PoS - Proceedings of Science
Volume 301 - 35th International Cosmic Ray Conference (ICRC2017) - Session Cosmic-Ray Indirect. CRI-instrumentation EAS
SiPM-based Camera Research and Development for the Wide Field of View Cherenkov Telescope Array of LHAASO
S. Zhang,* B.Y. Bi, B. Bi, C. Wang, Z. Cao, L. Yin, T. Montaruli, D. Dellavolpe, M. Heller on behalf of the LHAASO Collaboration
*corresponding author
Full text: pdf
Pre-published on: August 16, 2017
Published on: August 03, 2018
Abstract: Wide Field of View Cherenkov Telescope Array (WFCTA) of LHAASO consists of 18 air image Cherenkov telescopes. Each Cherenkov telescope consists of an array of 32×32 SiPM array which cover a field of view 14°×16° with a pixel size of 0.5°. The main scientific goal of WFCTA is to measure the ultra-high energy cosmic ray composition and energy spectrum from 30 TeV to a couple of EeV. Because SiPM cannot be aging under strong light exposure, SiPM-based camera can be operated in moon conditions, thus achieve a longer duty cycle than PMT-based camera, e.g. the duty cycle of SiPM-based camera is about 30%, while the PMT-based camera is about 10%. The SiPM-based camera is designed and developed for WFCTA. The square SiPM with photosensitive area of 15 mm×15 mm and Geiger-APD size of 25 mm is used to meet the required dynamic range from 10 photoelectrons (pes) to 32000 pes. Because SiPM can reach higher photon detection efficiency than quantum efficiency×collection efficiency of PMT, SiPM-based camera has almost the same signal to noise ratio with PMT-based camera of WFCTA prototype, although SiPM has higher dark count rate than PMT.
DOI: https://doi.org/10.22323/1.301.0423
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