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IceCube Neutrino Telescope and the GZK n detection

TAUP2003. IceCube Neutrino Telescope and the GZK n detection. Shigeru Yoshida, Chiba University. The IceCube Collaboration. Institutions: 11 US, 9 European institutions and 1 Japanese institution ; ≈150 people Bartol Research Institute, University of Delaware, USA BUGH Wuppertal, Germany

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IceCube Neutrino Telescope and the GZK n detection

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  1. TAUP2003 IceCube Neutrino Telescope and the GZK n detection Shigeru Yoshida, Chiba University

  2. The IceCube Collaboration Institutions: 11 US, 9 European institutions and1 Japanese institution; ≈150 people • Bartol Research Institute, University of Delaware, USA • BUGH Wuppertal, Germany • Dept. of Physics, Chiba University, JAPAN • Universite Libre de Bruxelles, Brussels, Belgium • CTSPS, Clark-Atlanta University, Atlanta USA • DESY-Zeuthen, Zeuthen, Germany • Institute for Advanced Study, Princeton, USA • Dept. of Technology, Kalmar University, Kalmar, Sweden • Lawrence Berkeley National Laboratory, Berkeley, USA • Department of Physics, Southern University and A\&M College, Baton Rouge, LA, USA • Dept. of Physics, UC Berkeley, USA • Institute of Physics, University of Mainz, Mainz, Germany • Department of Physics, University of Maryland, USA • University of Mons-Hainaut, Mons, Belgium • Dept. of Physics and Astronomy, University of Pennsylvania, Philadelphia, USA • Dept. of Astronomy, Dept. of Physics, SSEC, University of Wisconsin, Madison, USA • Physics Department, University of Wisconsin, River Falls, USA • Division of High Energy Physics, Uppsala University, Uppsala, Sweden • Fysikum, Stockholm University, Stockholm, Sweden • University of Alabama, USA • Vrije Universiteit Brussel, Brussel, Belgium

  3. TAUP 2003 Project status • Approved by U.S. the National Science Board • Startup funding is allocated. 100 DOMs are produced and being tested this year. • Assembling of the drill/IceTop prototypes is carried out at the pole this season. • Full Construction start in 04/05; takes 6 years to complete. • Then 16 strings per season, increased rate may be possible.

  4. TAUP 2003 GZK EHEn detection • What is the GZK mechanism? • EHE n/m/t Propagation in the Earth • Expected intensities at the IceCube depth • Atmospheric m – background • Event rate

  5. t/mappeared in 10 PeV- EeV are our prime target on GZK n detection. 1/100-1/500 of primary n intensity! Downwardt and m make main contributions in PeV -EeV Energy Estimation would be a key for the bg reduction Because atmospheric m spectrum ~ E3.7 TAUP 2003 Summary GZK n is DETECTABLE by IceCube 0.2-40 events/year (BG 0.05 events/year)

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