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

Статья опубликована в высокорейтинговом журнале
Статья опубликована в журнале из списка Web of Science и/или Scopus

Работа с статьей


[1] Cherenkov eas arrays in the tunka astrophysical center: From tunka-133 to the taiga gamma and cosmic ray hybrid detector / L. Kuzmichev, I. Astapov, P. Bezyazeekov et al. // Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment. — 2018. One of the most informative methods of cosmic ray studies is the detection of Cherenkov light from extensiveair showers (EAS). The primary energy reconstruction is possible by using the Earth’s atmosphere as a hugecalorimeter. The EAS Cherenkov light array Tunka-133, with∼3 km2geometrical area, is taking data since2009. Tunka-133 is located in the Tunka Astrophysical Center at∼50 km west of Lake Baikal. This array allowsus to perform a detailed study of the energy spectrum and the mass composition in the energy range from6⋅1015eVto1018eV. Most of the ongoing efforts are focused on the construction of the first stage of the detectorTAIGA (Tunka Advanced Instrument for cosmic ray physics and Gamma Astronomy). The latter is designed forthe study of gamma rays and charged cosmic rays in the energy range of1013eV–1018eV. The TAIGA prototypewill consist of∼100 wide angle timing Cherenkov stations (TAIGA-HiSCORE) and three IACTs deployed overan area of∼1 km2. The installation of the array is planned to be finished in 2019 while the data-taking canstart already during the commissioning phase. The joint reconstruction of energy, direction, and core position ofthe 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 sensitivityfor energies≥30–50 TeV make this pioneering technique very attractive for exploring galactic PeVatrons andcosmic rays. In addition to the Cherenkov light detectors we intend to deploy surface and underground muondetectors over an area of 1 km2with a total area of about 1000 m2. The results of the first season of coincidentoperation of the first∼4 m diameter IACT with an aperture of∼10◦with 30 stations of TAIGA-HiSCORE will represented. [ DOI ]

Публикация в формате сохранить в файл сохранить в файл сохранить в файл сохранить в файл сохранить в файл сохранить в файл скрыть