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Error-analysis and comparison to analytical models of numerical waveforms produced by the NRAR Collaboration

Hinder, Ian and Reisswig, Christian and Scheel, Mark A. and Sperhake, Ulrich and Szilágyi, Bela and Zenginoğlu, Anıl and Buchman, Luisa T. and Chu, Tony and Haas, Roland and Hemberger, Daniel A. and Lovelace, Geoffrey and Mösta, Philipp and Taylor, Nicholas W. and Teukolsky, Saul A. (2014) Error-analysis and comparison to analytical models of numerical waveforms produced by the NRAR Collaboration. Classical and Quantum Gravity, 31 (2). Art. No. 025012. ISSN 0264-9381. https://resolver.caltech.edu/CaltechAUTHORS:20140224-082418165

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Abstract

The Numerical–Relativity–Analytical–Relativity (NRAR) collaboration is a joint effort between members of the numerical relativity, analytical relativity and gravitational-wave data analysis communities. The goal of the NRAR collaboration is to produce numerical-relativity simulations of compact binaries and use them to develop accurate analytical templates for the LIGO/Virgo Collaboration to use in detecting gravitational-wave signals and extracting astrophysical information from them. We describe the results of the first stage of the NRAR project, which focused on producing an initial set of numerical waveforms from binary black holes with moderate mass ratios and spins, as well as one non-spinning binary configuration which has a mass ratio of 10. All of the numerical waveforms are analysed in a uniform and consistent manner, with numerical errors evaluated using an analysis code created by members of the NRAR collaboration. We compare previously-calibrated, non-precessing analytical waveforms, notably the effective-one-body (EOB) and phenomenological template families, to the newly-produced numerical waveforms. We find that when the binary's total mass is ~100–200M_⊙, current EOB and phenomenological models of spinning, non-precessing binary waveforms have overlaps above 99% (for advanced LIGO) with all of the non-precessing-binary numerical waveforms with mass ratios ≤4, when maximizing over binary parameters. This implies that the loss of event rate due to modelling error is below 3%. Moreover, the non-spinning EOB waveforms previously calibrated to five non-spinning waveforms with mass ratio smaller than 6 have overlaps above 99.7% with the numerical waveform with a mass ratio of 10, without even maximizing on the binary parameters.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0264-9381/31/2/025012DOIArticle
http://iopscience.iop.org/0264-9381/31/2/025012/PublisherArticle
http://arxiv.org/abs/1307.5307arXivDiscussion Paper
ORCID:
AuthorORCID
Sperhake, Ulrich0000-0002-3134-7088
Additional Information:© 2014 Institute of Physics Publishing Ltd. Received 23 July 2013, revised 29 October 2013. Published 5 December 2013. We thank Beverly Berger and Kip Thorne for helping to establish the NRAR collaboration, Duncan Brown and Frans Pretorius for their work as members of the NRAR executive committee, Duncan Brown, Evan Ochsner and B Sathyaprakash for useful discussions in the first stage of the NRAR collaboration when the scientific plan and accuracy requirements were established. We also thank John Baker, Peter Diener, Bernard Kelly and Riccardo Sturani for useful interactions. It is also a pleasure to thank David Hilditch for useful discussions on the hyperbolicity of BSSN, Roman Gold for useful discussions on requirements for accurate computation of gravitational waves and P Ajith for help with performing and interpreting the IMRPhenom comparisons. We also thank Bruce Loftis and Christal Yost at the National Institute for Computational Sciences (NICS) for their support. Caltech acknowledges support from the Sherman Fairchild Foundation and NSF grants PHY-1068881, PHY-1005655, and DMS-1065438. M Hannam was supported by Science and Technology Facilities Council grants ST/H008438/1 and ST/I001085/1. CITA acknowledges support from NSERC of Canada, the Canada Chairs Program, and the Canadian Institute for Advanced Research. Cornell acknowledges support from the