1. The Tunka-133 EAS Cherenkov light array: status 2011 N.Budnev, Irkutsk State University, on behalf of the Tunka Collaboration

2. S.F.Beregnev, S.N.Epimakhov, N.N. Kalmykov, N.I.Karpov, E.E. Korosteleva, V.A. Kozhin, L.A. Kuzmichev, M.I. Panasyuk, E.G.Popova, V.V. Prosin, A.A. Silaev, A.A. Silaev(ju), A.V. Skurikhin, L.G.Sveshnikova I.V. Yashin, Skobeltsyn Institute of Nucl. Phys. of Moscow State University, Moscow, Russia; N.M. Budnev, O.A. Chvalaev, O.A. Gress, A.V.Dyachok, E.N.Konstantinov, A.V.Korobchebko, R.R. Mirgazov, L.V. Pan ’ kov, V.A.Poleshuk, Yu.A. Semeney, A.V. Zagorodnikov Institute of Applied Phys. of Irkutsk State University, Irkutsk, Russia; B.K. Lubsandorzhiev, B.A. Shaibonov(ju), N.B. Lubsandorzhiev Institute for Nucl. Res. of Russian Academy of Sciences, Moscow, Russia; V.S. Ptuskin IZMIRAN, Troitsk, Moscow Region, Russia; Ch. Spiering, R. Wischnewski DESY-Zeuthen, Zeuthen, Germany; A.Chiavassa Dip. di Fisica Generale Universita' di Torino and INFN, Torino, Italy. A.Haungs, F. Schroeder Karlsruhe Institute of Technology, Karlsruhe, Germany D. Besson, J. Snyder, M. Stockham Department of Physics and Astronomy, University of Kansas, USA Tunka - Collaboration

3. Search for the Acceleration Limit of Galactic Sources - Energy range 10 16 -10 18 eV demands: - 1 km² with spacing smaller than that at Auger - complementary techniques IceTop IceCube - KASCADE-Grande terminated - IceTop/IceCube in operation - Tunka-133 ( calorimetric) in operation - NEVOD-DÉCOR in operation -GAMMA in operation - Auger low energy extension 80% ready - HiSCORE planned - LHAASO planned V.Ptuskin and V.Zirakashvili,2010 Tunka-13 3

4. Tunka-133 – 1 km 2 “dense” EAS Cherenkov light array Energy threshold 10 15 eV Accuracy: core position ~ 10 m energy resolution ~ 15%  X max < 25 g∙cm -2

5. Tunka-133: 19 clusters, 7 detectors in each cluster Optical cable Cluster Electronic box DAQ center EMI 9350 Ø 20 cm 4 channel FADC 200 MHz, 12 bit Optical detector Cluster box

6. Optical detector of the Tunka-133 Angular sensitivity PMT EMI 9350 Ø 20 cm

7. Electronics of cluster box 1. ADC AD9430, 12 bit, 200 MHz 2. FPGA XILINX Spartan-3 Port for FADC connection (trigger, requests) Optical transceiver (central DAQ connection

8. Two seasons of the array operation 2009 - 2010 :286 hours of good weather. 2010 – 2011: 270 hours of good weather. > 4  10 6 events with energy  10 15 эВ. Trigger counting rate during one night. Distribution of the number of hitted clusters in one event.  50 detectors  10 16 eV  10 events during every night with number of hitted optical detectors more than 100.

9. Fitting experimental points with Lateral Distribution function Thershold Lg Q exp (R ) LDF WDF Lg  (R ) Fitting of  ( R) with Width – Distance Function. An event characteristics

10. Example of an event The energy - 2.0  10 17 eV The zenith angle - 12.6 ° 125 hitted detectors R  lg ( I light ) Core position: LDF -method WDF -method

11. The a ll particles energy spectrum (# 250, L.Kuzmichev ) E = 6 ·10 15 - 2·10 16 eV γ 1 = 3.21 ± 0.01 ± 0.05 E = 2 ·10 16 - 10 17 eV γ 2 = 2.94 ±0.01 ± 0.05 E = 10 17 - 10 18 eV γ 3 = 3.2 ± 0.06 ±0.05 Two seasons: 2009-2010, 2010 -2011 of the Tunka-133 operation

12. Mean depth of EAS maximum (#184, V.Prosin)

13. Future of the Tunka experiment 1.Deployment of 6 distant clusters with 42 optical detectors to increase an effective aria and accuracy of EAS parameters reconstruction. 2. Complement the Tunka-133 with radio antennas in a first step for common operation with the Cherenkov array to investigate the dependencies of the measured radio signal on the EAS parameters and to explore of this novel detection technique. 3. Creation a non-imaging air shower array HiSCORE (Hundred*i Square-km Cosmic ORigin Explorer) with 10 km² area to explore the γ-ray sky beyond 10 TeV and cosmic rays from 100 TeV to 1 EeV

14. Future of the Tunka experiment 4. Upgrading the Tunka-133 array with scintillation detectors for charged particle registration (muons and electrons) to reduce the systematic uncertainties in the measurement of energy spectrum and mass composition of CRs. 5. Construction of a system for monitoring of air transparency. 6. Deployment of fluorescent detector at 10 km from the array for common operation.

15. 1 km. 6 additional clusters ( 42 detectors) Increasing of an effective area in 4 times for energy more than 10 17 eV In operation Statistics in 2012 ( > 10 17 eV) : 600 (inner events) + 600 (out events) All: 1200 events

16. Example of event LDF -method WDF -method

17. Radio detection of EAS Antennas are connected to the free FADC channels of Tunka-133 cluster electronics Short Aperiodic Loaded Loop Antenna (SALLA) (A.Haungs et al. Institute fur Kernphysick, Forschungszentrum, Karslruhe, Germany 2 antennas + 4 (this summer) + 19 (next summer) Nearly 70 radio EAS candidates

18. One of 70 selected EAS radio candidates A radio pulse in both polarizations shortly before PMT signals PMT signals

19. Correlation with Energy + Distance Energy distribution of selected radio pulses Distance from EAS core of selected radio pulses All radio candidates are events with rather big energy and their cores were not far the SALLA from.

20. Events with largest energy – near to 10 19 eV – was found out with the help of radio antenna

21. HiSCORE project – wide-angle gamma-telescope with area 100 km 2 and threshold 30 TeV (M.Tluczykont et al, ArXiv: 0909.0445) HiSCORE:Hundred i Square-km Cosmic ORigin Explorer Time schedule 1. First SCORE Station will be installed at Tunka in autumn this year. 2. 25 station at 2012 – 1 sq. km wide-angle gamma telescope Energy spectrum from 10 14 - 10 17 eV - compare with Tunka-25 and Tunka-133 results

22. Pevatron emission predicted by a pp model, as compared to the sensitivities of the H.E.S.S survey and the HiSCORE sensitivity goal.

23. The scintillation detectors for charged particle registration and absolute energy calibration (# 250, Kuzmichev ) 40 detectors on the area of 1km 2

24. Conclusion 1. The completed new Cherenkov array Tunka- 133 takes data since October 2009. 2. The energy spectrum and mass composition of CR, obtained from the two years of Tunka- 133 operation are in rather good agreement with KASCADE-Grande and Tibet results. 3.With respect to charged Cosmic Rays, we want to substantially upgrade the Cherenkov light detector Tunka-133, and complement it with radio antennas and scintillation detectors. 4. We plan to deploy new a non-imaging air shower array with 10 km² area for γ-ray and cosmic ray observations.

25. Thank You Thank you!