Multipolar effective-one-body waveforms for precessing binary black holes: Construction and validation
By S. Ossokine, A. Buonanno, S. Marsat, R. Cotesta, Stanislav Babak, Tim Dietrich, Roland Haas, Ian Hinder, Harald P. Pfeiffer, Michael Pürrer and 5 more. Physical Review D, 2020
163 citations recorded by the source corpus.
As gravitational-wave detectors become more sensitive, 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 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 systems, 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 inspiral, merger and ringdown (IMR) 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 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 new 118 precessing NR waveforms, which span mass ratios 1-4 and 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 $20-200 M_\odot$, is below $3\%$ ($1\%$). Those numbers become $83\%$ ($20\%$) when using the IMR, multipolar, precessing phenomenological model IMRPhenomPv3HM. We investigate the impact of such unfaithfulness values with two parameter-estimation studies on synthetic signals. We also compute the unfaithfulness between those waveform models and 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.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/7d14f798acc062d17fa987f1cd7a2eccf87425e1
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In Astronomy and Astrophysics
Citations in the corpus
- Bayesian inference for compact binary coalescences with bilby: validation and application to the first LIGO–Virgo gravitational-wave transient catalogue (2020, background): “…expensive to evaluate, e.g., time-domain signal models such as spin-precessing effective-one-body models with higher-order modes (Bohé et al. 2017; Ossokine et al. 2020), numerical-relativity surrogate models (Blackman et al. 2017) and models including tidal effects (Nagar et al. 2018; Lackey et…”
- GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run (2020, methodology): “8−22.4 M⊙, where we average over SEOBNRv4PHM, NRSur7dq4, and IMRPhenomPv3HM waveform families.”