Underground water Cherenkov muon detector array with the Tibet air shower array for gamma-ray astronomy in the 100 TeV region
Issue Title: The Multi-Messenger Approach to High-Energy Gamma-Ray Sources: Third Workshop on the Nature of Unidentified High-Energy Sources We propose to build a large water-Cherenkov-type muon-detector array (Tibet MD array) around the 37000 m^sup 2^ Tibet air shower array (Tibet AS array) already...
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| Veröffentlicht in: | Astrophysics and space science 2007-06, Vol.309 (1-4), p.435-439 |
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| creator | Amenomori, M. Ayabe, S. Bi, X. J. Chen, D. Cui, S. W. Danzengluobu Ding, L. K. Ding, X. H. Feng, C. F. Feng, Zhaoyang Feng, Z. Y. Gao, X. Y. Geng, Q. X. Guo, H. W. He, H. H. He, M. Hibino, K. Hotta, N. Hu, Haibing Hu, H. B. Huang, J. Huang, Q. Jia, H. Y. Kajino, F. Kasahara, K. Katayose, Y. Kato, C. Kawata, K. Labaciren Le, G. M. Li, A. F. Li, J. Y. Lu, H. Lu, S. L. Meng, X. R. Mizutani, K. Mu, J. Munakata, K. Nagai, A. Nanjo, H. Nishizawa, M. Ohnishi, M. Ohta, I. Onuma, H. Ouchi, T. Ozawa, S. Ren, J. R. Saito, T. Saito, T. Y. Sakata, M. Sako, T. K. Sasaki, T. Shibata, M. Shiomi, A. Shirai, T. Sugimoto, H. Takita, M. Tan, Y. H. Tateyama, N. Torii, S. Tsuchiya, H. Udo, S. Wang, B. Wang, H. Wang, X. Wang, Y. G. Wu, H. R. Xue, L. Yamamoto, Y. Yan, C. T. Yang, X. C. Yasue, S. Ye, Z. H. Yu, G. C. Yuan, A. F. Yuda, T. Zhang, H. M. Zhang, J. L. Zhang, N. J. Zhang, X. Y. Zhang, Y. Zhang, Yi Zhaxisangzhu Zhou, X. X. |
| description | Issue Title: The Multi-Messenger Approach to High-Energy Gamma-Ray Sources: Third Workshop on the Nature of Unidentified High-Energy Sources We propose to build a large water-Cherenkov-type muon-detector array (Tibet MD array) around the 37000 m^sup 2^ Tibet air shower array (Tibet AS array) already constructed at 4300 m above sea level in Tibet, China. Each muon detector is a waterproof concrete pool, 6 m wide × 6 m long × 1.5 m deep in size, equipped with a 20 inch-in-diameter PMT. The Tibet MD array consists of 240 muon detectors set up 2.5 m underground. Its total effective area will be 8640 m^sup 2^ for muon detection. The Tibet MD array will significantly improve gamma-ray sensitivity of the Tibet AS array in the 100 TeV region (10-1000 TeV) by means of gamma/hadron separation based on counting the number of muons accompanying an air shower. The Tibet AS+MD array will have the sensitivity to gamma rays in the 100 TeV region by an order of magnitude better than any other previous existing detectors in the world. [PUBLICATION ABSTRACT] |
| doi_str_mv | 10.1007/s10509-007-9395-x |
| format | Article |
