TY - JOUR

T1 - Phenomenological gravitational-wave model for precessing black-hole binaries with higher multipoles and asymmetries

AU - Thompson, Jonathan E.

AU - Hamilton, Eleanor

AU - London, Lionel

AU - Ghosh, Shrobana

AU - Kolitsidou, Panagiota

AU - Hoy, Charlie

AU - Hannam, Mark

N1 - Funding Information: J. T., S. G., P. K., C. H., and M. H. 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. J. T. also acknowledges support from the NASA LISA Preparatory Science grant 20-LPS20-0005. E. H. was supported in part by Swiss National Science Foundation (SNSF) Grant No. IZCOZ0-189876 and by the UZH Postdoc Grant (Forschungskredit). L. L. was supported at King’s College London by Royal Society University Research Grant No. URF\R1\211451; and at the University of Amsterdam by the GRavitation AstroParticle Physics Amsterdam (GRAPPA) Prize. S. G. was also supported 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. C. H. thanks the UKRI Future Leaders Fellowship for support through the Grant No. MR/T01881X/1. E. H. was also supported in part by the Universitat de les Illes Balears (UIB); the Spanish Agencia Estatal de Investigación Grants No. PID2022-138626NB-I00, PID2019–106416GB-I00, No. RED2022-134204-E, No. RED2022-134411-T, funded by MCIN/AEI/10.13039/501100011033; the MCIN with funding from the European Union NextGenerationEU/PRTR (PRTR-C17.I1); Comunitat Autonòma de les Illes Balears through the Direcció General de Recerca, Innovació I Transformació Digital with funds from the Tourist Stay Tax Law (PDR2020/11—ITS2017-006), the Conselleria d’Economia, Hisenda i Innovació Grants No. SINCO2022/18146 and No. SINCO2022/6719, cofinanced by the European Union and FEDER Operational Program 2021–2027 of the Balearic Islands; the “ERDF A way of making Europe.” The catalog of numerical simulations against which this model was calibrated 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 Oracle Cloud Infrastructure. The authors are additionally grateful for computational resources provided by the LIGO laboratory and supported by National Science Foundation Grants No. PHY-0757058 and No. PHY-0823459, which were used to perform the match comparisons presented in this paper. Most parameter estimation analyses were performed on the Sciama High Performance Compute (HPC) cluster, which is supported by the Institute of Cosmology and Gravitation (ICG), SEPNet and the University of Portsmouth. Additional parameter estimation and further analyses were performed on 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 part-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. This research has made use of data or software obtained from the Gravitational Wave Open Science Center (), a service of the LIGO Scientific Collaboration, the Virgo Collaboration, and KAGRA. This material is based upon work supported by NSF’s LIGO Laboratory which is a major facility fully funded by the National Science Foundation, as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. Virgo is funded, through the European Gravitational Observatory (EGO), by the French Centre National de Recherche Scientifique (CNRS), the Italian Istituto Nazionale di Fisica Nucleare (INFN) and the Dutch Nikhef, with contributions by institutions from Belgium, Germany, Greece, Hungary, Ireland, Japan, Monaco, Poland, Portugal, Spain. KAGRA is supported by Ministry of Education, Culture, Sports, Science and Technology (MEXT), Japan Society for the Promotion of Science (JSPS) in Japan; National Research Foundation (NRF) and Ministry of Science and ICT (MSIT) in Korea; Academia Sinica (AS) and National Science and Technology Council (NSTC) in Taiwan.

PY - 2024/3/11

Y1 - 2024/3/11

N2 - In this work we introduce phenomxo4a, the first phenomenological, frequency-domain gravitational waveform model to incorporate multipole asymmetries and precession angles tuned to numerical relativity. We build upon the modeling work that produced the phenompnr model and incorporate our additions into the imrphenomx framework, retuning the coprecessing frame model and extending the tuned precession angles to higher signal multipoles. We also include, for the first time in frequency-domain models, a recent model for spin-precession-induced multipolar asymmetry in the coprecessing frame to the dominant gravitational-wave multipoles. The accuracy of the full model and its constituent components is assessed through comparison to numerical relativity and numerical relativity surrogate waveforms by computing mismatches and performing parameter estimation studies. We show that, for the dominant signal multipole, we retain the modeling improvements seen in the phenompnr model. We find that the relative accuracy of current full IMR models varies depending on location in parameter space and the comparison metric, and on average they are of comparable accuracy. However, we find that variations in the pointwise accuracy do not necessarily translate into large biases in the parameter estimation recoveries.

AB - In this work we introduce phenomxo4a, the first phenomenological, frequency-domain gravitational waveform model to incorporate multipole asymmetries and precession angles tuned to numerical relativity. We build upon the modeling work that produced the phenompnr model and incorporate our additions into the imrphenomx framework, retuning the coprecessing frame model and extending the tuned precession angles to higher signal multipoles. We also include, for the first time in frequency-domain models, a recent model for spin-precession-induced multipolar asymmetry in the coprecessing frame to the dominant gravitational-wave multipoles. The accuracy of the full model and its constituent components is assessed through comparison to numerical relativity and numerical relativity surrogate waveforms by computing mismatches and performing parameter estimation studies. We show that, for the dominant signal multipole, we retain the modeling improvements seen in the phenompnr model. We find that the relative accuracy of current full IMR models varies depending on location in parameter space and the comparison metric, and on average they are of comparable accuracy. However, we find that variations in the pointwise accuracy do not necessarily translate into large biases in the parameter estimation recoveries.

UR - http://www.scopus.com/inward/record.url?scp=85187667150&partnerID=8YFLogxK

U2 - 10.1103/PhysRevD.109.063012

DO - 10.1103/PhysRevD.109.063012

M3 - Article

AN - SCOPUS:85187667150

VL - 109

JO - Physical Review D

JF - Physical Review D

SN - 2470-0010

IS - 6

M1 - 063012

ER -