The TIBET AS+MD project; progress report 2015

M. Amenomori; X. J. Bi; D. Chen; T. L. Chen; W. Y. Chen; S. W. Cui; Danzengluobu; L. K. Ding; C. F. Feng; Zhaoyang Feng; Z. Y. Feng; Q. B. Gou; Y. Q. Guo; H. H. He; Z. T. He; K. Hibino; N. Hotta; Haibing Hu; H. B. Hu; J. Huang; H. Y. Jia; L. Jiang; F. Kajino; K. Kasahara; Y. Katayose; C. Kato; K. Kawata; M. Kozai; Labaciren; 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; I. Ohta; Shunsuke 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; M. Takita; Y. H. Tan; N. Tateyama; Shoji Torii; H. Tsuchiya; S. Udo; H. Wang; H. R. Wu; L. Xue; Y. Yamamoto; K. Yamauchi; Z. Yang; S. Yasue; A. F. Yuan; T. Yuda; L. M. Zhai; H. M. Zhang; J. L. Zhang; X. Y. Zhang; Y. Zhang; Yi Zhang; Ying Zhang; Zhaxisangzhu; X. X. Zhou

The TIBET AS+MD project; progress report 2015

M. Amenomori, X. J. Bi, D. Chen, T. L. Chen, W. Y. Chen, S. W. Cui, Danzengluobu, L. K. Ding, C. F. Feng, Zhaoyang Feng, Z. Y. Feng, Q. B. Gou, Y. Q. Guo, H. H. He, Z. T. He, K. Hibino, N. Hotta, Haibing Hu, H. B. Hu, J. HuangH. Y. Jia, L. Jiang, F. Kajino, K. Kasahara, Y. Katayose, C. Kato, K. Kawata, M. Kozai, Labaciren, 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, I. Ohta, Shunsuke 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, M. Takita, Y. H. Tan, N. Tateyama, Shoji Torii, H. Tsuchiya, S. Udo, H. Wang, H. R. Wu, L. Xue, Y. Yamamoto, K. Yamauchi, Z. Yang, S. Yasue, A. F. Yuan, T. Yuda, L. M. Zhai, H. M. Zhang, J. L. Zhang, X. Y. Zhang, Y. Zhang, Yi Zhang, Ying Zhang, Zhaxisangzhu, X. X. Zhou

Waseda Research Institute for Science and Engineering

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Abstract

We plan to build a large (approximately 10,000 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 will make a progress report on the project, as some part of it started data-taking in 2014.

Original language	English
Article number	969
Journal	Unknown Journal
Volume	30-July-2015
Publication status	Published - 2015

ASJC Scopus subject areas

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Amenomori, M, Bi, XJ, Chen, D, Chen, TL, Chen, WY, Cui, SW, Danzengluobu, Ding, LK, Feng, CF, Feng, Z, Feng, ZY, Gou, QB, Guo, YQ, He, HH, He, ZT, Hibino, K, Hotta, N, Hu, H, Hu, HB, Huang, J, Jia, HY, Jiang, L, Kajino, F, Kasahara, K, Katayose, Y, Kato, C, Kawata, K, Kozai, M, Labaciren, Le, GM, Li, AF, Li, HJ, Li, WJ, Liu, C, Liu, JS, Liu, MY, Lu, H, Meng, XR, Miyazaki, T, Mizutani, K, Munakata, K, Nakajima, T, Nakamura, Y, Nanjo, H, Nishizawa, M, Niwa, T, Ohnishi, M, Ohta, I, Ozawa, S, Qian, XL, Qu, XB, Saito, T, Saito, TY, Sakata, M, Sako, TK, Shao, J, Shibata, M, Shiomi, A, Shirai, T, Sugimoto, H, Takita, M, Tan, YH, Tateyama, N, Torii, S, Tsuchiya, H, Udo, S, Wang, H, Wu, HR, Xue, L, Yamamoto, Y, Yamauchi, K, Yang, Z, Yasue, S, Yuan, AF, Yuda, T, Zhai, LM, Zhang, HM, Zhang, JL, Zhang, XY, Zhang, Y, Zhang, Y, Zhang, Y, Zhaxisangzhu & Zhou, XX 2015, 'The TIBET AS+MD project; progress report 2015', Unknown Journal, vol. 30-July-2015, 969.

