- Conference date: 8–9 October 2012
- Location: Mexico City, Mexico
The Pierre Auger Observatory was designed to measure ultra-high energy cosmic rays above 1018eV with high accuracy using a hybrid air shower detection technique. A Surface Detector (SD) with 1600 water-Cherenkov stations on a 1500 m triangular grid covers an area of 3000 km2. The atmosphere above the array is viewed by a Fluorescence Detector (FD) with 24 telescopes at 4 sites in the periphery of the SD. As an enhancement to this baseline design, in order to reach a lower energy threshold below 1017eV, the Collaboration has implemented extensions to the Observatory. The SD extension is AMIGA (Auger Muons and Infill for the Ground Array), an infilled area with detectors at a smaller spacing than in the main array and with buried scintillator counters. The FD is complemented by HEAT (High Elevation Auger Telescopes), with 3 additional telescopes that are tilted upwards to extend the elevation range. A review of the status and the main results from the observatory is presented with the emphasis given to the measurement of energy spectrum above 1018 eV where we observe a suppression for energies larger than 3×1019 eV, chemical composition, arrival directions, the search for photons and neutrinos as primary particles and finally the importance of the extensions of the Auger Observatory due that they allow to study the energy range where the transition from a Galactic to an extra-Galactic origin of cosmic rays may occur.
- Cosmic rays
- Chemical composition
- Cosmic ray energy spectra
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