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Matching post-Newtonian and numerical relativity waveforms: Systematic errors and a new phenomenological model for nonprecessing black hole binaries

Santamaría, L. and Ohme, F. and Ajith, P. and Brügmann, B. and Dorband, N. and Hannam, M. and Husa, S. and Mösta, P. and Pollney, D. and Reisswig, C. and Robinson, E. L. and Seiler, J. and Krishnan, B. (2010) Matching post-Newtonian and numerical relativity waveforms: Systematic errors and a new phenomenological model for nonprecessing black hole binaries. Physical Review D, 82 (6). Art. No. 064016. ISSN 0556-2821. http://resolver.caltech.edu/CaltechAUTHORS:20101004-085415232

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Abstract

We present a new phenomenological gravitational waveform model for the inspiral and coalescence of nonprecessing spinning black hole binaries. Our approach is based on a frequency-domain matching of post-Newtonian inspiral waveforms with numerical relativity based binary black hole coalescence waveforms. We quantify the various possible sources of systematic errors that arise in matching post-Newtonian and numerical relativity waveforms, and we use a matching criteria based on minimizing these errors; we find that the dominant source of errors are those in the post-Newtonian waveforms near the merger. An analytical formula for the dominant mode of the gravitational radiation of nonprecessing black hole binaries is presented that captures the phenomenology of the hybrid waveforms. Its implementation in the current searches for gravitational waves should allow cross-checks of other inspiral-merger-ringdown waveform families and improve the reach of gravitational-wave searches.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1103/PhysRevD.82.064016 DOIUNSPECIFIED
http://prd.aps.org/abstract/PRD/v82/i6/e064016PublisherUNSPECIFIED
Additional Information:© 2010 The American Physical Society. Received 4 June 2010; published 13 September 2010. We thank Doreen Müller for carrying out some of the BAH simulations, and Stas Babak, Vitor Cardoso, Steve Fairhurst, Ian Hinder, Doreen Müller, Dirk Putzfeld, Bangalore Sathyaprakash and Bernard Schutz for useful comments and discussions. L. S. has been partially supported by DAAD Grant No. A/06/12630. M.H. was supported by FWF Lise-Meitner Project No. M1178-N16 at the University of Vienna. S. H. was supported by DAAD Grant No. D/07/13385 and Grant No. FPA-2007-60220 from the Spanish Ministry of Science. D. P. has been supported by Grant No. CSD-2007-00042 of the Spanish Ministry of Science. D. P. and C. R. received support from the Bundesministerium für Bildung und Forschung, Germany. BAH simulations were performed at computer centers LRZ Munich, ICHEC Dublin, VSC Vienna, CESGA Santiago the Compostela and at MareNostrum at Barcelona Supercomputing Center—Centro Nacional de Supercomputación (Spanish National Supercomputing Center). This work was supported in part by the DFG Grant No. SFB/Transregio 7 "Gravitational-wave astronomy" and by the DLR (Deutsches Zentrum für Luft- und Raumfahrttechnik).
Group:TAPIR
Funders:
Funding AgencyGrant Number
Deutscher Akademischer Austausch Dienst (DAAD)A/06/12630
FWF Lise-Meitner at the University of Vienna M1178-N16
Spanish Ministry of Science D/07/13385
Spanish Ministry of Science FPA-2007-60220
Spanish Ministry of Science CSD-2007-00042
Bundesministerium fur Bildung und Forschung, Germany UNSPECIFIED
Classification Code:PACS: 04.30.Db, 04.25.dc, 04.25.Nx, 04.80.Nn
Record Number:CaltechAUTHORS:20101004-085415232
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20101004-085415232
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:20267
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:05 Oct 2010 16:45
Last Modified:26 Dec 2012 12:29

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