Speaker
Description
Summary
For the energy range 30 – 200 TeV the sensitivity of 1 km^2 area TAIGA detector for the detection of local sources is expected to be 5 10^{−13} erg cm^{−2} sec^{−1} for 500 h of observations. Combination of the wide angle Cherenkov timing detector TAIGA-HiSCORE with the 4-m class Imaging Atmospheric Cherenkov Telescopes (TAIGA-IACT) offers a cost effective-way to construct in future a 10 km^2 scale array. Reconstruction of a given EAS energy, incoming direction and its core position, based on the TAIGA-HiSCORE data allow one to increase a distance between the IACTs up to 600-1000 m. The low investments together with the high sensitivity for energies ≥ 30-50 TeV make this pioneering technique very attractive for exploring the galactic PeVatrons and cosmic rays. In addition to the Cherenkov light detectors we intend to deploy an array of muon detectors (TAIGA-Muon array) spread over an area of 1 km^2 with a total area of about 2000 m^2. The TAIGA-IACT together with the TAIGA-Muon array will be used for selection of gamma-ray induced EAS. At present the TAIGA first stage has been constructed in Tunka valley, ~50 km West from the Lake Baikal.. We are planning to test operation of IACT in the single operation mode in coincidence with the HiSCORE up to shower impact distances of ~500-600 m. The first experimental results with the TAIGA first stage will be reported.
