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  Including higher order multipoles in gravitational-wave models for precessing binary black holes

Khan, S., Ohme, F., Chatziioannou, K., & Hannam, M. (2020). Including higher order multipoles in gravitational-wave models for precessing binary black holes. Phyisical Review D, 101(2): 024056. doi:10.1103/PhysRevD.101.024056.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0005-4D34-B Version Permalink: http://hdl.handle.net/21.11116/0000-0005-C16D-7
Genre: Journal Article

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 Creators:
Khan, Sebastian1, Author              
Ohme, Frank1, Author              
Chatziioannou , Katerina, Author
Hannam , Mark, Author
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1Binary Merger Observations and Numerical Relativity, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, ou_2461691              

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Free keywords: General Relativity and Quantum Cosmology, gr-qc, Astrophysics, Solar and Stellar Astrophysics, astro-ph.SR
 Abstract: Estimates of the source parameters of gravitational-wave (GW) events produced by compact binary mergers rely on theoretical models for the GW signal. We present the first frequency-domain model for inspiral, merger and ringdown of the GW signal from precessing binary-black-hole systems that also includes multipoles beyond the leading-order quadrupole. Our model, {\tt PhenomPv3HM}, is a combination of the higher-multipole non-precessing model {\tt PhenomHM} and the spin-precessing model {\tt PhenomPv3} that includes two-spin precession via a dynamical rotation of the GW multipoles. We validate the new model by comparing to a large set of precessing numerical-relativity simulations and find excellent agreement across the majority of the parameter space they cover. For mass ratios $<5$ the mismatch improves, on average, from $\sim6\%$ to $\sim 2\%$ compared to {\tt PhenomPv3} when we include higher multipoles in the model. However, we find mismatches $\sim8\%$ for the mass-ratio $6$ and highly spinning simulation. As a first application of the new model we have analysed the binary black hole event GW170729. We find larger values for the primary black hole mass of $58.25^{+11.73}_{-12.53} \, M_\odot$ (90\% credible interval). The lower limit ($\sim 46 \, M_\odot$) is comparable to the proposed maximum black hole mass predicted by different stellar evolution models due to the pulsation pair-instability supernova (PPISN) mechanism. If we assume that the primary \ac{BH} in GW170729 formed through a PPISN then out of the four PPISN models we considered only the model of Woosley (2017) is consistent with our mass measurements at the 90\% level.

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 Dates: 2019-11-142020
 Publication Status: Published in print
 Pages: 13 pages, 8 figures
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 Rev. Method: -
 Identifiers: arXiv: 1911.06050
URI: http://arxiv.org/abs/1911.06050
DOI: 10.1103/PhysRevD.101.024056
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Title: Phyisical Review D
Source Genre: Journal
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Pages: - Volume / Issue: 101 (2) Sequence Number: 024056 Start / End Page: - Identifier: -