多频数据组合在周跳探测和修复上的应用

利用模拟的L5观测数据，结合传统的伪距／载波组合法，对周跳的探测与修复进行了实例计算，并与双频组合观测值的周跳探测方法进行了比较。结果证明，不管对大周跳还是小周跳，该方法均能在单历元间准确地探测出各个频率上发生的周跳，较之双频组合观测值的探测方法具有更大的优越性。     

基于k阶Voronoi多边形划分的k阶数据场拟合

讨论了k阶Voronoi图的离散点集的生成算法，挖掘了k阶Voronoi图的性质并加以证明；参照k阶Voronoi图的定义提出了k阶空间数据场的定义，并结合参考点利用其影响因子给出了低阶空间数据场的拟合函数通式；利用k阶Voronoi图对平面空间的平面区域最近邻近划分实现了对空间数据场的分割，从而将大量参考点集数据场化解为多个单元数据场的低阶拟舍，有效地降低了数据场拟舍的难度；提出了合并拟合和叠加拟合策略，实现了将单元数据场综合为完整的空间数据场。     

数字地图合并的平差原理与方法

提出了一种基于最小二乘平差的数字地图合并方法，采用平差原理以求得实体调整合并后的空间位置。实验表明，与其他方法相比，该方法具有较高的精度，且较好地保持了原有实体的特征。     

空间数据模糊聚类的有效性评价

基于模糊划分中存在的分类不确定性因素和空间数据的空间位置特征,提出了一种新的空间数据模糊聚类有效性函数。实验结果表明,这种新的有效性函数能够对模糊聚类结果的有效性进行正确的评价,特别是对于空间数据模糊聚类有效性评价,其分类效果较理想,同其他有效性指标相比,能得到较优的分类数。     

基于数字地价模型的地价监测点配置研究

从数字地价模型的建立、格网数字地价模型向TIN转化、TIN节点与宗地图层叠加拟合完成地价监测点的定位配置、结合市场比较法的监测点地价更新、TIN数字地价模型更新等几个方面详细阐述了数字地价模型运用于地价监测点配置的具体方法。并将这一配置模式与以标准宗地为载体的配置模式进行了比较分析。     

基于决策树的高光谱数据特征选择及其对分类结果的影响分析

本文利用OM IS高光谱数据,研究了决策树算法（Decision Tree,DT）特征选择的特点以及特征选择对决策树分类结果的影响。设计了三种特征选择方法：SEP,MDLM和RELIEF,将它们与DT特征选择的结果以及特征选择后的分类精度（考虑了三种分类器：最大似然法、后向传播神经网络、最邻近法）进行对比,并分析了这三种特征选择方法对决策树结构和分类精度的影响。结果显示,DT是一种比较好的特征选择方法;经过特征选择后再生成的决策树比直接生成的决策树,用到更少的特征（平均减少了43.36%）、有更多的节点（平均增加了18.61%）和更高的分类精度（平均提高了0.35%）,当样本数量少时,分类精度的提高幅度最大,而树的大小却基本没有增加。     

武汉台形变观测与降雨参数之间的定量分析与研究

基于“前兆台网(站)观测数据跟踪分析平台”,对武汉台形变观测资料进行了系统分析,提取出观测曲线受降雨干扰影响的事件,采用降雨总量、初始驱动降雨量和瞬时降雨量最大值等降雨参数对降雨干扰事件进行统计分析。结果表明:降雨总量达40 mm、初始驱动降雨量为0.3 mm或瞬时降雨量最大值达0.6 mm时,DSQ型水管倾斜仪易受降雨干扰;SSY型铟瓦棒伸缩仪当降雨总量超60 mm或瞬时降雨量最大值大于0.5 mm时易受降雨干扰;VS型垂直摆倾斜仪受降雨干扰与降雨总量、初始驱动降雨量和瞬时降雨量最大值无显著相关关系;降雨总量对形变仪器观测物理量的影响基本呈现线性;而形变仪器观测物理量与初始驱动降雨量、瞬时降雨量最大值无显著相关关系。认为武汉台形变观测受降雨影响主要来自降雨渗透影响和周边水体荷载变化影响两个方面。     

DO WE NEED TO MODEL PLATES AT ALL?

The historical method of obtaining equatorial coordinates for stars observed via astronomical photography has been to convert the measured coordinates to equatorial coordinates with the aid of a plate model which corrects for a variety of effects. However, we now have at our disposal novel smoothing techniques, of considerable generality, which in conjunction with modern star catalogues can reproduce the essence of the plate model while dramatically minimizing both the fortuitous and systematic errors of observation. In this paper we demonstrate that, with this technique and extant catalogues, one can obtain, with at least the same precision and better accuracy, the information necessary to transform the measured coordinates successfully into standard coordinates by a process that involves no sophisticated model for the plate. Using external checks we estimate the increase in accuracy to be of the order of 25 per cent.     

An optimal extraction algorithm for imaging photometry

This paper is primarily an investigation of whether the 'optimal extraction' techniques used in CCD spectroscopy can be applied to imaging photometry. It is found that using such techniques provides a gain of around 10 per cent in signal-to-noise ratio over normal aperture photometry. Formally, it is shown to be equivalent to profile fitting, but offers advantages of robust error estimation, freedom from bias introduced by mis-estimating the point spread function, and convenience. In addition some other techniques are presented, which can be applied to profile fitting, aperture photometry and the 'optimal' photometry. Code implementing these algorithms is available at http://www.astro.keele.ac.uk/~timn/.     

Non-parametric reconstruction of distribution functions from observed galactic discs

A general inversion technique for the recovery of the underlying distribution function for observed galactic discs is presented and illustrated. Under the assumption that these discs are axisymmetric and thin, the proposed method yields a unique distribution compatible with all the observables available. The derivation may be carried out from the measurement of the azimuthal velocity distribution arising from positioning the slit of a spectrograph along the major axis of the galaxy. More generally, it may account for the simultaneous measurements of velocity distributions corresponding to slits presenting arbitrary orientations with respect to the major axis. The approach is non-parametric, i.e. it does not rely on a particular algebraic model for the distribution function. Special care is taken to account for the fraction of counter-rotating stars, which strongly affects the stability of the disc. An optimization algorithm is devised — generalizing the work of Skilling &38; Bryan — to carry this truly two-dimensional ill-conditioned inversion efficiently. The performance of the overall inversion technique with respect to the noise level and truncation in the data set is investigated with simulated data. Reliable results are obtained up to a mean signal-to-noise ratio of 5, and when measurements are available up to 4  R _e. A discussion of the residual biases involved in non-parametric inversions is presented. The prospects of application of the algorithm to observed galaxies and other inversion problems are discussed.