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Abstract
Abstract The question of the emission of very high and ultra high energy γ rays from the Galactic plane is an experimentally unresolved question. We discuss the detectability of the expected flux in the VHE range by means of ultraviolet Cherenkov telescopes, even with no requirement for hadron-γ discrimination, using a technique alternative to imaging in data analysis. We point out that this kind of measure is probably pertinent for ultraviolet Cherenkov systems, before any measure of discrete sources (the Crab included); this could be then the proper bench-mark for the sensitivity of these systems.
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