Hemispheric Imaging of Galactic Neutral Hydrogen with a Phased Array Antenna System

The thousand element array (THEA) system is a phased array system consisting of 1 m² tiles having 64 Vivaldi elements each, arranged on a regular 8-by-8 grid, which has been developed as a demonstrator of technology and applicability for SKA. In this paper we present imaging results of Galactic neutral hydrogen with THEA. Measurements have been taken using a dense 2-by-2 array of four tiles as a four tile adder. The results are compared with results from the Leiden-Dwingeloo Survey, showing qualitative agreement, but also indicating that further studies are needed on the instrumental characteristics.     

Effective Sensitivity of A Non-uniform Phased Array of Short Dipoles

Short dipoles are a key element in new low frequency array antennas as proposed for LOFAR and other astronomical applications. Unfortunately standard texts on short dipole antennas are based on the effective area and do not lead to an astronomically useful sensitivity formulation in a straightforward manner. The concept of maximum effective area is applied to arrays of short dipoles and allows expressing the sensitivity as the ratio of this area over the effective sky brightness temperature as long as the output noise power is dominated by the antenna input radiation. For both quantities we only need to know the array directivity pattern that includes the mutual coupling effects when the actual loading conditions of the array elements are taken into account. Short dipole elements have a constant directivity pattern for frequencies below resonance, but they exhibit strong complex impedance variations that provide only narrow band performance when power matching is applied as required in transmit applications. However, in receive applications voltage or current sensing can be realized, for example with an active balun. Assisted by the steep increase of the sky brightness with wavelength for frequencies below 300 MHz, this can provide sky noise dominated performance over at least a three to one frequency range. Still the low frequency limit is determined by the amplifier noise contribution and the losses in the antenna and in the dielectric ground surrounding the elements. We show that for a sparse array with the elements non-uniformly distributed according to an exponential shell model, a constant sensitivity can be obtained over a frequency range of at least two octaves. In addition, such a configuration has a factor of six greater sensitivity than a rectangular array for a large part of the frequency band.     

电荷守恒与CCD孔径测光

Lick天文台的CCD控制器是一类新型控制器,它能够在同一CCD系统内实现MPP(Multi—pinned phase)和通常工作模式间的转换．自2002年起中国至少有4架 CCD照相机使用这类控制器．此控制器的弱点是溢出发生在非线性前,而且远在饱和以前．虽然这对亮的面光源观测不利,并且它妨碍了使用亮星构建点扩散函数(psf)．但是由于电荷守恒原理,对亮的点源(恒星)的孔径测光依然可行．观测证明了此结论．     

HY-2B星载GPS数据质量及简化动力学精密定轨分析

对HY-2B卫星星载GPS数据进行质量检查,分析伪随机脉冲先验值对简化动力学精密定轨的影响。结果发现,在所有时间间隔中,先验标准差为1×10^-8 m/s²时定轨精度最高,最优伪随机脉冲时间间隔为6 min。估计天线相位中心变化（PCV）,分析不同分辨率（10°×10°、5°×5°）PCV模型对定轨结果的影响,并使用载波相位残差、重叠轨道比较和SLR检核对定轨结果进行检验。结果表明,99%以上的历元能观测到4颗以上GPS卫星,数据完整率达到99.65%,L1、L2波段的多路径误差RMS均值分别为15.7 cm、9.5 cm,证明HY2国产接收机性能良好。轨道内符合精度均达到cm级;未加PCV模型时,SLR检核RMS值为27.8 mm,加入10°×10°、5°×5° PCV模型后,SLR检核RMS值分别提高0.9 mm和1.2 mm,说明轨道外符合精度也达到cm级。     

北斗三号卫星天线相位中心改正模型对精密定轨和定位的影响

基于实测数据分析天线相位中心PCO改正模型和观测值频点选择对北斗三号卫星精密定轨和定位的影响。结果表明,基于北斗官方CSNO发布的PCO模型定轨定位表现稍优于IGS协议模型。此外,相较于两者PCO模型差异的影响,B1C/B2a与B1I/B3I观测值频点的选择对精密定位影响更为显著。以IGS B1I/B3I PCO模型为参考,CSNO B1C/B2a PCO模型定位坐标在E、N、U方向上的精度分别提升约5%、13%、14%,可应用于北斗高精度数据处理。     

