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arxiv: 1708.00404 · v4 · submitted 2017-08-01 · 🌀 gr-qc

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First higher-multipole model of gravitational waves from spinning and coalescing black-hole binaries

Lionel London , Sebastian Khan , Edward Fauchon-Jones , Cecilio Garc\'ia , Mark Hannam , Sascha Husa , Xisco Jim\'enez Forteza , Chinmay Kalaghatgi
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Frank Ohme Francesco Pannarale
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classification 🌀 gr-qc
keywords modelbinarymultipolesbinariesblackblack-holecurrentlydominant
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Gravitational-wave observations of binary black holes currently rely on theoretical models that predict the dominant multipoles (l,m) of the radiation during inspiral, merger and ringdown. We introduce a simple method to include the subdominant multipoles to binary black hole gravitational waveforms, given a frequency-domain model for the dominant multipoles. The amplitude and phase of the original model are appropriately stretched and rescaled using post-Newtonian results (for the inspiral), perturbation theory (for the ringdown), and a smooth transition between the two. No additional tuning to numerical-relativity simulations is required. We apply a variant of this method to the non-precessing PhenomD model. The result, PhenomHM, constitutes the first higher-multipole model of spinning black-hole binaries, and currently includes the (l,m) = (2,2), (3,3), (4,4), (2,1), (3,2), (4,3) radiative moments. Comparisons with numerical-relativity waveforms demonstrate that PhenomHM is more accurate than dominant-multipole-only models for all binary configurations, and typically improves the measurement of binary properties.

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