Abstract:The Tibet-ASγ experiment has a water-Cherenkov muon-detector array (MD) as a part of 3 different arrays with specific purposes. To increase the ability of getting the primary proton, helium and iron spectra up to 10 16 eV and clarifing their spectral "knee" positions, we need to upgrade current PMT capabiltty in each MD cell. The current dynamic range of the PMTs is 5 to 2000 photoelectrons (PEs) which is enough for the purpose of observation of high-energy celestial gamma rays. However, according to Monte-Car… Show more
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