Underground water Cherenkov muon detector array with the Tibet air shower array for gamma-ray astronomy in the 100 TeV region

Amenomori, M.; Ayabe, S.; Bi, X. J.; Chen, D.; Cui, S. W.; Danzengluobu,; Ding, L. K.; Ding, X. H.; Feng, C.; Feng, Z.; Gao, X. Y.; Geng, Q. X.; Guo, H. W.; He, H. H.; He, M.; Hibino, K.; Hotta, N.; Hu, Haibing; 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.; Lü, H.; Lu, S. L.; Meng, X. R.; Mizutani, K.; Mu, J.; Munakata, K.; Nagai, A.; Nanjo, H.; Nakamura, Masaki; Ohnishi, M.; Ohta, I.; Onuma, H.; Ouchi, T.; Ozawa, S.; Ren, J. R.; Saito, T.; Sakata, M.; Sako, T. K.; Sasaki, Takashi; Shibata, M.; Shirai, T.; Sugimoto, H.; Takita, M.; Tan, Y. H.; Tateyama, N.; Torii, Shoji; 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, Xu

doi:10.1007/s10509-007-9395-x

Cited by 11 publications

(5 citation statements)

References 8 publications

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“…Although gamma-ray initiated showers produce nearly exclusively gamma-ray and e ± particles, in the case of hadron-induced showers, there is an additional component represented by muons, which are much more penetrative. Therefore, the inclusion of additional particle counters located under a natural, deep layer of absorbing material (typically earth or water) provides a measurement of the muon content of the shower, which can be used in the selection of gamma-ray showers [19].…”

Section: Sa and Wcd Techniquesmentioning

confidence: 99%

TeV Instrumentation: Current and Future

Sitarek

2022

Galaxies

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During the last 20 years, TeV astronomy has turned from a fledgling field, with only a handful of sources, into a fully-developed astronomy discipline, broadening our knowledge on a variety of types of TeV gamma-ray sources. This progress has been mainly achieved due to the currently operating instruments: imaging atmospheric Cherenkov telescopes, surface arrays and water Cherenkov detectors. Moreover, we are at the brink of a next generation of instruments, with a considerable leap in performance parameters. This review summarizes the current status of the TeV astronomy instrumentation, mainly focusing on the comparison of the different types of instruments and analysis challenges, as well as providing an outlook into the future installations. The capabilities and limitations of different techniques of observations of TeV gamma rays are discussed, as well as synergies to other bands and messengers.

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Section: Sa and Wcd Techniquesmentioning

confidence: 99%

TeV Instrumentation: Current and Future

Sitarek

2022

Galaxies

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“…While gammaray initiated showers produce nearly exclusively gamma-ray and e ± particles, in the case of hadron-induced shower there is an additional component from muons, that are much more penetrative. Therefore inclusion of additional particle counters located under a natural, deep layer of absorbing material (typically earth or water) provides a measurement of the muon content of the shower that can be used in selection of gamma-ray showers [19].…”

Section: Sa and Wcd Techniquementioning

confidence: 99%

TeV Instrumentation: current and future

Sitarek¹

2022

Preprint

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During the last 20 years, TeV astronomy turned from a fledgling field, with only a handful of sources into a fully-developed astronomy discipline, broadening our knowledge on a variety of types of TeV gamma-ray sources. This progress has been mainly achieved due to currently operating instruments: Imaging Atmospheric Cherenkov Telescopes, Surface Array and Water Cherenkov detectors. Moreover, we are at the brink of a next generation of instruments, with a considerable leap of performance parameters. This review summarises the current status of the TeV astronomy instrumentation, mainly focusing on the comparison of the different types of instruments and analysis challenges, as well as provides an outlook into the future installations. The capabilities and limitations of different techniques of observations of TeV gamma rays are discussed, as well as synergies to other bands and messengers.

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“…The polygonato parametrization (Hörandel, 2003) of the cosmic ray spectra for each nucleus-type was folded with the area corresponding to the closest nucleus out of the group of four simulated (proton, Helium, Nitrogen, Iron). The resulting point-source sensitivities for instrumented detector areas of 10 and 100 km 2 are shown in Figure 4 along with point-source sensitivities of other experiments CTA Consortium, 2010;Amenomori et al, 2007;HAWC collaboration, 2011), and an upper limit by KASKADE (Antoni et al, 2004). HiSCORE will be complementary to other instruments in different ways.…”

Section: Gamma-ray Sensitivitymentioning

confidence: 99%

The ground-based large-area wide-angle γ-ray and cosmic-ray experiment HiSCORE

Tluczykont

Hampf

Horns

et al. 2011

Advances in Space Research

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The question of the origin of cosmic rays and other questions of astroparticle and particle physics can be addressed with indirect air-shower observations above 10 TeV primary energy. We propose to explore the cosmic ray and γ-ray sky (accelerator sky) in the energy range from 10 TeV to 1 EeV with the new ground-based large-area wide angle (∆Ω ∼0.85 sterad) airshower detector HiSCORE (Hundred*i Square-km Cosmic ORigin Explorer). The HiSCORE detector is based on non-imaging air-shower Cherenkov light-front sampling using an array of light-collecting stations. A full detector simulation and basic reconstruction algorithms have been used to assess the performance of HiSCORE. First prototype studies for different hardware components of the detector array have been carried out. The resulting sensitivity of HiSCORE to γ-rays will be comparable to CTA at 50 TeV and will extend the sensitive energy range for γ-rays up to the PeV regime. HiSCORE will also be sensitive to charged cosmic rays between 100 TeV and 1 EeV.

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Underground water Cherenkov muon detector array with the Tibet air shower array for gamma-ray astronomy in the 100 TeV region

Cited by 11 publications

References 8 publications

TeV Instrumentation: Current and Future

TeV Instrumentation: Current and Future

TeV Instrumentation: current and future

The ground-based large-area wide-angle γ-ray and cosmic-ray experiment HiSCORE

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