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Targeted large mass ratio numerical relativity surrogate waveform model for GW190814

Yoo, Jooheon and Varma, Vijay and Giesler, Matthew and Scheel, Mark A. and Haster, Carl-Johan and Pfeiffer, Harald P. and Kidder, Lawrence E. and Boyle, Michael (2022) Targeted large mass ratio numerical relativity surrogate waveform model for GW190814. Physical Review D, 106 (4). Art. No. 044001. ISSN 2470-0010. doi:10.1103/physrevd.106.044001.

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Gravitational wave observations of large mass ratio compact binary mergers like GW190814 highlight the need for reliable, high-accuracy waveform templates for such systems. We present nrhybsur2dq15, a new surrogate model trained on hybridized numerical relativity (NR) waveforms with mass ratios q≤15 and aligned spins |χ1z| ≤ 0.5 and χ2z = 0. We target the parameter space of GW190814-like events as large mass ratio NR simulations are very expensive. The model includes the (2, 2), (2, 1), (3, 3), (4, 4), and (5, 5) spin-weighted spherical harmonic modes and spans the entire LIGO-Virgo bandwidth (with flow = 20 Hz) for total masses M ≳ 9.5  M⊙. nrhybsur2dq15 accurately reproduces the hybrid waveforms, with mismatches below ∼2 × 10⁻³ for total masses 10 M⊙ ≤ M ≤ 300 M⊙. This is at least an order of magnitude improvement over existing semianalytical models for GW190814-like systems. Finally, we reanalyze GW190814 with the new model and obtain source parameter constraints consistent with previous work.

Item Type:Article
Related URLs:
URLURL TypeDescription
Yoo, Jooheon0000-0002-3251-0924
Varma, Vijay0000-0002-9994-1761
Giesler, Matthew0000-0003-2300-893X
Haster, Carl-Johan0000-0001-8040-9807
Pfeiffer, Harald P.0000-0001-9288-519X
Kidder, Lawrence E.0000-0001-5392-7342
Boyle, Michael0000-0002-5075-5116
Additional Information:We thank Hector Estelles and Alessandro Nagar for comments on the manuscript. This work was supported in part by the Sherman Fairchild Foundation and by National Science Foundation (NSF) Grants No. PHY-2011961, No. PHY-2011968, and No. OAC-1931266 at Caltech, and NSF Grants No. PHY-1912081 and No. OAC-1931280 at Cornell. V. V. acknowledges funding from the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie Grant Agreement No. 896869. V. V. was supported by a Klarman Fellowship at Cornell and also received support from a Marie Curie Fellowship. C.-J. H. acknowledges support of the NSF and the LIGO Laboratory. NR simulations were conducted on the Frontera computing project at the Texas Advanced Computing Center. Additional computations were performed on the Wheeler cluster at Caltech, which is supported by the Sherman Fairchild Foundation and by Caltech, and the High Performance Cluster at Caltech. This material is based upon work supported by NSF’s LIGO Laboratory which is a major facility fully funded by the NSF. This research made use of data, software, and/or web tools obtained from the Gravitational Wave Open Science Center [89], a service of the LIGO Laboratory, the LIGO Scientific Collaboration, and the Virgo Collaboration.
Funding AgencyGrant Number
Sherman Fairchild FoundationUNSPECIFIED
Marie Curie Fellowship896869
Cornell UniversityUNSPECIFIED
Issue or Number:4
Record Number:CaltechAUTHORS:20220830-590227900
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:116633
Deposited By: Tony Diaz
Deposited On:30 Aug 2022 23:53
Last Modified:31 Aug 2022 17:12

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