1 Tibet Air Shower Array plus Muon Detector Array for the 100 TeV Gamma-Ray Wide Sky Survey K. Kawata For the Tibet ASCollaboration ICRR, University of Tokyo Locating PeV Cosmic-Ray Accelerators: Future Detectors in Multi-TeV Gamma-Ray Astronomy Adelaide 6 - 8 December 2006
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1 Tibet Air Shower Array plus Muon Detector Array for the 100 TeV Gamma-Ray Wide Sky Survey K. Kawata For the Tibet AS Collaboration ICRR, University.
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Tibet Air Shower Arrayplus Muon Detector Array
for the 100 TeV Gamma-RayWide Sky Survey
K. Kawata
For the Tibet AS Collaboration
ICRR, University of Tokyo
Locating PeV Cosmic-Ray Accelerators: Future Detectors in Multi-TeV Gamma-Ray AstronomyAdelaide 6 - 8 December 2006
X.Y.Zhang,7 Y.Zhang,3 Yi Zhang,3 Zhaxisangzhu,6 and X.X.Zhou 8
(1) Dep. of Phys., Hirosaki Univ., Hirosaki, Japan(2) Dep. of Phys., Saitama Univ., Saitama, Japan(3) Key Lab. of Particle Astrophys., IHEP, CAS, Beijing, China(4) Fac. of Eng., Yokohama National Univ., Yokohama , Japan(5) Dep. of Phys., Hebei Normal Univ., Shijiazhuang, China(6) Dep. of Math. and Phys., Tibet Univ., Lhasa, China(7) Dep. of Phys., Shandong Univ., Jinan, China(8) Inst. of Modern Phys., South West Jiaotong Univ., Chengdu, China(9) Dep. of Phys., Yunnan Univ., Kunming, China(10) Fac. of Eng., Kanagawa Univ, Yokohama, Japan(11) Fac. f of Educ., Utsunomiya Univ., Utsunomiya, Japan(12) ICRR., Univ. of Tokyo, Kashiwa, Japan(13) Dep of Phys., Konan Univ., Kobe, Japan(14) Fac. of Systems Eng., Shibaura Inst. of Tech., Saitama, Japan
(15) Dep. of Phys., Shinshu Univ., Matsumoto, Japan(16) Center of Space Sci. and Application Research, CAS, Beijing, China(17) Phys. Dep. and Tsinghua Center for Astrophys., Tsinghua Univ., Beijing, China (18) Advanced Research Inst. for Sci. and Engin., Waseda Univ., Tokyo, Japan(19) Advanced Media Network Center, Utsunomiya University, Utsunomiya, Japan(20) National Inst. of Info., Tokyo, Japan(21) Tochigi Study Center, Univ. of the Air, Utsunomiya, Japan(22) Tokyo Metropolitan College of Industrial Tech., Tokyo, Japan(23) Max-Planck-Institut fuer Physik, Muenchen, Germany (24) Shonan Inst. of Tech., Fujisawa, Japan(25) RIKEN, Wako, Japan(26) School of General Educ.,Shinshu Univ., Matsumoto, Japan
The Tibet AS Collaboration
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Contents
1. Introduction2. Tibet Air Shower Array Tibet Muon Detector Array3. Sensitivity Simulation4. Outlook5. Costs6. Summary
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1. IntroductionCosmic ray Acceleration Origin
New 14 HESS sources
Hard spectral indices
Faint in other wavelengths
Theoretical
possibility
• 0 decay• IC*• …
• Old SNR• Asymmetric PWN• …
Key observation 100 TeV region Wide sky survey
Aharonian et al, ApJ, 636, 777 (2006)
* >100TeV IC is difficult due to sync. cooling & KN effect
Soil + Cherenkov det. (Tibet MD) - GEANT4 8.0 Reflectance at walls 70% Att. length ~40m@400nm (Dependant on wave length)
Quantum Eff. ~20%@400nm (Dependant on wave length)
Accidental muons 300 Hz/m2 x 9540m2 x 200 ns = ~0.57 muons/an air shower (Poisson noise distribution)
AS
MD
MD (Type2)
AS
3. Sensitivity Simulation
