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Pierre Auger Observatory for UHE Cosmic Rays

Pierre Auger Observatory for UHE Cosmic Rays. Gianni Navarra (INFN-University of Torino) for the Pierre Auger Collaboration. • Science Case : the need for Auger • Principles and Advantages of a Hybrid Detector • Present Status of the Observatory • First preliminary Data • Perspectives.

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Pierre Auger Observatory for UHE Cosmic Rays

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  1. Pierre Auger Observatoryfor UHE Cosmic Rays Gianni Navarra (INFN-University of Torino) for the Pierre Auger Collaboration •Science Case: the need for Auger •Principles and Advantages ofaHybrid Detector •Present Statusof the Observatory •First preliminary Data •Perspectives XXXXth Rencontres de Moriond ElectroWeak Interactions and Unified Theories La Thuile 5-12th March 2005

  2. 16 Countries 50 Institutions ~350 Scientists Pierre Auger Collaboration ItalyArgentina Czech RepublicAustralia FranceBrazil Germany Bolivia* GreeceMexico PolandUSA SloveniaVietnam* Spain United Kingdom *Associate Countries Spokesperson: Alan Watson

  3. UHE Cosmic Rays Surface particle detectors Eo >1020 eV: 1 part / (km2 century sr)  102 – 103 km2 collecting areas

  4. atmospheric fluorescence detectors UHE Cosmic Rays Atmospheric fluorescence detectors Eo >1020 eV: 1 part / (km2 century sr)  102 – 103 km2 collecting areas

  5. HiRes vs AGASA Surface particle detectors ~ 30 % Syst. Error AGASA HiReS ?? Atmospheric fluorescence detectors D. Bergmann

  6. B intergalactic pair production energy loss B = 1 nG 3 Gpc pion production energy loss pion production rate - 10 eV 21 Astrophysics? GZK? Cosmic ray sources are close by (<100 Mpc) Dq ~ degree  Sources !!!

  7. Relic Particles in Galactic Halo ? Fundamental Physics ? 2 Sakar & Toldrà, Nucl.Phys.B621:495-520,2002 Toldrà, astro-ph/0201151 8 16 + Composition (p,…Fe,g,n) + Astronomy (point sources) Mrelic = 1022 eV; SUSY evolution, n-body decay

  8. Required to solve EHECR-Puzzle: • Better understanding of Syst. Errors • Better Resolution in Energy and Direction • Much more Statistics • Hybrid Approach: Independent EAS-observation techniques Shower-by-Shower in one Experiment • Much larger Experiment

  9. Atmospheric fluorescence detectors Atmospheric fluorescence detectors UHE Cosmic Rays with Auger Surface particle detectors Atmospheric fluorescence detectors Eo >1020 eV: 1 part / (km2 century sr)  102 – 103 km2 collecting areas

  10. LOMA AMARILLA Southern Site Pampa Amarilla; Province of Mendoza 3000 km2, 875 g/cm2, 1400 m Surface Array: 1600 Water Tanks 1.5 km spacing 3000 km2 Lat.: 35.5° south Fluorescence Detectors: 4 Sites 6 Telescopes per site (180° x 30°) 24 Telescopes total 70 km

  11. View of Los LeonesFluorescence Site

  12. Six Telescopes viewing 30°x30° each

  13. Schmidt Telescope using 11 m2 mirrors UV optical filter (also: provide protection from outside dust) Schmidt corrector ring  2.2 m opt. Filter (MUG-6) Camera with 440 PMTs (Photonis XP 3062)

  14. Lomo Amarilla (in preparation) Morados handed to Collaboration 1.9.04 Los Leones (fully operational) Coihueco (fully operational)

  15. Aligned Water Tanksas seen from Los Leones

  16. Communicationantenna GPSantenna Electronics enclosure 40 MHz FADC, local triggers, 10 Watts Solar Panel three 9” PMTs Plastic tank with 12 tons of water Battery box Water Tank in the Pampa

  17. installation of electronics receiving tanks Water deployment Transportation into field Tank Preparation and Assembly Installation Chain

  18. Coihueco > 10 x AGASA AGASA Los Leones Southern Site as of Febr. 2005 650 Water Tanks (out of 1600) + 12 Telescopes

  19. Calibration

  20. SD Calibration by Single Muon Triggers Agreement with GEANT4 Simulation up to 10 VEM (Vertical Equivalent Muons). VEM ~ 100 PE /PMT Huge Statistics! Systematic error ~5% Sum PMT 1 VEM Peak Local EM Shower PMT 2 PMT 3

