An optical system of a Schmidt-type telescope for orbital detection is proposed. The system contains a spherical mirror and correction plate with one aspherical surface and has the following characteristics: field of view (FoV) is 40 deg, entrance pupil diameter is 2.5 m, diameter of spherical mirror is 4 m, and f-number is 0.74. The system with the described parameters has image spot size of 3.2-mm (RMS) diameter for the axial beam and 4 mm (RMS) on the edge of the FoV, which is less than the diagonal of the detectors square pixel of 3×3 mm2.
Idea of ultrahigh cosmic rays (UHECR) measurement from satellites was suggested by Linsley in 1981 and since
has being developed into projects of cosmic rays telescopes for International Space Station (ISS): JEM-EUSO -
to be installed on the Japanese experimental module and KLYPVE - on the Russian ISS segment. A series of
space-based detectors for measurements of background phenomena in those telescopes were developed in Russia
(Universitetsky-Tatiana, Universitetsky-Tatiana-2 , Chibis satellites). The satellite Lomonosov with UHECR
detector TUS on its board will be launched in 2013. TUS contains multi-channel photo receiver and Fresnel-type
mirror manufactured with use of special multi-layer carbon plastic technology in RSC “Energia". In this paper
one and two component optical systems with 360 cm entrance diameter and 400 cm focal distance for wide angle
detector KLYPVE are studied. In one component case using generalized Davies-Cotton systems (Fresnel-type
mirror with ellipsoidal gross surface) it is possible to obtain 8-10° field of view (FoV) with focal spot size less
than pixel size equal to 15 x 15 mm. In two component system (parabolic mirror and a Fresnel lens, mounted
close to photo receiver) it is possible to increase FoV up to 10-12° and significantly simplify the primary mirror
construction.
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