Выдержка

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 km 2 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⋅10 15 eV to 10 18 eV. 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 10 13 eV–10 18 eV. The TAIGA prototype will consist of ∼100 wide angle timing Cherenkov stations (TAIGA-HiSCORE) and three IACTs deployed over an area of ∼1 km 2 . 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 km 2 with a total area of about 1000 m 2 . 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.

Язык оригиналаанглийский
Номер статьи161830
Число страниц4
ЖурналNuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment
Том952
DOI
СостояниеОпубликовано - 1 фев 2020

Отпечаток

Cosmic rays
cosmic ray showers
Gamma rays
cosmic rays
astrophysics
gamma rays
Detectors
detectors
Air
stations
Earth atmosphere
energy
Astronomy
Photodetectors
Calorimeters
Lakes
Costs
astronomy
lakes
Physics

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@article{a4019c8a12fd42478f68e862092348a4,
title = "Cherenkov EAS arrays in the Tunka astrophysical center: From Tunka-133 to the TAIGA gamma and cosmic ray hybrid detector",
abstract = "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 km 2 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⋅10 15 eV to 10 18 eV. 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 10 13 eV–10 18 eV. The TAIGA prototype will consist of ∼100 wide angle timing Cherenkov stations (TAIGA-HiSCORE) and three IACTs deployed over an area of ∼1 km 2 . 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 km 2 with a total area of about 1000 m 2 . 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.",
keywords = "Cosmic rays, EAS Cherenkov light array, Energy spectrum, Gamma-ray astronomy, IACT",
author = "{TAIGA Collaboration} and L. Kuzmichev and I. Astapov and P. Bezyazeekov and A. Borodin and M. Br{\"u}ckner and N. Budnev and A. Chiavassa and O. Gress and T. Gress and O. Grishin and A. Dyachok and O. Fedorov and A. Gafarov and A. Garmash and V. Grebenyuk and A. Grinyuk and D. Horns and N. Kalmykov and Y. Kazarina and V. Kindin and V. Kiryuhin and P. Kirilenko and R. Kokoulin and K. Kompaniets and E. Korosteleva and V. Kozhin and E. Kravchenko and A. Kryukov and A. Lagutin and V. Lenok and B. Lubsandorzhiev and N. Lubsandorzhiev and R. Mirgazov and R. Mirzoyan and R. Monkhoev and E. Osipova and A. Pakharukov and A. Pan and M. Panasyuk and L. Pankov and A. Petrukhin and V. Poleschuk and M. Popesku and E. Popova and A. Porelli and E. Postnikov and V. Prosin and V. Ptuskin and A. Pushnin and A. Sokolov",
year = "2020",
month = "2",
day = "1",
doi = "10.1016/j.nima.2019.01.056",
language = "English",
volume = "952",
journal = "Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment",
issn = "0168-9002",
publisher = "Elsevier Science B.V.",

}

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

В: Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, Том 952, 161830, 01.02.2020.

Результат исследования: Научные публикации в периодических изданияхстатья

TY - JOUR

T1 - Cherenkov EAS arrays in the Tunka astrophysical center

T2 - From Tunka-133 to the TAIGA gamma and cosmic ray hybrid detector

AU - TAIGA Collaboration

AU - Kuzmichev, L.

AU - Astapov, I.

AU - Bezyazeekov, P.

AU - Borodin, A.

AU - Brückner, M.

AU - Budnev, N.

AU - Chiavassa, A.

AU - Gress, O.

AU - Gress, T.

AU - Grishin, O.

AU - Dyachok, A.

AU - Fedorov, O.

AU - Gafarov, A.

AU - Garmash, A.

AU - Grebenyuk, V.

AU - Grinyuk, A.

AU - Horns, D.

AU - Kalmykov, N.

AU - Kazarina, Y.

AU - Kindin, V.

AU - Kiryuhin, V.

AU - Kirilenko, P.

AU - Kokoulin, R.

AU - Kompaniets, K.

AU - Korosteleva, E.

AU - Kozhin, V.

AU - Kravchenko, E.

AU - Kryukov, A.

AU - Lagutin, A.

AU - Lenok, V.

AU - Lubsandorzhiev, B.

AU - Lubsandorzhiev, N.

AU - Mirgazov, R.

AU - Mirzoyan, R.

AU - Monkhoev, R.

AU - Osipova, E.

AU - Pakharukov, A.

AU - Pan, A.

AU - Panasyuk, M.

AU - Pankov, L.

AU - Petrukhin, A.

AU - Poleschuk, V.

AU - Popesku, M.

AU - Popova, E.

AU - Porelli, A.

AU - Postnikov, E.

AU - Prosin, V.

AU - Ptuskin, V.

AU - Pushnin, A.

AU - Sokolov, A.

PY - 2020/2/1

Y1 - 2020/2/1

N2 - 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 km 2 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⋅10 15 eV to 10 18 eV. 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 10 13 eV–10 18 eV. The TAIGA prototype will consist of ∼100 wide angle timing Cherenkov stations (TAIGA-HiSCORE) and three IACTs deployed over an area of ∼1 km 2 . 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 km 2 with a total area of about 1000 m 2 . 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.

AB - 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 km 2 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⋅10 15 eV to 10 18 eV. 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 10 13 eV–10 18 eV. The TAIGA prototype will consist of ∼100 wide angle timing Cherenkov stations (TAIGA-HiSCORE) and three IACTs deployed over an area of ∼1 km 2 . 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 km 2 with a total area of about 1000 m 2 . 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.

KW - Cosmic rays

KW - EAS Cherenkov light array

KW - Energy spectrum

KW - Gamma-ray astronomy

KW - IACT

UR - http://www.scopus.com/inward/record.url?scp=85060671031&partnerID=8YFLogxK

U2 - 10.1016/j.nima.2019.01.056

DO - 10.1016/j.nima.2019.01.056

M3 - Article

AN - SCOPUS:85060671031

VL - 952

JO - Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment

JF - Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment

SN - 0168-9002

M1 - 161830

ER -