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Constraints on Ultrahigh-Energy Cosmic-Ray Sources from a Search for Neutrinos above 10 PeV with IceCube.
Aartsen, M G; Abraham, K; Ackermann, M; Adams, J; Aguilar, J A; Ahlers, M; Ahrens, M; Altmann, D; Andeen, K; Anderson, T; Ansseau, I; Anton, G; Archinger, M; Argüelles, C; Auffenberg, J; Axani, S; Bai, X; Barwick, S W; Baum, V; Bay, R; Beatty, J J; Becker Tjus, J; Becker, K-H; BenZvi, S; Berghaus, P; Berley, D; Bernardini, E; Bernhard, A; Besson, D Z; Binder, G; Bindig, D; Bissok, M; Blaufuss, E; Blot, S; Bohm, C; Börner, M; Bos, F; Bose, D; Böser, S; Botner, O; Braun, J; Brayeur, L; Bretz, H-P; Burgman, A; Carver, T; Casier, M; Cheung, E; Chirkin, D; Christov, A; Clark, K.
Affiliation
  • Aartsen MG; Department of Physics, University of Adelaide, Adelaide 5005, Australia.
  • Abraham K; Physik-department, Technische Universität München, D-85748 Garching, Germany.
  • Ackermann M; DESY, D-15735 Zeuthen, Germany.
  • Adams J; Department of Physics and Astronomy, University of Canterbury, Private Bag 4800 Christchurch, New Zealand.
  • Aguilar JA; Université Libre de Bruxelles, Science Faculty CP230, B-1050 Brussels, Belgium.
  • Ahlers M; Department of Physics and Wisconsin IceCube Particle Astrophysics Center, University of Wisconsin, Madison, Wisconsin 53706, USA.
  • Ahrens M; Oskar Klein Centre and Department of Physics, Stockholm University, SE-10691 Stockholm, Sweden.
  • Altmann D; Erlangen Centre for Astroparticle Physics, Friedrich-Alexander-Universität Erlangen-Nürnberg, D-91058 Erlangen, Germany.
  • Andeen K; Department of Physics, Marquette University, Milwaukee, Wisconsin 53201, USA.
  • Anderson T; Department of Physics, Pennsylvania State University, University Park, Pennsylvania 16802, USA.
  • Ansseau I; Université Libre de Bruxelles, Science Faculty CP230, B-1050 Brussels, Belgium.
  • Anton G; Erlangen Centre for Astroparticle Physics, Friedrich-Alexander-Universität Erlangen-Nürnberg, D-91058 Erlangen, Germany.
  • Archinger M; Institute of Physics, University of Mainz, Staudinger Weg 7, D-55099 Mainz, Germany.
  • Argüelles C; Department of Physics, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA.
  • Auffenberg J; III. Physikalisches Institut, RWTH Aachen University, D-52056 Aachen, Germany.
  • Axani S; Department of Physics, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA.
  • Bai X; Physics Department, South Dakota School of Mines and Technology, Rapid City, south Dakota 57701, USA.
  • Barwick SW; Department of Physics and Astronomy, University of California, Irvine, California 92697, USA.
  • Baum V; Institute of Physics, University of Mainz, Staudinger Weg 7, D-55099 Mainz, Germany.
  • Bay R; Department of Physics, University of California, Berkeley, California 94720, USA.
  • Beatty JJ; Department of Physics and Center for Cosmology and Astro-Particle Physics, Ohio State University, Columbus, Ohio 43210, USA.
  • Becker Tjus J; Department of Astronomy, Ohio State University, Columbus, Ohio 43210, USA.
  • Becker KH; Fakultät für Physik & Astronomie, Ruhr-Universität Bochum, D-44780 Bochum, Germany.
  • BenZvi S; Department of Physics, University of Wuppertal, D-42119 Wuppertal, Germany.
  • Berghaus P; Department of Physics and Astronomy, University of Rochester, Rochester, New York 14627, USA.
  • Berley D; National Research Nuclear University MEPhI (Moscow Engineering Physics Institute), 115409, Moscow, Russia.
  • Bernardini E; Department of Physics, University of Maryland, College Park, Maryland 20742, USA.
