tunka-133: cosmic ray mass composition at 10 16 – 10 18 ev
DESCRIPTION
Tunka-133: Cosmic Ray Mass Composition at 10 16 – 10 18 eV. Vasily Prosin (SINP MSU) For the Tunka Collaboration. Tunka Collaboration. - PowerPoint PPT PresentationTRANSCRIPT
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Tunka-133: Cosmic Ray Mass Composition at 1016 – 1018 eV
Vasily Prosin (SINP MSU)
For the Tunka Collaboration
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Tunka Collaboration S.F. Beregnev, S.N. Epimakhov, N.N. Kalmykov, E.E. Korosteleva, N.I. Karpov, 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 Inst. of Nucl. Phys. of Lomonosov Moscow State Univ., Moscow, Russia;
N.M. Budnev, A.V. Dyachok , O.A. Chvalaev, O.A. Gress, A.V. Korobchenko, R.R. Mirgazov, L.V. Pan’kov, Yu.A. Semeney, A.V. Zagorodnikov– Inst. of Applied Phys. of Irkutsk State Univ., Irkutsk, Russia;
B.K. Lubsandorzhiev, B.A. Shaibonov(ju) – Inst. 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. Stockham– Department of Physics and Astronomy, University of Kansas, USA
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Tunka-133 (update 2011)
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Rkn
Qkn
Q(R) = Qkn·exp((Rkn-R)·(1+3/(R+3))/R0)
Q(R) = Qkn·(Rkn/R)2.2
R0 = 102.95-0.245·P [m]
Rkn = 109 - 24.5·(P-4) [m]
b = 4.84 - 2.83∙log10(6.5-P)
CORSIKA: Simulated lateral distributions and fitting function (LDF)
LDF has a single variable parameter
of shape - steepness:
P=Q(100)/Q(200)
0 < R < 700 m
1 - P=5.0 2 – P=4.1 3 – P=3.2 Q(R) = Q(200)·((R/200+1)/2)-
b
Q175
E0 ~ Q1750.93
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An example of real shower of 16.03.2010
WDF
LDFP – analysisFWHM(400)
– analysis
The limits for distances used now to unify Xmax analysis for all energy range:
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3. The new methods of analysis for high core distances
LDF
LDF steepness analysis
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EXPERIMENT:Every event = 7 – 133 pairs of records:
The primary data record for each Cherenkov light detector containes 1024 points of amplitude vs. time with the 5 ns time step:
anode
dynode
1. Pulse selection 2. Apparatus distortions correction 3. Pulse waveform fitting
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EXPERIMENT:The main parameters determination – area (light flux) Qi, amplitude Ai, width FWHMi and front delay ti at 0.25Ai.(The more accurate FWHM = τeff/1.24, τeff = Qi/Ai)
anode
dynode
ti
FWHMi
Ai
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CORSIKA: Core location – LDF and ADF
Core location: Amplitude – Distance Function (ADF), ADF tail fit: A(R) = A(400)·((R/400+1)/2)-bA steepness: bA
LDF tail fit: Q(R) = Q(300)·((R/300+1)/2)-bQ steepness: bQ
bA > bQ
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Accuracy of the EAS core reconstruction
For R< 450 m: ΔRcore ~ 10 mFor 450 m < R < 800 m: ΔRcore ~ 20 m for ADF methodand ΔRcore ~ 30 m for LDF method
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CORSIKA: EAS Cherenkov light front
tfront = (R+200)2/SΔθ < 0.5° for Nclusters > 4
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Recalculation from Cherenkov light flux Q200 to
the primary energy E0
E0 = A·Q200g
g = 0.94
CORSIKA simulation:~ 500 protons~ 500 ironZenith angles: 0°, 30°, 45°
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Zenith angular distribution for E0 > 2·1016 eV
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CORSIKA: Xmax reconstruction
∆Xmax = 2767 - 3437∙log10(bA-2), g∙cm-2
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PHENOMENOLOGICAL APPROACH:Experimental LDF steepness vs. zenith angle for
E0 = 3·1016 eV
~3500 events: 16.4 < log10(E0/eV) < 16.5
cosθ ΔXmax = X0/cosθ – Xmax
X0 = 965 g·cm-2
<Xmax> = 570 g·cm-2 for E0 = 3·1016 eV
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PHENOMENOLOGY: Xmax reconstruction
∆Xmax = 2870 – 3520∙log10(bA-2), g∙cm-2
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Example of internal event
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Shower front
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Example of external event
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Shower front
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Plan
Light distribution
Shower front
Pulse width
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Plan
Light distribution
Shower front
Pulse width
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Plan
Light distribution
Shower front
Pulse width
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anode
dynode
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anode
dynode
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anode
dinode
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Experimental data
3 winter seasons 2009-2010, 2010-2011 and 2011-2012165 clean moonless nights
~ 980 h of data acquisition with trigger rate ~ 2-3 Hz~7 000 000 events
Zenith angle θ ≤ 45°, Rcore < 450 m:~ 170 000 events with E0 > 6·1015 eV – 100% efficiency
~ 62 000 events with E0 > 1016 eV~ 590 events with E0 >1017 eV
Zenith angle θ ≤ 45°, Rcore < 800 m:~ 1800 events with E0 >1017 eV – 100% efficiency
~ 150 events with E0 > 3·1017 eV~ 8 events with E0 >1018 eV
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Mean Depth of EAS maximum Xmax g·cm-2
PRELIMINARY
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EXPERIMENT:Mean logarithm of primary mass.PRELIMINARY
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Mean logarithm of CR atomic numberBerezhko 2009
Experiment:
ATIC-2 (Panov et al. 2006)
JACEE (Asakimori et al. 1998)
KASKADE (QGSJET, SIBYLL) (Hörandel 2005)HiRes (QGSJET, SIBYLL) (Abbasi et al. 2005)
CRs from SNRs +CRs from AGNs
Yakutsk CRs from SNRs +reacceleration +Extragalactic CRs
Accurate determination of CR composition at ε = 1017- 1019 eV is neededto find transition from galactic to extragalactic CR component
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CONCLUSION
1. Primary mass composition changes from light (He) at the knee to heavy at 3·1016 eV
2. The mass composition is heavy till at least 1017 eV3. More statistics is needed at the energy range 1017 – 1018 eV
PLANS
1.More statistics.2.The new simulations. 3.Xmax distribution analysis.
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Thank you!