Low energy γ-ray events in imaging Čerenkov telescope arrays

Details Low energy γ-ray events in imaging Čerenkov telescope arrays Low energy γ-ray events in imaging Čerenkov telescope arrays

Sep 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995exa.....6..285k&link_type=abstract

Experimental Astronomy, Volume 6, Issue 3, pp.285-292

Astronomy and Astrophysics

Astronomy

6

Imaging Atmospheric &Ccaron, Erenkov Telescope Array, Low Energy Tev-&Gamma, -Ray Events, &Gamma, /Hadron-Separation

Scientific paper

One of the major goals in VHE-γ-ray astronomy is to open the energy range below 100 GeV with earthbound detectors. This paper demonstrates a new method for analyzing Čerenkov light of a shower in a Čerenkov telescope array. This method is successful for showers in this low energy regime where previous techniques (e.g. alpha analysis) are not applicable. A Monte Carlo simulation is applied to a system of 19 Whipple type [3, Cawley 1990] Imaging Atmospheric Čerenkov telescopes (IAČT), each built as a 10 m diameter reflector and equipped with a 109 photomultiplier tube camera. The energy threshold for a single detector of this type is given [5, Kerrick et al. 1995] as 250 GeV. Analysis of simulated coincident events of the system for those events not having enough light to apply a standard imaging analysis [4, Hillas 1985], leads to a considerably lower threshold of 85 GeV. With a new analysis method of these events it is shown that it should be possible to distinguish between γ-ray induced and proton induced showers. The improvement of sensitivity (Q = figure of merit) of this analysis method is found to be Q=2.9.

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