ADS 80数码航摄仪L0级影像后处理试验

介绍了三线阵数码航摄仪ADS 80,探讨了其Level 0级影像的后处理技术,分析了不同软件在相同地面分辨率下不同地面控制条件下的后处理精度。得出的结论是控制点分布、数量、位置和航摄影像地面分辨率对ADS 80相机L0级影像空三解算和生成的L1级影像精度影响较大;在充分考虑以上因素的情况下,ADS 80相机在获取的航摄影像地面分辨率低于成图比例尺要求时仍能得到较高的校正精度。     

模糊Hough变换算法在城市道路提取中的应用

采用形态学细化算法,将二值化影像形态学细化之后再进行峰值检测,有效地去除了虚假峰值,提高了道路提取精度及计算效率,为此,利用用模糊Hough变换算法提取遥感影像中的城市道路。试验表明,其方法在计算效率、提取精度以及内存占用方面具有明显优势。     

中波红外图像条纹处理方法

卫星搭载的有效载荷在进行在轨对地观测过程中,受仪器本身特性和地球固有特性因素的影响,在图像上会产生多种观测失准和干扰现象。如图像旋转现象,蝴蝶结效应以及探元非均匀性条纹现象等。针对这类可以预见到的冗余和条纹,对仪器设计优化以及借助卫星星历轨道等辅助数据和成熟的图像处理算法可以对其实现有效地恢复。仪器在轨运行期间新引入的周期性或非周期性干扰,则需综合运用多种数据来源和关于干扰产生原理的先验知识,并结合图像处理手段实现图像恢复,同时保存原有辐射信息的真实性,为定量研究提供高质量可靠的数据准备。本研究针对某卫星中波红外图像干扰条纹,利用星上定标数据,并通过条纹现象分析和产生机理分析,探索了一种新的基于空域信号补偿原理的图像干扰条纹处理算法,通过大量图像数据处理实践证明,该算法对图像质量改善明显,且在动态范围和辐射信息保存方面优于传统频域滤波算法。     

几何失真对SAR图像匹配的影响及校正方法分析

合成孔径雷达SAR用于图像匹配导航系统,可大大提高导航精度。然而地形起伏和大气干扰等因素使得SAR实时图存在几何失真,降低了匹配性能。通过对SAR实时图几何失真成因分析,提出了一种二维可分离的几何校正方法,并得出方位向几何失真可跟随成像处理预先校正,图像后处理只需校正距离向。利用数字高程模型DEM和正射图模拟得到了3幅具有不同地形特征的SAR实时图,并分别利用3种几何校正方法对其进行统计实验,得到了不同地形SAR实时图几何校正方法选取的准则。     

多特征差分核支持向量机模型的湿地变化检测

文章通过对不同特征空间、不同时相信息和不同类别引入多核函数组合和类别加权方式,构建了基于多特征差分核的加权支持向量机变化检测模型,能够获得平衡样本大小、综合多特征空间的变化检测结果.以上海崇明岛东端地区为例,利用4期ETM+/TM影像数据,基于构建的SVM变化检测模型,最终得到研究区湿地资源的空间变化格局,结果表明检测模型能够有效、准确地提取多种湿地变化类别的空间分布信息;并从景观水平上对检测结果进行格局分析,为湿地保护和管理提供科学参考.     

New brown dwarf candidates in the Pleiades

We have performed deep, wide‐field imaging on a ∼0.4 deg² field in the Pleiades (Melotte 22). The selected field was not yet target of a deep search for low mass stars and brown dwarfs. Our limiting magnitudes are R ∼ 22 mag and I ∼ 20 mag, sufficient to detect brown dwarf candidates down to 40 M_J. We found 197 objects, whose location in the (I, R – I) color magnitude diagram is consistent with the age and the distance of the Pleiades. Using CTK R and I as well as JHK photometry from our data and the 2MASS survey we were able to identify 7 new brown dwarf candidates. We present our data reduction technique, which enables us to resample, calibrate, and co‐add many images by just two steps. We estimate the interstellar extinction and the spectral type from our optical and the NIR data using a two‐dimensional χ² fitting (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Cosmic‐ray rejection for single spectroscopic CCD images by means of template matching

This article describes a novel algorithm for cosmic‐ray rejection in single spectroscopic CCD images. This algorithm is based on a variation of template matching. It focuses on identifying those pixels belong to spectra, while other conventional algorithms tried to locate the cosmic‐ray hits directly. The main principle is applying template matching to find suspicious blocks, which is followed by surface patching to locate the legitimate pixels accurately. Therefore, the rest pixels are the ones corrupted by cosmic‐ray hits. Meanwhile, almost all the parameters are automatically extracted from the images. Examples of its performance are given for both simulated and observed images. It shows an advantage of significantly low false alarm rate with relatively high detection rate (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

A novel multifrequency technique for the detection of point sources in cosmic microwave background maps

In this work we address the problem of simultaneous multifrequency detection of extragalactic point sources in the maps of the cosmic microwave background. We apply a new linear filtering technique, the 'matched matrix filters', that incorporates full spatial information, including the cross-correlation among channels, without making any a priori assumption about the spectral behaviour of the sources. A substantial reduction of the background is achieved thanks to the optimal combination of filtered maps. We describe the new technique in detail and apply it to the detection of radio sources and estimation of their parameters in realistic all-sky Planck simulations at 30, 44, 70 and 100 GHz. Then, we compare the results with the single-frequency approach based on the standard matched filter, in terms of reliability, completeness and flux accuracy of the resulting point source catalogues. The new filters outperform the standard matched filters for all these indexes at 30, 44 and 70 GHz, whereas at 100 GHz both kinds of filters have a similar performance. We find a notable increment of the number of true detections for a fixed reliability level. In particular, for a 95 per cent reliability we practically double the number of detections at 30, 44 and 70 GHz.     

Wavelet domain Bayesian denoising of string signal in the cosmic microwave background

An algorithm is proposed for denoising the signal induced by cosmic strings in the cosmic microwave background. A Bayesian approach is taken, based on modelling the string signal in the wavelet domain with generalized Gaussian distributions. Good performance of the algorithm is demonstrated by simulated experiments at arcminute resolution under noise conditions including primary and secondary cosmic microwave background anisotropies, as well as instrumental noise.     

Automatic morphological classification of galaxy images

We describe an image analysis supervised learning algorithm that can automatically classify galaxy images. The algorithm is first trained using manually classified images of elliptical, spiral and edge-on galaxies. A large set of image features is extracted from each image, and the most informative features are selected using Fisher scores. Test images can then be classified using a simple Weighted Nearest Neighbour rule such that the Fisher scores are used as the feature weights. Experimental results show that galaxy images from Galaxy Zoo can be classified automatically to spiral, elliptical and edge-on galaxies with an accuracy of ∼90 per cent compared to classifications carried out by the author. Full compilable source code of the algorithm is available for free download, and its general-purpose nature makes it suitable for other uses that involve automatic image analysis of celestial objects.