1. AGASA update M. Teshima ICRR, U of Tokyo @ CfCP mini workshop Oct 4 2002

2. AGASA Akeno Giant Air Shower Array 111 Electron Det. 27 Muon Det. 0 4km

3. Exposures in various experiments AGASA: Ground Array HiRes: Air Fluorescence

4. Energy Determination Local density at 600m Good energy estimator by M.Hillas E=2x10 20 eV, E min = 1.6x10 20 eV

5. Attenuation curve S(600) vs N ch 10 18 eV Proton Atmospheric depth

6. S600 Intrinsic fluctuation for proton and iron Proton Iron

7. Energy Determination in AGASA Please read astro-ph/0209422

8. Detector Calibration in AGASA experiment Detector Gain by muons in each run Cable delay (optic fiber cable) Gain as a function of time (11years data) Accuracy of 100ps by measuring the round trip time in each run Detector Position Survey from Airplane Δ Ｘ， Δ Ｙ＝ 0.1m, Δ Ｚ＝ 0.3m Linearity as a function of time (11years data)

9. Detector Simulation ( GEANT) Detector Housing (Fe 0.4mm) Detector Box (Fe 1.6mm) Scintillator (50mm) Earth (Backscattering) vertical θ = 60deg Detector Response Energy spectra of shower particles

10. Energy Resolution Angular Resolution AGASA

11. Energy Resolution

12. The Conversion from S600 to Energy

13. Time profile of shower particles Over estimation factor Due to the shower front thickness

14. Delayed particles and Over estimation factor

15. Major Systematics in AGASA astro-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%

16. Energy Spectrum by AGASA (θ<45) 10 obs. / 1.6 exp. 4.0σ

17. Red -Inside Array Green –Well Inside 4.6 x 10 16 m 2 s sr

18. Energy determined by Ne and Energy determined by S600 Ne  8.5x10 18 eV S600  9.3x10 18 eV

19. Akeno 1km 2 and AGASA

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

21. AGASA & HiRes 2001 ICRC 1999 ICRC 2002 Astro-ph

22. Possible Systematics in HiRes Most of them are energy dependent Air Fluorescence yield Total yield is known with 10% accuracy Yields of individual lines are not known well Rayleigh Scattering effect ( ∝ 1/λ 4 ) Light transmission in air Mie Scattering Horizontal attenuation, Scale Height, Wind velocity, Temperature  single model represents whole data Horizontal 12km (1999)  25km (2001) Cherenkov light subtraction Errors in Mono analysis Aperture estimation (Narrow F.O.V.) Chemical composition / Interaction dependent

23. Arrival Direction Distribution Arrival directions of 59events > 4 x10 19 eV observed by AGASA No Large Scale Anisotropy. Event Clusters: 1Triplet and 6 doublets P(chance) ~ 0.07%. Interacting Galaxy VV141 in the direction of triplet at 100Mpc.

24. Arrival Direction Distribution of EHE cosmic rays >4x10 19 eV >10 19 eV

25. The distribution of Space angle between events Suggest compact sources!! 5 sigma effect >4x10 19 eV >10 19 eV 3 sigma effect

26. V 1 - V 2 plot in Galactic coordinate Outer Galaxy region |b II |<60, 90<l II <180 Log(E)>19.0019.1519.70 1. From 10 19 eV 2. Extended linearly Δ ｂ II Δ ｌ II 20 o x20 o

27. The polarization angle 40 degrees 1.8 degree x 10 degree box 10 19 eV

28. Cosmic Ray propagation in Galactic Magnetic Field By Stanev Δ ｂ II Δ ｌ II Aperture

29. Energy spectrum of Cluster events ∝ E -1.8+-0.3 Cluster Component

30. Gamma Rays in EHECR With 95% C.L. γ/all 10 19 eV γ/all 10 19.5 eV

31. Summary Super GZK particles exist AGASA  HiRes inconsistency??? Statistically consistent, but we need cross-calibration Origin of EHECR (Possible scenario) Decay of Heavy Relics in our Halo Z-burst by EHE neutrino Violation of Special Relativity AGN ’ s, GRB ’ s or other astronomical objects Clear evidence for point sources of EHECR Elongated shaped excess of ~10°in 2-D correlation map Consistent with the charged particle deflection by G.M.F. The beginning of the EHECR astronomy