A measurement of the cosmic-ray spectrum for energies exceeding 4x10^18 eV is presented, which is based on the analysis of showers with zenith angles greater than 60° detected with the Pierre Auger Observatory between 1 January 2004 and 31 December 2013. The measured spectrum confirms a flux suppression at the highest energies. Above 5.3x10^18 eV, the "ankle", the flux can be described by a power law E^-gamma with index gamma = 2.70+/-0.02 (stat)+/-0.1 (sys) followed by a smooth suppression region. For the energy (Es) at which the spectral flux has fallen to one-half of its extrapolated value in the absence of suppression, we find Es = (5.12 +/- 0.25 (stat)+1.0+/-1.2 (sys))x10^19 eV.

Measurement of the cosmic ray spectrum above 4 × 10^18eV using inclined events detected with the Pierre Auger Observatory

De Mitri I.;
2015

Abstract

A measurement of the cosmic-ray spectrum for energies exceeding 4x10^18 eV is presented, which is based on the analysis of showers with zenith angles greater than 60° detected with the Pierre Auger Observatory between 1 January 2004 and 31 December 2013. The measured spectrum confirms a flux suppression at the highest energies. Above 5.3x10^18 eV, the "ankle", the flux can be described by a power law E^-gamma with index gamma = 2.70+/-0.02 (stat)+/-0.1 (sys) followed by a smooth suppression region. For the energy (Es) at which the spectral flux has fallen to one-half of its extrapolated value in the absence of suppression, we find Es = (5.12 +/- 0.25 (stat)+1.0+/-1.2 (sys))x10^19 eV.
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/20.500.12571/535
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