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  The Samurai Project: verifying the consistency of black-hole-binary waveforms for gravitational-wave detection

Hannam, M., Husa, S., Baker, J. G., Boyle, M., Bruegmann, B., Chu, T., et al. (2009). The Samurai Project: verifying the consistency of black-hole-binary waveforms for gravitational-wave detection. Physical Review D., 79: 084025. doi:10.1103/PhysRevD.79.084025.

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Item Permalink: http://hdl.handle.net/11858/00-001M-0000-0012-BC73-4 Version Permalink: http://hdl.handle.net/11858/00-001M-0000-0012-BC75-F
Genre: Journal Article

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0901.2437 (Preprint), 527KB
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 Creators:
Hannam, Mark, Author
Husa, Sascha1, Author              
Baker, John G., Author
Boyle, Michael, Author
Bruegmann, Bernd, Author
Chu, Tony, Author
Dorband, Nils1, Author              
Herrmann, Frank, Author
Hinder, Ian1, Author              
Kelly, Bernard J., Author
Kidder, Lawrence E., Author
Laguna, Pablo, Author
Matthews, Keith D., Author
van Meter, James R., Author
Pfeiffer, Harald P., Author
Pollney, Denis1, Author              
Reisswig, Christian1, Author              
Scheel, Mark A., Author
Shoemaker, Deirdre, Author
Affiliations:
1Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, escidoc:24013              

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Free keywords: General Relativity and Quantum Cosmology, gr-qc
 Abstract: 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 $(\ell=2,| m | =2)$ 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 $(\ell=2,| m| =2)$ modes is better than $10^{-3}$ for binary masses above $60 M_{\odot}$ with respect to the Enhanced LIGO detector noise curve, and for masses above $180 M_{\odot}$ with respect to Advanced LIGO, Virgo and Advanced Virgo. Between the waveforms with the best agreement, the mismatch is below $2 \times 10^{-4}$. 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 $\approx14$, or less than $\approx25$ in the best cases.

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 Dates: 2009-01-162009-03-272009
 Publication Status: Published in print
 Pages: 17 pages, 9 figures. Version accepted by PRD
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 Rev. Method: -
 Identifiers: arXiv: 0901.2437
DOI: 10.1103/PhysRevD.79.084025
URI: http://arxiv.org/abs/0901.2437
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Title: Physical Review D.
  Alternative Title : Phys. Rev. D.
Source Genre: Journal
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Publ. Info: Lancaster, Pa. : Published for the American Physical Society by the American Institute of Physics
Pages: - Volume / Issue: 79 Sequence Number: 084025 Start / End Page: - Identifier: Other: 111088197762258
Other: 0556-2821