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 and  on beahlf of the Tibet ASgamma Collaborationet al. (click to show)
Full text: pdf
Pre-published on: August 18, 2017
Published on: August 03, 2018
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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