XMM-Newton study of soft excess X-ray emission in clusters of galaxies

We discuss the detection of soft excess X-ray emission in a sample of 19 clusters of galaxies observed by XMM-Newton. In 6/19 clusters evidence for a soft X-ray excess is found. Four of these clusters show soft X-ray and O VII line emission from gas with a temperature of 0.2 keV. The centroid of this oxygen line is consistent with the redshift of the cluster. The intensity and spatial extend of the soft excess agrees with previous PSPC measurements. These observations are interpreted as emission from warm-hot intergalactic medium filaments, with density enhancements near the cluster centers, consistent with theoretical predictions. In the other two soft excess clusters a non-thermal origin is consistent with the data.     

Evolution of galaxy cluster scaling from XMM-Newton observation of the galaxy clusters at z ⩾ 0.4

We present here new XMM-Newton observations of 3 relatively cool clusters at z ≈ 0.4, complemented by archival observations of 3 other clusters at similar redshift. We derived the M–T and R–T relations from the hydrostatic equation using an isothermal temperature distribution.     

XMM-Newton survey of non-thermal shell candidates: Preliminary results on DA 530

The investigation of the general properties of non-thermal (NT) X-ray shell supernova remnants (SNRs), of which SN 1006 is the prototype, is important to understand how electrons are accelerated in SNR shocks and what is the origin of cosmic rays. Using the XMM-Newton satellite, we are carrying on a survey of putative non-thermal SNR candidates previously unknown or little studied in the X-ray band, in order to investigate the different manifestations of NT emission in SNR shells. The SNRs we have selected are likely to expand in a low density medium, and therefore to have a low thermal X-ray emission, that usually outshines the non-thermal one. We report here preliminary results obtained on the SNR shell DA 530.     

用大面积源检定核应急机载/车载伽玛能谱仪

人工核素大面积源标准是核工业航测遥感中心等单位经过十余年研究建立的新型计量保障标准,使用该标准,可对监测核应急伽玛辐射环境的机载/车载伽玛能谱仪进行检定.使用大面积源标准检定,可以有效地弥补因机载/车载伽玛能谱仪系统的角响应影响因素复杂而难于模拟计算的缺陷,为监测核应急伽玛辐射环境的机载/车载伽玛能谱仪提供了量值传递的保障.本文介绍了大面积源检定的原理和技术方法.     

A neutral gas mass spectrometer to measure the chemical composition of the stratosphere

The Polar Balloon Atmospheric Composition Experiment (P-BACE) is a new generation of neutral gas mass spectrometer based on the time-of-flight principle. P-BACE is the scientific experiment on the Mars Environment Analog Platform (MEAP) flown successfully on a balloon mission in summer 2008. The MEAP mission was flown with a 334,000 m³ helium balloon in the stratosphere on a semicircular trajectory from northern Sweden around the North Pole to Canada using the summer northern hemispheric wind current. The atmospheric conditions at an atmospheric altitude of 35–40 km are remarkably similar to those on the surface of Mars and thus the balloon mission was an ideal testbed for our mass spectrometer P-BACE. Originally this instrument was designed for in situ measurements of the chemical composition of the Martian atmosphere.P-BACE has a unique mass range from 0 to 1000 amu/q with a mass resolution m/Δm (FWHM) > 1000, and the dynamic range is at least six orders of magnitude. During this experiment, the acquisition of one mass spectrum is a sum of 65,535 single spectra, recorded in a time frame of 66 s.The balloon mission lasted 5 days and had successfully demonstrated the functionality of the P-BACE instrument during flight conditions. We had recorded more than 4500 mass spectra. With little modifications, P-BACE can be used on a planetary mission for Mars, but for example also for Venus or Mercury, if placed on a satellite.     

金属多层膜超晶格结构研究

用高分辨的三晶体x—射线衍射仪测量了Zr、Cu金属交替的多层膜的x—射线小角反射谱。用扩展了的Born—wolf光学模型对Zr、Cu多层膜的x—射线小角反射数据进行了定量分析。结果表明，该金属多层膜在其生长方向具有超晶格结构。在两层金属膜之间的界面上，由于内扩散，形成了界面交混层，它使x—射线小角反射所产生的高阶Bragg峰的强度减弱。由于两种金属膜的晶格不匹配，使高阶Bragg峰加宽。界面的粗糙度可用来模拟x—射线小角反射曲线的阻尼振荡效应。     

星载SAR在轨成像实时处理算法研究

星载合成孔径雷达(SAR)分辨率和幅宽的不断提高,其产生的原始数据率越来越大,采用在轨实时成像处理形成图像,在图像域再进行传统的图像数据处理和传输,有助于降低星-地数据传输速率,为了提高星载SAR在轨成像处理的实时性,文章分析了星上特殊条件对星载SAR处理算法实时性所提出的约束,对RD、波束域、CS等经典的星载SAR成像处理算法的运算量进行了比较,以CS算法为例,研究了相位补偿因子对CS成像处理算法的实时性影响,提出了一种补偿因子区域不变的CS成像算法,它极大地减少了成像处理算法的运算量,并通过仿真实验结果验证了该算法的有效性。     

三维激光成像系统的点云模型真彩色处理方法

三维激光成像系统获得的点云数据精度高并且保有高精度的高程信息,然而特征信息不明显,没有保留全部的点和点的拓扑关系,无法直接判读地面物体;影像数据空间分辨率和精度低,并且缺少高程信息,然而其影像的特征连续,光谱信息丰富.因此,进行点云数据与影像数据融合方法的研究是目前三维激光成像系统研制的前沿性课题.针对点云数据与影像数据融合方法的研究,提出了一种三维激光成像系统点云模型真彩色处理的方法.实验结果显示,采用所提出的方法,不仅能够获得被扫描物体的位置信息和大小信息,而且能够得到被扫描物体的表面纹理细节信息.     

基于DCT-CS的脉冲星周期超快速估计方法

受快速傅里叶变换（fast Fourier transform，FFT）的影响，基于FFT和压缩感知（compressive sensing, CS）的脉冲星周期快速估计算法的计算量大。为进一步减小计算量并提高计算精度，利用离散余弦变换（discrete cosine transform，DCT)取代FFT，提出了一种基于DCT-CS的脉冲星周期超快速估计算法。在该方法中，利用DCT提取脉冲星信号的低频部分构建低频DCT矩阵；构建畸变轮廓字典并获取累积轮廓；提出了利用最大值超分辨率稀疏恢复估计脉冲星周期的方法。仿真结果表明，DCT-CS的脉冲星周期估计精度达到了3.82×10-12 s，计算时间达到了9.31 ms。与FFT-CS相比，周期估计精度提高了约16%，计算时间缩短了约37.5%，实现了实时高精度的脉冲星周期估计。     

Soft X-ray observations of helmet structures from SXT/Yohkoh

We present soft X-ray observations of helmet structures in solar active regions obtained from SXT/Yohkoh. These helmet structures are observed to form in the flare decay phase and to be associated with active region loop interactions. Their morphology is similar to the much larger scale helmet streamers that appear in the outer corona as shown in optical images of solar eclipse. The observed X-ray helmet structures appear to be in quasi-equilibrium with lifetimes greater than the MHD time scale. Using the filter ratio method for the X-ray observations, we find that the cusp region has lower temperature and higher density than that in the stalk region above it. The plasma pressure in the cusp region is about the same or slightly higher than that in the stalk region.