恒星干涉仪延迟线系统地面随机振动响应分析

研究地面随机微振动对恒星干涉仪关键部件-光学延迟线系统性能的影响。利用美国蓝氏(Lansmont)集团生产的SAVER 3X型三轴振动仪实测地面随机振动信号,以输出的G加速度功率谱密度为激励,运用Workbench有限元分析软件计算该结构系统的随机振动响应;根据抛物镜面节点数据拟合出抛物镜面的Zernike多项式系数、抛物镜刚体平移量和抛物镜面PV和RMS值;将Zernike多项式系数导入光学系统中分析光学延迟线系统光学性能;最后利用ELCOWAT 3000电子自准直仪测量抛物镜刚体平移量,分析实际测量结果和计算理论结果偏差。分析计算结果与实验数据最大偏差7.6%,计算抛物镜面形RMS值为9.6 nm,PV值为46.1 nm,波前差为0.043λ。目前的光学延迟线的地面振动满足光学延迟线系统的稳定性要求。使用动态光学性能标准分析判断微振动对系统光学性能的影响程度,为恒星干涉仪其他子系统优化设计和隔振补偿措施提供参考。     

大冷量同轴型脉冲管制冷机蓄冷器周向温度分布实验研究

针对一台液氮温区可产生100 W制冷量的脉冲管制冷机,通过控制变量的方法实验研究了工作频率、输入功率、冷头热负荷量对蓄冷器圆周方向温度分布和最大温差的影响。研究结果表明:工作频率的改变对蓄冷器的周向温度分布影响不大,增大输入功率导致蓄冷器的周向温度不均匀性明显变强,增大冷头热负荷量可以减小蓄冷器的周向温度不均匀性。     

基于曲面拟合的光学偏折系统显示屏标定方法

针对透射式光学偏折系统中最关键的标定环节,提出使用曲面拟合方式拟合显示屏幕面形分布。建立基于透射式光学偏折术的波前检测仿真模型,分析两种不同的显示屏面形拟合方法对波前测量的影响。仿真结果显示：平面屏幕模型波前像差均方根误差(RMS)值为0.837 5μm,而曲面屏幕模型仿真波前像差RMS值仅为0.059 6μm。采用透射式光学偏折系统对球面透镜进行波前测量,曲面屏幕模型中波前像差RMS值为0.137 1μm,平面屏幕模型中波前像差RMS值为1.432 6μm。实验结果表明：使用曲面拟合效果明显优于平面拟合效果,证明了曲面拟合屏幕模型的可行性。     

非导电胶膜互连的液晶显示屏翘曲模拟

为研究非导电胶膜封装的液晶显示屏可靠性,用有限元法分析玻璃覆晶模块的温度及应力场.建立玻璃覆晶模块的三维模型,应用热-力耦合分析的顺序耦合法求解热压键合、卸载冷却过程中的模块翘曲和热应力分布.结果表明,热压键合是近稳态的热过程,凸点附近的玻璃基板和芯片温度一致,非导电胶膜在固化过程中吸收热应力、松弛热应变,玻璃覆晶模块的内部温差小、翘曲量小;卸载冷却是非稳态的热过程,模块中各点的温度相差较大,但随时间而逐渐下降并趋于一致,玻璃覆晶模块的内部温差大、热应力大、翘曲量大.减小热压键合过程中的机械载荷和卸载冷却过程中模块的温差,有利于降低液晶显示屏内部的残余热应力及翘曲.     

热贮料作用下浅圆筒仓温度效应研究

为了研究热贮料对筒仓位移及内力的影响并方便设计时计算由热贮料产生的温度效应,本文推导了热贮料作用下仓壁位移和内力的计算公式,并通过数值模拟验证了公式的准确性。利用所推导公式分析了竖向温差对钢筒仓和内外、竖向温差对混凝土筒仓的影响。结果表明竖向温差使钢筒仓在冷热贮料交界面附近的仓壁出现较大的径向位移差;并导致温度应力显著增大;该温度应力随着径厚比的减小而增大。内外温差使混凝土筒仓上端产生较大的周向拉力;竖向温差也使筒仓中部的周向力增大;且径厚比对周向力的影响与钢筒仓相似。     

曲率波前传感器波前重构算法的研究

运用衍射理论计算出两个离焦面上的光强分布,从而获得波前曲率和孔径边缘的波前径向倾斜。根据Zernike多项式的微分特性,采用两种不同的方法分别处理曲率和倾斜,使用积分的方法解决了在边界上δ函数很难处理的问题。由探测器的几何分布预先算出控制矩阵,用Zernike多项式曲线拟合的方法重构出波前。计算机仿真表明,波前残差小于5％,验证了此波前重构算法的可行性。     

