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Observation of high energy atmospheric neutrinos with the Antarctic muon and neutrino detector array
Physical Review D 66, 012005 (2002)
Handle: Document-17272
Owner: Site Administrator (User-2, admin:DocuShare)DS
Friday, October 14, 2005 03:29:20 PM CDT
Tuesday, April 3, 2007 05:49:40 PM CDT
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  • Downgoing muons were generated by atmospheric shower simulations of isotropic protons with BASIEV @6# or protons and heavier nuclei with CORSIKA using the QGSJET generator @7,8#, and tracked to the detector with the muon propagation code MUDEDX @9,10#.
  • Two other muon propagation codes were used to check for systematic differences: PROPMU @11# with a 30% lower rate and MMC @12# with a slightly higher rate.
  • This fit is a simple x2 minimization of the apparent photon flux direction, for which an analytic solution can be calculated quickly @21#~see also @1#! We use time intervals of @215 ns,125 ns# and @215 ns, 175 ns#, and denote the corresponding parameters as Ndir (25) and Ndir (75) , ...
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Appears In: 2005
Preferred Version: Observation of high energy atmospheric neutrinos with the Antarctic muon and neutrino detector array

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