High resolution observation by means of tomographic adaptive optics

为提高大望远镜的空间分辨率，本课题开展了具有实用价值的自适应光学系统的研究。(1)为Okayama 188 cm望远镜的红外光谱仪研制了波前倾斜校正系统，即所谓的稳像器，并进行了实际使用标定。为了提高系统的效率，设计、测试和实现了伺服回路的自适应控制系统。(2)介绍了与CFHT小组在现有望远镜外壳上进行的内部穹顶视度评估的联合实验，并制作了专用的原始仪器--穹顶视宁仪并进行了标定。(3)直径50 mm、厚度0.5 mm的变形镜，(4)与JPL合作，设计并制造了一种新型的具有跳跃式结构的平读CCD，以降低读取噪声，保证快速的帧速率。(5)建立了由波前误差计算驱动信号的控制算法。(6)模拟曲率传感来评价湍流大气的垂直结构。(7)研究了利用层析成像方法评价湍流空气三维结构的实际问题，并研究了解决这些困难的可能途径。这些成果符合本项目最初的研究目标，为建立适用于天文学的自适应光学系统开辟了一条切实可行的途径。

Researches carried out in this project were to establish the adaptive optics systems of practical use in order to improve the spatial resolution of large telescopes.(1) The wavefront tilt correcting system, the so-called image stabilizer, optimized for the Coude infrared spectrograph of Okayama 188cm telescope was assembled and calibrated for actual usage. In order to enhance the efficieny of this system, an adptive control system of the servo loop was designed, tested, and implemented.(2) A joint experiment with the CFHT group to evaluate the internal dome seeing at the existing telescope enclosure is outlined and a special original instrument, named a dome-seeing monitor, was fabricated and calibrated.(3) A deformable mirror, 50mm in diameter, 0.5mm in thickness, mounted on 37 piezo actuators was fabricated and calibrated.(4) A new type parallel-read CCD with skipper architecture to reduce the read noise and ensure fast frame rate was designed and manufactured in collaboration with the JPL.An electronic system to evaluate the performance of this system is under construction.(5) Control algorithm to calculate the drive signal from wavefront error was etablished.(6) Simulation of curvature sensing to evaluate the vertical structure of the turbulent atmosphere was made.(7) Practical problems of evaluating the 3D structure of turbulent air using tomographic methods were assecced and possible ways to solve these difficulties were studied.These achievements are in line with the original research goals of the present project and opened a practical way to establish an adaptive optives system useful for astronomy.