O-rich SR and Mira variables in DENIS

Previous VLA observations of the triple radio continuum source in Serpens showed that it has very unusual and extraordinary characteristics. While this source is associated with a star forming region, its outer components exhibit a combination of thermal and nonthermal spectra and large proper motions, Furthermore, the NW lobe has knotty and extended emission connecting the central source with the bright outer knot. Here, we present results of new VLA radio continuum high-angular resolution observations of this Radio Jet. Combining these observations with those obtained previously, we find that: a) one of the knots along the main body of the radio jet (knot G) exhibits proper motions similar to those observed in the outer NW and SE components, and the time variable knot A; b) the outer knots are moving away from the central source in slightly different directions; and c) the orientation of the central source seems to change with time. These results are consistent with a central precessing source that undergoes periodic ejection of material.     

AMT勘查贵州铁(稀土)多金属矿效果分析

贵州铁(稀土)多金属矿资源储量丰厚,但是因其赋存条件的特殊性,勘查具有一定的挑战性,在此开展铁(稀土)多金属矿的物探方法试验研究,对今后勘查工作具有重要的指导意义。这里简要介绍了AMT(音频大地电磁法)工作方法以及贵州威宁秋木构工区的地质和地球物理特征,重点讨论了AMT在秋木构工区铁(稀土)多金属矿勘查中的应用效果,通过对电阻率断面图的综合推断解释,划分出了二叠系宣威组与峨嵋山玄武岩组地层界面,圈出了含矿有利部位。经钻孔验证,取得了良好的找矿效果。     

加速迭代硬阈值ISAR稀疏成像

加速迭代硬阈值(AIHT)作为一种压缩感知(CS)算法,具有计算复杂度低、内存占用小的特点,在较小数目的观测下,经过有限次迭代便能获得较好的重建效果。因此,本文将该算法应用到逆合成孔径雷达(ISAR)稀疏成像,对该方法的具体特征和适用性进行了详细分析。仿真结果表明,在相同信噪比和回波脉冲数条件下,基于AIHT的ISAR成像方法,相比于稀疏贝叶斯算法(SBL),在重建时间上缩短了至少2个量级;相比于迭代加权最小二乘法(IRLS)和平滑l0范数算法,在重建质量上提高了约3倍。经实测数据处理结果验证,在1/4原始脉冲数条件下,该方法仍具有良好的聚焦性能和压低旁瓣效果。     

稳健估计下的坐标系统转换总体最小二乘算法

针对传统的应用最小二乘法建立高斯-马尔科夫(G-M)模型实现坐标系统转换的方法导致转换模型参数精度低下的问题,该文提出一种基于总体最小二乘算法的坐标系统转换方法。考虑到粗差会导致控制点坐标精度差异较大,因此根据稳健估计理论进行迭代定权,在总体最小二乘算法下建立G-M模型,以便求解转换模型参数,并通过算例比较不同算法的转换精度。实验结果表明:基于稳健估计的总体最小二乘抗差算法实现的空间坐标转换精度高于传统方法的转换精度。     

扎龙保护区丹顶鹤栖息地适宜性评价

结合TM影像和ENVISAT ASAR(HH/HV)数据,以扎龙保护区丹顶鹤栖息地为研究对象,在分布式定量提取评价因子(植被类型、生境结构、巢下水深、植被盖度、人为干扰)的基础上,建立HSI模型对丹顶鹤栖息地质量进行评价,并根据实测巢址空间分布情况对评价结果进行验证。结果表明:基于主观专家知识建立的HSI模型得到丹顶鹤高适宜栖息地面积为48km2,适宜栖息地面积为265km2,低适宜栖息地面积为385km2,不适宜栖息地面积为1 403km2,结合实测数据验证,得出高适宜、适宜和低适宜栖息地巢址共占实测巢址的92.86%,不适宜栖息地巢址占7.14%。经检验HSI模型对淡水沼泽湿地典型水禽栖息地的质量评价有良好的适用性。     

基于ETM~+数据和GIS技术的缅甸铜金矿成矿预测

在利用遥感数据和地理信息系统(GIS)技术的矿产资源勘查与评价中,矿化蚀变信息提取和构造信息提取起着至关重要的作用。以缅甸铜金矿为例,利用ETM+遥感图像,采用比值法、阈值分割和主成分分析(PCA)提取羟基蚀变信息;利用数字高程模型和遥感数据提取与铜金矿化有关的线环构造,结合地质资料和上述信息,利用证据权和分形方法进行整合,确定该研究区的成矿远景区。结果发现,已知铜金矿均分布于成矿靶区中,综合信息可为下一步的矿产资源勘探工作提供决策依据。     

Discovery of a new blue quasar: SDSS J022218.03–062511.1

We report the discovery of a bright blue quasar: SDSS J022218.03–062511.1. This object was discovered spectroscopically while searching for hot white dwarfs that may be used as calibration sources for large sky surveys such as the Dark Energy Survey or the Large Synoptic Survey Telescope project. We present the calibrated spectrum, spectral line shifts and report a redshift of z = 0.521±0.0015 and a rest‐frame g‐band luminosity of 8.71×10¹¹ L_⊙. (© 2015 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Ultraviolet spectroscopic study of EU UMa and ST LMi from HST and IUE observations

We present the first orbit-resolved ultraviolet spectroscopic observations of the two polar systems EU UMa and ST LMi obtained with the Hubble Space Telescope Faint Object Spectrograph (HST FOS) and International Ultraviolet Explorer (IUE) during their intermediate- and low-luminosity states in the period between 1982 and 2003. Different line profiles of the two systems showing variations of line fluxes at different orbital phases are presented. This paper focuses on the C IV emission line at 1550 Å produced in the accretion stream, presenting calculations of spectral line fluxes, ultraviolet luminosities, and accretion rates for the two systems. Our analysis of the spectroscopic data reveals changes with orbital phase of the emission line profiles that correspond to the light curve variations of both EU UMa and ST LMi in the optical and infrared bands. The variations of line fluxes are attributed to variations of both density and temperature as a result of a changing rate of mass transfer from the secondary star to the white dwarf. The ultraviolet luminosity and accretion rate of EU UMa are smaller than the ultraviolet luminosity and accretion rate of ST LMi.