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Journal Article

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

MPS-Authors
http://pubman.mpdl.mpg.de/cone/persons/resource/persons4287

Husa,  Sascha
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

http://pubman.mpdl.mpg.de/cone/persons/resource/persons20656

Dorband,  Nils
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

http://pubman.mpdl.mpg.de/cone/persons/resource/persons20659

Hinder,  Ian
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

http://pubman.mpdl.mpg.de/cone/persons/resource/persons20666

Pollney,  Denis
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

http://pubman.mpdl.mpg.de/cone/persons/resource/persons20669

Reisswig,  Christian
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Fulltext (public)

0901.2437
(Preprint), 527KB

PRD79_084025.pdf
(Any fulltext), 627KB

Supplementary Material (public)
There is no public supplementary material available
Citation

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.


Cite as: http://hdl.handle.net/11858/00-001M-0000-0012-BC73-4
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.