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Ultra High Energy Cosmic Rays -- observational results --

Ultra High Energy Cosmic Rays -- observational results --. M.Teshima Max-Planck-Institut f ü r Physik, M ü nchen Erice Summer School July. 2004. Discovery of Cosmic Rays. Victor Hess 1912. John Linsley at Volcano Ranch (~1960). First discovery of super-GZK events. GZK mechanism. Ｎ. P.

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Ultra High Energy Cosmic Rays -- observational results --

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  1. Ultra High Energy Cosmic Rays-- observational results -- M.Teshima Max-Planck-Institut für Physik, München Erice Summer School July. 2004

  2. Discovery of Cosmic Rays Victor Hess 1912

  3. John Linsley at Volcano Ranch (~1960) First discovery of super-GZK events

  4. GZK mechanism Ｎ P Δ Super GZK part. ~1/km2 century π γ3K Cosmic Ray Energy Spectrum AGASA Energy Spectrum

  5. Pair creation GZK Background Radiations in the universe Cosmic Rays and Neutrino

  6. Candidates for EHE C.R. accelerator A.G.N. Pulsar SNR GRB Radio Galaxy Lobe

  7. Synchrotron radiation GZK limit Hidden HILLAS PLOT II Ann. Rev. Astron. Astrophys. 1984, 22; p425-444

  8. Cosmic Ray Propagation in our Galaxy • Deflection angle ~ 1 degree at 1020eV • Astronomy by hadronic particles?

  9. Cosmic Ray Propagation inGalactic Disk and Inter Gal.

  10. Exposure in ICRC2003

  11. Air Shower Phenomena

  12. AGASAAkeno Giant Air Shower Array 111 Electron Det. 27 Muon Det. 0 4km

  13. HiRes Experiment Air Fluorescence detector

  14. HiRes Experiment Air Fluorescence technique Measure Shower Development in the atmosphere Essentially Carolimetric measurement

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

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

  17. EnergyDetermination • Local density at 600m • Good energy estimator by M.Hillas E=2.13x1020eV, E >= 1.6x1020eV

  18. Third Highest event 97/03/30 150EeV 40 detecters were hit

  19. The Highest Energy Event (~2.46 x1020eV) on 10 May 2001

  20. S(600) vs Nch Attenuation curve 1018eV Proton Atmospheric depth

  21. S600 Attenuation curve 0-60° 20.0 19.5 19.0 18.5 18.0 0-45° Atmospheric depth

  22. The Conversion from S600 to Energy Muon/Neutrino Ele. Mag

  23. Proton S600 Intrinsic fluctuation for proton and iron Iron

  24. 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 ±15% • Air shower phenomenology • Lateral distribution function ± 7% • S(600) attenuation ± 5% • Shower front structure ± 5% • Delayed particle(neutron) ± 5% • Total± 18%

  25. 25% 30% Energy Resolution mainly due to measurement errors (particle density measurement and core location determination)not due to shower fluctuation

  26. Energy Spectrum by AGASA (θ<45) 11 obs. / 1.8 exp. 4.2σ 5.1 x 1016 m2 s sr

  27. The Energy spectrum by AGASA Red: well inside the array (Cut the event near the boundary of array)

  28. Akeno 1km2 and AGASA

  29. HiRes NSF events200-300EeV

  30. HiRes I, II mono spectrum

  31. AGASA vs HiRes (astro-ph)

  32. Recent spectra (AGASA vs. HiRes@Tsukuba ICRC) vs. HiRes-II vs. HiRes-I • ~2.5 sigma discrepancy between AGASA & HiRes • Energy scale difference by 25% vs. HiRes-stereo

  33. World Energy Spectrum by M.Nagano 2002

  34. Stecker 2003

  35. 20% energy variation AGASA vs HiRes by Douglas Bergman

  36. Statistics ~2.4 σ HiRes AGASA ~2.3 σ ~4.2σ ~ 0σ ~ 0 σ Extended spectrum Super-GZK GZK-Hypothesis

  37. 40% uncertainty Air Fluorescence yield Measurement Impact parameter 1. Bunner 2. Kakimoto et al 3. Nagano et al Rayleigh Scattering ∝λ‐4

  38. Possible Systematics in HiResMost of them are energy dependent Air Fluorescence yield • Total yield is known with 10~20% accuracy • Yields of individual lines are not known well • Rayleigh Scattering effect (∝1/λ4) 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 Bias by Narrow FOV in elevation angle Errors in Mono analysis • Aperture estimation (Narrow F.O.V.) • Chemical composition / Interaction dependent

  39. Arrival Direction Distribution >4x1019eVzenith 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(>3.9x1019eV) and a new doublet(<2.6deg)

  40. Space Angle Distribution of Arbitrary two events >4x1019eV

  41. Arrival Direction Distribution >1019eV

  42. Space Angle Distribution Log E>19.0 Log E>19.2 Log E>19.4 Log E>19.6

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

  44. Density of sourcesby Kachelriess and Semikos 2004

  45. 2D-Correlation Map in (ΔlII ,ΔbII ) Log E >19.0eV, 3. 4σ Log E >19.2eV, 3. 0σ ΔbII ΔlII Log E >19.4eV, 2.0σ Log E >19.6eV, 4.4σ

  46. Cosmic Ray propagation in Galactic Magnetic Field ΔｂII ΔｌII Aperture By Stanev

  47. Correlation with BL Lacsby Gorbnov et al. 2004

  48. Full sky map of deflection angles By K.Dolag, D.Grasso, V.Springel, and I.Tkachev

  49. Expected Auto correlationYoshiguchi et al. 2004 Number density of sources ~10-5 Mpc-3

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