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Argentina Australia Bolivia * Brasil Croatia Czech Republic France Germany Italy Poland Mexico

Argentina Australia Bolivia * Brasil Croatia Czech Republic France Germany Italy Poland Mexico Netherlands Portugal Romania* Slovenia Spain United Kingdom USA Vietnam *. ~ 500 Scientists 19 Countries. Up to the “knee” – observe nuclei from H to Fe and beyond.

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Argentina Australia Bolivia * Brasil Croatia Czech Republic France Germany Italy Poland Mexico

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  1. Argentina Australia Bolivia* Brasil Croatia Czech Republic France Germany Italy Poland Mexico Netherlands Portugal Romania* Slovenia Spain United Kingdom USA Vietnam* ~ 500 Scientists 19 Countries

  2. Up to the “knee” – observe nuclei from H to Fe and beyond ~ E-2.7 Very low flux … Very big detectors ~ E-3.1 Above 1020 eV (50 Joules!): Φ ≈ 1 per km2 per century

  3. (cosmic ray proton) Extensive Air Showers (1019eV) N ~1010 particles 90% e+/-10% μ +/-(primary proton) e+/- ~ 5 MeVμ +/- ~ 5 GeV

  4. Reconstructed longitudinal profiles

  5. Protons are trapped in our Galaxy up to ~1018eV • Protons can travel straight above ~1020eV • Charged-Particle Astronomy E=1018eV Trajectories of Cosmic Ray Protons in the Galaxy E=1019eV E=1020eV

  6. How to get particles to extreme energy • Fermi Acceleration (Bottom-Up) - repeated encounters with strong plasma shocks - naturally produces power-law with correct index - maximum energy can be extremely large - observed in nature • “Exotic” (Top-Down) - decay of massive relic particles - interaction of nu’s w/cosmic background neutrinos (-> Z) - topological defects, other things ? - Signature: photons, neutrinos

  7. B Emax = β B L Ze βcshock speed Zeparticle charge L

  8. Acceleration can occur both at remote termination shocks and at shocks near the central engine AGN VLA image of Cygnus A An active galaxy M. Urry, astro-ph/0312545

  9. 38° South, Argentina, Mendoza, Malargue

  10. Surface Array 1650 detector stations 1.5 Km spacing 3000 km2 Fluorescence Detectors 4 Telescope enclosures 6 Telescopes per enclosure 24 Telescopes total

  11. View of Los Leones Fluorescence Site

  12. The Fluorescence Detector FADC trace 100 s Spherical surface camera 440 PMT with light collectors Large 300x300 field of view 1.5º pixel fov (spot 1/3 of pixel) PMT camera 3.4 m spherical mirror

  13. Energy reconstructed from measured maximum size --- calorimetric (minimal MC)

  14. telescope calibration includes the atmosphere Mike Sutherland

  15. μ e

  16. “GZK” First pointed out in 1966 in two papers, one by Greisen and one by Zatsepin & Kuz’min • p + (2.7oK)  p 0 • n + Nuclei photo-disintegrate at similar thresholds, distances

  17. Improved!

  18. Proton-Air Cross Section from the Depth of Shower Maximum “Tail” dominated by protons

  19. Phys. Rev. Lett. 109 (2012) 062002

  20. (Only about 10% of all events can have Xmax measured directly) 2013 update of Physical Review Letters 104 (2010) 091101

  21. SD: Development of Muons in Shower SD: Asymmetry of Shower front thickness FD: Mean depth of Shower Max FD: Fluctuations of Shower Max Spectral “Ankle”

  22. Update: Correlation with nearby AGN E > 55 EeV, within 3.1o of VCV catalog AGN, d < 75 Mpc,Cover of Science! Through summer 2007: 20 of 27 events correlate 5.7 expected if isotropic (21%) Probability ~ 10-3 Science 318 (2007) p.939

  23. Update: Correlation with nearby AGN Status in 2013 Fraction correlating Bah, Humbug! Cumulative event total

  24. Cen A ... Full Moon 2 Events Closest (4 Mpc) powerful radio galaxy with characteristics jets and lobes, candidate for UHECR acceleration.

  25. Cumulative total within Ψ (degrees)

  26. Azadeh Keivani R = “Rigidity” = E/Z(rL= E/qB = R/B ) e.g.: R = 10 EV for 10 EeV proton, 260 EeV iron R ~ 100 EV R ~ 20 EV R ~ 10 EV

  27. Amir Shadkam, LSU Some fun: double bumps

  28. http://bit.ly/augerstorm http://www.youtube.com/watch?v=E0h36hPpeJE

  29. Summary • Energy spectrum exhibits ankle and GZKsuppression • The sources are extragalactic, within the “GZK sphere”: (weak) anisotropy persists above ~60 EeV • The composition is baryonic, appearing to become iron-dominated (or new particle physics … models do not give enough muons) • p-Air, p-p cross sections beyond the LHC energy • Few/no photons or neutrinos (disfavors exotic “top down” models) • Photons/neutrinos nearing GZK regime

  30. What’s Next? Auger has been “operating” since 2004, fully deployed since 2008. The international agreement runs for ~2 more years (end of 2015) We hope to continue after that, are exploring new technologies in use now or can be started very soon … -- Auger Engineering Radio Array - AERA -- Microwave, GHz, ... prototypes operating -- Focus on better composition determination through new muon detectors, new fluorescence techniques, … R&D

  31. Electronics Upgrade Increase the speed of the FADC by a factor of three; Increase dynamic range 40 MHz 120 MHz

  32. Reconstructed Muons and Muon LDF

  33. Scintillators near or under (or over) SD tanks

  34. Segmented Tank

  35. Muon Detection: RPCs

  36. RPC prototypes • First Lab Prototype • 0.5 x 1 m2 • 0.3 mm gaps • Original RPC design for timing (st~200ps) • Main goal: test low gas flux • Second Lab Prototype • 0.5 x 1 m2 • 2 x 1 mm gap • Main Goal: • Optimize efficiency • Optimize signal

  37. Muon signals : tank vs RPCproton, 1019.5 eVq=40o Hits in RPC

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