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, -4) Msun and 29 (+4, -4) Msun, and the final black hole mass is 62 (+4, -4) Msun, with 3.0 (+0.5, -0.5) Msun 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.

Observation of gravitational waves from a binary black hole merger

BALDACCINI, FRANCESCA;GAMMAITONI, Luca;PUNTURO, MICHELE;TRAVASSO, FLAVIO;VOCCA, Helios;
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, -4) Msun and 29 (+4, -4) Msun, and the final black hole mass is 62 (+4, -4) Msun, with 3.0 (+0.5, -0.5) Msun 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
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11391/1404174
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