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1 September 1996 Infrared adaptive optical system of the 2.16 meter telescope and its wavefront detecting error and performance analysis
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Proceedings Volume 2778, 17th Congress of the International Commission for Optics: Optics for Science and New Technology; 2778DL (1996) https://doi.org/10.1117/12.2316178
Event: 17th Congress of the International Commission for Optics: Optics for Science and New Technology, 1996, Taejon, Korea, Republic of
Abstract
A 21-element adaptive optical system[1] has been built and installed at the 2.16 meter telescope of Beijing Astronomical Observatory. It consists of a pair of photon counting shearing interferometers as the wavefront detector, a 21-element deformable mirror and a fast steering mirror as the wavefront correctors, a digital processor for computing the phase angles from the photon counts of the shearing interferometers and wavefront reconstruction and control algorithm, 23 channels of high voltage amplifier. The wavefront error sensing is in the visible wavelength and the compensated images are detected in infrared (2.2 mm) by a Pt Si CCD camera offered by the National Observatory of Japan. The installation of the adaptive optics system and the experimental observation in visible wavelength have been completed. Due to delay in development of IR CCD, observation in IR wavelength has not been completed yet. In this paper, the system and its preliminary observation results will be briefly reported. Fig. 1 shows the images of a binary star (SAO 99587) in visible wavelength with and without correction.
© (1996) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.
Wenhan Jiang "Infrared adaptive optical system of the 2.16 meter telescope and its wavefront detecting error and performance analysis", Proc. SPIE 2778, 17th Congress of the International Commission for Optics: Optics for Science and New Technology, 2778DL (1 September 1996); https://doi.org/10.1117/12.2316178
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