Hybrid Cosmic Ray Detector at Pico de Orizaba

Details Hybrid Cosmic Ray Detector at Pico de Orizaba Hybrid Cosmic Ray Detector at Pico de Orizaba

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003icrc....2.1013c&link_type=abstract

Proceedings of the 28th International Cosmic Ray Conference. July 31-August 7, 2003. Trukuba, Japan. Under the auspices of the I

Physics

Scientific paper

In this work we present the design features and simulation of the hybrid detector under construction at 4300 m.a.s.l. equivalent to 620 g /cm2 .The goal of this observatory is to study the mass composition of the cosmic rays in the energy range of 1015 - 1018 eV. The observation technique include particle counting and fluorescence detection in order to improve the Energy and Xmax determination. This approach allow us to contribute in the knowledge of the knee composition, corresponding to medium to heavy nuclei. Introduction One of the open problems of the high energy cosmic ray is the composition of the primary particles with energies from 1 × 1015 to 1 × 1018 . In order to contribute to solve this issue, we have design and hybrid detector to be located in the Pico de Orizaba and Sierra la Negra Volcano es. One of the advantages of the site is the altitude, 4200 m.a.s.l, which may help us to observe the extended air showers nearby their maximum development, improving the determination of the parameters of the primary particle. The optical properties of the site have been studied by several years, showing stability and darkness to declare it as a good optical astronomical site. So, we thought that the installation of an fluorescence telescope, should complement the ground array and improve the overall performance of this observatory. In the other side, the implementation of the hybrid technique, based in montecarlo simulations, may allow us to separate the light and the heavy primary components. Based in simulations, we expect good quality measurement of the number of secondary particles due to the proximity of the array to the level of maximum development of the EAS Xmax .

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