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Constraints on cosmic strings from the LIGO-Virgo gravitational-wave detectors.
Aasi, J; Abadie, J; Abbott, B P; Abbott, R; Abbott, T; Abernathy, M R; Accadia, T; Acernese, F; Adams, C; Adams, T; Adhikari, R X; Affeldt, C; Agathos, M; Aggarwal, N; Aguiar, O D; Ajith, P; Allen, B; Allocca, A; Amador Ceron, E; Amariutei, D; Anderson, R A; Anderson, S B; Anderson, W G; Arai, K; Araya, M C; Arceneaux, C; Areeda, J; Ast, S; Aston, S M; Astone, P; Aufmuth, P; Aulbert, C; Austin, L; Aylott, B E; Babak, S; Baker, P T; Ballardin, G; Ballmer, S W; Barayoga, J C; Barker, D; Barnum, S H; Barone, F; Barr, B; Barsotti, L; Barsuglia, M; Barton, M A; Bartos, I; Bassiri, R; Basti, A; Batch, J.
Afiliación
  • Aasi J; LIGO-California Institute of Technology, Pasadena, California 91125, USA.
  • Abadie J; LIGO-California Institute of Technology, Pasadena, California 91125, USA.
  • Abbott BP; LIGO-California Institute of Technology, Pasadena, California 91125, USA.
  • Abbott R; LIGO-California Institute of Technology, Pasadena, California 91125, USA.
  • Abbott T; Louisiana State University, Baton Rouge, Louisiana 70803, USA.
  • Abernathy MR; LIGO-California Institute of Technology, Pasadena, California 91125, USA.
  • Accadia T; Laboratoire d'Annecy-le-Vieux de Physique des Particules (LAPP), Université de Savoie, CNRS/IN2P3, F-74941 Annecy-le-Vieux, France.
  • Acernese F; INFN, Sezione di Napoli, Complesso Universitario di Monte S.Angelo, I-80126 Napoli, Italy and Università di Salerno, Fisciano, I-84084 Salerno, Italy.
  • Adams C; LIGO-Livingston Observatory, Livingston, Louisiana 70754, USA.
  • Adams T; Cardiff University, Cardiff CF24 3AA, United Kingdom.
  • Adhikari RX; 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; Nikhef, Science Park, 1098 XG Amsterdam, The Netherlands.
  • Aggarwal N; LIGO-Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA.
  • Aguiar OD; Instituto Nacional de Pesquisas Espaciais, 12227-010, São José dos Campos, SP, Brazil.
  • Ajith P; LIGO-California Institute of Technology, Pasadena, California 91125, USA.
  • Allen B; Albert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-30167 Hannover, Germany and University of Wisconsin-Milwaukee, Milwaukee, Wisconsin 53201, USA and Leibniz Universität Hannover, D-30167 Hannover, Germany.
  • Allocca A; INFN, Sezione di Pisa, I-56127 Pisa, Italy and Università di Siena, I-53100 Siena, Italy.
  • Amador Ceron E; University of Wisconsin-Milwaukee, Milwaukee, Wisconsin 53201, USA.
  • Amariutei D; University of Florida, Gainesville, Florida 32611, USA.
  • Anderson RA; LIGO-California Institute of Technology, Pasadena, California 91125, USA.
  • Anderson SB; LIGO-California Institute of Technology, Pasadena, California 91125, USA.
  • Anderson WG; University of Wisconsin-Milwaukee, Milwaukee, Wisconsin 53201, USA.
  • Arai K; LIGO-California Institute of Technology, Pasadena, California 91125, USA.
  • Araya MC; LIGO-California Institute of Technology, Pasadena, California 91125, USA.
  • Arceneaux C; The University of Mississippi, University, Mississippi 38677, USA.
  • Areeda J; California State University Fullerton, Fullerton, California 92831, USA.
  • Ast S; Leibniz Universität Hannover, D-30167 Hannover, Germany.
  • Aston SM; LIGO-Livingston Observatory, Livingston, Louisiana 70754, USA.
  • Astone P; INFN, Sezione di Roma, I-00185 Roma, Italy.
  • Aufmuth P; Leibniz Universität Hannover, D-30167 Hannover, Germany.
  • Aulbert C; Albert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-30167 Hannover, Germany.
  • Austin L; LIGO-California Institute of Technology, Pasadena, California 91125, USA.
  • Aylott BE; University of Birmingham, Birmingham B15 2TT, United Kingdom.
  • Babak S; Albert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-14476 Golm, Germany.
  • Baker PT; Montana State University, Bozeman, Montana 59717, USA.
  • Ballardin G; European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy.
  • Ballmer SW; Syracuse University, Syracuse, New York 13244, USA.
  • Barayoga JC; LIGO-California Institute of Technology, Pasadena, California 91125, USA.
  • Barker D; LIGO-Hanford Observatory, Richland, Washington 99352, USA.
  • Barnum SH; LIGO-Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA.
  • Barone F; INFN, Sezione di Napoli, Complesso Universitario di Monte S.Angelo, I-80126 Napoli, Italy and Università di Salerno, Fisciano, I-84084 Salerno, Italy.
  • Barr B; SUPA, University of Glasgow, Glasgow G12 8QQ, United Kingdom.
  • Barsotti L; LIGO-Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA.
  • Barsuglia M; APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, F-75205 Paris Cedex 13, France.
  • Barton MA; LIGO-Hanford Observatory, Richland, Washington 99352, USA.
  • Bartos I; Columbia University, New York, New York 10027, USA.
  • Bassiri R; SUPA, University of Glasgow, Glasgow G12 8QQ, United Kingdom and Stanford University, Stanford, California 94305, USA.
  • Basti A; INFN, Sezione di Pisa, I-56127 Pisa, Italy and Università di Pisa, I-56127 Pisa, Italy.
  • Batch J; LIGO-Hanford Observatory, Richland, Washington 99352, USA.
Phys Rev Lett ; 112(13): 131101, 2014 Apr 04.
Article en En | MEDLINE | ID: mdl-24745400
ABSTRACT
Cosmic strings can give rise to a large variety of interesting astrophysical phenomena. Among them, powerful bursts of gravitational waves (GWs) produced by cusps are a promising observational signature. In this Letter we present a search for GWs from cosmic string cusps in data collected by the LIGO and Virgo gravitational wave detectors between 2005 and 2010, with over 625 days of live time. We find no evidence of GW signals from cosmic strings. From this result, we derive new constraints on cosmic string parameters, which complement and improve existing limits from previous searches for a stochastic background of GWs from cosmic microwave background measurements and pulsar timing data. In particular, if the size of loops is given by the gravitational backreaction scale, we place upper limits on the string tension Gµ below 10(-8) in some regions of the cosmic string parameter space.
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Base de datos: MEDLINE Idioma: En Revista: Phys Rev Lett Año: 2014 Tipo del documento: Article
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Base de datos: MEDLINE Idioma: En Revista: Phys Rev Lett Año: 2014 Tipo del documento: Article