激光导星角度与聚焦非等晕性综合分析

采用自适应光学(AO)系统对湍流大气进行校正时,非等晕性误差的影响不可避免。基于空间谱滤波技术,围绕湍流大气角度、聚焦、角度与聚焦相耦合非等晕性问题,进行了统一建模,给出了不同情况下的理论描述公式,分析了纯角度和纯聚焦非等晕误差中不同泽尼克模式分量所占比份。针对典型AO系统工作模式,分析了不同高度大气层对非等晕性误差的贡献。实际应用时,根据应用场景,应对AO系统工作模式和信标模式做优化匹配选择。     

Laser beacon wave-front sensing without focal anisoplanatism

Wave-front sensing from artificial beacons is normally performed by formation of a focused spot in the atmosphere and sensing of the wave-front distortions produced during the beam's return passage. We propose an alternative method that senses the distortions produced during the outgoing path by forming an intensity pattern in the atmosphere that is then viewed from the ground. A key advantage of this method is that a parallel beam is used, and therefore the wave-front measurements will not suffer from the effects of focal anisoplanatism. We also envisage other geometries, all based on the concept of projecting a pupil pattern onto the atmosphere.     

基于同步探测的脉冲钠导星聚焦非等晕性实验研究

本文提出在大气Greenwood时间常数内采用同步探测技术实现钠导星聚焦非等晕性测量, 开展了脉冲体制钠导星探测实验, 实现了对大气平流层顶端钠导星和同路径自然星可见光波段的哈特曼点阵的同步探测, 并获得钠导星回光单帧波面, 从波面一致性对比、Zernike系数比较、模拟成像校正等方面对实验结果进行较全面分析. 实验结果表明, 在当前实验条件下, 虽然脉冲钠导星的单帧哈特曼点阵的成像对比度较低, 制约了波面恢复精度, 但同步测量的两组波面始终能保持相似性, 其Zernike系数在前36阶一致性较好, 模拟结果表明钠导星探测波面有助于实现对自然星成像的有效校正, 扣除波面恢复误差后的聚焦非等晕性方差小于0.1 rad², 十分接近理论结果.     

Simulation of MCAO on (extremely) large telescopes

In this article, we describe the different methods to simulate Multi-Conjugate Adaptive Optics (MCAO) systems. First, analytical (error-budget type) and semi-analytical (Fourier) methods are described. We then describe the different modules required to make end-to-end (Monte Carlo) simulations of these systems. Finally, we present some of the computational challenges associated with the simulation of MCAO on Extremely Large Telescopes (ELTs). To cite this article: M. Le Louarn et al., C. R. Physique 6 (2005).     

重复高压脉冲产生与成形一体化装置研制

介绍了脉冲变压器与分布参量形成线相结合的高功率脉冲产生与成形一体技术,简要阐述了采用该技术的高压脉冲发生器的基本设计思想。研制的脉冲变压器与形成线一体化装置利用变压器的同轴开环铁芯来充当分布电参量脉冲形成线的内外导体,将脉冲功率源中最重要的两个独立部件有机结合起来,实现了结构的紧凑性。高压脉冲发生器在重复频率100 Hz、变压器工作电压1.65 MV时能够稳定运行,输出脉冲电压760 kV,峰值功率23 GW,脉冲宽度大于40 ns。     

1.2 m望远镜自适应光学系统中激光导引星聚焦非等晕性

分析了云南天文台1.2 m望远镜61单元自适应光学系统上如果配置激光导引星,由信标上方以及信标下方采样不完整性造成的聚焦非等晕性误差大小。为了减小聚焦非等晕性误差,可以采用投射多重信标方法。同时讨论了多重信标方法造成的信标位置测量误差和圆锥倾斜误差两种额外误差,理论分析并数值模拟了当投射2~5颗钠导星和瑞利导星时其误差大小。结果表明:随着导星高度以及导星数的增加,该方法可以有效地减小聚焦非等晕性误差,对于钠导星其误差小于1 rad2。     

Versatile Raman fiber laser for sodium laser guide star

Robust high‐power narrow‐linewidth lasers at 589 nm are required for sodium laser guide star adaptive optics in astronomy. A high‐power 589 nm laser based on Raman fiber amplifier is reported here, which works in both continuous‐wave and pulsed formats. In the continuous‐wave case, the laser produces more than 50 W output. In the pulsed case, the same laser produces square‐shaped pulses with tunable repetition rate (500 Hz to 10 kHz) and duration (1 ms to 30 μs). The peak power is as high as 84 W and remains constant during the tuning. The laser also emits an adjustable sideband at 1.71 GHz away from the main laser frequency for better sodium excitation. The versatility of the laser offers much flexibility in laser guide star application.     

