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GW150914: The Advanced LIGO Detectors in the Era of First Discoveries.
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; 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; Barr, B.
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 Sant'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, The Netherlands.
  • Aggarwal N; Nikhef, Science Park, 1098 XG Amsterdam, The 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.
  • Araya MC; INFN, Sezione di Pisa, I-56127 Pisa, Italy.
  • Arceneaux CC; Australian National University, Canberra, Australian Capital Territory 0200, Australia.
  • Areeda JS; LIGO, California Institute of Technology, Pasadena, California 91125, USA.
  • Arnaud N; University of Wisconsin-Milwaukee, Milwaukee, Wisconsin 53201, USA.
  • Arun KG; LIGO, California Institute of Technology, Pasadena, California 91125, 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, 91400 Orsay, France.
  • Astone P; Chennai Mathematical Institute, Siruseri 603103, India.
  • 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, The 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.
  • Barr B; European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy.
Phys Rev Lett ; 116(13): 131103, 2016 Apr 01.
Article en En | MEDLINE | ID: mdl-27081966
ABSTRACT
Following a major upgrade, the two advanced detectors of the Laser Interferometer Gravitational-wave Observatory (LIGO) held their first observation run between September 2015 and January 2016. With a strain sensitivity of 10^{-23}/sqrt[Hz] at 100 Hz, the product of observable volume and measurement time exceeded that of all previous runs within the first 16 days of coincident observation. On September 14, 2015, the Advanced LIGO detectors observed a transient gravitational-wave signal determined to be the coalescence of two black holes [B. P. Abbott et al., Phys. Rev. Lett. 116, 061102 (2016)], launching the era of gravitational-wave astronomy. The event, GW150914, was observed with a combined signal-to-noise ratio of 24 in coincidence by the two detectors. Here, we present the main features of the detectors that enabled this observation. At full sensitivity, the Advanced LIGO detectors are designed to deliver another factor of 3 improvement in the signal-to-noise ratio for binary black hole systems similar in mass to GW150914.
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Texto completo: 1 Colección: 01-internacional Base de datos: MEDLINE Idioma: En Revista: Phys Rev Lett Año: 2016 Tipo del documento: Article País de afiliación: Estados Unidos
Texto completo
Añadir a Mi BVS
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Texto completo: 1 Colección: 01-internacional Base de datos: MEDLINE Idioma: En Revista: Phys Rev Lett Año: 2016 Tipo del documento: Article País de afiliación: Estados Unidos