Abstract
The IceCube Neutrino Observatory at the geographic South Pole, with its surface array IceTop, detects three different components of extensive air showers: the total signal at the surface, low energy muons on the periphery of the showers, and high energy muons in the deep In Ice array of IceCube. These measurements enable determination of the energy spectrum and composition of cosmic rays from PeV to EeV energies, the anisotropy in the distribution of cosmic ray arrival directions, the muon density of cosmic ray air showers, and the PeV gamma-ray flux. Furthermore, IceTop can be used as a veto for the neutrino measurements. The latest results from these IceTop analyses will be presented along with future plans.
Highlights
Introduction to Cosmic RayPhysics with the IceCube Neutrino ObservatoryThe IceCube Neutrino Observatory at the geographic South Pole, completed in December of 2010, is a world-class neutrino observatory but is an excellent instrument to study cosmic rays
A depth of 1500 m, these strings are instrumented with 60 digital optical modules (DOMs) apiece [1]
Both the IceTop and IceCube-InIce DOMs are fully integrated into the data acquisition system of the observatory
Summary
The IceCube Neutrino Observatory at the geographic South Pole, completed in December of 2010, is a world-class neutrino observatory but is an excellent instrument to study cosmic rays. The IceCube-InIce array consists of 86 strings buried beneath the surface of the Antarctic ice sheet to a depth of 2500 m. Each IceCube-InIce string is topped with two ice-Cherenkov tanks separated by 10 m. These two tanks are referred to as a station, and all the surface stations together comprise the IceTop array [3]. Each tank is viewed by two DOMs apiece, one running at low gain, the other at high gain, to maximize the dynamic range. Both the IceTop and IceCube-InIce DOMs are fully integrated into the data acquisition system of the observatory
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