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The Tunka-133 EAS Cherenkov light array: status of 2011

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arxiv 1201.2122 v1 pith:LCSO7Q3M submitted 2012-01-10 astro-ph.HE

The Tunka-133 EAS Cherenkov light array: status of 2011

S. F. Berezhnev , D. Besson , A. V. Korobchenko , N. M. Budnev , A. Chiavassa , O. A. Chvalaev , O. A. Gress , A. N. Dyachok
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S. N. Epimakhov A. Haungs N. I. Karpov N. N. Kalmykov E. N. Konstantinov E. E. Korosteleva V. A. Kozhin L. A. Kuzmichev B. K. Lubsandorzhiev N. B. Lubsandorzhiev R. R. Mirgazov M. I. Panasyuk L. V. Pankov E. G. Popova V. V. Prosin V. S. Ptuskin Yu. A. Semeney B. A. Shaibonov Jr. A. A. Silaev A. A. Silaev Jr. A. V. Skurikhin J. Snyder C. Spiering F. G. Schreoder M. Stockham L. G. Sveshnikova R. Wischnewski I. V. Yashin A. V. Zagorodnikov
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keywords arrayenergycherenkovlightcalibrationdepthdiscussedmaximum
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A new EAS Cherenkov light array, Tunka-133, with ~1 km^2 geometrical area has been installed at the Tunka Valley (50 km from Lake Baikal) in 2009. The array permits a detailed study of cosmic ray energy spectrum and mass composition in the energy range 10^16 - 10^18 eV with a uniform method. We describe the array construction, DAQ and methods of the array calibration.The method of energy reconstruction and absolute calibration of measurements are discussed. The analysis of spatial and time structure of EAS Cherenkov light allows to estimate the depth of the EAS maximum X_max. The results on the all particles energy spectrum and the mean depth of the EAS maximum X_max vs. primary energy derived from the data of two winter seasons (2009 -- 2011), are presented. Preliminary results of joint operation of the Cherenkov array with antennas for detection of EAS radio signals are shown. Plans for future upgrades -- deployment of remote clusters, radioantennas and a scintillator detector network and a prototype of the HiSCORE gamma-telescope -- are discussed.

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