  • Bernhard A; DESY, D-15735 Zeuthen, Germany.
  • Besson DZ; Physik-department, Technische Universität München, D-85748 Garching, Germany.
  • Binder G; Department of Physics and Astronomy, University of Kansas, Lawrence, Kansas 66045, USA.
  • Bindig D; Department of Physics, University of California, Berkeley, California 94720, USA.
  • Bissok M; Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA.
  • Blaufuss E; Department of Physics, University of Wuppertal, D-42119 Wuppertal, Germany.
  • Blot S; III. Physikalisches Institut, RWTH Aachen University, D-52056 Aachen, Germany.
  • Bohm C; Department of Physics, University of Maryland, College Park, Maryland 20742, USA.
  • Börner M; DESY, D-15735 Zeuthen, Germany.
  • Bos F; Oskar Klein Centre and Department of Physics, Stockholm University, SE-10691 Stockholm, Sweden.
  • Bose D; Department of Physics, TU Dortmund University, D-44221 Dortmund, Germany.
  • Böser S; Fakultät für Physik & Astronomie, Ruhr-Universität Bochum, D-44780 Bochum, Germany.
  • Botner O; Department of Physics, Sungkyunkwan University, Suwon 440-746, Korea.
  • Braun J; Institute of Physics, University of Mainz, Staudinger Weg 7, D-55099 Mainz, Germany.
  • Brayeur L; Department of Physics and Astronomy, Uppsala University, Box 516, S-75120 Uppsala, Sweden.
  • Bretz HP; Department of Physics and Wisconsin IceCube Particle Astrophysics Center, University of Wisconsin, Madison, Wisconsin 53706, USA.
  • Burgman A; Vrije Universiteit Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
  • Carver T; DESY, D-15735 Zeuthen, Germany.
  • Casier M; Department of Physics and Astronomy, Uppsala University, Box 516, S-75120 Uppsala, Sweden.
  • Cheung E; Département de physique nucléaire et corpusculaire, Université de Genève, CH-1211 Genève, Switzerland.
  • Chirkin D; Vrije Universiteit Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
  • Christov A; Department of Physics, University of Maryland, College Park, Maryland 20742, USA.
  • Clark K; Department of Physics and Wisconsin IceCube Particle Astrophysics Center, University of Wisconsin, Madison, Wisconsin 53706, USA.
Phys Rev Lett ; 117(24): 241101, 2016 Dec 09.
Article in En | MEDLINE | ID: mdl-28009216
ABSTRACT
We report constraints on the sources of ultrahigh-energy cosmic rays (UHECRs) above 10^{9} GeV, based on an analysis of seven years of IceCube data. This analysis efficiently selects very high- energy neutrino-induced events which have deposited energies from 5×10^{5} GeV to above 10^{11} GeV. Two neutrino-induced events with an estimated deposited energy of (2.6±0.3)×10^{6} GeV, the highest neutrino energy observed so far, and (7.7±2.0)×10^{5} GeV were detected. The atmospheric background-only hypothesis of detecting these events is rejected at 3.6σ. The hypothesis that the observed events are of cosmogenic origin is also rejected at >99% CL because of the limited deposited energy and the nonobservation of events at higher energy, while their observation is consistent with an astrophysical origin. Our limits on cosmogenic neutrino fluxes disfavor the UHECR sources having a cosmological evolution stronger than the star formation rate, e.g., active galactic nuclei and γ-ray bursts, assuming proton-dominated UHECRs. Constraints on UHECR sources including mixed and heavy UHECR compositions are obtained for models of neutrino production within UHECR sources. Our limit disfavors a significant part of parameter space for active galactic nuclei and new-born pulsar models. These limits on the ultrahigh-energy neutrino flux models are the most stringent to date.
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Full text: 1 Collection: 01-internacional Database: MEDLINE Language: En Journal: Phys Rev Lett Year: 2016 Document type: Article Affiliation country: Australia
Fulltext
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Full text: 1 Collection: 01-internacional Database: MEDLINE Language: En Journal: Phys Rev Lett Year: 2016 Document type: Article Affiliation country: Australia