AMANDA-II is a neutrino telescope composed of 677 optical sensors organized along 19 strings buried deep in the Antarctic ice cap.It is designed to detect Cherenkov light produced by cosmic-ray- and neutrino-induced muons.The majority of events recorded by AMANpA-II are caused by muons which are produced in the atmosphere by high-energy cosmic rays.The leading uncertainties in simulating such events come from the choice of the high-energy model used to describe the first interaction of the cosmic rays,uncertainties in our knowledge and implementation of the ice properties at the depth of the detector,and individual optical module sensitivities.A method is developed that results in a flux measurement of cosmic rays with energies 1.5-200 TeV per nucleon (95% of primaries causing low-multiplicity events in AMANDA-II have energies in this range) independent of ice model and optical module sensitivities.Predictions of six commonly-used high-energy interaction models -
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