9/26/2006katsushi arisaka, ucla 1 katsushi arisaka university of california, los angeles department...
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![Page 1: 9/26/2006Katsushi Arisaka, UCLA 1 Katsushi Arisaka University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu Unveiling](https://reader034.vdocument.in/reader034/viewer/2022051517/56649d4e5503460f94a2e69e/html5/thumbnails/1.jpg)
9/26/2006 Katsushi Arisaka, UCLA 1
Katsushi ArisakaKatsushi Arisaka
University of California, Los Angeles
Department of Physics and Astronomy
Unveiling the Mystery of Ultra High Energy Cosmic
Rays
Unveiling the Mystery of Ultra High Energy Cosmic
Rays
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9/26/2006 Katsushi Arisaka, UCLA 2
Energy Spectrum of Cosmic Rays
• Energy Spectrum ~ E-3
• The spectrum extends beyond 1020 eV (=1011 GeV =100 EeV).
• Beyond 1020 eV, Flux is only one particle per km2-century.
TeVGeV EeVPeV
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9/26/2006 Katsushi Arisaka, UCLA 3
Talk Outline
Physics Motivation Why is 1020 eV so special?
Past and Ongoing Experiments AGASA HiRes Pierre-Auger
Preliminary Results from Pierre-Auger Energy Spectrum Composition Angular Distribution
Future Projects
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9/26/2006 Katsushi Arisaka, UCLA 4
Physics Motivation
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9/26/2006 Katsushi Arisaka, UCLA 5
Particle Physics in Early Universe
10-45sec
10-40
10-35
10-30
10-25
10-20
10-15
10-10
10-5
105 sec
1
1 year103
106
109 year
Time (sec)
Temp. (oK)
1018
1015
1012
109
1PeV
1TeV
1GeV
1MeV
1KeV
1eV
1030
1025
1020
1015
1010
105
1
Energy (GeV)
10-3eV
Planck
EW
Now
GUT
Gra
vit
atio
n
Str
on
g
We
ak
Ele
ctr
om
agn
eti
c
FundamentalInteraction
Ele
ctr
o-W
eak
GU
T
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9/26/2006 Katsushi Arisaka, UCLA 6
Particle Physics in Early Universe
10-45sec
10-40
10-35
10-30
10-25
10-20
10-15
10-10
10-5
105 sec
1
1 year103
106
109 year
Time (sec)
Temp. (oK)
1018
1015
1012
109
1PeV
1TeV
1GeV
1MeV
1KeV
1eV
1030
1025
1020
1015
1010
105
1
Energy (GeV)
10-3eV
Planck
EW
Now
GUT
Super Symmetry
Super StringQuantum GravityGrand Unification
Inflation
Dark Matter
Dark Energy
Big Bang!
Baryogenesys
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9/26/2006 Katsushi Arisaka, UCLA 7
Particle Physics in Early Universe
10-45sec
10-40
10-35
10-30
10-25
10-20
10-15
10-10
10-5
105 sec
1
1 year103
106
109 year
Time (sec)
Temp. (oK)
1018
1015
1012
109
1PeV
1TeV
1GeV
1MeV
1KeV
1eV
1030
1025
1020
1015
1010
105
1
Energy (GeV)
10-3eV
Planck
EW
Now
GUT
Accelerator
Telescope
UHE Cosmic Rays
Inflation
Dark Matter
Dark Energy
Big Bang!
Baryogenesys
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9/26/2006 Katsushi Arisaka, UCLA 8
Top-down or Bottom-up?
10-45sec
10-40
10-35
10-30
10-25
10-20
10-15
10-10
10-5
105 sec
1
1 year103
106
109 year
Time (sec)
Temp. (oK)
1018
1015
1012
109
1PeV
1TeV
1GeV
1MeV
1KeV
1eV
1030
1025
1020
1015
1010
105
1
Energy (GeV)
10-3eV
Planck
EW
Now
GUT
Big Bang
Active Galactic Nuclei
Gamma Ray Burst
Supernova Neutron Star Black Holes
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9/26/2006 Katsushi Arisaka, UCLA 9
The Extreme Universe
Pulsar
GRB
AGN
SNR
Radio Galaxy
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9/26/2006 Katsushi Arisaka, UCLA 10
Possible Acceleration Sites
• Several possible accelerators in nature up to 1020 eV.
• Extremely difficult to accelerate above 1020 eV.
