Contributors: Abbott, B. P.; Abbott; Acernese, F.; Ackley; Adhikari, R. X.; Adya; Agatsuma, K.; Aggarwal, A.; Ajith, P.; Allen; Anderson, S. B.; Anderson; Araya, M. C.; Arceneaux; Arun, K. G.; Ascenzi; Astone, P.; Aufmuth, P.; Bader, M. K. M.; Baker; Ballardin, G.; Ballmer; Barish, B. C.; Barker; Barsotti, L.; Barsuglia; Barton, M. A.; Bartos, C.; Baune, C.; Bavigadda; Bejger, M.; Belczynski; Berger, B. K.; Bergman; Bhandare, R.; Bilenko; Birney, R.; Birnholtz, M.; Biwer, C.; Bizouard, D.; Blair, D. G.; Blair; Bodiya, T. P.; Boer; Bojtos, P.; Bond, A.; Bork, R.; Boschi; Bozzi, A.; Bradaschia; Branchesi, M.; Brau; Brinkmann, M.; Brisson; Brown, D. A.; Brown; Buikema, A.; Bulik; Buskulic, D.; Buy; Cagnoli, G.; Cahillane; Callister, T.; Calloni, J.; Capano, C. D.; Capocasa; Diaz, J. Casanueva; Casentini, M.; Cavalier, F.; Cavalieri; Baiardi, L. Cerboni; Cerretani; Chakraborty, R.; Chalermsongsak, M.; Chao, S.; Charlton, Y.; Chen, Y.; Cheng; Cho, H. S.; Cho; Chua, S.; Chung; Cleva, F.; Coccia; Collette, C. G.; Cominsky; Conti, L.; Cook; Cortese, S.; Costa; Coulon, J. P; Countryman; Coward, D. M.; Cowart; Craig, K.; Creighton; Crowder, S. G.; Cruise; Cuoco, E.; Dal, Canton
نبذة مختصرة : 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 x 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 sigma. The source lies at a luminosity distance of 410(-180)(+160) Mpc corresponding to a redshift z = 0.09(-0.01)(+0.03). In the source frame, the initial black hole masses are 36(-4)(+5)M(circle dot) and 29(-4)(+4)M(circle dot), and the final black hole mass is 62(-4)(+4) M-circle dot, with 3.0(-0.5)(+0.5) M(circle dot)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.
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