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Cherenkov EAS arrays in the Tunka astrophysical center: From Tunka-133 to the TAIGA gamma and cosmic ray hybrid detector

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dc.contributor.authorKuzmichev, L.
dc.contributor.authorBezyazeekov, P.
dc.contributor.authorBorodin, A.
dc.contributor.authorBruckner, M.
dc.contributor.authorAstapov, I.
dc.contributor.authorKindin, V.
dc.contributor.authorKokoulin, R.
dc.contributor.authorKompaniets, K.
dc.contributor.authorPetrukhin, A.
dc.contributor.authorYashin, I.
dc.contributor.authorАстапов, Иван Иванович
dc.contributor.authorКиндин, Виктор Владимирович
dc.contributor.authorКокоулин, Ростислав Павлович
dc.contributor.authorКомпаниец, Константин Георгиевич
dc.contributor.authorПетрухин, Анатолий Афанасьевич
dc.contributor.authorЯшин, Игорь Иванович
dc.date.accessioned2024-11-25T14:40:27Z
dc.date.available2024-11-25T14:40:27Z
dc.date.issued2020
dc.description.abstract© 2019 Elsevier B.V. One of the most informative methods of cosmic ray studies is the detection of Cherenkov light from extensive air showers (EAS). The primary energy reconstruction is possible by using the Earth's atmosphere as a huge calorimeter. The EAS Cherenkov light array Tunka-133, with ∼3 km2 geometrical area, is taking data since 2009. Tunka-133 is located in the Tunka Astrophysical Center at ∼50 km west of Lake Baikal. This array allows us to perform a detailed study of the energy spectrum and the mass composition in the energy range from 6⋅1015eV to 1018eV. Most of the ongoing efforts are focused on the construction of the first stage of the detector TAIGA (Tunka Advanced Instrument for cosmic ray physics and Gamma Astronomy). The latter is designed for the study of gamma rays and charged cosmic rays in the energy range of 1013eV–1018eV. The TAIGA prototype will consist of ∼100 wide angle timing Cherenkov stations (TAIGA-HiSCORE) and three IACTs deployed over an area of ∼1 km2. The installation of the array is planned to be finished in 2019 while the data-taking can start already during the commissioning phase. The joint reconstruction of energy, direction, and core position of the imaging and non-imaging detectors will allow us to increase the distance between the IACTs up to 800 m, therefore providing a low-cost, highly sensitive detector. The relatively low cost together with the high sensitivity for energies ≥30–50 TeV make this pioneering technique very attractive for exploring galactic PeVatrons and cosmic rays. In addition to the Cherenkov light detectors we intend to deploy surface and underground muon detectors over an area of 1 km2 with a total area of about 1000 m2. The results of the first season of coincident operation of the first ∼4 m diameter IACT with an aperture of ∼10°with 30 stations of TAIGA-HiSCORE will be presented.
dc.identifier.citationCherenkov EAS arrays in the Tunka astrophysical center: From Tunka-133 to the TAIGA gamma and cosmic ray hybrid detector / Kuzmichev, L. [et al.] // Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment. - 2020. - 952. - 10.1016/j.nima.2019.01.056
dc.identifier.doi10.1016/j.nima.2019.01.056
dc.identifier.urihttps://www.doi.org/10.1016/j.nima.2019.01.056
dc.identifier.urihttps://www.scopus.com/record/display.uri?eid=2-s2.0-85060671031&origin=resultslist
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dc.identifier.urihttps://openrepository.mephi.ru/handle/123456789/19971
dc.relation.ispartofNuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment
dc.titleCherenkov EAS arrays in the Tunka astrophysical center: From Tunka-133 to the TAIGA gamma and cosmic ray hybrid detector
dc.typeArticle
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oaire.citation.volume952
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