1 / 27

AGASA results Anisotropy of EHE CR arrival direction distribution

AGASA results Anisotropy of EHE CR arrival direction distribution. M. Teshima ICRR, U of Tokyo. Contents. Anisotropy at 10 18 eV Good evidence for Galactic Cosmic Rays Anisotropy above 10 19 eV Clusters in the arrival directions New Astrophysics. Cosmic Ray Propagation in our Galaxy.

gay-morrow
Download Presentation

AGASA results Anisotropy of EHE CR arrival direction distribution

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. AGASA resultsAnisotropy of EHE CR arrival direction distribution M. Teshima ICRR, U of Tokyo

  2. Contents • Anisotropy at 1018eV • Good evidence for Galactic Cosmic Rays • Anisotropy above 1019eV • Clusters in the arrival directions • New Astrophysics

  3. Cosmic Ray Propagation in our Galaxy • Deflection angle < 1 degree at 1020eV • Neutrons can travel galactic scale without decaying above 1018eV By M.Takeda

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

  5. Data A20: (~12km2) for 5years AGASA(~100km2) for 10years Event selection Core Location: inside the array Nhit >= 6 detectors χcore2<5.0, χdir2<5.0 Number of Events 284,000 events (>1017eV) Anisotropy at 1018eV

  6. First Harmonic Analysis (Sep.1986-May.2001, 284,416 events)

  7. Galactic Cosmic Rays up to 1018eV ●Use 284,000events over 15yrs operation by AGASA+AGASA Prototype ● >4σ near G.C. and -4σ near A.G.C. Amplitude ~4% Statistical Significance

  8. Point Sources or Cosmic Ray flow

  9. Dipole (G.C.-AGC) distribution Log(E) = 18.0-18.5 G.C Anti G.C.

  10. DC excess with 6 degrees rad. Aperture Log(E) = 18.0-18.5

  11. Auto-correlation at 18.0-18.5

  12. Conclusion • Harmonic Analysis, Global excess map (p.s. = 20o) • Pch < 10-4 (consistent with previous reports) • 4 σ near the GC and -4σ near AGC • The anisotropy of cosmic ray arrival direction at 1018eV observed by AGASA can be fitted with dipole distribution (GC --- AGC) • Point source analysis(p.s. = 6o), Self-correlation analysis No evidence for point sources. The data favors the diffuse sources.

  13. Arrival Direction Distribution No Large Scale Anisotropy. Event Clusters: 1Triplet and 6 doublets P(chance) ~ 0.07%. Interacting Galaxy VV141 in the direction of triplet at 100Mpc. Arrival directions of 59events > 4 x1019eV observed by AGASA

  14. Arrival Direction DistributionCompact sources!! ~5 sigma effect

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

  16. V1-V2 plot in Galactic coordinateOuter Galaxy region|bII|<60, 90<lII<180 1. From 1019eV 2. Extended linearly ΔｂII 20ox20o ΔｌII Log(E)>19.00 19.15 19.70

  17. The polarization angle 3.5σ at 40 degrees 1019eV 1.8 degree x 10 degree box

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

  19. Linearly extended halo in 2-D correlation map can be understood as deflected charged particles by G.M.F. Restrict G.M.F. structures (by GMT and MT) Magnetic field in disk Axial Symmetric Bi-symmetric Parity Even Odd Magnetic field in Halo Strength Bz~0.3μG Parity Odd  Even On going Trace back cosmic rays up to Galactic Halo surface of 20kpc Identify sources!!

  20. Self-correlation 2D-map (20ox20o) >19.0 >19.1 >19.2 >19.3 >19.4 >19.5 >19.6 >19.7

  21. X1.51 X2.95 X2.04 X2.63 Differential Energy Spectrum of pair events(bin width = 0.2 decade) Structure? dF/dE ~ E-1.8+-0.3

  22. He ? ? x1.86(+0.32-0.21) x4.46(+0.55-0.48) X2.4 Correlation as func. Of energy ratio between two events

  23. Fe Naturally, Fe is expected at 2-3x1020eV. Possible Scenario Rigidity dependent? Photo-disintegration cutoff? First bump --- 1ry and 2ndry p/n Second bump --- 1ry He Third bump --- 1ry BCNO p.d. p.d. BCNO He P

  24. Monte Carlo Realization By T.Yamamoto et al Uniform Source Standard Chem. Comp. 10nG Magnetic Field Require Clustering Preliminary

  25. Conclusion (>1019eV) • 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. • Interesting structures in the energy spectrum of cluster events (Three bumps?) • Consistent with P, He, BCNO composition The beginning of the EHECR astronomy

  26. To the future Clusters give you important information • Sources (Fe primary favors GRB remnants) • the chemical composition study for super GZK particle is important • G.M.F. structure can be uniquely solved • Constrain the inter-galactic Magnetic Field • 4πcoverage of sky is really important • Northern Hemisphere; Easy to understand G.M.F. structure, because it is simple toward outer galaxy. • Southern hemisphere; Observation is essentially important to understand whole G.M.F. structure.

  27. Systematics and Resolution • In Mono analysis • Composition Proton/Fe??? • Interaction QGSJET/SIBYLL • Scale height of Mie layer • In Atmosphere (In Mie Scattering) • Horizontal attenuation • Scale height • 1-D model  reality (locality) • E (Rp) dependence • 10,000km2sr  100% efficiency upto Rp ~ 40km

More Related