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Transcript of Tunka-133: status and results L.A.Kuzmichev (SINP MSU) On behalf on the Tunka Collaboration Moscow,...
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Tunka-133: status and results
L.A.Kuzmichev (SINP MSU)
On behalf on the Tunka Collaboration
Moscow, May 2011
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S.F.Beregnev, S.N.Epimakhov, N.N. Kalmykov, N.I.KarpovE.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, A.V.Diajok , O.A. Chvalaev, O.A. Gress, A.V.Dyachok, E.N.Konstantinov, A.V.Korobchebko, R.R. Mirgazov, L.V. Pan’kov, 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.
D. Besson, J. Snyder, M. StockhamDepartment of Physics and Astronomy, University of Kansas, USA
Tunka Collaboration
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Search for the Acceleration Limit of Galactic Sources- Energy range 1016-1018 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
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V.Ptuskin andV.Zirakashvili,2010
Tunka-133
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OUTLINE 1. Non-imaging Air Cherenkov Technique
2. Tunka-133: construction and deployment.
3. Results after first season.
4. Plan for the Tunka-133 upgrading.
5. Future plans.
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20-30km
P, A For Ee >25 MeVVe > C/ n – light velocity in air
Cherenkov light
Photons detectors
Q tot N(x) dx ~ E
Atmosphere as a huge calorimeter
E (PeV) = 0.4 Q(175) ph· ev-1 cm-2
LateralDistributionFunction
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Advantage of Cherenkov Technique:
1. Good energy resolution - up to 15%2. Good accuracy of Xmax - 20 -25 g/cm2
3. Good angular resolution - 0.1 – 0.3 deg4. Low cost – Tunka-133 – 1 km2 array: 0.5 106 E ( construction and deployment) + 0.2 106 E( PMTs) Cost of 100 km2 array - 107 E
Disadvantage:
1.Small time of operation ( moonless, cloudless nights) – 5-10% 2. Existence of moving lids on modules
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Summary of methodic used in Tunka-133
( more detail in V.Prosin report at Wednesday)
1. Energy: E (PeV) = 0.4 Q(175) ph· ev-1 cm-2
From CORSIKA, no dependence from hadronic model
2. Core location: LFD and WDF ( width-distance function) accuracy – 10 m
3. Energy resolution: 15%
4.Xmax - p (steepness from LDF) - τ(400) – time width at 400 m from the core
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Tunka-133 – 1 km2 “dense” EAS Cherenkov light array
Energy threshold 1015 eV
Accuracy: core location ~ 10 m energy resolution ~ 15% Xmax < 25 g∙cm-2
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Tunka-133: 19 clusters, 7 detectors in each cluster
Optical cableClusterElectronic box
DAQcenter
PMTEMI 9350Ø 20 cm
4 channel FADC boards 200 MHz, 12 bit
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Array depoliment Optical cables
Detectors
Testing PMTs
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DAQ systemCluster
Local trigger: > 3 hit detectors in 0.5 µs
Optical detector
ClusterElectronicbox
1 Gb Ethernet:Data transmission +Synchronization
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Optical detector of Tunka-133
PMTEMI 9350Ø 20 cm
Angular sensitivity
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4 channel FADC
1. ADC AD9430, 12 bit, 200 MHz2. FPGA XILINX Spartan-3
Port for FADCconnection(trigger, requests)
Optical transceiver(central DAQconnection
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Time synchronization chain
Accuracy of time synchronization 10 ns
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Two seasons of array operation
2009 - 2010 :286 hours of good weather . 2010 – 2011: 270 hours of good weather. 4106 events with energy 1015 эВ.
Trigger counting rate during one night .
Distribution of the number of hitted clusters in one event.
50 detectors 1016 eV
10 events during every night with number of hitted detectors more than 100.
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Experiment:Every event = 3 – 133 pair pulses:
Reconstruction of parameters:1) Delay at the level 0.25Amax, 2) the full area under pulse, 3) FWHM
anode
dynode
ti
FWHM
11th cluster 19th cluster 500 m
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EAS zenith angular distribution (E0>1016 eV)
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Energy spectrum (from first season data)
Core position insidecircle: R = 450 mZenith angle < 45°
All: 1 117 907
>1016 eV : 18714> 1017 eV: 202
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Example of event Energy: 2.01017 eV zenith angle : 12.6 °
125 detectors
R lg ( I light )
Core position:
LDF -method
WDF -method
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.A– Fitting experimental points with LDF
B – Fitting of ( R) with Width – Distance Function.
