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Multipolar effective-one-body waveforms for precessing binary black holes: Construction and validation

Ossokine, Serguei and Buonanno, Alessandra and Marsat, Sylvain and Cotesta, Roberto and Babak, Stanislav and Dietrich, Tim and Haas, Roland and Hinder, Ian and Pfeiffer, Harald P. and Pürrer, Michael and Woodford, Charles J. and Boyle, Michael and Kidder, Lawrence E. and Scheel, Mark A. and Szilágyi, Béla (2020) Multipolar effective-one-body waveforms for precessing binary black holes: Construction and validation. Physical Review D, 102 (4). Art. No. 044055. ISSN 2470-0010. https://resolver.caltech.edu/CaltechAUTHORS:20200909-074320784

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Abstract

As gravitational-wave detectors become more sensitive and broaden their frequency bandwidth, we will access a greater variety of signals emitted by compact binary systems, shedding light on their astrophysical origin and environment. A key physical effect that can distinguish among different formation scenarios is the misalignment of the spins with the orbital angular momentum, causing the spins and the binary’s orbital plane to precess. To accurately model such precessing signals, especially when masses and spins vary in the wide astrophysical range, it is crucial to include multipoles beyond the dominant quadrupole. Here, we develop the first multipolar precessing waveform model in the effective-one-body (EOB) formalism for the entire coalescence stage (i.e., inspiral, merger and ringdown) of binary black holes: SEOBNRv4PHM. In the nonprecessing limit, the model reduces to SEOBNRv4HM, which was calibrated to numerical-relativity (NR) simulations, and waveforms from black-hole perturbation theory. We validate SEOBNRv4PHM by comparing it to the public catalog of 1405 precessing NR waveforms of the Simulating eXtreme Spacetimes (SXS) collaboration, and also to 118 SXS precessing NR waveforms, produced as part of this project, which span mass ratios 1-4 and (dimensionless) black-hole’s spins up to 0.9. We stress that SEOBNRv4PHM is not calibrated to NR simulations in the precessing sector. We compute the unfaithfulness against the 1523 SXS precessing NR waveforms, and find that, for 94% (57%) of the cases, the maximum value, in the total mass range 20−200  M⊙, is below 3% (1%). Those numbers change to 83% (20%) when using the inspiral-merger-ringdown, multipolar, precessing phenomenological model IMRPhenomPv3HM. We investigate the impact of such unfaithfulness values with two Bayesian, parameter-estimation studies on synthetic signals. We also compute the unfaithfulness between those waveform models as a function of the mass and spin parameters to identify in which part of the parameter space they differ the most. We validate them also against the multipolar, precessing NR surrogate model NRSur7dq4, and find that the SEOBNRv4PHM model outperforms IMRPhenomPv3HM.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1103/physrevd.102.044055DOIArticle
https://arxiv.org/abs/2004.09442arXivDiscussion Paper
ORCID:
AuthorORCID
Ossokine, Serguei0000-0002-2579-1246
Cotesta, Roberto0000-0001-6568-6814
Haas, Roland0000-0003-1424-6178
Hinder, Ian0000-0003-3548-9101
Pfeiffer, Harald P.0000-0001-9288-519X
Pürrer, Michael0000-0002-3329-9788
Woodford, Charles J.0000-0003-4174-0577
Kidder, Lawrence E.0000-0001-5392-7342
Szilágyi, Béla0000-0001-7744-6180
Additional Information:© 2020 Published by the American Physical Society under the terms of the Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to the author(s) and the published article’s title, journal citation, and DOI. Open access publication funded by the Max Planck Society. Received 29 April 2020; accepted 7 July 2020; published 31 August 2020. It is our pleasure to thank Andrew Matas for providing us with the scripts to make the parameter-estimation plots, and Sebastian Khan for useful discussions on the faithfulness calculation. We would also like to thank the SXS collaboration for help and support with the spec code in producing the new NR simulations presented in this paper, and for making the large catalog of BBH simulations publicly available. R. H. acknowledges support through OAC-1550514, OAC-2004879, and ACI-1238993. The new 118 SXS NR simulations were produced using the high-performance compute (HPC) cluster Minerva at the Max Planck Institute for Gravitational Physics in Potsdam, on the Hydra cluster at the Max Planck Society at the Garching facility, and on the SciNet cluster at the University of Toronto. The data-analysis studies were obtained with the HPC clusters Hypatia and Minerva at the Max Planck Institute for Gravitational Physics. The transformation and manipulation of waveforms were done using the gwframes package [83,130].
Group:TAPIR
Funders:
Funding AgencyGrant Number
NSFOAC-1550514
NSFOAC-2004879
NSFACI-1238993
Max Planck SocietyUNSPECIFIED
Issue or Number:4
Record Number:CaltechAUTHORS:20200909-074320784
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20200909-074320784
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:105286
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:09 Sep 2020 17:29
Last Modified:09 Sep 2020 17:29

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