Laying the foundation of the effective-one-body waveform models SEOBNRv5: improved accuracy and efficiency for spinning non-precessing binary black holes
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| Natura: | Preprint |
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2023
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| author | Pompili, Lorenzo Buonanno, Alessandra Estellés, Héctor Khalil, Mohammed van de Meent, Maarten Mihaylov, Deyan P. Ossokine, Serguei Pürrer, Michael Ramos-Buades, Antoni Mehta, Ajit Kumar Cotesta, Roberto Marsat, Sylvain Boyle, Michael Kidder, Lawrence E. Pfeiffer, Harald P. Scheel, Mark A. Rüter, Hannes R. Vu, Nils Dudi, Reetika Ma, Sizheng Mitman, Keefe Melchor, Denyz Thomas, Sierra Sanchez, Jennifer |
| author_facet | Pompili, Lorenzo Buonanno, Alessandra Estellés, Héctor Khalil, Mohammed van de Meent, Maarten Mihaylov, Deyan P. Ossokine, Serguei Pürrer, Michael Ramos-Buades, Antoni Mehta, Ajit Kumar Cotesta, Roberto Marsat, Sylvain Boyle, Michael Kidder, Lawrence E. Pfeiffer, Harald P. Scheel, Mark A. Rüter, Hannes R. Vu, Nils Dudi, Reetika Ma, Sizheng Mitman, Keefe Melchor, Denyz Thomas, Sierra Sanchez, Jennifer |
| contents | We present SEOBNRv5HM, a more accurate and faster inspiral-merger-ringdown gravitational waveform model for quasi-circular, 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, iv) incorporates information from second-order gravitational self-force (2GSF) 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 $10-300 M_{\odot}$ 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 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. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2303_18039 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | Laying the foundation of the effective-one-body waveform models SEOBNRv5: improved accuracy and efficiency for spinning non-precessing binary black holes Pompili, Lorenzo Buonanno, Alessandra Estellés, Héctor Khalil, Mohammed van de Meent, Maarten Mihaylov, Deyan P. Ossokine, Serguei Pürrer, Michael Ramos-Buades, Antoni Mehta, Ajit Kumar Cotesta, Roberto Marsat, Sylvain Boyle, Michael Kidder, Lawrence E. Pfeiffer, Harald P. Scheel, Mark A. Rüter, Hannes R. Vu, Nils Dudi, Reetika Ma, Sizheng Mitman, Keefe Melchor, Denyz Thomas, Sierra Sanchez, Jennifer General Relativity and Quantum Cosmology We present SEOBNRv5HM, a more accurate and faster inspiral-merger-ringdown gravitational waveform model for quasi-circular, 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, iv) incorporates information from second-order gravitational self-force (2GSF) 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 $10-300 M_{\odot}$ 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 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. |
| title | Laying the foundation of the effective-one-body waveform models SEOBNRv5: improved accuracy and efficiency for spinning non-precessing binary black holes |
| topic | General Relativity and Quantum Cosmology |
| url | https://arxiv.org/abs/2303.18039 |