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

In: Physics of Particles and Nuclei, Vol. 49, No. 4, 01.07.2018, p. 589-598.

Research output: Contribution to journal › Article › peer-review

Harvard

the TAIGA Collaboration 2018, 'The TAIGA Experiment: From Cosmic Ray Physics to Gamma Astronomy in the Tunka Valley', Physics of Particles and Nuclei, vol. 49, no. 4, pp. 589-598. https://doi.org/10.1134/S1063779618040172

APA

the TAIGA Collaboration (2018). The TAIGA Experiment: From Cosmic Ray Physics to Gamma Astronomy in the Tunka Valley. Physics of Particles and Nuclei, 49(4), 589-598. https://doi.org/10.1134/S1063779618040172

Vancouver

the TAIGA Collaboration. The TAIGA Experiment: From Cosmic Ray Physics to Gamma Astronomy in the Tunka Valley. Physics of Particles and Nuclei. 2018 Jul 1;49(4):589-598. doi: 10.1134/S1063779618040172

Author

the TAIGA Collaboration. / The TAIGA Experiment : From Cosmic Ray Physics to Gamma Astronomy in the Tunka Valley. In: Physics of Particles and Nuclei. 2018 ; Vol. 49, No. 4. pp. 589-598.

BibTeX

@article{72257c53a6f740b9bd65f75992206133,
title = "The TAIGA Experiment: From Cosmic Ray Physics to Gamma Astronomy in the Tunka Valley",
abstract = "Abstract: 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 km2 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–2s–1.",
keywords = "ARRAY",
author = "{the TAIGA Collaboration} and Budnev, {N. M.} and Astapov, {I. I.} and Bezyazeekov, {P. A.} and Boreyko, {A. V.} and Borodin, {A. N.} and Garmash, {A. Yu} and Gafarov, {A. R.} and Gorbunov, {N. V.} and Grebenyuk, {V. M.} and Gress, {O. A.} and Gress, {T. I.} and Grinyuk, {A. A.} and Grishin, {O. G.} and Dyachok, {A. N.} and Zhurov, {D. P.} and Zagorodnikov, {A. V.} and Zurbanov, {V. L.} and Ivanova, {A. L.} and Kazarina, {Yu A.} and Kalmykov, {N. N.} and Kindin, {V. V.} and Kirilenko, {P. S.} and Kiryuhin, {S. N.} and Kozhin, {V. A.} and Kokoulin, {R. P.} and Kompaniets, {K. G.} and Korosteleva, {E. E.} and Kostunin, {D. G.} and Kravchenko, {E. I.} and Kuzmichev, {L. A.} and Lemeshev, {Yu E.} and Lenok, {V. V.} and Lubsandorzhiev, {B. K.} and Lubsandorzhiev, {N. B.} and Mirgazov, {R. R.} and R. Mirzoyan and Monkhoev, {R. D.} and Osipova, {E. A.} and Panasyuk, {M. I.} and Pankov, {L. V.} and Pakhorukov, {A. L.} and Petrukhin, {A. A.} and Poleschuk, {V. A.} and Popova, {E. G.} and Postnikov, {E. B.} and Prosin, {V. V.} and Ptuskin, {V. S.} and Pushnin, {A. A.} and Rubtsov, {G. I.} and Sokolov, {A. V.}",
year = "2018",
month = jul,
day = "1",
doi = "10.1134/S1063779618040172",
language = "English",
volume = "49",
pages = "589--598",
journal = "Physics of Particles and Nuclei",
issn = "1063-7796",
publisher = "Maik Nauka-Interperiodica Publishing",
number = "4",

}

RIS

TY - JOUR

T1 - The TAIGA Experiment

T2 - From Cosmic Ray Physics to Gamma Astronomy in the Tunka Valley

AU - the TAIGA Collaboration

AU - Budnev, N. M.

AU - Astapov, I. I.

AU - Bezyazeekov, P. A.

AU - Boreyko, A. V.

AU - Borodin, A. N.

AU - Garmash, A. Yu

AU - Gafarov, A. R.

AU - Gorbunov, N. V.

AU - Grebenyuk, V. M.

AU - Gress, O. A.

AU - Gress, T. I.

AU - Grinyuk, A. A.

AU - Grishin, O. G.

AU - Dyachok, A. N.

AU - Zhurov, D. P.

AU - Zagorodnikov, A. V.

AU - Zurbanov, V. L.

AU - Ivanova, A. L.

AU - Kazarina, Yu A.

AU - Kalmykov, N. N.

AU - Kindin, V. V.

AU - Kirilenko, P. S.

AU - Kiryuhin, S. N.

AU - Kozhin, V. A.

AU - Kokoulin, R. P.

AU - Kompaniets, K. G.

AU - Korosteleva, E. E.

AU - Kostunin, D. G.

AU - Kravchenko, E. I.

AU - Kuzmichev, L. A.

AU - Lemeshev, Yu E.

AU - Lenok, V. V.

AU - Lubsandorzhiev, B. K.

AU - Lubsandorzhiev, N. B.

AU - Mirgazov, R. R.

AU - Mirzoyan, R.

AU - Monkhoev, R. D.

AU - Osipova, E. A.

AU - Panasyuk, M. I.

AU - Pankov, L. V.

AU - Pakhorukov, A. L.

AU - Petrukhin, A. A.

AU - Poleschuk, V. A.

AU - Popova, E. G.

AU - Postnikov, E. B.

AU - Prosin, V. V.

AU - Ptuskin, V. S.

AU - Pushnin, A. A.

AU - Rubtsov, G. I.

AU - Sokolov, A. V.

PY - 2018/7/1

Y1 - 2018/7/1

N2 - Abstract: 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 km2 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–2s–1.

AB - Abstract: 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 km2 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–2s–1.

KW - ARRAY

UR - http://www.scopus.com/inward/record.url?scp=85049861557&partnerID=8YFLogxK

U2 - 10.1134/S1063779618040172

DO - 10.1134/S1063779618040172

M3 - Article

AN - SCOPUS:85049861557

VL - 49

SP - 589

EP - 598

JO - Physics of Particles and Nuclei

JF - Physics of Particles and Nuclei

SN - 1063-7796

IS - 4

ER -

ID: 14709466