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Results of the first coincident observations by two laser-interferometric gravitational wave detectors

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Schutz,  Bernard F.
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Strain,  Kenneth A.
Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

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Danzmann,  Karsten
Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

Niebauer,  T. M.
Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

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Rüdiger,  Albrecht
Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

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Schilling,  Roland
Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

Schnupp,  L.
Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

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Winkler,  Walter
Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

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60227.pdf
(Publisher version), 509KB

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Citation

Nicholson, D., Dickson, C. A., Watkins, W. J., Schutz, B. F., Shuttleworth, J. R., Jones, G. S., et al. (1996). Results of the first coincident observations by two laser-interferometric gravitational wave detectors. Physics Letters A, 218(3-6), 175-180. doi:10.1016/0375-9601(96)00438-0.


Cite as: http://hdl.handle.net/11858/00-001M-0000-0013-10E0-1
Abstract
We report an upper bound on the strain amplitude of gravitational wave bursts in a waveband from around 800 Hz to 1.25 kHz. In an effective coincident observing period of 62 hours, the prototype laser interferometric gravitational wave detectors of the University of Glasgow and Max Planck Institute for Quantum Optics, have set a limit of 4.9 × 10-16, averaging over wave polarizations and incident directions. This is roughly a factor of 2 worse than the theoretical best limit that the detectors could have set, the excess being due to unmodelled non-Gaussian noise. The experiment has demonstrated the viability of the kind of observations planned for the large-scale interferometers that should be on-line in a few years time.