Ultraviolet astronomical observations are significant for studying the early-type stars including O, B, A-type stars, white dwarfs, and central stars of planetary nebulae, which could have the strongest radiation in the ultraviolet region. Since ultraviolet astronomical observations are mainly carried out in space, this paper proposed several compact, light-weight and large-field ultraviolet astronomical optical systems for space observations, including refractive optical systems, catadioptric optical systems, off-axis three-mirror systems, and coaxial four-mirror systems. Combined with the optical designs, we discussed the characteristics of the designed systems, and the possibility for infrared observation by all reflective optics. In the paper, we introduced four compact optical designs: the 100 mm aperture F/2.5 refractive system with 12-degree field of view, the 100 mm aperture F/2.5 catadioptric system with 10-degree field of view, the 100 mm aperture F/3 off-axis three-mirror system with 10-degree field of view, the 100 mm aperture F/2 coaxial four-mirror system with 6-degree field of view. Optical performances and space adaptability of these designed telescopes are analyzed and compared in this paper.
The telescope's image quality will deteriorate dramatically when the sensitive optical components are misaligned. Therefore, a dynamic interferometer or star simulator is usually used to measure the misalignment information of the sensitive optical components, which can guide the calibration of these misalignments. In this work, we proposed a new alignment method that the pupil of the telescope is structurally illuminated by a bundle of collimated laser beams firstly, then the low order aberrations of coma and astigmatism generated by the misalignments are calculated by the deformed pattern of the laser beams which are recorded by the CCD at the position of in-focus and out-focus, the misalignment information can be inversely calculated by these aberrations and the telescope can be calibrated by the misalignment information. Compared to the existing alignment method, this technology can significantly decrease the requirements of precision measuring instruments or standard star points, etc., and can be used in the alignments of the telescope with different apertures and different working environments, such as the Antarctica telescope.
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