Navarra

Slide1: 

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

Pierre Auger Collaboration: 

Pierre Auger Collaboration Spokesperson: Alan Watson 16 Countries 50 Institutions ~350 Scientists Italy Argentina Czech Republic Australia France Brazil Germany Bolivia* Greece Mexico Poland USA Slovenia Vietnam* Spain United Kingdom *Associate Countries

UHE Cosmic Rays: 

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

UHE Cosmic Rays: 

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

HiRes vs AGASA: 

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

GZK?: 

GZK? Cosmic ray sources are close by (<100 Mpc) Dq ~ degree  Sources !!! Astrophysics?

Relic Particles in Galactic Halo ?: 

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

Required to solve EHECR-Puzzle:: 

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

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

Southern Site: 

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

View of Los LeonesFluorescence Site: 

View of Los Leones Fluorescence Site

Six Telescopes viewing 30°x30° each: 

Six Telescopes viewing 30°x30° each

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Schmidt Telescope using 11 m2 mirrors

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Coihueco (fully operational) Los Leones (fully operational)

Aligned Water Tanksas seen from Los Leones: 

Aligned Water Tanks as seen from Los Leones

Water Tank in the Pampa: 

Water Tank in the Pampa

Installation Chain: 

Installation Chain

Southern Site as of Febr. 2005: 

650 Water Tanks (out of 1600) + 12 Telescopes Southern Site as of Febr. 2005

Calibration: 

Calibration

SD Calibration by Single Muon Triggers: 

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% VEM Peak Sum PMT 1 PMT 2 PMT 3 Local EM Shower

SD calibration & monitoring: 

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

FD Calibration : 

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

Atmospheric Monitoring: 

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

PerformancedemonstratedbyFirst Preliminary Data: 

Performance demonstrated by First Preliminary Data

Vertical (q~35o) & Inclined (q~72o) : 

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

Young & Old Shower: 

Young & Old Shower ‘young’ shower ‘old’ shower

Vertical vs Horizontal Showers: 

Vertical vs Horizontal Showers ‘young’ showers • Wide time distribution • Strong curvature • Steep lateral distribution ‘old’ showers • Narrow time distribution • Weak curvature • Flat lateral distribution ~ 0.2 µs

A Big One: ~1020 eV, q ~60°: 

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

EAS as seen by FD-cameras: 

EAS as seen by FD-cameras 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 Two-Mirror event EAS as seen by FD-cameras

Energy Reconstruction: 

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

A Stereo Hybrid; q ~70°: 

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

A stereo hybrid; q ~70°: 

A stereo hybrid; q ~70° ~37 km ~24km

A stereo hybrid; q ~70°: 

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

The Power of Hybrid Observations: 

The Power of Hybrid Observations

The Power of Hybrid Observations: 

The Power of Hybrid Observations y

Slide36: 

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”

Slide37: 

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

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

Two Candidate Sites: 

Two Candidate Sites AUGER NORTH

CONCLUSIONS: 

CONCLUSIONS Auger construction in rapid progress in south Physics 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

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Pampa Amarilla

Hybrid Reconstruction Quality: 

Hybrid Reconstruction Quality 68% error bounds given detector is optimized for 1019eV, but good Hybrid reconstruction quality at lower energy statistical errors only zenith angles < 60O

High-Energy Neutrinos in Auger: 

High-Energy Neutrinos in Auger  ns expected from distant AGN a/o decay of TDs  X-section @ 1020 eV ≈~10-32 cm2 (Earth opaque for En 1015 eV)  detection by horizontal EAS  If nm  nt Oscillations  advantageous for observation of nt induced Showers n Tests of many AGN & TD Models in range AGN TD

LDF in Hybrid Events: 

LDF in Hybrid Events • good agreement of SD and FD • good agreement of SD and MC LDF for 1018 eV Showers (Energy from FD) Data points scaled from SD < EFD > = 1.21018 eV

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Neutrino Sensitivities (per site) X. Bertou et. al. Astropart. Phys. 17 (2002) 183 Expected no. per year  Limit (E-2) for 5 years  Sensitivity e and  Sensitivity High DIS None

Slide46: 

Integrated Sensitivity of Various Experiments

Slide47: 

High-Energy Neutrinos in Auger  ns expected from distant AGN a/o decay of TDs  X-section @ 1020 eV ≈~10-32 cm2 (Earth opaque for En 1015 eV)  detection by horizontal EAS  If nm  nt Oscillations  advantageous for observation of nt induced Showers n Neutrino Sensitivity (per flavor)