Your browser doesn't support javascript.
loading
Flavor Ratio of Astrophysical Neutrinos above 35 TeV in IceCube.
Aartsen, M G; Ackermann, M; Adams, J; Aguilar, J A; Ahlers, M; Ahrens, M; Altmann, D; Anderson, T; Arguelles, C; Arlen, T C; Auffenberg, J; 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; Blumenthal, J; Boersma, D J; Bohm, C; Bos, F; Bose, D; Böser, S; Botner, O; Brayeur, L; Bretz, H-P; Brown, A M; Buzinsky, N; Casey, J; Casier, M; Cheung, E; Chirkin, D; Christov, A; Christy, B; Clark, K; Classen, L; Clevermann, F; Coenders, S; Cowen, D F.
Afiliação
  • Aartsen MG; School of Chemistry and Physics, University of Adelaide, Adelaide, South Australia 5005, Australia.
  • 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.
  • Anderson T; Department of Physics, Pennsylvania State University, University Park, Pennsylvania 16802, USA.
  • Arguelles C; Department of Physics and Wisconsin IceCube Particle Astrophysics Center, University of Wisconsin, Madison, Wisconsin 53706, USA.
  • Arlen TC; Department of Physics, Pennsylvania State University, University Park, Pennsylvania 16802, USA.
  • Auffenberg J; III. Physikalisches Institut, RWTH Aachen University, D-52056 Aachen, Germany.
  • 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 und 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 Wisconsin IceCube Particle Astrophysics Center, University of Wisconsin, Madison, Wisconsin 53706, USA.
  • Berley D; DESY, D-15735 Zeuthen, Germany.
  • Bernardini E; Department of Physics, University of Maryland, College Park, Maryland 20742, USA.
  • Bernhard A; DESY, D-15735 Zeuthen, Germany.
  • Besson DZ; 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.
  • Blumenthal J; III. Physikalisches Institut, RWTH Aachen University, D-52056 Aachen, Germany.
  • Boersma DJ; Department of Physics, University of Maryland, College Park, Maryland 20742, USA.
  • Bohm C; III. Physikalisches Institut, RWTH Aachen University, D-52056 Aachen, Germany.
  • Bos F; Department of Physics and Astronomy, Uppsala University, Box 516, S-75120 Uppsala, Sweden.
  • Bose D; Oskar Klein Centre and Department of Physics, Stockholm University, SE-10691 Stockholm, Sweden.
  • Böser S; Fakultät für Physik und Astronomie, Ruhr-Universität Bochum, D-44780 Bochum, Germany.
  • Botner O; Department of Physics, Sungkyunkwan University, Suwon 440-746, Korea.
  • Brayeur L; Institute of Physics, University of Mainz, Staudinger Weg 7, D-55099 Mainz, Germany.
  • Bretz HP; Department of Physics and Astronomy, Uppsala University, Box 516, S-75120 Uppsala, Sweden.
  • Brown AM; Vrije Universiteit Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
  • Buzinsky N; DESY, D-15735 Zeuthen, Germany.
  • Casey J; Department of Physics and Astronomy, University of Canterbury, Private Bag 4800, Christchurch, New Zealand.
  • Casier M; Department of Physics, University of Alberta, Edmonton, Alberta, Canada T6G 2E1.
  • Cheung E; School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, Atlanta, Georgia 30332, USA.
  • Chirkin D; Vrije Universiteit Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
  • Christov A; Department of Physics, University of Maryland, College Park, Maryland 20742, USA.
  • Christy B; Department of Physics and Wisconsin IceCube Particle Astrophysics Center, University of Wisconsin, Madison, Wisconsin 53706, USA.
  • Clark K; Département de physique nucléaire et corpusculaire, Université de Genève, CH-1211 Genève, Switzerland.
  • Classen L; Department of Physics, University of Maryland, College Park, Maryland 20742, USA.
  • Clevermann F; Department of Physics, University of Toronto, Toronto, Ontario, Canada, M5S 1A7.
  • Coenders S; Erlangen Centre for Astroparticle Physics, Friedrich-Alexander-Universität Erlangen-Nürnberg, D-91058 Erlangen, Germany.
  • Cowen DF; Department of Physics, TU Dortmund University, D-44221 Dortmund, Germany.
Phys Rev Lett ; 114(17): 171102, 2015 May 01.
Article em En | MEDLINE | ID: mdl-25978221
ABSTRACT
A diffuse flux of astrophysical neutrinos above 100 TeV has been observed at the IceCube Neutrino Observatory. Here we extend this analysis to probe the astrophysical flux down to 35 TeV and analyze its flavor composition by classifying events as showers or tracks. Taking advantage of lower atmospheric backgrounds for showerlike events, we obtain a shower-biased sample containing 129 showers and 8 tracks collected in three years from 2010 to 2013. We demonstrate consistency with the (fefµfτ)⊕≈(111)⊕ flavor ratio at Earth commonly expected from the averaged oscillations of neutrinos produced by pion decay in distant astrophysical sources. Limits are placed on nonstandard flavor compositions that cannot be produced by averaged neutrino oscillations but could arise in exotic physics scenarios. A maximally tracklike composition of (010)⊕ is excluded at 3.3σ, and a purely showerlike composition of (100)⊕ is excluded at 2.3σ.
Buscar no Google
Imprimir
XML
PubMed Links

Base de dados: MEDLINE Idioma: En Ano de publicação: 2015 Tipo de documento: Article
Buscar no Google
Imprimir
XML
PubMed Links

Base de dados: MEDLINE Idioma: En Ano de publicação: 2015 Tipo de documento: Article