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摘要:
自适应光学(AO)是校正动态光学波前误差的技术。本文概述了近50年来AO的发展历程，包括发展初期，“星球大战”期间美国的发展，以及在地基高分辨力成像望远镜，激光系统(特别是惯性约束聚变)以及眼科等方面的应用，此外还给出AO的发展趋势。通过引用每一项技术发展，首创者的首篇文献，给出了比较清晰的发展脉络。
Abstract:Adaptive optics (AO) is the technology for correcting the dynamic optical wavefront errors. This article reviews the development process of AO in recent 50 years including: the first stage of development, progresses of United States in the period of "Star War", and the applications of AO in the fields of high resolution imaging of ground-based telescopes, laser systems, especially for inertial confinement fusion (ICF), and ophthalmology. Moreover the development trends of AO are also presented. For each technical innovation, the first published paper of the innovator is cited as far as possible. Giving a development skeleton of AO is the purpose of this paper.
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Key words:
- adaptive optics /
- wavefront correction /
- high resolution imaging
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Overview: Adaptive optics (AO) is the technology for correcting the dynamic optical wavefront errors. This article reviews the development process of AO in recent 50 years. Giving a development skeleton of AO is the purpose of this paper. The original ideas of Adaptive Optics were proposed by American astronomer H. W. Babcock in 1953, and Soviet astronomer V. P Linnik in 1957. At that time, there were no technical basics for realizing the proposes. Until late of the 60th decade of 20th century ARPA of US initiated to support fundamental researches of AO, the first papers of AO were published in 1997. In the period of Strategy Defense Initiatives(SDI)，since 1985 AO had its booming period, many innovations appeared, including: the theory of atmosphere turbulence and its correction, high resolution imaging of satellites, laser guide star, laser propagation through atmosphere and thermal blooming. From the 90th decade of 20th century, The applications of AO in different areas were expanded quickly. High resolution imaging of astronomical objects is firstly realized by the Come-On project of European Southern Observatory (ESO). Now AO becomes the standard configuration of large astronomical telescopes. Three giant optical telescopes of 30~50 meters are being constructed. In each of these projects, sophisticated AO systems with large scale wavefront correctors, wavefront sensors and constellation of laser guide stars are being developed. Ground based imaging of satellites is another important application of AO. The Air Force of US constructed two AO telescope with 3.6 meters mirror. In 1986 the first solar AO system was used for high resolution observation of the surface structure of the Sun. Correction of wavefront errors in large laser system such as Inertial Confinement Fusion (ICF) is another important application of AO. The first AO system used in ICF was realized in China in 1985. Since then, many AO systems were developed in ICF facilities in China and LLNL of US. The first AO system for civilian use was the retinal imaging of human eye in 1997 by Rochester University. The developing trends of AO are briefly reviewed in this paper, including expanding the correction field of AO system by Multi-layer Conjugation AO (MCAO) using constellation of laser guide stars, extreme AO for elimination the halo around the core of the corrected point spread function (PSF), miniaturization of AO system by using miniaturizing the wavefront correctors and sensors. In every section of the paper, the developments of AO in China, especially in Institute of Optics and Electronics (IOE), are also included. For each technical innovation, the first published paper of the innovator is cited as far as possible.
