光斑质心亚像素定位误差的实验研究

根据误差的来源将光斑质心亚像素定位误差归类为随机误差和系统误差,提出一种简单有效的实验方法对光斑质心定位误差进行定量测试.利用高精度一维电动平移台、POINT GREY Flea2-14S3 CCD相机和LED光源构建了测试系统,对测试结果进行研究和讨论,发现了测试系统LED光斑质心定位系统误差的周期性变化规律,计算得到了基于Flea2-14S3 CCD相机的光斑质心定位随机误差为0.018 pixels,系统误差为0.06 pixels,总体误差为0.063 pixels(约1/15 pixels),能够应用于以光斑质心检测为手段的测量系统中.实验表明,该测试系统可以作为估算光斑质心定位误差大小的一种有效的手段.     

Centroid error analysis of Shack–Hartmann wave-front sensor induced by the sensitivity non-uniformity

Centroid error is the crucial limit to the performance of the Shack–Hartmann wave-front sensor. The previous studies showed that the centroid error was affected by the discrete sample, the photon noise and the readout noise of the CCD. For many special characters, a CMOS camera is also used in the Shack–Hartmann wave-front sensor. Compared to a CCD, the sensitivity of a CMOS camera is obviously non-uniform. In this paper, a detailed analysis of the centroid error induced by the sensitivity non-uniformity of pixels is presented. The theoretical results are represented and demonstrated through an experiment. The results show that the error induced by the sensitivity non-uniformity is only dependent upon the detector, and has no relationship with the other factors. For the CMOS camera mentioned in this paper, the centroid error is less than 0.015 pixels.     

CCD 超分辨率位置测量方法及性能分析

从理论上分析了光信号的分布形式及分布规律对 CCD 超分辨力位置测量的影响, 以高斯分布和均匀分布信号为例进行了具体分析与比较. 在此基础上提出了一种基于划分一维宏像素计算质心序列点, 通过拟合序列点剔除噪声影响的 CCD 超分辨力位置估计方法, 分析了这一算法的不确定度. 理论与实验表明, 这一算法的位置测量精度达到 0.02 个像素. 实验中通过与边缘拟合法、传统质心法的比较, 表明这一方法具有更强的抗噪声能力和较高的准确性.     

脉冲激光光谱测试仪的设计

设计了一种基于ISP技术的线阵CCD的驱动电路和高速脉冲光谱数据采集卡,建立了一套智能化脉冲激光光谱测试系统。该系统主要由分光系统、CCD传感器、光脉冲同步信号发生器、数据采集卡及计算机等部分组成。CCD将光强信号转换为电信号输出,经A/D转换器转换后的数字信号存入数据采集卡的帧存储器中,由计算机控制进行光谱数据的分析、处理。提出了用重心法对脉冲激光器的重复频率进行评估的方法,使测量精度达到了亚像素级。对系统所用脉冲激光器谱线峰值波长的复现性进行了测量,其标准差为0.0327nm。     

星敏感器曝光时间的优化

星敏感器曝光时间是影响星敏感器星点定位精度的因素之一.建立星敏感器星点像移模型和CCD噪声影响模型,分析了星点质心定位精度与曝光时间的关系,并以CCD47-20为例,对星敏感器的曝光时间进行了优化.结果表明:对于6.5等星,当星点光斑像移速度为4.67 pixels/s时,采用5×5窗口的亚像元质心算法,亚像元质心算法精度随曝光时间的延长而降低,CCD噪声对星点质心定位精度的影响随曝光时间的增加而减小;星敏感器的最佳曝光时间为200 ms,此时的星点质心定位精度优于1/50 pixel.     

自适应系统中哈特曼波前传感器光斑质心的最佳标定位置

自适应光学系统中采用CCD作为哈特曼波前传感器的光斑质心位置探测器时,由于光斑的高斯宽度较小会带来大采样误差.针对该问题,本文详细分析了采样误差形成的原因,建立了采样误差、位移敏感度和开环动态范围与光斑高斯宽度、光斑位置以及子孔径大小的数学模型,提出标定时光斑质心的最佳位置是子孔径中心四像素的中心.因为在该位置处,CCD的质心探测具有闭环时采样误差为0,位移敏感度最大,且开环时动态范围最大的特点,为哈特曼波前传感器的标定方法的研究提供了理论依据.     

