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

London, Lionel, Khan, Sebastian, Fauchon-Jones, Edward, García, Cecilio, Hannam, Mark, Husa, Sascha, Jiménez-Forteza, Xisco, Kalaghatgi, Chinmay, Ohme, Frank and Pannarale, Francesco 2018. First higher-multipole model of gravitational waves from spinning and coalescing black-hole binaries. Physical Review Letters 120 (16) , 161102. 10.1103/PhysRevLett.120.161102

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Abstract

Gravitational-wave observations of binary black holes currently rely on theoretical models that predict the dominant multipoles ( ℓ = 2 , | m | = 2 ) 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 nonprecessing PhenomD model. The result, PhenomHM, constitutes the first higher-multipole model of spinning and coalescing 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.

Item Type:	Article
Date Type:	Publication
Status:	Published
Schools:	Advanced Research Computing @ Cardiff (ARCCA) Physics and Astronomy
Publisher:	American Physical Society
ISSN:	0031-9007
Date of First Compliant Deposit:	3 May 2018
Date of Acceptance:	19 April 2018
Last Modified:	20 Oct 2020 01:42
URI:	http://orca.cf.ac.uk/id/eprint/111171

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