A B
Thershold
Lg Qexp (R )
LDF
WDF
Lg (R )
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Events with largest energy – near to 1019 eV – was found out with the help of radio antenna
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353 events
277
Good pointing for the existing of “ bump”
4.2 December 2010
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373
293
4.2
MAY 2011
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Specter with 2 types of sources Eknee =4 PeV (0.75)+4x150 PeV (0.25
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104 105 106 107 108 109 1010 1011 1012104
105
106
107
108
3.38E6
Pure Galactic
0.20
E2knee=4x150
Sum Gal+Metag 025
F(E
) E3.
0
E, GeV
Tun133 GrandeKas Hires1 Hires2 EASTOP Tibet KASKADE Tunka25 MGUIE3 AKENO Augergv Hires1M3 All z1 z2 z6 z8 z10 z14 z16 z18 z20 z26 tot B tot
Specter with 2 types of sources Eknee =4 PeV (0.75)+4x150 PeV (0.25)
Here we need to knowMeta-Galactic
PHe
C,O
Fe
Si
Total all –particle spectrum in our model
Galactic sources
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Mass composition: 3 dif. variants
• 1) Emax (P)
• In Galaxy ; 4 PeV
• 2) Emax (P)=4 and
• 600 PeV
• This variant predicts a heavy composition at 1018 eV
• 3) SNR Ia + He stars +MetaGalactic with mixed composition in sources
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Plan for Tunka-133 upgrading
- Far distant clusters for increasing effective area
- Net of radioantennas
- Low threshold array
- Scintillation muon counters
E0 , Xmax ( from Tunka-133 ), Nµ
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1 km
.6 additionalclusters( 42 detectors)
IncreasingEffectiveArea in 4 timesfor energymore than1017 eV In operation
Statistics in 2012 ( > 1017 eV) : 600 (inner events) +600 (out events) All: 1200 events
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Registration of radio signals from EAS
Antennas are connected to the free FADC
channels of Tunka-133 cluster electronics
Choosing the type of antennas:Now 2 types of antennas were
installed at Tunka Array
Log-periodic antenna (D. Besson et al. University of Kansas, USA)
Short Aperiodic Loaded LoopAntenna (SALLA)(A.Haungs et al. Institute furKernphysick, Forschungszentrum,Karslruhe, Germany
6 antennas
2 antennas
Nearly 100 candidates
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SCORE project – wide-angle gamma-telescope with area 10 -100 km2 and threshold 30 тэВ(M.Tluczykont et al , ArXiv: 0909.0445)
SCORE: Study for Cosmic ORigin Explorer
Time schedule 1.First SCORE Station will be installed at Tunkain this summer-autumn2.20 station at 2012 – 1 sq. km telescope ( good chance)3. ??
Energy spectrum from 1014 - 1017 eV - compare with Tunka-25 and Tunka-133 results
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Muon detectores
lgNµ (corr)= lgNµ -
1500
Xmax - 600
S = 5 m2
40 muon detectors on the area of 1km2
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766 г/см2
675 г/см2
Search for diffuse gamma radiation at high energy
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Future plan: 100 km2 array
1. Spacing between detectors – 250 m2. Cluster principle of organization: 8-10 detector in one cluster3. PMT - with 20 cm diameter photocathode 4. Energy threshold (3-5) 1016 eV 5. Digitization of signals in optical detectors 6. Optical cables for data transmission and synchronization
PMT - 1500 -2000 piecesCable – 1000 km
Total price - 107 Eu
Time schedule 1. Proposal to the end of 2012 2. When - ?3. Where ?? May be with Auger-Next
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Conclusion 1.The spectrum from 1016 to 1017 eV cannot be fitted with one power law index g : 3.2 to 3.0 at 2 1016 eV.
2. Very good agreement with KASKADE-Grande results ( up to 71016 ).
3. For energy > 1017 eV we need much more statistics.
4. “Bump” at 8.1016 eV - possible indication of a bump + agreement with GAMMA. But not seen by KASKADE-Grande.
5. Indication on light composition at energy > 1017 eV
6. Update 2011: - Far distant clusters. - Net of radio antennas. - First SCORE detectors.
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Thank You