Energy Spectrum of Primary Cosmic Rays, According to TUNKA-133 and TAIGA-HiSCORE EAS Cherenkov Light Data
- Prosin, V. V.
- Astapov, I. I.
- Gorbunov, N. V.
- Grebenyuk, V. M.
- Gress, O. A.
- Gress, T. I.
- Grinyuk, A. A.
- Grishin, O. G.
- Dyachok, A. N.
- Zhurov, D. P.
- Zagorodnikov, A. V.
- Zurbanov, V. L.
- Bezyazeekov, P. A.
- Ivanova, A. L.
- Kazarina, Yu. A.
- Kalmykov, N. N.
- Kindin, V. V.
- Kirilenko, P. S.
- Kiryuhin, S. N.
- Kozhin, V. A.
- Kokoulin, R. P.
- Kompaniets, K. G.
- Korosteleva, E. E.
- Boreyko, V.
- Kravchenko, E. A.
- Kuzmichev, L. A.
- Kunnas, M.
- Chiavassa, A.
- Lagutin, A. A.
- Lemeshev, Yu.
- Lenok, V. V.
- Lubsandorzhiev, B. K.
- Lubsandorzhiev, N. B.
- Mirgazov, R. R.
- Borodin, A. N.
- Mirzoyan, R.
- Monkhoev, R. D.
- Osipova, E. A.
- Panasyuk, M. I.
- Pankov, L. V.
- Pakhorukov, A. L.
- Petrukhin, A. A.
- Poleschuk, V. A.
- Popescu, M.
- Popova, E. G.
- Brueckner, M.
- Porelli, A.
- Postnikov, E. B.
- Ptuskin, V. S.
- Pushnin, A. A.
- Raikin, R. I.
- Rubtsov, G. I.
- Rjabov, E. V.
- Sabirov, B. M.
- Sagan, Y. I.
- Samoliga, V. S.
- Budnev, N. M.
- Sveshnikova, L. G.
- Semeney, Yu. A.
- Sidorenkov, A. Yu.
- Silaev, A. A.
- Silaev, A. A.
- Skurikhin, A. V.
- Slunecka, M.
- Sokolov, A. V.
- Tabolenko, V. A.
- Tarashansky, B. A.
- Wischnewski, R.
- Tkachev, L. G.
- Tkachenko, A. V.
- Tluczykont, M.
- Fedorov, O. L.
- Horns, D.
- Spiering, C.
- Yashin, I. I.
- Garmash, A. Yu.
- Gafarov, A. R.
DOIAbstract
The Tunka-133 Cherenkov complex for recording extensive air showers (EAS) collected data over seven winters from 2009 to 2017. The differential energy spectra of all particles was acquired in the 6 × 1015–3 × 1018 eV range of energies over 2175 h. The TAIGA-HiSCORE complex is continually being expanded and upgraded. Data acquired by 30 first-line stations over 35 days during the period 2017–2018 is analyzed in this work. As at the Tunka-133 setup, the primary particle energies above 1015 eV are measured using the density of the Cherenkov light flux at a distance of 200 m from a shower’s axis. Data on lower energies are collected by determining the energy of the light flux near a shower’s axis. This results in a spectrum of 2 × 1014–1017 eV....
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