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

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2303.18039.pdf

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PhysRevD.108.124035.pdf

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##### Citation

Pompili, L., Buonanno, A., Estellés Estrella, H., Khalil, M., van de Meent, M., Mihaylov, D., et al. (2023).
Laying the foundation of the effective-one-body waveform models SEOBNRv5: Improved accuracy and efficiency for spinning nonprecessing
binary black holes.* Physical Review D,* *108*(12): 124035.
doi:10.1103/PhysRevD.108.124035.

Cite as: https://hdl.handle.net/21.11116/0000-000C-E78E-0

##### Abstract

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.

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.