CaltechAUTHORS
  A Caltech Library Service

High-accuracy waveforms for black hole-neutron star systems with spinning black holes

Foucart, Francois and Chernoglazov, Alexander and Boyle, Michael and Hinderer, Tanja and Miller, Max and Moxon, Jordan and Scheel, Mark A. and Deppe, Nils and Duez, Matthew D. and Hébert, François and Kidder, Lawrence E. and Throwe, William and Pfeiffer, Harald P. (2021) High-accuracy waveforms for black hole-neutron star systems with spinning black holes. Physical Review D, 103 (6). Art. No. 064007. ISSN 2470-0010. https://resolver.caltech.edu/CaltechAUTHORS:20210305-080828408

[img] PDF - Published Version
See Usage Policy.

5Mb
[img] PDF - Submitted Version
See Usage Policy.

4Mb

Use this Persistent URL to link to this item: https://resolver.caltech.edu/CaltechAUTHORS:20210305-080828408

Abstract

The availability of accurate numerical waveforms is an important requirement for the creation and calibration of reliable waveform models for gravitational wave astrophysics. For black hole-neutron star binaries (BHNS), very few accurate waveforms are however publicly available. Most recent models are calibrated to a large number of older simulations with good parameter space coverage for low-spin nonprecessing binaries but limited accuracy, and a much smaller number of longer, more recent simulations limited to nonspinning black holes. In this paper, we present long, accurate numerical waveforms for three new systems that include rapidly spinning black holes, and one precessing configuration. We study in detail the accuracy of the simulations, and in particular perform for the first time in the context of BHNS binaries a detailed comparison of waveform extrapolation methods to the results of Cauchy characteristic extraction. The new waveforms have <0.1  rad phase errors during inspiral, rising to ∼(0.2–0.4)  rad errors at merger, and ≲1% error in their amplitude. We compute the faithfulness of recent analytical models to these numerical results for the late inspiral and merger phases covered by the numerical simulations, and find that models specifically designed for BHNS binaries perform well (faithfulness F > 0.99) for binaries seen face on. For edge-on observations, particularly for precessing systems, disagreements between models and simulations increase, and models that include precession and/or higher-order modes start to perform better than BHNS models that currently lack these features.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1103/physrevd.103.064007DOIArticle
https://arxiv.org/abs/2010.14518arXivDiscussion Paper
ORCID:
AuthorORCID
Foucart, Francois0000-0003-4617-4738
Boyle, Michael0000-0002-5075-5116
Hinderer, Tanja0000-0002-3394-6105
Moxon, Jordan0000-0001-9891-8677
Scheel, Mark A.0000-0001-6656-9134
Deppe, Nils0000-0003-4557-4115
Duez, Matthew D.0000-0002-0050-1783
Kidder, Lawrence E.0000-0001-5392-7342
Throwe, William0000-0001-5059-4378
Pfeiffer, Harald P.0000-0001-9288-519X
Additional Information:© 2021 American Physical Society. Received 29 October 2020; accepted 27 January 2021; published 4 March 2021. The authors thank Geert Raaijmakers and Andrew Matas for their help with the use of pyCBC. UNH authors gratefully acknowledges support from the NSF through Grant No. PHY-1806278, from the DOE through Grant No. DE-SC0020435, and from NASA through Grant No. 80NSSC18K0565. M. D. gratefully acknowledges support from the NSF through Grant No. PHY-1806207. H. P. gratefully acknowledges support from the NSERC Canada. L. K. acknowledges support from NSF Grants No. PHY-1912081 and No. OAC-1931280. F. H. and M. S. acknowledge support from NSF Grants No. PHY-170212 and No. PHY-1708213. F. H., L. K., N. D. and M. S. also thank the Sherman Fairchild Foundation for their support. T. H. acknowledges support from the Delta Institute for Theoretical Physics (DeltaITP) and NWO Projectruimte grant GW-EM NS, and from the NWO sectorplan. This research is part of the Frontera computing project at the Texas Advanced Computing Center. Frontera is made possible by National Science Foundation award OAC-1818253. This work used the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation Grant No. ACI-1548562. Simulations were performed on the Bridges cluster at the Pittsburgh Supercomputing Center and on the comet cluster at the San Diego Supercomputing Center, though XSEDE award TG-PHY990007N. Computations were also performed on the Wheeler clusters at Caltech, supported by the Sherman Fairchild Foundation and by Caltech.
Group:TAPIR, Walter Burke Institute for Theoretical Physics
Funders:
Funding AgencyGrant Number
NSFPHY-1806278
Department of Energy (DOE)DE-SC0020435
NASA80NSSC18K0565
NSFPHY-1806207
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
NSFPHY-1912081
NSFOAC-1931280
NSFPHY-170212
NSFPHY-1708213
Sherman Fairchild FoundationUNSPECIFIED
Delta Institute for Theoretical PhysicsUNSPECIFIED
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)GW-EM NS
NSFOAC-1818253
NSFACI-1548562
NSFTG-PHY990007N
Issue or Number:6
Record Number:CaltechAUTHORS:20210305-080828408
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20210305-080828408
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:108324
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:08 Mar 2021 20:39
Last Modified:08 Mar 2021 20:39

Repository Staff Only: item control page