Ultra High Energy Cosmic Rays Origin and Propagation of UHECRs

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Ultra High Energy Cosmic Rays-- Origin and
Propagation of UHECRs --

• M.Teshima
• Max-Planck-Institut für Physik, München
• Erice Summer School
• July. 2004

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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
• Heavy relic particles in our galactic Halo
• Rectilinear propagation
• Clusters of events

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Background Radiations
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Greisen-Zatsepin-Kuzmin (GZK) effect
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Energy Spectrum modification by the interaction
with CMBRby Yoshida and Teshima
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Berezinsky 2004
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The history of the energy of C.R.traveling CMBR
sea
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Energy loss time of nucleiYamamoto et al. 2003
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Energy spectrum of Nucleiby T.Wibig 2004
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GZK effect

• Energy Spectrum of cosmic rays are modified
  suppression above 4x1019eV
• Secondary particles
• po ? 2? ? cascade
• ? pair creation
• e Inverse compton, synchrotron
• p? ?
• Generally, proton supply the energy to neutrino
  and gammas

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Attenuation length p, ?, e
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By G.Sigl
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Z-burst model violates EGRET diffuse gamma flux
(G.Sigl)
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Optimistic Z-burst model (Only neutrino produced
at sources) by G.Sigl and D.Semikos
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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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Candidates for EHE C.R. accelerator
A.G.N.
Pulsar
SNR
GRB
Radio Galaxy Lobe
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Matter and galaxies within 93Mpc
By A.Kravtsov
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Cosmic Ray Energy Spectrumfrom GRBs(10100) by
E.Waxman
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Cosmic Ray Propagation inGalactic Disk and Inter
Gal.
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Arrival Direction Distribution gt4x1019eVzenith
angle lt50deg.

• Isotropic in large scale ? Extra-Galactic
• 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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Expected Auto correlationYoshiguchi et al. 2004
Number density of sources 10-5 Mpc-3
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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

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Ultra High Energy Cosmic Rays-- Next generation
experiments,mainly about EUSO --

• M.Teshima
• Max-Planck-Institut für Physik, München
• Erice Summer School
• July. 2004

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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
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See the presentation by H.Klages
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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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TA Scintillator Development
proto 50 cm x 50 cm, 1cm thick
Wave Length Shifter Fiber readout 50
modules used in L3 for 2.5 years.
cutting 1.5 mm deep groove
WLS BCF-91A ( 1 mm F )
Final 3 m2 by 2 PMT readout.
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Telescope 3mF Spherical Mirror
TA Telescope Development
Electronics 100 ns 14 bit AD conv. Signal
recognition by FPGA
Imaging Camera16X16 PMT Array
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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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Energy Threshold
5x1019eV
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Possible EUSO measurement
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Exposure (AGASA unit)
EUSO
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Angular Resolution
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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
Bright Future ofUHECR observation!!
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EUSO in ISS
Cosmic Ray observations
Accommodation in ISS