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The set-up and principle of operation of the systems of the SBG telescope, which was upgraded in 2005-2006 at the Kourovka Astronomical observatory, are described in detail. The reduction of the field of view (photographic plates replaced by a CCD) is compensated by an increased operation speed, achieved by automating both the telescope drives and image processing procedure.

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We report the algorithms used in the software of the upgraded SBG camera. Fast-moving satellites are observed in the "rotated" coordinate system where one of the axes points towards the pole of the object's orbit. The ephemeris for this coordinate system is computed based on the ephemeris for the equatorial coordinate system using special transition matrices. The parameters of the matrices are the coordinates of the orbital pole, which are found by averaging the vector products of the radius vectors of the consecutive positions of the satellite. The position angle of the image is computed as the difference between the hour angles of the orbital and celestial poles in the coordinate system, the pole of which coincides with the optical center of the frame. The speed of object tracking is computed via quadratic interpolation of the ephemeris in the "rotated" coordinate system.

Dynamical evolution of paired asteroids sharing close orbits was investigated. Candidates were chosen from AstDyS database by Kholshevnikov metric value. Only 33 of 105 pairs with close orbits were associated as family members. Further orbit evolution modeling was performed by Orbit9 software. Each pair had 49 overall model scenarios due to different Yarkovsky drift values for semimajor axis. Close encounters between paired objects providing time estimations and feasible mechanisms of formation were evaluated. Uncertainties of Yarkovsky drift values affected orbit evolution and caused substantial distinctions in time formation evaluating. Dwarf planet Ceres and massive asteroids (Pallas, Vesta, etc.) perturbations should be taken into account and dynamical evolution research for asteroid pairs in close orbits under passing through resonances is considered in future numerical simulations.