The TAIGA Experiment: From Cosmic Ray Physics to Gamma Astronomy in the Tunka Valley

Kalmykov, N.N.; Kozhin, V.A.; Korosteleva, E.E.; Kuzmichev, L.A.; Lubsandorzhiev, N.B.; Osipova, E.A.; Panasyuk, M.I.; Popova, E.G.; Postnikov, E.B.; Prosin, V.V.; Ptuskin, V.S.; Sveshnikova, L.G.; Silaev, A.A.; Silaev, A.A.; Skurikhin, A.V.; TAIGA, C.

Авторы: Kalmykov N.N., Kozhin V.A., Korosteleva E.E., Kuzmichev L.A., Lubsandorzhiev N.B., Osipova Eleonora A., Panasyuk M.I., Popova Elena G., Postnikov E.B., Prosin V.V., Ptuskin V.S., Sveshnikova L.G., Silaev A.A., Silaev Alexey A., Skurikhin A.V., TAIGA Collaboration
Журнал: Physics of Particles and Nuclei
Том: 49
Номер: 4
Год издания: 2018
Издательство: Pleiades Publishing, Inc.
Местоположение издательства: New York, USA
Первая страница: 589
Последняя страница: 598
DOI: 10.1134/s1063779618040172
Аннотация: The article presents the relevance and advantages of the new gamma observatory TAIGA (Tunka Advanced Instrument for cosmic ray physics and Gamma Astronomy), which is being constructed in the Tunka Valley 50 km from Lake Baikal. Various detectors of the six TAIGA gamma observatory arrays register the Cherenkov and radio radiation, as well as the electron and muon components of EAS. The primary objective of the TAIGA gamma observatory is to study the high-energy part of the gamma-ray spectrum, in particular, in order to search for Galactic PeVatrons. The energy, direction, and position of the EAS axis are reconstructed in the observatory based on the data of the wide-angle Cherenkov detectors of the TAIGA-HiSCORE experiment. Taking into account this information, the gamma quanta are distinguished from the hadron background using the data obtained by the muon detectors and telescopes that register the EAS image in the Cherenkov light. In this hybrid mode of operation, the atmospheric Cherenkov telescopes can operate in the mono-mode, and the distance between them can be increased to 800–1000 m, which makes it possible to construct an array with an area of 5 km^2 and more at relatively low cost and in a short time. By 2019, the first stage of the gamma observatory with an area of 1 km2 will be constructed; its expected integral sensitivity for detecting the gamma radiation with an energy of 100 TeV at observation of the source for 300 hours will be approximately 2.5×10^{–13} TeV cm^{–2}s^{–1}.
Добавил в систему: Постников Евгений Борисович

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The TAIGA Experiment: From Cosmic Ray Physics to Gamma Astronomy in the Tunka Valleyстатья

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