First Results Obtained with Wide-Angle Cerenkov Light Telescope BEO p. Mussala

Details First Results Obtained with Wide-Angle Cerenkov Light Telescope BEO p. Mussala First Results Obtained with Wide-Angle Cerenkov Light Telescope BEO p. Mussala

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003icrc....1..225m&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

The first results from experiment using Cerenkov light of EAS, reflected from the snow surface of Ice Lake p. Mussala, Bulgaria are described. The construction of the telescope was started in autumn 2000.The first measurements with 1-meter diameter reflectors and FEU110 were carried out in winter 2000-2001. During 2002-2003 the detector was improved. The first results obtained in winter 2002-2003 are presented in this paper. Introduction Our experiment is based on the Prof. A.E. Chudakov (1972)[1] idea to detect the Cerenkov light from EAS reflected by snow surface.The special feature of that method is the possibility to use a sensitive area over some hundred square kilometers with comparatively small detectors. The intensity of Cerenkov light from EAS is proportional to the energy of the primary cosmic ray particle so this method is a calorimetric one. It gives the possibility for experimental investigation of the primary spectrum of the cosmic rays with very and ultra high energies. The Basic Environmental Observatory on peak Mussala (2925-m a.s.l) provides a real opportunity for realization of that method. The Ice Lake is located in the Mussala circus region, at 200 m below the peak (2925-m a.s.l). The lake's area is approximately 20.103 m2 . Its surface retains an ice-cover approximately 7 to 8 months annually. Detector is situated on the 212m high mountain ledge nearby Ice Lake and registers the Cerenkov light of the air showers reflected from the snow surface of the lake.The limits of the zenith angle for the photons descended by the reflecting surface, are determined by the terrain's specifics: d=0.73 rad The detector setting up consists of two parab olic reflectors with 1.40-meter diameter each. The light spots are detected by two photomultipliers (FEU-49B),

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