Abstract
In this talk, we describe the status and the perspectives of the hybrid Air Shower Array TAIGA (Tunka Advanced Instrument for cosmic rays and Gamma Astronomy) which is currently under construction in the Tunka Valley close to Lake Baikal and is taking data in its initial configurations. TAIGA is designed for the study of gamma rays and charged cosmic rays in the energy range of 1013 eV - 1018 eV. It has the potential to play an important role in the search for Galactic Pevatrons and within a multi-messenger approach to explore the high-energy sky.
Highlights
The first of the presently operating installations in the Tunka valley was the Cherenkov light array Tunka-133, with ∼3 km2 geometrical area, taking data since 2009
Tunka-133 is devoted to the study of energy spectrum and mass composition of cosmic rays in the energy range from 6 × 1015 to 1018 eV
The preliminary cosmic rays spectrum as measured with HiSCORE is compared in Fig. 2 to the results of previous experiments in the Tunka Valley, as well as with the results of the balloon experiment ATIC-2 [16], the satellite experiment NUCLEON [17] and a new experimental spectrum obtained by the HAWC experiment [18] in Mexico
Summary
The first of the presently operating installations in the Tunka valley was the Cherenkov light array Tunka-133, with ∼3 km geometrical area, taking data since 2009. Most of the ongoing effort, is focused on the construction of the first stage of TAIGA (Tunka Advanced Instrument for cosmic ray physics and Gamma Astronomy) This array is designed to study gamma rays and charged cosmic rays in the energy range of 1013 − 1018 eV. TAIGA will include a network of wide field of view (0.6 sr) timing Cherenkov light stations, named TAIGA-HiSCORE [5],[6] (High Sensitivity Cosmic Origin Explorer), and up to 16 imaging atmospheric Cherenkov telescopes (Fig. 1), covering an area of 10 km2 The capabilities of these Cherenkov arrays are enhanced by muon detectors (TAIGA-Muon) with a total coverage of 2000 m2, distributed over an area of 1 km. The detection sensitivity of a 10 km installation for poinr sources in the energy range of 30 – 200 TeV is expected to be 5 · 10−14 TeV cm−2 sec−1 for 500 h of observation or 10 detected events
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