@article{be013e16a102427a96b50c82c4948c52,

title = "The TIBET AS+MD project; progress report 2015",

abstract = "We plan to build a large (approximately 10,000 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 will make a progress report on the project, as some part of it started data-taking in 2014.",

author = "M. Amenomori and Bi, {X. J.} and D. Chen and Chen, {T. L.} and Chen, {W. Y.} and Cui, {S. W.} and Danzengluobu and Ding, {L. K.} and Feng, {C. F.} and Zhaoyang Feng and Feng, {Z. Y.} and Gou, {Q. B.} and Guo, {Y. Q.} and He, {H. H.} and He, {Z. T.} and K. Hibino and N. Hotta and Haibing Hu and Hu, {H. B.} and J. Huang and Jia, {H. Y.} and L. Jiang and F. Kajino and K. Kasahara and Y. Katayose and C. Kato and K. Kawata and M. Kozai and Labaciren and Le, {G. M.} and Li, {A. F.} and Li, {H. J.} and Li, {W. J.} and C. Liu and Liu, {J. S.} and Liu, {M. Y.} and H. Lu and Meng, {X. R.} and T. Miyazaki and K. Mizutani and K. Munakata and T. Nakajima and Y. Nakamura and H. Nanjo and M. Nishizawa and T. Niwa and M. Ohnishi and I. Ohta and Shunsuke Ozawa and Qian, {X. L.} and Qu, {X. B.} and T. Saito and Saito, {T. Y.} and M. Sakata and Sako, {T. K.} and J. Shao and M. Shibata and A. Shiomi and T. Shirai and H. Sugimoto and M. Takita and Tan, {Y. H.} and N. Tateyama and Shoji Torii and H. Tsuchiya and S. Udo and H. Wang and Wu, {H. R.} and L. Xue and Y. Yamamoto and K. Yamauchi and Z. Yang and S. Yasue and Yuan, {A. F.} and T. Yuda and Zhai, {L. M.} and Zhang, {H. M.} and Zhang, {J. L.} and Zhang, {X. Y.} and Y. Zhang and Yi Zhang and Ying Zhang and Zhaxisangzhu and Zhou, {X. X.}",

year = "2015",

language = "English",

volume = "30-July-2015",

journal = "Nuclear Physics A",

issn = "0375-9474",

publisher = "Elsevier",

}

TY - JOUR

T1 - The TIBET AS+MD project; progress report 2015

AU - Amenomori, M.

AU - Bi, X. J.

AU - Chen, D.

AU - Chen, T. L.

AU - Chen, W. Y.

AU - Cui, S. W.

AU - Danzengluobu,

AU - Ding, L. K.

AU - Feng, C. F.

AU - Feng, Zhaoyang

AU - Feng, Z. Y.

AU - Gou, Q. B.

AU - Guo, Y. Q.

AU - He, H. H.

AU - He, Z. T.

AU - Hibino, K.

AU - Hotta, N.

AU - Hu, Haibing

AU - Hu, H. B.

AU - Huang, J.

AU - Jia, H. Y.

AU - Jiang, L.

AU - Kajino, F.

AU - Kasahara, K.

AU - Katayose, Y.

AU - Kato, C.

AU - Kawata, K.

AU - Kozai, M.

AU - Labaciren,

AU - Le, G. M.

AU - Li, A. F.

AU - Li, H. J.

AU - Li, W. J.

AU - Liu, C.

AU - Liu, J. S.

AU - Liu, M. Y.

AU - Lu, H.

AU - Meng, X. R.

AU - Miyazaki, T.

AU - Mizutani, K.

AU - Munakata, K.

AU - Nakajima, T.

AU - Nakamura, Y.

AU - Nanjo, H.

AU - Nishizawa, M.

AU - Niwa, T.

AU - Ohnishi, M.

AU - Ohta, I.

AU - Ozawa, Shunsuke

AU - Qian, X. L.

AU - Qu, X. B.

AU - Saito, T.

AU - Saito, T. Y.

AU - Sakata, M.

AU - Sako, T. K.

AU - Shao, J.

AU - Shibata, M.

AU - Shiomi, A.

AU - Shirai, T.

AU - Sugimoto, H.

AU - Takita, M.

AU - Tan, Y. H.

AU - Tateyama, N.

AU - Torii, Shoji

AU - Tsuchiya, H.

AU - Udo, S.

AU - Wang, H.

AU - Wu, H. R.

AU - Xue, L.

AU - Yamamoto, Y.

AU - Yamauchi, K.

AU - Yang, Z.

AU - Yasue, S.

AU - Yuan, A. F.

AU - Yuda, T.

AU - Zhai, L. M.

AU - Zhang, H. M.

AU - Zhang, J. L.

AU - Zhang, X. Y.

AU - Zhang, Y.

AU - Zhang, Yi

AU - Zhang, Ying

AU - Zhaxisangzhu,

AU - Zhou, X. X.

PY - 2015

Y1 - 2015

N2 - We plan to build a large (approximately 10,000 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 will make a progress report on the project, as some part of it started data-taking in 2014.

AB - We plan to build a large (approximately 10,000 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 will make a progress report on the project, as some part of it started data-taking in 2014.

UR - http://www.scopus.com/inward/record.url?scp=84988700582&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84988700582&partnerID=8YFLogxK

M3 - Article

AN - SCOPUS:84988700582

VL - 30-July-2015

JO - Nuclear Physics A

JF - Nuclear Physics A

SN - 0375-9474

M1 - 969

ER -

The TIBET AS+MD project; progress report 2015

Abstract

ASJC Scopus subject areas

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