Testing the surface detector simulation for the Pierre Auger Observatory

Abstract

The building block of the surface detector of the Pierre Auger Observatory is a water Cherenkov tank. The response to shower particles is simulated using a dedicated program based on GEANT4. To check the simulation chain, we compare the simulated signals produced by cosmic muons at various zenith angles with experimental data from a special Cherenkov detector equipped with a muon hodoscope. The signals from muon-decay electrons and the evolution of the charge with water level are also studied.

Upper Limit on the Diffuse Flux of Ultrahigh Energy Tau Neutrinos from the Pierre Auger Observatory

“…The TAUOLA package [Jadach et al(1993)] is used to simulate τ decay and obtain the secondary particles and their energies. Showers induced by the products of decaying τ s with energies between 10 17 to 3 × 10 20 eV are simulated at zenith angles ranging between 90.1 • and 95.9 • and at an altitude of the decay point above the Pierre Auger Observatory in the range 0 − 2500 m. Finally, to evaluate the response of the SD to such events, the particles reaching the ground in the simulation are stored and injected into a detailed simulation of the SD [Ghia(2007)].…”

Layered water Cherenkov detector for the study of ultra high energy cosmic rays

“…In the Auger surface array, the calibration of the WCD is based on the energy deposited by a vertical muon traversing the WCD volume at its centre [21,22]. The energy deposited by such muons is about 240 MeV and is called a VEM (Vertical Equivalent Muon).…”