  21. SD calibration & monitoring Base-Temperature vs Time Single tank response single muons Noise Signal-Height vs Time Signal-Height vs Base-Temp ± 3% Huge Statistics! Systematic error ~5%

  22. FD Calibration Absolute:End to End Calibration N Photons at diaphragm  FADC counts A Drum device installed at the aperture uniformly illuminates the camera with light from a calibrated source (1/month) Mirror Calibrated light source Camera Diffusely reflective drum Drum from outside telescope building Relative: UV LED + optical fibers (1/night) • Alternative techniques for cross checks • Scattered light from laser beam • Calibr. light source flown on balloon All agreed within 10% for the EA

  23. •LIDAR at each eye •cloud monitors at each eye • central laser facility • regular balloon flights Atmospheric Monitoring steerable LIDAR facilities located at each FD eye Central laser facility (fibre linked to tank) LIDAR at each FD building • light attenuation length • Aerosol concentration Balloon probes  (T,p)-profiles

  24. PerformancedemonstratedbyFirst Preliminary Data

  25. Vertical (q~35o) & Inclined (q~72o) 35 tanks 14 tanks 14 km ~ 13 km Energy ~ (6-7) 10 19 eV ~ 7 km

  26. density falls by factor ~150 … by factor ~4 Young & Old Shower ‘young’ shower ‘old’ shower

  27. n Only a neutrino can induce a young horizontal shower ! Vertical vs Horizontal Showers ~ 0.2 µs ‘young’ showers • Wide time distribution • Strong curvature • Steep lateral distribution ‘old’ showers • Narrow time distribution • Weak curvature • Flat lateral distribution

  28. A Big One: ~1020 eV, q ~60° 34 tanks ~60° ~ 8 km (m) ~ 14 km propagation time of 40 µs Lateral Distribution Function ~1020eV ~11020eV

  29. EAS as seen by FD-cameras EAS as seen by FD-cameras Two-Mirror event Only pixels with ≥ 40 pe/100 ns are shown (10 MHz FADC  ≤ 4 g/cm2;12 bit resol., 15 bit dynamic range) Pixel-size = 1.5° ; light spot: 0.65° (90%) 1019 eV events trigger up to ~ 30 km

  30. Energy Reconstruction Integral of Longitudinal Shower Profile Energy ~ 4.8 Photons / m / electron (~ 0.5 % of dE/dx) preliminary

  31. …zoom A Stereo Hybrid; q ~70° ~70° global view Coihueco Fluores. Telescope ~37 km Lateral Distribution Function ~8·1019eV ~24km Los Leones Fluores. Telescope

  32. A stereo hybrid; q ~70° ~37 km ~24km

  33. A stereo hybrid; q ~70° Shower Profile ~7·1019eV (SD: ~8·1019eV)

  34.  SD times Verified by using central laser facility  FD times x y Mono vs Hybrid: uncertainties of Shower core & angle of incidence Mono 26.15 ± 0.55 km Hybrid 25.96 ± 0.02 km mono hybrid The Power of Hybrid Observations y

  35. Some numbers: data taking from Jan. 2004 SD: number of tanks in operation 650 fully efficient above ~ 3.1018 eV number of events ~ 120,000 reconstructed ( > 3fold, >1018 eV) ~ 16,500 at present ~ 600 events/day FD: number of sites in operation 2 SD+FD: number of hybrids 1750 ~ 350 “golden”

  36. Preliminary Sky Plot no energy cut applied Auger-S >85o Auger-S >60o

  37. Distribution of Nearby Matter 7-21 Mpc Auger-S >60o Auger-N >60o Jim Cronin, astro-ph/0402487

  38. 15,000km2 10,000km2 Utah Colorado “Standard”3,100 km2 Auger North (3,100 km2) TA (800km2) AUGER NORTH Two Candidate Sites

  39. CONCLUSIONS Auger construction in rapid progress in southPhysics data taking since January 2004 • Stable operation, excellent performance • Hybrid approach is a great advantage! • Neutrino sensitivity First physics results by summer 2005 • Energy spectrum • Sky map Auger North proposal in progress

  40. Pampa Amarilla

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