The tibet AS+MD project; status report 2017

Tibet ASγCollaboration

研究成果: Conference article

抄録

We built a large (approximately 4,000 m2) 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.

元の言語English
ジャーナルProceedings of Science
出版物ステータスPublished - 2017 1 1
イベント35th International Cosmic Ray Conference, ICRC 2017 - Bexco, Busan, Korea, Republic of
継続期間: 2017 7 102017 7 20

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Tibet
muons
cosmic ray showers
cosmic rays
gamma rays
detectors
sea level
field of view
counting
accelerators
galaxies
water

ASJC Scopus subject areas

  • General

これを引用

The tibet AS+MD project; status report 2017. / Tibet ASγCollaboration.

:: Proceedings of Science, 01.01.2017.

研究成果: Conference article

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title = "The tibet AS+MD project; status report 2017",
abstract = "We built a large (approximately 4,000 m2) 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.",
author = "{Tibet ASγCollaboration} and 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 Shoji Torii",
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T1 - The tibet AS+MD project; status report 2017

AU - Tibet ASγCollaboration

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 - Torii, Shoji

PY - 2017/1/1

Y1 - 2017/1/1

N2 - We built a large (approximately 4,000 m2) 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.

AB - We built a large (approximately 4,000 m2) 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.

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M3 - Conference article

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JO - Proceedings of Science

JF - Proceedings of Science

SN - 1824-8039

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