基于FPGA技术的波前斜率处理方法

以61单元自适应光学系统中的高速实时波前处理机为例，分析了传统基于DSP的波前斜率处理方法的优缺点，提出了一种基于FPGA技术，采用单像素控制的新型波前斜率处理方法，该方法可以使得波前斜率处理机的实时性更强，体积更小，并能适用于不同子孔径布局和不同子孔径数的自适应光学系统。     

大口径拼接望远镜成像系统的远场特性

本文根据衍射光学理论和几何光学理论,利用已得到的拼接望远镜的理论解析表达式和建立的数值仿真模型,对拼接望远镜光学系统的远场特性进行了分析计算,包括系统的理论衍射光斑直径、点扩散函数、斯特列尔比以及光学传递函数等。并根据仿真模型分析了拼接主镜中分块镜平移误差和倾斜误差对拼接望远镜系统远场的影响。分析结果表明,拼接主镜的平移误差和倾斜误差都影响系统的点扩散函数、斯特列尔比和光学传递函数,并使远场成像模糊;其中分块镜倾斜误差会额外引入平移量,如果补偿掉平移量对望远镜系统的远场性能有很大提高。     

基于高斯光斑的相关HS波前斜率处理器

大规模自适应光学系统要求哈特曼-夏克波前传感器的子孔径数目巨大,这势必会增加波前斜率提取电路实现的难度.为了在大规模自适应光学系统中进行波前斜率提取,提出了一种相关算法的实现结构,以高斯光斑作为参考模板,通过两次级联滤波完成子孔径光斑之间的相关运算,并得到局部波前斜率.与多通道并行处理的实现结构相比,本文所提出的结构实现的硬件成本不会随着子孔径规模的增大而显著增加,特别适用于大规模自适应光学系统的波前斜率提取.实验结果表明:对于8×8方形排布的哈特曼-夏克波前传感器图像,本文的结构用FPGA内实现,在27 MHz的工作频率下,完成一帧所有子孔径斜率计算的延迟为1.2 μs,均方根误差小于0.02个像素,最大误差不超过0.04个像素,而资源消耗仅仅为925个Slices.本结构能够满足大规模自适应光学系统中波前斜率探测高速实时和高精度要求.     

掠入射光学系统成像质量评价

为了能够全面评价掠入射光学系统的成像质量,基于像差理论和傅里叶光学原理,使用Matlab 编程语言编写了针对掠入射系统的像质评价程序,并利用此程序结合ZEMAX 软件对用于太阳观测的Wolter I 型和双曲面-双曲面(H-H)型掠入射系统的成像质量做了详细的分析.结果表明,该像质评价程序能够计算不同口径和焦距的掠入射系统在不同视场,不同工作波长时的点扩散函数、能量集中度、线扩散函数和调制传递函数,对掠入射系统的设计和优化具有指导作用.     

基于FPGA+DSP的USB高速数据采集系统设计与实现

为了满足高速数据采集系统的实时性、高速性和结构小型化要求,设计完成了基于FPGA+DSP+USB控制器架构的嵌入式数据采集与处理系统.利用FPGA实现多通道高速数据采集,利用DSP完成对已采集数据的处理.系统采用高速USB2.0控制器完成对数据的高速传输.实验表明,该系统采样速率最高可达10 MSPS,并具有较高的实时性与稳定性.     

小波分析方法描述光学系统传递函数

本文运用小波尺度函数描述了光学系统的传递函数。根据小波光学波前滤波思想,把光学系统看作滤波器,认为是光学系统对光波进行滤波,滤波后的光场将按权重重新分配,并以小波尺度函数来描述光学系统的点扩散函数。     

基于脉动阵列的自适应光学实时波前处理机设计

针对自适应光学系统对波前处理机高计算量、高实时性的要求,本文提出了一种基于脉动阵列的自适应光学实时波前处理方法.该方法将脉动阵列的概念引入波前处理机设计,完成了波前斜率计算、复原运算和控制运算向脉动阵列的映射,合理地建立了数据的深度流水线,同时分析了以FPGA技术实现时系统的计算延时.对于48个子孔径,61单元的自适应光学系统,以一片Xilinx Virex-Ⅱ XC2V3000芯片实现了基于脉动阵列的实时波前处理机,实验测得计算延时仅8.6μs,结果表明该方法能极大地提高系统的实时性,集成度、通用性和扩展性.     

