短波红外用于白天卫星探测的研究

从白天天空背景、卫星光学特性及红外波段在大气中的传输特性三方面分析了白天卫星探测的可行性。在此基础上,采用光谱滤波的方法,利用红外焦平面阵列(IRFPA),在短波红外波段进行了卫星跟踪与测量。理论分析和白天的测星实验表明,用短波红外波段能够实现白天卫星的跟踪与测量;通过与已知星等的G型光谱类型恒星测量值的比对得到了目标卫星的星等为6.34,给出了探测系统的跟踪误差。     

基于恒星观测的静止轨道成像仪指向偏差在轨修正

在建立基于恒星观测的成像仪指向偏差在轨修正模型的基础上 ,提出了模型中若干关键参数(包括最低观测星等、待观测恒星及成像仪凝视观测化置等)的选取方法.同时,开展了数字延迟积分技术,系统点源扩展函数等对指向偏差测量精度的影响分析,提出了指向偏差确定精度达1"的在轨修正方案,并利用GOES-9卫星成像仪实际恒星观测数据进行了部分定量验证.研究成果将为后续风云四号卫星成像仪高精度指向偏差在轨修正的业务模式设计和工程实施,提供重要的技术参考.     

低仰角蒙气差精密修正的新方法

由于蒙气差随着大气密度、温度和压力等条件的变化而变化,为降低蒙气差对光电测量设备测量精度的影响，提出了精密恒星回扫的新方法。在标准大气条件下，通过理论计算得到的蒙气差与实际测量值存在偏差，采用精密恒星星库，引导测量设备对观测目标附近的恒星进行事后回扫测量，对回扫测量数据进行拟合可以得到蒙气差的修正量。分析了恒星回扫方法中影响修正精度的轴系、编码器等因素，通过外场实验，在大气湍流变化均匀的情况下，采用该方法对20°仰角以下星体进行观测，测量精度可以达到1″。     

基于视频遥感卫星的空间目标光度测量

基于"吉林一号"视频系列卫星开展空间目标光度测量试验,阐述了视频星对空间目标成像以及光度反演原理,利用相机探测器输出图像的灰度值反演计算目标光度学特征。根据误差传递原理分析了辐射定标系数偏差和目标图像噪声对反演精度的影响,并以恒星作为标准辐射源对反演精度进行验证,结果表明恒星类点目标光度反演误差小于0.15Mv。列举了空间目标拍摄及反演结果样例,并对视频星观测试验结果进行了统计和说明,得到视频星的极限探测距离、捕获概率以及观测效能,分析结果表明视频星的灵活成像模式可较好地适用于空间目标观测任务。     

利用恒星辐射测量整层大气透过率的多目标星定标

 介绍了整层大气透过率测量仪及其测量原理和Langley-Plot定标方法,提出了基于恒星整层大气透过率仪测量大气透过率的多目标星定标方法,并分别进行了K,A光谱类型恒星定标试验,得到了基于K,A两种光谱类型恒星辐射的定标值。对多目标星定标方法与单颗恒星的Langley-Plot定标方法进行了对比实验,验证了多目标星定标方法的合理性与准确性。当实时测量同类型的恒星辐射整层大气透过率时,就可以根据对应的定标参数进行测量研究。     

用于在线E-FRET定量成像的自动背景识别与数据筛选

因灵敏性高、无损伤和测量速度快等特性,基于3-cube的荧光能量共振转移(E-FRET)显微成像术是目前最流行的活细胞定量FRET成像技术。为了实现活细胞在线实时FRET定量成像,首先提出了一种细胞图像背景自动识别与图像阈值设定的方法:逐像素统计灰度值出现的次数,第1个峰值处的灰度值确定为背景值;将背景值的β(经验常数)倍设为阈值,将扣除背景的供体激发供体探测通道图像和受体激发受体探测通道图像再次扣除阈值,负值置零后进行逻辑与运算制作用于数据筛选的布尔逻辑模板,并将其用于FRET效率和供受体浓度比的数据筛选。利用所提出的方法对转染了不同FRET质粒的细胞进行活细胞在线动态定量E-FRET成像,得到了与期望值一致的测量结果。     

适用于星敏感器的导航星表构造算法研究

导航星表的性能对于星敏感器姿态测量的实时性及精度至关重要。为了克服星等过滤算法的缺点,将支持向量机应用于导航星表的构造算法中。将基本星表中的恒星视为待分类的数据点,选取抽样视场中最亮的k颗星作为导航星,而非导航星的数量由抽样视场中恒星的密度决定。为了获得具有最大推广能力的抽样数据,采用了一种球面螺旋形算法生成抽样视场视轴指向,使用抽样数据构建最优导航星分类器,应用最优导航星分类器对基本星表中每一颗恒星进行分类判决。仿真结果表明,在满足8°×8°视场中至少出现3颗导航星的条件下,该算法生成的导航星表导航星总数约为星等过滤算法的33%,比传统支持向量机算法减少了7.8%,其标准差仅为星等过滤算法的21%,这表明本算法在导航星表容量及导航星分布均匀性方面大大优于星等过滤算法和传统支持向量机算法。     