用于全景成像系统的一种新型光学非球面

介绍一种用于全景成像系统的单个复杂非球面前置元件,从几何光学的基本原理出发,给出了这种非球面的高斯分析和不同情况下的面形方程,利用正交拟合算法得到了便于实现光路计算的多项式表述,并成功地运用于光线追迹和像差计算。     

非球面非零位横向剪切干涉检测与波前重建

本文分析了非球面非零位检测中3种典型的非球面度及其变化率、调整误差、回程误差以及干涉仪系统误差,提出了非球面度变化率是影响检测误差的主要因素,并给出了非球面非零位检测面形加工误差的确定方法.对基于Zernike多项式拟合的最小二乘法和系数转换法进行了对比研究,分析了剪切量和多项式拟合阶数对波前重建精度的影响,并给出了数值模拟结果.为了验证以上方法的可行性及检测精度,针对一单点金刚石车削的抛物面反射镜,利用顶点球作为测试波前进行非零位横向剪切干涉检测,并用最小二乘法进行波前重建.实验结果表明,在非球面度变化率最大的反射镜边缘处面形误差最大,达到0.203μm,研究结果为横向剪切干涉仪用于非球面加工过程中在位检测提供了技术支撑.     

受大气湍流影响的光学波前模拟

大气湍流对光学波前的影响可以用Ｚｅｒｎｉｋｅ模式分析，由于Ｚｅｒｎｉｋｅ模式并非统计独立，需要转而寻找一种称为Ｋａｒｈｕｎｅｎ－Ｌｏｅｖｅ（简称Ｋ－Ｌ）函数的系数，它们统计独立，而且可以展开为Ｚｅｒｎｉｋｅ多项式的形式。本文介绍的就是用Ｋ－Ｌ函数构造随机波前的原理和仿真构造尝试。     

碲酸盐系统玻璃组成和结构对非线性光学性能的影响

碲酸盐系统重金属氧化物玻璃是一种优秀的非线性光学玻璃材料，具有较大的三阶非线性光学效应、超快光学响应、较宽红外透过范围、较好稳定性以及广泛应用前景。碲酸盐系统玻璃中的中间离子和网络外离子的加入会改变组成网络的配位多面体组成、键性和能带结构，进而影响玻璃的非线性光学性能。探讨了碲酸盐系统玻璃的网络结构，阐述了玻璃组成、结构以及纳米簇和非线性光学性能之间的相互关系。     

Gaussian weighting of ocular wave-front measurements

The measurement of ocular wave-front error gives insight into the optical performance of the eye and possibly a means for assessing visual performance. The visual system responds not only to the quality of the optical image formed on the retina but also to the processing that occurs in the retina and the brain. To develop a metric of visual performance based on wave-front error measurements, these latter processes must somehow be incorporated. In representing the wave-front error in terms of Zernike polynomials, it appears that terms with lower angular frequency have a greater deleterious effect on visual performance than higher-angular-frequency terms. A technique for weighting the pupil function of the eye with a Gaussian filter is demonstrated. It is further demonstrated that the variance of the Gaussian-weighted wave-front error is well correlated with visual performance.     

Statistical variation of aberration structure and image quality in a normal population of healthy eyes

A Shack-Hartmann aberrometer was used to measure the monochromatic aberration structure along the primary line of sight of 200 cyclopleged, normal, healthy eyes from 100 individuals. Sphero-cylindrical refractive errors were corrected with ophthalmic spectacle lenses based on the results of a subjective refraction performed immediately prior to experimentation. Zernike expansions of the experimental wave-front aberration functions were used to determine aberration coefficients for a series of pupil diameters. The residual Zernike coefficients for defocus were not zero but varied systematically with pupil diameter and with the Zernike coefficient for spherical aberration in a way that maximizes visual acuity. We infer from these results that subjective best focus occurs when the area of the central, aberration-free region of the pupil is maximized. We found that the population averages of Zernike coefficients were nearly zero for all of the higher-order modes except spherical aberration. This result indicates that a hypothetical average eye representing the central tendency of the population is nearly free of aberrations, suggesting the possible influence of an emmetropization process or evolutionary pressure. However, for any individual eye the aberration coefficients were rarely zero for any Zernike mode. To first approximation, wave-front error fell exponentially with Zernike order and increased linearly with pupil area. On average, the total wave-front variance produced by higher-order aberrations was less than the wave-front variance of residual defocus and astigmatism. For example, the average amount of higher-order aberrations present for a 7.5-mm pupil was equivalent to the wave-front error produced by less than 1/4 diopter (D) of defocus. The largest pupil for which an eye may be considered diffraction-limited was 1.22 mm on average. Correlation of aberrations from the left and right eyes indicated the presence of significant bilateral symmetry. No evidence was found of a universal anatomical feature responsible for third-order optical aberrations. Using the Marechal criterion, we conclude that correction of the 12 largest principal components, or 14 largest Zernike modes, would be required to achieve diffraction-limited performance on average for a 6-mm pupil. Different methods of computing population averages provided upper and lower limits to the mean optical transfer function and mean point-spread function for our population of eyes.     

