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New twists in compact binary waveform modelling: a fast time domain model for precession

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arxiv 2105.05872 v2 pith:CTDDU7G4 submitted 2021-05-12 gr-qc

Héctor Estellés , Marta Colleoni , Cecilio García-Quirós , Sascha Husa , David Keitel , Maite Mateu-Lucena , Maria de Lluc Planas , Antoni Ramos-Buades This is my paper · ORCID
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keywords domainmodelanglesapproximationeulerprecessingtimebinary
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We present IMRPhenomTPHM, a phenomenological model for the gravitational wave signals emitted by the coalescence of quasi-circular precessing binary black holes systems. The model is based on the "twisting up" approximation, which maps non-precessing signals to precessing ones in terms of a time dependent rotation described by three Euler angles, and which has been utilized in several frequency domain waveform models that have become standard tools in gravitational wave data analysis. Our model is however constructed in the time domain, which allows several improvements over the frequency domain models: we do not use the stationary phase approximation, we employ a simple approximation for the precessing Euler angles for the ringdown signal, and we implement a new method for computing the Euler angles through the evolution of the spin dynamics of the system, which is more accurate and also computationally efficient.

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Forward citations

Cited by 10 Pith papers

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    astro-ph.CO 2026-08 conditional novelty 6.0 of 10

    The rate of compound gravitational-wave lensing by intermediate-mass black holes in globular clusters is at most about 10^-3 of galaxy-scale lensed events, disfavoring GW231123 as such an event.

  2. Ensemble-Based Residual Tests of GW231123 across Waveform Models

    gr-qc 2026-08 conditional novelty 6.0 of 10

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    Fusing a simulation-trained common-source mass posterior with waveform features raises lensed-event detection efficiency from 20.8% to 35.2% at 1% false-positive rate and lowers the SNR for 50% efficiency from 45.3 to 33.5.

  4. 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.

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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.

  6. TDI on the fly

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    A sparse-sampling algorithm computes TDI response for any gravitational waveform on a coarse grid, reducing cost by roughly 10^4 while matching full-cadence results.

  7. Fast frequency-domain gravitational waveforms for precessing binaries with a new twist

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    IMRPhenomXPHM-SpinTaylor computes precession angles by numerically solving post-Newtonian spin equations in the frequency domain and improves match to numerical relativity from mean mismatch 6.3e-3 to 5.1e-3.

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    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.

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