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Observation of Gravitational Waves from a Binary Black Hole Merger.
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, V B; Affeldt, C; Agathos, M; Agatsuma, K; Aggarwal, N; Aguiar, O D; Aiello, L; Ain, A; Ajith, P; Allen, B; Allocca, A; Altin, P A; Anderson, S B; Anderson, W G; Arai, K; Arain, M A; Araya, M C; Arceneaux, C C; Areeda, J S; Arnaud, N; Arun, K G; Ascenzi, S; Ashton, G; Ast, M; Aston, S M; Astone, P; Aufmuth, P; Aulbert, C; Babak, S; Bacon, P; Bader, M K M; Baker, P T; Baldaccini, F; Ballardin, G; Ballmer, S W; Barayoga, J C; Barclay, S E; Barish, B C; Barker, D; Barone, F.
Afiliación
  • Abbott BP; LIGO, California Institute of Technology, Pasadena, California 91125, USA.
  • Abbott R; LIGO, California Institute of Technology, Pasadena, California 91125, USA.
  • Abbott TD; Louisiana State University, Baton Rouge, Louisiana 70803, USA.
  • Abernathy MR; LIGO, California Institute of Technology, Pasadena, California 91125, USA.
  • Acernese F; Università di Salerno, Fisciano, I-84084 Salerno, Italy.
  • Ackley K; INFN, Sezione di Napoli, Complesso Universitario di Monte S. Angelo, I-80126 Napoli, Italy.
  • Adams C; University of Florida, Gainesville, Florida 32611, USA.
  • Adams T; LIGO Livingston Observatory, Livingston, Louisiana 70754, USA.
  • Addesso P; Laboratoire d'Annecy-le-Vieux de Physique des Particules (LAPP), Université Savoie Mont Blanc, CNRS/IN2P3, F-74941 Annecy-le-Vieux, France.
  • Adhikari RX; Università di Salerno, Fisciano, I-84084 Salerno, Italy.
  • Adya VB; LIGO, California Institute of Technology, Pasadena, California 91125, USA.
  • Affeldt C; Albert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-30167 Hannover, Germany.
  • Agathos M; Albert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-30167 Hannover, Germany.
  • Agatsuma K; Nikhef, Science Park, 1098 XG Amsterdam, Netherlands.
  • Aggarwal N; Nikhef, Science Park, 1098 XG Amsterdam, Netherlands.
  • Aguiar OD; LIGO, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA.
  • Aiello L; Instituto Nacional de Pesquisas Espaciais, 12227-010 São José dos Campos, São Paulo, Brazil.
  • Ain A; INFN, Gran Sasso Science Institute, I-67100 L'Aquila, Italy.
  • Ajith P; INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy.
  • Allen B; Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India.
  • Allocca A; International Centre for Theoretical Sciences, Tata Institute of Fundamental Research, Bangalore 560012, India.
  • Altin PA; Albert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-30167 Hannover, Germany.
  • Anderson SB; University of Wisconsin-Milwaukee, Milwaukee, Wisconsin 53201, USA.
  • Anderson WG; Leibniz Universität Hannover, D-30167 Hannover, Germany.
  • Arai K; Università di Pisa, I-56127 Pisa, Italy.
  • Arain MA; INFN, Sezione di Pisa, I-56127 Pisa, Italy.
  • Araya MC; Australian National University, Canberra, Australian Capital Territory 0200, Australia.
  • Arceneaux CC; LIGO, California Institute of Technology, Pasadena, California 91125, USA.
  • Areeda JS; University of Wisconsin-Milwaukee, Milwaukee, Wisconsin 53201, USA.
  • Arnaud N; LIGO, California Institute of Technology, Pasadena, California 91125, USA.
  • Arun KG; University of Florida, Gainesville, Florida 32611, USA.
  • Ascenzi S; LIGO, California Institute of Technology, Pasadena, California 91125, USA.
  • Ashton G; The University of Mississippi, University, Mississippi 38677, USA.
  • Ast M; California State University Fullerton, Fullerton, California 92831, USA.
  • Aston SM; LAL, Université Paris-Sud, CNRS/IN2P3, Université Paris-Saclay, Orsay, France.
  • Astone P; Chennai Mathematical Institute, Chennai, India 603103.
  • Aufmuth P; INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy.
  • Aulbert C; Università di Roma Tor Vergata, I-00133 Roma, Italy.
  • Babak S; University of Southampton, Southampton SO17 1BJ, United Kingdom.
  • Bacon P; Universität Hamburg, D-22761 Hamburg, Germany.
  • Bader MK; LIGO Livingston Observatory, Livingston, Louisiana 70754, USA.
  • Baker PT; INFN, Sezione di Roma, I-00185 Roma, Italy.
  • Baldaccini F; Albert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-30167 Hannover, Germany.
  • Ballardin G; Albert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-30167 Hannover, Germany.
  • Ballmer SW; Albert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-14476 Potsdam-Golm, Germany.
  • Barayoga JC; APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, F-75205 Paris Cedex 13, France.
  • Barclay SE; Nikhef, Science Park, 1098 XG Amsterdam, Netherlands.
  • Barish BC; Montana State University, Bozeman, Montana 59717, USA.
  • Barker D; Università di Perugia, I-06123 Perugia, Italy.
  • Barone F; INFN, Sezione di Perugia, I-06123 Perugia, Italy.
Phys Rev Lett ; 116(6): 061102, 2016 Feb 12.
Article en En | MEDLINE | ID: mdl-26918975
ABSTRACT
On September 14, 2015 at 095045 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(-180)(+160) Mpc corresponding to a redshift z=0.09(-0.04)(+0.03). In the source frame, the initial black hole masses are 36(-4)(+5)M⊙ and 29(-4)(+4)M⊙, and the final black hole mass is 62(-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.
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Texto completo: 1 Base de datos: MEDLINE Idioma: En Revista: Phys Rev Lett Año: 2016 Tipo del documento: Article
Texto completo
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Texto completo: 1 Base de datos: MEDLINE Idioma: En Revista: Phys Rev Lett Año: 2016 Tipo del documento: Article