1. Ultra High Energy Cosmic Rays -- Origin and Propagation of UHECRs -- M.Teshima Max-Planck-Institut f ü r Physik, M ü nchen Erice Summer School July. 2004

2. 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

3. Background Radiations

4. Greisen-Zatsepin-Kuzmin (GZK) effect  -resonance multi-pion production pair production energy loss pion production energy loss pion production rate

5. Energy Spectrum modification by the interaction with CMBR by Yoshida and Teshima

6. Berezinsky 2004

7. The history of the energy of C.R. traveling CMBR sea

8. Energy loss time of nuclei Yamamoto et al. 2003

9. Energy spectrum of Nuclei by T.Wibig 2004

10. GZK effect Energy Spectrum of cosmic rays are modified; suppression above 4x10 19 eV Secondary particles π o  2γ  cascade γ; pair creation e; Inverse compton, synchrotron π ±  ν Generally, proton supply the energy to neutrino and gammas

11. Attenuation length p, γ, e

12. By G.Sigl

13. Z-burst model violates EGRET diffuse gamma flux (G.Sigl)

14. Optimistic Z-burst model (Only neutrino produced at sources) by G.Sigl and D.Semikos

15. By Kolb, 2003

18. Candidates for EHE C.R. accelerator PulsarSNR A.G.N. GRB Radio Galaxy Lobe

19. Matter and galaxies within 93Mpc By A.Kravtsov

20. Cosmic Ray Energy Spectrum from GRBs(10~100) by E.Waxman

21. Cosmic Ray Propagation in Galactic Disk and Inter Gal.

22. Arrival Direction Distribution >4x10 19 eV zenith angle <50deg. Isotropic in large scale  Extra-Galactic But, Clusters in small scale ( Δθ< 2.5deg) 1triplet and 6 doublets (2.0 doublets are expected from random) One doublet  triplet(>3.9x10 19 eV) and a new doublet(<2.6deg)

23. Expected Auto correlation Yoshiguchi et al. 2004 Number density of sources ~10 -5 Mpc -3

24. Summary; origin of UHECRs UHECRs  Diffuse γ, 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

25. Ultra High Energy Cosmic Rays -- Next generation experiments, mainly about EUSO -- M.Teshima Max-Planck-Institut f ü r Physik, M ü nchen Erice Summer School July. 2004

26. New Projects for UHECRs

27. Auger Project Hybrid measurement 1500 water tanks 3 Air fluorescence stations Aperture ~ X30 AGASA

28. Nature 419, 2002 See the presentation by H.Klages

29. Telescope Array Project X10 AGASA

30. Millard County Utah/USA ~600 Scintillators (1.2 km spacing) AGASA x 9 3 x Fluorescence Stations AGASA x 4 TA Detector Configuration ExpRes. AGASA1.6 0 TA SD~1.0 0 TA FD0.6 0 TA Hyb.0.4 0 Low Energy Hybrid Extension

31. 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 m 2 by 2 PMT readout. TA Scintillator Development

32. Imaging Camera ：１６Ｘ１６ PMT Array Electronics ： 100 ns 14 bit AD conv. ＋ Signal recognition by FPGA Shower Image Telescope ： ３ｍ Φ Spherical Mirror TA Telescope Development

33. EUSO Extreme Universe Space Observatory x300, x3000 AGASA

34. EUSO Concept Large Distance and Large F.O.V.  Large Aperture ~6x10 5 km 2 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

35. Effective Area ~200,000km 2 1/2 Deutschland (360,000km 2 )

36. Signal of photons

37. Shower Track Image (M.C. Simulation) 10 20 eV shower zenith angle =60 degree Total signal ~ 700p.e.

38. Atmospheric Transmission better than ground based air fluorescence detector Small effect by Mie scattering Worst ~20% Cloud go down 2~3km altitude in the night Smaller Absorption in absolute value ~ x0.3 Ground based x0.1~0.01

39. Detector Element Focal Surface Support Structure Electronics Entrance pupil Fresnel Lens 2 Fresnel Lens 1

40. Euso Optics Wide Angle and High Resolution F.O.V. +-30° δθ ～ 0.1°

41. 10 particle/0.1 decade EUSO 1 particle/0.1 decade EUSO 10 particle by AGASA/HiRes 1 particle by AGASA/HiRes

42. Focal Surface Detector Baseline design

43. Hamamatsu MAPMT New Development by Riken Group Higher Photon Collection efficiency R8900-M16/M25 (45%  85%) R7600-M64 Flat Panel MAPMT Hamamatsu H8500

45. Energy Threshold 5x10 19 eV

46. Possible EUSO measurement

47. Exposure (AGASA unit) EUSO

48. Angular Resolution

49. Neutrino Detection capability Proton Showers Neutrino Showers Zenith Angle vs. XmaxZenith Angle vs. Shower Time width Neutrino domain Just using observables No need for Cherenkov ref.

50. Neutrino sensitivity (downward neutrino) Auger EUSO 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.

51. Gamma Ray Identification Geomagnetic Cascade Xmax distribution 10 20 eV photon Pair Electrons Synchrotron Photons ~ 100 x 10 18 eV h~5000km Pair Production prob. Energy & Direction

52. New Projects for UHECRs Bright Future of UHECR observation!!

53. EUSO in ISS Accommodation in ISS Cosmic Ray observations