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EUSO Science Cosmic Ray

EUSO Science Cosmic Ray. M.Teshima MPI for Physics, Munich EUSO General meeting @NSSTC HUntsuville, AL May 2003. AGASA vs HiRes (astro-ph). See new paper: Energy determination in AGASA (astro-ph/0209422). AGASA and HiRes Spectrum. Major Systematics in AGASA astro-ph/0209422. Detector

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EUSO Science Cosmic Ray

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  1. EUSO ScienceCosmic Ray M.Teshima MPI for Physics, Munich EUSO General meeting @NSSTC HUntsuville, AL May 2003

  2. AGASA vs HiRes (astro-ph) See new paper: Energy determination in AGASA (astro-ph/0209422)

  3. AGASA and HiRes Spectrum

  4. Major Systematics in AGASAastro-ph/0209422 • Detector • Detector Absolute gain ± 0.7% • Detector Linearity ± 7% • Detector response(box, housing) ± 5% • Energy Estimator S(600) • Interaction model, P/Fe, Height -10% ±15% • Air shower phenomenology • Lateral distribution function ± 7% • S(600) attenuation ± 5% • Shower front structure +5% ± 5% • Delayed particle(neutron) +5% ± 5% • Total±0% ± 18%

  5. Statistics ~2.4 σ ~1.5 σ (P.Blasi) HiRes AGASA ~2.3 σ ~4.2σ ~ 0σ ~ 0 σ Extended spectrum Super-GZK GZK-Hypothesis

  6. Arrival Direction Distribution of EHE cosmic rays >4x1019eV >1019eV

  7. The distribution of Space angle between eventsSuggest compact sources!! 5 sigma effect 3 sigma effect >1019eV >4x1019eV

  8. The number of point sources Assume the same intensity sources, fit the multiplicity distribution 120 – 430 sources

  9. Energy spectrum of Cluster events∝E -1.8+-0.5 Cluster Component

  10. EUSO Science • Study of Energy Spectrum • 4000 events above 4x1019eV • 100-1000 events above 1020eV • GZK feature? • Possibility to detect 1021eV Cosmic Rays • Study of Anisotropy • Large scale • Small scale • Chemical composition • P, Gamma, Neutrino • Neutrino Physics

  11. Number of events in each experiment

  12. 10 particle/0.1 decade EUSO 10 particle by AGASA/HiRes 1 particle/0.1 decade EUSO 1 particle by AGASA/HiRes

  13. Study of EECR Energy Spectrum

  14. Large Scale Anisotropy I • Large Scale Anisotropy • 4x1019eV (4000 events)  2% accuracy • 1020eV (1000 events)  5% accuracy • 1020eV(150 events, GZK hypothesis)  11% • Expected anisotropy • Heavy Relics in Halo; 20-30% • Matter density <100Mpc; ??? % • AGN <100Mpc; ???%

  15. Small Scale Anisotropy • Small Scale Anisotropy(4000 events) • 200~600 Sources in the sky, let’s assume 400. • Multiplicity; ~10 particles/source on average • Source identification • >8 particles necessary Pch~10-5 • ~80 sources/400 can be identified (LogS-LogN) • x50 intensity variation • Maximum multiplicity ~ 150 particles  spectrum • High Angular Resolution ~0.5deg  Identification of neutral particles • Study of GMF with 80 point sources • 4πsky coverage

  16. EUSO skymap >1020eV maximum cluster 60~70, by P.Blasi

  17. EUSO Auto correlationby P.Blasi

  18. 5 sigma detection ~0.1eV/cm2s 0.1eV/cm2s Sensitivity to Point sources

  19. 1020eV photon h~5000km Pair Electrons Synchrotron Photons ~ 100 x 1018eV Gamma Ray IdentificationGeomagneticCascade Pair Production prob. Energy & Direction Xmax distribution

  20. Summary • Super GZK particle • Yes/No • Source identification • Clusters • EUSO EHECR source catalogue ~80 • Spectrum study on some intense sources • We can discuss the GZK mechanism on known distance • Exact check of relativity • Neutral particle / charged particle  0.5 deg. Resolution • Flare detection? • Chemical Composition • P, Anti-P, gamma rays, neutrino

  21. Comparison with other observatories M.Teshima MPI for Physics, Munich EUSO General meeting @NSSTC HUntsuville, AL May 2003

  22. Number of events in each experiment • AGASA, HiRes, Auger Hybrid are negligible small • EUSO/Auger = 6~10 • EUSO/Auger (Instantaneous) = 60~100 • Gamma/Neutrino bursts

  23. Exposure (AGASA unit)

  24. EUSO Air fluorescence Calorimetric Ele. Mag. Showers ΔE/E = ±3% Auger Ionization in 1m thick water E.M.(50%) + μ(50%) ΔE/E = ±15% Muon/Neutrino Ele. Mag Energy Determination(Detector characteristics)

  25. Sky Coverage  Anisotropy • EUSO 4π uniform coverage • Auger Southern sky only • EUSO has advantage on • Study on large scale anisotropy • Galactic center enhancement • Super galactic plane enhancement • Study on Galactic Magnetic Field structure • Using 20~80 point sources

  26. Summary • EUSO has a largest aperture • Better study on energy spectrum above GZK energy • Instantaneous aperture, 60-100xAuger • EUSO energy measurement is calorimetric • 4πsky coverage • Large scale anisotropy • Heavy relics / Matter density / AGN distribution • Small scale anisotropy • EHECR source catalogue • G.M.F. structure (Tomography of our galaxy)

  27. Auger

  28. Auger Sky map maximum multiplicity 60-70

  29. EUSO hi zoom

  30. EUSO low

  31. EUSO low zoom

  32. EUSO low skymap

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