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
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
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
V.Ptuskin andV.Zirakashvili,2010
Tunka-133
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.
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
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
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
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
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
Array depoliment Optical cables
Detectors
Testing PMTs
DAQ systemCluster
Local trigger: > 3 hit detectors in 0.5 µs
Optical detector
ClusterElectronicbox
1 Gb Ethernet:Data transmission +Synchronization
Optical detector of Tunka-133
PMTEMI 9350Ø 20 cm
Angular sensitivity
4 channel FADC
1. ADC AD9430, 12 bit, 200 MHz2. FPGA XILINX Spartan-3
Port for FADCconnection(trigger, requests)
Optical transceiver(central DAQconnection
Time synchronization chain
Accuracy of time synchronization 10 ns
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.
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
EAS zenith angular distribution (E0>1016 eV)
Energy spectrum (from first season data)
Core position insidecircle: R = 450 mZenith angle < 45°
All: 1 117 907
>1016 eV : 18714> 1017 eV: 202
Example of event Energy: 2.01017 eV zenith angle : 12.6 °
125 detectors
R lg ( I light )
Core position:
LDF -method
WDF -method
.A– Fitting experimental points with LDF
B – Fitting of ( R) with Width – Distance Function.
A B
Thershold
Lg Qexp (R )
LDF
WDF
Lg (R )
Events with largest energy – near to 1019 eV – was found out with the help of radio antenna
353 events
277
Good pointing for the existing of “ bump”
4.2 December 2010
373
293
4.2
MAY 2011
Specter with 2 types of sources Eknee =4 PeV (0.75)+4x150 PeV (0.25
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
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
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
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
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
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
Muon detectores
lgNµ (corr)= lgNµ -
1500
Xmax - 600
S = 5 m2
40 muon detectors on the area of 1km2
766 г/см2
675 г/см2
Search for diffuse gamma radiation at high energy
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
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.
Thank You