The Pierre Auger Observatory [1] is being used to study cosmic rays with energies larger than 10 eV with unprecedented precision and statistics. An essential quantity that must be deduced from data is the lateral distribution function (LDF) that describes the decreasing of the signals in the watertanks as a function of distance. Knowledge of the LDF is important for the reconstruction of the sh...

KASCADE-Grande is a multi detector setup for the investigation of extensive air showers in the 10 − 10 eV energy range. With the Grande array it is possible to reconstruct the shower core position, the arrival direction and the total number of charged particles in the shower. The Grande array measures in coincidence with the original KASCADE muon array consisting of 622 m shielded scintillators...

Wavefront sampling experiments record arrival times of Čerenkov photons with high precision at various locations in Čerenkov pool using a distributed array of telescopes. It was shown earlier that this photon front can be fitted with a spherical surface traveling at a speed of light and originating from a single point on the shower axis. Radius of curvature of the spherical shower front (R) is ...

The capability of the Muon Tracking Detector to measure the radial and tangential angles of muons in extensive air showers, in combination with the shower direction as determined by the scintillator array of KASCADE experiment, has been investigated. Due to different characteristics in shower development of light and heavy primary particles the radial angle is sensitive to the mass of them. For...

Data taken during half a year of operation of 10 LOPES antennas (LOPES-10), triggered by EAS observed with KASCADE-Grande have been analysed. We report about the analysis of correlations of radio signals measured by LOPES-10 with extensive air shower events reconstructed by KASCADE-Grande, including shower cores at large distances. The efficiency of detecting radio signals induced by air shower...

In most high energy cosmic ray surface arrays, the primary energy is currently determined from the value of the lateral distribution function at a fixed distance from the shower core, r0. The value of r0 is mainly related to the geometry of the array and is, therefore, considered as fixed independently of the shower energy or direction. We argue, however, that the dependence of r0 on energy and...

We discuss the statistical and systematic uncertainties in the event reconstruction (core location, and determination of S(1000), i.e., the signal at a distance of 1000 m from the shower core) by the Pierre Auger surface detector for showers with zenith angle less than 60 degrees. The method is based on a maximum likelihood method where the reference lateral distribution function is obtained th...

Preprint submitted to Elsevier Preprint 5 February 2008 The time profiles of Cherenkov images of cosmic-ray showers and of γ-ray showers are investigated, using data gathered with the HEGRA system of imaging atmospheric Cherenkov telescopes during the 1997 outbursts of Mrk 501. Photon arrival times are shown to vary across the shower images. The dominant feature is a time gradient along the maj...

Previous EAS investigations have shown that for a fixed primary energy the charged particle density becomes independent of the primary mass at certain (fixed) distances from the shower axis. This feature can be used as an estimator for the primary energy. We present results on the reconstruction of the primary energy spectrum of cosmic rays from the experimentally recorded S(500) observable (th...

The surface detector technique has been successfully used to detect cosmic ray showers for several decades. Scintillators or Cerenkov water tanks can be used to measure the number of particles and/or the energy density at a given depth in the atmosphere and reconstruct the primary particle properties. It has been shown that the experiment configuration and the resolution in reconstructing the c...