Abstract
The extensive air shower Cherenkov light array Tunka-133 collected data during 7 winter seasons from 2009 to 2017. From 2175 hours of data taking, we derived the differential energy spectrum of cosmic rays in the energy range 6 · 1015 2 · 1018 eV. The TAIGA-HiSCORE array is in the process of continuous expansion and modernization. Here we present the results obtained with 28 stations of the first HiSCORE stage from 35 clear moonless nights in the winter of 2017-2018. The combined spectrum of two arrays covers a range of 2 · 1014 – 2 · 1018 eV.
Highlights
The Tunka Astrophysical Center in the Tunka Valley (50 km from Lake Baikal) was created to study very high energy cosmic rays (VHE CR) ≥ 1015 eV
The final version of the observatory will include a network of wide field of view (0.6 sr) timing Cherenkov light stations, called TAIGAHiSCORE (High Sensitivity Cosmic Ray Explorer) [7, 8], and up to 16 imaging atmospheric Cherenkov telescopes (IACT) (Fig. 2), covering an area of 10 km2
The absolute primary energy calibration is carried out, as for all Tunka Valley Cherenkov light experiments, by normalizing the obtained every night integral spectra to the integral spectrum obtained in the Tunka-25 experiment [14], normalized in its turn to the absolute intensity of cosmic rays, obtained in the QUEST experiment [15]
Summary
The Tunka Astrophysical Center in the Tunka Valley (50 km from Lake Baikal) was created to study very high energy cosmic rays (VHE CR) ≥ 1015 eV. Tunka-133 array contains 175 optical detectors, spaced over an area of 3 km. The final version of the observatory will include a network of wide field of view (0.6 sr) timing Cherenkov light stations, called TAIGAHiSCORE (High Sensitivity Cosmic Ray Explorer) [7, 8], and up to 16 imaging atmospheric Cherenkov telescopes (IACT) (Fig. 2), covering an area of 10 km. The final version of the observatory will include a network of wide field of view (0.6 sr) timing Cherenkov light stations, called TAIGAHiSCORE (High Sensitivity Cosmic Ray Explorer) [7, 8], and up to 16 imaging atmospheric Cherenkov telescopes (IACT) (Fig. 2), covering an area of 10 km2 The capabilities of these Cherenkov arrays will be enhanced by muon. We present the data obtained using the 28 stations, shown as the filled squares in the Fig. 3 for 35 clear moon-
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