抑制微光波前传感器随机噪声的方法研究

在自适应光学系统微光波前传感器中采用像增强器后，高帧频CCD输出的图像中会产生严重的随机噪声，影响光斑质心计算精度，从而使自适应光学系统波前探测精度降低。本文根据微光波前传感器中CCD输出图像的特点对中值滤波，均值滤波，自相关，延时相关等多种方法进行了仿真和实验比较，并提出了一系列评价方法。研究表明延时相关算法是最佳选择。     

激光偏角测量技术研究

介绍一种采用激光测量反射镜偏角的方法 ,它适合于光学系统装配时的测量。采用 CCD细分技术对成象光斑质心进行提取 ,提高了偏角测量精度 ,在 1 .2 5°的测量范围内 ,可以达到± 3″的测量精度     

数字同轴和数字离轴全息系统分析

利用最高空间频率分析法,通过逐点分析记录在 CCD 上的空间频率信息,研究了物体可允许记录的最大横向尺寸、最小记录距离、全息图的信息量、空间分辨力、再现像的横向分辨力、轴向分辨力及散斑大小,并得到了数学表达式。理论分析和实验结果表明,数字同轴全息系统放宽了对 CCD 分辨力的要求,有较高的分辨力,较低的散斑噪声、灵活、简单的系统结构及较高的 CCD 空间带宽利用率,在增强系统性能方面要优于数字离轴全息系统。这一研究为数字全息系统的设计和操作提供了一定的理论和实验指导。     

光重心法在光纤位置检测中的精度研究与应用

为了确保LAMOST(大天区面积多目标光纤光谱天文望远镜)系统准确运转,需要对其焦面板上光纤的位置进行检测.本文即从实际应用的角度出发,阐述了光重心法在LAMOST光纤位置检测中的精度问题.在理论分析的基础上结合实验,具体研究光斑尺寸、相机光圈、光纤端面的发光强度等检测条件,并详细分析了它们与光重心法自身精度的关系.另外,还揭示了因光强变化而产生的"重心偏移"现象.最终,依据实验结果,为实际检测提供了一个最佳的测量条件.     

Position and displacement sensing with shack-hartmann wave-front sensors

The use of a Shack-Hartmann wave-front sensor as a position-sensing device is proposed and demonstrated. The coordinates of a pointlike object are determined from the modal Zernike coefficients of the wave fronts emitted by the object and detected by the sensor. The position of the luminous centroid of a moderately extended incoherent flat object can also be measured with this device. Experimental results with off-the-shelf CCD cameras and conventional relay optics as well as inexpensive diffractive microlens arrays show that axial positioning accuracies of 74 mum rms at 300 mm and angular accuracies of 4.3 murad rms can easily be achieved.     

Fabry-Perot CCD annular-summing spectroscopy: study and implementation for aeronomy applications

The technique of Fabry-Perot CCD annular-summing spectroscopy, with particular emphasis on applications in aeronomy, is discussed. Parameter choices for optimizing performance by the use of a standard format CCD array are detailed. Spectral calibration methods, techniques for determining the ring pattern center, and effects imposed by limited radial resolution caused by superpixel size, variable by on-chip binning, are demonstrated. The technique is carefully evaluated experimentally relative to the conventional scanning Fabry-Perot that uses a photomultiplier detector. We evaluate three extreme examples typical of aeronomical spectroscopy using calculated signal-to-noise ratios. Predicted sensitivity gains of 10-30 are typical. Of the cases considered, the largest savings in integration time are estimated for the day sky thermospheric O(1)D case, in which the bright sky background dominates the CCD read noise. For profile measurements of faint night sky emission lines, such as exospheric hydrogen Balmer-α, long integration times are required to achieve useful signal-to-noise ratios. In such cases, CCD read noise is largely overcome. Predictions of a factor of 10-15 savings in integration time for night sky Balmer-α observations are supported by field tests. Bright, isolated night sky lines such as thermospheric O(1)D require shorter integration times, and more modest gains dependent on signal level are predicted. For such cases it appears from estimate results that the Fabry-Perot CCD annular-summing technique with a conventional rectangular format may be outperformed by a factor of 2-5 by special CCD formats or by unusual optical coupling configurations that reduce the importance of read noise, based on the ideal transmission for any additional optics used in these configurations.     

