Primary cosmic ray energy spectrum and mean mass composition using data from the TAIGA astrophysical complex

The corrected dependence of the mean depth of the EAS maximum X_{max} X m a x on the energy was obtained from the data of the Tunka-133 array for 7 years and the TAIGA-HiSCORE array for 2 years. The parameter \langle\ln A\rangle ⟩ ln A ⟪ , characterizing the mean mass compositon was derived from these results. The differential energy spectrum of primary cosmic rays in the energy range of 2\cdot 10^{14} 2 ⋅ 10 14 – 2\cdot 10^{16} 2 ⋅ 10 16 eV was reconstructed using the new parameter Q_{100} Q 100 the Cherenkov light flux at the core distance 100 m. Change of the parameter for the energy reconstuction for the TAIGA-HiSCORE from Q_{200} Q 200 to Q_{100} Q 100 provides a decreasing energy threshold for the spectrum to about 200 TeV.