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Multipolar Effective-One-Body Waveforms for Precessing Binary Black Holes: Construction and Validation

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arxiv 2004.09442 v1 pith:UJCGMS66 submitted 2020-04-20 gr-qc

Serguei Ossokine , Alessandra Buonanno , Sylvain Marsat , Roberto Cotesta , Stanislav Babak , Tim Dietrich , Roland Haas , Ian Hinder
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Harald P. Pfeiffer Michael Pürrer Charles J. Woodford Michael Boyle Lawrence E. Kidder Mark A. Scheel Béla Szilágyi
This is my paper · ORCID
classification gr-qc
keywords precessingmodelwaveformsbinarymultipolarseobnrv4phmspinsunfaithfulness
verification ladder T0 review T1 audit T2 compute T3 formal
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abstract

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.

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Cited by 7 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Fast, accurate, and differentiable: a neural-network surrogate for NRSur7dq4 precessing binary black hole waveforms

    gr-qc 2026-07 accept novelty 6.0 of 10

    A piecewise MLP surrogate emulates NRSur7dq4 over its full domain at NR-faithful accuracy with ~1 ms GPU latency and a fully differentiable JAX likelihood pipeline.

  2. Gravitational-wave astronomy requires population-informed parameter estimation

    gr-qc 2026-04 unverdicted novelty 6.0 of 10

    Single-event GW parameter estimates under reference priors are population-biased; hierarchical, population-informed re-analysis is needed and changes the identification of the most extreme black holes in the catalog.

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    gr-qc 2026-03 conditional novelty 6.0 of 10

    SEOB-TML cuts dephasing by up to an order of magnitude in the test-mass limit by Q-factorizing the flux (including horizon absorption) and by modeling mode mixing with extracted QNM coefficients.

  4. AthenaK simulations of the binary black hole merger GW150914

    gr-qc 2025-06 conditional novelty 5.0 of 10

    A new open-source GPU code, AthenaK, reproduces the GW150914 merger: remnant mass within 0.01%, spin within 0.02%, and waveform phase within about 0.35 radians of established simulations.

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    High-SNR BBH events GW230814 and GW250114 yield ΔQ/Q posteriors consistent with zero in full, inspiral, and post-inspiral analyses using the Ψ_FD model, supporting Kerr within current sensitivity.

  6. PhenomXPNR: An improved gravitational wave model linking precessing inspirals and NR-calibrated merger-ringdown

    gr-qc 2025-07 conditional novelty 4.0 of 10

    PhenomXPNR is a fast frequency-domain gravitational-wave template for spinning black-hole mergers that combines post-Newtonian inspiral precession with numerical-relativity-calibrated merger and ringdown.

  7. Effectiveness of Stacks in the Stacked Hilbert-Huang Transform

    astro-ph.IM 2025-06 reject novelty 4.0 of 10

    Averaging many Hilbert spectra of noise-added trials, called sHHT, is claimed to trace rapid frequency changes more clearly than standard HHT, with an approximate bias formula that has a missing term.

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