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Aligned-spin neutron-star–black-hole waveform model based on the effective-one-body approach and numerical-relativity simulations

Matas, Andrew and Dietrich, Tim and Buonanno, Alessandra and Hinderer, Tanja and Pürrer, Michael and Foucart, Francois and Boyle, Michael and Duez, Matthew D. and Kidder, Lawrence E. and Pfeiffer, Harald P. and Scheel, Mark A. (2020) Aligned-spin neutron-star–black-hole waveform model based on the effective-one-body approach and numerical-relativity simulations. Physical Review D, 102 (4). Art. No. 043023. ISSN 2470-0010.

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After the discovery of gravitational waves from binary black holes (BBHs) and binary neutron stars (BNSs) with the LIGO and Virgo detectors, neutron-star black holes (NSBHs) are the natural next class of binary systems to be observed. In this work, we develop a waveform model for aligned-spin NSBHs combining a BBH baseline waveform (available in the effective-one-body approach) with a phenomenological description of tidal effects (extracted from numerical-relativity simulations) and correcting the amplitude during the late inspiral, merger and ringdown to account for the NS tidal disruption. In particular, we calibrate the amplitude corrections using NSBH waveforms obtained with the numerical-relativity spectral Einstein code (SpEC) and the SACRA code. The model was calibrated using simulations with NS masses in the range 1.2–1.4  M⊙, tidal deformabilities up to 4200 (for a 1.2  M⊙ NS), and dimensionless BH spin magnitude up to 0.9. Based on the simulations used and on checking that sensible waveforms are produced, we recommend our model to be employed with a NS mass in the range 1–3  M⊙, tidal deformability 0–5000, and (dimensionless) BH spin magnitude up to 0.9. We also validate our model against two new, highly accurate NSBH waveforms with BH spin 0.9 and mass ratios 3 and 4, characterized by tidal disruption, produced with SpEC, and find very good agreement. Furthermore, we compute the unfaithfulness between waveforms from NSBH, BBH, and BNS systems, finding that it will be challenging for the Advanced LIGO-Virgo detector network at design sensitivity to distinguish different source classes. We perform a Bayesian parameter-estimation analysis on a synthetic numerical-relativity signal in zero noise to study parameter biases. Finally, we reanalyze GW170817, with the hypothesis that it is a NSBH. We do not find evidence to distinguish the BNS and NSBH hypotheses; however, the posterior for the mass ratio is shifted to less equal masses under the NSBH hypothesis.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Matas, Andrew0000-0001-6299-7414
Hinderer, Tanja0000-0002-3394-6105
Pürrer, Michael0000-0002-3329-9788
Foucart, Francois0000-0003-4617-4738
Duez, Matthew D.0000-0002-0050-1783
Kidder, Lawrence E.0000-0001-5392-7342
Pfeiffer, Harald P.0000-0001-9288-519X
Scheel, Mark A.0000-0001-6656-9134
Additional Information:© 2020 Published by the American Physical Society under the terms of the Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to the author(s) and the published article’s title, journal citation, and DOI. Open access publication funded by the Max Planck Society. Received 26 April 2020; accepted 6 August 2020; published 27 August 2020. We would like to thank Koutarou Kyutoku and Masaru Shibata for providing us with the numerical-relativity waveforms from the sacra code. We would like to thank Frank Ohme, Jonathan Thompson, Edward Fauchon-Jones, and Shrobana Ghosh for reviewing the LAL implementation of the SEOBNR_NSBH waveform model. We are grateful to Katerina Chatziioannou for comments on the manuscript and Luca Prudenzi for useful discussions. T. D. acknowledges support by the European Unions Horizon 2020 research and innovation program under Grant Agreement No. 749145, BNS mergers. T. H. acknowledges support from Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO) Projectruimte grant GW-EM NS and the DeltaITP and thanks the Yukawa International Seminar (YKIS) 2019 “Black Holes and Neutron Stars with Gravitational Waves.” F. F. gratefully acknowledges support from the U.S. National Science Foundation (NSF) through Grant No. PHY-1806278. M. D. gratefully acknowledges support from the NSF through Grant No. PHY-1806207. H. P. P. gratefully acknowledges support from the NSERC Canada. L. E. K. acknowledges support from NSF Grants No. PHY-1606654 and No. PHY-1912081. M. A. S. acknowledge support from NSF Grants PHY170212 and PHY-1708213. L. K. and M. S. also thank the Sherman Fairchild Foundation for their support. Computations for the review were done on the Hawk high-performance compute (HPC) cluster at Cardiff University, which is funded by STFC Grant No. ST/I006285/1. Other computations for this work were done on the HPC clusters Hypatia at the Max Planck Institute for Gravitational Physics in Potsdam, and at CIT at Caltech, funded by National Science Foundation Grants No. PHY-0757058 and No. PHY-0823459. We extensively used the numpy [110], scipy [111], and matplotlib [112] libraries. This research has made use of data, software and/or web tools obtained from the Gravitational Wave Open Science Center, a service of LIGO Laboratory, the LIGO Scientific Collaboration and the Virgo Collaboration. LIGO is funded by the U.S. National Science Foundation. Virgo is funded by the French Centre National de Recherche Scientifique (CNRS), the Italian Istituto Nazionale della Fisica Nucleare (INFN) and the Dutch Nikhef, with contributions by Polish and Hungarian institutes.
Group:TAPIR, Walter Burke Institute for Theoretical Physics
Funding AgencyGrant Number
European Research Council (ERC)749145
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)UNSPECIFIED
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Sherman Fairchild FoundationUNSPECIFIED
Science and Technology Facilities Council (STFC)ST/I006285/1
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Istituto Nazionale di Fisica Nucleare (INFN)UNSPECIFIED
Max Planck SocietyUNSPECIFIED
Issue or Number:4
Record Number:CaltechAUTHORS:20200828-123016604
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:105144
Deposited By: Tony Diaz
Deposited On:28 Aug 2020 21:32
Last Modified:28 Aug 2020 21:32

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