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

Hannam, Mark ORCID: https://orcid.org/0000-0001-5571-325X, Husa, Sascha, Baker, John, Boyle, Michael, Brügmann, Bernd, Chu, Tony, Dorband, Nils, Herrmann, Frank, Hinder, Ian, Kelly, Bernard, Kidder, Lawrence, Laguna, Pablo, Matthews, Keith, van Meter, James, Pfeiffer, Harald, Pollney, Denis, Reisswig, Christian, Scheel, Mark and Shoemaker, Deirdre 2009. Samurai project: Verifying the consistency of black-hole-binary waveforms for gravitational-wave detection. Physical Review D 79 (8) , 084025. 10.1103/PhysRevD.79.084025

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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 (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 (ℓ=2,|m|=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 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 ≈14, or less than ≈25 in the best cases.

Item Type:	Article
Date Type:	Publication
Status:	Published
Schools:	Physics and Astronomy
Subjects:	Q Science > QB Astronomy
Publisher:	American Physical Society
ISSN:	1550-7998
Last Modified:	20 Oct 2022 08:13
URI:	https://orca.cardiff.ac.uk/id/eprint/27608

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