地基光度测量方式对比

介绍了地基测量空间目标光度的两种方式。首先介绍了系统组成及对比测量原理,然后基于工程角度分析提出了宽谱段测量和滤光片测量两种方式,并给出了两种测量方式的误差分析。若G型恒星及空间目标在同一视场可选择宽谱段测量方式,若途经天区G型定标星较少,可以选择滤光片测量方式。外场实验验证表明,宽谱段测量方式信噪比较高,可探测的极限星等为16等星,在天气条件较好的情况下测量精度在0.15星等左右,而滤光片测量方式由于探测到的能量较少,在相同信噪比下可探测极限星等为14等星,天气变化较小条件下测量精度在0.02星等左右,两种测量方式误差相当,但宽谱段测量方式定标恒星数量增加2.4倍,便于数据处理与计算。     

高精度数字图像相关测量系统及其技术研究

研制双CCD长距显微数字图像相关测量系统,它融合光电子、数字图像相关方法和散斑技术于一体,具有非接触式、高精度、宽量程、准实时、测试方法简便等优点,它可用于材料力学性能(特别是柔性高分子材料力学性能)测量、低膨胀系数新型材料线胀系数等的测量。若将其用于应变测量,灵敏度优于1με,而传统数字图像相关方法测量应变的理论灵敏度为20με。利用列阵光学元件解决了0.05 mm高衬比度微小标记的方便设置;提出消除了数字图像灰度噪声的时间平均法,使相关测量精度稳定地达到0.01 pixel。还给出金属材料拉应变的测量结果,实验结果与经典理论值相当接近。此外,还阐述数字图像相关测量技术是一种超光学系统衍射极限分辨力的测量技术。     

光度测量图像智能阈值降噪方法

为了提高光度测量精度,通过对光度测量过程中的入射散粒噪声、天光散粒噪声、暗电流散粒噪声、读出噪声的来源进行详细分析,有针对性地描述了降低各种噪声的方法,并针对暗电流散粒噪声与读出噪声及其他噪声残留提出了一种基于灰度直方图统计的智能阈值降噪方法;大幅消除了噪声对测量结果的影响,通过对恒星测光图像降噪前后光度计算结果的精度比对发现,采用这种方法将光度测量精度从原来的0.314 Mv提高到0.092 4 Mv,精度改善效果明显,并且解决了使用CCD测量光度结果不稳定的问题,具有较好的应用价值。     

Search for carbon stars and DZ white dwarfs in SDSS spectra survey through machine learning

Carbon stars and DZ white dwarfs are two types of rare objects in the Galaxy.In this paper,we have applied the label propagation algorithm to search for these two types of stars from Data Release Eight(DR8)of the Sloan Digital Sky Survey(SDSS),which is verified to be efcient by calculating precision and recall.From nearly two million spectra including stars,galaxies and QSOs,we have found 260 new carbon stars in which 96 stars have been identified as dwarfs and 7 identified as giants,and 11 composition spectrum systems(each of them consists of a white dwarf and a carbon star).Similarly,using the label propagation method,we have obtained 29 new DZ white dwarfs from SDSS DR8.Compared with PCA reconstructed spectra,the 29 findings are typical DZ white dwarfs.We have also investigated their proper motions by comparing them with proper motion distribution of 9,374 white dwarfs,and found that they satisfy the current observed white dwarfs by SDSS generally have large proper motions.In addition,we have estimated their efective temperatures by fitting the polynomial relationship between efective temperature and g-r color of known DZ white dwarfs,and found 12 of the 29 new DZ white dwarfs are cool,in which nine are between 6,000 K and 6,600 K,and three are below 6,000 K.     

Applications of two-way satellite time and frequency transfer in the BeiDou navigation satellite system

A two-way satellite time and frequency transfer(TWSTFT) device equipped in the BeiDou navigation satellite system(BDS)can calculate clock error between satellite and ground master clock. TWSTFT is a real-time method with high accuracy because most system errors such as orbital error, station position error, and tropospheric and ionospheric delay error can be eliminated by calculating the two-way pseudorange difference. Another method, the multi-satellite precision orbit determination(MPOD)method, can be applied to estimate satellite clock errors. By comparison with MPOD clock estimations, this paper discusses the applications of the BDS TWSTFT clock observations in satellite clock measurement, satellite clock prediction, navigation system time monitor, and satellite clock performance assessment in orbit. The results show that with TWSTFT clock observations, the accuracy of satellite clock prediction is higher than MPOD. Five continuous weeks of comparisons with three international GNSS Service(IGS) analysis centers(ACs) show that the reference time difference between BeiDou time(BDT) and golbal positoning system(GPS) time(GPST) realized IGS ACs is in the tens of nanoseconds. Applying the TWSTFT clock error observations may obtain more accurate satellite clock performance evaluation in the 104 s interval because the accuracy of the MPOD clock estimation is not sufficiently high. By comparing the BDS and GPS satellite clock performance, we found that the BDS clock stability at the 103 s interval is approximately 10.12, which is similar to the GPS IIR.     

