The surface detector system of the Pierre Auger Observatory

Allekotte, I.; Barbosa, A. F.; Bauleo, P.; Bonifazi, C.; Civit, Bárbara María; Escobar, C. O.; García, Beatriz; Guedes, G. P.; Berisso, M. Gómez; Harton, J. L.; Healy, M. D.; Kaducak, M.; Mantsch, P.; Mazur, Péter; Newman-Holmes, C.; Pepe, I. M.; Rodríguez-Cabo, I.; Salazar, H.; Grande, N. Smetniansky-De; Warner, D.

doi:10.1016/j.nima.2007.12.016

Cited by 146 publications

(70 citation statements)

References 11 publications

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“…These detectors are used to observe the longitudinal development of extensive air showers by detecting the fluorescence light emitted by excited nitrogen molecules and the Cherenkov light induced by the shower particles. Details of the design and status of the Observatory are given elsewhere [13][14][15]. The energy spectrum of ultra-high energy cosmic rays at energies greater than 2.5 × 10 18 eV has been derived using data from the surface detector array of the Pierre Auger Observatory [2].…”

Section: Introductionmentioning

confidence: 99%

Measurement of the energy spectrum of cosmic rays above 1018 eV using the Pierre Auger Observatory

et al. 2010

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Editor: S. DodelsonWe report a measurement of the flux of cosmic rays with unprecedented precision and statistics using the Pierre Auger Observatory. Based on fluorescence observations in coincidence with at least one surface detector we derive a spectrum for energies above 10 18 eV. We also update the previously published energy spectrum obtained with the surface detector array. The two spectra are combined addressing the systematic uncertainties and, in particular, the influence of the energy resolution on the spectral shape. 242Pierre Auger Collaboration / Physics Letters B 685 (2010) The spectrum can be described by a broken power law E −γ with index γ = 3.3 below the ankle which is measured at log 10 (E ankle /eV) = 18.6. Above the ankle the spectrum is described by a power law with index 2.6 followed by a flux suppression, above about log 10 (E/eV) = 19.5, detected with high statistical significance.

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Section: Introductionmentioning

confidence: 99%

Measurement of the energy spectrum of cosmic rays above 1018 eV using the Pierre Auger Observatory

et al. 2010

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“…The water-Cherenkov detectors are described in [11] . The surface scintillators are comprised of 27 strips of plastic scintillator (1 cm thick, 4 cm wide, and 180 cm long; total area: 1.94 m 2 ) placed on top of the water-Cherenkov detectors.…”

Section: Detector Simulationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

A generalized description of the signal size in extensive air shower detectors and its applications

Ave

Engel

Roth

et al. 2017

Astroparticle Physics

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“…The fluorescence detector (Abraham et al 2010a) comprises a set of imaging telescopes to measure the light emitted by excited atmospheric nitrogen molecules as the EAS develops. A surface detector (SD; Allekotte et al 2008) measures EAS particles on the ground with an array of water-Cherenkov detectors ("stations"). Each SD station contains 12 tonnes of water viewed by three 9 photomultipliers.…”

Section: Introductionmentioning

confidence: 99%

Search for Point-Like Sources of Ultra-High Energy Neutrinos at the Pierre Auger Observatory and Improved Limit on the Diffuse Flux of Tau Neutrinos

Abreu

Aglietta

Ahlers

et al. 2012

ApJ

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The surface detector array of the Pierre Auger Observatory can detect neutrinos with energy E ν between 10 17 eV and 10 20 eV from point-like sources across the sky south of +55• and north of −65 • declinations. A search has been performed for highly inclined extensive air showers produced by the interaction of neutrinos of all flavors in the atmosphere (downward-going neutrinos), and by the decay of tau leptons originating from tau neutrino interactions in Earth's crust (Earth-skimming neutrinos). No candidate neutrinos have been found in data up to 2010 May 31. This corresponds to an equivalent exposure of ∼3.5 years of a full surface detector array for the Earth-skimming channel and ∼2 years for the downward-going channel. An improved upper limit on the diffuse flux of tau neutrinos has been derived. Upper limits on the neutrino flux from point-like sources have been derived as a function of the source declination. Assuming a differential neutrino flux k PS · E −2 ν from a point-like source, 90% confidence level upper limits for k PS at the level of ≈5 × 10 −7 and 2.5 × 10 −6 GeV cm −2 s −1 have been obtained over a broad range of declinations from the searches for Earth-skimming and downward-going neutrinos, respectively.

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The surface detector system of the Pierre Auger Observatory

Abstract: The Pierre Auger Observatory is designed to study cosmic rays with energies greater than 10 19 eV. Two sites are envisaged for the observatory, one in each hemisphere,

Cited by 146 publications

References 11 publications

Measurement of the energy spectrum of cosmic rays above 1018 eV using the Pierre Auger Observatory

Measurement of the energy spectrum of cosmic rays above 1018 eV using the Pierre Auger Observatory

A generalized description of the signal size in extensive air shower detectors and its applications

Search for Point-Like Sources of Ultra-High Energy Neutrinos at the Pierre Auger Observatory and Improved Limit on the Diffuse Flux of Tau Neutrinos

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