Hannam, Mark and Husa, Sascha and Baker, John G. and Boyle, Michael and Brügmann, Bernd and Chu, Tony and Dorband, Nils and Herrmann, Frank and Hinder, Ian and Kelly, Bernard J. and Kidder, Lawrence E. and Laguna, Pablo and Matthews, Keith D. and van-Meter, James R. and Pfeiffer, Harald P. and Pollney, Denis and Reisswig, Christian and Scheel, Mark A. and Shoemaker, Dierdre (2009) Samurai project: Verifying the consistency of black-hole-binary waveforms for gravitational-wave detection. Physical Review D, 79 (8). 084025. ISSN 0556-2821. http://resolver.caltech.edu/CaltechAUTHORS:20090828-110556553
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We quantify the consistency of numerical-relativity black-hole-binary waveforms for use in gravitational-wave (GW) searches with current and planned ground-based detectors. We compare previously published results for the ([script-l]=2,|m|=2) mode of the gravitational waves from an equal-mass nonspinning binary, calculated by five numerical codes. We focus on the 1000M (about six orbits, or 12 GW cycles) before the peak of the GW amplitude and the subsequent ringdown. We find that the phase and amplitude agree within each code's uncertainty estimates. The mismatch between the ([script-l]=2,|m|=2) modes is better than 10^(-3) for binary masses above 60M_([sun]) with respect to the Enhanced LIGO detector noise curve, and for masses above 180M_([sun]) with respect to Advanced LIGO, Virgo, and Advanced Virgo. Between the waveforms with the best agreement, the mismatch is below 2×10^(-4). We find that the waveforms would be indistinguishable in all ground-based detectors (and for the masses we consider) if detected with a signal-to-noise ratio of less than [approximate]14, or less than [approximate]25 in the best cases.
|Additional Information:||©2009 The American Physical Society. Received 20 January 2009; published 17 April 2009. The authors thank Badri Krishnan for the Enhanced LIGO noise curve, as provided by Rana Adhikari on behalf of the LIGO Scientific Collaboration, and Giovanni Losurdo for providing the Advanced Virgo noise curve on behalf of the Virgo Collaboration; Ben Owen and Alberto Vecchio for helpful comments on the manuscript; and Doreen Mu¨ ller for alerting us to a mislabeling of Fig. 4. M. Hannam was supported by SFI Grant No. 07/RFP/ PHYF148, and thanks the Albert Einstein Institute in Potsdam for hospitality while some of this work was carried out. S. Husa has been supported in part by VESF and the European Gravitational Observatory (EGO), by DAAD Grant No. D/07/13385, and by Grant No. FPA- 2007-60220 from the Spanish Ministerio de Educacio´n y Ciencia. B. Kelly was supported by the NASA Postdoctoral Program at the Oak Ridge Associated Universities. F. Herrmann, I. Hinder, P. Laguna, and D. Shoemaker acknowledge the support of the Center for Gravitational Wave Physics at Penn State funded by the National Science Foundation under Cooperative Agreement No. PHY-0114375. P. Laguna and D. Shoemaker were also supported by NSF Grant No. PHY-0653443, No. PHY-065303, and No. PHY-0555436. F. Herrmann was also supported by NSF Grant No. PHY-0801213. J. Baker, M. Boyle, M. Hannam, F. Herrmann, S. Husa, L. Kidder, H. Pfeiffer, and M. Scheel thank the Kavli Institute for Theoretical Physics (KITP) Santa Barbara for hospitality during the workshop ‘‘Interplay between Numerical Relativity and Data Analysis,’’ where this work was initiated; the Kavli Institute is supported by NSF Grant No. PHY05-51164. BAM simulations were carried out at LRZ Munich. CCATIE simulations were supported by Teragrid Grant No. TG-MCA02N014. Hahndol simulations were carried out using Project Columbia at NASA Ames Research Center. Some of the SpEC simulations discussed here were produced with LIGO Laboratory computing facilities. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the National Science Foundation, and operates under Cooperative Agreement No. PHY-0107417. This work was supported in part by the DFG Grant No. SFB/Transregio 7 ‘‘GravitationalWave Astronomy’’; by grants from the Sherman Fairchild Foundation to Caltech and Cornell, and from the Brinson Foundation to Caltech; by NSF Grant No. PHY-0601459, No. PHY-0652995, No. DMS-0553302, and NASA Grant No. NNG05GG52G at Caltech; by NSF Grant No. PHY- 0652952, No. DMS-0553677, No. PHY-0652929, and NASA Grant No. NNG05GG51G at Cornell; and by NASA Grant No. O5-BEFS-05-0044 at Goddard. PACS numbers: 04.25.D, 04.20.Ex, 04.30.Db, 95.30.Sf|
|Subject Keywords:||PACS: 04.25.D-; 04.20.Ex; 04.30.Db; 95.30.Sf|
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|Deposited By:||Ruth Sustaita|
|Deposited On:||08 Sep 2009 22:36|
|Last Modified:||26 Dec 2012 11:16|
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