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Published December 15, 2023 | Published
Journal Article Open

Laying the foundation of the effective-one-body waveform models SEOBNRv5: Improved accuracy and efficiency for spinning nonprecessing binary black holes

Abstract

We present SEOBNRv5HM, a more accurate and faster inspiral-merger-ringdown gravitational waveform model for quasicircular, spinning, nonprecessing binary black holes within the effective-one-body (EOB) formalism. Compared to its predecessor, SEOBNRv4HM, the waveform model (i) incorporates recent high-order post-Newtonian results in the inspiral, with improved resummations, (ii) includes the gravitational modes (ℓ,|m|)=(3,2),(4,3), in addition to the (2,2), (3,3), (2,1), (4,4), (5,5) modes already implemented in SEOBNRv4HM, (iii) is calibrated to larger mass ratios and spins using a catalog of 442 numerical-relativity (NR) simulations and 13 additional waveforms from black-hole perturbation theory, and (iv) incorporates information from second-order gravitational self-force in the nonspinning modes and radiation-reaction force. Computing the unfaithfulness against NR simulations, we find that for the dominant (2,2) mode the maximum unfaithfulness in the total mass range 10–300 M_⊙ is below 10⁻³ for 90% of the cases (38% for SEOBNRv4HM). When including all modes up to ℓ=5 we find 98% (49%) of the cases with unfaithfulness below 10⁻² (10⁻³), while these numbers reduce to 88% (5%) when using SEOBNRv4HM. Furthermore, the model shows improved agreement with NR in other dynamical quantities (e.g., the angular momentum flux and binding energy), providing a powerful check of its physical robustness. We implemented the waveform model in a high-performance python package (pyseobnr), which leads to evaluation times faster than SEOBNRv4HM by a factor of 10 to 50, depending on the configuration, and provides the flexibility to easily include spin-precession and eccentric effects, thus making it the starting point for a new generation of EOBNR waveform models (SEOBNRv5) to be employed for upcoming observing runs of the LIGO-Virgo-KAGRA detectors.

Copyright and License

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.

Acknowledgement

It is our pleasure to thank Geraint Pratten, Stanislav Babak, Alice Bonino, Eleanor Hamilton, N. V. Krishnendu, Piero Rettegno, Riccardo Sturani, and Jooheon Yoo for performing the LIGO-Virgo-KAGRA review of the SEOBNRv5 models. Part of M. K.'s work on this paper is supported by the Perimeter Institute for Theoretical Physics. Research at Perimeter Institute is supported in part by the Government of Canada through the Department of Innovation, Science and Economic Development and by the Province of Ontario through the Ministry of Colleges and Universities. M. v. d. M. is supported by VILLUM FONDEN (Grant No. 37766), and the Danish Research Foundation. R. C. is supported by NSF Grants No. AST-2006538, No. PHY-2207502, No. PHY-090003, and No. PHY-20043, and NASA Grants No. 19-ATP19-0051, No. 20-LPS20-0011, and No. 21-ATP21-0010. H. R. is supported by the Fundação para a Ciência e Tecnologia (FCT) within the Projects No. UID/04564/2021, No. UIDB/04564/2020, No. UIDP/04564/2020, and No. EXPL/FIS-AST/0735/2021. This work was supported in part by the Sherman Fairchild Foundation, by NSF Grants No. PHY-2011961, No. PHY-2011968, and No. OAC-1931266 at Caltech; by NSF Grants No. PHY-1912081, No. PHY-2207342, No. OAC-1931280, and No. OAC-2209655 at Cornell; by NSF Awards No. AST-1559694 and No. PHY-1654359; by Nicholas and Lee Begovich; and by the Dan Black Family Trust. The computational work for this manuscript was carried out on the hypatia computer cluster at the Max Planck Institute for Gravitational Physics in Potsdam. SEOBNRv5HM is publicly available through the python package pyseobnr [221]. Stable versions of pyseobnr are published through the Python Package Index (PyPI), and can be installed via pip install pyseobnr. This research has made use of data or software obtained from the Gravitational Wave Open Science Center ([222]), a service of LIGO Laboratory, the LIGO Scientific Collaboration, the Virgo Collaboration, and KAGRA. LIGO Laboratory and Advanced LIGO are funded by the United States National Science Foundation (NSF) as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. Virgo is funded, through the European Gravitational Observatory (EGO), by the French Centre National de Recherche Scientifique (CNRS), the Italian Istituto Nazionale di Fisica Nucleare (INFN) and the Dutch Nikhef, with contributions by institutions from Belgium, Germany, Greece, Hungary, Ireland, Japan, Monaco, Poland, Portugal, and Spain. KAGRA. is supported by the Ministry of Education, Culture, Sports, Science and Technology (MEXT), Japan Society for the Promotion of Science (JSPS) in Japan; the National Research Foundation (NRF) and Ministry of Science and ICT (MSIT) in Korea; and Academia Sinica (AS) and the National Science and Technology Council (NSTC) in Taiwan.

Code Availability

SEOBNRv5_ROM is publicly available through lalsuite [199].

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Additional details

Created:
December 19, 2023
Modified:
December 19, 2023