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J. ; Chen, D. ; Cui, S. W. ; Danzengluobu ; Ding, L. K. ; Ding, X. H. ; Feng, C. F. ; Feng, Zhaoyang ; Feng, Z. Y. ; Gao, X. Y. ; Geng, Q. X. ; Guo, H. W. ; He, H. H. ; He, M. ; Hibino, K. ; Hotta, N. ; Hu, Haibing ; Hu, H. B. ; Huang, J. ; Huang, Q. ; Jia, H. Y. ; Kajino, F. ; Kasahara, K. ; Katayose, Y. ; Kato, C. ; Kawata, K. ; Labaciren ; Le, G. M. ; Li, A. F. ; Li, J. Y. ; Lu, H. ; Lu, S. L. ; Meng, X. R. ; Mizutani, K. ; Mu, J. ; Munakata, K. ; Nagai, A. ; Nanjo, H. ; Nishizawa, M. ; Ohnishi, M. ; Ohta, I. ; Onuma, H. ; Ouchi, T. ; Ozawa, S. ; Ren, J. R. ; Saito, T. ; Saito, T. Y. ; Sakata, M. ; Sako, T. K. ; Sasaki, T. ; Shibata, M. ; Shiomi, A. ; Shirai, T. ; Sugimoto, H. ; Takita, M. ; Tan, Y. H. ; Tateyama, N. ; Torii, S. ; Tsuchiya, H. ; Udo, S. ; Wang, B. ; Wang, H. ; Wang, X. ; Wang, Y. G. ; Wu, H. R. ; Xue, L. ; Yamamoto, Y. ; Yan, C. T. ; Yang, X. C. ; Yasue, S. ; Ye, Z. H. ; Yu, G. C. ; Yuan, A. F. ; Yuda, T. ; Zhang, H. M. ; Zhang, J. L. ; Zhang, N. J. ; Zhang, X. Y. ; Zhang, Y. ; Zhang, Yi ; Zhaxisangzhu ; Zhou, X. X.</creator><creatorcontrib>Amenomori, M. ; Ayabe, S. ; Bi, X. J. ; Chen, D. ; Cui, S. W. ; Danzengluobu ; Ding, L. K. ; Ding, X. H. ; Feng, C. F. ; Feng, Zhaoyang ; Feng, Z. Y. ; Gao, X. Y. ; Geng, Q. X. ; Guo, H. W. ; He, H. H. ; He, M. ; Hibino, K. ; Hotta, N. ; Hu, Haibing ; Hu, H. B. ; Huang, J. ; Huang, Q. ; Jia, H. Y. ; Kajino, F. ; Kasahara, K. ; Katayose, Y. ; Kato, C. ; Kawata, K. ; Labaciren ; Le, G. M. ; Li, A. F. ; Li, J. Y. ; Lu, H. ; Lu, S. L. ; Meng, X. R. ; Mizutani, K. ; Mu, J. ; Munakata, K. ; Nagai, A. ; Nanjo, H. ; Nishizawa, M. ; Ohnishi, M. ; Ohta, I. ; Onuma, H. ; Ouchi, T. ; Ozawa, S. ; Ren, J. R. ; Saito, T. ; Saito, T. Y. ; Sakata, M. ; Sako, T. K. ; Sasaki, T. ; Shibata, M. ; Shiomi, A. ; Shirai, T. ; Sugimoto, H. ; Takita, M. ; Tan, Y. H. ; Tateyama, N. ; Torii, S. ; Tsuchiya, H. ; Udo, S. ; Wang, B. ; Wang, H. ; Wang, X. ; Wang, Y. G. ; Wu, H. R. ; Xue, L. ; Yamamoto, Y. ; Yan, C. T. ; Yang, X. C. ; Yasue, S. ; Ye, Z. H. ; Yu, G. C. ; Yuan, A. F. ; Yuda, T. ; Zhang, H. M. ; Zhang, J. L. ; Zhang, N. J. ; Zhang, X. Y. ; Zhang, Y. ; Zhang, Yi ; Zhaxisangzhu ; Zhou, X. X.</creatorcontrib><description>Issue Title: The Multi-Messenger Approach to High-Energy Gamma-Ray Sources: Third Workshop on the Nature of Unidentified High-Energy Sources We propose to build a large water-Cherenkov-type muon-detector array (Tibet MD array) around the 37000 m^sup 2^ Tibet air shower array (Tibet AS array) already constructed at 4300 m above sea level in Tibet, China. Each muon detector is a waterproof concrete pool, 6 m wide × 6 m long × 1.5 m deep in size, equipped with a 20 inch-in-diameter PMT. The Tibet MD array consists of 240 muon detectors set up 2.5 m underground. Its total effective area will be 8640 m^sup 2^ for muon detection. The Tibet MD array will significantly improve gamma-ray sensitivity of the Tibet AS array in the 100 TeV region (10-1000 TeV) by means of gamma/hadron separation based on counting the number of muons accompanying an air shower. The Tibet AS+MD array will have the sensitivity to gamma rays in the 100 TeV region by an order of magnitude better than any other previous existing detectors in the world. 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H.</creatorcontrib><creatorcontrib>Tateyama, N.</creatorcontrib><creatorcontrib>Torii, S.