The angular micro-vibration of a high resolution camera mounting on an agile satellite was achieved based on pairs of liner accelerometers alignment and numerical integration method. Three pairs of sensors were mounted at different portion of the satellite for studying the structure transfer character, including the Reaction Wheel (RW)interface, the camera interface and the camera tail. The results showed that the RW original micro-vibration standard deviation (STD) output acquired at the RW interference was 1.63μrad at RW 400rpm and increased to 2.43μrad when the RW speed up to 800rpm. When transferring from RW to the camera interface, the angular vibration response STD was attenuated to 0.31μrad@400rpm and 0.27μrad@800rpm, and finally to the camera tail the angular vibration response STD became 0.31μrad@400rpm and 0.30μrad@800rpm. We can see that the satellite-camera structure has a good attenuation effect on the micro-vibration, the output angular micro-vibration STD is about 0.31μrad with an input of 1.63μrad~2.43μrad. the stiffness of the camera is pretty good, ensuring that the micro-vibration STD difference between the camera flange and the camera tail is smaller 0.03μrad. In addition, we found that the FOGs useful bandwidth wasn’t insufficient when acquiring about 340Hz main frequency vibration signal in our case, even though a higher stiffness flange was recommended which connecting the FOG and camera.
Detection and recognition of space objects with ground-based photoelectric systems is one of the major technical ways for space situational awareness. During the past thirty years, there has been significant development of optical telescopes dedicated to wide-field surveys of time-dependent deep space phenomena, slow-moving near-earth objects (NEOs) and fast-moving earth-orbiting space debris. While telescope fields of view have gradually increased, a single technical approach has not emerged as the dominant design. To design an effective wide-field telescope for sky survey or space surveillance, It is necessary to carefully match the characteristics of the optical system (layout, aperture, focal ratio and modulation transfer function) with those of the observing site (sky brightness, transparency, seeing and elevation), the detector (pixel pitch, quantum efficiency, read rate and read noise), and the observing program (target brightness, target motion, observing strategy and feature extraction software). In this paper, we design a telescope with wide field of view (≥2.5°×3.5°) and large aperture (1.1m). The focal length of the system is 1.5m, F/# is 1.36. Because of the small Fnumber and wide field of view, we choose the prime focus corrector structure which has single mirrors with refractive prime focus correctors. Moreover, the especial requirements of the Modulation Transfer Function (MTF), spot, energy concentration, and distortion etc. are all satisfied.