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  First higher-multipole model of spinning binary-black-hole gravitational waveforms

London, L., Khan, S., Fauchon-Jones, E., Forteza, X. J., Hannam, M., Husa, S., et al. (2018). First higher-multipole model of spinning binary-black-hole gravitational waveforms. Physical Review Letters, 120: 161102. doi:10.1103/PhysRevLett.120.161102.

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Item Permalink: http://hdl.handle.net/11858/00-001M-0000-002D-DBB5-B Version Permalink: http://hdl.handle.net/21.11116/0000-0002-F6A4-F
Genre: Journal Article

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 Creators:
London, Lionel, Author
Khan, Sebastian1, Author              
Fauchon-Jones, Edward, Author
Forteza, Xisco Jiménez, Author
Hannam, Mark, Author
Husa, Sascha, Author
Kalaghatgi, Chinmay, Author
Ohme, Frank2, Author              
Pannarale, Francesco, Author
Affiliations:
1Binary Merger Observations and Numerical Relativity, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, ou_2461691              
2Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_24013              

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Free keywords: General Relativity and Quantum Cosmology, gr-qc
 Abstract: Gravitational-wave observations of binary black holes currently rely on theoretical models that predict the dominant multipole radiation during the coalescence. Here we introduce a simple method to include the subdominant multipole contributions to binary black hole gravitational waveforms, given a frequency-domain model for the dominant $(\ell=2,|m|=2)$ multipoles. The amplitude and phase of the original model are appropriately stretched and rescaled using leading-order 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 $(\ell,|m|) = (2,2), (3,3), (4,4), (2,1), (3,2), (4,3)$. Comparisons with a set of numerical-relativity waveforms demonstrate that PhenomHM is more accurate than PhenomD for all binary configurations, and using PhenomHM typically leads to improved measurements of the binary's properties. Our approach can be extended to precessing systems, enabling wide-ranging studies of the impact of higher harmonics on gravitational-wave astronomy, and tests of fundamental physics.

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 Dates: 2017-08-012017-08-032018
 Publication Status: Published in print
 Pages: 5 pages, 4 figures
 Publishing info: -
 Table of Contents: -
 Rev. Method: -
 Identifiers: arXiv: 1708.00404
URI: http://arxiv.org/abs/1708.00404
DOI: 10.1103/PhysRevLett.120.161102
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Title: Physical Review Letters
  Abbreviation : Phys. Rev. Lett.
Source Genre: Journal
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Publ. Info: Woodbury, N.Y. : American Physical Society
Pages: - Volume / Issue: 120 Sequence Number: 161102 Start / End Page: - Identifier: ISSN: 0031-9007
CoNE: /journals/resource/954925433406_1