Phenomenological model for the gravitational-wave signal from precessing binary black holes with two-spin effects

Khan, Sebastian ORCID: https://orcid.org/0000-0003-4953-5754, Chatziioannou, Katerina, Hannam, Mark ORCID: https://orcid.org/0000-0001-5571-325X and Ohme, Frank 2019. Phenomenological model for the gravitational-wave signal from precessing binary black holes with two-spin effects. Physical Review D 100 (2) , 024059. 10.1103/PhysRevD.100.024059

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Abstract

The properties of compact binaries, such as masses and spins, are imprinted in the gravitational waves (GWs) they emit and can be measured using parametrized waveform models. Accurately and efficiently describing the complicated precessional dynamics of the various angular momenta of the system in these waveform models is the object of active investigation. One of the key models extensively used in the analysis of LIGO and Virgo data is the single-precessing-spin waveform model IMRPhenomPv2. In this article we present a new model IMRPhenomPv3, which includes the effects of two independent spins in the precession dynamics. Whereas IMRPhenomPv2 utilizes a single-spin frequency-dependent post-Newtonian rotation to describe precession effects, the improved model, IMRPhenomPv3, employs a double-spin rotation that is based on recent developments in the description of precessional dynamics. Besides double-spin precession, the improved model benefits from a more accurate description of precessional effects. We validate our new model against a large set of precessing numerical-relativity simulations. We find that IMRPhenomPv3 has better agreement with the inspiral portion of precessing binary-black-hole simulations and is more robust across a larger region of the parameter space than IMRPhenomPv2. As a first application we analyze the gravitational-wave event GW151226 with an efficient frequency-domain waveform model that describes two-spin precession. Within statistical uncertainty our results are consistent with published results. IMRPhenomPv3 will allow studies of the measurability of individual spins of binary black holes using GWs and can be used as a foundation upon which to build further improvements, such as modeling precession through merger, extending to higher multipoles, and including tidal effects.

Item Type:	Article
Date Type:	Publication
Status:	Published
Schools:	Physics and Astronomy
Publisher:	American Physical Society
ISSN:	2470-0010
Date of First Compliant Deposit:	30 January 2020
Date of Acceptance:	29 July 2019
Last Modified:	07 May 2023 12:58
URI:	https://orca.cardiff.ac.uk/id/eprint/129179

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