</creatorcontrib><creatorcontrib>Tsuchiya, H.</creatorcontrib><creatorcontrib>Udo, S.</creatorcontrib><creatorcontrib>Wang, B.</creatorcontrib><creatorcontrib>Wang, H.</creatorcontrib><creatorcontrib>Wang, X.</creatorcontrib><creatorcontrib>Wang, Y. G.</creatorcontrib><creatorcontrib>Wu, H. R.</creatorcontrib><creatorcontrib>Xue, L.</creatorcontrib><creatorcontrib>Yamamoto, Y.</creatorcontrib><creatorcontrib>Yan, C. T.</creatorcontrib><creatorcontrib>Yang, X. C.</creatorcontrib><creatorcontrib>Yasue, S.</creatorcontrib><creatorcontrib>Ye, Z. H.</creatorcontrib><creatorcontrib>Yu, G. C.</creatorcontrib><creatorcontrib>Yuan, A. F.</creatorcontrib><creatorcontrib>Yuda, T.</creatorcontrib><creatorcontrib>Zhang, H. M.</creatorcontrib><creatorcontrib>Zhang, J. L.</creatorcontrib><creatorcontrib>Zhang, N. J.</creatorcontrib><creatorcontrib>Zhang, X. Y.</creatorcontrib><creatorcontrib>Zhang, Y.</creatorcontrib><creatorcontrib>Zhang, Yi</creatorcontrib><creatorcontrib>Zhaxisangzhu</creatorcontrib><creatorcontrib>Zhou, X. X.</creatorcontrib><title>Underground water Cherenkov muon detector array with the Tibet air shower array for gamma-ray astronomy in the 100 TeV region</title><title>Astrophysics and space science</title><description>Issue Title: The Multi-Messenger Approach to High-Energy Gamma-Ray Sources: Third Workshop on the Nature of Unidentified High-Energy Sources We propose to build a large water-Cherenkov-type muon-detector array (Tibet MD array) around the 37000 m^sup 2^ Tibet air shower array (Tibet AS array) already constructed at 4300 m above sea level in Tibet, China. Each muon detector is a waterproof concrete pool, 6 m wide × 6 m long × 1.5 m deep in size, equipped with a 20 inch-in-diameter PMT. The Tibet MD array consists of 240 muon detectors set up 2.5 m underground. Its total effective area will be 8640 m^sup 2^ for muon detection. The Tibet MD array will significantly improve gamma-ray sensitivity of the Tibet AS array in the 100 TeV region (10-1000 TeV) by means of gamma/hadron separation based on counting the number of muons accompanying an air shower. The Tibet AS+MD array will have the sensitivity to gamma rays in the 100 TeV region by an order of magnitude better than any other previous existing detectors in the world. [PUBLICATION ABSTRACT]</description><subject>Astronomy</subject><subject>Astrophysics</subject><subject>Atoms & subatomic particles</subject><subject>Energy sources</subject><subject>Gamma rays</subject><issn>0004-640X</issn><issn>1572-946X</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2007</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GNUQQ</sourceid><recordid>eNpdkTtPAzEQhC0EEiHwA-gsGirD-l4-lyjiJUWiSVA6y-fbJBdyNtg-khT8dy4EGqqd0X67GmkIueRwwwHEbeCQg2S9ZDKVOdsekQHPRcJkVsyOyQAAMlZkMDslZyGseisLKQbka2pr9AvvOlvTjY7o6WiJHu2b-6Rt5yytMaKJzlPtvd7RTROXNC6RTpoKI9WNp2HpNvi3n_fkQretZnunQ_TOunZHG_tz1YelE3ylHheNs-fkZK7XAS9-55BMH-4noyc2fnl8Ht2NmUkhiyzN01JglUFRmkpyWc5zSIDzilcyFVxmCHVhjBRaaii0kcaIrMxKiYnBCng6JNeHv-_efXQYomqbYHC91hZdF1QJIhFJXhQ9efWPXLnO2z6cEnkfXooy6SF-gIx3IXicq3fftNrvFAe1r0Md6lB7ua9DbdNvNjl-Qw</recordid><startdate>200706</startdate><enddate>200706</enddate><creator>Amenomori, M.