Gamma Ray Astronomy from 1011 to 1014 eV Using the Atmospheric Cerenkov Technique

Details Gamma Ray Astronomy from 1011 to 1014 eV Using the Atmospheric Cerenkov Technique Gamma Ray Astronomy from 1011 to 1014 eV Using the Atmospheric Cerenkov Technique

Nov 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977saosr.381.....p&link_type=abstract

SAO Special Report #381 (1977)

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The atmospheric Cerenkov technique has been widely used over the past two decades to search for point sources of 1011 to 1014 eV gamma rays. In this technique the gamma rays are detected by the Cerenkov light emission from the s that they create in the atmosphere. The basic principles underlying the technique are reviewed with particular reference to the experiments performed to date, (September 1977). The production and absorption processes that pertain to this energy region are discussed. There is strong evidence for the detection of 1012 eV gamma rays from NP0532, Centaurus A and Cygnus X-3. Models for these, and other sources for which upper limits have been derived, are outlined. There appears to be no other technique that can compete with the atmospheric Cerenkov technique in this energy range. The methods by which the present flux sensitivity can be reduced by factors of 10 - 100 are discussed; it is also possible to extend observations into the previously unexplored 10 - 100 Gev energy range.

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