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9/26/2006 Katsushi Arisaka, UCLA 11
Interaction Length of UHE Protons
Blasi, astro-ph/0307067
PhotopionLoss Length
InteractionLength
PairProduction
10Mpc
1Gpcp + (2.7oK) p + ’s
GZK Cutoff
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9/26/2006 Katsushi Arisaka, UCLA 12
E=1019 eVE=1020 eV E=1018 eV
Trajectory of Protons in the Galaxy
Galactic Magnetic Field ~ 2 µG
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9/26/2006 Katsushi Arisaka, UCLA 13
Deflection of Protons >41019eV
Dolag, astro-ph/0310902
0o360o
< 100 Mpc Extra Galactic Magnetic Field ~ 1 nG
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9/26/2006 Katsushi Arisaka, UCLA 14
1019 eV
1021 eV
1020 eV
1018 eV
Top-Down?
GZK?
Bent by Extra-Galactic B (~nG)
Ankle
Charge Particle Astronomy
Trapped by Inner-Galactic B (~G)
Bottom-Up
UHE Gamma Rays
UHE Neutrinos
Straight Trajectories
?
Rich Physics and Astronomy
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9/26/2006 Katsushi Arisaka, UCLA 15
Past and Ongoing Experiments
AGASAHiResPierre-Auger
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9/26/2006 Katsushi Arisaka, UCLA 16
Detection Technique
e
Fluorescence Fluorescence Detector (FD)Detector (FD)
10km
~ 27Xo
~ 11I
MC Simulation of 1019eV Proton Shower
Surface Detector (SD)
AGASA
HiRes
Pierre-Auger
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9/26/2006 Katsushi Arisaka, UCLA 17
SD vs. FD
SD (Surface Detector) used by AGASA. Operational 24 hours a day, but Sparse sampling at the tail of shower.
FD (Fluorescence Detector) used by HiRes. Totally calorimetric energy measurement, but ~10% duty factor (only at moonless night).
Pierre-Auger utilizes both!
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9/26/2006 Katsushi Arisaka, UCLA 18
Akeno Giant Air Shower Array
0 4km
• 111 Electron Detectors• 100 km2
• 27 Muon Detectors• Operation 1991 - 2004
M. Teshima
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9/26/2006 Katsushi Arisaka, UCLA 19
The Highest Energy Event by AGASA
2.5 x 102.5 x 1020 20 eV on 10 May 2001eV on 10 May 2001
M. Teshima
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9/26/2006 Katsushi Arisaka, UCLA 20
Energy Spectrum by AGASA
M. Teshima
Bottom-upwith GZK Cutoff
Top-down?
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9/26/2006 Katsushi Arisaka, UCLA 21
Two HiRes Detectors HiRes1 21 mirrors, 1 ring 3o < altitude < 17o
HiRes212.6 km SW of HiRes1.42 mirrors, 2 rings3o < altitude < 31o
G. Thomson
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9/26/2006 Katsushi Arisaka, UCLA 22
Stereo View by HiRes 1 & 2
C. Finley
HiRes 1
HiRes 2
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9/26/2006 Katsushi Arisaka, UCLA 23
Energy Spectrum by HiRes
Consistentwith GZK Cutoff
C. Finley
(1999-2004)(1996-2005)
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9/26/2006 Katsushi Arisaka, UCLA 24
Energy Spectrum by HiRes
C. Finley
Consistent withGZK Cutoff !!
