- - HiSCORE:

.. ( )

, , 7 2013

-133 2013 : -

2. -

3. - -HiSCORE.

. . .- .

-133: 175 3 2

1

( 3 ).The power law index at E0>1017 is similar to that obtained by the Giant Experiments: TA, HiRes, Auger.

.Agreement with KASCADE-GrandeAgreement with old Flys Eye, HiRes and TA spectra.

vs. E0Agreement with HiRes-MIA and Auger results at 1017 1018 eV

EXPERIMENT: MEAN vs. E0

ANALYSIS of Xmax DISTRIBUTIONFit with weighted sum of 4 group MC simulated distributions: Fe, CNO, He, p

Energy spectrum of these group : will be presented at ICRC-2013

(80080040) XP3462384

- 5 1016 - 5 1017 - - ? - ( )

2. 1015 - 1016 +

1 10

If IceCube see PeV Galactic neutrino then we should see PeV gamma -raysWith muon ( 2)Only cascade ( 15 )28 events

Flux from one source: E F(>E) ~ 10 -12 erg / cm2 secFop et al : arXiv: 1305.6606 E F(>E) ~3 10 -11 erg / cm2 sec

200-600 muons for 30 TeVfor pronots

100 times more muons for 3 Pev

With 100 m2 muon detectors

2-6 muons possible toseparate gamma from proton

Decreasing Tunka-133 energy thershold ( changing plex)

Increasing accuracy of Tunka clusters synchronization

Increasing accuracy of angle reconstruction

-

1873

( ):

CTA ( 2017-18) - ~150 . (?)2. HAWC (2014) - ~30 . 3. LAWCA (2015) ~ 30 . 3. LHAASO (2013-2018) ~150 .

:

- HiSCORE2. 5@5 (.. .) >20-30 10 -100 2 . - HiSCORE

unka-HiSCORE : wide-angle Cherenkov gamma-observatoryArea : from 1 to 100 km2

FOV ~ 0.6 ster ( 30 )

Energy threshold ~ 20 TeV

Total cost ~ 50 106 Euro HiSCORE Hundred* i Square-km Cosmic Origin Explorer

CollaborationTunka-HiSCOREGermany Russia Hamburg University(Hamburg) MSU( SINP)( Moscow)DESY (Zeuthen) ISU (API) (Irkutsk)MPI (Munich) INR RAS (Moscow) IZMIRAN (Troitsk) JINR (Dubna) MEPHI (Moscow) ASU (Barnaul) IKFIA(Yakutsk)

Gamma-ray AstronomySearch for the PeVatrons. VHE spectra of known sources: where do they stop?Absorption in IRF and CMB.Diffuse emission: Galactic plane, Local supercluster.

Charged cosmic ray physicsEnergy spectrum and mass composition from 1014 to1018 eV.107 events (in 1 km2 array) with energy > 1014 eV per one season (400 hours). Particle physicsAxion/photon conversion.Hidden photon/photon oscillations.Lorentz invariance violation.pp cross-section measurement.Quark-gluon plasma.Main Topics

Methodical approaches for 3 stagesShower front and LDFsampling technique (at the first stages). Angular resolution 0.1 deg, Xmax measurement for hadron rejection.

Using of small mirrors net with cheap matrix of PMTs for imaging technique.

3. Using of large area muon detectors for hadron rejection.

150 m9352KB8, ETTunka-HiSCORE 1 km2 1 stage

= S P S I T T 5P ~ E - E ~ I T S S ~ 0.1 2 0.1 : E 100 S - .P T - -

I 2.1012

2 1

- 4 ( K = 1/ sin2 (tet) tet=30 - K =4 )

S n ( n ) n =4

Tsignal 7-10

4. QE max = 35-40%

5. - - 1.5 -2 . Eth ~ ( Sdet. )-1/2 (Tsignal )1/2

1 0.1 ( 150 ) 179 1 .

E = 25 TeV ( Themistocle) 5 .

( FOV -0.05 ) , 2 2 (20 ) 7-10 : ~ 0.5 . ( + ) ()

Tunka-HiSCORE 1 km2 stage 3: 10000 m2 muon detectors(1% of array area)Scintillation detectors developed in Mephi30 TeV proton 2-6 muonsRejection of hadron background by 10 times at 20-30 TeV

2.