Sherman Fairchild Foundation and NSF grants PHY-0969111 and PHY-1005426. FAU acknowledges financial support via the NSF grants 0855315 and 1204334. GA Tech acknowledges financial support via NSF grants 1205864, 1212433, 0903973, 0941417, and 0955825. Jena and the AEI acknowledge financial support via the DFG SFB/Transregio 7. US acknowledges financial support via the Ramόn y Cajal Programme of the Ministry of Education and Science in Spain, the FP7-PEOPLE-2011-CIG grant 293412 CBHEO, the STFC GR Roller grant ST/I002006/1, the ERC Starting grant ERC-2010-StG DyBHo, and the FP7-PEOPLE-2011-IRSES grant 295189 NRHEP. A Nerozzi acknowledges support by the Fundação para a Ciência e Tecnologia through grants SFRH/BPD/47955/2008 and PTDC/FIS/116625/2010. HW acknowledges support by the ERC-2011-StG 279363–HiDGR ERC Starting Grant and by the DyBHo–256667 ERC Starting Grant. HW acknowledges support by FCT–Portugal through grant nos. SFRH/BD/46061/2008 and CERN/FP/123593/2011 at early stages of this work. CR acknowledges financial support from NASA via the Einstein Postdoctoral Fellowship grant PF2-130099 awarded by the Chandra X-ray center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. RIT acknowledges financial support via NSF grants AST-1028087, PHY-0929114, PHY-0969855, PHY-0903782, OCI-0832606, and DRL-1136221, and NASA grant 07-ATFP07-0158. HN would also like to acknowledge support by the grand-in-aid for (24103006). UIUC acknowledges financial support via NSF grants PHY-0963136, AST-1002667, and NASA grants NNX11AE11G, NNX13AH44G. VP would also like to acknowledge financial support from a Fortner Research Fellowship. UMD acknowledges financial support via NSF grants PHY-0903631 and PHY-1208881, and NASA grants NNX09AI81G and NNX12AN10G. We also acknowledge the hospitality of the Kavli Institute for Theoretical Physics during the program ‘Chirps, Mergers and Explosions’ (supported by the NSF grant PHY11-25915). Computing time for this project was provided by the NSF on the TeraGrid (now XSEDE) systems Athena and Kraken at NICS. AEI used computational resources on the Datura cluster at AEI. Caltech and Cornell used additional computational resources on the Zwicky cluster at Caltech, which is supported by the Sherman Fairchild Foundation and by NSF award PHY-0960291, and on the NSF XSEDE network under grant TG-PHY990007N. CITA used additional computational resources at the SciNet HPC Consortium on the GPC system. FAU used additional computational resources via TeraGrid allocations TG-AST100021 and TGPHY100051 at NICS on the Kraken system. GA Tech used additional computational resources via XSEDE allocation TG-PHY120016, and at Georgia Tech on the Cygnus cluster. JCP used additional computational resources at the LRZ, Munich, and as part of the European PRACE petascale computing initiative on the clusters Hermit, Curie and SuperMUC; simulations were were also carried out at Advanced Research Computing (ARCCA) at Cardiff. US, AN and HW used additional computational resources via XSEDE allocation PHY-090003 at SDCS on the Trestles system and at NICS on the Kraken system, via the Barcelona Supercomputing Center (BSC) allocation AECT-2012-3-0011, via the Centro de Supercomputaciόn de Galicia (CESGA) allocation ICTS-2011-234, the Baltasar-Sete-Sόis cluster at CENTRA/IST Lisbon, the CANE cluster in Poland through PRACE DECI-7 and at the DiRAC HPC Facility on the COSMOS supercomputer supported by STFC and BIS. RIT used additional computational resources at TACC on the Ranger system via XSEDE allocation TG-PHY060027N, and at RIT on the NewHorizons/BlueSky system supported by NSF grants PHY-0722703, DMS-0820923, AST-1028087 and PHY-1229173. UIUC used additional computational resources at TACC on the Stampede system via XSEDE allocation TG-MCA99S008. Hosting for the NRAR data set and collaboration tools was provided by the Syracuse University Gravitational wave Group, supported by NSF awards PHY-0847611, PHY-1040231 and PHY-1104371. The EOBNRv2, SEOBNRv1, IMRPhenomB and IMRPhenomC templates were produced using the public LIGO Algorithm Library [233], while the IHES-EOB templates were produced using the public code in [234].
