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 5.1 σ . The source lies at a luminosity distance of 41 0 + 160 − 180     Mpc corresponding to a redshift z = 0.0 9 + 0.03 − 0.04 . In the source frame, the initial black hole masses are 3 6 + 5 − 4 M ⊙ and 2 9 + 4 − 4 M ⊙ , and the final black hole mass is 6 2 + 4 − 4 M ⊙ , with 3. 0 + 0.5 − 0.5 M ⊙ c 2 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.

Observation of Gravitational Waves from a Binary Black Hole Merger

Branchesi M;Coccia E;Drago M;Harms J;
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 5.1 σ . The source lies at a luminosity distance of 41 0 + 160 − 180     Mpc corresponding to a redshift z = 0.0 9 + 0.03 − 0.04 . In the source frame, the initial black hole masses are 3 6 + 5 − 4 M ⊙ and 2 9 + 4 − 4 M ⊙ , and the final black hole mass is 6 2 + 4 − 4 M ⊙ , with 3. 0 + 0.5 − 0.5 M ⊙ c 2 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.
Astrophysical studies of gravity,Classical black holes,Gravitational wave detection,Gravitational wave sources, Gravitation, Cosmology & Astrophysics
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/20.500.12571/2989
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