基于独立成分分析的高光谱变化检测

现有的变化检测方法并未充分研究变化前后高光谱遥感影像端元的联系,不能准确地分析地物变化信息。本文提出了一种基于独立成分分析的高光谱遥感影像变化检测方法,对差值影像进行基于偏斜度的独立成分分析,在不同组分图中分别显示单一地物的变化情况,进而提取变化信息。实验表明,该方法能够在获得较高检测率的同时维持较低的误检率,检测效果优于传统方法。     

一种融合中分辨率多光谱与高分辨率全色图像的方法

针对中分辨率多光谱与高分辨率全色图像空间分辨率差异大,导致融合结果难以较好平衡光谱信息保持和空间信息保持能力的问题,该文分析了7种常用融合方法用于中分辨率多光谱与高分辨率全色图像融合的优缺点及其融合质量的影响因素,提出了一种组合融合方法。该方法在保留Gram-Schmidt方法的细节注入方式的基础上,综合利用高通滤波法和Gram-Schmidt方法的优势构造低分辨率全色图像,确保在提高融合图像空间分辨率的同时有效降低其光谱变形。通过CBERS-02多光谱和IRS-P5全色图像的实验,证明了新融合方法的有效性。     

Late-time photometry of two nearby type II-P supernovae： 2004dj and 2004et

We present late-time photometry for two bright type II-P supernovae （SNe） 2004dj and 2004et, extending over 400 d after the explosion, which are measured with a set of intermediate-band filters that have the advantage of tracing the strength variations of some spectral features. Although these two SNe II-P exhibit similar photometric evolution at earlier times, they diverge during the nebular phase. SN 2004dj shows a slow late-time decline rate with - 0.7 ±0.1 mag （100d）^-1 during the period ranging from t ≈ 200 - 300 d after the explosion, while SN 2004et shows a much faster decline rate at a comparable phase, e.g., 1.3 ± 0.1 mag （100d）^-1. The steeper decay rate seen in SN 2004et is likely due to dust formation in the explosion ejecta. Based on intermediate-band photometry, we derived the evolution of the feature lines [e.g., Hα] of SNe 2004dj and 2004et which are similar in flux at comparable phases but perhaps with significantly different decay rates. The origin of the observed variations in the continuum and the feature lines is briefly discussed.     

群星的族谱——天文学星表纵览（5）

（接上期） 二十世纪初摄影术的出现,不仅自身成为天文研究的得力工具,还唤醒了沉寂多年的分光术。虽然早在1817年普鲁士的夫朗和费（Joseph Fraunhofer）就用自己发明的分光计发现了太阳光谱中的暗线。     

A modified stratified model for the 3C 273 jet

We present a modified stratified jet model to interpret the observed spectral energy distributions of knots in the 3C 273 jet. Based on the hypothesis of the single index of the particle energy spectrum at injection and identical emission processes among all the knots, the observed difference of spectral shape among different 3C 273 knots can be understood as a manifestation of the deviation of the equivalent Doppler factor of stratified emission regions in an individual knot from a characteristic one. The summed spectral energy distributions of all ten knots in the 3C 273 jet can be well fitted by two components: a low-energy component (radio to optical) dominated by synchrotron radiation and a high-energy component (UV, X-ray and γ-ray) dominated by inverse Compton scattering of the cosmic microwave background. This gives a consistent spectral index of α= 0.88 (Sv α v-α) and a characteristic Doppler factor of 7.4. Assuming the average of the summed spectrum as the characteristic spectrum of each knot in the 3C 273 jet, we further get a distribution of Doppler factors. We discuss the possible implications of these results for the physical properties in the 3C 273 jet. Future GeV observations with GLASTcould separate the γ-ray emission of 3C 273 from the large scale jet and the small scale jet (i.e.the core) through measuring the GeV spectrum.     

Automated spectral classification using template matching

An automated spectral classification technique for large sky surveys is pro-posed. We firstly perform spectral line matching to determine redshift candidates for an observed spectrum, and then estimate the spectral class by measuring the similarity be-tween the observed spectrum and the shifted templates for each redshift candidate. As a byproduct of this approach, the spectral redshift can also be obtained with high accuracy. Compared with some approaches based on computerized learning methods in the liter-ature, the proposed approach needs no training, which is time-consuming and sensitive to selection of the training set. Both simulated data and observed spectra are used to test the approach; the results show that the proposed method is efficient, and it can achieve a correct classification rate as high as 92.9%, 97.9% and 98.8% for stars, galaxies and quasars, respectively.     

统计SDSS-DR7中的CEMP星并分析其温度和光谱型

统计了SDSS(The Sloan Digital Sky Survey)最新发布的DR7(Data Release 7)数据中的CEMP星(Carbon-Enhanced Metal-Poor Stars).分析了样本的温度、光谱型、颜色等物理参量,同时给出了CEMP星在SDSS贫金属星中占的比例约为11%.统计得到SDSS_SSPP(The SEGUE Stellar Parameter Pipeline)发布的CEMP星样本的温度主要集中在6000～9000 K范围内.采用PLSR(偏最小二乘回归)方法计算样本的温度并给出其光谱型,结果显示与SSPP发布的温度比较没有系统误差,但在温度较高时,随机误差较大,这与SSPP中采用不同方法给出的温度值是一致的.从颜色-颜色图上看,选出的CEMP星主要包含两类星:BHB/BS和F(F Turn-Off),前者温度较高且温度误差相对较大.通过样本在Log(g)-颜色图上的划分,可以区分BHB和BS样本.最后讨论了BHB/BS和F(F Turn-Off)中C元素的来源.     

西北地区典型地物光谱数据库建设

使用FieldSpecProFR2500便携式光谱仪,在甘肃典型区域,测定了一些特色农作物和典型植被的反射光谱。利用计算机编程技术,建立了西北地区典型地物光谱数据库。文章主要介绍了光谱数据的采集,数据库系统的建立过程以及数据库的应用和存在的一些问题。     

大分子烃类拉曼光谱特征及在烃包裹体研究中的意义

拉曼光谱分析发现,无论大分子烃类含碳数如何不同,分子结构如何复杂,大分子烃类的拉曼谱图有很多相同性,即烃类的拉曼谱图只受烷烃骨架、环烷基和苯环等的影响,并由此形成了四类大分子烃类的拉曼谱图：烷烃类、复杂烷烃类（以环烷基为主）、结构平坦相连的芳香烃类和结构复杂的芳香烃类。烃是石油的主要组分,因此,被包裹在矿物中的石油——烃包裹体的拉曼谱图也只有四种：发强荧光烃包裹体、含沥青烃包裹体、含低碳数芳烃包裹体和烷烃包裹体。激光拉曼对烃包裹体组分有个总体特征的体现,用激光拉曼分析烃包裹体组分中具体烃的种类是不科学的。但通过烃包裹体的拉曼谱图特征,可以研究烃包裹体组分特征、古油藏成熟度及油气演化程度等信息。     

Sentinel-2密集时间序列数据和Google Earth Engine的潮间带湿地快速自动分类

潮间带湿地是滨海湿地的重要组成部分,具有维持生物多样性、促进碳汇等重要生态功能.及时、准确地掌握潮间带湿地现状是实现潮间带湿地可持续管理目标的基础.先前的潮间带湿地分类研究依赖于训练样本、人工设定阈值或后处理等,本研究基于GEE (Google Earth Engine)平台开发一种自动、快速、高精度的潮间带湿地分类方...