Galactic
Extra-Galactic
(1999-2004)(1996-2005)
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9/26/2006 Katsushi Arisaka, UCLA 25
Energy Spectrum
Ralph Engel
AGASA (SD)
HiRes (FD)
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9/26/2006 Katsushi Arisaka, UCLA 26
Pierre-Auger
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9/26/2006 Katsushi Arisaka, UCLA 27
Pierre Auger Collaboration
15 Countries 50 Institutions~350 Scientists
Italy Argentina
Czech Republic Australia France BrazilGermany Bolivia* Poland MexicoSlovenia USASpain Vietnam* United Kingdom
*Associate Countries
Jim Cronin Alan Watson
Founders
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9/26/2006 Katsushi Arisaka, UCLA 28
#S
#SS
Pierre-Auger Observatory
N
Northern Augerin Colorado
Southern Augerin Argentina
50km
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9/26/2006 Katsushi Arisaka, UCLA 2950km
Southern-Auger in Argentina
Surface Detector 1600 Water Tanks 1.5 km spacing 3100 km2
Fluorescence Detector 4 Telescope Sites 6 Telescopes per Site 24 Telescopes Total
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9/26/2006 Katsushi Arisaka, UCLA 30Aerial view of Los Leones Fluorescence Site
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9/26/2006 Katsushi Arisaka, UCLA 31
Six Telescopes looking at 30o x 30o each
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9/26/2006 Katsushi Arisaka, UCLA 32
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9/26/2006 Katsushi Arisaka, UCLA 33
corrector lens
Camera440 PMTs
11 m2 Mirror
UV-Filter 300-400 nm
Corrector Ring
Optical
Shutter
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9/26/2006 Katsushi Arisaka, UCLA 34Tanks aligned seen from Los Leones
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9/26/2006 Katsushi Arisaka, UCLA 35
Water Tank on Site
Real water tank under operation at Malargue
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9/26/2006 Katsushi Arisaka, UCLA 36
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9/26/2006 Katsushi Arisaka, UCLA 37
Installing Electronics
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9/26/2006 Katsushi Arisaka, UCLA 38
Southern Auger as of Sept. 2006
50km
1100 Water Tanks (out of 1600)~ 20 x AGASA
AGASA
Los Leones
Coihueco
Los Marados
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9/26/2006 Katsushi Arisaka, UCLA 39
All the rest will be deployed by Summer of 2007
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9/26/2006 Katsushi Arisaka, UCLA 40
Comparison of Integrated Aperture
100
1000
10000
100000
1000000
1985 1990 1995 2000 2005 2010 2015 2020Year
Inte
gra
ted
Ap
ertu
re (
km2 *s
tr*y
ear)
Fly'e Eye
AGASA
HiRes
Auger-S
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9/26/2006 Katsushi Arisaka, UCLA 41
A Typical Event (“Young” Shower, Zenith~35o)
203
204
116
114S(1000)~81019eV
S(1000)~71019eV
203
204
116
114
215
217
Lateral Distribution Function
206
1.05
( ) 1700 700
(1000) sec
r rS r k
m m
E S f
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9/26/2006 Katsushi Arisaka, UCLA 42
A Typical Event (“Young” Shower, Zenith~35o)
EM
EM
Muon
Muon
203
204
116
114
203
204
215
217
(nsec)
S(1000)~71019eV
Muon
EM
EM
Muon
217
215
Lateral Distribution Function
206
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9/26/2006 Katsushi Arisaka, UCLA 43
A Typical Inclined Event(“Old” Shower, Zenith~72o)
Muon
~61019eV
Direct Cherenkovon PMT 1
Muon
Lateral Distribution Function
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9/26/2006 Katsushi Arisaka, UCLA 44
A Stereo-Hybrid Event (Zenith~70o)
Fluores.Telescope
Fluores.Telescope
~81019eV
Lateral Distribution Function
26 June 2004
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9/26/2006 Katsushi Arisaka, UCLA 45
A Stereo-Hybrid Event (Zenith~70o)
Coihueco
Los Leones
Fluores.Telescope
Fluores.Telescope
26 June 2004
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9/26/2006 Katsushi Arisaka, UCLA 46
A Stereo-Hybrid Event (Zenith~70o)
Los Leones
Pulse findingTime vs fit
Coihueco
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A Stereo-Hybrid Event (Zenith~70o)
Coihueco
Los Leones
Time vs fitShower Profile
~61019eV
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Preliminary Results
Energy SpectrumCompositionAngular Distribution
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Energy Spectrum
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S(1000) at 38o vs. FD Energy
S(1000) at 38o
1 EeV 10 EeV 100 EeV
50
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Proton, SIBYLL (AIRES)
Proton, QGSJET (AIRES)
Proton, GEISHA, QGSJET (CORSIKA)
Proton, FLUKA, QGSJET (CORSIKA)
Proton, GEISHA, QGSJET2 (CORSIKA)
Proton, FLUKA, QGSJET2 (CORSIKA)
Iron, SIBYLL (AIRES)
Iron, QGSJET (AIRES)
50
34
(VEM)
SD+MC Average ( 18%)
FD Average ( 30%)
Fixed Beta
Floating Beta
Proton, SIBYLL (AIRES)
Proton, QGSJET (AIRES)
Proton, GEISHA, QGSJET (CORSIKA)
Proton, FLUKA, QGSJET (CORSIKA)
Proton, GEISHA, QGSJET2 (CORSIKA)
Proton, FLUKA, QGSJET2 (CORSIKA)
Iron, SIBYLL (AIRES)
Iron, QGSJET (AIRES)
Summary of S(1000) at 38o and 10 EeV
Proton
Iron
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9/26/2006 Katsushi Arisaka, UCLA 52
Energy Spectrum E3 (FD Energy)
Presented at ICRC 2005(only one year of data)
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9/26/2006 Katsushi Arisaka, UCLA 53
Energy boosted by 30%
Energy Spectrum E3 (SD+MC Energy)
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9/26/2006 Katsushi Arisaka, UCLA 54
Summary of Energy Spectrum
Energy spectrum based on FD Energy is consistent with HiRes. fits reasonably well with the GZK cutoff. Injection spectrum of 1/E2.6.
