Abstract
Some new developments in EAS methods made in the framework of the Pamir-XXI project are presented. First, primary energy and direction definition accuracies by a network of fast scintillators are considered, optimum network cell size is defined for 10 PeV showers. Second, the same accuracies for a network of fast optical (Cherenkov) detectors are considered for 30 TeV–10 PeV showers. Third, the possibilities of separation of EAS initiated by protons, nitrogen and iron nuclei of 1 and 10 PeV energies using a wide-angle Cherenkov telescope are discussed. Finally, the results of the extraction of 30–50 TeV gamma showers from the proton shower background with the same telescope are presented. Presumably, our developments can help in the study of PCR mass composition and ultra high energy gamma ray astronomy in other projects.
Highlights
The Pamir-XXI project was originally planned as a multi-component study of EAS in a wide energy range 30 TeV–1 EeV bearing in mind the solution of astrophysical problems and the problems of hadron interaction at super high energies including exotic phenomena in EAS cores
That is why we insist that a detector array and data processing methods should be optimized with respect to the informatively most exacting problems, namely, the primary mass estimation and the γ -event selection
50 TeV γ – 100 TeV p 0.0025/0.255 0.0025/0.545 these measured data the core location and arrival direction are estimated as well as particle lateral distribution function which is integrated to give a E0 estimate; b) all CORSIKA particles within a detector are tracked through its body (2 mm of Al + 2 cm of polystyrene), by the deposited energies and centers of mass of ionization pulses the same event parameters as in a) are estimated
Summary
The Pamir-XXI project was originally planned as a multi-component study of EAS in a wide energy range 30 TeV–1 EeV bearing in mind the solution of astrophysical problems (detailed studies of PCR energy spectrum and mass composition, detection of γ -rays of point-like and diffuse sources above 30 TeV) and the problems of hadron interaction at super high energies including exotic phenomena in EAS cores. At present there is no certainty in the terms of realizing the project, but we still continue developing the experimental procedures using detailed simulations of EAS characteristics. To reach the denoted aims a complex detector array is required, incorporating numerous detectors of different types [1]. – Cherenkov γ -ray astronomy; – PCR energy spectrum and mass composition studies
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