Abstract
The high energy end of γ-ray source spectra might provide important clues regarding the nature of the processes involved in γ-ray emission. Several galactic sources with hard emission spectra extending up to more than 30 TeV have already been reported. Measurements around 100 TeV and above should be an important goal for the next generation of high energy γ-ray astronomy experiments. Here we present several techniques providing the required exposure (∼ 100 km2 ⋅ h). We focus our study on three Imaging Atmospheric Cherenkov Technique (IACT) based approaches: low elevation observations, large field of view telescopes, and large telescope arrays. We comment on the advantages and disadvantages of each approach and report simulation based estimates of their energy ranges and sensitivities.
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