一种新型多电平逆变门信号发生器的设计

早期的实现5级MSMI的在线PWM(脉宽调制)开关的开发,是用DSP控制器,任务仅能在采样时间的100μs内完成,提出基于FPGA的多电平逆变门信号发生器,采用一个在线最佳PWM(脉宽调制)开关来控制其输出电压,减轻用DSP实现门信号产生中消耗时间的计算任务,产生门信号的取样时间被减为,详细介绍以FPGA为基础的门信号发生器的设计和开发,最后给出用MAX+PLUSII软件进行实时仿真的结果,并用FLEX10K20(Altera公司的FPGA器件)对结果加以验证。     

用CCD测量光学系统OTF的研究

线性光学系统的光学传递函数可由线扩散函数的付立叶变换求出。本文研究了用电荷耦合器件测量光学系统OTF的系统,用CCD作为光电转换器件,对CCD接收到的LSF的光强信号进行视频放大,采样一保持、A/D转换接口到计算机,可方便而精确地测得光学系统的OTF。为了避免采用高速A/D和DMA方式,对CCD的信号处理采用分时处理。用CCD测量MTF的误差为3%,不重复性为1%,能在2分钟之内测试出物镜的10种空间频率的MTF值。     

连续扫描成像光学系统MTF的数值分析(英文)

为了实现高分辨力,在地球静止轨道上工作的遥感系统通常装备大口径光学系统,但光学系统的视场通常很小。扫描成像技术可使地球静止轨道上的高分辨力遥感光学系统获得更大的观测范围。但在扫描镜转动时像点一直在移动,所以在CCD曝光时间内会出现像点混叠。因此,扫描成像光学系统的调制传递函数将变差。本文采用动态光学传递函数分析方法研究了连续扫描成像光学系统成像性能。结果表明,在曝光时间范围0.5~1.5 ms,扫描镜的旋转角度应小于(7×10-6)o以保持较高的MTF。最后,给出了连续扫描镜的驱动方法并分析了扫描镜驱动不稳定性对MTF的影响。本文的研究结果可为连续扫描成像光学系统的深入研究和制作提供参考。     

Estimating the effects of structural vibration on adaptive optics system performance

This paper presents analytical tools developed for estimating the effects of structural vibration on closed-loop adaptive optics system image quality. The general equation for the normalized intensity distribution of an image subject to structural vibration is derived. The resulting two-dimensional theoretical point spread function is computed numerically and compared with empirical data obtained on sky at the Multiple Mirror Telescope Observatory. A simplified analytical expression for the normalized intensity distribution is derived for long exposures and used to quantify the effects on Strehl and spot full width at half-maximum as a function of vibration amplitude, telescope diameter, and observation wavelength.     

Modal compensation and the atmospheric-turbulence outer scale: computer simulations

The influence of the turbulence outer scale on the Strehl ratio obtained with low-order adaptive optics systems is examined by numerical simulation. The Karhunen-Loeve approach is used to generate wave-front samples. A method that allows construction of the outer-scale-dependent Karhunen-Loeve functions is described. It is shown that the Strehl ratio produced by a second-order adaptive optics correction (tip-tilt, defocus, and astigmatism) is affected quite strongly by the finite outer scale. For the higher-order correction, the effect under study is weak and appears only when the outer-scale magnitude becomes less than the aperture diameter. It is also shown that the finite outer scale has a positive effect on the Strehl ratio of the uncorrected long-exposure image.     

Comparison of curvature-based and Shack-Hartmann-based adaptive optics for the Gemini telescope

We present the results of independent numerical simulations of adaptive optics systems for 8-m astronomical telescopes that use both Shack-Hartmann and wave-front curvature sensors. Four differents codes provided consistency checks and redundancy. All four simulate a complete system and model noise and servo-lag effects. A common atmospheric turbulence generator was used for consistency. We present the main characteristics of the codes, and we report the system performance in term of Strehl ratio and full width at half-maximum versus the magnitude of the (on-axis) guide star. We show that a Shack-Hartmann plus stacked actuator mirror system with 10 x 10 subapertures or a curvature plus bimorph mirror system with 56 subapertures yields a 50% Strehl ratio at 1.6 mum for a m(R) = 14.7 magnitude star, with almost equivalent performance at both brighter and dimmer light levels.     

Adaptive optics for in-orbit aberration correction: spherical aberration feasibility study

We investigate the feasibility of using an adaptive mirror for in-orbit aberration corrections. The advantage of an in situ aberration correction of optical components in the space environment is that the mirror shape can be adjusted in an iterative fashion until the best image is obtained. Using the actuator spacing, corresponding to one half of the Nyquist frequency, the Strehl ratio of the corrected wave front improves to 0.95 when the mirror is fabricated with 6.5 waves of spherical aberration. The Strehl ratio decreases to 0.86 when the number of actuators is reduced by a factor of 4, in a two-dimensional adaptive optics model.     