Wind-induced deformations in a segmented mirror

A Zernike expansion of wind-induced deformations in a segmented mirror is described. The wind model is a frozen turbulent field with a Kolmogorov spectrum for scales smaller than the outer scale and a flat spectrum for scales larger than the outer scale. The approach allows a mode-by-mode comparison of the wave-front error contributions from atmospheric phase distortions, wind-induced deformations, and the mirror control system noise. This is used to design a controller that minimizes the mirror surface errors by application of corrections based on edge sensor measurements and wave-front measurements on a guide star.     

Hubble Space Telescope Faint Object Camera calculated point-spread functions

A set of observed noisy Hubble Space Telescope Faint Object Camera point-spread functions is used to recover the combined Hubble and Faint Object Camera wave-front error. The low-spatial-frequency wave-front error is parameterized in terms of a set of 32 annular Zernike polynomials. The midlevel and higher spatial frequencies are parameterized in terms of set of 891 polar-Fourier polynomials. The parameterized wave-front error is used to generate accurate calculated point-spread functions, both pre- and post-COSTAR (corrective optics space telescope axial replacement), suitable for image restoration at arbitrary wavelengths. We describe the phase-retrieval-based recovery process and the phase parameterization. Resultant calculated precorrection and postcorrection point-spread functions are shown along with an estimate of both pre- and post-COSTAR spherical aberration.     

Noise propagation in wave-front sensing with phase diversity

The phase diversity technique is studied as a wave-front sensor to be implemented with widely extended sources. The wave-front phase expanded on the Zernike polynomials is estimated from a pair of images (in focus and out of focus) by use of a maximum-likelihood approach. The propagation of the photon noise in the images on the estimated phase is derived from a theoretical analysis. The covariance matrix of the phase estimator is calculated, and the optimal distance between the observation planes that minimizes the noise propagation is determined. The phase error is inversely proportional to the number of photons in the images. The noise variance on the Zernike polynomials increases with the order of the polynomial. These results are confirmed with both numerical and experimental validations. The influence of the spectral bandwidth on the phase estimator is also studied with simulations.     

Model MTF for the mosaic window

An electro-optical targeting system mounted either within an airframe or housed in separate pods requires a window to form an environmental barrier to the outside world. In current practice, such windows usually use a mosaic or segmented window. When scanning the target, internally gimbaled systems sweep over the window, which can affect the modulation transfer function (MTF) due to wave-front division and optical path differences arising from the thickness/wedge differences between panes. In this paper, a mathematical model of the MTF of the mosaic window is presented that allows an analysis of influencing factors; we show how the model may be integrated into ZEMAX® software for optical design. The model can be used to guide both the design and the tolerance analysis of optical systems that employ a mosaic window.     

Visualization of surface figure by the use of Zernike polynomials

Commercial software in modern interferometers used in optical testing frequently fit the wave-front or surface-figure error to Zernike polynomials; typically 37 coefficients are provided. We provide visual representations of these data in a form that may help optical fabricators decide how to improve their process or how to optimize system assembly.     

Atmospheric turbulence characterization with the Keck adaptive optics systems. I. Open-loop data

We present a detailed investigation of different methods of the characterization of atmospheric turbulence with the adaptive optics systems of the W. M. Keck Observatory. The main problems of such a characterization are the separation of instrumental and atmospheric effects and the accurate calibration of the devices involved. Therefore we mostly describe the practical issues of the analysis. We show that two methods, the analysis of differential image motion structure functions and the Zernike decomposition of the wave-front phase, produce values of the atmospheric coherence length r0 that are in excellent agreement with results from long-exposure images. The main error source is the calibration of the wave-front sensor. Values determined for the outer scale L0 are consistent between the methods and with typical L0 values found at other sites, that is, of the order of tens of meters.     

Wave-front analysis with high accuracy by use of a double-grating lateral shearing interferometer

A phase-stepped double-grating lateral shearing interferometer to be used for wave-front analysis is presented. The resulting interference patterns are analyzed with a differential Zernike polynomial matrix-inversion method. Possible error sources are analyzed in the design stage, and it is shown that the inaccuracy can be kept within 2-5 mλ rms. The apparatus was tested and evaluated in practice. Comparison with a phase-stepped Twyman-Green interferometer demonstrates that the accuracy of the two methods is comparable. Lateral shearing interferometry scores better on reproducibility, owing to the stability and robustness of the method.