The TIBET AS+MD Project; progress report 2013

THE TIBET ASγ COLLABORATION

Research output: Chapter in Book/Report/Conference proceedingConference contribution

Abstract

We plan to build a large (approximately 10,000 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. The 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 the number of muons in an air shower by the muon detector array. We will make a progress report on the project, as 5/12 of it is under construction now.

Original languageEnglish
Title of host publicationProceedings of the 33rd International Cosmic Rays Conference, ICRC 2013
PublisherSociedade Brasileira de Fisica
Volume2013-October
ISBN (Electronic)9788589064293
Publication statusPublished - 2013 Jan 1
Event33rd International Cosmic Rays Conference, ICRC 2013 - Rio de Janeiro, Brazil
Duration: 2013 Jul 22013 Jul 9

Other

Other33rd International Cosmic Rays Conference, ICRC 2013
CountryBrazil
CityRio de Janeiro
Period13/7/213/7/9

Fingerprint

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

Keywords

  • Cosmic rays
  • Gamma rays
  • Muon
  • Tibet
  • Water Cherenkov

ASJC Scopus subject areas

  • Nuclear and High Energy Physics

Cite this

THE TIBET ASγ COLLABORATION (2013). The TIBET AS+MD Project; progress report 2013. In Proceedings of the 33rd International Cosmic Rays Conference, ICRC 2013 (Vol. 2013-October). Sociedade Brasileira de Fisica.

The TIBET AS+MD Project; progress report 2013. / THE TIBET ASγ COLLABORATION.

Proceedings of the 33rd International Cosmic Rays Conference, ICRC 2013. Vol. 2013-October Sociedade Brasileira de Fisica, 2013.

Research output: Chapter in Book/Report/Conference proceedingConference contribution

THE TIBET ASγ COLLABORATION 2013, The TIBET AS+MD Project; progress report 2013. in Proceedings of the 33rd International Cosmic Rays Conference, ICRC 2013. vol. 2013-October, Sociedade Brasileira de Fisica, 33rd International Cosmic Rays Conference, ICRC 2013, Rio de Janeiro, Brazil, 13/7/2.
THE TIBET ASγ COLLABORATION. The TIBET AS+MD Project; progress report 2013. In Proceedings of the 33rd International Cosmic Rays Conference, ICRC 2013. Vol. 2013-October. Sociedade Brasileira de Fisica. 2013
THE TIBET ASγ COLLABORATION. / The TIBET AS+MD Project; progress report 2013. Proceedings of the 33rd International Cosmic Rays Conference, ICRC 2013. Vol. 2013-October Sociedade Brasileira de Fisica, 2013.
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abstract = "We plan to build a large (approximately 10,000 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. The 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 the number of muons in an air shower by the muon detector array. We will make a progress report on the project, as 5/12 of it is under construction now.",
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author = "{THE TIBET ASγ COLLABORATION} 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 K. Mizutani and K. Munakata and H. Nanjo and M. Nishizawa 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 Shoji Torii",
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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 - Mizutani, K.

AU - Munakata, K.

AU - Nanjo, H.

AU - Nishizawa, M.

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 - Torii, Shoji

PY - 2013/1/1

Y1 - 2013/1/1

N2 - We plan to build a large (approximately 10,000 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. The 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 the number of muons in an air shower by the muon detector array. We will make a progress report on the project, as 5/12 of it is under construction now.

AB - We plan to build a large (approximately 10,000 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. The 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 the number of muons in an air shower by the muon detector array. We will make a progress report on the project, as 5/12 of it is under construction now.

KW - Cosmic rays

KW - Gamma rays

KW - Muon

KW - Tibet

KW - Water Cherenkov

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M3 - Conference contribution

AN - SCOPUS:85052403165

VL - 2013-October

BT - Proceedings of the 33rd International Cosmic Rays Conference, ICRC 2013

PB - Sociedade Brasileira de Fisica

ER -