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Humberto Salazar (FCFM-BUAP) for the Pierre Auger Collaboration ,

Ultrahigh Cosmic Rays: The highest energy frontier. Humberto Salazar (FCFM-BUAP) for the Pierre Auger Collaboration , CTEQ- Fermilab School Lima, Peru, August 2012. The Auger Observatory in the Southern Hemisphere Hybrid shower measurements

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Humberto Salazar (FCFM-BUAP) for the Pierre Auger Collaboration ,

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  1. Ultrahigh Cosmic Rays: The highest energy frontier Humberto Salazar (FCFM-BUAP) for the Pierre Auger Collaboration, CTEQ- Fermilab School Lima, Peru, August 2012

  2. The Auger Observatory in the Southern Hemisphere Hybrid shower measurements Fully deployed in Argentina since June 2008 1600 water Cherenkov stations 24 fluorescence telescopes (30˚x30˚) 60 km

  3. A Water Cherenkov Station

  4. 4 Fluorescence Detector Eyes with Six Telescopes (30°x30°) each

  5. 30o x 30o Field of View An Air Fluorescence Telescope 30o x 30o Field of View Camera440 PMTs UV-Filter 300-400 nm UV-Filter 300-400 nm 2.2m diameter aperture stop with Schmidt corrector ring. Camera440 PMTs 2.2m diameter aperture stop with Schmidt corrector ring. 3.8m x 3.8m mirror 3.8m x 3.8m mirror

  6. Enhancements at Auger South HEAT: High Elevation Auger Telescopes AMIGA: Auger Muon and Infill Ground Array , AERA: Auger Engineering Radio Array

  7. The Auger Sky above 60 EeV 58 events now (with Swift-BAT AGN density map) 27 events as of November 2007 Simulated data sets based on isotropy (I) and Swift-BAT model (II) compared to data (black line/point). Log(Likelihood)

  8. Shower Depths of Maximum Xmax Shower Depths of Maximum Xmax

  9. Hi-Res Xm - results favor protons Evidence for proton dominated composition above 1.6 EeV HiRes Collaboration arXiv:0910.4184 Mean depth of maximum vs energy PRL 104 161101 (2010) Width of distribution vs energy 23

  10. Trans-GZK composition is simpler Light and intermediate nuclei photodisintegrate rapidly. Only protons and/or heavy nuclei survive more than 20 Mpc distances. Cosmic magnetic fields should make highly charged nuclei almost isotropic.

  11. The Auger UHE Neutrino Observatory Neutrinos can be identified as “young” showers at very great atmospheric slant depth (either upward or downward). Auger exposure to tau Neutrinos

  12. The UHE Gamma Ray Astronomical Window Photon attenuation length exceeds 10 Mpc for E > 2 EeV Photon showers penetrate deeper than hadronic showers. They can be recognized individually with hybrid measurements. A photon component can be measured statistically by the surface array.

  13. Accepted for publication in PRL-July, 2012 According to composition studies, primaries are mainly protons at energies 1018 - 1018.5 eV.

  14. proton-air production cross section The p-air cross section can be deduced from the average penetration length that is related to the tail of Xmax distribution.

  15. The relation between penetration length and p-air cross section can be • found from simulations after correcting the low energy values using • Tevatron measurements, and Glauber theory. R. Ulrich, ICRC 2011

  16. Proton-proton cross section Using Glauber theory is possible to estimate the proton-proton inelastic cross section. Totem @ 7 TeV TOTEM Collaboration, CERN-PH-EP-2011-158

  17. Far greater exposure is needed to • Identify the class of sources via anisotropy • Measure the spectra of bright sources or source regions • Determine the particle type(s) above 55 EeV • If protons, measure interaction properties above 250 TeV (CM) • Determine the diffuse cosmogenic intensity of neutrinos and photons • Detect cosmogenic neutrinos and photons

  18. Science Latest Results • Spectrum with clear ankle and “GZK” suppression • Anisotropy of arrival directions above 55 EeV • Limit on photon flux at 10 EeV using surface detector • Limit on photon flux at 3 EeV using fluorescence detector • Limit on Earth-skimming tau neutrinos • New limit on all flavors of neutrinos using near-horizontal showers • Statistical analysis of Xmax values for energies up to 30 EeV

  19. UHECR 2012: CERN Meeting, Future directions

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