Abstract
Measurement of the all-particle cosmic ray energy spectrum with IceTop
Highlights
The IceTop air shower array is currently under construction at the geographic South Pole as the surface component of the IceCube Neutrino Observatory (e.g. Achterberg et al, 2006)
A method to reconstruct shower size and primary energy spectrum from data measured by IceTop is described
An IceTop station consists of two frozen water tanks with two Digital Optical Modules (DOMs) each to detect Cherenkov light produced by charged particles
Summary
The IceTop air shower array is currently under construction at the geographic South Pole as the surface component of the IceCube Neutrino Observatory (e.g. Achterberg et al, 2006). After completion in January 2011, it consists of 81 detector stations arranged on a triangular grid with a nominal spacing of 125m covering a total area of 1km. IceTop is designed to detect air showers with primary energies between 500 TeV and 1EeV. This has several advantages: local shower density fluctuations are relatively small, and the dominant component of the air shower are photons and electrons. In combination with IceCube, which can only be reached by muons with an energy of more than about 300GeV, IceTop provides a new handle on the primary mass by measuring the air shower parameters at the surface in coincidence with TeV muons reaching the deep detector.
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