Funders:
Funding AgencyGrant Number
National Institute for Computational Sciences (NCIS)UNSPECIFIED
Sherman Fairchild FoundationUNSPECIFIED
NSFPHY-1068881
NSFPHY-1005655
NSFDMS-1065438
Science and Technology Facilities Council (STFC)ST/H008438/1
Science and Technology Facilities Council (STFC)ST/I001085/1
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Canada Chairs ProgramUNSPECIFIED
Canadian Institute for Advanced Research (CIAR)UNSPECIFIED
NSFPHY-0969111
NSFPHY-1005426
NSF0855315
NSF1204334
NSF1205864
NSF1212433
NSF0903973
NSF0941417
NSF0955825
Deutsche Forschungsgemeinschaft (DFG)SFB/Transregio 7
Ramόn y Cajal ProgrammeUNSPECIFIED
FP7-PEOPLE-2011-CIGCBHEO-293412
Science and Technology Facilities Council (STFC)ST/I002006/1
European Research Council (ERC)ERC-2010-StGDyBHo
FP7-PEOPLE-2011-IRSES295189 NRHEP
Fundação para a Ciência e Tecnologia (FCT)SFRH/BPD/47955/2008
Fundação para a Ciência e Tecnologia (FCT)PTDC/FIS/116625/2010
European Research Council (ERC)ERC-2011-StG 279363–HiDGR
European Research Council (ERC)DyBHo-256667
Fundação para a Ciência e Tecnologia (FCT)SFRH/BD/46061/2008
Fundação para a Ciência e Tecnologia (FCT)CERN/FP/123593/2011
NASA Einstein Postdoctoral FellowshipPF2-130099
NASANAS8-03060
NSFAST-1028087
NSFPHY-0929114
NSFPHY-0969855
NSFPHY-0903782
NSFOCI-0832606
NSFDRL-1136221
NASA07-ATFP07-0158
Ministry of Education, Culture, Sports, Science and Technology (MEXT)24103006
NSFPHY-0963136
NSFAST-1002667
NASANNX11AE11G
NASANNX13AH44G
Fortner Research FellowshipUNSPECIFIED
NSFPHY-0903631
NSFPHY-1208881
NASANNX09AI81G
NASANNX12AN10G
NSFPHY11-25915
NSFPHY-0960291
NSFPHY-990007N
NSFAST-100021
TeraGridPHY-100051
NSFTG-PHY120016
NSFPHY-090003
Barcelona Supercomputing Center (BSC)AECT-2012-3-0011
Centro de Supercomputaciόn de Galicia (CESGA)ICTS-2011-234
NSFPHY-060027N
NSFPHY-0722703
NSFDMS-0820923
NSFAST-1028087
NSFPHY-1229173
NSFMCA-99S008
NSFPHY-0847611
NSFPHY-1040231
NSFPHY-1104371
Issue or Number:2
Classification Code:PACS: 04.25.D-; 97.60.Lf; 07.60.Ly; 95.55.Ym; 04.70.-s; 04.80.Nn. MSC: 83C35; 83C57
Record Number:CaltechAUTHORS:20140224-082418165
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20140224-082418165
Official Citation:Error-analysis and comparison to analytical models of numerical waveforms produced by the NRAR Collaboration Ian Hinder et al 2013 Class. Quantum Grav. 31 025012
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:43937
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:24 Feb 2014 18:09
Last Modified:03 Oct 2019 06:12

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