Optimal filter for phase correction of anisoplanatism

An optimal filter algorithm for adaptive optics provides a powerful method for phase correction for propagation through the Earth's turbulent atmosphere involving anisoplanatism. In the new algorithm the outward phase correction is the sum of the product of a weighting function (the optimal filter) and all the wave-front measurements at the pupil, greatly improving the Strehl ratio. Two simplified cases are presented for illustration: (1) a collimated beam traversing a layer of uniform isotropic turbulence (angle anisoplanatism) and (2) focus anisoplanatism. It compares favorably with tomographic techniques. The technique can be extended to the case of thick, strong turbulence in the far field of a subaperture of an adaptive optics system.     

Calibration of a deformable mirror and Strehl ratio measurements by use of phase diversity

Calibration experiments with a bimorph mirror are presented. Phase-diversity wave-front sensing is used for measuring the control matrix, nulling wave-front errors in the optical setup, including the mirror, and measuring Strehl ratios and residual higher-order aberrations. The Strehl ratio of the calibrated system is measured to be 0.975, corresponding to 1/40 wave rms in the residual wave front. The conclusion is that a phase-diversity wave-front sensor is easier to install and use than interferometers and can replace them in optical setups for testing adaptive optics systems.     

Adaptive optics with four laser guide stars: correction of the cone effect in large telescopes

We study the performance of an adaptive optics (AO) system with four laser guide stars (LGSs) and a natural guide star (NGS). The residual cone effect with four LGSs is obtained by a numerical simulation. This method allows the adaptive optics system to be extended toward the visible part of the spectrum without tomographic reconstruction of three-dimensional atmospheric perturbations, resolving the cone effect in the visible. Diffraction-limited images are obtained with 17-arc ms precision in median atmospheric conditions at wavelengths longer than 600 nm. The gain achievable with such a system operated on an existing AO system is studied. For comparison, performance in terms of achievable Strehl ratio is also computed for a reasonable system composed of a 40 x 40 Shack-Hartmann wave-front sensor optimized for the I band. Typical errors of a NGS wave front are computed by use of analytical formulas. With the NGS errors and the cone effect, the Strehl ratio can reach 0.45 at 1.25 microm under good-seeing conditions with the Nasmyth Adaptive Optics System (NAOS; a 14 x 14 subpupil wave-front sensor) at the Very Large Telescope and 0.8 with a 40 x 40 Shack-Hartmann wave-front sensor.     

Improving the performance of a pyramid wavefront sensor with modal sensitivity compensation

We describe a solution to increase the performance of a pyramid wavefront sensor (P-WFS) under bad seeing conditions. We show that most of the issues involve a reduced sensitivity that depends on the magnitude of the high frequency atmospheric distortions. We demonstrate in end-to-end closed loop adaptive optics simulations that with a modal sensitivity compensation method a high-order system with a nonmodulated P-WFS is robust in conditions with the Fried parameter r 0 at 0.5 microm in the range of 0.05-0.10 m. We also show that the method makes it possible to use a modal predictive control system to reach a total performance improvement of 0.06-0.45 in Strehl ratio at 1.6 microm. Especially at r 0=0.05 m the gain is dramatic.     

Image-quality metrics for characterizing adaptive optics system performance

Adaptive optics system (AOS) performance is a function of the system design, seeing conditions, and light level of the wave-front beacon. It is desirable to optimize the controllable parameters in an AOS to maximize some measure of performance. For this optimization to be useful, it is necessary that a set of image-quality metrics be developed that vary monotonically with the AOS performance under a wide variety of imaging environments. Accordingly, as conditions change, one can be confident that the computed metrics dictate appropriate system settings that will optimize performance. Three such candidate metrics are presented. The first is the Strehl ratio; the second is a novel metric that modifies the Strehl ratio by integration of the modulus of the average system optical transfer function to a noise-effective cutoff frequency at which some specified image spectrum signal-to-noise ratio level is attained; and the third is simply the cutoff frequency just mentioned. It is shown that all three metrics are correlated with the rms error (RMSE) between the measured image and the associated diffraction-limited image. Of these, the Strehl ratio and the modified Strehl ratio exhibit consistently high correlations with the RMSE across a broad range of conditions and system settings. Furthermore, under conditions that yield a constant average system optical transfer function, the modified Strehl ratio can still be used to delineate image quality, whereas the Strehl ratio cannot.