Samurai project: Verifying the consistency of black-hole-binary waveforms for gravitational-wave detection

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dc.contributor.authorHannam, Mark
dc.contributor.authorHusa, Sascha
dc.contributor.authorBaker, John G.
dc.contributor.authorBoyle, Michael
dc.contributor.authorBruegmann, Bernd
dc.contributor.authorChu, Tony
dc.contributor.authorDorband, Nils
dc.contributor.authorHerrmann, Frank
dc.contributor.authorHinder, Ian
dc.contributor.authorKelly, Bernard J.
dc.contributor.authorKidder, Lawrence E.
dc.contributor.authorLaguna, Pablo
dc.contributor.authorMatthews, Keith D.
dc.contributor.authorvan Meter, James R.
dc.contributor.authorPfeiffer, Harald P.
dc.contributor.authorPollney, Denis
dc.contributor.authorReisswig, Christian
dc.contributor.authorScheel, Mark A.
dc.contributor.authorShoemaker, Deirdre
dc.contributor.funderEuropean Gravitational Observatory
dc.contributor.funderVirgo-EGO Scientific Forum
dc.contributor.funderScience Foundation Ireland
dc.date.accessioned2017-08-29T09:04:01Z
dc.date.available2017-08-29T09:04:01Z
dc.date.issued2009
dc.description.abstractWe 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 (center dot=2,vertical bar m vertical bar=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 (center dot=2,vertical bar m vertical bar=2) modes is better than 10(-3) for binary masses above 60M with respect to the Enhanced LIGO detector noise curve, and for masses above 180M with respect to Advanced LIGO, Virgo, and Advanced Virgo. Between the waveforms with the best agreement, the mismatch is below 2x10(-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 to 14, or less than approximate to 25 in the best cases.en
dc.description.sponsorshipScience Foundation Ireland (07/RFP/PHYF148);European Gravitational Observatory (D/07/13385)en
dc.description.statusPeer revieweden
dc.description.versionPublished Versionen
dc.format.mimetypeapplication/pdfen
dc.identifier.articleid84025
dc.identifier.citationHannam, M., Husa, S., Baker, J. G., Boyle, M., Brügmann, B., Chu, T., Dorband, N., Herrmann, F., Hinder, I., Kelly, B. J., Kidder, L. E., Laguna, P., Matthews, K. D., van Meter, J. R., Pfeiffer, H. P., Pollney, D., Reisswig, C., Scheel, M. A. and Shoemaker, D. (2009) 'Samurai project: Verifying the consistency of black-hole-binary waveforms for gravitational-wave detection', Physical Review D, 79(8), 084025 (17pp). doi: 10.1103/PhysRevD.79.084025en
dc.identifier.doi10.1103/PhysRevD.79.084025
dc.identifier.issn2470-0010
dc.identifier.issn2470-0029
dc.identifier.issued8
dc.identifier.journaltitlePhysical Review Den
dc.identifier.urihttps://hdl.handle.net/10468/4570
dc.identifier.volume79
dc.language.isoenen
dc.publisherAmerican Physical Societyen
dc.relation.urihttps://journals.aps.org/prd/abstract/10.1103/PhysRevD.79.084025
dc.rights© 2009, American Physical Societyen
dc.subjectBoundary value-problemen
dc.subjectNumerical relativityen
dc.subjectInitial dataen
dc.subjectGeneral-relativityen
dc.subjectEinstein equationsen
dc.subjectCompact binariesen
dc.subjectModeling kicksen
dc.subjectSpinen
dc.subjectEvolutionen
dc.subjectRadiationen
dc.titleSamurai project: Verifying the consistency of black-hole-binary waveforms for gravitational-wave detectionen
dc.typeReviewen
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