On September 14, 2015 at 09:50:45 UTC the two detectors of the Laser Interferometer Gravitational-Wave Observatory simultaneously observed a transient gravitational-wave signal. The signal sweeps upwards in frequency from 35 to 250 Hz with a peak gravitational-wave strain of 1.0×10−21. It matches the waveform predicted by general relativity for the inspiral and merger of a pair of black holes and the ringdown of the resulting single black hole. The signal was observed with a matched-filter signal-to-noise ratio of 24 and a false alarm rate estimated to be less than 1 event per 203 000 years, equivalent to a significance greater than 5.1σ. The source lies at a luminosity distance of 410+160−180  Mpc corresponding to a redshift z=0.09+0.03−0.04. In the source frame, the initial black hole masses are 36+5−4M⊙ and 29+4−4M⊙, and the final black hole mass is 62+4−4M⊙, with 3.0+0.5−0.5M⊙c2 radiated in gravitational waves. All uncertainties define 90% credible intervals. These observations demonstrate the existence of binary stellar-mass black hole systems. This is the first direct detection of gravitational waves and the first observation of a binary black hole merger.

Abbott, B. ., Abbott, R., Abbott, T. ., Abernathy, M. ., Acernese, F., Ackley, K., et al. (2016). Observation of Gravitational Waves from a Binary Black Hole Merger. PHYSICAL REVIEW LETTERS, 116(6), 061102-1-061102-16 [10.1103/PhysRevLett.116.061102].

Observation of Gravitational Waves from a Binary Black Hole Merger

BRANCHESI, MARICA;CERBONI BAIARDI, LORENZO;Cuoco, E.;GRECO, GIUSEPPE;GUIDI, GIANLUCA MARIA;MONTANI, MATTEO;PIERGIOVANNI, FRANCESCO;VICERE', ANDREA;
2016

Abstract

On September 14, 2015 at 09:50:45 UTC the two detectors of the Laser Interferometer Gravitational-Wave Observatory simultaneously observed a transient gravitational-wave signal. The signal sweeps upwards in frequency from 35 to 250 Hz with a peak gravitational-wave strain of 1.0×10−21. It matches the waveform predicted by general relativity for the inspiral and merger of a pair of black holes and the ringdown of the resulting single black hole. The signal was observed with a matched-filter signal-to-noise ratio of 24 and a false alarm rate estimated to be less than 1 event per 203 000 years, equivalent to a significance greater than 5.1σ. The source lies at a luminosity distance of 410+160−180  Mpc corresponding to a redshift z=0.09+0.03−0.04. In the source frame, the initial black hole masses are 36+5−4M⊙ and 29+4−4M⊙, and the final black hole mass is 62+4−4M⊙, with 3.0+0.5−0.5M⊙c2 radiated in gravitational waves. All uncertainties define 90% credible intervals. These observations demonstrate the existence of binary stellar-mass black hole systems. This is the first direct detection of gravitational waves and the first observation of a binary black hole merger.
2016
Abbott, B. ., Abbott, R., Abbott, T. ., Abernathy, M. ., Acernese, F., Ackley, K., et al. (2016). Observation of Gravitational Waves from a Binary Black Hole Merger. PHYSICAL REVIEW LETTERS, 116(6), 061102-1-061102-16 [10.1103/PhysRevLett.116.061102].
Abbott, B.  .p.; Abbott, R.; Abbott, T.  .d.; Abernathy, M.  .r.; Acernese, F.; Ackley, K.; Adams, C.; Adams, T.; Addesso, P.; Adhikari, R.  .x.; Adya...espandi
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11585/865824
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