A dual pixel-type array for imaging and motion centroid localization

An imager chip has been designed, fabricated, and tested having two unique pixel types interleaved on the same array. The dual-pixel design enables optimization for two separate tasks. One type of pixel is an active pixel sensor (APS), which is used to produce a low-noise image. The other type is a custom-designed pixel optimized for computing the centroid of a moving object in the scene. The APS array is 120 columns /spl times/36 rows, with a pixel size of 14.7/spl times/14.7 /spl mu/m. The centroid array has 60 columns and 36 rows, with a larger pixel size of 29.4/spl times/29.4 /spl mu/m. The chip was fabricated using standard scalable rules on a 0.5 /spl mu/m 1P3M CMOS process. APS images were taken at a frame rate of 30 fps-8300 fps and centroid data was taken at a rate of 180-3580 (x,y) coordinates per second. The chip consumed 2.6 mW.     

CCD目标灰度质心算法的动态误差分析

针对传统静态误差分析方法忽略目标运动对测量影响的不足,本文在分析运动对目标形状影响的基础上建立了灰度质心算法误差与灰度噪声、动态目标尺寸的数学模型,该模型表明当曝光时间内目标移动量远小于目标静态尺寸时,动态误差与静态误差接近;而当目标移动量与目标静态尺寸的比值大于6%时,灰度质心算法动态测量误差方差将比静态测量误差方差...     

CCD信号处理技术及其在长度测量中的应用

论述线阵ＣＣＤ信号处理技术及其在几何尺寸测量中的应用,对线阵ＣＣＤ的特点和信号的处理方法给予较为详细的论述。特别是对ＣＣＤ信号的二值化问题,提出实现方法,结合这一技术在马钢初轧厂连轧坯测长和配尺应用的实例,进一步论述这一技术在大尺寸测量中的具体应用。     

一种新型的基于LQI的加权质心定位算法

提出一种基于链路质量指示(LQI)的测距技术与加权质心定位算法相结合的新型定位算法。经过数据分析比较,验证了LQI要比接收信号强度指示(RSSI)更稳定、抗干扰能力更强。采用高斯滤波模型对实验测量值进行处理,增加了数据的准确性。建立基于RSSI和LQI的对数拟合测距公式,利用质心定位算法进行仿真实验,结果表明:采用基于LQI测距的加权质心算法定位,其定位精度有了较大提高,达到了较为理想的定位效果。     

基于CCD器件特征的图像噪声消除

根据CCD器件的工作原理,对CCD图像的噪声组成进行分析,建立了较为完整的泊松-高斯噪声模型,并根据实际的应用情况进行合理的简化,取得了良好的应用效果。采用最大相似估计法对CCD图像的成像模糊进行相应的补偿,并完成了对模型的简化,最后给出了实例。     

卷边槽钢偏心受压构件极限承载力的直接强度计算方法研究

直接强度法是确定薄壁构件承载力非常有效的一种新方法。利用ANSYS分析确定了卷边槽钢截面的有效形心偏移量,并建立了有效形心偏移的计算公式。在此基础上,提出了对称轴平面内偏心受压状态下,卷边槽钢简支构件在弯矩作用平面内的稳定承载力直接强度计算方法。方法中考虑了局部与整体以及畸变与整体的相关屈曲,并考虑了截面有效形心的偏移。与试验及有限元分析结果的对比表明,用该方法确定卷边槽钢截面有效形心的偏移及偏压构件的极限承载力是可行的。     

Use of artificial neural networks for Hartmann-sensor lenslet centroid estimation

For adaptive optical systems to compensate for atmospheric-turbulence effects, the wave-front perturbation must be measured with a wave-front sensor (WFS). A Hartmann WFS typically divides the optical aperture into subapertures and then measures the slope of the wave front within each subaperture. Hartmann WFS slope measurements are based on estimating the location of the centroid of the image that is formed from a guide star within each subaperture. Conventional techniques for centroid estimation involve the use of a linear estimator and conversion tables. Neural networks provide nonlinear solutions to this problem. We address the use of neural networks for estimating the location of the centroid from the subaperture image. We find that neural networks provide more accurate estimates over a larger dynamic range and with less variance than do the conventional linear centroid estimator.