Adaptive optics microscopy with direct wavefront sensing using fluorescent protein guide stars

We introduce a direct wavefront sensing method using structures labeled with fluorescent proteins in tissues as guide stars. An adaptive optics confocal microscope using this method is demonstrated for imaging of mouse brain tissue. A dendrite and a cell body of a neuron labeled with yellow fluorescent protein are tested as guide stars without injection of other fluorescent labels. Photobleaching effects are also analyzed. The results shows increased image contrast and 3× improvement in the signal intensity for fixed mouse tissues at depths of 70?μm.     

辐射温度的数据处理方法

辐射温度是间接驱动惯性约束聚变实验中可以定量测量的重要物理量。引进了一种通过直接计算辐射通量来得到辐射温度的方法,该方法的主要优点是计算简单,避免了某些时刻不能计算辐射温度的情况。由该方法得到的辐射温度与传统方法计算结果符合较好,不确定度均为7%。通过与冲击波测量温度峰值的结果对比确认了数据处理方法的正确性。在此基础上建立了国内某大型激光装置上的新型15道软X光能谱仪的数据处理系统。     

激光导星自适应光学系统一阶理论模型

激光导星可以部分解决自适应光学系统信标难题。给出典型激光导星自适应光学系统主要误差空间功率谱的简化计算模型。与常用的Monte-Carlo类型的模拟相比,该模型提供了激光导星自适应光学系统性能随主要控制参数变化的一种快速有效的评估手段。     

Asymmetric cryptography based on wavefront sensing

A system of asymmetric cryptography based on wavefront sensing (ACWS) is proposed for the first time to our knowledge. One of the most significant features of the asymmetric cryptography is that a trapdoor one-way function is required and constructed by analogy to wavefront sensing, in which the public key may be derived from optical parameters, such as the wavelength or the focal length, while the private key may be obtained from a kind of regular point array. The ciphertext is generated by the encoded wavefront and represented with an irregular array. In such an ACWS system, the encryption key is not identical to the decryption key, which is another important feature of an asymmetric cryptographic system. The processes of asymmetric encryption and decryption are formulized mathematically and demonstrated with a set of numerical experiments.     

Image jitter of a laser guide star in a monostatic formation scheme

The image jitter of a spherical wave with a random center is calculated. A rigorous formula is proposed for a random vector that determines the image position of the spherical wave at the focus of the telescope under the condition that the source position also fluctuates. The variance of these fluctuations is calculated. The dependence of the variance on parameters describing the optical experiment is analyzed. The analysis of this problem is of interest for solving of a number of practical tasks including the analysis of the possibility of solution of the tilt problem upon using a laser guide star.     

Optimizing Rayleigh laser guide star range-gate depth during initial loop closing

The use of a Rayleigh laser guide star (LGS) as a wavefront reference for adaptive optics (AO) allows complete control over the distance to, and depth of, the slice of the Rayleigh plume that is selected. By altering the LGS range-gate depth (RGD) and distance at three defined stages during closed-loop operations, the LGS performance can be optimized. For the given example of a 20 km LGS on a 4.2 m telescope the application of this technique would increase the permissible RGD from 200to930 m after optimization. This can allow either an increase in LGS altitude or an increase in wavefront sensor frame rate, thereby increasing AO system performance.     

大型光学天文望远镜风载作用分析

风载对光学天文望远镜结构和镜面的作用将直接影响望远镜的面形精度和跟踪指向控制,从而降低望远镜的像质。特别是未来大型望远镜越来越多地采用主动光学技术,风载的作用将是影响主动光学子镜的主动控制及望远镜整体性能的重要因素。回顾了大型望远镜风载作用的分析方法和随机风载的性质,详细介绍了采用风速功率谱密度方法进行随机风载分析的过程和采用有限元方法分析建模的方法;建立了一个拼接镜面主动光学望远镜的完整计算模型,研究了子镜及望远镜整体在风载作用下的静态和动态响应,并分析了风载对镜面面形和望远镜的跟踪指向精度的影响。     

Experimental validation of a technique to measure tilt from a laser guide star

We have experimentally demonstrated for what is believed to be the first time a method for sensing wave-front tilt with a laser guide star (LGS). The tilt components of wave fronts were measured synchronously from the LGS by use of a telescope with a 0.75-m effective aperture and from the star Polaris by use of a 1.5-m telescope. The Rayleigh guide star was formed at an altitude of 6 km and at a corresponding range of 10.5 km by projection of a focused beam at Polaris from the full aperture at the 1.5-m telescope. Both telescope mounts were unpowered and bolted in place, allowing us to reduce substantially the telescope vibration. The maximum value of the measured cross-correlation coefficient between the tilt for Polaris and the LGS is 0.71. The variations of the measured cross-correlation coefficient in the range from 0.22 to 0.71 are caused by turbulence at altitudes above 6 km, which was not sampled by the laser beacon but affected tilt for Polaris, the cone effect for turbulence below 6 km, residual mount jitter of the telescopes, and variations of the signal/noise ratio. The results support our concept of sensing atmospheric tilt by observing a LGS with an auxiliary telescope and indicate that this method is a possible solution for the tip-tilt problem.     

