Ultra High Energy Cosmic Rays and space mission EUSO

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Ultra High Energy Cosmic Rays and space mission
EUSO

• M.Teshima
• Max-Planck-Institut für Physik, München
• _at_INR Moscow
• Apr. 2005

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Cosmic Ray Energy Spectrum
AGASA Energy Spectrum
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Candidates for UHE C.R. accelerator
A.G.N.
Pulsar
SNR
GRB
Radio Galaxy Lobe
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Cosmic Ray Propagation in our Galaxy

• Deflection angle 1 degree at 1020eV
• Astronomy by hadronic particles?

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Cosmic Ray Propagation inGalactic Disk and Inter
Gal.
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Full sky map of deflection angles
By K.Dolag, D.Grasso, V.Springel, and I.Tkachev
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Important Aspects of UHECRs

• GZK mechanism
• Sources must be nearby
• Secondary Gamma rays, neutrinos
• Limited candidates of accelerators in the
  Universe
• AGNs, GRBs, Colliding galaxies
• Heavy relic particles in our galactic Halo
• Linear propagation
• Clusters of events / point sources

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Exposure in ICRC2003
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Air Shower Phenomena
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AGASAAkeno Giant Air Shower Array
111 Electron Det. 27 Muon Det.
0 4km
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The Highest Energy Event (2.46 x1020eV) on 10
May 2001
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Third Highest event 97/03/30 150EeV
40 detecters were hit
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Energy Spectrum by AGASA (?lt45)
11 obs. / 1.8 exp. 4.2s Systematic error in E
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5.1 x 1016 m2 s sr
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The Energy spectrum by AGASA Red well inside
the array (Cut the event near the boundary of
array)
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HiRes Experiment Air Fluorescence detector
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HiRes NSF events200-300EeV
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HiRes I, II mono spectrum
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Recent spectra (AGASA vs. HiRes_at_Tsukuba ICRC)
vs. HiRes-II
vs. HiRes-I

• 2.5 sigma discrepancy between AGASA HiRes
• Energy scale difference by 25

vs. HiRes-stereo
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AGASA vs HiRes
by Douglas Bergman
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The energy of C.R.traveling in CMBR
In the origin they may be 1021 eV
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The Biggest event in my experimentIACT Telescope
Array(9597)
Mrk501
Mrk501
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New TeV Gamma Ray Source1ES1959650

• Low Red shift X-BL Lac z0.048
• Observation in 1998
• MJD 50956-50965 5.3 s
• MJD 50996-51023 5.0 s

• Significance Map 4x 4FOV

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Nightmare in Dec. 97in Dugway Proving Ground
Estimated Energy 1028eV A Planck Mass Scale
Event
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Matter (90Mpc) and Galaxy(45Mpc) distribution
By A.Kravtsov
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Arrival Direction Distribution gt4x1019eVzenith
angle lt50deg.

• Isotropic in large scale ? Extra-Galactic origin
• But, Clusters in small scale (??lt2.5deg)
• 1triplet and 6 doublets (2.0 doublets are
  expected from random)
• One doublet ? triplet(gt3.9x1019eV) and a new
  doublet(lt2.6deg)

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Space Angle Distribution of Arbitrary two events
gt4x1019eV
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Expected Auto correlationYoshiguchi et al. 2004
Number density of sources 10-5 Mpc-3
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By Kolb, 2003
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By Kolb, 2003
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By Kolb, 2003
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Compilation by Anchordoqui et al. 2004 a
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Compilation by Anchordoqui et al. 2004 a
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Summary origin of UHECRs

• UHECRs ?? Diffuse ?, UHE neutrinos
• Fe galactic origin or neaby galaxies
• most economical
• can not explain AGASA clusters
• P Over density of nearby sources or very hard
  energy spectrum, GRBs, AGNs
• Super Heavy Relics in our Halo
• we should see strong anisotropy
• Neutrino with large cross section
• Violation of Lorentz invariance

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Ultra High Energy Cosmic Rays-- Next generation
experiments,mainly about EUSO --
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New Projects for UHECRs
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Auger Project
Hybrid measurement 1500 water tanks 3 Air
fluorescence stations Aperture X30
AGASA Several events above 1020eV No clusters
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Telescope Array Project
X10 AGASA
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TA Detector Configuration
Millard County Utah/USA
600 Scintillators (1.2 km spacing) AGASA x 9
3 x Fluorescence Stations AGASA x 4
Low Energy Hybrid Extension
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EUSO Extreme Universe Space Observatory x300,
x3000 AGASA
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EUSO Concept

• Large Distance and Large F.O.V. ? Large Aperture
• 6x105 km2 sr
• Good Cosmic Ray detector
• 3000 times sensitive to C.R. bursts
• 1500 Giga-ton atmosphere
• Good neutrino detector
• All Sky coverage
• North and south skys are covered uniformly. ?
  sensitive to large scale anisotropy
• Complementary to the observation from the ground
• Different energy scale and systematics
• Shower Geometry is well defined
• Constant distance from detector

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Effective Area 200,000km2 1/2 Deutschland (360,00
0km2)
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Signal of photons
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Shower Track Image(M.C. Simulation)
1020eV shower zenith angle 60 degree Total
signal 700p.e.
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Atmospheric Transmissionbetter than ground based
air fluorescence detector

• Small effect by Mie scattering
• Worst 20
• Cloud go down 23km altitude in the night
• Smaller Absorption in absolute value
• x0.3
• Ground based x0.10.01

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Detector Element
Electronics
Focal Surface Support Structure
Focal Surface
Fresnel Lens 2
Entrance pupil
Fresnel Lens 1
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Euso Optics
Wide Angle and High Resolution F.O.V. -30
d?0.1
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Focal Surface DetectorBaseline design
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Hamamatsu MAPMT
New Development by Riken Group Higher Photon
Collection efficiency R8900-M16/M25 (45 ? 85)
R7600-M64
Flat Panel MAPMT Hamamatsu H8500
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SiPM for TESLA by Dolgoshein et al. MEPhI

• 3mm x 3mm was successfully
• Made in the collaboration.
• Next step
• 10mm ? or 20mm ?
• Drift Back illumination

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HLL Back illumination SiPM80-90
photo-collection eff.
Electric field structure of Micro-Pixel
Structure of Micro-Pixel
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Energy Threshold
5x1019eV
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Possible EUSO measurement
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Exposure (AGASA unit)
EUSO
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Neutrino Detection capability
Just using observables No need for Cherenkov ref.
Zenith Angle vs. Xmax
Zenith Angle vs. Shower Time width
Neutrino Showers
Proton Showers
Neutrino domain
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Neutrino sensitivity (downward neutrino)
Sensitivity 1 events/decade/year
EUSO has 10 times larger Aperture than Auger
above GZK energy
EUSO is sensitive Z-Burst, Top Down Models and
highGZK flux.
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Gamma Ray IdentificationGeomagneticCascade
Pair Production prob. Energy Direction
Xmax distribution
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New Projects for UHECRs
Golden period ofUHECR observation!!