轨道末期星载相机侧摆成像匹配分析与实验

通过分析卫星轨道末期星载TDI CCD相机成像面临的数据读出频率过大、像移失配严重等瓶颈问题, 提出了轨道末期卫星侧摆成像匹配方案. 依据轨道衰减高度, 设计侧摆成像匹配模型, 计算出轨道高度与匹配成像侧摆角度之间的变化关系, 对侧摆成像时的像移速度矢量、偏流角度、成像畸变等进行了定量的可行性分析, 并利用蒙特卡洛方法分析了满足侧摆成像的卫星姿态指向精度和稳定度. 利用基于小型三轴气浮台的小卫星姿态控制系统和TDI CCD相机成像系统进行仿真试验, 结果表明, 仿真图像的MTF函数和互相关相似性测度均在0.85以上, 侧摆成像匹配方案能较好地满足轨道末期成像需求.     

视觉检测中椭圆中心成像畸变误差模型研究

针对在三维视觉检测应用中,空间椭圆的中心经摄像机针孔成像后存在畸变误差的问题进行了研究.基于透视投影变换和空间解析几何理论,建立了在摄像机的像平面上该畸变误差的数学模型,从而为圆孔(椭圆孔)或圆柱(椭圆柱)类工件中心位置的视觉检测、结构光三维视觉检测应用以及视觉检测中的CCD摄像机内部参数标定等问题的解决提供了一个有效的理论依据,具有一定的理论意义和工程应用价值.      

Chandra imaging spectroscopy of the central region of AWM7

We report on the results of Chandra observations of the galaxy cluster AWM7. The ACIS image reveals new substructures with a spatial extent of more than 8″ (4 kpc at AWM7) near the cD galaxy center, represented by a hard sub-peak and a soft peak. These substructures suggest that a dynamical process related to the formation of the cD galaxy is now taking place. Inside the cluster core within a radius of 2′, annular spectra with every 10″ step are fitted well by single temperature models. The temperature gradually drops from 4.2 keV at a radius of 60 kpc (2′) to 1.8 keV at the cluster center. The radial abundance profile shows a gradient with a peak metallicity of 1.5 solar at a radius of about 15″ (7 kpc). A two-dimensional map shows two high metallicity blob-like regions, which may be the gas expelled from the cD galaxy.     

基于单视点调节相机模型的水下图像三维重构

水下图像成像过程中,每个场景点所对应的光线在传播过程中均经过多种折射率不同的介质,因此水下图像会产生折射变形,导致传统基于单视点相机模型的水下图像三维重构方法精度极大降低.在理论分析一个新的单视点调节模型对水下图像折射变形的补偿能力的基础上,提出一种高效、自动的水下图像三维重构及其非线性优化方法.为了验证该方法的性能,利用合成数据和真实图像对其进行测试,并依据重构有效性、重构误差等定量指标考察分析了实验结果.实验结果表明,提出的多视图水下三维重构方法可有效补偿水下场景成像空间变形,进而显著提高传统基于单视点相机模型的水下三维重构质量.     

全方向长期伴飞卫星集群轨道设计与仿真

主要研究在J2摄动的影响下,在中心卫星周围全方向上部署长期相对有界伴飞卫星的轨道设计方法。首先,利用J2不变的条件,由已知中心卫星轨道根数建立伴飞卫星的半长轴、偏心率及轨道倾角之间关系。然后,通过对伴飞卫星和中心卫星之间初始相对位置及轨道根数之间关系的分析,得到伴飞卫星的全部初始轨道根数,使其能够部署到中心卫星周围的任意方向上,从而能实现卫星集群在中心卫星的周围全方向长期有界伴飞。最后,通过轨道仿真验证了该方法的有效性。     

“嫦娥三号”探测器软着陆自主导航与制导技术

\"嫦娥三号\"探测器首次实现了我国航天器在地外天体软着陆,制导导航与控制技术是软着陆任务成功的关键。针对高安全和高可靠软着陆任务的要求,设计了包含接力避障的软着陆飞行程序,提出了单波束分时修正与多波束融合修正的自主导航方法和自适应动力显式制导、无迭代多项式粗避障制导以及内外环结合的精避障制导等方法。实际在轨飞行结果表明,导航算法提供了高精度的状态估计,制导算法实现了高精度状态控制和有效避障机动,确保了软着陆落月的安全性和可靠性。     

Near-infrared study of open clusters Teutsch 10 and Teutsch 25

The astrophysical parameters have been estimated for two unstudied open star clusters Teutsch 10 and Teutsch 25 using the Two Micron All Sky Survey ($2\mathit{MASS}$) database. Radius is estimated as 4.5 arcmin for both clusters using radial density profiles. We have estimated proper motion values in both RA and DEC directions as $2.28\pm 0.3$ and $-0.38\pm 0.11$?mas?yr^?1 for Teutsch 10 and $0.48\pm 0.3$ and $3.35\pm 0.16$?mas?yr^?1 for Teutsch 25 using $\mathit{PPMXL}$¹ catalog. By estimating the stellar membership probabilities, we have identified 30 and 28 most likely members for Teutsch 10 and Teutsch 25 respectively. We have estimated the reddening as $E(B-V)=0.96\pm 0.3$?mag for Teutsch 10 and $0.58\pm 0.2$?mag for Teutsch 25, while the corresponding distances are $2.4\pm 0.2$ and $1.9\pm 0.1$?kpc. Ages of $70\pm 10$?Myr for Teutsch 10 and $900\pm 100$?Myr for Teutsch 25 are estimated using the theoretical isochrones of metallicity Z?=?0.019. The mass function slopes are derived as $1.23\pm 0.30$ and $1.09\pm 0.35$ for Teutsch 10 and Teutsch 25 respectively. Estimated mass function slope for both the clusters are close to the Salpeter value ($x=1.35$) within the errors. Estimated values of dynamical relaxation time are found to be less than cluster’s age for these objects. This concludes that both objects are dynamically relaxed. The possible reason for relaxation may be due to dynamical evolution or imprint of star formation or both.     

高精度VLBI技术在深空探测中的应用

介绍了适合单探测器测定轨的高精度VLBI技术和适合多探测器测定位的同波束VLBI技术的研究进展。利用\"嫦娥3号\"着陆器的ΔDOR型VLBI观测,得到了误差0.67ns的VLBI群时延数据。利用\"嫦娥3号\"着陆器和月球车的同波束VLBI观测,得到了随机误差0.3ps的差分相时延数据,以数厘米的灵敏度监测出月球车的移动、转弯等动作,并把月球车的相对定位精度提高至1m。针对深空探测,提出了使VLBI时延测量精度进一步提高所需要开展的部分研究内容。     

X-ray and radio observations of the galaxy cluster 3C 129

The galaxy cluster 3C 129 contains two radio galaxies, the prototypical head tail radio galaxy 3C 129 and the weaker radio galaxy 3C 129.1. The tail of the first radio galaxy extends over more than 15′ across the sky. In this paper, we report on Chandra spectroscopy observations of the galaxy cluster, complemented by new and archival radio data taken with the Very Large Array (VLA) at 0.33, 1.4, 5, and 8 GHz and by HI-observations performed with the dominion radio astrophysical observatory (DRAO). We describe the Chandra results on the properties of the Intra-Cluster Medium (ICM) and discuss extended X-ray emission detected from the host galaxy of the radio galaxy 3C 129.1 and from the inner jet of the radio galaxy 3C 129. Finally, we report on the results of an ICM/radio plasma pressure balance study along the tail of the radio galaxy 3C 129.