PoS - Proceedings of Science
Volume 301 - 35th International Cosmic Ray Conference (ICRC2017) - Session Gamma-Ray Astronomy. GA-instrumentation
The Tibet AS+MD Project; status report 2017
M. Takita,* M. Amenomori, X.J. Bi, D. Chen, W.Y. Chen, S.W. Cui Danzengluobu, L.K. Ding, C.F. Feng, Z. Feng, Z.Y. Feng, Q.B. Gou, Y.Q. Guo, H.H. He, Z.T. He, K. Hibino, N. Hotta, H. Hu, H.B. Hu, J. Huang, H.Y. Jia, L. Jiang, F. Kajino, K. Kasahara, Y. Katayose, C. Kato, K. Kawata, M. Kozai, G.M. Le, A.F. Li, H.J. Li, W.J. Li, C. Liu, J.S. Liu, M.Y. Liu, H. Lu, X.R. Meng, T. Miyazaki, K. Mizutani, K. Munakata, T. Nakajima, Y. Nakamura, H. Nanjo, M. Nishizawa, T. Niwa, M. Ohnishi, T. Ohta, S. Ozawa, X.L. Qian, X.B. Qu, T. Saito, T.Y. Saito, M. Sakata, T.K. Sako, J. Shao, M. Shibata, A. Shiomi, T. Shirai, H. Sugimoto, Y.H. Tan, N. Tateyama, S. Torii, H. Tsuchiya, S. Udo, H. Wang, H.R. Wu, L. Xue, Y. Yamamoto, K. Yamauchi, Z. Yang, A.F. Yuan, T. Yuda, L.M. Zhai, H.M. Zhang, J.L. Zhang, Y. Zhang, Y. Zhang, Y. Zhang, Z. Na, X.X. Zhou on beahlf of the Tibet ASgamma Collaboration
*corresponding author
Full text: pdf
Pre-published on: August 18, 2017
Published on: August 03, 2018
Abstract
We built a large (approximately 4,000 m**2) water Cherenkov-
type muon detector array under the existing Tibet air shower array at
4,300 m above sea level, to observe 10-1000 TeV gamma rays from
cosmic-ray accelerators in our Galaxy with wide field of view
at very low background level. A gamma-ray induced air shower has
significantly less muons compared with a cosmic-ray induced one.
Therefore, we can effectively discriminate between primary gamma rays
and cosmic-ray background events by means of counting number of
muons in an air shower event by the muon detector array. We make a
status report on the experiment.
DOI: https://doi.org/10.22323/1.301.0831
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