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Particle Physics with High Energy Cosmic Rays

Particle Physics with High Energy Cosmic Rays. Mário Pimenta Valencia, 10/2011. Particle Physics. e +. K +-. H 0 ?. γ , W + ,W - , Z 0. G 1, , …., G 8. Accelerators. The Large Hadron Collider (LHC). 14 TeV. Energy (GeV). High Luminosity Sophisticated detectors

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Particle Physics with High Energy Cosmic Rays

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  1. Particle Physics with High Energy Cosmic Rays Mário Pimenta Valencia, 10/2011

  2. Particle Physics e+ K+- H0 ? γ, W+,W-, Z0 G1,, …., G8

  3. Accelerators The Large Hadron Collider (LHC) 14 TeV Energy (GeV) High Luminosity Sophisticated detectors Central region Energy limited ~ 10 MeV Year of completion ~1930

  4. Cosmic rays John Linsley, 1962 Flux (m2 sr s GeV)-1 Forward Region Extreme Energies Small fluxes indirect measurements 100 TeV Energy (eV) LHC

  5. Cosmic rays “rain”

  6. Cosmic rays “rain”

  7. Cosmic rays “rain”

  8. Cosmic rays “rain”

  9. Cosmic rays “rain”

  10. Cosmic rays “rain”

  11. Cosmic rays “rain”

  12. Cosmic rays “rain”

  13. Cosmic rays “rain”

  14. Cosmic rays “rain”

  15. Cosmic rays “rain” P(Fe) Air Baryons(leading, net-baryon ≠ 0)  π0(π0    e+e- e+e-…)  π ±( π ±  ν±if Ldecay< Lint )  K±, D. …

  16. Shower detection

  17. Shower development Xmax X1 Xmax = X1 + ΔX ΔX em profile N muonic profile E  Ne 

  18. 60 km The Pierre Auger Observatory Area ~ 3000 km2 24 fluorescence telescopes South Hemisphere 1600 water Cerenkov detectors Nov 2009 Malargüe, Argentina

  19. 1.5 km

  20. telescope building “Los Leones” LIDAR station communication tower

  21. telescope building “Los Leones” LIDAR station communication tower

  22. v ~ c Ground array measurements From (ni, ti): The direction The core position The Energy

  23. E.M. and  signal at the SD S(1000) contributions Individual time traces Proton, ϴ =45º , E= 1019 eV , d= 1000m

  24. The fluorescence detectors (FD)

  25. The fluorescence detectors (FD)

  26. The fluorescence detectors (FD)

  27. Fly’s Eye E~3x1020 eV E  Ne  Fluorescence detector measurements The direction Light profiles (Xmax, Energy, …) Xmax

  28. A 4 eyes hybrid event !

  29. SD Energy Calibration FD SD S38 Total Energy uncertainty: 22%

  30. Exposure Auger has already more than 10 times the Agasa Exposure

  31. AMIGA/HEAT 23.5 km2, 42 extra SDs on 750m grid (infill array) associated with 30m2 buried scintillators, 3 extra FD telescopes tilted upwards 30 E ~3 × 1017 eV with full efficiency

  32. The results

  33. Energy spectrum

  34. Energy spectrum Ankle p N Δ π g 2.7K GZK like suppression !!!

  35. Energy spectrum (interpretation ) Kotera &Olinto GZK: p γ →  →p N Dip (Berezinsky et al) : p γ → p e+ e- Spectrum of UHECRs multiplied by E3 observed by HiRes I and Auger. Overlaid are simulated spectra obtained for different models of the Galactic to extragalactic transition and different injected chemical compositions and spectral indices, s.

  36. Correlation with AGNs 28 out of 84 correlates Vernon-Cetty-Vernon AGN catalog P = 0.006, f = 33 ± 5%

  37. Cen A Closest (4.6 Mpc) powerful radio galaxy with characteristics jets and lobes, candidate for UHECR acceleration E> 57 1018 eV Lower energies No significant anisotropies But particles with the same rigidity (E/Z) follows the same paths !!! scenarios in which high energy anisotropies are caused by heavy primaries and having a significant light component at lower energies are disfavoured

  38. Xmax distributions ΔX

  39. Proton cross-section If % p > 20%, % He < 25% Slightly lower than expected by most of the models but in good agreement with recent LHC data.

  40. Xmax distributions As the energy increases the distributions become narrower !!!

  41. γ p Fe <Xmax> and RMS(Xmax) Heavy nuclei ? Wrong Physics models ?

  42. But if just proton and iron …  : iron fraction ; (1-): proton fraction

  43. But if just proton and iron …  : iron fraction ; (1-): proton fraction

  44. But if just proton and iron …  : iron fraction ; (1-): proton fraction

  45. But if just proton and iron …  : iron fraction ; (1-): proton fraction

  46. But if just proton and iron …  : iron fraction ; (1-): proton fraction

  47. But if just proton and iron …  : iron fraction ; (1-): proton fraction

  48. But if just proton and iron …  : iron fraction ; (1-): proton fraction

  49. But if just proton and iron …  : iron fraction ; (1-): proton fraction

  50. But if just proton and iron …  : iron fraction ; (1-): proton fraction

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