Energy spectrum based on SD+MC Energy is similar to AGASA. a hint of Super-GZK events? but not as many as AGASA observed.
Possible Causes: FD: Poor measurement of fluorescence photon yield. SD: MC can not produce enough number of muons.
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9/26/2006 Katsushi Arisaka, UCLA 55
Composition
Constant Intensity CutPhoton Flux LimitNeutrino Flux Limit
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Constant Intensity Cut
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9/26/2006 Katsushi Arisaka, UCLA 57
S(1000) vs. Sec()
60o45o30o 38o
50 VEM
34 VEM
SD+CIC
Iron
Proton
Photon
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9/26/2006 Katsushi Arisaka, UCLA 58
S(1000) MC/CIC vs. sec() at 10 EeV
60o45o30o 38o
FD+CIC
SD+CIC
Sensitive to Xmax
Sensitive to Muon Richness
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9/26/2006 Katsushi Arisaka, UCLA 59
Muon Richness vs. Xmax
Iron/QGSJET
Iron/SIBYLL
Proton/QGSJET
Proton/SIBYLL
Gamma/QGSJETGamma/SIBYLL
CICXmax Proton likeMuon Richness Iron like
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Photon Limit
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9/26/2006 Katsushi Arisaka, UCLA 61
What is Dark Matter?
Super HeavyDark Matter
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9/26/2006 Katsushi Arisaka, UCLA 62
Super Heavy Dark Matter fit to AGASA
Photon flux can be predicted by decay of Super Heavy Dark Matter based on AGASA data
Gelmini, et al, astro-ph/0506128
AGASA Data
Bottomup Proton
P from SHDM
from SHDM
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Photon (MC Simulation)
Photon (> 10 EeV)
Muon Rich Muon Poor
Dee
p X
max
S
hallo
w X
max
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9/26/2006 Katsushi Arisaka, UCLA 64
Proton (MC Simulation)
Proton (> 20 EeV)
Muon Rich Muon Poor
Dee
p X
max
S
hallo
w X
max
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Expected Photon Fraction Limit
Super Heavy Dark Matter
Topological Defects
Z Burst
Expected Limit
GZK Photons
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Expected Sensitivity on Photon Flux
Expected Limit
Super Heavy Dark Matter
Topological Defects
Z Burst
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Future Sensitivity on Photon Flux
Topological Defects
Z BurstExpected Limit
2010
2015
Super Heavy Dark Matter
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9/26/2006 Katsushi Arisaka, UCLA 68
Summary of Photon Limit
Pierre-Auger Observatory Surface Detector is a background free photon detector. Extremely sensitive to top-down models.
Pierre-Auger already has enough data to test top-down models inspired by the AGASA spectrum. Analysis of real data is being prepared for
publication.
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Neutrino Limit
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Detection of Neutrino
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9/26/2006 Katsushi Arisaka, UCLA 71
Neutrino Sensitivities (per year)
by Dmitri Semikoz
AGNCore
ExoticHadron
GZK(Max)
GZK(W&B)
TopDown
AUGER
AUGER e
ICECUBE
AMANDA II
ANITA 30 days
ray BoundRICE
Atmospheric
EUSO
Strong DIS
No DIS
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Angular Distribution
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9/26/2006 Katsushi Arisaka, UCLA 73
Clustering of UHECR (>40 EeV) by AGASA
• 6 doublets and 1 triplet within 2.5o cone.
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AGASA Auto-Correlation
40 EeV 2.5o
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9/26/2006 Katsushi Arisaka, UCLA 75
HiRes Correlation with BL Lacs
Gorbunov et al., astro-ph 0406654
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Six combinations were tested with independent data (with m<18):
Note: These are not independent results: the samples overlap. Analysis has been a posteriori, so F values are not true probabilities. Must be tested with independent data
R.U. Abbasi et al., Astrophys.J. 636 (2006) 680 [astro-ph/0507120]
New HiRes Analysis
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9/26/2006 Katsushi Arisaka, UCLA 77
Angular Resolution of Auger SD
>10 EeV
>3 EeV
>1 EeV
HiRes (Stereo)
AGASA
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AGASA Galactic Center
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Auger Galactic Center
AGASA
Sugar
G.C
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9/26/2006 Katsushi Arisaka, UCLA 80
Summary of Auger
Pierre-Auger is finally a reality. SD: 30 times larger than AGASA. (2/3 complete) FD: 4 stations of HiRes-like telescopes. (3/4 complete.)