-

R5912 (Hamamatsu) ( 8) QE max - 23-25%

2. 9352 KB (Electron Tube) (8) 6 CuBe 1300 , 1000

R7081 (10) QE max - 35-40% 5000

4. R11780 ( 12) QE max - 35-40% 10000 , 5000

5. - .

3 2012

200 m431150 m 2150150 -

Station Electronics4 PMTsCalibrationlight source

: 5 :

Q eff = 0.07

T = 25 Q eff = 0.07Q = 0.16

121 : Q eff =0.07 T =25 ns

2: Q eff =0.10 T=10 ns30 TeV100 TeV

150 mTunka-HiSCORE 1km2 2 stage600 mmR11780 12 R7081 10 Hamamatsu

20 TeV50 TeV N hit 5 detectors100%10%1%Efficiency1-st stage2 stage

150 mTunka-HiSCORE 1km2 2 stage300 m600 mm2 m 2 mirror,7 FOV,

Installingmatrix ofPMT,Image technique

1 1 km2, 4 PMTs per station ( 8 PMT)2 1 km2, + additional station ( 10 PMT) + net of mirrors (S = 2 m2, 7-10 FOV, without imaging)2 mounting of matrix in each mirror (not yet simulated)3 104 m2 muon detectors4 10 km2 , 4 PMTs per station ( 8PMT) for 12 PMT (not yet simulated)5 100 km2 (8 PMT)Tunka-HiSCORE:50 events or 5 RMS,T = 500 hours

LHAASO: 50 events or 5 RMS 1 year12345

Tunka-HiSCORE: 50 events or 5 RMS, T = 500 hours

12345Casa-miaIceCubeneutrino

S=1 km2, 60 stations, 150 m step, 240 PMTs (150 PMTs are available), 1 M Euro, 2012 2014S = 10 km2, 225 station , 200 m step, 1000 PMT, 5-6 M Euro.S = 100 km2, 2000 station, 1 PMT in station10-12 M EuroS = 1 km2, 60 station with240 PMT (10) + 15 mirrors( S = 2 m2 ) Without matrix of PMTs- With matrix of PMTs Cost: 5 M Euro. 3 stations in October 2012 10000 m2 scintillation detectors(1% of the whole area) 2-5 muons from 25 TeV protonsCost: 20-25 M Euro. Decreasing of energy thresholdIncreasing ofarea of arrayChoose newPlace for deployment

0.1 3. !S, km2D.HamphfPh.D 2012

DRS-4 - DRS ( Domino Ring Sampler) 4 9- 0.2 1024 80 .

Alanod-4300

Cas A

radio polarization in red (VLA),X-rays in green (CHANDRA),optical in blue (HST)1.1933 2. 1949 3. 1963 , 10% 4. 1977 1978 -, 5. 1993-1996 . .6. 2003-2005 , , Emax ~ Z 1015 eV

KASCADE-Grande 20 - 2013

What we can see with 1 km2 array (short list)

NameRAdegreesDeclFlux F at 1 TeV, 10-12cm-2 s1TeV-1 Flux F at 35 TeV, 10-17cm-2 s-1TeV-1(from Milagro)Time of observation per one year( 0.5- weater factor) Number of events per one season E> 20 TeVTycho SNR (J0025+641)6.35964.130.17 0.05=1.95 0.5236h 88 Crab83.632922.0145 32.6 .9.0=2.6 0.3162.6 9.4110h,680SNR IC443(MAGIC J0616+225)94.179222.53000.58 0.12=3.1 0.3028.8 9.5112h, 2 (from MAGIC)50 ( from Milagro)Geminga MGRO C3PSR98.5017.7637.7 10.7102h, 80M82 (Starburst Galaxy)148.769.70.25 0.12=2.5 0.60.2325h,22 Mkn 421 (BL, z=0.031Variable )166.11438.2088 50-200=2.0-2.6140h 20 - 1000

SNR 106.6+2.7(J2229.0+6114) 337.2661.341.42 0.33 0.41=2.29 0.33 0.3070.9 10.8167h140 ( from VERITAS235 ( from Milagro)Cas A (SNR, G111.7-2.1)[6]350.853 58.8154 1.26 0.18=2.61 0.240.2177h 40CTA_1(SNR,PWN)1.572.81.3=2.3266 h200

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