telescope array for extremely high energy cosmic rays. july 30th, 2003 masaki fukushima
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Telescope Array for Extremely High Energy Cosmic Rays.
July 30th, 2003Masaki FUKUSHIMAICRR, Univ. of Tokyo
Galactic Extra‐Galactic
HiRes: Composition Changefrom Heavy to Light
Ankle Structure
0
3
2
1
MagneticConfinement
AGASA:Anisotropy
towards Galactic Center
We are starting to collect
First samples of extra-galactic
Matter-Particles
Galactic to extra-galactic transition
Energy Spectrum of the Highest Energy Cosmic Rays
There is a Horizon forCosmic Rays with Energy
exceeding 10 20 eV
by GZK mechanism
Cosmic Rays with Energy above GZK cutoff exists.
No obvious astronomical counterpart within ~ 50 Mpc.
Log ( ENERGY [ eV ])
L
og (
FLU
X x
E3 )
AGASA
AGASA
Arrival Directions and Clustering “Point”
Sources
Isotropic Distribution
E > 10 19 eV
E > 10 19.6 eV > 10 20.0 eV
> 10 19.6 eV
> 10 19.0 eV
Possibilities of creating continued spectrum exceeding GZK-cutoff
mechanism reason signature
1Decay of super-heavy X
Particle ( big bang origin )
concentration in
galactic halo
γ+ν
gal. center
2EHEν +C ν B → Z0 C ν B over-density
in super-clusterγ + ν
EHEν with extra-dimensionσ ~ 100 mB
( shower in atmosph. )
shower-profile
3 Violation of Lorentz inv. No Δ(1232) prod. proton
4“Ordinary” galaxies ;Excess in super-cluster
over-density ~10within 50 Mpc
point source
5 Experimental Problem? Statistics, SystematicsAcceleration problem unresolved for 2-4.
“AGASA” x 10 Plastic Scintillator Array
+3-station “HiRes”
Fluorescence Telescope +
Low energy extension
20 km
20 km
Millard CountyUtah/USA
24 x 24 Scintillators(1.2 km spacing)
AGASA x 9
3 x Fluorescence StationsAGASA x 10
TA Detector Configuration Exp Res.
AGASA 1.60
TA SD ~1.00
TA FD 0.60
TA Hyb. 0.40
Low Energy HybridExtension
Energy Calibration by SD-FD Coincidence Meas..
SD - FD ; Two Independent Methods for Energy Determination.
○ E > 1019 eV ~ 100 ev. / Year ○ E > 1020 eV ~ 1 ev. / Year
Phase-1 Hybrid TA gives ENERGY SCALE by ● SCINTILLATOR ARRAY● AIR FLUORESCENCE
Energy Spectrum by Only-one, Unique Energy Scale
( Systematic Energy Uncertainty < 10% Aimed )
Calibration
e /γ meas.
Comparison
proto: 50 cm x 50 cm, 1cm thick Wave Length Shifter Fiber readout 50 modules used in L3 for 2.5 years.
WLS: BCF-91A( 1 mm Φ )
cutting 1.5 mm deep groove
Final: 3 m2 by 2 PMT readout.
TA Scintillator Development
Energy Loss in the Air “μ” Density at 1km for p/Fe
AUGER water tank simulation
p Fe
EA
IR /
E0
~10% ofTotal Energy
~90% ofTotal Energy
MODELp / Fe
Uncertainty
Plastic Scintillator: Water Tank:
e + e - μ + μ - & soft γ
Electron Measurement by Scintillator● Reasonable resolution● Small model / composition dependence
Imaging Camera :16X16 PMT Array
Electronics :200 ns continuous ADC
+Signal recognition
by software
Shower Image
1 0 x 1 0 FoV/PMT
Telescope : 3m Φ Spherical Mirror
TA Telescope Development
①
③②
3 independent energy meas.for 60% of events at 1020 eV
Estimate of Systematics ・ Atmosph. Clarity ・ Cherenkov Light
3 Fold Stereo Measurement
Shoot electron Linac beam into the sky.
20 MeV / particle x 109 ppp = 2 x 1016 eV total energy deposit. Absolute End-to-End energy calibration. Feasibility study
20 MeV 40 MeV100 m away 100 m away
望遠鏡
カメラ 東工大:垣本・荻尾、 愛媛大:吉井、 武蔵工大:門多望遠鏡躯体・回路・インフ
ラ
ICRR:福島・瀧田・林田・大西・桜井・大岡・下平・鳥居、MPI:手嶋**
大気較正 近畿大:千川、 通総研:篠野回路・DAQ 全般 KEK:松田・藤井・田中・新井*、長崎総科大:田中*
地表検出器
検出器大阪市大:川上・林・吉越、 広島市大:田中、 高知大:中村
AGASA較正 山梨大:本田・橋本・石井
回路・DAQ 千葉大:吉田・河合、 放医研:内堀・安田Simulation & Analysis
-埼玉大:井上、 芝工大 : 笠原、 神奈川:日比野、東大:寺沢**
合計 31 名 米国
サイト Utah: P.Sokolsky(**), K.Martens, C.Jui, J.Mathiews, Z.Cao
Rutgers: G.Thomson,S.Schnetzer, Montana: J.Belz,
(英国) Leeds: A.Watson**
合計 9 名
Participants
* : Advisers ** : Kakenhi Reviewers
Construction Plan of Hybrid TA:
AGASA
HiRes
AUGERAUGER
SD only
SD + FD
constructionobservation
2003
SITE PREPARATION
TELESCOPE TEST IN UTAH
ARRAY PRODUCTION
ARRAY TEST IN UTAH
TELESCOPE INSTAL.
TELESCOPE PRODUCTION
ARRAY PRODUCTION
Start Hybrid Obs.
CALIB. with AGASA
Start Obs. with SD only
Telescope Array ; Summary
1. Well-defined purposes; ① Establish galactic to extra-galactic transition. ② Confirm/Refute cluster + super-GZK.
2. Seamless coverage from 1016 to 1020.5 eV.
3. Fluorescence + Surface hybrid.
4. Common technology and existing resources based on AGASA + HiRes.
5. Start measurement in 2006(SD) / 2007(+FD).
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