基于天顶观测的光学系统精确标定方法

针对光学系统在实际应用中与载体坐标系协调的问题,将光学系统基准面放置于站心地平坐标系水平面上并摄取星图,对星图处理获取星像坐标,应用天体自动辨识技术和恒星视位置计算技术得到对应天体的赤道坐标,以天顶点为原点建立天球切平面基准坐标系,把星体赤道坐标转化为所对应的基准坐标,利用天顶点切平面与站心地平坐标系的对应关系,将天体基准坐标转换为站心像平面坐标,建立星体站心像平面坐标与星图像平面坐标的标定方程,解算光学系统综合标定参数。实验结果表明:标定精度达到角秒量级,实现光学系统像平面坐标系到载体坐标系的高精度转换。     

自发喇曼成像法在线测量流场组分浓度（Ⅱ）

介绍了利用自发Raman散射光谱测量低压气流组分绝对浓度的方法，在流动状态下得到了不同压力的自发喇曼散射光谱，检测最低压力为133Pa；对于含N2氧气流在已知N2浓度时实时标定检测了O2的绝对浓度，测量误差小于8％。，     

High-latitude thermospheric winds: Satellite data and model calculations

The thermospheric crosswind velocities at an altitude of 400 km measured by an accelerometer on board of the CHAMP satellite are compared with the results of model calculations performed using the Upper Atmosphere Model (UAM). The results of measurements averaged over the year in 2003 reveal a two-vortex structure of high-latitude winds corresponding to magnetospheric-ionospheric convection of ions in the F2 ionosphere region. A similar picture with similar speed values was obtained in model calculations. A comparison of the crosswind speed obtained in individual measurements on October 28, 2003 with the corresponding model values revealed close agreement between them in some flights and differences in others. Taking into account the dependence of convection electric field on the B _y component of interplanetary magnetic field sometimes improved agreement between thermospheric crosswind speeds obtained in model calculations and measured using the satellite.     

Accurate measurement of translational diffusion coefficients: a practical method to account for nonlinear gradients

For NMR probes equipped with pulsed field gradient coils, which are not optimized for gradient linearity, the precision and accuracy of experimentally measured translational diffusion coefficients are limited by the linearity of the gradient pulses over the sample volume. This study shows that the accuracy and precision of measured diffusion coefficients by the Stejskal--Tanner spin-echo pulsed field gradient experiment can be significantly improved by mapping the gradient z-profile and by using the mapped calibration parameters in the data analysis. For practical applications the gradient distribution may be approximated by a truncated linear distribution defined by minimum and maximum values of the gradient. By including the truncated linear gradient distribution function in the Stejskal--Tanner equation, the systematic deviation between the fitted curve and the experimental attenuation curve decreases by an order of magnitude. The gradient distribution may be calibrated using an intense NMR signal from a sample with a known diffusion coefficient. The diffusion coefficient of an unknown sample may then be determined from a two-parameter fit, using the known gradient distribution function.     

Spectrometric method for detecting exoplanets as another test to verify the invariance of the velocity of light

This paper analyzes the hypothetical influence of variability in the velocity of light associated with the motion parameters of a source on the results of spectral measurements of stars within an exoplanet search program. The accelerations of stars relative to the barycenter of the host star-planets system are taken into account. The dependence of the velocity of light on the barycentric radial velocity and the radial acceleration components of the barycentric stars is shown to lead to a substantial increase (up to an order of magnitude) in the semimajor axes of the orbits of detected candidate extrasolar planets. Consequently, a correct comparison of the spectral method with other well-known modern methods for detecting extrasolar planets allows one to consider the results obtained in this paper as a reliable test for the invariance of the velocity of light.     

小型星模拟器系统的设计研究

基于超小型P13XM015型TFT-LCD技术的小型星模拟器的工作原理,及其在工程应用中整个系统的设计、制造、加工、调试和检测技术,提出对星间间距采用软件修正以及先分别测量再组合修正的方法,对星等采用使用相适应的仪器星等的方法。采用模块化方法设计了小型星模拟器系统的光学系统准直物镜、模拟星库的编制、坐标转换、位置解算、系统控制软件等。在实验室实现了整个系统的组装,搭建了控制和测试平台,并给出了实验结果。实验结果表明:本系统的星库精度及星位置解算误差12,角分辨率误差23.43。