基于背景纹影波前传感技术的气动光学波前重构与校正

背景纹影波前传感(backgroud oriented schlieren based wavefront sensing, BOS-WS) 是利用背景纹影技术测量光学波前二维分布的新型实验手段, 可定量测量光线通过干扰场后产生的光学畸变并给出光程差. 为了利用BOS-WS技术获得光线因气动光学效应产生的畸变信息, 并通过已知畸变信息还原原始图像, 进而探索一种新型的超声速成像制导方法, 本文通过理论分析, 验证了利用背景纹影技术测量光学波前的方法, 探索了利用已知波前信息预测畸变位移场以及利用已知位移场进行波前重构的计算方法. 通过数值模拟比较了一阶梯形积分算法和Southwell方法在波前重构上的误差大小和结果合理性, 并通过误差分析证明了Southwell方法更加精确合理. 通过蜡烛火焰上方流场畸变实验和透镜对波前的扰动实验, 创造性地探索了利用已知光学光程差还原畸变位移场及用其校正畸变图像的方法, 并通过验证性实验证明了校正方法的有效性.     

超短脉冲激光装置波前校正实验研究

为了提高光束质量和能量集中度,在SILEX I超强超短脉冲钛宝石激光装置上进行了自适应光学波前校正系统实验研究,研究了波前校正系统对波前畸变、远场焦斑及能量集中度的改善情况。该系统基于相位共轭原理,主要由哈特曼波前传感器、变形镜、电控单元及控制软件等组成。实验结果表明：进行波前校正后,波前峰谷值从1.885 μm下降到0.438 μm,均方根值从0.379 μm下降到0.052 μm;远场焦斑有明显改善;超过峰值通量1/e2的区域的能量与总能量之比为72.4%。     

空间插值在功率谱密度计算中的应用

为了提高光学元件波前中频PSD计算的精度和有效频谱宽度,提出了填补波前无效数据的双线性插值法和抑制欠采样噪声的六采样点插值法。模拟计算和实验结果表明:双线性插值法有效地保证了填充数据与真实数据的一致性,抑制了零填充方法引入的虚假中高频信息,使得填补后的PSD与原始PSD较好地吻合;六采样点插值法有效地分离了信号和欠采样噪声,使得有效PSD频谱上限从1/2 Nyquist频率提高到Nyquist频率。     

直接液体冷却薄片激光器中抽运光均匀性对光束波前畸变的影响

近年来,直接液体冷却薄片激光器因其体积功率比小,热管理能力强等优势而成为研究热点.本文建立了一套直接液体冷却薄片激光器波前畸变的分析方法.应用该方法研究了直接液体冷却薄片激光器中抽运光均匀性对光束波前畸变的影响.计算分析了均匀性为92%, 80%和70%,且总的抽运功率不变时,激光器高阶像差分布情况.随着均匀性逐渐减弱,激光器中高阶像差逐渐增强,低阶像差量基本保持不变.实验中,设计加入波导和未加入波导结构,构建了均匀性为92%和70%的抽运光分布,分别测量了两种情况下的波前抖动情况以及波前畸变分布,抽运功率为5 k W时,测量获得了整个增益模块的光程差高阶分量(OPD_H),其畸变量均方根(RMS)值为0.66μm和0.79μm,实验结果和理论分析结果基本趋势一致.     

波前解卷积方法中的高频噪声抑制

 介绍了一种波前解卷积中噪声抑制规整化的新方法，并将此方法应用于室内模拟点源实验中。该方法通过在图像复原算法中增加针对图像高频部分的限制条件来抑制高频噪声，以达到对图像复原问题病态特性的规整化。实验结果表明：该规整化方法可以有效地抑制解卷积过程中高频噪声的影响，恢复出达到理论衍射极限分辨率的图像。对于噪声水平较高的降质图像，通过这种解卷积方法可以有效地提高信噪比。同维纳逆滤波方法相比，该方法可以在有效抑制导致病态的高频噪声的基础上充分保持图像的低频；与基于贝叶斯估计的近视解卷积算法相比，该方法不需要知道噪声水平或噪声类型等先验知识，只是从噪声本质出发，通过抑制降质图像高频部分，有效地解决了病态特性问题。