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Phenomenological model for the gravitational-wave signal from precessing binary black holes with two-spin effects

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arxiv 1809.10113 v1 pith:HUDLYMN3 submitted 2018-09-26 gr-qc

Sebastian Khan , Katerina Chatziioannou , Mark Hannam , Frank Ohme This is my paper · ORCID
classification gr-qc
keywords modeleffectsprecessionimrphenompv3waveformdynamicsimrphenompv2models
verification ladder T0 review T1 audit T2 compute T3 formal
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The properties of compact binaries, such as masses and spins, are imprinted in the gravitational-waves they emit and can be measured using parameterised waveform models. Accurately and efficiently describing the complicated precessional dynamics of the various angular momenta of the system in these waveform models is the object of active investigation. One of the key models extensively used in the analysis of LIGO and Virgo data is the single-precessing-spin waveform model IMRPhenomPv2. In this article we present a new model IMRPhenomPv3 which includes the effects of two independent spins in the precession dynamics. Whereas IMRPhenomPv2 utilizes a single-spin frequency-dependent post-Newtonian rotation to describe precession effects, the improved model, IMRPhenomPv3, employs a double-spin rotation that is based on recent developments in the description of precessional dynamics. Besides double-spin precession, the improved model benefits from a more accurate description of precessional effects. We validate our new model against a large set of precessing numerical-relativity simulations. We find that IMRPhenomPv3 has better agreement with the inspiral portion of precessing binary-black-hole simulations and is more robust across a larger region of the parameter space than IMRPhenomPv2. As a first application we analyse, for the first time, the gravitational-wave event GW151226 with a waveform model that describes two-spin precession. Within statistical uncertainty our results are consistent with published results. IMRPhenomPv3 will allow studies of the measurability of individual spins of binary black holes using GWs and can be used as a foundation upon which to build further improvements, such as modeling precession through merger, extending to higher multipoles, and including tidal effects.

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Cited by 9 Pith papers

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

  1. Impact of numerical-relativity waveform calibration on parametrized post-Einsteinian tests

    gr-qc 2026-03 accept novelty 6.0 of 10

    NR late-inspiral calibration systematics in IMRPhenomD produce false ppE GR violations at O5 SNRs ≳60; an uncertainty-aware baseline restores consistency with GR up to SNR 330.

  2. Advancing the Effective-One-Body Framework in the Test-Mass Limit

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    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.

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    gr-qc 2025-12 conditional novelty 6.0 of 10

    Eccentric BBH signals can masquerade as wave-optics microlensing in quasicircular analyses, but eccentric recovery templates break the degeneracy.

  4. Coincident morphological transitions in precessing black-hole binaries

    gr-qc 2025-08 conditional novelty 6.0 of 10

    Every coincident double or triple spin-morphology transition in post-Newtonian black-hole binaries is derived analytically, giving closed-form radii (rwide, rUD±) and parameter conditions for five allowed cases and on...

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    astro-ph.HE 2026-07 conditional novelty 5.0 of 10

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  7. 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.

  8. Considering lensing effect on gravitational wave signals from black holes in mass gap

    astro-ph.HE 2025-12 reject novelty 4.0 of 10

    Gravitational lensing could in principle explain apparent mass-gap black-hole mergers, but the required magnifications are μ≈12–39 for GW190521 and μ≈320–444 for GW231123 depending on assumptions—and the paper's abstr...

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    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.

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