The atmospheric Cherenkov technique in gamma-ray astronomy - The early days

Details The atmospheric Cherenkov technique in gamma-ray astronomy - The early days The atmospheric Cherenkov technique in gamma-ray astronomy - The early days

Jun 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981rspta.301..611j&link_type=abstract

(Royal Society, Discussion on Gamma-Ray Astronomy, London, England, Nov. 27, 28, 1980.) Royal Society (London), Philosophical Tr

Astronomy and Astrophysics

Astronomy

1

Cerenkov Radiation, Gamma Ray Astronomy, Gamma Ray Bursts, Radiation Measurement, Atmospheric Radiation, Cosmic Ray Showers, Technology Assessment

Scientific paper

The detection of ultra-high-energy gamma-rays in the energy range from 0.1 to 10 trillion eV by means of the atmospheric Cerenkov technique is considered. The technique depends on the detection of the Cerenkov light produced by the vast swarm of charged particles, mainly electrons and positrons, generated in the atmosphere as a result of primary high-energy gamma-rays entering the top of the atmosphere. The Cerenkov technique is the only one that is available for studies of gamma-rays of such high energy. It is unique in that it is ground-based, directional, and relatively simple and cheap. The one serious limitation is that there is no simple way of distinguising between the gamma-ray induced extensive air shower (e.a.s.) and the far more abundant proton-induced e.a.s. except by the fine angular structure expected from gamma-ray sources. Attention is given to reminiscences of early days in the field and the characteristics of atmospheric Cerenkov radiation produced by the e.a.s.

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