</creator><creator>Ayabe, S.</creator><creator>Bi, X. 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Y. ; Gao, X. Y. ; Geng, Q. X. ; Guo, H. W. ; He, H. H. ; He, M. ; Hibino, K. ; Hotta, N. ; Hu, Haibing ; Hu, H. B. ; Huang, J. ; Huang, Q. ; Jia, H. Y. ; Kajino, F. ; Kasahara, K. ; Katayose, Y. ; Kato, C. ; Kawata, K. ; Labaciren ; Le, G. M. ; Li, A. F. ; Li, J. Y. ; Lu, H. ; Lu, S. L. ; Meng, X. R. ; Mizutani, K. ; Mu, J. ; Munakata, K. ; Nagai, A. ; Nanjo, H. ; Nishizawa, M. ; Ohnishi, M. ; Ohta, I. ; Onuma, H. ; Ouchi, T. ; Ozawa, S. ; Ren, J. R. ; Saito, T. ; Saito, T. Y. ; Sakata, M. ; Sako, T. K. ; Sasaki, T. ; Shibata, M. ; Shiomi, A. ; Shirai, T. ; Sugimoto, H. ; Takita, M. ; Tan, Y. H. ; Tateyama, N. ; Torii, S. ; Tsuchiya, H. ; Udo, S. ; Wang, B. ; Wang, H. ; Wang, X. ; Wang, Y. G. ; Wu, H. R. ; Xue, L. ; Yamamoto, Y. ; Yan, C. T. ; Yang, X. C. ; Yasue, S. ; Ye, Z. H. ; Yu, G. C. ; Yuan, A. F. ; Yuda, T. ; Zhang, H. M. ; Zhang, J. L. ; Zhang, N. J. ; Zhang, X. Y. ; Zhang, Y. ; Zhang, Yi ; Zhaxisangzhu ; Zhou, X. 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X.</creatorcontrib><collection>CrossRef</collection><collection>ProQuest Central (Corporate)</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>ProQuest Central (purchase pre-March 2016)</collection><collection>Science Database (Alumni Edition)</collection><collection>Technology Research Database</collection><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>ProQuest Central (Alumni) (purchase pre-March 2016)</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest One Sustainability</collection><collection>ProQuest Central UK/Ireland</collection><collection>Advanced Technologies & Aerospace Collection</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>ProQuest Central Student</collection><collection>Aerospace Database</collection><collection>SciTech Premium Collection</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Science Database</collection><collection>Advanced Technologies & Aerospace Database</collection><collection>ProQuest Advanced Technologies & Aerospace Collection</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central Basic</collection><jtitle>Astrophysics and space science</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Amenomori, M.</au><au>Ayabe, S.</au><au>Bi, X. J.</au><au>Chen, D.</au><au>Cui, S. W.</au><au>Danzengluobu</au><au>Ding, L. K.</au><au>Ding, X. H.</au><au>Feng, C. F.</au><au>Feng, Zhaoyang</au><au>Feng, Z. Y.</au><au>Gao, X. Y.</au><au>Geng, Q. X.</au><au>Guo, H. W.</au><au>He, H. H.</au><au>He, M.</au><au>Hibino, K.</au><au>Hotta, N.</au><au>Hu, Haibing</au><au>Hu, H. B.</au><au>Huang, J.</au><au>Huang, Q.</au><au>Jia, H. Y.</au><au>Kajino, F.</au><au>Kasahara, K.</au><au>Katayose, Y.</au><au>Kato, C.</au><au>Kawata, K.</au><au>Labaciren</au><au>Le, G. M.</au><au>Li, A. F.</au><au>Li, J. Y.</au><au>Lu, H.</au><au>Lu, S. L.</au><au>Meng, X. R.</au><au>Mizutani, K.</au><au>Mu, J.</au><au>Munakata, K.