Abstract
The time spread of the rays collected by a large diameter imaging atmospheric Cherenkov telescope (d∼20–30 m) is investigated. We compare the influence of the geometry of the spherical and parabolic reflectors on the shape and duration of collected Cherenkov light. It is shown that the design‐induced additional widening of the collected Cherenkov light pulse is essential for the spherical reflector of Davies‐Cotton type, and is negligibly small for the parabolic reflector. At the detection of 10 GeV γ‐showers, the pulse width on the spherical telescope’s focal plane may reach 15–20 ns instead of 5–8 ns inherent to the incident light pulse itself. In the case with a parabolic telescope the pulse widths of the light incident on the telescope disk and collected onto the camera are almost identical.
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