Diaz
Deposited On:21 Aug 2021 16:46
Last Modified:21 Aug 2021 16:46

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