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图 1 Babcock设想的Seeing校正系统。望远镜物镜的刀口像成像在超正析管上，由此管探测的图像信号转化为投射到反射镜油膜上的电荷，以此来改变波前相位，实现波前反馈[2]
Figure 1. The seeing correction system proposed by Babcock, the knife edge image of telescope's pupil is detected by the orthicon, the image is converted to correction signal which is projected by an electron beam at the oil film on the Eidophor, changing the wavefront phase, thus forms a feedback close loop[2]
图 2 Linnik设想的方案，次镜N由多个子镜组成，由驱动器调节光程，入射光经干涉仪I形成干涉条纹由探测器P探测，P的分区与次镜N相对应[3]
Figure 2. The proposal of Linnik. The secondary mirror N consists of several sub-mirrors, driven by actuators to change the optical light path, the interferometer I forms fringes of the incident light which are detected by the detector P, the detecting zones of P match with the sub-mirrors of the secondary mirror N[3]
图 3 补偿成像系统CIS获取的双星和哈勃卫星的AO校正前(a1, b1)和校正后(a2, b2)的图像。(a1, a2)双星(摄于1982年5月18日)；(b1, b2)哈勃卫星(摄于1991年7月24日)[5]
Figure 3. Uncompensated (a1, b1) and compensated (a2, b2) images of binary stars and Hubble space telescope taken by CIS[5]. (a1, a2) Binary stars (taken on 18th May 1982); (b1, b2) Hubble space telescope (taken on 24th July 1991) [5]
图 5 三台超大型望远镜的主镜布局，与之对比也画出篮球场和人体的大小
Figure 5. Primary mirrors arrangement of three super large astronomical telescopes, for comparing, the sizes of basketball field and human body are also shown (update from Wikipedea)
图 12 TMT计划的钠导星星座。(a)根据不同AO系统的星座; (b) 9套钠激光发射系统(IOE提供)
Figure 12. The planned constellation of Na beacons for TMT. (a) Constituents of the constellation, different stars used for different AO system; (b) Launching system of 9 Na lasers (provided by IOE)
图 15 IOE研制的几种小型变形镜。(a)分立式驱动器，1085单元间距3 mm；(b) Bimorph变形镜，35单元，间距3 mm；(c) MEMS变形镜140单元，间距0.4 mm。(图均由光电所提供)
Figure 15. Miniature deformable mirrors developed by IOE. (a) DM with discrete actuators, 1085 element spacing 3 mm; (b) Bimorph DM, 35 element spacing 3 mm; (c) MEMS DM spacing 0.4 mm (provided by IOE)
表 1 三台超大型光学天文望远镜的主要参数
Table 1. The primary parameters of three extreme large astronomical telescopes
望远镜名称 口径/m 主镜构成 主镜材料 集光面积/m2 ELT 39.3 798×1.4 m mULE 978 TMT 30 738×1.21 m ULE 655 GMT 24.5 7×8.4 m 硼硅酸盐 368 
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表 2 TMT的首光AO系统主要参数
Table 2. The primary parameters of the first light adaptive optical systems of TMT telescope
AO系统 变形镜 导星和波前传感器 NFIRAOS (MCAO) 60×60单元，共轭高度0 km，行程8 mm~10 mm＞30×30单元，共轭高度12 km，行程＞4 mm 钠导星6~9，功率17 W~25 W，倾斜及聚焦导星1~3，红外自然导星 MIRAO 单元数15×15到30×30 钠导星1~3，功率17 W~25 W，倾斜及聚焦导星1，红外自然导星
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表 3 IOE研制的ICF用的AO系统
Table 3. AO systems for ICF developed by IOE
No. ICF facility Act. of DM Aperture of DM Wavefront sensor Set Year 1 Shenguang Ⅰ 19 Φ70 mm Hill-climbing 1 1985 2 “Shenguang Ⅲ” prototype 45 70 mm×70 mm HS 22×22 1 2004 3 “Shenguang Ⅲ” prototype 45 70 mm×70 mm HS 22×22 8 2007 4 “Shenguang Ⅱ” petaWatt 55 Φ380 mm HS 22×22 1 2009 5 “Shenguang Ⅲ” 31 390 mm×390 mm HS 22×22 24 2011
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表 4 两套极致AO系统主要参数
Table 4. The primary parameters of two extreme adaptive optical systems
系统 望远镜 口径 变形镜类型及单元数 波前传感器 帧频 波前处理算法 星冕仪 GPI Gemini 8 m 高价MEMS 1493低阶压电44单元 空间滤波SH沿直径43子孔径 2500 Hz 傅里叶变换和LQG 孔径截趾
Lyot光阑SPHERE VLT 8 m CILAS压电41×41 空间滤波SH 40×40子孔径 1200 Hz 积分和LQG 孔径截趾
Lyot光阑
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