TY - JOUR

T1 - First frequency-domain phenomenological model of the multipole asymmetry in gravitational-wave signals from binary-black-hole coalescence

AU - Ghosh, Shrobana

AU - Kolitsidou, Panagiota

AU - Hannam, Mark

N1 - Funding Information: The authors were supported in part by Science and Technology Facilities Council (STFC) Grant No. ST/V00154X/1 and European Research Council (ERC) Consolidator Grant No. 647839. S. G. acknowledges support from the Max Planck Society’s Independent Research Group program. P. K. was also supported by the GW consolidated grant: STFC Grant No. ST/V005677/1. Simulations used in this work were performed on the DiRAC@Durham facility, managed by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility (). The equipment was funded by BEIS capital funding via STFC capital Grants No. ST/P002293/1 and No. ST/R002371/1, Durham University and STFC operations Grant No. ST/R000832/1. In addition, several of the simulations used in this work were performed as part of an allocation graciously provided by Oracle to explore the use of our code on the o racle Cloud Infrastructure. This research also used the supercomputing facilities at Cardiff University operated by Advanced Research Computing at Cardiff (ARCCA) on behalf of the Cardiff Supercomputing Facility and the HPC Wales and Supercomputing Wales (SCW) projects. We acknowledge the support of the latter, which is partly funded by the European Regional Development Fund (ERDF) via the Welsh Government. In part the computational resources at Cardiff University were also supported by STFC Grant No. ST/I006285/1. Various plots and analyses in this paper were made using p ython software packages lals uite , p y cbc , gwsurrogate , m atplotlib , n um p y , and lmfit and s ci p y .

PY - 2024/1/30

Y1 - 2024/1/30

N2 - Gravitational-wave signals from binaries that contain spinning black holes in general include an asymmetry between the +m and -m multipoles that is not included in most signal models used in LIGO-Virgo-KAGRA analysis to date. This asymmetry manifests itself in out-of-plane recoil of the final black hole and its inclusion in signal models is necessary both to measure this recoil, but also to accurately measure the full spin information of each black hole. We present the first model of the antisymmetric contribution to the dominant coprecessing-frame signal multipole throughout inspiral, merger, and ringdown. We model the antisymmetric contribution in the frequency domain, and take advantage of the approximations that the antisymmetric amplitude can be modeled as a ratio of the (already modeled) symmetric amplitude, and analytic relationships between the symmetric and antisymmetric phases during the inspiral and ringdown. The model is tuned to single-spin numerical-relativity simulations up to mass-ratio 8 and spin magnitudes of 0.8, and has been implemented in a recent phenomenological model for use in the fourth LIGO-Virgo-KAGRA observing run. However, the procedure described here can be easily applied to other time- or frequency-domain models.

AB - Gravitational-wave signals from binaries that contain spinning black holes in general include an asymmetry between the +m and -m multipoles that is not included in most signal models used in LIGO-Virgo-KAGRA analysis to date. This asymmetry manifests itself in out-of-plane recoil of the final black hole and its inclusion in signal models is necessary both to measure this recoil, but also to accurately measure the full spin information of each black hole. We present the first model of the antisymmetric contribution to the dominant coprecessing-frame signal multipole throughout inspiral, merger, and ringdown. We model the antisymmetric contribution in the frequency domain, and take advantage of the approximations that the antisymmetric amplitude can be modeled as a ratio of the (already modeled) symmetric amplitude, and analytic relationships between the symmetric and antisymmetric phases during the inspiral and ringdown. The model is tuned to single-spin numerical-relativity simulations up to mass-ratio 8 and spin magnitudes of 0.8, and has been implemented in a recent phenomenological model for use in the fourth LIGO-Virgo-KAGRA observing run. However, the procedure described here can be easily applied to other time- or frequency-domain models.

UR - http://www.scopus.com/inward/record.url?scp=85183943039&partnerID=8YFLogxK

U2 - 10.48550/arXiv.2310.16980

DO - 10.48550/arXiv.2310.16980

M3 - Article

AN - SCOPUS:85183943039

VL - 109

JO - Physical Review D

JF - Physical Review D

SN - 2470-0010

IS - 2

M1 - 024061

ER -