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Time domain phenomenological model of gravitational wave subdominant harmonics for quasi-circular non-precessing binary black hole coalescences

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arxiv 2012.11923 v1 pith:I7MNRRCG submitted 2020-12-22 gr-qc

Héctor Estellés , Sascha Husa , Marta Colleoni , David Keitel , Maite Mateu-Lucena , Cecilio García-Quirós , Antoni Ramos-Buades , Angela Borchers This is my paper · ORCID
classification gr-qc
keywords modeldomaingravitationalharmonicsmodephenomenologicalwavebinary
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abstract

In this work we present an extension of the time domain phenomenological model IMRPhenomT for gravitational wave signals from binary black hole coalescences to include subdominant harmonics, specifically the $(l=2, m=\pm 1)$, $(l=3, m=\pm 3)$, $(l=4, m=\pm 4)$ and $(l=5, m=\pm 5)$ spherical harmonics. We also improve our model for the dominant $(l=2, m=\pm 2)$ mode and discuss mode mixing for the $(l=3, m=\pm 2)$ mode. The model is calibrated to numerical relativity solutions of the full Einstein equations up to mass ratio 18, and to numerical solutions of the Teukolsky equations for higher mass ratios. This work complements the latest generation of traditional frequency domain phenomenological models (IMRPhenomX), and provides new avenues to develop computationally efficient models for gravitational wave signals from generic compact binaries.

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Cited by 3 Pith papers

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

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

    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.

  2. A stepping stone toward detecting gravitational wave memory: a cumulative analysis with the full $(\ell=2, m=0)$ spherical harmonic using events from GWTC-4.0 and GWTC-5.0

    gr-qc 2026-07 conditional novelty 5.5 of 10

    Cumulative log10 Bayes factor of 1.38±0.79 favors the full (2,0) mode in GWTC-4.0; decisive evidence is projected to need ~166 events under optimistic assumptions.

  3. Revisiting GW150914 with a non-planar, eccentric waveform model

    gr-qc 2025-05 conditional novelty 5.0 of 10

    Using a waveform model that includes both eccentricity and spin precession, the authors confirm GW150914 was a quasi-circular, slowly spinning black hole merger, with eccentricity below 0.08 at 15 Hz.

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