The holes visible in the array map arise due to difficulties in accessing the sites or with local landowners.ĭata-taking started on 1 January 2004 with 154 Stable data-taking started on 1 January 2004 with 154 water-Cherenkov detectors and two fluorescence detectors partly operational. Site is located between latitudes 35.0°S and 35.3°S and between longitudes The Observatory is at a mean altitude of about 1400 m,Ĭorresponding to an atmospheric overburden of about 875 g cm -2. Leones, Los Morados, Loma Amarilla and Coihueco. Spread over 3000 km 2 on a 1500 m triangular grid, overlooked by 24Īir-fluorescence telescopes (FD, blue dots in the map).
Water-Cherenkov particle detector stations (SD, black dots in the map)
The Observatory features an array of 1600 Schematic map of the Pierre Auger Observatory Shower crosses the atmosphere, while the particles reaching the groundĬan be sampled by large arrays of detectors.Įxtensive air-showers are measured to determine the energy and arrivalĭirection of each cosmic ray and to provide a statistical determination of the They can be observed by telescopes that pick up theįluorescence radiation emitted from nitrogen molecules excited as the The phenomenon ofĮxtensive air-showers must be exploited to study cosmic rays at very high energies.Ĭreated by the interaction of a single cosmic-ray with the EarthĪtmosphere. The rate falls to about 1 per km 2 per year. Measurement with satisfactory statistical precision from balloons or in space. Particles per square meter per day and thus too low to allow for direct Of high energy cosmic rays (those above about 10 14 eV) is only a few World's largest cosmic ray observatory and is used to study the extensiveĪir-showers produced by cosmic rays above ~10 17 eV. Vast, high-altitude plain in Argentina, in the Province of Mendoza, is the The Pierre Auger Observatory, located on a
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