</au><au>Nagai, A.</au><au>Nanjo, H.</au><au>Nishizawa, M.</au><au>Ohnishi, M.</au><au>Ohta, I.</au><au>Onuma, H.</au><au>Ouchi, T.</au><au>Ozawa, S.</au><au>Ren, J. R.</au><au>Saito, T.</au><au>Saito, T. Y.</au><au>Sakata, M.</au><au>Sako, T. K.</au><au>Sasaki, T.</au><au>Shibata, M.</au><au>Shiomi, A.</au><au>Shirai, T.</au><au>Sugimoto, H.</au><au>Takita, M.</au><au>Tan, Y. H.</au><au>Tateyama, N.</au><au>Torii, S.</au><au>Tsuchiya, H.</au><au>Udo, S.</au><au>Wang, B.</au><au>Wang, H.</au><au>Wang, X.</au><au>Wang, Y. G.</au><au>Wu, H. R.</au><au>Xue, L.</au><au>Yamamoto, Y.</au><au>Yan, C. T.</au><au>Yang, X. C.</au><au>Yasue, S.</au><au>Ye, Z. H.</au><au>Yu, G. C.</au><au>Yuan, A. F.</au><au>Yuda, T.</au><au>Zhang, H. M.</au><au>Zhang, J. L.</au><au>Zhang, N. J.</au><au>Zhang, X. Y.</au><au>Zhang, Y.</au><au>Zhang, Yi</au><au>Zhaxisangzhu</au><au>Zhou, X. X.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Underground water Cherenkov muon detector array with the Tibet air shower array for gamma-ray astronomy in the 100 TeV region</atitle><jtitle>Astrophysics and space science</jtitle><date>2007-06</date><risdate>2007</risdate><volume>309</volume><issue>1-4</issue><spage>435</spage><epage>439</epage><pages>435-439</pages><issn>0004-640X</issn><eissn>1572-946X</eissn><abstract>Issue Title: The Multi-Messenger Approach to High-Energy Gamma-Ray Sources: Third Workshop on the Nature of Unidentified High-Energy Sources We propose to build a large water-Cherenkov-type muon-detector array (Tibet MD array) around the 37000 m^sup 2^ Tibet air shower array (Tibet AS array) already constructed at 4300 m above sea level in Tibet, China. Each muon detector is a waterproof concrete pool, 6 m wide × 6 m long × 1.5 m deep in size, equipped with a 20 inch-in-diameter PMT. The Tibet MD array consists of 240 muon detectors set up 2.5 m underground. Its total effective area will be 8640 m^sup 2^ for muon detection. The Tibet MD array will significantly improve gamma-ray sensitivity of the Tibet AS array in the 100 TeV region (10-1000 TeV) by means of gamma/hadron separation based on counting the number of muons accompanying an air shower. The Tibet AS+MD array will have the sensitivity to gamma rays in the 100 TeV region by an order of magnitude better than any other previous existing detectors in the world. [PUBLICATION ABSTRACT]</abstract><cop>Dordrecht</cop><pub>Springer Nature B.V</pub><doi>10.1007/s10509-007-9395-x</doi><tpages>5</tpages></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0004-640X |
| ispartof | Astrophysics and space science, 2007-06, Vol.309 (1-4), p.435-439 |
| issn | 0004-640X 1572-946X |
| language | eng |
| recordid | cdi_proquest_miscellaneous_807272566 |
| source | Springer Nature - Complete Springer Journals |
| subjects | Astronomy Astrophysics Atoms & subatomic particles Energy sources Gamma rays |
| title | Underground water Cherenkov muon detector array with the Tibet air shower array for gamma-ray astronomy in the 100 TeV region |
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