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Air Shower Reconstruction by AS Array Energy - Sum of particle density by all scintillation detectors (we do not use the lateral function in this talk.)Direction - Relative timings at each detectors
~10 TeV Air Shower (Simulation)
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Energy & Angular Resolution (Simulation)
10 TeV ~+70%-40%100 TeV ~+40%-30%(Gamma rays)
10 TeV ~0.4 degrees100 TeV ~0.2 degrees(Gamma rays)
Energy Resolution Angular Resolution
two typical air-shower size bins
~10 TeV
~100 TeV
10TeV 100TeV 1000TeV
11NPE
~100TeV
NPE
~10TeV
Muon Number vs. Shower Size (Type2 Simulation)
( Shower Size)
NP
E(
Muo
n N
um
ber)
10TeV 100TeV 1000TeV
20%50%80%
: Sum of particle density by all scintillation det. Shower SizeNPE:Sum of photoelectrons by all muon det. Muon number G CR
G CR
0
0
10TeV:Cut value NPE=~40Background: ~99% RejectionGamma rays: ~60% SurvivalSensitivity: ~6 times Improved
100TeV:Cut value NPE=~600Background: >99.8% RejectionGamma rays: ~100% SurvivalSensitivity: >20 times Improved
(gamma)
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Survival Efficiency (Type2 Simulation)
CR
Gamma
10TeV 100TeV 1000TeVE:10 TeV:Cut value NPE=~40Background: ~99% RejectionGamma rays: ~60% SurvivalSensitivity: ~6 times Improved
100 TeV:Cut value NPE=~600Background: >99.8% RejectionGamma rays: ~100% SurvivalSensitivity: >20 times Improved Almost background free!
~new 14 detected (SNR-like)~new 14 detectable?? (SNR-like)optimistic value?But, could not be 0?
Expectation of the number of SNR-like sources in the Northern Sky
Aharonian et al, ApJ, 636, 777 (2006)
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5. Costs
Items Remarks Unit price
(US $)
Quantity Total
(US $)
PMT 20” PMT 5,000 368 1.84M
ElectronicsADC, TDC, HV,
Cable, …800 184 0.147M
Water poolConstruction fee
(Waterproof paint, Concrete, … )
250/m2 9,540m2 2.39M
Water purification & circulation
MF filters, … 0.15M
Others +
Total (US $) 4.5M +
Total ~5M US$
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Tibet MD Project 50,000 m2 Tibet air shower array + 9,540 m2 Water cherenkov muon detector array
~5M US$ - 100 TeV gamma-ray wide sky survey.
Sensitivity simulation Detailed simulation was done (two configurations). F(>100TeV) ~2 x 10-15 cm-2 s-1 (1 calender year, 5or 10 events). Improve sensitivity by an order of magnitude. Inner MDs are very important.
Candidates of 100 TeV sources in the northern sky Promising: Crab, TeV J2032+4130, HESS J1837-069, MGRO J2019+37 Interesting: Cas A, HESS J1834-089, LS I +61 303 (Need several years)
+ several new sources?
6. Summary
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Tibet AS+MD200?~
CASA-MIA1991~1996
Milagro2000~
KASCADE1996~
Grapes-III2001~
Location 30.102N 90.522E Tibet 4300m(606g/cm2)
40.2N 112.8WUtah1500m(870g/cm2)
35.9N 106.7W NewMexico 2650m (750g/ cm2)
49.1 N8.4E Karlsruhe 110m(1022 g/cm2)
11.4N 76.7EOoty 2200m(800 g/cm2)
EnergyETH75%
1-104.5TeV10TeV
50-104.5TeV60TeV
~0.1TeV-?10TeV
100-104.5TeV260TeV
10-104TeV?
Energy Resolution
40% (100TeV) 100%(100TeV) ? ? ?
AngularResolution
0.4° (>10TeV)0.2° (>100TeV)
2 °(>~100TeV)0.5°(>~700TeV)
1°(>~1TeV)0.55°(>~600TeV)
?
AS Eff Area(Particle coverage)
50,000m2
Scinti. (0.9%)230,000m2
Scinti. (0.7%) 4,800m2 Water (100%) (with Outrigger 34,000m2)