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IMRPhenomXHM: A multi-mode frequency-domain model for the gravitational wave signal from non-precessing black-hole binaries

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arxiv 2001.10914 v2 pith:F72H4EJ4 submitted 2020-01-29 gr-qc

Cecilio García-Quirós , Marta Colleoni , Sascha Husa , Héctor Estellés , Geraint Pratten , Antoni Ramos-Buades , Maite Mateu-Lucena , Rafel Jaume This is my paper · ORCID
classification gr-qc
keywords modelimrphenomxhmbinariesharmonicsinspiralnon-precessingnumericalwaveform
verification ladder T0 review T1 audit T2 compute T3 formal
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abstract

We present the IMRPhenomXHM frequency domain phenomenological waveform model for the inspiral, merger and ringdown of quasi-circular non-precessing black hole binaries. The model extends the IMRPhenomXAS waveform model, which describes the dominant quadrupole modes $\ell = |m| = 2$, to the harmonics $(\ell, |m|)=(2,1), (3,3), (3,2), (4,4)$, and includes mode mixing effects for the $(3,2)$ spherical harmonic. IMRPhenomXHM is calibrated against hybrid waveforms, which match an inspiral phase described by the effective-one-body model and post-Newtonian amplitudes for the subdominant harmonics to numerical relativity waveforms and numerical solutions to the perturbative Teukolsky equation for large mass ratios up to 1000. A computationally efficient implementation of the model is available as part of the LSC Algorithm Library Suite.

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