Research on influencing factors of coupling in SIMO antenna

In the process of radar data acquisition,limited amount of information can be provided to post-processing interpretation by the data acquisition method of single-input and single-output,however,the location and physical parameter information of geological body can be obtained more accurately by using Multi-Input Multi-Output(MIMO)antenna with multiple transmitters and multiple receivers.Especially when collecting borehole radar data and the aperture is very narrow,but the antenna is required to be able to ensure better results in a larger frequency band,therefore,the size of the antenna will be greatly challenged.Meanwhile,the close arrangement of multiple transmitting and receiving antennas will inevitably affect the signal radiation.Based on the borehole radar,this paper simulates and optimizes the Single-Input Multi-Output antenna(SIMO antenna),the size of which meets the aperture requirements,using HFSS antenna simulation software,and explores the factors affecting the antenna return loss and isolation.Among them,the radius of the dipole has little effect on the return loss and isolation,whereas increasing the number of receiving antennas or increasing the transceiver distance will significantly affect the antenna coupling,with a significant reduction in the amplitude of isolation.     

基于两步最小均方的宽带波束形成算法

针对空时二维滤波器结构,提出了修正两步最小均方波束形成算法,通过修正每次迭代运算中的期望阵列响应幅度和方向矩阵,显著地减少了矩阵运算量,达到快速准确求解期望方向图的相位和相应权矢量的目的。该算法在不改变天线阵元数的情况下,比传统空域滤波增加了时域处理维数,提高了波束形成质量,并利用了期望方向图相位的随机性,通过迭代更新期望方向图的相位和相应权矢量,实现了方向图的旁瓣控制,理论上可以形成任意控制的旁瓣波束,满足不同应用场合的需求。经计算机仿真实验,算法可以很好的收敛到期望的方向图,验证了该算法的有效性。该算法可广泛应用于多天线的GNSS导航接收机或抗干扰接收机中,在提高接收机在复杂环境下的可用性和灵敏度上具有重要的意义。     

GNSS天线相位中心偏差检定及不确定度分析

GNSS天线相位中心偏差是GNSS天线接收卫星信号的电气中心与其机械几何中心之差。相位偏差具有一定的稳定性,呈现系统误差性质。现行规程将相位偏差按限差要求加以检测,而没有按系统误差加以检定并进行改正,本文对规程的检定方法加以改进,定量检定天线相位偏差半径r和偏差角a,并依据r值的大小,给出相位偏差在GNSS测量中的采用原则,对两种改进方法进行了测量不确定度分析。     

一种新型测地线双锥天线的研究

介绍了一种新型测地线双锥天线,该天线能够实现全方位面上的波束扫描,具有广阔的应用空间。采用几何光学法结合测地线理论分析了其工作原理,重点阐述了圆柱面上射线传输路径的问题,并对该天线在单端口和双端口激励情况下的方向图分别进行了分析和计算。在以上基础上,设计加工完成了一款工作在6～8 G Hz的新型测地线双锥天线,给出了其具体结构和尺寸。理论结果与实测结果具有较好的一致性,表明了几何光学法在测地线双锥天线分析和设计中的适用性。     

新一代天气雷达天馈系统故障分析诊断方法和技巧

故障分析诊断技术对保障气象大型装备可靠业务运行具有重要作用。依据CINRAD/SB型新一代天气雷达天馈系统信号流程,通过对新一代天气雷达天馈系统故障诊断方法进行研究,总结出天馈系统漏气、打火故障检测方法,天馈系统损耗大的故障诊断流程和故障定位6种方法。按照故障诊断流程和其中的外接信号源联合频谱仪法,分析诊断、定位并修复了天馈系统天线座内环流器故障导致的雷达观测回波强度偏弱、灵敏度降低故障的典型个例。结果表明,根据雷达现场配备仪表状况,通过故障诊断流程,采用合适方法和技巧,可达到快速定位天馈系统故障部位、在最短时间修复雷达故障目的。