Hybrid observation is giving critical information to determine the energy and composition. Why AGASA and HiRes differ ~30% in energy? Cosmic rays appear much richer than expected!
New physics results are expected soon. Energy Spectrum Photon and Neutrino limits, or discovery! Clustering, BL Lac correlation…
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Future Projects
TAAuger-NorthEUSO
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TA(Telescope Array)
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9/26/2006 Katsushi Arisaka, UCLA 83
3 x Fluorescence StationsAGASA x 4
576 CountersAGASA x 9
Low Energy Extension
TALETALE
Comm. Tower
CLF
Millard County in Utah / USA
M. Fukushima
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9/26/2006 Katsushi Arisaka, UCLA 84M. Fukushima
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9/26/2006 Katsushi Arisaka, UCLA 85M. Fukushima
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9/26/2006 Katsushi Arisaka, UCLA 86M. Fukushima
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350 assembled in Utah in Feb - Mar 2006, 150 to be produced after July18 test-deployed. 500 to be deployed in several batches this year.
M. Fukushima
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9/26/2006 Katsushi Arisaka, UCLA 88
Auger-South Upgradeand Auger-North
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9/26/2006 Katsushi Arisaka, UCLA 89
1019 eV
1021 eV
1020 eV
1018 eV
Top-Down?
GZK?
Bent by Extra-Galactic B (~nG)
Ankle
Charge Particle Astronomy
Trapped by Inner-Galactic B (~G)
Bottom-Up
Straight Trajectories
?
Original AugerSD
Hybrid
Infill + 2-FD
Auger-South
Expanded Auger
Auger-North
Future Expansion of Auger
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Auger-North in Colorado State
Colorado State
Auger-North
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Auger-North
Total area: 10,000 km2
100 x AGASA 3 x Auger-South
4000 surface detector 1 mile (1.6 km) spacing 84 x 48 mile rectangle
Lamar
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Pruitt Mound in Colorado Site
View to west, Sept 23, 2003
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Neutrino Sensitivities
by Dmitri Semikoz
AGNCore
ExoticHadron
GZK(Max)
GZK(W&B)
TopDown AUGER (S+N, 5 years)
AUGER
AUGER e
ICECUBE
AMANDA II
ANITA 30 days
ray BoundRICE
Atmospheric
EUSO
Strong DIS
No DIS
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EUSO(Extreme UniverseSpace Observatory)
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Observation Principle of EUSO
F. Kajino
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9/26/2006 Katsushi Arisaka, UCLA 96
JEM-EUSO Telescope at ISS
JEM-EUSO Telescope will be attached to Exposure Facility of Japanese Experiment Module (JEM/EF) of ISS in about 2012.
Vertical Mode Tilted Mode
Larger effective area with ~45°tiltF. Kajino
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9/26/2006 Katsushi Arisaka, UCLA 97
JEM-EUSO Telescope Structure
Multi-pixel PMT
Electronics
Fresnel Lens
F. Kajino
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Shower Image on the EUSO Focal Surface
Y
X
20 events of 1020eV proton showers are superimposed on the EUSO focal surface with 192 k pixels.
x-t view y-t view
F. Kajino
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Summary
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Comparison of Integrated Aperture
100
1000
10000
100000
1000000
1985 1990 1995 2000 2005 2010 2015 2020Year
Inte
gra
ted
Ap
ertu
re (
km2 *s
tr*y
ear)
Fly'e Eye
AGASA
HiRes
Auger-S
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9/26/2006 Katsushi Arisaka, UCLA 101
Comparison of Integrated Aperture
100
1000
10000
100000
1000000
1985 1990 1995 2000 2005 2010 2015 2020Year
Inte
gra
ted
Ap
ertu
re (
km2 *s
tr*y
ear)
Fly'e Eye
AGASA
HiRes
Auger-S Auger-N
Auger (S+N)
TA
EUSO
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Conclusions
The origin of UHECR is still unknown. Any events beyond the GZK cutoff? If so, signals from the early Universe??
Pierre-Auger (South) is nearly complete. Already 2.5 years of data with partial detectors.
• ~3 x AGASA statistics Several publications expected soon.
• Energy Spectrum, Photon Limit, Angular Distribution…
More experiments will follow Auger. TA, Auger-North, EUSO…